FN Thomson Reuters Web of Science™ VR 1.0 PT J AU McKernan, B Ford, KES Kocsis, B Haiman, Z AF McKernan, B. Ford, K. E. S. Kocsis, B. Haiman, Z. TI Ripple effects and oscillations in the broad Fe K alpha line as a probe of massive black hole mergers SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE accretion, accretion discs; gravitational waves; radiation mechanisms: general; planet-disc interactions; protoplanetary discs; galaxies: active ID ACTIVE GALACTIC NUCLEI; X-RAY SPECTROSCOPY; GAS PILE-UP; GRAVITATIONAL-WAVES; ACCRETION DISCS; ELLIPTIC GALAXIES; STANDARD SIRENS; EMISSION-LINES; BINARY-SYSTEMS; STRONG GRAVITY AB When a sufficiently massive satellite (or secondary) black hole is embedded in a gas disc around a (primary) supermassive black hole, it can open an empty gap in the disc. A gap-opening secondary close to the primary will leave an imprint in the broad component of the Fe K alpha emission line, which varies in a unique and predictable manner. If the gap persists into the innermost disc, the effect consists of a pair of dips in the broad line which ripple blue-ward and red-ward from the line centroid energy, respectively, as the gap moves closer to the primary. This ripple effect could be unambiguously detectable and allow an electromagnetic monitoring of massive black hole mergers as they occur. As the mass ratio of the secondary to primary black hole increases to q greater than or similar to 0.01, we expect the gap to widen, possibly clearing a central cavity in the inner disc, which shows up in the broad Fe K alpha line component. If the secondary stalls at >= 10(2)r(g) in its in-migration, due to low corotating gas mass, a detectable ripple effect occurs in the broad line component on the disc viscous time-scale as the inner disc drains and the outer disc is dammed. If the secondary maintains an accretion disc within a central cavity, due to dam bursting or leakage, a periodic 'see-saw' oscillation effect is exhibited in the observed line profile. Here, we demonstrate the range of ripple effect signatures potentially detectable with Astro-H and IXO/Athena, and oscillation effects potentially detectable with XMM-Newton or LOFT for a wide variety of merger and disc conditions, including gap width (or cavity size), disc inclination angle and emissivity profile, damming of the accretion flow by the secondary, and a minidisc around the satellite black hole. A systematic study of ripple effects would require a telescope effective area substantially larger than that planned for IXO/Athena. Future mission planning should take this into account. Observations of the ripple effect and periodic oscillations can be used to provide an early warning of gravitational radiation emission from the AGN. Once gravitational waves consistent with massive black hole mergers are detected, an archival search for the Fe K alpha ripple effect or periodic oscillations will help in localizing their origin. C1 [McKernan, B.; Ford, K. E. S.] CUNY, Borough Manhattan Community Coll, Dept Sci, New York, NY 10007 USA. [McKernan, B.; Ford, K. E. S.] Amer Museum Nat Hist, Dept Astrophys, New York, NY 10024 USA. [McKernan, B.; Ford, K. E. S.] CUNY, Grad Ctr, New York, NY 10016 USA. [Kocsis, B.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Haiman, Z.] Columbia Univ, Dept Astron, New York, NY 10027 USA. RP McKernan, B (reprint author), CUNY, Borough Manhattan Community Coll, Dept Sci, New York, NY 10007 USA. EM bmckernan@amnh.org RI Kocsis, Bence/C-3061-2013 OI Kocsis, Bence/0000-0002-4865-7517 FU NASA [NNX11AE05G] FX We acknowledge very useful discussions with Clement Baruteau, Laura Blecha, Massimo Dotti, Frits Paerels, Alberto Sesana and Tahir Yaqoob. We thank Allyn Tennant for maintaining Web-QDP and HEASARC at NASA GSFC for maintaining Webspec. We acknowledge support from NASA grant NNX11AE05G (to ZH). NR 120 TC 14 Z9 14 U1 0 U2 5 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 JUN PY 2013 VL 432 IS 2 BP 1468 EP 1482 DI 10.1093/mnras/stt567 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 156OP UT WOS:000319832300049 ER PT J AU Rapaport, LG Kloc, B Warneke, M Mickelberg, JL Ballou, JD AF Rapaport, Lisa G. Kloc, Briana Warneke, Mark Mickelberg, Jennifer L. Ballou, Jonathan D. TI Do mothers prefer helpers? Birth sex-ratio adjustment in captive callitrichines SO ANIMAL BEHAVIOUR LA English DT Article DE callimico; Callimico goeldii; fragile male hypothesis; golden lion tamarin; Leontopithecus rosalia; local resource enhancement hypothesis; secondary sex ratio ID LOCAL RESOURCE COMPETITION; LION TAMARINS LEONTOPITHECUS; HUNGARIAN GYPSY POPULATION; MONKEYS CALLIMICO-GOELDII; AT-THE-NEST; INFANT CARE; CALLITHRIX-JACCHUS; WILD; STRATEGIES; SELECTION AB Parental investment theory predicts that natural selection will favour a parental ability to bias the offspring sex ratio in favour of that which will yield the highest benefit-cost payoff. The local resource enhancement hypothesis posits that in cooperative breeders, parents may favour offspring that will mitigate parental effort by helping to raise younger siblings. Conversely, the fragile male hypothesis suggests that parents will adjust the sex ratio in favour of the sex that experiences higher mortality. We examined international studbook data of two cooperatively breeding primate species with differing reproductive strategies: golden lion tamarins, Leontopithecus rosalia, which typically give birth to twins, and callimicos, Callimico goeldii, which almost always give birth to singletons. The tamarins showed a stronger secondary sex-ratio bias in favour of males than did the callimicos, as predicted by the local resource enhancement hypothesis, because tamarins sustain higher per-parturition costs and because sons may invest more effort in caring for their younger siblings than do daughters. However, a generalized linear regression failed to reveal factors that may influence this variation. There was no significant predictor of male bias based on mother's age, mother's number of previous parturitions or group size. Contrary to predictions of the fragile male hypothesis, sons were no less likely to survive the postnatal period of parental investment than were daughters. A greater understanding of this phenomenon is needed because the adult sex-ratio bias in favour of males has become so pronounced, especially in golden lion tamarins, as to cause management difficulties for the conservation of these endangered species. (C) 2013 The Association for the Study of Animal Behaviour. Published by Elsevier Ltd. All rights reserved. C1 [Rapaport, Lisa G.; Kloc, Briana] Clemson Univ, Dept Biol Sci, Clemson, SC 29634 USA. [Warneke, Mark] Chicago Zool Soc Brookfield Zoo, Brookfield, IL USA. [Mickelberg, Jennifer L.; Ballou, Jonathan D.] Smithsonian Conservat Biol Inst, Ctr Conservat & Evolutionary Genet, Front Royal, VA USA. RP Rapaport, LG (reprint author), Clemson Univ, Dept Biol Sci, 132 Long Hall, Clemson, SC 29634 USA. EM lrapapo@clemson.edu NR 44 TC 3 Z9 3 U1 2 U2 71 PU ACADEMIC PRESS LTD- ELSEVIER SCIENCE LTD PI LONDON PA 24-28 OVAL RD, LONDON NW1 7DX, ENGLAND SN 0003-3472 J9 ANIM BEHAV JI Anim. Behav. PD JUN PY 2013 VL 85 IS 6 BP 1295 EP 1302 DI 10.1016/j.anbehav.2013.03.018 PG 8 WC Behavioral Sciences; Zoology SC Behavioral Sciences; Zoology GA 167RM UT WOS:000320651200019 ER PT J AU Matsumasa, M Murai, M Christy, JH AF Matsumasa, Masatoshi Murai, Minoru Christy, John H. TI A low-cost sexual ornament reliably signals male condition in the fiddler crab Uca beebei SO ANIMAL BEHAVIOUR LA English DT Article DE blood glucose; blood lactate; costs; courtship; fiddler crab; reliability; sexual signal; Uca beebei ID CARCINUS-MAENAS L; FEMALE CHOICE; MATE CHOICE; ANAEROBIC METABOLISM; CONDITION DEPENDENCE; SUBSEQUENT RECOVERY; PILLAR FUNCTION; FIELD CRICKETS; HOUSE FINCH; DISPLAY AB Empirical studies of the reliability of sexual signals are needed to test the prediction that females should prefer males in good condition. We examined whether an attractive sexual signal used by male fiddler crabs, Uca beebei, reliably indicates male condition by measuring male blood glucose and lactate levels in the field. The signal is a mud structure, a 'pillar', that attracts females for mating. Blood lactate levels (a measure of energy expenditure) of pillar builders (P males) immediately after they built their pillars did not differ from those of nonbuilders (NP males), suggesting that the cost of building a pillar is small. However, P male lactate levels were significantly higher than those of NP males late in the activity cycle after P males had invested more in vigorous courtship using claw 'waving'. Whereas P males maintained their glucose levels (a measure of energy availability as the major fuel for ATP production) at around 30 mg/dl throughout their daily activity period, NP males showed significantly lower levels in the middle of the period. These results confirm that pillars reliably signal a male's condition, as measured by his ability to maintain a blood glucose level necessary for costly courtship, even though the construction of a pillar has minimal energetic cost. (C) 2013 The Association for the Study of Animal Behaviour. Published by Elsevier Ltd. All rights reserved. C1 [Matsumasa, Masatoshi] Iwate Med Univ, Ctr Liberal Arts & Sci, Yahaba, Iwate 0283694, Japan. [Murai, Minoru] Univ Ryukyus, Trop Biosphere Res Ctr, Nishihara, Okinawa 90301, Japan. [Christy, John H.] Smithsonian Trop Res Inst, Balboa, Panama. RP Matsumasa, M (reprint author), Iwate Med Univ, Ctr Liberal Arts & Sci, Dept Biol, Yahaba, Iwate 0283694, Japan. EM mmasa@iwate-med.ac.jp FU Smithsonian Tropical Research Institute; Japan Society for the Promotion of Science [10041175, 22570027] FX We thank the Smithsonian Tropical Research Institute for support and the Unidad Administrativa de Bienes Revertidos of the Ministerio de Economia y Finanzas, the Servicio Nacional Aeronaval, and the Autoridad del Canal de Panama (ACP), Republic of Panama, for access to the field site in the intertidal zone near the old Rodman Naval Base. This study was also supported by a Grant-in-Aid from the Japan Society for the Promotion of Science (No. 10041175 and 22570027). We thank also Mark Briffa and two anonymous referees for comments on an earlier draft. NR 54 TC 2 Z9 2 U1 2 U2 35 PU ACADEMIC PRESS LTD- ELSEVIER SCIENCE LTD PI LONDON PA 24-28 OVAL RD, LONDON NW1 7DX, ENGLAND SN 0003-3472 J9 ANIM BEHAV JI Anim. Behav. PD JUN PY 2013 VL 85 IS 6 BP 1335 EP 1341 DI 10.1016/j.anbehav.2013.03.024 PG 7 WC Behavioral Sciences; Zoology SC Behavioral Sciences; Zoology GA 167RM UT WOS:000320651200024 ER PT J AU Geipel, I Kalko, EKV Wallmeyer, K Knornschild, M AF Geipel, Inga Kalko, Elisabeth K. V. Wallmeyer, Katja Knoernschild, Mirjam TI Postweaning maternal food provisioning in a bat with a complex hunting strategy SO ANIMAL BEHAVIOUR LA English DT Article DE common big-eared bat; extended parental care; female care; gleaning insectivore; maternal tuition; Micronycteris microtis; postweaning investment; prey transfer; prolonged offspring dependence; social learning ID PARENT-OFFSPRING CONFLICT; VAMPIRE BAT; ECHOLOCATING BATS; CARE; EVOLUTION; BEHAVIOR; WILD; MAMMALS; PRIMATES; MEERKATS AB Adult animals of many taxa exhibit extended parental care by transferring food to inexperienced offspring, thus allocating nutritional and sometimes even informational benefits such as the acquisition of adult dietary preferences and foraging skills. In bats, postweaning food provisioning is severely understudied, despite the taxon's diverse and complex foraging strategies. The Neotropical common big-eared bat, Micronycteris microtis, preys on relatively large insects gleaned from vegetation, finding its silent and motionless prey by echolocation. The demands of this cognitively challenging hunting strategy make M. microtis a likely candidate for maternal postweaning food provisioning. We studied five free-living mother -pup pairs in their night roost using infrared video recordings. Each mother exclusively fed her own pup and mother-pup recognition was mutual. Provisioned pups were volant and had started their own hunting attempts. Weaned pups were provisioned for 5 subsequent months with a variety of insects, reflecting the adult diet. Mothers transferred over 50% of their prey to pups. Maternal prey transfers declined as pups matured, whereas the pups' own prey captures increased. During prey transfers, aggressive behaviour between mothers and pups was rare. We argue that postweaning maternal food provisioning might yield two informational benefits for M. microtis pups. First, learning how to handle large and well-defended prey is mandatory for inexperienced pups and could be practised with prey items provided by their mothers. Second, acoustically characteristic echo images of prey items could be gained during mother-pup prey transfers, probably facilitating the successful acquisition of M. microtis's complex hunting strategy. (C) 2013 The Association for the Study of Animal Behaviour. Published by Elsevier Ltd. All rights reserved. C1 [Geipel, Inga; Kalko, Elisabeth K. V.; Knoernschild, Mirjam] Univ Ulm, Fac Nat Sci, Inst Expt Ecol, D-89069 Ulm, Germany. [Kalko, Elisabeth K. V.] Smithsonian Trop Res Inst, Balboa, Panama. [Wallmeyer, Katja] Univ Tubingen, Inst Evolut & Ecol, Tubingen, Germany. RP Geipel, I (reprint author), Univ Ulm, Inst Expt Ecol, Albert Einstein Allee 11, D-89069 Ulm, Germany. EM inga.geipel@uni-ulm.de RI Knornschild, Mirjam/C-9401-2011 FU Smithsonian Tropical Research Institute FX Valuable comments by T. Jonsson, M. Metz and M. Tschapka substantially improved the manuscript. We thank P. Smiseth, H. Kunc and two anonymous referees for their helpful suggestions. The Panamanian authorities and the Smithsonian Tropical Research Institute gave both support and research permissions. The Biological Station BCI provided excellent logistics and technical support. We are especially indebted to O. Acevedo for her generous help. NR 62 TC 6 Z9 6 U1 2 U2 63 PU ACADEMIC PRESS LTD- ELSEVIER SCIENCE LTD PI LONDON PA 24-28 OVAL RD, LONDON NW1 7DX, ENGLAND SN 0003-3472 EI 1095-8282 J9 ANIM BEHAV JI Anim. Behav. PD JUN PY 2013 VL 85 IS 6 BP 1435 EP 1441 DI 10.1016/j.anbehav.2013.03.040 PG 7 WC Behavioral Sciences; Zoology SC Behavioral Sciences; Zoology GA 167RM UT WOS:000320651200035 ER PT J AU Lozano, J Malo, AF AF Lozano, Jorge Malo, Aurelio F. TI RELATIONSHIPS BETWEEN HUMAN ACTIVITY AND RICHNESS AND ABUNDANCE OF SOME BIRD SPECIES IN THE PARAGUAY RIVER (PANTANAL, BRAZIL) SO ARDEOLA LA English DT Article DE Anhinga anhinga; anthropic impact; Chauna torquata; disturbance; ecotourism; Egretta alba; Megaceryle torquata; wildlife management ID SPATIAL AUTOCORRELATION; PROTECTED AREAS; DISTURBANCE; ECOTOURISM; WATERBIRDS AB The Pantanal region (Brazil) is under increasing anthropic pressure partly due to an increase in tourism and there is a lack of information about the influence of human presence on avifauna. Here we study the relationships between human activity in the river (boats and fishermen) and 15 bird species along a 70 km stretch of the Paraguay River, also including other confounding factors such as distance to towns and spatial autocorrelation. Human density along the river was low and as expected decreased with distance from towns. Bird richness and density were negatively associated with human density and the distance to towns along the river, suggesting a permanent impact on avifauna. Riparian forests had higher bird density. Four species were apparently sensitive to human presence: the anhinga Anhinga anhinga, the great white egret Egretta alba, the ringed kingfisher Megaceryle torquata and the southern screamer Chauna torquata. Thus, these species could serve as indicators of human pressure. Any management plan for sustainable development of the study area should preserve the riparian forest, consider the control of numbers of tourists and people in the river, and monitor the bird community, especially the sensitive species. C1 [Lozano, Jorge] Univ Rey Juan Carlos, Dept Biol & Geol, E-28933 Mostoles, Madrid, Spain. [Malo, Aurelio F.] Smithsonian Inst, Natl Zool Pk, Ctr Conservat & Evolutionary Genet, Washington, DC 20008 USA. RP Lozano, J (reprint author), Univ Rey Juan Carlos, Dept Biol & Geol, C Tulipan S-N, E-28933 Mostoles, Madrid, Spain. EM j.lozano.men@gmail.com FU MEC/Fulbright fellowship from the Spanish Ministry of Education and Science [FU2005-0893]; Grupo de Ecologia Aplicada FX We are grateful to Fenelon Arias, our local guide on the Paraguay River, for his navigation skills which allowed us to collect the data for this study. Oscar Quiroga, head of 'Asociacion Hombre y Naturaleza: Bolivia' in Puerto Suarez, provided the basic material for performing the censuses and gave us constant support. D. L. Huertas revised an early version of the manuscript. A. F. Malo was partly supported by of a MEC/Fulbright fellowship from the Spanish Ministry of Education and Science (FU2005-0893). The 'Grupo de Ecologia Aplicada' partially financed this study. Two anonymous referees provided useful comments which greatly improved the final version of the manuscript. NR 56 TC 0 Z9 0 U1 5 U2 41 PU SOC ESPANOLA ORNITOLGIA PI MADRID PA MELQUIADAS BIENCINTO 34, E-28053 MADRID, SPAIN SN 0570-7358 J9 ARDEOLA JI Ardeola PD JUN PY 2013 VL 60 IS 1 BP 99 EP 112 PG 14 WC Ornithology SC Zoology GA 172TQ UT WOS:000321028200008 ER PT J AU Abramowski, A Acero, F Aharonian, F Akhperjanian, AG Anguner, E Anton, G Balenderan, S Balzer, A Barnacka, A Becherini, Y Tjus, JB Bernlohr, K Birsin, E Bissaldi, E Biteau, J Boisson, C Bolmont, J Bordas, P Brucker, J Brun, F Brun, P Bulik, T Carrigan, S Casanova, S Cerruti, M Chadwick, PM Chalme-Calvet, R Chaves, RCG Cheesebrough, A Chreetien, M Colafrancesco, S Cologna, G Conrad, J Couturier, C Dalton, M Daniel, MK Davids, ID Degrange, B Deil, C deWilt, P Dickinson, HJ Djannati-Atai, A Domainko, W Drury, LO Dubus, G Dutson, K Dyks, J Dyrda, M Edwards, T Egberts, K Eger, P Espigat, P Farnier, C Fegan, S Feinstein, F Fernandes, MV Fernandez, D Fiasson, A Fontaine, G Forster, A Fussling, M Gajdus, M Gallant, YA Garrigoux, T Gast, H Giebels, B Glicenstein, JF Goring, D Grondin, MH Grudzinska, M Haffner, S Hague, JD Hahn, J Harris, J Heinzelmann, G Henri, G Hermann, G Hervet, O Hillert, A Hinton, JA Hofmann, W Hofverberg, P Holler, M Horns, D Jacholkowska, A Jahn, C Jamrozy, M Janiak, M Jankowsky, F Jung, I Kastendieck, MA Katarzynski, K Katz, U Kaufmann, S Khelifi, B Kieffer, M Klepser, S Klochkov, D Kluzniak, W Kneiske, T Kolitzus, D Komin, N Kosack, K Krakau, S Krayzel, F Kruger, PP Laffon, H Lamanna, G Lefaucheur, J Lemoine-Goumard, M Lenain, JP Lennarz, D Lohse, T Lopatin, A Lu, CC Marandon, V Marcowith, A Maurin, G Mayer, M McComb, TJL Medina, MC Mehault, J Menzler, U Meyer, M Moderski, R Mohamed, M Moulin, E Murach, T Naumann, CL de Naurois, M Nedbal, D Niemiec, J Nolan, SJ Oakes, L Ohm, S Wilhelmi, ED Opitz, B Ostrowski, M Oya, I Panter, M Parsons, RD Arribas, MP Pekeur, NW Pelletier, G Perez, J Petrucci, PO Peyaud, B Pita, S Poon, H Puhlhofer, G Quirrenbach, A Raab, S Raue, M Reimer, A Reimer, O Renaud, M Reyes, RD Rieger, F Rob, L Rosier-Lees, S Rowell, G Rudak, B Rulten, CB Sahakian, V Sanchez, DA Santangelo, A Schlickeiser, R Schussler, F Schulz, A Schwanke, U Schwarzburg, S Schwemmer, S Sol, H Spengler, G Spiess, F Stawarz, L Steenkamp, R Stegmann, C Stinzing, F Stycz, K Sushch, I Szostek, A Tavernet, JP Terrier, R Tluczykont, M Trichard, C Valerius, K van Eldik, C Vasileiadis, G Venter, C Viana, A Vincent, P Volk, HJ Volpe, F Vorster, M Wagner, SJ Wagner, P Ward, M Weidinger, M White, R Wierzcholska, A Willmann, P Wornlein, A Wouters, D Zacharias, M Zajczyk, A Zdziarski, AA Zech, A Zechlin, HS AF Abramowski, A. Acero, F. Aharonian, F. Akhperjanian, A. G. Anguener, E. Anton, G. Balenderan, S. Balzer, A. Barnacka, A. Becherini, Y. Tjus, J. Becker Bernloehr, K. Birsin, E. Bissaldi, E. Biteau, J. Boisson, C. Bolmont, J. Bordas, P. Brucker, J. Brun, F. Brun, P. Bulik, T. Carrigan, S. Casanova, S. Cerruti, M. Chadwick, P. M. Chalme-Calvet, R. Chaves, R. C. G. Cheesebrough, A. Chretien, M. Colafrancesco, S. Cologna, G. Conrad, J. Couturier, C. Dalton, M. Daniel, M. K. Davids, I. D. Degrange, B. Deil, C. deWilt, P. Dickinson, H. J. Djannati-Atai, A. Domainko, W. Drury, L. O'C. Dubus, G. Dutson, K. Dyks, J. Dyrda, M. Edwards, T. Egberts, K. Eger, P. Espigat, P. Farnier, C. Fegan, S. Feinstein, F. Fernandes, M. V. Fernandez, D. Fiasson, A. Fontaine, G. Foerster, A. Fuessling, M. Gajdus, M. Gallant, Y. A. Garrigoux, T. Gast, H. Giebels, B. Glicenstein, J. F. Goering, D. Grondin, M. -H. Grudzinska, M. Haeffner, S. Hague, J. D. Hahn, J. Harris, J. Heinzelmann, G. Henri, G. Hermann, G. Hervet, O. Hillert, A. Hinton, J. A. Hofmann, W. Hofverberg, P. Holler, M. Horns, D. Jacholkowska, A. Jahn, C. Jamrozy, M. Janiak, M. Jankowsky, F. Jung, I. Kastendieck, M. A. Katarzynski, K. Katz, U. Kaufmann, S. Khelifi, B. Kieffer, M. Klepser, S. Klochkov, D. Kluzniak, W. Kneiske, T. Kolitzus, D. Komin, Nu. Kosack, K. Krakau, S. Krayzel, F. Krueger, P. P. Laffon, H. Lamanna, G. Lefaucheur, J. Lemoine-Goumard, M. Lenain, J. -P. Lennarz, D. Lohse, T. Lopatin, A. Lu, C. -C. Marandon, V. Marcowith, A. Maxted, N. Mayer, M. McComb, T. J. L. Medina, M. C. Mehault, J. Menzler, U. Meyer, M. Moderski, R. Mohamed, M. Moulin, E. Murach, T. Naumann, C. L. de Naurois, M. Nedbal, D. Niemiec, J. Nolan, S. J. Oakes, L. Ohm, S. Wilhelmi, E. de Ona Opitz, B. Ostrowski, M. Oya, I. Panter, M. Parsons, R. D. Arribas, M. Paz Pekeur, N. W. Pelletier, G. Perez, J. Petrucci, P. -O. Peyaud, B. Pita, S. Poon, H. Punch, M. Quirrenbach, A. Raab, S. Raue, M. Reimer, A. Reimer, O. Renaud, M. de los Reyes, R. Rieger, F. Rob, L. Rosier-Lees, S. Rowell, G. Rudak, B. Rulten, C. B. Sahakian, V. Sanchez, D. A. Santangelo, A. Schlickeiser, R. Schuessler, F. Schulz, A. Schwanke, U. Schwarzburg, S. Schwemmer, S. Sol, H. Spengler, G. Spiess, F. Stawarz, L. Steenkamp, R. Stegmann, C. Stinzing, F. Stycz, K. Sushch, I. Szostek, A. Tavernet, J. -P. Terrier, R. Tluczykont, M. Trichard, C. Valerius, K. van Eldik, C. Vasileiadis, G. Venter, C. Viana, A. Vincent, P. Voelk, H. J. Volpe, F. Vorster, M. Wagner, S. J. Wagner, P. Ward, M. Weidinger, M. White, R. Wierzcholska, A. Willmann, P. Woernlein, A. Wouters, D. Zacharias, M. Zajczyk, A. Zdziarski, A. A. Zech, A. Zechlin, H. -S. CA HESSCollaboration TI Discovery of high and very high-energy emission from the BL Lacertae object SHBL J001355.9-185406 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE BL Lacertae objects: individual: SHBL J001355.9-185406; gamma rays: general ID LARGE-AREA TELESCOPE; ATMOSPHERIC CHERENKOV TELESCOPES; ACTIVE GALACTIC NUCLEI; LAC OBJECTS; BACKGROUND-RADIATION; FERMI OBSERVATIONS; GAMMA-RAYS; SKY SURVEY; EGRET DATA; BLAZARS AB The detection of the high-frequency peaked BL Lac object (HBL) SHBL J001355.9-185406 (z = 0.095) at high (HE; 100 MeV < E < 300 GeV) and very high-energy (VHE; E > 100 GeV) with the Fermi Large Area Telescope (LAT) and the High Energy Stereoscopic System (H.E.S.S.) is reported. Dedicated observations were performed with the H. E. S. S. telescopes, leading to a detection at the 5.5 sigma significance level. The measured flux above 310 GeV is (8.3 +/- 1.7(stat) +/- 1.7(sys)) x 10(-13) photons cm(-2) s(-1) (about 0.6% of that of the Crab Nebula), and the power-law spectrum has a photon index of Gamma = 3.4 +/- 0.5(stat) +/- 0.2(sys). Using 3.5 years of publicly available Fermi-LAT data, a faint counterpart has been detected in the LAT data at the 5.5 sigma significance level, with an integrated flux above 300 MeV of (9.3 +/- 3.4(stat) +/- 0.8(sys)) x 10(-10) photons cm(-2) s(-1) and a photon index of Gamma = 1.96 +/- 0.20(stat) +/- 0.08(sys). X-ray observations with Swift-XRT allow the synchrotron peak energy in vF(v) representation to be located at similar to 1.0 keV. The broadband spectral energy distribution is modelled with a one-zone synchrotron self-Compton (SSC) model and the optical data by a black-body emission describing the thermal emission of the host galaxy. The derived parameters are typical of HBLs detected at VHE, with a particle-dominated jet. C1 [Abramowski, A.; Fernandes, M. V.; Heinzelmann, G.; Horns, D.; Kastendieck, M. A.; Kneiske, T.; Marandon, V.; Meyer, M.; Opitz, B.; Raue, M.; Spiess, F.; Tluczykont, M.; Zechlin, H. -S.] Univ Hamburg, Inst Expt Phys, D-22761 Hamburg, Germany. [Acero, F.; Feinstein, F.; Fernandez, D.; Gallant, Y. A.; Marcowith, A.; Renaud, M.; Vasileiadis, G.; Zajczyk, A.] Univ Montpellier 2, CNRS IN2P3, Lab Univers & Particules Montpellier, CC 72, F-34095 Montpellier 5, France. [Aharonian, F.; Brun, F.; Carrigan, S.; Casanova, S.; Chaves, R. C. G.; Deil, C.; Domainko, W.; Edwards, T.; Eger, P.; Foerster, A.; Gast, H.; Grondin, M. -H.; Hague, J. D.; Hahn, J.; Hermann, G.; Hillert, A.; Hofmann, W.; Hofverberg, P.; Lennarz, D.; Lu, C. -C.; Marandon, V.; Wilhelmi, E. de Ona; Panter, M.; Parsons, R. D.; Poon, H.; de los Reyes, R.; Rieger, F.; Sanchez, D. A.; Viana, A.; Voelk, H. J.; Volpe, F.] Max Planck Inst Kernphys, D-69029 Heidelberg, Germany. [Aharonian, F.; Drury, L. O'C.] Dublin Inst Adv Studies, Dublin 2, Ireland. [Aharonian, F.; Akhperjanian, A. G.; Sahakian, V.] Natl Acad Sci Republ Armenia, Yerevan, Armenia. [Akhperjanian, A. G.; Sahakian, V.] Yerevan Phys Inst, Yerevan 375036, Armenia. [Anguener, E.; Birsin, E.; Gajdus, M.; Lohse, T.; Marandon, V.; Murach, T.; Oakes, L.; Oya, I.; Arribas, M. Paz; Schwanke, U.; Spengler, G.; Sushch, I.; Wagner, P.] Humboldt Univ, Inst Phys, D-12489 Berlin, Germany. [Anton, G.; Brucker, J.; Haeffner, S.; Jahn, C.; Jung, I.; Katz, U.; Lopatin, A.; Marandon, V.; Raab, S.; Stinzing, F.; Valerius, K.; van Eldik, C.; Willmann, P.; Woernlein, A.] Univ Erlangen Nurnberg, Inst Phys, D-91058 Erlangen, Germany. [Balenderan, S.; Chadwick, P. M.; Cheesebrough, A.; Daniel, M. K.; Harris, J.; McComb, T. J. L.; Nolan, S. J.; Sahakian, V.; Ward, M.] Univ Durham, Dept Phys, Durham DH1 3LE, England. [Balzer, A.; Klepser, S.; Marandon, V.; Schulz, A.; Stegmann, C.; Stycz, K.] DESY, D-15735 Zeuthen, Germany. [Balzer, A.; Fuessling, M.; Holler, M.; Mayer, M.; Stegmann, C.] Univ Potsdam, Inst Phys & Astron, D-14476 Potsdam, Germany. [Barnacka, A.; Dyks, J.; Janiak, M.; Kluzniak, W.; Moderski, R.; Rudak, B.; Zajczyk, A.; Zdziarski, A. A.] Nicolaus Copernicus Astron Ctr, PL-00716 Warsaw, Poland. [Becherini, Y.; Cologna, G.; Grondin, M. -H.; Jankowsky, F.; Kaufmann, S.; Marandon, V.; Mohamed, M.; Quirrenbach, A.; Schwemmer, S.; Wagner, S. J.] Heidelberg Univ, D-69117 Heidelberg, Germany. [Becherini, Y.; Djannati-Atai, A.; Espigat, P.; Lefaucheur, J.; Pita, S.; Punch, M.; Terrier, R.] Univ Paris Diderot, CNRS IN2P3, CEA Irfu, Observ Paris,Sorbonne Paris Cite, F-75205 Paris 13, France. [Becherini, Y.; Biteau, J.; Degrange, B.; Fegan, S.; Fontaine, G.; Giebels, B.; Khelifi, B.; Laffon, H.; Marandon, V.; de Naurois, M.] Ecole Polytech, Lab Leprince Ringuet, CNRS IN2P3, F-91128 Palaiseau, France. [Tjus, J. Becker; Krakau, S.; Menzler, U.; Schlickeiser, R.; Weidinger, M.; Zacharias, M.] Ruhr Univ Bochum, Inst Theoret Phys, Lehrstuhl Weltraum & Astrophys 4, D-44780 Bochum, Germany. [Bissaldi, E.; Egberts, K.; Kolitzus, D.; Perez, J.; Reimer, A.; Reimer, O.] Leopold Franzens Univ Innsbruck, Inst Astro & Teilchenphys, A-6020 Innsbruck, Austria. [Boisson, C.; Cerruti, M.; Hervet, O.; Rulten, C. B.; Sol, H.; Zech, A.] Univ Paris Diderot, CNRS, Observ Paris, LUTH, F-92190 Meudon, France. [Bolmont, J.; Chalme-Calvet, R.; Chretien, M.; Couturier, C.; Garrigoux, T.; Jacholkowska, A.; Kieffer, M.; Lenain, J. -P.; Naumann, C. L.; Tavernet, J. -P.; Vincent, P.] Univ Paris 07, CNRS IN2P3, Univ Paris 06, LPNHE, F-75252 Paris 5, France. [Bordas, P.; Klochkov, D.; Santangelo, A.; Schwarzburg, S.] Univ Tubingen, Inst Astron & Astrophys, D-72076 Tubingen, Germany. [Brun, P.; Chaves, R. C. G.; Glicenstein, J. F.; Kosack, K.; Medina, M. C.; Moulin, E.; Peyaud, B.; Schuessler, F.; Wouters, D.] CEA Saclay, DSM Irfu, F-91191 Gif Sur Yvette, France. [Bulik, T.; Grudzinska, M.] Univ Warsaw, Astron Observ, PL-00478 Warsaw, Poland. [Casanova, S.; Marandon, V.; Pekeur, N. W.; Sushch, I.; Venter, C.; Vorster, M.] North West Univ, Unit Space Phys, ZA-2520 Potchefstroom, South Africa. [Cerruti, M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Colafrancesco, S.] Univ Witwatersrand, Sch Phys, ZA-2050 Johannesburg, South Africa. [Conrad, J.; Dickinson, H. J.; Farnier, C.] Stockholm Univ, Albanova Univ Ctr, Oskar Klein Ctr, Dept Phys, S-10691 Stockholm, Sweden. [Dalton, M.; Laffon, H.; Lemoine-Goumard, M.; Mehault, J.] Univ Bordeaux 1, CNRS IN2P3, Ctr Etud Nucl Bordeaux Gradignan, F-33175 Gradignan, France. [Davids, I. D.; Steenkamp, R.] Univ Namibia, Dept Phys, Windhoek, Namibia. [deWilt, P.; Maxted, N.; Rowell, G.] Univ Adelaide, Sch Chem & Phys, Adelaide, SA 5005, Australia. [Dubus, G.; Henri, G.; Pelletier, G.; Petrucci, P. -O.] UJF Grenoble 1, CNRS INSU, IPAG UMR 5274, F-38041 Grenoble, France. [Dutson, K.; Hinton, J. A.; Ohm, S.; White, R.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. [Dyrda, M.; Niemiec, J.] Inst Fizyki Jadrowej PAN, Krakow, Poland. [Fiasson, A.; Komin, Nu.; Krayzel, F.; Lamanna, G.; Rosier-Lees, S.; Trichard, C.] Univ Savoie, CNRS IN2P3, Lab Annecy le Vieux Phys Particules, F-74941 Annecy Le Vieux, France. [Jamrozy, M.; Ostrowski, M.; Stawarz, L.; Szostek, A.; Wierzcholska, A.] Uniwersytet Jagiellonski, Obserwatorium Astronomiczne, PL-30244 Krakow, Poland. [Katarzynski, K.] Nicolaus Copernicus Univ, Torun Ctr Astron, PL-87100 Torun, Poland. [Nedbal, D.; Rob, L.] Charles Univ Prague, Fac Math & Phys, Inst Particle & Nucl Phys, CR-18000 Prague 8, Czech Republic. [Ohm, S.] Univ Leeds, Sch Phys & Astron, Leeds LS2 9JT, W Yorkshire, England. RP Biteau, J (reprint author), Ecole Polytech, Lab Leprince Ringuet, CNRS IN2P3, F-91128 Palaiseau, France. EM biteau@in2p3.fr; david.sanchez@mpi-hd.mpg.de RI Couturier, Camille/K-7585-2013; Tjus, Julia/G-8145-2012; Jamrozy, Marek/F-4507-2015; Casanova, Sabrina/J-8935-2013; Anton, Gisela/C-4840-2013; Katz, Uli/E-1925-2013; Fontaine, Gerard/D-6420-2014; van Eldik, Christopher/C-3901-2013; Venter, Christo/E-6884-2011; Reimer, Olaf/A-3117-2013; Schussler, Fabian/G-5313-2013; Katarzynski, Krzysztof/G-4528-2014; Meyer, Manuel/E-2697-2016; Bissaldi, Elisabetta/K-7911-2016; Drury, Luke/B-1916-2017; Moulin, Emmanuel/B-5959-2017; Daniel, Michael/A-2903-2010; Komin, Nukri/J-6781-2015 OI Couturier, Camille/0000-0002-0168-1106; Casanova, Sabrina/0000-0002-6144-9122; Anton, Gisela/0000-0003-2039-4724; Katz, Uli/0000-0002-7063-4418; van Eldik, Christopher/0000-0001-9669-645X; Venter, Christo/0000-0002-2666-4812; Reimer, Olaf/0000-0001-6953-1385; Schussler, Fabian/0000-0003-1500-6571; Lenain, Jean-Philippe/0000-0001-7284-9220; Maxted, Nigel/0000-0003-2762-8378; Punch, Michael/0000-0002-4710-2165; Sushch, Iurii/0000-0002-2814-1257; Bordas, Pol/0000-0002-0266-8536; Oya, Igor/0000-0002-3881-9324; de Ona Wilhelmi, Emma/0000-0002-5401-0744; Rowell, Gavin/0000-0002-9516-1581; Meyer, Manuel/0000-0002-0738-7581; Bissaldi, Elisabetta/0000-0001-9935-8106; Drury, Luke/0000-0002-9257-2270; Moulin, Emmanuel/0000-0003-4007-0145; Chadwick, Paula/0000-0002-1468-2685; Kneiske, Tanja M./0000-0002-3210-6200; mohamed, mahmoud/0000-0002-4625-6242; Daniel, Michael/0000-0002-8053-7910; de los Reyes Lopez, Raquel/0000-0003-0485-9552; Kruger, Paulus/0000-0003-0664-8521; Komin, Nukri/0000-0003-3280-0582 FU German Ministry for Education and Research (BMBF); Max Planck Society; French Ministry for Research; CNRS-IN2P3; Astroparticle Interdisciplinary Programme of the CNRS; UK Particle Physics and Astronomy Research Council (PPARC); IPNP of the Charles University; South African Department of Science and Technology; National Research Foundation; University of Namibia; National Aeronautics and Space Administration; Istituto Nazionale di Astrofisica in Italy; Centre National d'Etudes Spatiales in France FX The support of the Namibian authorities and of the University of Namibia in facilitating the construction and operation of H.E.S.S. is gratefully acknowledged, as is the support by the German Ministry for Education and Research (BMBF), the Max Planck Society, the French Ministry for Research, the CNRS-IN2P3 and the Astroparticle Interdisciplinary Programme of the CNRS, the UK Particle Physics and Astronomy Research Council (PPARC), the IPNP of the Charles University, the South African Department of Science and Technology and National Research Foundation, and by the University of Namibia. We appreciate the excellent work of the technical support staff in Berlin, Durham, Hamburg, Heidelberg, Palaiseau, Paris, Saclay, and in Namibia in the construction and operation of the equipment. The Fermi LAT Collaboration acknowledges generous ongoing support from a number of agencies and institutes that have supported both the development and the operation of the LAT as well as scientific data analysis. These include the National Aeronautics and Space Administration and the Department of Energy in the US, the Commissariat a l'Energie Atomique and the Centre National de la Recherche Scientifique/Institut National de Physique Nuclaire et de Physique des Particules in France, the Agenzia Spaziale Italiana and the Istituto Nazionale di Fisica Nucleare in Italy, the Ministry of Education, Culture, Sports, Science and Technology (MEXT), High Energy Accelerator Research Organization (KEK) and Japan Aerospace Exploration Agency (JAXA) in Japan, and the K. A. Wallenberg Foundation, the Swedish Research Council and the Swedish National Space Board in Sweden. Additional support for science analysis during the operations phase is gratefully acknowledged from the Istituto Nazionale di Astrofisica in Italy and the Centre National d'Etudes Spatiales in France. 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. This research has made use of the VizieR catalogue access tool, CDS, Strasbourg, France. This publication makes use of data products from the Wide-field Infrared Survey Explorer, which is a joint project of the University of California, Los Angeles, and the Jet Propulsion Laboratory/California Institute of Technology, funded by the National Aeronautics and Space Administration. The authors want to thank D. Paneque for the useful comments that improved the paper. NR 58 TC 9 Z9 9 U1 3 U2 25 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD JUN PY 2013 VL 554 AR A72 DI 10.1051/0004-6361/201220996 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 164XA UT WOS:000320444200071 ER PT J AU Covino, E Esposito, M Barbieri, M Mancini, L Nascimbeni, V Claudi, R Desidera, S Gratton, R Lanza, AF Sozzetti, A Biazzo, K Affer, L Gandolfi, D Munari, U Pagano, I Bonomo, AS Cameron, AC Hebrard, G Maggio, A Messina, S Micela, G Molinari, E Pepe, F Piotto, G Ribas, I Santos, NC Southworth, J Shkolnik, E Triaud, AHMJ Bedin, L Benatti, S Boccato, C Bonavita, M Borsa, F Borsato, L Brown, D Carolo, E Ciceri, S Cosentino, R Damasso, M Faedi, F Fiorenzano, AFM Latham, DW Lovis, C Mordasini, C Nikolov, N Poretti, E Rainer, M Lopez, RR Scandariato, G Silvotti, R Smareglia, R Alcala, JM Cunial, A Di Fabrizio, L Di Mauro, MP Giacobbe, P Granata, V Harutyunyan, A Knapic, C Lattanzi, M Leto, G Lodato, G Malavolta, L Marzari, F Molinaro, M Nardiello, D Pedani, M Prisinzano, L Turrini, D AF Covino, E. Esposito, M. Barbieri, M. Mancini, L. Nascimbeni, V. Claudi, R. Desidera, S. Gratton, R. Lanza, A. F. Sozzetti, A. Biazzo, K. Affer, L. Gandolfi, D. Munari, U. Pagano, I. Bonomo, A. S. Cameron, A. Collier Hebrard, G. Maggio, A. Messina, S. Micela, G. Molinari, E. Pepe, F. Piotto, G. Ribas, I. Santos, N. C. Southworth, J. Shkolnik, E. Triaud, A. H. M. J. Bedin, L. Benatti, S. Boccato, C. Bonavita, M. Borsa, F. Borsato, L. Brown, D. Carolo, E. Ciceri, S. Cosentino, R. Damasso, M. Faedi, F. Martinez Fiorenzano, A. F. Latham, D. W. Lovis, C. Mordasini, C. Nikolov, N. Poretti, E. Rainer, M. Rebolo Lopez, R. Scandariato, G. Silvotti, R. Smareglia, R. Alcala, J. M. Cunial, A. Di Fabrizio, L. Di Mauro, M. P. Giacobbe, P. Granata, V. Harutyunyan, A. Knapic, C. Lattanzi, M. Leto, G. Lodato, G. Malavolta, L. Marzari, F. Molinaro, M. Nardiello, D. Pedani, M. Prisinzano, L. Turrini, D. TI The GAPS programme with HARPS-N at TNG I. Observations of the Rossiter-McLaughlin effect and characterisation of the transiting system Qatar-1 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE techniques: radial velocities; stars: late-type; stars: fundamental parameters; stars: individual: Qatar-1 ID IN EXTRASOLAR PLANETS; SOLAR-TYPE STARS; CA-II H; HOT JUPITERS; GIANT PLANET; TIDAL DISSIPATION; EQUIVALENT WIDTH; STELLAR ACTIVITY; INCLINED ORBIT; HOST STARS AB Context. Our understanding of the formation and evolution of planetary systems is still fragmentary because most of the current data provide limited information about the orbital structure and dynamics of these systems. The knowledge of the orbital properties for a variety of systems and at different ages yields information on planet migration and on star-planet tidal interaction mechanisms. Aims. In this context, a long-term, multi-purpose, observational programme has started with HARPS-N at TNG and aims to characterise the global architectural properties of exoplanetary systems. The goal of this first paper is to fully characterise the orbital properties of the transiting system Qatar-1 as well as the physical properties of the star and the planet. Methods. We exploit HARPS-N high-precision radial velocity measurements obtained during a transit to measure the Rossiter-McLaughlin effect in the Qatar-1 system, and out-of-transit measurements to redetermine the spectroscopic orbit. New photometric-transit light-curves were analysed and a spectroscopic characterisation of the host star atmospheric parameters was performed based on various methods (line equivalent width ratios, spectral synthesis, spectral energy distribution). Results. We achieved a significant improvement in the accuracy of the orbital parameters and derived the spin-orbit alignment of the system; this information, combined with the spectroscopic determination of the host star properties (rotation, T-eff, log g, metallicity), allows us to derive the fundamental physical parameters for star and planet (masses and radii). The orbital solution for the Qatar-1 system is consistent with a circular orbit and the system presents a sky-projected obliquity of lambda = -8.4 +/- 7.1 deg. The planet, with a mass of 1.33 +/- 0.05 M-J, is found to be significantly more massive than previously reported. The host star is confirmed to be metal-rich ([Fe/H] = 0.20 +/- 0.10) and slowly rotating (v sin I = 1.7 +/- 0.3 km s(-1)), though moderately active, as indicated by the strong chromospheric emission in the Ca II H&K line cores (log R'(HK) approximate to -4.60). Conclusions. We find that the system is well aligned and fits well within the general lambda versus T-eff trend. We can definitely rule out any significant orbital eccentricity. The evolutionary status of the system is inferred based on gyrochronology, and the present orbital configuration and timescale for orbital decay are discussed in terms of star-planet tidal interactions. C1 [Covino, E.; Biazzo, K.; Alcala, J. M.] Osserv Astron Capodimonte, INAF, I-80131 Naples, Italy. [Esposito, M.; Rebolo Lopez, R.; Di Fabrizio, L.; Harutyunyan, A.; Pedani, M.] Inst Astrofis Canarias, San Cristobal la Laguna 38205, Tenerife, Spain. [Barbieri, M.; Nascimbeni, V.; Piotto, G.; Borsato, L.; Carolo, E.; Damasso, M.; Cunial, A.; Granata, V.; Malavolta, L.; Marzari, F.; Nardiello, D.] Univ Padua, Dipartimento Fis & Astron Galileo Galilei, I-35122 Padua, Italy. [Mancini, L.; Mordasini, C.; Nikolov, N.] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Nascimbeni, V.; Claudi, R.; Desidera, S.; Gratton, R.; Munari, U.; Bedin, L.; Benatti, S.; Boccato, C.; Bonavita, M.] Osserv Astron Padova, INAF, I-35122 Padua, Italy. [Lanza, A. F.; Biazzo, K.; Pagano, I.; Messina, S.; Scandariato, G.; Leto, G.] Osserv Astrofis Catania, INAF, I-95123 Catania, Italy. [Sozzetti, A.; Bonomo, A. S.; Damasso, M.; Giacobbe, P.; Lattanzi, M.] Osserv Astron Torino, INAF, I-10025 Pino Torinese, Italy. [Affer, L.; Maggio, A.; Micela, G.; Prisinzano, L.] Osserv Astron Palermo, INAF, I-90134 Palermo, Italy. [Gandolfi, D.] ESTEC ESA, Res & Sci Support Dept, NL-2200 AG Noordwijk, Netherlands. [Cameron, A. Collier; Brown, D.] Univ St Andrews, Sch Phys & Astron, SUPA, St Andrews KY16 9SS, Fife, Scotland. [Molinari, E.; Cosentino, R.; Martinez Fiorenzano, A. F.] INAF, Fdn Galileo Galilei, Brena Baja 38712, TF, Spain. [Molinari, E.] IASF Milano, INAF, I-20133 Milan, Italy. [Pepe, F.; Triaud, A. H. M. J.; Lovis, C.] Univ Geneva, Astron Observ, CH-1290 Versoix, Switzerland. [Ribas, I.] Inst Ciencies Espai CSIC IEEC, Fac Ciencies, Bellaterra 08193, Spain. [Santos, N. C.] Univ Porto, Ctr Astrofis, P-4150762 Oporto, Portugal. [Santos, N. C.] Univ Porto, Fac Ciencias, Dept Fis & Astron, P-4150762 Oporto, Portugal. [Southworth, J.] Keele Univ, Astrophys Grp, Keele ST5 5BG, Staffs, England. [Faedi, F.] Univ Warwick, Dept Phys, Coventry CV4 7AL, W Midlands, England. [Esposito, M.] Univ La Laguna, Dept Astrofis, San Cristobal la Laguna 38206, Tenerife, Spain. [Borsa, F.; Poretti, E.; Rainer, M.] Osserv Astron Brera, INAF, I-23807 Merate, LC, Italy. [Hebrard, G.] Univ Paris 06, UMR CNRS 7095, Inst Astrophys Paris, F-75014 Paris, France. [Smareglia, R.; Knapic, C.] Osserv Astron Trieste, INAF, I-34143 Trieste, Italy. [Shkolnik, E.] Lowell Observ, Flagstaff, AZ 86001 USA. [Triaud, A. H. M. J.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Latham, D. W.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Borsa, F.] Univ Insubria, Dipartimento Sci & Alta Tecnol, I-22100 Como, Italy. [Damasso, M.; Giacobbe, P.] Osservatorio Astron Reg Autonoma Aosta, I-11020 Nus, Aosta, Italy. [Di Mauro, M. P.; Turrini, D.] INAF Ist Fis & Planetol Spaziali, I-00133 Rome, Italy. [Lodato, G.] Univ Milan, Dipartimento Fis, I-20133 Milan, Italy. RP Covino, E (reprint author), Osserv Astron Capodimonte, INAF, Via Moiariello 16, I-80131 Naples, Italy. EM ovino@oacn.inaf.it RI Leto, Giuseppe/N-3355-2015; Maggio, Antonio/P-5700-2015; Pagano, Isabella/I-6934-2015; Santos, Nuno/E-9957-2011; Ribas, Ignasi/M-2134-2014 OI Sozzetti, Alessandro/0000-0002-7504-365X; Lattanzi, Mario Gilberto/0000-0003-0429-7748; bedin, luigi/0000-0003-4080-6466; Turrini, Diego/0000-0002-1923-7740; Cameron, Andrew/0000-0002-8863-7828; Alcala, Juan Manuel/0000-0001-8657-095X; Poretti, Ennio/0000-0003-1200-0473; Lanza, Antonino Francesco/0000-0001-5928-7251; Messina, Sergio/0000-0002-2851-2468; Boccato, Caterina/0000-0002-6177-9703; Barbieri, Mauro/0000-0001-8362-3462; GRANATA, Valentina/0000-0002-1425-4541; Molinaro, Marco/0000-0001-5028-6041; Micela, Giuseppina/0000-0002-9900-4751; Desidera, Silvano/0000-0001-8613-2589; Smareglia, Riccardo/0000-0001-9363-3007; Molinari, Emilio/0000-0002-1742-7735; Gandolfi, Davide/0000-0001-8627-9628; Munari, Ulisse/0000-0001-6805-9664; Piotto, Giampaolo/0000-0002-9937-6387; Di Mauro, Maria Pia/0000-0001-7801-7484; Gratton, Raffaele/0000-0003-2195-6805; Leto, Giuseppe/0000-0002-0040-5011; Maggio, Antonio/0000-0001-5154-6108; Pagano, Isabella/0000-0001-9573-4928; Silvotti, Roberto/0000-0002-1295-8174; Biazzo, Katia/0000-0002-1892-2180; Knapic, Cristina/0000-0002-4752-6777; Covino, Elvira/0000-0002-6187-6685; Prisinzano, Loredana/0000-0002-8893-2210; Santos, Nuno/0000-0003-4422-2919; Ribas, Ignasi/0000-0002-6689-0312 FU PRIN-INAF; Universita di Padova through the "progetto di Ateneo" [CPDA103591]; European Research Council/European Community under the FP7 [239953]; Fundacao para a Ciencia e a Tecnologia (FCT) through program Ciencia; FCT/MCTES (Portugal); POPH/FSE (EC); Spanish Ministry of Economy and Competitiveness (MINECO); "Fondo Europeo de Desarrollo Regional" (FEDER) [AYA2009-06934, AYA2012-39612-C03-01]; Swiss National Science Foundation [PBGEP2_145594]; [PTDC/CTE-AST/098528/2008]; [PTDC/CTE-AST/120251/2010] FX The HARPS-N instrument has been built by the HARPS-N Consortium, a collaboration between the Geneva Observatory (PI Institute), the Harvard-Smithonian Center for Astrophysics, the University of St. Andrews, the University of Edinburgh, the Queen's University of Belfast, and INAF. This work has been partially supported by PRIN-INAF 2010. This research made use of the SIMBAD database, operated at the CDS (Strasbourg, France). This work has made use of BaSTI web tools. E.C., M.E. and K.B. thank Giulio Capasso, Fabrizio Cioffi and Andrea Di Dato for their support with the OAC computing facilities. E.C. thanks Paolo Molaro for stimulating discussions, V.N. and G.P. acknowledge partial support by the Universita di Padova through the "progetto di Ateneo" #CPDA103591. N.C.S. acknowledges the support by the European Research Council/European Community under the FP7 through Starting Grant agreement number 239953, as well as from Fundacao para a Ciencia e a Tecnologia (FCT) through program Ciencia 2007 funded by FCT/MCTES (Portugal) and POPH/FSE (EC), and in the form of grants reference PTDC/CTE-AST/098528/2008 and PTDC/CTE-AST/120251/2010. I.R. acknowledges financial support from the Spanish Ministry of Economy and Competitiveness (MINECO) and the "Fondo Europeo de Desarrollo Regional" (FEDER) through grants AYA2009-06934 and AYA2012-39612-C03-01. A.T. is supported by the Swiss National Science Foundation fellowship number PBGEP2_145594. NR 77 TC 32 Z9 32 U1 0 U2 13 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 JUN PY 2013 VL 554 AR A28 DI 10.1051/0004-6361/201321298 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 164XA UT WOS:000320444200028 ER PT J AU Desidera, S Sozzetti, A Bonomo, AS Gratton, R Poretti, E Claudi, R Latham, DW Affer, L Cosentino, R Damasso, M Esposito, M Giacobbe, P Malavolta, L Nascimbeni, V Piotto, G Rainer, M Scardia, M Schmid, VS Lanza, AF Micela, G Pagano, I Bedin, LR Biazzo, K Borsa, F Carolo, E Covino, E Faedi, F Hebrard, G Lovis, C Maggio, A Mancini, L Marzari, F Messina, S Molinari, E Munari, U Pepe, F Santos, N Scandariato, G Shkolnik, E Southworth, J AF Desidera, S. Sozzetti, A. Bonomo, A. S. Gratton, R. Poretti, E. Claudi, R. Latham, D. W. Affer, L. Cosentino, R. Damasso, M. Esposito, M. Giacobbe, P. Malavolta, L. Nascimbeni, V. Piotto, G. Rainer, M. Scardia, M. Schmid, V. S. Lanza, A. F. Micela, G. Pagano, I. Bedin, L. R. Biazzo, K. Borsa, F. Carolo, E. Covino, E. Faedi, F. Hebrard, G. Lovis, C. Maggio, A. Mancini, L. Marzari, F. Messina, S. Molinari, E. Munari, U. Pepe, F. Santos, N. Scandariato, G. Shkolnik, E. Southworth, J. TI The GAPS programme with HARPS-N at TNG II. No giant planets around the metal-poor star HIP 11952 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE stars: individual: HIP 11952; techniques: radial velocities; planetary systems ID EXTRA-SOLAR PLANETS; HIRES DOPPLER SEARCH; METALLICITY; MASS; COMPANIONS; FREQUENCY; BINARIES; SAMPLE; RANGE AB In the context of the programme Global Architecture of Planetary Systems (GAPS), we have performed radial velocity monitoring of the metal-poor star HIP 11952 on 35 nights during about 150 days using the newly installed high-resolution spectrograph HARPS-N at the TNG and HARPS at the ESO 3.6 m telescope. The radial velocities show a scatter of 7 m s(-1), compatible with the measurement errors for such a moderately warm metal-poor star (T-eff = 6040 +/- 120 K; [Fe/H] = -1.9 +/- 0.1). We exclude the presence of the two giant planets with periods of 6.95 +/- 0.01 d and 290.0 +/- 16.2 d and radial velocity semi-amplitudes of 100.3 +/- 19.4 m s(-1) and 105.2 +/- 14.7 m s(-1), respectively, which have recently been announced. This result is important because HIP 11952 was thought to be the most metal-poor star hosting a planetary system with giant planets, which challenged some models of planet formation. C1 [Desidera, S.; Gratton, R.; Claudi, R.; Malavolta, L.; Nascimbeni, V.; Piotto, G.; Bedin, L. R.; Carolo, E.; Marzari, F.; Munari, U.] Osserv Astron Padova, INAF, I-35122 Padua, Italy. [Sozzetti, A.; Bonomo, A. S.; Damasso, M.; Giacobbe, P.] Osserv Astron Torino, INAF, I-10025 Pino Torinese, Italy. [Poretti, E.; Rainer, M.; Scardia, M.; Borsa, F.] Osserv Astron Brera, INAF, I-23807 Merate, LC, Italy. [Latham, D. W.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Affer, L.; Micela, G.; Maggio, A.] Osserv Astron Palermo, INAF, I-90134 Palermo, Italy. [Cosentino, R.; Lanza, A. F.; Pagano, I.; Messina, S.; Scandariato, G.] Osserv Astrofis Catania, INAF, I-9512 Catania, Italy. [Cosentino, R.; Molinari, E.] INAF, Fdn Galileo Galilei, Brena Baja 38712, Spain. [Damasso, M.; Malavolta, L.; Nascimbeni, V.; Piotto, G.] Univ Padua, Dip Fis & Astron Galileo Galilei, I-35122 Padua, Italy. [Damasso, M.] Osservatorio Astron Reg Autonoma Aosta, I-11020 Nus, Aosta, Italy. [Esposito, M.] Inst Astrofis Canarias, E-38200 San Cristobal la Laguna, Tenerife, Spain. [Esposito, M.] Univ La Laguna, Dept Astrofis, San Cristobal la Laguna 38205, Tenerife, Spain. [Giacobbe, P.] Univ Trieste, Dipartimento Fis, I-34143 Trieste, Italy. [Malavolta, L.; Lovis, C.; Pepe, F.] Univ Geneva, Observ Astron, CH-1290 Versoix, Switzerland. [Schmid, V. S.] Katholieke Univ Leuven, Inst Sterrenkunde, B-3001 Heverlee, Belgium. [Biazzo, K.; Covino, E.] Osserv Astron Capodimonte, INAF, I-80131 Naples, Italy. [Borsa, F.] Univ Insubria, Dipartimento Sci & Alta Tecnol, I-22100 Como, Italy. [Faedi, F.] Univ Warwick, Dept Phys, Coventry CV4 7AL, W Midlands, England. [Hebrard, G.] Univ Paris 06, UMR CNRS 7095, Inst Astrophys Paris, F-75014 Paris, France. [Mancini, L.] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Marzari, F.] Univ Padua, Dipartimento Fis & Astron Galileo Galilei, I-35122 Padua, Italy. [Molinari, E.] IASF Milano, INAF, I-20133 Milan, Italy. [Santos, N.] Univ Porto, Ctr Astrofis, P-4150762 Oporto, Portugal. [Santos, N.] Univ Porto, Fac Ciencias, Dept Fis & Astron, P-4099002 Oporto, Portugal. [Shkolnik, E.] Lowell Observ, Flagstaff, AZ 86001 USA. [Southworth, J.] Keele Univ, Astrophys Grp, Keele ST5 5BG, Staffs, England. RP Desidera, S (reprint author), Osserv Astron Padova, INAF, Vicolo Osservatorio 5, I-35122 Padua, Italy. EM desidera@oapd.inaf.it RI Santos, Nuno/E-9957-2011; Maggio, Antonio/P-5700-2015; Pagano, Isabella/I-6934-2015; OI Poretti, Ennio/0000-0003-1200-0473; Lanza, Antonino Francesco/0000-0001-5928-7251; Messina, Sergio/0000-0002-2851-2468; Munari, Ulisse/0000-0001-6805-9664; Piotto, Giampaolo/0000-0002-9937-6387; Gratton, Raffaele/0000-0003-2195-6805; Desidera, Silvano/0000-0001-8613-2589; Santos, Nuno/0000-0003-4422-2919; Maggio, Antonio/0000-0001-5154-6108; Pagano, Isabella/0000-0001-9573-4928; Molinari, Emilio/0000-0002-1742-7735; Biazzo, Katia/0000-0002-1892-2180; Covino, Elvira/0000-0002-6187-6685; Sozzetti, Alessandro/0000-0002-7504-365X; bedin, luigi/0000-0003-4080-6466; Micela, Giuseppina/0000-0002-9900-4751 FU PRIN-INAF; ERC/EC under the FP7 [239953]; Fundacao para a Ciencia e a Tecnologia (FCT) through prog. Ciencia; FCT/MCTES (Portugal); POPH/FSE (EC); [PTDC/CTE-AST/098528/2008]; [PTDC/CTE-AST/120251/2010] FX We thank the TNG staff for help in the preparation of the observations and R. Smareglia and collaborators for the kind assistance with the data retrieval from TNG archive. This work was partially funded by PRIN-INAF 2010. NCS acknowledges the support by the ERC/EC under the FP7 through Starting Grant agreement n. 239953, as well as the support from Fundacao para a Ciencia e a Tecnologia (FCT) through prog. Ciencia 2007 funded by FCT/MCTES (Portugal) and POPH/FSE (EC), and in the form of grants ref. PTDC/CTE-AST/098528/2008 and PTDC/CTE-AST/120251/2010. NR 30 TC 16 Z9 16 U1 0 U2 8 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 JUN PY 2013 VL 554 AR A29 DI 10.1051/0004-6361/201321155 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 164XA UT WOS:000320444200029 ER PT J AU Pinilla, P Birnstiel, T Benisty, M Ricci, L Natta, A Dullemond, CP Dominik, C Testi, L AF Pinilla, P. Birnstiel, T. Benisty, M. Ricci, L. Natta, A. Dullemond, C. P. Dominik, C. Testi, L. TI Explaining millimeter-sized particles in brown dwarf disks SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE accretion, accretion disks; protoplanetary disks; circumstellar matter; brown dwarfs; planets and satellites: formation ID DUST GROWTH PEBBLES; T-TAURI STARS; PROTOPLANETARY DISKS; GRAIN-GROWTH; CIRCUMSTELLAR DISKS; MAGNETOHYDRODYNAMIC SIMULATIONS; MAGNETOROTATIONAL TURBULENCE; BOUNCING BARRIER; ACCRETION DISKS; UPPER SCORPIUS AB Context. Planets have been detected around a variety of stars, including low-mass objects, such as brown dwarfs. However, such extreme cases are challenging for planet formation models. Recent sub-millimeter observations of disks around brown dwarf measured low spectral indices of the continuum emission that suggest that dust grains grow to mm-sizes even in these very low mass environments. Aims. To understand the first steps of planet formation in scaled-down versions of T-Tauri disks, we investigate the physical conditions that can theoretically explain the growth from interstellar dust to millimeter-sized grains in disks around brown dwarf. Methods. We modeled the evolution of dust particles under conditions of low-mass disks around brown dwarfs. We used coagulation, fragmentation, and disk-structure models to simulate the evolution of dust, with zero and non-zero radial drift. For the non-zero radial drift, we considered strong inhomogeneities in the gas surface density profile that mimic long-lived pressure bumps in the disk. We studied different scenarios that could lead to an agreement between theoretical models and the spectral slope found by millimeter observations. Results. We find that fragmentation is less likely and rapid inward drift is more significant for particles in brown dwarf disks than in T-Tauri disks. We present different scenarios that can nevertheless explain millimeter-sized grains. As an example, a model that combines the following parameters can fit the millimeter fluxes measured for brown dwarf disks: strong pressure inhomogeneities of similar to 40% of amplitude, a small radial extent similar to 15 AU, a moderate turbulence strength alpha(turb) = 10(-3), and average fragmentation velocities for ices nu(f) = 10 m s(-1). C1 [Pinilla, P.; Dullemond, C. P.] Heidelberg Univ, Inst Theoret Astrophys, D-69120 Heidelberg, Germany. [Pinilla, P.] Heidelberg Univ, IMPRS Astron & Cosm Phys, D-69120 Heidelberg, Germany. [Birnstiel, T.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Birnstiel, T.] Excellence Cluster Universe, D-85748 Garching, Germany. [Benisty, M.] CNRS UJF UMR 5571, Astrophys Lab, Observ Grenoble, F-38041 Grenoble 9, France. [Ricci, L.] CALTECH, Pasadena, CA 91125 USA. [Natta, A.; Testi, L.] INAF Osservatorio Astrofis Arcetri, I-50125 Florence, Italy. [Natta, A.] Dublin Inst Adv Studies, Sch Cosm Phys, Dublin 2, Ireland. [Dominik, C.] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1090 GE Amsterdam, Netherlands. [Dominik, C.] Radboud Univ Nijmegen, Dept Astrophys IMAPP, NL-6500 GL Nijmegen, Netherlands. [Testi, L.] European So Observ, D-85748 Garching, Germany. RP Pinilla, P (reprint author), Heidelberg Univ, Inst Theoret Astrophys, Albert Ueberle Str 2, D-69120 Heidelberg, Germany. EM pinilla@uni-heidelberg.de OI Dullemond, Cornelis/0000-0002-7078-5910; Birnstiel, Tilman/0000-0002-1899-8783 FU NASA Origins of Solar Systems [NNX12AJ04G]; Ministry for Education and Research (Bundesministerium fur Bildung und Forschung); Ministry for Science, Research and Arts Baden-Wuerttemberg (Ministerium fur Wissenschaft, Forschung und Kunst Baden-Wurttemberg) FX We thank the anonymous referee for his/her constructive report, which helped us to improve and clarify the main results of the paper. T. Birnstiel acknowledges support from NASA Origins of Solar Systems grant NNX12AJ04G. P. Pinilla acknowledges the CPU time for running simulations in bwGRiD, member of the German D-Grid initiative, funded by the Ministry for Education and Research (Bundesministerium fur Bildung und Forschung) and the Ministry for Science, Research and Arts Baden-Wuerttemberg (Ministerium fur Wissenschaft, Forschung und Kunst Baden-Wurttemberg). NR 69 TC 9 Z9 9 U1 1 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 JUN PY 2013 VL 554 AR A95 DI 10.1051/0004-6361/201220875 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 164XA UT WOS:000320444200094 ER PT J AU Rivilla, VM Martin-Pintado, J Jimenez-Serra, I Rodriguez-Franco, A AF Rivilla, V. M. Martin-Pintado, J. Jimenez-Serra, I. Rodriguez-Franco, A. TI The role of low-mass star clusters in massive star formation. The Orion case SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE stars: formation; stars: low-mass; stars: massive; stars: pre-main sequence; ISM: clouds; X-rays: stars ID RADIATION-HYDRODYNAMIC SIMULATIONS; YOUNG STELLAR OBJECTS; NEBULA-CLUSTER; X-RAY; MOLECULAR CLOUDS; BINARY-SYSTEMS; GRAVITATIONAL COLLAPSE; COMPETITIVE ACCRETION; COLLISIONAL FORMATION; ULTRADEEP PROJECT AB Context: Different theories have been proposed to explain the formation of massive stars: two are based on accretion processes (monolithic core accretion and competitive accretion), and another on coalescence of low- and intermediate-mass stars. To distinguish between these theories, it is crucial to establish the distribution, the extinction, and the density of young low-mass stars in massive star-forming regions. X-ray observations can penetrate the very obscured cradles of massive stars, directly sampling the distribution of the population of pre-main sequence (PMS) low-mass stars in these regions. Aims. Our aim is to analyze deep X-ray observations of the Orion massive star-forming region using the Chandra Orion Ultradeep Project (COUP) catalog, to reveal the distribution of the population and clustering of PMS low-mass stars, and to study their possible role in massive star formation. Methods. We studied the distribution of PMS low-mass stars with X-ray emission in Orion as a function of extinction with two different methods: a spatial gridding and a close-neigbors method with cells of similar to 0.03 x 0.03 pc(2), the typical size of protostellar cores. We derived density maps of the stellar population and calculated cluster stellar densities. Results. Consistent with previous studies, we found that PMS low-mass stars cluster toward the three massive star-forming regions: the Trapezium cluster (TC), the Orion hot core (OHC), and the OMC1-S region. We derived PMS low-mass stellar densities of 10(5) stars pc(-3) in the TC and OMC1-S, and of 10(6) stars pc(-3) in the OHC. The close association between the low-mass star clusters with massive star cradles supports the role of these clusters in the formation of massive stars. The X-ray observations show for the first time in the TC that low-mass stars with intermediate extinction are clustered toward the position of the most massive star theta(1) Ori C, which is surrounded by a ring of non-extincted PMS low-mass stars. This "envelope-core" structure is also supported by infrared and optical observations. Our analysis suggests that at least two basic ingredients are needed in massive star formation: the presence of dense gas and a cluster of low-mass stars. The scenario that better explains our findings assumes high fragmentation in the parental core, accretion at subcore scales that forms a low-mass stellar cluster, and subsequent competitive accretion. Finally, although coalescence does not seem a common mechanism for building up massive stars, we show that a single stellar merger may have occurred in the evolution of the OHC cluster, favored by the presence of disks, binaries, and gas accretion. C1 [Rivilla, V. M.; Martin-Pintado, J.; Rodriguez-Franco, A.] Ctr Astrobiol CSIC INTA, Madrid 28850, Spain. [Jimenez-Serra, I.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Rivilla, VM (reprint author), Ctr Astrobiol CSIC INTA, Km 4, Madrid 28850, Spain. EM rivilla@cab.inta-csic.es RI Martin-Pintado, Jesus/H-6107-2015 OI Martin-Pintado, Jesus/0000-0003-4561-3508 FU MICINN [ESP2007-65812-C02-C01, AYA2010-21697-C05-01]; AstroMadrid [CAM S2009/ESP-1496]; Spanish CSIC FX We thank the Spanish MICINN for the support provided through grants ESP2007-65812-C02-C01 and AYA2010-21697-C05-01, and AstroMadrid (CAM S2009/ESP-1496), and the Spanish CSIC for the grant Jae-Predoc2008. V.M.R. acknowledges Jorge Sanz-Forcada for the very useful discussions about the X-ray science contained in this work. NR 92 TC 12 Z9 12 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 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD JUN PY 2013 VL 554 AR A48 DI 10.1051/0004-6361/201117487 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 164XA UT WOS:000320444200047 ER PT J AU Stute, M Luna, GJM Pillitteri, IF Sokoloski, JL AF Stute, M. Luna, G. J. M. Pillitteri, I. F. Sokoloski, J. L. TI Detection of X-rays from the jet-driving symbiotic star Hen 3-1341 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE binaries: symbiotic; white dwarfs; X-rays: stars; ISM: jets and outflows; stars: individual: Hen 3-1341 (V2523 Oph) ID EMISSION-LINE STARS; CH-CYGNI; HYDRODYNAMICAL SIMULATIONS; WAVELET TRANSFORMS; WHITE-DWARF; R-AQUARII; CLASSIFICATION; OUTBURST; DECLINE; SYSTEMS AB Context. Hen 3-1341 is a symbiotic binary system consisting of a white dwarf and a red giant star that is one of about ten symbiotics that show hints of jets. The bipolar jets have been detected through displaced components of emission lines during its outburst from 1998 to 2004. These components disappeared when Hen 3-1341 reached quiescence. On February 23, 2012, Hen 3-1341 started a new outburst with the emergence of new bipolar jets on March 3, 2012. Aims. We observed Hen 3-1341 during quiescence with XMM-Newton in March 2010 with an effective exposure time of 46.8 ks and with Swift on March 8-11, 2012 as ToO observations with an effective exposure time of 10 ks in order to probe the interaction of the jet with the ambient medium and also the accretion onto the white dwarf. Methods. We fitted the XMM-Newton X-ray spectra with XSPEC and examined the X-ray and UV light curves. Results. We report the detection of X-ray emission during quiescence from Hen 3-1341 with XMM-Newton. The spectrum can be fitted with an absorbed one-temperature plasma or an absorbed blackbody. We did not detect Hen 3-1341 during our short Swift exposure. Neither periodic or aperiodic X-ray nor UV variability were found. Conclusions. Our XMM-Newton data suggest that interaction of the residual jet with the interstellar medium might survive for a long time after outbursts and might be responsible for the observed X-ray emission during quiescence. Additional data are strongly needed to confirm these suggestions. C1 [Stute, M.] Univ Tubingen, Inst Astron & Astrophys, Sect Computat Phys, D-72076 Tubingen, Germany. [Luna, G. J. M.] Inst Astron & Fis Espacio CONICET UBA, Buenos Aires, DF, Argentina. [Luna, G. J. M.; Pillitteri, I. F.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Sokoloski, J. L.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA. RP Stute, M (reprint author), Univ Tubingen, Inst Astron & Astrophys, Sect Computat Phys, Morgenstelle 10, D-72076 Tubingen, Germany. EM matthias.stute@tat.physik.uni-tuebingen.de RI Pillitteri, Ignazio/L-1549-2016 OI Pillitteri, Ignazio/0000-0003-4948-6550 FU ESA Member States; USA (NASA); NASA [NNX09AP88G, NNX10AK31G]; National Aeronautics and Space Administration; National Science Foundation FX We acknowledge helpful comments and suggestions by an anonymous referee. 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). We thank NASA for funding this work through XMM-Newton AO-8 awards NNX09AP88G to GJML and JLS, and NNX10AK31G to J.L.S.. We gratefully acknowledge the effort of the entire Swift team for the execution of our ToO request. 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 acknowledge with thanks the variable star observations from the AAVSO International Database contributed by observers worldwide and used in this research. NR 38 TC 1 Z9 1 U1 1 U2 1 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD JUN PY 2013 VL 554 AR A56 DI 10.1051/0004-6361/201218998 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 164XA UT WOS:000320444200055 ER PT J AU van der Tak, FFS Chavarria, L Herpin, F Wyrowski, F Walmsley, CM Van Dishoeck, EF Benz, AO Bergin, EA Caselli, P Hogerheijde, MR Johnstone, D Kristensen, LE Liseau, R Nisini, B Tafalla, M AF van der Tak, F. F. S. Chavarria, L. Herpin, F. Wyrowski, F. Walmsley, C. M. van Dishoeck, E. F. Benz, A. O. Bergin, E. A. Caselli, P. Hogerheijde, M. R. Johnstone, D. Kristensen, L. E. Liseau, R. Nisini, B. Tafalla, M. TI Water in star-forming regions with Herschel (WISH) IV. A survey of low-J H2O line profiles toward high-mass protostars SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE stars: formation; ISM: molecules; astrochemistry ID H-II-REGIONS; ULTRACOMPACT HII-REGIONS; YOUNG STELLAR OBJECTS; NGC 6334 I; EARLY EVOLUTIONARY STAGES; TRIGONOMETRIC PARALLAXES; HIFI OBSERVATIONS; DISTANCE AMBIGUITIES; GALACTIC STRUCTURE; HYDROGEN-FLUORIDE AB Context. Water is a key constituent of star-forming matter, but the origin of its line emission and absorption during high-mass star formation is not well understood. Aims. We study the velocity profiles of low-excitation H2O lines toward 19 high-mass star-forming regions and search for trends with luminosity, mass, and evolutionary stage. Methods. We decompose high-resolution Herschel-HIFI line spectra near 990, 1110 and 1670 GHz into three distinct physical components. Dense cores (protostellar envelopes) are usually seen as narrow absorptions in the H2O 1113 and 1669 GHz ground-state lines, the H2O 987 GHz excited-state line, and the (H2O)-O-18 1102 GHz ground-state line. In a few sources, the envelopes appear in emission in some or all studied lines, indicating higher temperatures or densities. Broader features due to outflows are usually seen in absorption in the H2O 1113 and 1669 GHz lines, in 987 GHz emission, and not seen in (H2O)-O-18, indicating a lower column density and a higher excitation temperature than the envelope component. A few outflows are detected in (H2O)-O-18, indicating higher column densities of shocked gas. In addition, the H2O 1113 and 1669 GHz spectra show narrow absorptions by foreground clouds along the line of sight. The lack of corresponding features in the 987 GHz and (H2O)-O-18 lines indicates a low column density and a low excitation temperature for these clouds, although their derived H2O ortho/para ratios are close to 3. Results. The intensity of the ground state lines of H2O at 1113 and 1669 GHz does not show significant trends with source luminosity, envelope mass, or evolutionary state. In contrast, the flux in the excited-state 987 GHz line appears correlated with luminosity and the (H2O)-O-18 line flux appears correlated with the envelope mass. Furthermore, appearance of the envelope in absorption in the 987 GHz and (H2O)-O-18 lines seems to be a sign of an early evolutionary stage, as probed by the mid-infrared brightness and the L-bol/M-env ratio of the source. Conclusions. The ground state transitions of H2O trace the outer parts of the envelopes, so that the effects of star formation are mostly noticeable in the outflow wings. These lines are heavily affected by absorption, so that line ratios of H2O involving the ground states must be treated with caution, especially if multiple clouds are superposed as in the extragalactic case. The isotopic (H2O)-O-18 line appears to trace the mass of the protostellar envelope, indicating that the average H2O abundance in high-mass protostellar envelopes does not change much with time. The excited state line at 987 GHz increases in flux with luminosity and appears to be a good tracer of the mean weighted dust temperature of the source, which may explain why it is readily seen in distant galaxies. C1 [van der Tak, F. F. S.] SRON Netherlands Inst Space Res, NL-9747 AD Groningen, Netherlands. [van der Tak, F. F. S.] Univ Groningen, Kapteyn Astron Inst, NL-9700 AB Groningen, Netherlands. [Chavarria, L.; Herpin, F.] Univ Bordeaux, LAB, F-33270 Floirac, France. [Chavarria, L.; Herpin, F.] CNRS, LAB, F-33271 Floirac, France. [Chavarria, L.] Ctr Astrobiol CSIC INTA, Madrid 28850, Spain. [Wyrowski, F.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Walmsley, C. M.] INAF Osservatorio Astrofis Arcetri, I-50125 Florence, Italy. [Walmsley, C. M.] Dublin Inst Adv Studies, Dublin 4, Ireland. [van Dishoeck, E. F.; Hogerheijde, M. R.; Kristensen, L. E.] Leiden Univ, Leiden Observ, Leiden, Netherlands. [van Dishoeck, E. F.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Benz, A. O.] Swiss Fed Inst Technol, Inst Astron, 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. [Johnstone, D.] Joint Astron Ctr, Hilo, HI 96720 USA. [Kristensen, L. E.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Liseau, R.] Chalmers, Onsala Space Observ, S-41296 Gothenburg, Sweden. [Nisini, B.] INAF Osservatorio Astrofis Roma, Rome, Italy. [Tafalla, M.] Observ Astron Nacl, Madrid 28049, Spain. RP van der Tak, FFS (reprint author), SRON Netherlands Inst Space Res, Landleven 12, NL-9747 AD Groningen, Netherlands. EM vdtak@sron.nl RI Kristensen, Lars/F-4774-2011; OI Kristensen, Lars/0000-0003-1159-3721; , Brunella Nisini/0000-0002-9190-0113 FU Spanish MINECO [AYA2009-07304] FX This paper is dedicated to the memory of Annemieke Gloudemans-Boonman, a pioneer of H2O observations with ISO, who passed away on 11 October 2010 at the age of 35. We thank Umut Yildiz for maintaining the WISH data archive (the "live show"), Agata Karska for providing PACS continuum fluxes of our sources, and the referee for carefully reading our manuscript and writing a constructive report. This work has used the spectroscopic databases of JPL (Pickett et al. 1998) and CDMS (Muller et al. 2001), and the facilities of the Canadian Astronomy Data Centre operated by the the National Research Council of Canada with the support of the Canadian Space Agency. L.C. thanks the Spanish MINECO for funding support from grant AYA2009-07304. HIFI has been designed and built by a consortium of institutes and university departments from across Europe, Canada and the US under the leadership of SRON Netherlands Institute for Space Research, Groningen, The Netherlands 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, Arcetri-INAF; Netherlands: SRON, TUD; Poland: CAMK, CBK; Spain: Observatorio Astronomico Nacional (IGN), Centro de Astrobiologia (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. NR 96 TC 31 Z9 31 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 JUN PY 2013 VL 554 AR A83 DI 10.1051/0004-6361/201220976 PG 34 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 164XA UT WOS:000320444200082 ER PT J AU Vargas-Magana, M Bautista, JE Hamilton, JC Busca, NG Aubourg, E Labatie, A Le Goff, JM Escoffier, S Manera, M McBride, CK Schneider, DP Willmer, CNA AF Vargas-Magana, M. Bautista, J. E. Hamilton, J. -Ch. Busca, N. G. Aubourg, E. Labatie, A. Le Goff, J. -M. Escoffier, S. Manera, M. McBride, C. K. Schneider, D. P. Willmer, Ch. N. A. TI An optimized correlation function estimator for galaxy surveys SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE surveys; large-scale structure of Universe; galaxies: statistics; distance scale; cosmology: observations; methods: data analysis ID DIGITAL SKY SURVEY; OSCILLATION SPECTROSCOPIC SURVEY; BARYON ACOUSTIC-OSCILLATIONS; LUMINOUS RED GALAXIES; ANGULAR-CORRELATION FUNCTIONS; 2-POINT CORRELATION-FUNCTION; SDSS-III; DATA RELEASE; COSMOLOGICAL CONSTANT; REDSHIFT-SPACE AB Measuring the two-point correlation function of the galaxies in the Universe gives access to the underlying dark matter distribution, which is related to cosmological parameters and to the physics of the primordial Universe. The estimation of the correlation function for current galaxy surveys makes use of the Landy-Szalay estimator, which is supposed to reach minimal variance. This is only true, however, for a vanishing correlation function. We study the Landy-Szalay estimator when these conditions are not fulfilled and propose a new estimator that provides the smallest variance for a given survey geometry. Our estimator is a linear combination of ratios between pair counts of data and/or random catalogues (DD, RR, and DR). The optimal combination for a given geometry is determined by using lognormal mock catalogues. The resulting estimator is biased in a model-dependent way, but we propose a simple iterative procedure for obtaining an unbiased model-independent estimator. Our method can be easily applied to any dataset and requires few extra mock catalogues compared to the standard Landy-Szalay analysis. Using various sets of simulated data (lognormal, second-order LPT, and N-body), we obtain a 20-25% gain on the error bars on the two-point correlation function for the SDSS geometry and Lambda CDM correlation function. When applied to SDSS data (DR7 and DR9), we achieve a similar gain on the correlation functions, which translates into a 10-15% improvement over the estimation of the densities of matter Omega(m) and dark energy Omega(A) in an open ACDM model. The constraints derived from DR7 data with our estimator are similar to those obtained with the DR9 data and the Landy-Szalay estimator, which covers a volume twice as large and has a density that is three times higher. C1 [Vargas-Magana, M.; Bautista, J. E.; Hamilton, J. -Ch.; Busca, N. G.; Aubourg, E.] Univ Paris Diderot, Sorbonne Paris Cite, Observ Paris, CNRS IN2P3,CEA Irfu,APC, F-75205 Paris 13, France. [Labatie, A.] CEA DSM CNRS Univ Paris Diderot, Ctr Saclay, Serv Astrophys, IRFU,SEDI SAP,Lab AIM, F-91191 Gif Sur Yvette, France. [Le Goff, J. -M.] CEA Ctr Saclay, Irfu SPP, F-91191 Gif Sur Yvette, France. [Escoffier, S.] Aix Marseille Univ, CNRS IN2P3, CPPM, F-13288 Marseille 9, France. [Manera, M.] Univ Portsmouth, Inst Cosmol & Gravitat, Portsmouth PO1 3FX, Hants, England. [McBride, C. K.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Schneider, D. P.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Schneider, D. P.] Penn State Univ, Inst Gravitat & Cosmos, University Pk, PA 16802 USA. [Willmer, Ch. N. A.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. RP Vargas-Magana, M (reprint author), Univ Paris Diderot, Sorbonne Paris Cite, Observ Paris, CNRS IN2P3,CEA Irfu,APC, 10 Rue Alice Domon & Lonie Duquet, F-75205 Paris 13, France. EM mariana@apc.univ-paris7.fr OI Escoffier, Stephanie/0000-0002-2847-7498 FU Agence Nationale de la Recherche [ANR-08-BLAN-0222]; Alfred P. Sloan Foundation; National Science Foundation; U.S. Department of Energy Office of Science; University of Arizona; Brookhaven National Laboratory; University of Cambridge; Carnegie Mellon University; University of Florida; German Participation Group; Harvard University; Instituto de Astrofisica de Canarias; Michigan State/Notre Dame/JINA Participation Group; Johns Hopkins University; Lawrence Berkeley National Laboratory; Max Planck Institute for Astrophysics; Max Planck Institute for Extraterrestrial Physics; New Mexico State University; New York University; Ohio State University; Pennsylvania State University; University of Portsmouth; Princeton University; University of Tokyo; University of Utah; Vanderbilt University; University of Virginia; University of Washington; Yale University FX We would like to thank the SDSS-III collaboration for such wonderful data. We thank N. Padmanabhan, and J.K. Parejko for making their kd-tree code available. We used the "gamma" release LRG galaxy mock catalogues produced by the LasDamas projecta and we thank the LasDamas collaboration for providing us with this data. We would like to thank R. Skibba, Chia-Hsun Chuang, Lado Samushia, and Graziano Rossi for helpful suggestions and comments. This project was supported by the Agence Nationale de la Recherche under contract ANR-08-BLAN-0222. Funding for SDSS-III has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, and the U.S. Department of Energy Office of Science. The SDSS-III web site is http://www.sdss3.org/. SDSS-III is managed by the Astrophysical Research Consortium for the Participating Institutions of the SDSS-III Collaboration including the University of Arizona, the Brazilian Participation Group, Brookhaven National Laboratory, University of Cambridge, Carnegie Mellon University, University of Florida, the French Participation Group, the German Participation Group, Harvard University, the Instituto de Astrofisica de Canarias, the Michigan State/Notre Dame/JINA Participation Group, Johns Hopkins University, Lawrence Berkeley National Laboratory, Max Planck Institute for Astrophysics, Max Planck Institute for Extraterrestrial Physics, New Mexico State University, New York University, Ohio State University, Pennsylvania State University, University of Portsmouth, Princeton University, the Spanish Participation Group, University of Tokyo, University of Utah, Vanderbilt University, University of Virginia, University of Washington, and Yale University. NR 46 TC 3 Z9 3 U1 1 U2 8 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 JUN PY 2013 VL 554 AR A131 DI 10.1051/0004-6361/201220790 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 164XA UT WOS:000320444200130 ER PT J AU Clark, JL Skog, LE AF Clark, John L. Skog, Laurence E. TI Novae Gesneriaceae Neotropicarum XVIII: Columnea carinata, a new species of Gesneriaceae from northwestern Ecuador SO BRITTONIA LA English DT Article DE Columnea; Ecuador; Episcieae; Gesneriaceae; Pentadenia; taxonomy ID NORTHERN ECUADOR AB A new species of Columnea (Gesneriaceae, tribe Episcieae) is described from the Choc floristic region of the western Andean slopes of northern Ecuador. Columnea carinata differs from other congeners by the presence of elongate shoots, isophyllous leaves, and a uniformly bright red corolla, with nearly complete fusion of the upper two corolla lobes and an elongate keel on the dorsal surface of the corolla tube. C1 [Clark, John L.] Univ Alabama, Dept Biol Sci, Tuscaloosa, AL 35487 USA. [Clark, John L.; Skog, Laurence E.] Natl Museum Nat Hist, Smithsonian Inst, Dept Bot, Washington, DC 20013 USA. RP Clark, JL (reprint author), Univ Alabama, Dept Biol Sci, Box 870345, Tuscaloosa, AL 35487 USA. EM jlc@ua.edu; skogl@si.edu FU National Science Foundation [DEB-841958, DEB-0949169] FX This study was supported by funds from the National Science Foundation (DEB-841958 and DEB-0949169). We thank Christian Feuillet for providing the Latin diagnosis and help in selecting the specific epithet; Laura Clavijo for providing the Spanish translation of the abstract; Jeremy Keene and Alain Chautems for providing helpful reviews of the manuscript; and Alice Tangerini for preparing the illustration. The first author made the initial discovery of Columnea carinata while assisting Walter Palacios (QCNE) as a U. S. Peace Corps Volunteer in 1994. The first author would like to express gratitude to Walter Palacios for his collegiality and mentorship from 1994 to 1998. Special thanks are due to Maria Eliza Manteca Onate for her heroic efforts in promoting biodiversity and conservation through the Cerro Golondrinas Cloudforest Conservation Project and Reserve in 1991 and now through the Fundacion Golondrinas. NR 11 TC 0 Z9 0 U1 0 U2 0 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0007-196X J9 BRITTONIA JI Brittonia PD JUN PY 2013 VL 65 IS 2 BP 186 EP 190 DI 10.1007/s12228-012-9277-6 PG 5 WC Plant Sciences SC Plant Sciences GA 168TT UT WOS:000320729400008 ER PT J AU de Stapf, MNS Silva, TRD AF Sanchez de Stapf, Maria Natividad dos Santos Silva, Tania Regina TI Four new species of genus Cordia (Cordiaceae, Boraginales) from Brazil SO BRITTONIA LA English DT Article DE Cordia; Cordiaceae; neotropical; taxonomy AB We describe four new species of Cordia (Cordiaceae) from Brazil: Cordia fusca, C. glabrifolia, C. restingae, and C. tarodae. These are illustrated, and data on habitat, phenology, and distribution are provided. C1 [Sanchez de Stapf, Maria Natividad; dos Santos Silva, Tania Regina] Univ Estadual Feira de Santana, Dept Ciencias Biol, BR-44031460 Feira De Santana, BA, Brazil. [Sanchez de Stapf, Maria Natividad] Smithsonian Trop Res Inst, Balboa 084303092, Panama. RP de Stapf, MNS (reprint author), Univ Estadual Feira de Santana, Dept Ciencias Biol, Km 03,BR 116, BR-44031460 Feira De Santana, BA, Brazil. EM stapfm@si.edu; tsilva@uefs.br FU Organization American States (OAS); Secretaria Nacional de Ciencia y Tecnologia (SENACYT) of Panama; CNPq FX We thank to Organization American States (OAS) and Secretaria Nacional de Ciencia y Tecnologia (SENACYT) of Panama for a Ph.D. fellowship for the first author, and the Kew Latin America Research Fellowship Programme (KLARF), for having provided support to visit European herbaria. We thank the curators of the following herbaria for providing loans of specimens or access to collections: ALCB, BHCB, CEPEC, HUEFS, K, MBM, MO, NY, SJRP and UEC. We also thank Dr. Cassio van den Berg for helping with the Latin diagnoses, and Carla de Lima for the illustrations. T. R. S. Silva was supported by CNPq. NR 3 TC 2 Z9 2 U1 1 U2 3 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0007-196X J9 BRITTONIA JI Brittonia PD JUN PY 2013 VL 65 IS 2 BP 191 EP 199 DI 10.1007/s12228-012-9268-7 PG 9 WC Plant Sciences SC Plant Sciences GA 168TT UT WOS:000320729400009 ER PT J AU Pratt, PD Makinson, J Purcell, M Pogue, MG Rayamajhi, MB Center, TD AF Pratt, Paul D. Makinson, Jeff Purcell, Matthew Pogue, Michael G. Rayamajhi, Min B. Center, Ted D. TI RHODOMYRTUS TOMENTOSA (MYRTALES: MYRTACEAE): NEW HOST RECORDS FOR METANASTRIA GEMELLA (LEPIDOPTERA: LASIOCAMPIDAE) AND ARNA BIPUNCTAPEX (LEPIDOPTERA: LYMANTRIIDAE) SO FLORIDA ENTOMOLOGIST LA English DT Editorial Material DE biological control; herbivores; host specificity; invasive species; rose myrtle AB Surveys for host specific natural enemies of Rhodomyrtus tomentosa (Myrtales: Myrtaceae), rose myrtle, in China (mainland and Hong Kong) resulted in the discovery of 2 lepidopteran species that have not been previously reported as herbivores of the plant: Metanastria gemella Lajonquiere (Lasiocampidae) and Arna bipunctapex Hampson (Lymantriidae). Multiple generations of both species were reared on R. tomentosa in a quarantine laboratory, demonstrating that the plant is a developmental host. However, neither species demonstrates sufficient host specificity to be considered for biological control of R. tomentosa in the USA. C1 [Pratt, Paul D.; Rayamajhi, Min B.; Center, Ted D.] ARS, USDA, Invas Plant Res Lab, Ft Lauderdale, FL 33314 USA. [Makinson, Jeff; Purcell, Matthew] CSIRO Ecosyst Sci, ARS, USDA, Australian Biol Control Lab, Brisbane, Qld 4001, Australia. [Pogue, Michael G.] ARS, USDA, Systemat Entomol Lab, Smithsonian Inst, Washington, DC 20013 USA. RP Pratt, PD (reprint author), ARS, USDA, Invas Plant Res Lab, 3225 Coll Ave, Ft Lauderdale, FL 33314 USA. EM Paul.Pratt@ars.usda.gov RI Makinson, Jeffrey/M-7031-2014 OI Makinson, Jeffrey/0000-0001-9870-5866 NR 6 TC 4 Z9 4 U1 0 U2 4 PU FLORIDA ENTOMOLOGICAL SOC PI LUTZ PA 16125 E LAKE BURRELL DR, LUTZ, FL 33548 USA SN 0015-4040 J9 FLA ENTOMOL JI Fla. Entomol. PD JUN PY 2013 VL 96 IS 2 BP 641 EP 642 PG 2 WC Entomology SC Entomology GA 168VY UT WOS:000320737200045 ER PT J AU Warner, D AF Warner, Deborah TI From Earth-Bound to Satellite: Telescopes, Skills, and Networks SO ISIS LA English DT Book Review C1 [Warner, Deborah] Smithsonian Inst, Natl Museum Amer Hist, Washington, DC 20560 USA. RP Warner, D (reprint author), Smithsonian Inst, Natl Museum Amer Hist, Washington, DC 20560 USA. NR 1 TC 0 Z9 0 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0021-1753 J9 ISIS JI Isis PD JUN PY 2013 VL 104 IS 2 BP 387 EP 387 DI 10.1086/672172 PG 1 WC History & Philosophy Of Science SC History & Philosophy of Science GA 172YW UT WOS:000321044500017 ER PT J AU Brown, JK AF Brown, Julie K. TI Popular Exhibitions, Science, and Showmanship, 1840-1910 SO ISIS LA English DT Book Review C1 [Brown, Julie K.] Smithsonian Inst, Natl Museum Amer Hist, Washington, DC 20560 USA. RP Brown, JK (reprint author), Smithsonian Inst, Natl Museum Amer Hist, Washington, DC 20560 USA. NR 1 TC 0 Z9 0 U1 3 U2 6 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0021-1753 EI 1545-6994 J9 ISIS JI Isis PD JUN PY 2013 VL 104 IS 2 BP 407 EP 408 DI 10.1086/672192 PG 4 WC History & Philosophy Of Science SC History & Philosophy of Science GA 172YW UT WOS:000321044500037 ER PT J AU Murphy, NA Young, AK Shen, CC Lin, J Ni, L AF Murphy, Nicholas A. Young, Aleida K. Shen, Chengcai Lin, Jun Ni, Lei TI The plasmoid instability during asymmetric inflow magnetic reconnection SO PHYSICS OF PLASMAS LA English DT Article ID EJECTION CURRENT SHEETS; CORONAL MASS EJECTIONS; SOLAR-FLARES; TEARING INSTABILITY; NUMERICAL EXPERIMENTS; DAYSIDE MAGNETOPAUSE; DENSITY ASYMMETRY; SIMULATION; ERUPTION; MODE AB Theoretical studies of the plasmoid instability generally assume that the reconnecting magnetic fields are symmetric. We relax this assumption by performing two-dimensional resistive magnetohydrodynamic simulations of the plasmoid instability during asymmetric inflow magnetic reconnection. Magnetic asymmetry modifies the onset, scaling, and dynamics of this instability. Magnetic islands develop preferentially into the weak magnetic field upstream region. Outflow jets from individual X-points impact plasmoids obliquely rather than directly as in the symmetric case. Consequently, deposition of momentum by the outflow jets into the plasmoids is less efficient, the plasmoids develop net vorticity, and shear flow slows down secondary merging between islands. Secondary merging events have asymmetry along both the inflow and outflow directions. Downstream plasma is more turbulent in cases with magnetic asymmetry because islands are able to roll around each other after exiting the current sheet. As in the symmetric case, plasmoid formation facilitates faster reconnection for at least small and moderate magnetic asymmetries. However, when the upstream magnetic field strengths differ by a factor of 4, the reconnection rate plateaus at a lower value than expected from scaling the symmetric results. We perform a parameter study to investigate the onset of the plasmoid instability as a function of magnetic asymmetry and domain size. There exist domain sizes for which symmetric simulations are stable but asymmetric simulations are unstable, suggesting that moderate magnetic asymmetry is somewhat destabilizing. We discuss the implications for plasmoid and flux rope formation in solar eruptions, laboratory reconnection experiments, and space plasmas. The differences between symmetric and asymmetric simulations provide some hints regarding the nature of the three-dimensional plasmoid instability. (C) 2013 AIP Publishing LLC. C1 [Murphy, Nicholas A.; Young, Aleida K.; Shen, Chengcai; Lin, Jun] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Young, Aleida K.] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA. [Shen, Chengcai; Lin, Jun; Ni, Lei] Chinese Acad Sci, Yunnan Astron Observ, Kunming 650011, Yunnan, Peoples R China. [Shen, Chengcai] Chinese Acad Sci, Grad Sch, Beijing 100049, Peoples R China. RP Murphy, NA (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM namurphy@cfa.harvard.edu RI LIN, JUN/B-9890-2017; OI Murphy, Nicholas/0000-0001-6628-8033 FU NASA [NNX09AB17G, NNX11AB61G, NNX12AB25G, NNM07AB07C]; NSF SHINE [AGS-1156076]; NSF-REU solar physics program at the Center for Astrophysics [ATM-0851866] FX This research was supported by NASA Grants NNX09AB17G, NNX11AB61G, and NNX12AB25G; NASA contract NNM07AB07C; and NSF SHINE Grant AGS-1156076 to the Smithsonian Astrophysical Observatory. A.K.Y. acknowledges support from the NSF-REU solar physics program at the Center for Astrophysics, Grant No. ATM-0851866. NR 115 TC 11 Z9 11 U1 0 U2 11 PU AMER INST PHYSICS PI MELVILLE PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1, MELVILLE, NY 11747-4501 USA SN 1070-664X EI 1089-7674 J9 PHYS PLASMAS JI Phys. Plasmas PD JUN PY 2013 VL 20 IS 6 AR 061211 DI 10.1063/1.4811470 PG 12 WC Physics, Fluids & Plasmas SC Physics GA 175ZT UT WOS:000321273200013 ER PT J AU Ni, L Lin, J Murphy, NA AF Ni, Lei Lin, Jun Murphy, Nicholas A. TI Effects of the non-uniform initial environment and the guide field on the plasmoid instability SO PHYSICS OF PLASMAS LA English DT Article ID RECONNECTING CURRENT SHEETS; MAGNETIC RECONNECTION; SECONDARY ISLANDS; ACCELERATION; FLARES AB Effects of non-uniform initial mass density and temperature on the plasmoid instability are studied via 2.5-dimensional resistive magnetohydrodynamic (MHD) simulations. Our results indicate that the development of the plasmoid instability is apparently prevented when the initial plasma density at the center of the current sheet is higher than that in the upstream region. As a result, the higher the plasma density at the center and the lower the plasma beta in the upstream region, the higher the critical Lundquist number needed for triggering secondary instabilities. When beta = 0.2, the critical Lundquist number is higher than 10(4). For the same Lundquist number, the magnetic reconnection rate is lower for the lower plasma beta case. Oppositely, when the initial mass density is uniform and the Lundquist number is low, the magnetic reconnection rate turns out to be higher for the lower plasma beta case. For the high Lundquist number case (>10(4)) with uniform initial mass density, the magnetic reconnection is not affected by the initial plasma beta and the temperature distribution. Our results indicate that the guide field has a limited impact on the plasmoid instability in resistive MHD. (C) 2013 AIP Publishing LLC. C1 [Ni, Lei; Lin, Jun] Chinese Acad Sci, Yunnan Astron Observ, Kunming 650011, Peoples R China. [Lin, Jun; Murphy, Nicholas A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Ni, L (reprint author), Chinese Acad Sci, Yunnan Astron Observ, Kunming 650011, Peoples R China. EM leini@ynao.ac.cn RI LIN, JUN/B-9890-2017; OI Murphy, Nicholas/0000-0001-6628-8033 FU NSFC [11147131]; NSFY [11203069]; 973 program [2013CBA01503]; CAS [KJCX2-EW-T07]; Yunnan Province [2011FB113]; NSF SHINE grant [AGS-1156076] FX This research was supported by NSFC (Grant No. 11147131), NSFY (Grant No. 11203069), the 973 program (Grant No. 2013CBA01503), CAS (Grant No. KJCX2-EW-T07), and the Yunnan Province (Grant No. 2011FB113). N.A.M. and J.L. also acknowledge support from NSF SHINE grant AGS-1156076. This work used the NIRVANA code v3.4 developed by Udo Ziegler at the Leibniz-Institut fur Astrophysik Potsdam. Calculations in this work were completed with the help of the HPC Center, Kunming Institute of Botany, CAS. NR 27 TC 7 Z9 7 U1 0 U2 6 PU AMER INST PHYSICS PI MELVILLE PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1, MELVILLE, NY 11747-4501 USA SN 1070-664X J9 PHYS PLASMAS JI Phys. Plasmas PD JUN PY 2013 VL 20 IS 6 AR 061206 DI 10.1063/1.4811144 PG 8 WC Physics, Fluids & Plasmas SC Physics GA 175ZT UT WOS:000321273200008 ER PT J AU Graves-Herring, JE Wildt, DE Comizzoli, P AF Graves-Herring, Jennifer E. Wildt, David E. Comizzoli, Pierre TI Retention of Structure and Function of the Cat Germinal Vesicle after Air-Drying and Storage at Suprazero Temperature SO BIOLOGY OF REPRODUCTION LA English DT Article DE desiccation; domestic cat; fertility preservation; gamete biology; germinal vesicle; meiotic maturation; oocyte ID IN-VITRO; MOUSE SPERMATOZOA; NUCLEAR TRANSFER; MAMMALIAN-CELLS; SOMATIC-CELLS; DOMESTIC CAT; OOCYTES; PRESERVATION; TREHALOSE; CRYOPRESERVATION AB The study explored a novel approach for preserving the maternal genome without the entire oocyte by air-drying the cat germinal vesicle (GV) in the presence of the disaccharide trehalose. Specifically, we examined GV structure and function after desiccation, storage at 4 degrees C (up to 32 wk), and rehydration including the ability to resume meiosis after injection into a fresh, conspecific cytoplast. In experiment 1, DNA integrity was similar to fresh controls after 1 and 4 wk storage in the presence of trehalose, but was more fragmented at later time points (especially after 32 wk). Nuclear envelope integrity was sustained in >90% of oocytes stored for 0, 4, or 16 wk regardless of protective treatment. In experiment 2, compacted, air-dried GVs were stored for 2 or 4 wk, rehydrated, and injected into fresh cytoplasts. After culture for 24 h in vitro, up to 73% of oocytes reconstructed with desiccated GVs preserved in trehalose resumed meiosis compared to 30% of those dried in the absence of the disaccharide. At each storage time point, trehalose presence during air-drying was advantageous for resumption of meiosis, with >20% of oocytes completing nuclear maturation to metaphase II. This demonstrates a potential for preserving the female genome using the GV alone and for multiple weeks after desiccation. Trehalose enhanced the process by retaining the ability of a dried and rehydrated GV to resume communication with the surrounding cytoplasm of the recipient oocyte to permit reaching metaphase II and likely sustain subsequent embryo development. C1 [Comizzoli, Pierre] Smithsonian Conservat Biol Inst, Natl Zool Pk, Washington, DC 20013 USA. Smithsonian Conservat Biol Inst, Natl Zool Pk, Front Royal, VA USA. RP Comizzoli, P (reprint author), Smithsonian Conservat Biol Inst, Natl Zool Pk, POB 37012,MRC 5502, Washington, DC 20013 USA. EM comizzolip@si.edu FU National Center for Research Resources [R01 RR026064]; National Institutes of Health (NIH); Office of Research Infrastructure Programs/Office of the Director [R01 OD 010948] FX Funded by the National Center for Research Resources (R01 RR026064), a component of the National Institutes of Health (NIH), and currently supported by the Office of Research Infrastructure Programs/Office of the Director (R01 OD 010948). Presented in part at the 44th Annual Meeting of the Society for the Study of Reproduction, 31 July-4 August 2011, Portland, Oregon. NR 42 TC 9 Z9 9 U1 0 U2 4 PU SOC STUDY REPRODUCTION PI MADISON PA 1691 MONROE ST,SUITE # 3, MADISON, WI 53711-2021 USA SN 0006-3363 J9 BIOL REPROD JI Biol. Reprod. PD JUN PY 2013 VL 88 IS 6 AR 139 DI 10.1095/biolreprod.113.108472 PG 7 WC Reproductive Biology SC Reproductive Biology GA 168RN UT WOS:000320723500002 PM 23575153 ER PT J AU Lohbeck, M Poorter, L Lebrija-Trejos, E Martinez-Ramos, M Meave, JA Paz, H Perez-Garcia, EA Romero-Perez, IE Tauro, A Bongers, F AF Lohbeck, Madelon Poorter, Lourens Lebrija-Trejos, Edwin Martinez-Ramos, Miguel Meave, Jorge A. Paz, Horacio Perez-Garcia, Eduardo A. Eunice Romero-Perez, I. Tauro, Alejandra Bongers, Frans TI Successional changes in functional composition contrast for dry and wet tropical forest SO ECOLOGY LA English DT Article DE acquisitive traits; community-weighted mean; conservative traits; dry deciduous forest; Mexico; secondary succession; wet evergreen forest ID LEAF LIFE-SPAN; SECONDARY SUCCESSION; SEED SIZE; NEOTROPICAL FORESTS; ECONOMICS SPECTRUM; WOODY-PLANTS; TRAITS; MORTALITY; DIVERSITY; WORLDWIDE AB We tested whether and how functional composition changes with succession in dry deciduous and wet evergreen forests of Mexico. We hypothesized that compositional changes during succession in dry forest were mainly determined by increasing water availability leading to community functional changes from conservative to acquisitive strategies, and in wet forest by decreasing light availability leading to changes from acquisitive to conservative strategies. Research was carried out in 15 dry secondary forest plots (5-63 years after abandonment) and 17 wet secondary forest plots (<1-25 years after abandonment). Community-level functional traits were represented by community-weighted means based on 11 functional traits measured on 132 species. Successional changes in functional composition are more marked in dry forest than in wet forest and largely characterized by different traits. During dry forest succession, conservative traits related to drought tolerance and drought avoidance decreased, as predicted. Unexpectedly acquisitive leaf traits also decreased, whereas seed size and dependence on biotic dispersal increased. In wet forest succession, functional composition changed from acquisitive to conservative leaf traits, suggesting light availability as the main driver of changes. Distinct suites of traits shape functional composition changes in dry and wet forest succession, responding to different environmental filters. C1 [Lohbeck, Madelon; Poorter, Lourens; Lebrija-Trejos, Edwin; Bongers, Frans] Wageningen Univ, Forest Ecol & Forest Management Grp, NL-6700 AA Wageningen, Netherlands. [Lohbeck, Madelon; Martinez-Ramos, Miguel; Paz, Horacio; Tauro, Alejandra] Univ Nacl Autonoma Mexico, Ctr Invest Ecosistemas, Morelia 58190, Michoacan, Mexico. [Lebrija-Trejos, Edwin] Smithsonian Trop Res Inst, Balboa Ancon, Panama. [Lebrija-Trejos, Edwin; Meave, Jorge A.; Perez-Garcia, Eduardo A.; Eunice Romero-Perez, I.] Univ Nacl Autonoma Mexico, Fac Ciencias, Dept Ecol & Recursos Nat, Mexico City 04510, DF, Mexico. RP Lohbeck, M (reprint author), Wageningen Univ, Forest Ecol & Forest Management Grp, POB 47, NL-6700 AA Wageningen, Netherlands. EM madelon.lohbeck@wur.nl RI Lohbeck, Madelon/M-6390-2014 OI Lohbeck, Madelon/0000-0002-3959-1800 FU Wageningen University and Research center; DiverSus project through the Inter-American Institute for Global Change Research (IAI) CRN; U.S. NSF [GEO-0452325, DEB-0639393]; CONACYT-SEMARNAT [2002-C01-0267]; PAPIIT [IN216007]; MABOTRO project EMARNAT-CONACYT [2002-C01-0597]; MABOTRO project EP-CONACYT [CB-2005-01-51043]; NWO-WOTRO [W85-326]; [SEP CONACYT-2009-01-128136] FX We are indebted to the people of Nizanda, Oaxaca, and Loma Bonita, Chiapas, for their hospitality and assistance during field work. We thank Jorge Rodriguez-Velazquez and Marco Romero for database management, and Eva van den Elzen, Erik Peters, Paul van Esch, Michiel van Breugel, Elisabeth Schuller, and Peter Hietz for contributing data. M. Lohbeck was supported by a research grant from Wageningen University and Research center. L. Poorter was partly funded by the DiverSus project through the Inter-American Institute for Global Change Research (IAI) CRN 2015, supported by the U.S. NSF (grant GEO-0452325). E. Lebrija-Trejos was supported by CONACYT-SEMARNAT (grant 2002-C01-0267) and PAPIIT (grant IN216007). M. Martinez-Ramos, H. Paz, and A. Tauro were supported by MABOTRO projects SEMARNAT-CONACYT 2002-C01-0597 and SEP-CONACYT CB-2005-01-51043. J. A. Meave, E. A. Perez-Garcia, and I. E. Romero-Perez were supported by SEP CONACYT-2009-01-128136. F. Bongers was supported by NWO-WOTRO grant W85-326. Fieldwork was partly supported by U.S. NSF grant DEB-0639393. NR 47 TC 41 Z9 44 U1 7 U2 112 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 JUN PY 2013 VL 94 IS 6 BP 1211 EP 1216 PG 6 WC Ecology SC Environmental Sciences & Ecology GA 168OG UT WOS:000320714800001 PM 23923479 ER PT J AU Freestone, AL Ruiz, GM Torchin, ME AF Freestone, Amy L. Ruiz, Gregory M. Torchin, Mark E. TI Stronger biotic resistance in tropics relative to temperate zone: effects of predation on marine invasion dynamics SO ECOLOGY LA English DT Article DE biotic resistance; invasion; invertebrates; latitude; marine; predation; temperate; tropics; tunicates ID LATITUDINAL DIVERSITY GRADIENT; PLANT INVASIONS; NORTH-AMERICA; COMMUNITIES; PATTERNS; BIOGEOGRAPHY; PRESSURE; INVASIBILITY; STRENGTH; FORESTS AB Latitudinal patterns of nonnative species richness suggest fewer successful invasions in the tropics, relative to temperate regions. One main hypothesis for this pattern is that biotic resistance to invasion is stronger in the tropics than at higher latitudes. Biotic resistance can limit the distribution and abundance of nonnative species and, in extreme cases, can prevent establishment. We provide the first experimental test of this hypothesis, comparing the strength of biotic resistance in a tropical and a temperate marine ecosystem. Predation is one mechanism of biotic resistance, and since predation can be stronger at lower latitudes, we predicted that predation will serve to increase biotic resistance more in the tropics than at higher latitude. We conducted predator-exclusion experiments on marine epifaunal communities, a heavily invaded system, focusing on nonnative tunicates as a model fauna. The effect of predation on species richness of nonnative tunicates was more than three times greater at sites in tropical Panama than in temperate Connecticut, consistent with the prediction of stronger biotic resistance in the tropics. In Connecticut, predation reduced the abundance of one nonnative tunicate but did not affect the abundances of any other nonnative tunicate species, and no species were excluded from communities. In contrast, predation resulted in striking reductions in abundance and often exclusion of nonnative tunicates from experimental communities in Panama. If proved to be general, latitudinal differences in the biotic resistance of communities to nonnative species establishment may help explain emerging patterns of global invasions. C1 [Freestone, Amy L.] Temple Univ, Dept Biol, Philadelphia, PA 19122 USA. [Freestone, Amy L.; Ruiz, Gregory M.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. [Torchin, Mark E.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. RP Freestone, AL (reprint author), Temple Univ, Dept Biol, Philadelphia, PA 19122 USA. EM amy.freestone@temple.edu OI Ruiz, Gregory/0000-0003-2499-441X FU Smithsonian Institution Marine Science Network FX We thank the Smithsonian Institution Marine Science Network for funding and our colleagues at University of Connecticut and the Smithsonian for field assistance, in particular, R. Osman, R. Whitlatch, C. Schloeder, K. Larson, and G. Ashton. NR 43 TC 19 Z9 19 U1 5 U2 103 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 JUN PY 2013 VL 94 IS 6 BP 1370 EP 1377 PG 8 WC Ecology SC Environmental Sciences & Ecology GA 168OG UT WOS:000320714800022 PM 23923500 ER PT J AU Oftedal, OT Dhouailly, D AF Oftedal, Olav T. Dhouailly, Danielle TI Evo-Devo of the Mammary Gland SO JOURNAL OF MAMMARY GLAND BIOLOGY AND NEOPLASIA LA English DT Review DE Evolution; Mammary gland; Lactation; Signaling; Morphogenesis ID HAIR FOLLICLE MORPHOGENESIS; HORMONE-RELATED PROTEIN; ONE-HALF RULE; BREAST DEVELOPMENT; SIGNALING PATHWAYS; SONIC-HEDGEHOG; RETINOIC ACID; EVOLUTION; SKIN; MOUSE AB We propose a new scenario for mammary evolution based on comparative review of early mammary development among mammals. Mammary development proceeds through homologous phases across taxa, but evolutionary modifications in early development produce different final morphologies. In monotremes, the mammary placode spreads out to form a plate-like mammary bulb from which more than 100 primary sprouts descend into mesenchyme. At their distal ends, secondary sprouts develop, including pilosebaceous anlagen, resulting in a mature structure in which mammary lobules and sebaceous glands empty into the infundibula of hair follicles; these structural triads (mammolobular-pilo-sebaceous units or MPSUs) represent an ancestral condition. In marsupials a flask-like mammary bulb elongates as a sprout, but then hollows out; its secondary sprouts include hair and sebaceous anlagen (MPSUs), but the hairs are shed during nipple formation. In some eutherians (cat, horse, human) MPSUs form at the distal ends of primary sprouts; pilosebaceous components either regress or develop into mature structures. We propose that a preexisting structural triad (the apocrine-pilo-sebaceous unit) was incorporated into the evolving mammary structure, and coupled to additional developmental processes that form the mammary line, placode, bulb and primary sprout. In this scenario only mammary ductal trees and secretory tissue derive from ancestral apocrine-like glands. The mammary gland appears to have coopted signaling pathways and genes for secretory products from even earlier integumentary structures, such as odontode (tooth-like) or odontode-derived structures. We speculate that modifications in signal use (such as PTHrP and BMP4) may contribute to taxonomic differences in MPSU development. C1 [Oftedal, Olav T.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. [Dhouailly, Danielle] Univ Grenoble 1, CNRS, EPHE, UJF,FRE 3405, F-38706 La Tronche, France. RP Oftedal, OT (reprint author), Smithsonian Environm Res Ctr, POB 28, Edgewater, MD 21037 USA. EM oftedalo@si.edu NR 112 TC 7 Z9 7 U1 7 U2 44 PU SPRINGER/PLENUM PUBLISHERS PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 1083-3021 J9 J MAMMARY GLAND BIOL JI J. Mammary Gland Biol. Neoplasia PD JUN PY 2013 VL 18 IS 2 SI SI BP 105 EP 120 DI 10.1007/s10911-013-9290-8 PG 16 WC Oncology; Endocrinology & Metabolism; Physiology SC Oncology; Endocrinology & Metabolism; Physiology GA 170SY UT WOS:000320875100003 PM 23681303 ER PT J AU Launius, RD AF Launius, Roger D. TI Blue Sky Metropolis: The Aerospace Century in Southern California. SO WESTERN HISTORICAL QUARTERLY LA English DT Book Review C1 [Launius, Roger D.] Smithsonian Inst, Natl Air & Space Museum, Washington, DC 20560 USA. RP Launius, RD (reprint author), Smithsonian Inst, Natl Air & Space Museum, Washington, DC 20560 USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU WESTERN HISTORY ASSOC PI LOGAN PA UTAH STATE UNIV, UMC 0740, LOGAN, UT 84322 USA SN 0043-3810 J9 WESTERN HIST QUART JI West. Hist. Q. PD SUM PY 2013 VL 44 IS 2 BP 203 EP 204 PG 2 WC History SC History GA 164PS UT WOS:000320422600014 ER PT J AU Dingwall, HL Hatala, KG Wunderlich, RE Richmond, BG AF Dingwall, Heather L. Hatala, Kevin G. Wunderlich, Roshna E. Richmond, Brian G. TI Hominin stature, body mass, and walking speed estimates based on 1.5 million-year-old fossil footprints at Ileret, Kenya SO JOURNAL OF HUMAN EVOLUTION LA English DT Article DE Bipedalism; Body size; Homo; Human evolution; Pleistocene ID AUSTRALOPITHECUS-AFARENSIS; SEXUAL-DIMORPHISM; HOMO-ERECTUS; SIZE DIMORPHISM; NATURAL-HISTORY; TURKANA BASIN; MODERN HUMANS; FOOT; EVOLUTION; LAETOLI AB The early Pleistocene marks a period of major transition in hominin body form, including increases in body mass and stature relative to earlier hominins. However, because complete postcranial fossils with reliable taxonomic attributions are rare, efforts to estimate hominin mass and stature are complicated by the frequent albeit necessary use of isolated, and often fragmentary, skeletal elements. The recent discovery of 1.52 million year old hominin footprints from multiple horizons in Ileret, Kenya, provides new data on the complete foot size of early Pleistocene hominins as well as stride lengths and other characteristics of their gaits. This study reports the results of controlled experiments with habitually unshod Daasanach adults from Ileret to examine the relationships between stride length and speed, and also those between footprint size, body mass, and stature. Based on significant relationships among these variables, we estimate travel speeds ranging between 0.45 m/s and 2.2 m/s from the fossil hominin footprint trails at Ileret The fossil footprints of seven individuals show evidence of heavy (mean = 50.0 kg; range: 41.5-60.3 kg) and tall individuals (mean = 169.5 cm; range: 152.6-185.8 cm), suggesting that these prints were most likely made by Homo erectus and/or male Paranthropus boisei. The large sizes of these footprints provide strong evidence that hominin body size increased during the early Pleistocene. (C) 2013 Elsevier Ltd. All rights reserved. C1 [Dingwall, Heather L.; Hatala, Kevin G.; Richmond, Brian G.] George Washington Univ, Dept Anthropol, Ctr Adv Study Hominid Paleobiol, Washington, DC 20052 USA. [Hatala, Kevin G.] George Washington Univ, Hominid Paleobiol Doctoral Program, Washington, DC 20052 USA. [Wunderlich, Roshna E.] James Madison Univ, Dept Biol, Harrisonburg, VA 22807 USA. [Richmond, Brian G.] Smithsonian Inst, Natl Museum Amer Hist, Human Origins Program, Washington, DC 20560 USA. RP Dingwall, HL (reprint author), George Washington Univ, Dept Anthropol, Ctr Adv Study Hominid Paleobiol, 2110 G St NW, Washington, DC 20052 USA. EM hdingwall@fas.harvard.edu; kevin.g.hatala@gmail.com; wunderre@jmu.edu; brich@gwu.edu FU National Science Foundation [BCS-1128170, BCS-0924476, DGE-0801634]; George Washington University's Selective Excellence Fund; University Facilitating Fund; George Gamow Undergraduate Research Fellowship; Office of the Vice President for Research Undergraduate Research Fellowship FX We thank David Green, David Braun, Purity Kiura, Emmanuel Ndiema, Jack Harris, the Koobi Fora Field School, the National Museums of Kenya, the people of Ileret, and the Daasanach experimental subjects for their contributions to this project. Additionally, we thank David Hunt, the Smithsonian's National Museum of Natural History, Will Harcourt-Smith, Eileen Westwig, and the American Museum of Natural History for access to skeletal collections. We also thank Bernard Wood and Herman Pontzer for their advice and assistance during the preparation of the manuscript, as well as Mark Teaford, the Associate Editor, and two anonymous reviewers for their helpful comments. Finally, we thank the following funding agencies for supporting this research: National Science Foundation's Biological Anthropology Program (BCS-1128170, -0924476) and Integrative Graduate Education and Research Traineeship Program (DGE-0801634); George Washington University's Selective Excellence Fund, University Facilitating Fund, George Gamow Undergraduate Research Fellowship, Office of the Vice President for Research Undergraduate Research Fellowship. NR 75 TC 19 Z9 19 U1 2 U2 66 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 JUN PY 2013 VL 64 IS 6 BP 556 EP 568 DI 10.1016/j.jhevol.2013.02.004 PG 13 WC Anthropology; Evolutionary Biology SC Anthropology; Evolutionary Biology GA 165KE UT WOS:000320482000006 PM 23522822 ER PT J AU Moratelli, R Wilson, DE AF Moratelli, Ricardo Wilson, Don E. TI Distribution and natural history of Myotis lavali (Chiroptera, Vespertilionidae) SO JOURNAL OF MAMMALOGY LA English DT Article DE bionomy; geographic distribution; Gloger's rule; Myotinae; range extension; South America ID SOUTH-AMERICAN POPULATIONS; MORPHOLOGICAL VARIATION; BATS; PARAGUAY AB LaVal's myotis (Myotis lavali) was recently described from the M. nigricans complex based on specimens from the Caatinga of northeastern Brazil. We present new distributional records for the Alto Chaco in Paraguay and for the Atlantic Forest of Brazil and Paraguay. These new records extend the distribution of the species approximately 2,000 km southwest and 400 km east, and document its co-occurrence with M. nigricans. Both results have taxonomic and ecological implications for M. lavali. Additionally, we provide comments on its natural history and reproduction. C1 [Moratelli, Ricardo] Fundacao Oswaldo Cruz, Pavilhao Olympia Fonseca Filho, BR-22713375 Rio De Janeiro, Brazil. [Wilson, Don E.] Smithsonian Inst, Natl Museum Nat Hist, Div Mammals, Washington, DC 20013 USA. RP Moratelli, R (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Div Mammals, Washington, DC 20013 USA. EM rmoratelli@fiocruz.br RI Rocha, Ricardo/A-5735-2013 OI Rocha, Ricardo/0000-0003-0942-6633 FU Conselho Nacional de Desenvolvimento Cientifico e Tecnologico, Brazil [CNPq 202612/2011-2] FX The following curators and collection staff provided access to specimens under their care: A. L. Peracchi (Universidade Federal Rural do Rio de Janeiro, Brazil); F. de C. Passos (Universidade Federal do Parana, Brazil); M. de Vivo and J. G. Barros (Museu de Zoologia da Universidade de Sao Paulo, Brazil); N. Simmons and E. Westwig (American Museum of Natural History, United States); and K. Helgen, D. Lunde, and L. Gordon (National Museum of Natural History, United States). A. L. Gardner (United States Geological Survey Patuxent Wildlife Research Center, United States) provided information on specimens he collected in northeastern Brazil. R. Gregorin (Universidade Federal de Lavras, Brazil) and R. L. M. Novaes (Universidade Federal do Estado do Rio de Janeiro, Brazil) provided photographs of specimens from Tocantins and Pernambuco, respectively. L. A. M. da Silva (Universidade Federal de Pernambuco, Brazil) provided photographs of the Caatinga of Pernambuco where specimens of M. lavali were captured. M. A. Mares and an anonymous reviewer provided comments that improved the manuscript. This work was partially supported by Conselho Nacional de Desenvolvimento Cientifico e Tecnologico, Brazil (CNPq 202612/2011-2). NR 42 TC 2 Z9 3 U1 3 U2 21 PU OXFORD UNIV PRESS INC PI CARY PA JOURNALS DEPT, 2001 EVANS RD, CARY, NC 27513 USA SN 0022-2372 EI 1545-1542 J9 J MAMMAL JI J. Mammal. PD JUN PY 2013 VL 94 IS 3 BP 650 EP 656 DI 10.1644/12-MAMM-A-257.1 PG 7 WC Zoology SC Zoology GA 165JF UT WOS:000320479100012 ER PT J AU Karmacharya, B Hostetler, JA Conner, LM Morris, G Oli, MK AF Karmacharya, Binab Hostetler, Jeffrey A. Conner, L. Mike Morris, Gail Oli, Madan K. TI The influence of mammalian predator exclusion, food supplementation, and prescribed fire on survival of Glaucomys volans SO JOURNAL OF MAMMALOGY LA English DT Article DE arboreal small mammal; capture-mark-recapture (CMR); capture probability; demography; Glaucomys volans; mammalian predator exclusion; prescribed fire; supplemental food; survival rate ID SOUTHERN FLYING SQUIRRELS; RED-COCKADED WOODPECKERS; POPULATION-GROWTH RATE; TAMIASCIURUS-HUDSONICUS; NORTHERN; HABITAT; SUCCESS; SIZE; REPRODUCTION; LIMITATION AB Little is known about demographic parameters of the southern flying squirrel (Glaucomys volans) or the factors influencing those parameters. We conducted capture-mark-recapture studies from January 2005 to September 2009, and from May to November 2010 to provide rigorous estimates of survival rates for the southern flying squirrel in a longleaf pine ecosystem. We also examined the effect of experimental food supplementation, prescribed fire, and mammalian predator exclusion on survival rates. Monthly apparent survival rates estimated from the 2 studies were 0.85 +/- 0.01 SE and 0.81 +/- 0.04, respectively. Prescribed fire positively influenced survival; survival increased for a period up to 9 months after burns. Evidence that food supplementation and mammalian predator exclusion substantially affected survival rates was weak. These results suggest that the southern flying squirrel population in our study site during the study period was not food-limited, and that mortality due to mammalian predators is insubstantial. However, we do not know if any reduction in mortality due to mammalian predator exclusion could have been compensated for by an increase in mortality due to predation by raptors and snakes. C1 [Karmacharya, Binab; Oli, Madan K.] Univ Florida, Dept Wildlife Ecol & Conservat, Gainesville, FL 32611 USA. [Hostetler, Jeffrey A.] Natl Zool Pk, Smithsonian Conservat Biol Inst, Migratory Bird Ctr, Washington, DC 20013 USA. [Conner, L. Mike; Morris, Gail] Joseph W Tones Ecol Res Ctr, Newton, GA 39870 USA. RP Conner, LM (reprint author), Joseph W Tones Ecol Res Ctr, 3988 Tones Ctr Dr, Newton, GA 39870 USA. EM mconner@jonesctr.org RI Hostetler, Jeffrey/A-3345-2011 OI Hostetler, Jeffrey/0000-0003-3669-1758 FU Jones Ecological Research Center; Department of Wildlife Ecology and Conservation, University of Florida; United States Foreign Fulbright Program Division FX We thank J. Rutledge for assistance with fieldwork and logistic arrangements and many technicians who contributed to the collection of data. Our warmest thanks are extended to M. Simmons, who worked diligently to manage our database. Prescribed burns were executed by J. Atkinson, S. Smith, C. Eddins, and B. Williamson. Fieldwork was funded by the Jones Ecological Research Center, and the graduate program for BK was supported by the Department of Wildlife Ecology and Conservation, University of Florida, and the United States Foreign Fulbright Program Division. NR 64 TC 1 Z9 1 U1 3 U2 41 PU OXFORD UNIV PRESS INC PI CARY PA JOURNALS DEPT, 2001 EVANS RD, CARY, NC 27513 USA SN 0022-2372 EI 1545-1542 J9 J MAMMAL JI J. Mammal. PD JUN PY 2013 VL 94 IS 3 BP 672 EP 682 DI 10.1644/12-MAMM-A-071.1 PG 11 WC Zoology SC Zoology GA 165JF UT WOS:000320479100015 ER PT J AU Muhs, DR Ruskin, J Tsoar, H Skipp, G Budahn, JR Sneh, A Porat, N Stanley, JD Katra, I Blumberg, DG AF Muhs, Daniel R. Ruskin, Joel Tsoar, Haim Skipp, Gary Budahn, James. R. Sneh, Amihai Porat, Naomi Stanley, Jean-Daniel Katra, Itzhak Blumberg, Dan G. TI Origin of the Sinai-Negev erg, Egypt and Israel: mineralogical and geochemical evidence for the importance of the Nile and sea level history SO QUATERNARY SCIENCE REVIEWS LA English DT Article DE Sinai-Negev erg; Dunes; Aeolian; Mineralogy; Geochemistry; Mineralogical maturity; Nile; Sea level; Holocene; Pleistocene; Israel; Egypt ID RUB AL-KHALI; SULTANATE-OF-OMAN; SIZED QUARTZ SILT; SAND DUNES; COASTAL-PLAIN; LATE PLEISTOCENE; SEDIMENT TRANSPORT; LOESS DEPOSITS; DESERT LOESS; LABORATORY SIMULATIONS AB The Sinai-Negev erg occupies an area of 13,000 km(2) in the deserts of Egypt and Israel. Aeolian sand of this erg has been proposed to be derived from the Nile Delta, but empirical data supporting this view are lacking. An alternative source sediment is sand from the large Wadi El Arish drainage system in central and northern Sinai. Mineralogy of the Negev and Sinai dunes shows that they are high in quartz, with much smaller amounts of K-feldspar and plagioclase. Both Nile Delta sands and Sinai wadi sands, upstream of the dunes, also have high amounts of quartz relative to K-feldspar and plagioclase. However, Sinai wadi sands have abundant calcite, whereas Nile Delta sands have little or no calcite. Overall, the mineralogical data suggest that the dunes are derived dominantly from the Nile Delta, with Sinai wadi sands being a minor contributor. Geochemical data that proxy for both the light mineral fraction (SiO2/10-Al2O3 + Na2O + K2O-CaO) and heavy mineral fraction (Fe2O3-MgO-TiO2) also indicate a dominant Nile Delta source for the dunes. Thus, we report here the first empirical evidence that the Sinai-Negev dunes are derived dominantly from the Nile Delta. Linkage of the Sinai-Negev erg to the Nile Delta as a source is consistent with the distribution of OSL ages of Negev dunes in recent studies. Stratigraphic studies show that during the Last Glacial period, when dune incursions in the Sinai-Negev erg began, what is now the Nile Delta area was characterized by a broad, sandy, minimally vegetated plain, with seasonally dry anastomosing channels. Such conditions were ideal for providing a ready source of sand for aeolian transport under what were probably much stronger glacial-age winds. With the post-glacial rise in sea level, the Nile River began to aggrade. Post-glacial sedimentation has been dominated by fine-grained silts and clays. Thus, sea level, along with favorable climatic conditions, emerges as a major influence on the timing of dune activity in the Sinai-Negev erg, through its control on the supply of sand from the Nile Delta. The mineralogy of the Sinai-Negev dunes is also consistent with a proposed hypothesis that these sediments are an important source of loess in Israel. Published by Elsevier Ltd. C1 [Muhs, Daniel R.; Skipp, Gary; Budahn, James. R.] US Geol Survey, Fed Ctr, Denver, CO 80225 USA. [Ruskin, Joel; Tsoar, Haim; Katra, Itzhak; Blumberg, Dan G.] Ben Gurion Univ Negev, Dept Geog & Environm Dev, IL-84105 Beer Sheva, Israel. [Sneh, Amihai; Porat, Naomi] Geol Survey Israel, IL-95501 Jerusalem, Israel. [Stanley, Jean-Daniel] Smithsonian Inst, Geoarchaeol Paleobiol Dept, Washington, DC 20013 USA. RP Muhs, DR (reprint author), US Geol Survey, Fed Ctr, MS 980,Box 25046, Denver, CO 80225 USA. EM dmuhs@usgs.gov RI BLUMBERG, DAN/F-1285-2012 OI BLUMBERG, DAN/0000-0001-9337-1617 FU United States-Israel Binational Science Foundation (Jerusalem); U.S. Geological Survey's Climate and Land Use Change Program FX This study was supported by the United States-Israel Binational Science Foundation (Jerusalem) and the U.S. Geological Survey's Climate and Land Use Change Program. We appreciate the efforts of Kristi Zellman and DeAnna Laurel of the USGS for their able assistance in the laboratory. We thank Dr. Amir Sandler for providing his XRD calibration method. Two anonymous reviewers and Jeff Pigati, Janet Slate, Tom Judkins, and Gene Ellis (U.S. Geological Survey) read an earlier version of this manuscript and made helpful comments for its improvement. NR 104 TC 18 Z9 19 U1 1 U2 16 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0277-3791 J9 QUATERNARY SCI REV JI Quat. Sci. Rev. PD JUN 1 PY 2013 VL 69 BP 28 EP 48 DI 10.1016/j.quascirev.2013.02.022 PG 21 WC Geography, Physical; Geosciences, Multidisciplinary SC Physical Geography; Geology GA 165LG UT WOS:000320484800003 ER PT J AU Gardullo, P AF Gardullo, Paul TI Spectacles of Slavery: Pageantry, Film and Early Twentieth-Century Public Memory SO SLAVERY & ABOLITION LA English DT Article AB Arguing that the early decades of the twentieth century represent a moment in which the flesh and blood memory of slavery was fading while the cultural contest over the meanings of slavery and race were increasingly in flux, Gardullo compares and analyses two key visual texts of the period. He sets in contrast the Star of Ethiopia, an early historical pageant conceived by W.E.B. Du Bois and D.W. Griffith's film The Birth of a Nation, presenting the pair as twinned and warring spectacles which attempted to advance a particular version of American history and the slave past to large portions of the American public. C1 Smithsonian Inst, Natl Museum African Amer Hist & Culture, Washington, DC 20560 USA. RP Gardullo, P (reprint author), Smithsonian Inst, Natl Museum African Amer Hist & Culture, Capital Gallery 7001 MRC 509, Washington, DC 20560 USA. EM gardullop@si.edu NR 22 TC 0 Z9 0 U1 0 U2 0 PU ROUTLEDGE JOURNALS, TAYLOR & FRANCIS LTD PI ABINGDON PA 4 PARK SQUARE, MILTON PARK, ABINGDON OX14 4RN, OXFORDSHIRE, ENGLAND SN 0144-039X J9 SLAVERY ABOLIT JI Slavery Abolit. PD JUN 1 PY 2013 VL 34 IS 2 SI SI BP 222 EP 235 DI 10.1080/0144039X.2013.791174 PG 14 WC History SC History GA 159XQ UT WOS:000320081000003 ER PT J AU Laliberte, E Grace, JB Huston, MA Lambers, H Teste, FP Turner, BL Wardle, DA AF Laliberte, Etienne Grace, James B. Huston, Michael A. Lambers, Hans Teste, Francois P. Turner, Benjamin L. Wardle, David A. TI How does pedogenesis drive plant diversity? SO TRENDS IN ECOLOGY & EVOLUTION LA English DT Article ID LONG-TERM CHRONOSEQUENCES; TEMPERATE RAIN-FOREST; ECOSYSTEM RETROGRESSION; COMMUNITY STRUCTURE; SPECIES-DIVERSITY; SOIL DEVELOPMENT; TERRESTRIAL ECOSYSTEMS; PRIMARY PRODUCTIVITY; NUTRIENT LIMITATION; WESTERN-AUSTRALIA AB Some of the most species-rich plant communities occur on ancient, strongly weathered soils, whereas those on recently developed soils tend to be less diverse. Mechanisms underlying this well-known pattern, however, remain unresolved. Here, we present a conceptual model describing alternative mechanisms by which pedogenesis (the process of soil formation) might drive plant diversity. We suggest that long-term soil chronosequences offer great, yet largely untapped, potential as 'natural experiments' to determine edaphic controls over plant diversity. Finally, we discuss how our conceptual model can be evaluated quantitatively using structural equation modeling to advance multivariate theories about the determinants of local plant diversity. This should help us to understand broader-scale diversity patterns, such as the latitudinal gradient of plant diversity. C1 [Laliberte, Etienne; Lambers, Hans; Teste, Francois P.] Univ Western Australia, Sch Plant Biol, Crawley, WA 6009, Australia. [Grace, James B.] US Geol Survey, Natl Wetlands Res Ctr, Lafayette, LA 70506 USA. [Huston, Michael A.] Texas State Univ, Dept Biol, San Marcos, TX 78666 USA. [Turner, Benjamin L.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. [Wardle, David A.] Swedish Univ Agr Sci, Dept Forest Ecol & Management, Fac Forestry, SE-90183 Umea, Sweden. RP Laliberte, E (reprint author), Univ Western Australia, Sch Plant Biol, 35 Stirling Highway, Crawley, WA 6009, Australia. EM etienne.laliberte@uwa.edu.au RI Turner, Benjamin/E-5940-2011; Laliberte, Etienne/B-6855-2008; Huston, Michael/B-1434-2009; Wardle, David/F-6031-2011; Lambers, Hans/A-1544-2008 OI Turner, Benjamin/0000-0002-6585-0722; Laliberte, Etienne/0000-0002-3167-2622; Huston, Michael/0000-0001-9513-1166; Wardle, David/0000-0002-0476-7335; Lambers, Hans/0000-0002-4118-2272 FU UWA; School of Plant Biology; Faculty of Natural and Agricultural Sciences; DECRA from the Australian Research Council [DE120100352]; NSF OPUS [0918927]; ARC; Wallenberg Scholars award FX This paper originated from a research workshop held at The University of Western Australia (UWA) on 20-25 February, 2012. Funding for this workshop was provided by UWA, specifically by the School of Plant Biology (40%), the Pro Vice-Chancellor (Research) (40%), and the Faculty of Natural and Agricultural Sciences (20%). We thank G. Zemunik for providing data and photos, and A. Wells for photos. E.L. was supported by a DECRA (DE120100352) from the Australian Research Council. M.A.H. was supported by NSF OPUS Grant 0918927. H.L. and F.T. were supported by an ARC Discovery grant. D.A.W. was supported by a Wallenberg Scholars award. NR 70 TC 43 Z9 45 U1 9 U2 161 PU ELSEVIER SCIENCE LONDON PI LONDON PA 84 THEOBALDS RD, LONDON WC1X 8RR, ENGLAND SN 0169-5347 J9 TRENDS ECOL EVOL JI Trends Ecol. Evol. PD JUN PY 2013 VL 28 IS 6 BP 331 EP 340 DI 10.1016/j.tree.2013.02.008 PG 10 WC Ecology; Evolutionary Biology; Genetics & Heredity SC Environmental Sciences & Ecology; Evolutionary Biology; Genetics & Heredity GA 168YA UT WOS:000320742700008 PM 23561322 ER PT J AU Britt, CT Torres, MAP Hynes, RI Jonker, PG Maccarone, TJ Greiss, S Steeghs, D Groot, P Knigge, C Dieball, A Nelemans, G Mikles, VJ Gossen, L AF Britt, C. T. Torres, M. A. P. Hynes, R. I. Jonker, P. G. Maccarone, T. J. Greiss, S. Steeghs, D. Groot, P. Knigge, C. Dieball, A. Nelemans, G. Mikles, V. J. Gossen, L. TI IDENTIFICATION OF FIVE INTERACTING BINARIES IN THE GALACTIC BULGE SURVEY SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries: close; novae, cataclysmic variables; stars: dwarf novae; stars: emission-line, Be; surveys; X-rays: binaries ID X-RAY SOURCES; HOLE EVENT HORIZONS; BLACK-HOLE; CATACLYSMIC VARIABLES; IMAGE SUBTRACTION; GLOBULAR-CLUSTERS; LOW-MASS; ACCRETION; STARS; TRANSIENTS AB We present optical light curves, spectroscopy, and classification of five X-ray sources in the Chandra Galactic Bulge Survey (CXOGBS J174009.1-284725 (CX5), CXOGBS J173935.7-272935 (CX18), CXOGBS J173946.9-271809 (CX28), CXOGBS J173729.1-292804 (CX37), CXOGBS J174607.6-261547 (CX561)). These objects were selected based on bright optical counterparts which were quickly found to have emission lines in their optical spectra. This paper presents an illustration of GBS optical follow-up, targeting emission line objects. Of these five objects, four exhibit photometric variability in the Sloan r' band. CX5 shows a tentative period of 2.1 hr and is clearly an intermediate polar (IP). CX28 and CX37 both exhibit flickering with no clear period. Both are also suggested to be IPs. CX18 was observed to undergo two dwarf nova outbursts. Finally, CX561 shows no detectable variability, although its characteristics would be consistent with either a quiescent low-mass X-ray binary or cataclysmic variable. C1 [Britt, C. T.; Hynes, R. I.; Mikles, V. J.; Gossen, L.] Louisiana State Univ, Dept Phys & Astron, Baton Rouge, LA 70803 USA. [Torres, M. A. P.; Jonker, P. G.] SRON Netherlands Inst Space Res, SRON, NL-3584 CA Utrecht, Netherlands. [Torres, M. A. P.; Jonker, P. G.; Steeghs, D.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Jonker, P. G.; Groot, P.; Nelemans, G.] Radboud Univ Nijmegen, Dept Astrophys IMAPP, NL-6500 GL Nijmegen, Netherlands. [Maccarone, T. J.; Knigge, C.; Dieball, A.] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England. [Greiss, S.; Steeghs, D.] Univ Warwick, Dept Phys, Coventry CV4 7AL, W Midlands, England. [Groot, P.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA. RP Jonker, PG (reprint author), Louisiana State Univ, Dept Phys & Astron, Baton Rouge, LA 70803 USA. RI Steeghs, Danny/C-5468-2009; Nelemans, Gijs/D-3177-2012; Groot, Paul/K-4391-2016 OI Steeghs, Danny/0000-0003-0771-4746; Nelemans, Gijs/0000-0002-0752-2974; Groot, Paul/0000-0002-4488-726X FU National Science Foundation [AST-0908789]; Louisiana Board of Regents; NAS/Louisiana Board of Regents [NNX07AT62A/LEQSF]; Netherlands Organisation for Scientific Research FX This work was supported by the National Science Foundation under grant No. AST-0908789, by the Louisiana Board of Regents Fellowship, by the NAS/Louisiana Board of Regents grant NNX07AT62A/LEQSF(2007-2010) Phase 3-02. P.G.J. and M. A. P. T. acknowledge support from the Netherlands Organisation for Scientific Research, and the work of their student Oliwia Madj. This research has made use of NASA's Astrophysics Data System Bibliographic Services and of SAOImage DS9, developed by Smithsonian Astrophysical Observatory. NR 49 TC 9 Z9 9 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 JUN 1 PY 2013 VL 769 IS 2 AR UNSP 120 DI 10.1088/0004-637X/769/2/120 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 158UM UT WOS:000319999100036 ER PT J AU Garcia, EV Stassun, KG Torres, G AF Garcia, E. V. Stassun, Keivan G. Torres, Guillermo TI REANALYSIS OF THE RADII OF THE BENCHMARK ECLIPSING BINARY V578 Mon SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries: close; binaries: eclipsing; stars: early-type; stars: massive ID DISENTANGLED COMPONENT SPECTRA; CURVES; LIGHT AB V578 Mon is an eclipsing binary system in which both stars have masses above 10 M-circle dot determined with an accuracy better than 3%. It is one of only five such massive eclipsing binaries known that also possess eccentric orbits and measured apsidal motions, thus making it an important benchmark for theoretical stellar evolution models. However, recently reported determinations of the radii of V578 Mon differ significantly from previously reported values. We reanalyze the published data for V578 Mon and trace the discrepancy to the use of an incorrect formulation for the stellar potentials in the most recent analysis. Here we report corrected radii for this important benchmark eclipsing binary. C1 [Garcia, E. V.; Stassun, Keivan G.] Vanderbilt Univ, Dept Phys & Astron, Nashville, TN 37235 USA. [Torres, Guillermo] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Garcia, EV (reprint author), Vanderbilt Univ, Dept Phys & Astron, VU Stn B 1807, Nashville, TN 37235 USA. EM eugenio.v.garcia@gmail.com NR 7 TC 1 Z9 1 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUN 1 PY 2013 VL 769 IS 2 AR 114 DI 10.1088/0004-637X/769/2/114 PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 158UM UT WOS:000319999100030 ER PT J AU Hwang, HS Geller, MJ AF Hwang, Ho Seong Geller, Margaret J. TI DUST-OBSCURED GALAXIES IN THE LOCAL UNIVERSE SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: active; galaxies: evolution; galaxies: formation; galaxies: starburst; infrared: galaxies; surveys ID SIMILAR-TO 2; ULTRALUMINOUS INFRARED GALAXIES; ACTIVE GALACTIC NUCLEI; SPECTRAL ENERGY-DISTRIBUTIONS; STAR-FORMING GALAXIES; DIGITAL SKY SURVEY; MU-M OBSERVATIONS; SUBMILLIMETER-SELECTED GALAXIES; SPACE-TELESCOPE MORPHOLOGIES; EXTRAGALACTIC LEGACY SURVEY AB We use Wide-field Infrared Survey Explorer (WISE), AKARI, and Galaxy Evolution Explorer (GALEX) data to select local analogs of high-redshift (z similar to 2) dust obscured galaxies (DOGs). We identify 47 local DOGs with S-12 mu m/S-0.22 mu m >= 892 and S-12 mu m > 20 mJy at 0.05 < z < 0.08 in the Sloan Digital Sky Survey data release 7. The infrared (IR) luminosities of these DOGs are in the range 3.4 x 10(10) (L-circle dot) less than or similar to L-IR less than or similar to 7.0 x 10(11) (L-circle dot) with a median L-IR of 2.1x10(11) (L-circle dot). We compare the physical properties of local DOGs with a control sample of galaxies that have lower S-12 mu m/S-0.22 mu m but have similar redshift, IR luminosity, and stellar mass distributions. Both WISE 12 mu m and GALEX near-ultraviolet (NUV) flux densities of DOGs differ from the control sample of galaxies, but the difference is much larger in the NUV. Among the 47 DOGs, 36% +/- 7% have small axis ratios in the optical (i.e., b/a < 0.6), larger than the fraction among the control sample (17% +/- 3%). There is no obvious sign of interaction for many local DOGs. No local DOGs have companions with comparable optical magnitudes closer than similar to 50 kpc. The large-and small-scale environments of DOGs are similar to the control sample. Many physical properties of local DOGs are similar to those of high-z DOGs, even though the IR luminosities of local objects are an order of magnitude lower than for the high-z objects: the presence of two classes (active galactic nuclei-and star formation-dominated) of DOGs, abnormal faintness in the UV rather than extreme brightness in the mid-IR, and diverse optical morphology. These results suggest a common underlying physical origin of local and high-z DOGs. Both seem to represent the high-end tail of the dust obscuration distribution resulting from various physical mechanisms rather than a unique phase of galaxy evolution. C1 [Hwang, Ho Seong; Geller, Margaret J.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Hwang, HS (reprint author), Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA. EM hhwang@cfa.harvard.edu; mgeller@cfa.harvard.edu FU Smithsonian Institution; National Aeronautics and Space Administration; Alfred P. Sloan Foundation; National Science Foundation; U. S. Department of Energy; Japanese Monbukagakusho; Max Planck Society; Higher Education Funding Council for England; American Museum of Natural History; Astrophysical Institute Potsdam; University of Basel; Cambridge University; Case Western Reserve University; University of Chicago; Drexel University; Fermilab; Institute for Advanced Study; Japan Participation Group; Johns Hopkins University; Joint Institute for Nuclear Astrophysics; Kavli Institute for Particle Astrophysics and Cosmology; Korean Scientist Group; Chinese Academy of Sciences (LAMOST); Los Alamos National Laboratory; Max-Planck-Institute for Astronomy (MPIA); Max-Planck-Institute for Astrophysics (MPA); New Mexico State University; Ohio State University; University of Pittsburgh; University of Portsmouth; Princeton University; United States Naval Observatory; University of Washington FX We thank the anonymous referee for many insightful comments that improved the manuscript. H. S. H. acknowledges the Smithsonian Institution for the support of his post-doctoral fellowship. The Smithsonian Institution also supports the research of M.J.G. This publication makes use of data products from the Wide-field Infrared Survey Explorer, which is a joint project of the University of California, Los Angeles, and the Jet Propulsion Laboratory/California Institute of Technology, funded by the National Aeronautics and Space Administration. This research is based on observations with AKARI, a JAXA project with the participation of ESA. 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. The Participating Institutions are the American Museum of Natural History, Astrophysical Institute Potsdam, University of Basel, Cambridge University, Case Western Reserve University, University of Chicago, Drexel University, Fermilab, the Institute for Advanced Study, the Japan Participation Group, Johns Hopkins University, the Joint Institute for Nuclear Astrophysics, the Kavli Institute for Particle Astrophysics and Cosmology, the Korean Scientist Group, the Chinese Academy of Sciences (LAMOST), Los Alamos National Laboratory, the Max-Planck-Institute for Astronomy (MPIA), the Max-Planck-Institute for Astrophysics (MPA), New Mexico State University, Ohio State University, University of Pittsburgh, University of Portsmouth, Princeton University, the United States Naval Observatory, and the University of Washington. 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 107 TC 5 Z9 5 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 JUN 1 PY 2013 VL 769 IS 2 AR UNSP 116 DI 10.1088/0004-637X/769/2/116 PG 21 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 158UM UT WOS:000319999100032 ER PT J AU Kim, KH Watson, DM Manoj, P Forrest, WJ Najita, J Furlan, E Sargent, B Espaillat, C Muzerolle, J Megeath, ST Calvet, N Green, JD Arnold, L AF Kim, K. H. Watson, Dan M. Manoj, P. Forrest, W. J. Najita, Joan Furlan, Elise Sargent, Benjamin Espaillat, Catherine Muzerolle, James Megeath, S. T. Calvet, Nuria Green, Joel D. Arnold, Laura TI TRANSITIONAL DISKS AND THEIR ORIGINS: AN INFRARED SPECTROSCOPIC SURVEY OF ORION A SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; infrared: stars; protoplanetary disks; stars: pre-main sequence; X-rays: stars ID T-TAURI STARS; SPITZER-SPACE-TELESCOPE; YOUNG STELLAR OBJECTS; SPECTRAL ENERGY-DISTRIBUTIONS; CIRCUMSTELLAR DUST DISKS; MAIN-SEQUENCE EVOLUTION; NEWTON EXTENDED SURVEY; X-RAY-RADIATION; PROTOPLANETARY DISKS; MOLECULAR CLOUD AB Transitional disks are protoplanetary disks around young stars, with inner holes or gaps which are surrounded by optically thick outer, and often inner, disks. Here we present observations of 62 new transitional disks in the Orion A star-forming region. These were identified using the Spitzer Space Telescope's Infrared Spectrograph and followed up with determinations of stellar and accretion parameters using the Infrared Telescope Facility's SpeX. We combine these new observations with our previous results on transitional disks in Taurus, Chamaeleon I, Ophiuchus, and Perseus, and with archival X-ray observations. This produces a sample of 105 transitional disks of "cluster" age 3 Myr or less, by far the largest hitherto assembled. We use this sample to search for trends between the radial structure in the disks and many other system properties, in order to place constraints on the possible origins of transitional disks. We see a clear progression of host-star accretion rate and the different disk morphologies. We confirm that transitional disks with complete central clearings have median accretion rates an order of magnitude smaller than radially continuous disks of the same population. Pre-transitional disks-those objects with gaps that separate inner and outer disks-have median accretion rates intermediate between the two. Our results from the search for statistically significant trends, especially related to (M) over dot, strongly support that in both cases the gaps are far more likely to be due to the gravitational influence of Jovian planets or brown dwarfs orbiting within the gaps, than to any of the photoevaporative, turbulent, or grain-growth processes that can lead to disk dissipation. We also find that the fraction of Class II YSOs which are transitional disks is large, 0.1-0.2, especially in the youngest associations. C1 [Kim, K. H.; Watson, Dan M.; Manoj, P.; Forrest, W. J.; Arnold, Laura] Univ Rochester, Dept Phys & Astron, Rochester, NY 14627 USA. [Najita, Joan; Furlan, Elise] Natl Opt Astron Observ, Tucson, AZ 85719 USA. [Sargent, Benjamin] Rochester Inst Technol, Ctr Imaging Sci, Rochester, NY 14623 USA. [Sargent, Benjamin] Rochester Inst Technol, Lab Multiwavelength Astrophys, Rochester, NY 14623 USA. [Espaillat, Catherine] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Muzerolle, James] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Megeath, S. T.] Univ Toledo, Dept Phys & Astron, Toledo, OH 43606 USA. [Calvet, Nuria] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Green, Joel D.] Univ Texas Austin, Dept Astron, Univ Stn 1, Austin, TX 78712 USA. [Arnold, Laura] SUNY Coll Brockport, Brockport, NY 14420 USA. RP Kim, KH (reprint author), Univ Rochester, Dept Phys & Astron, Rochester, NY 14627 USA. EM khkim@pas.rochester.edu OI Furlan, Elise/0000-0001-9800-6248 FU National Aeronautics and Space Administration; National Science Foundation; NASA [1407, 1257184, NNX08AH94G]; JPL/Caltech; Cornell [31419-5714] FX 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 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 Contract Number 1257184 issued by JPL/Caltech, and Cornell subcontracts 31419-5714 to the University of Rochester. N.C. acknowledges support from NASA Origins grant NNX08AH94G. C. E. was supported by a Sagan Exoplanet Fellowship from the National Aeronautics and Space Administration and administered by the NASA Exoplanet Science Institute (NExScI). NR 138 TC 29 Z9 29 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 JUN 1 PY 2013 VL 769 IS 2 AR UNSP 149 DI 10.1088/0004-637X/769/2/149 PG 40 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 158UM UT WOS:000319999100065 ER PT J AU Nicastro, F Elvis, M Krongold, Y Mathur, S Gupta, A Danforth, C Barcons, X Borgani, S Branchini, E Cen, R Dave, R Kaastra, J Paerels, F Piro, L Shull, JM Takei, Y Zappacosta, L AF Nicastro, F. Elvis, M. Krongold, Y. Mathur, S. Gupta, A. Danforth, C. Barcons, X. Borgani, S. Branchini, E. Cen, R. Dave, R. Kaastra, J. Paerels, F. Piro, L. Shull, J. M. Takei, Y. Zappacosta, L. TI CHANDRA VIEW OF THE WARM-HOT INTERGALACTIC MEDIUM TOWARD 1ES 1553+113: ABSORPTION-LINE DETECTIONS AND IDENTIFICATIONS. I. SO ASTROPHYSICAL JOURNAL LA English DT Article DE atomic processes; intergalactic medium; line: identification; opacity; X-rays: general ID X-RAY-ABSORPTION; PROBE WMAP OBSERVATIONS; XMM-NEWTON; OF-SIGHT; GRATING SPECTROMETER; INTERSTELLAR-MEDIUM; MISSING BARYONS; SCULPTOR WALL; ALPHA FOREST; LOW-REDSHIFT AB We present the first results from our pilot 500 ks Chandra Low Energy Transmission Grating Large Program observation of the soft X-ray brightest source in the z greater than or similar to 0.4 sky, the blazar 1ES 1553+113, aimed to secure the first uncontroversial detections of the missing baryons in the X-rays. We identify a total of 11 possible absorption lines, with single-line statistical significances between 2.2 sigma and 4.1 sigma. Six of these lines are detected at high single-line statistical significance (3.6 <= sigma <= 4.1), while the remaining five are regarded as marginal detections in association with either other X-ray lines detected at higher significance and/or far-ultraviolet (FUV) signposts. Three of these lines are consistent with metal absorption at z similar or equal to 0, and we identify them with Galactic OI and CII. The remaining eight lines may be imprinted by intervening absorbers and are all consistent with being high-ionization counterparts of FUV Hi and/or OVI intergalactic medium signposts. In particular, five of these eight possible intervening absorption lines (single-line statistical significances of 4.1 sigma, 4.1 sigma, 3.9 sigma, 3.8 sigma, and 2.7 sigma), are identified as Cv and C vi K sigma absorbers belonging to three WHIM systems at z(X) = 0.312, z(X) = 0.237, and < z(X)> = 0.133, which also produce broad Hi (and OVI for the z(X) = 0.312 system) absorption in the FUV. For two of these systems (z(X) = 0.312 and 0.237), the Chandra X-ray data led the a posteriori discovery of physically consistent broad Hi associations in the FUV (for the third system the opposite applies), so confirming the power of the X-ray-FUV synergy for WHIM studies. The true statistical significances of these three X-ray absorption systems, after properly accounting for the number of redshift trials, are 5.8 sigma (z(X) = 0.312; 6.3 sigma if the low-significance OV and CV K beta associations are considered), 3.9 sigma (z(X) = 0.237), and 3.8 sigma (< z(X)> = 0.133), respectively. C1 [Nicastro, F.; Zappacosta, L.] Osservatorio Astron Roma INAF, I-00040 Monte Porzio Catone, Italy. [Nicastro, F.; Elvis, M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Krongold, Y.] Univ Nacl Autonoma Mexico, Inst Astron, Mexico City 04510, DF, Mexico. [Mathur, S.; Gupta, A.] Ohio State Univ, Columbus, OH 43210 USA. [Danforth, C.; Shull, J. M.] Univ Colorado, Dept Astrophys & Planetary Sci, CASA, Boulder, CO 80309 USA. [Barcons, X.] Inst Fis Cantabria CSIC UC, E-39005 Santander, Spain. [Borgani, S.] Univ Trieste, Dipartimento Astron, I-34131 Trieste, Italy. [Borgani, S.] INAF Osservatorio Astron Trieste, I-34131 Trieste, Italy. [Branchini, E.] Univ Roma Tre, Dipartimento Fis E Amaldi, I-00146 Rome, Italy. [Cen, R.] Princeton Univ Observ, Princeton, NJ 08544 USA. [Dave, R.] Univ Arizona, Dept Astron, Tucson, AZ 85721 USA. [Kaastra, J.] SRON Netherlands Inst Space Res, NL-3584 CA Utrecht, Netherlands. [Paerels, F.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA. [Paerels, F.] Columbia Univ, Dept Astron, New York, NY 10027 USA. [Piro, L.] INAF IAPS, I-00133 Rome, Italy. [Takei, Y.] Japan Aerosp Explorat Agcy, Inst Space & Astronaut Sci, Chuo Ku, Sagamihara, Kanagawa 2525210, Japan. RP Nicastro, F (reprint author), Osservatorio Astron Roma INAF, Via Frascati 33, I-00040 Monte Porzio Catone, Italy. RI PIRO, LUIGI/E-4954-2013; Barcons, Xavier/L-3335-2014; OI PIRO, LUIGI/0000-0003-4159-3984; Branchini, Enzo/0000-0002-0808-6908; Borgani, Stefano/0000-0001-6151-6439; Barcons, Xavier/0000-0003-1081-8861; Nicastro, Fabrizio/0000-0002-6896-1364 FU Chandra Grant [GO1-12174X]; INAF-ASI ADAE [1.05.04.13.15]; COS [NNX08AC14G]; NASA; Spanish Ministry of Economy and Competitiveness [AYA2010-21490-C02-01] FX We thank Ehud Behar for providing wavelength, oscillator strengths, and transition probabilities of inner shell transitions of C, O, and Ne. F.N. acknowledges support from Chandra Grant GO1-12174X, and from INAF-ASI ADAE Grant 1.05.04.13.15. M. S. and C. D. acknowledge support from COS Grant NNX08AC14G to the University of Colorado, from NASA. X. B. acknowledges support by the Spanish Ministry of Economy and Competitiveness through grant AYA2010-21490-C02-01. NR 47 TC 16 Z9 16 U1 0 U2 9 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUN 1 PY 2013 VL 769 IS 2 AR UNSP 90 DI 10.1088/0004-637X/769/2/90 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 158UM UT WOS:000319999100006 ER PT J AU Prestwich, AH Tsantaki, M Zezas, A Jackson, F Roberts, TP Foltz, R Linden, T Kalogera, V AF Prestwich, A. H. Tsantaki, Maria Zezas, A. Jackson, F. Roberts, T. P. Foltz, R. Linden, T. Kalogera, V. TI ULTRA-LUMINOUS X-RAY SOURCES IN THE MOST METAL POOR GALAXIES SO ASTROPHYSICAL JOURNAL LA English DT Article DE stars: formation; X-rays: binaries ID FORMATION RATE INDICATORS; COMPACT DWARF GALAXIES; STAR-FORMING GALAXIES; NEARBY GALAXIES; CHANDRA OBSERVATIONS; FORMATION RATES; BLACK-HOLES; H-ALPHA; CALIBRATION; METALLICITY AB Ultra-luminous X-ray sources (ULX) are X-ray binaries with L-x > 10(39) erg s(-1). The most spectacular examples of ULX occur in starburst galaxies and are now understood to be young, luminous high mass X-ray binaries. The conditions under which ULX form are poorly understood, but recent evidence suggests they may be more common in low metallicity systems. Here we investigate the hypothesis that ULX form preferentially in low metallicity galaxies by searching for ULX in a sample of extremely metal poor galaxies (XMPG) observed with the Chandra X-Ray Observatory. XMPG are defined as galaxies with log(O/H) + 12 < 7.65, or less than 5% solar. These are the most metal-deficient galaxies known, and a logical place to find ULX if they favor metal poor systems. We compare the number of ULX (corrected for background contamination) per unit of star formation (N-ULX(SFR)) in the XMPG sample with N-ULX(SFR) in a comparison sample of galaxies with higher metallicities taken from the Spitzer Infrared Galaxy Sample. We find that ULX occur preferentially in the metal poor sample with a formal statistical significance of 2.3 sigma. We do not see strong evidence for a trend in the formation of ULX in the high metallicity sample: above 12+log(O/H) similar to 8.0 the efficiency of ULX production appears to be flat. The effect we see is strongest in the lowest metallicity bin. We discuss briefly the implications of these results for the formation of black holes in low metallicity gas. C1 [Prestwich, A. H.; Zezas, A.; Jackson, F.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Tsantaki, Maria; Zezas, A.] Univ Crete, Dept Phys, Iraklion 71003, Crete, Greece. [Tsantaki, Maria] Univ Porto, Ctr Astrofis, P-4150762 Oporto, Portugal. [Zezas, A.] Fdn Res & Technol Hellas, Iraklion 71110, Crete, Greece. [Roberts, T. P.] Univ Durham, Dept Phys, Durham DH1 3LE, England. [Foltz, R.] Univ Calif Riverside, Dept Phys & Astron, Riverside, CA 92521 USA. [Linden, T.] Univ Calif Santa Cruz, Dept Phys, Santa Cruz, CA 95064 USA. [Kalogera, V.] Northwestern Univ, CIERA, Evanston, IL 60208 USA. [Kalogera, V.] Northwestern Univ, Dept Phys & Astron, Evanston, IL 60208 USA. RP Prestwich, AH (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Zezas, Andreas/C-7543-2011; OI Zezas, Andreas/0000-0001-8952-676X; Tsantaki, Maria/0000-0002-0552-2313 FU National Aeronautics and Space Administration through Chandra Award by the Chandra X-ray Observatory Center [G0-11108A]; National Aeronautics Space Administration [NAS8-03060]; NASA [NAS5-98034] FX Thanks to the Leigh Jenkins and the Chandra SINGS teams for providing results prior to publication, to Doug Swartz for giving us details of galaxies with no detected ULX and to the referee Michela Mapelli for helping to clarify many points in the paper. Support for this work was provided by the National Aeronautics and Space Administration through Chandra Award Number G0-11108A 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 NAS8-03060. 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. Based on observations made with the NASA Galaxy Evolution Explorer. GALEX is operated for NASA by the California Institute of Technology under NASA contract NAS5-98034 NR 41 TC 33 Z9 33 U1 2 U2 7 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUN 1 PY 2013 VL 769 IS 2 AR 92 DI 10.1088/0004-637X/769/2/92 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 158UM UT WOS:000319999100008 ER PT J AU Shcherbakov, RV Pe'er, A Reynolds, CS Haas, R Bode, T Laguna, P AF Shcherbakov, Roman V. Pe'er, Asaf Reynolds, Christopher S. Haas, Roland Bode, Tanja Laguna, Pablo TI GRB060218 AS A TIDAL DISRUPTION OF A WHITE DWARF BY AN INTERMEDIATE-MASS BLACK HOLE SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; black hole physics; radiation mechanisms: general; supernovae: general; X-rays: bursts; X-rays: individual (GRB060218) ID GAMMA-RAY-BURSTS; ACTIVE GALACTIC NUCLEI; SUPERNOVA SHOCK BREAKOUT; 3-DIMENSIONAL MAGNETOHYDRODYNAMIC SIMULATIONS; GRB 060218/SN 2006AJ; ACCRETION FLOWS; NEUTRON-STAR; STELLAR DISRUPTION; GLOBULAR-CLUSTERS; PROMPT EMISSION AB The highly unusual pair of a gamma-ray burst (GRB) GRB060218 and an associated supernova, SN2006aj, has puzzled theorists for years. A supernova shock breakout and a jet from a newborn stellar mass compact object have been proposed to explain this pair's multiwavelength signature. Alternatively, we propose that the source is naturally explained by another channel: the tidal disruption of a white dwarf (WD) by an intermediate-mass black hole (IMBH). This tidal disruption is accompanied by a tidal pinching, which leads to the ignition of a WD and a supernova. Some debris falls back onto the IMBH, forms a disk, which quickly amplifies the magnetic field, and launches a jet. We successfully fit soft X-ray spectra with the Comptonized blackbody emission from a jet photosphere. The optical/UV emission is consistent with self-absorbed synchrotron emission from the expanding jet front. The temporal dependence of the accretion rate (M) over dot(t) in a tidal disruption provides a good fit to the soft X-ray light curve. The IMBH mass is found to be about 10(4) M-circle dot in three independent estimates: (1) fitting the tidal disruption (M) over dot(t) to the soft X-ray light curve, (2) computing the jet base radius in a jet photospheric emission model, and (3) inferring the mass of the central black hole based on the host dwarf galaxy's stellar mass. The position of the supernova is consistent with the center of the host galaxy, while the low supernova ejecta mass is consistent with that of a WD. The high expected rate of tidal disruptions in dwarf galaxies is consistent with one source observed by the Swift satellite over several years at a distance of 150 Mpc measured for GRB060218. Encounters with WDs provide much fuel for the growth of IMBHs. C1 [Shcherbakov, Roman V.; Reynolds, Christopher S.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Shcherbakov, Roman V.; Reynolds, Christopher S.] Univ Maryland, Joint Space Sci Inst, College Pk, MD 20742 USA. [Pe'er, Asaf] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Pe'er, Asaf] Natl Univ Ireland Univ Coll Cork, Dept Phys, Cork, Ireland. [Haas, Roland] CALTECH, Pasadena, CA 91125 USA. [Haas, Roland; Bode, Tanja; Laguna, Pablo] Georgia Inst Technol, Sch Phys, Ctr Relativist Astrophys, Atlanta, GA 30332 USA. RP Shcherbakov, RV (reprint author), Univ Maryland, Dept Astron, College Pk, MD 20742 USA. FU NASA Hubble Fellowship [HST-HF-51298.01]; NSF [1212433, 1205864, 0941417, 0903973, 0855423]; NASA [NNX10AE41G] FX The authors are thankful to Nathaniel Bulter, John Cannizzo, Coleman Miller, Ramesh Narayan, Eve Ostriker, Enrico Ramirez-Ruiz, and Leslie Sage for useful discussions and comments. Special thanks to Abderahmen Zoghbi for advice on temporal analysis, Ranjan Vasudevan for general help with XSPEC, and Demosthenes Kazanas and Jonathan McKinney for discussions of the generation of a large-scale magnetic field. We thank the anonymous referee for insightful comments which helped to improve the manuscript. R. V. S. is supported by NASA Hubble Fellowship grant HST-HF-51298.01, P. L. is supported by NSF grants 1212433, 1205864, 0941417, 0903973, 0855423, and 0903973. C. S. R. thanks NASA for support under Astrophysics Theory Program (ATP) grant NNX10AE41G. NR 163 TC 17 Z9 18 U1 0 U2 7 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUN 1 PY 2013 VL 769 IS 2 AR UNSP 85 DI 10.1088/0004-637X/769/2/85 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 158UM UT WOS:000319999100001 ER PT J AU van Weeren, RJ Fogarty, K Jones, C Forman, WR Clarke, TE Bruggen, M Kraft, RP Lal, DV Murray, SS Rottgering, HJA AF van Weeren, R. J. Fogarty, K. Jones, C. Forman, W. R. Clarke, T. E. Brueggen, M. Kraft, R. P. Lal, D. V. Murray, S. S. Rottgering, H. J. A. TI COMPLEX DIFFUSE RADIO EMISSION IN THE MERGING PLANCK ESZ CLUSTER A3411 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: clusters: individual (A3411); galaxies: clusters: intracluster medium; large-scale structure of universe; radiation mechanisms: non-thermal; X-rays: galaxies: clusters ID X-RAY-EMISSION; GALAXY CLUSTERS; PARTICLE-ACCELERATION; SHOCK ACCELERATION; COMA CLUSTER; COSMIC-RAYS; COSMOLOGICAL SIMULATIONS; DARK-MATTER; ABELL 2146; ASTROPHYSICAL SHOCKS AB We present Very Large Array (VLA) radio and Chandra X-ray observations of the merging galaxy cluster A3411. For the cluster, we find an overall temperature of 6.4(-1.0)(+0.6) keV and an X-ray luminosity of 2.8 +/- 0.1 x 10(44) erg s(-1) between 0.5 and 2.0 keV. The Chandra observation reveals the cluster to be undergoing a merger event. The VLA observations show the presence of large-scale diffuse emission in the central region of the cluster, which we classify as a 0.9 Mpc size radio halo. In addition, a complex region of diffuse, polarized emission is found in the southeastern outskirts of the cluster along the projected merger axis of the system. We classify this region of diffuse emission as a radio relic. The total extent of this radio relic is 1.9 Mpc. For the combined emission in the cluster region, we find a radio spectral index of -1.0 +/- 0.1 between 74 MHz and 1.4 GHz. The morphology of the radio relic is peculiar, as the relic is broken up into five fragments. This suggests that the shock responsible for the relic has been broken up due to interaction with a large-scale galaxy filament connected to the cluster or other substructures in the intracluster medium. Alternatively, the complex morphology reflects the presence of electrons in fossil radio bubbles that are re-accelerated by a shock. C1 [van Weeren, R. J.; Fogarty, K.; Jones, C.; Forman, W. R.; Kraft, R. P.; Murray, S. S.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Fogarty, K.; Murray, S. S.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Clarke, T. E.] USN, Res Lab, Remote Sensing Div, Washington, DC 20375 USA. [Brueggen, M.] Hamburger Sternwarte, D-21029 Hamburg, Germany. [Lal, D. V.] TIFR, Natl Ctr Radio Astrophys, Pune 411007, Maharashtra, India. [Rottgering, H. J. A.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. RP van Weeren, RJ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM rvanweeren@cfa.harvard.edu OI van Weeren, Reinout/0000-0002-0587-1660; Forman, William/0000-0002-9478-1682 FU NASA [PF2-130104, NAS8-03060]; Chandra X-ray Center; 6.1 Base funds; ESO Telescopes at the La Silla or Paranal Observatory under programme [070.B-0440(A)]; National Aeronautics and Space Administration; National Science Foundation; Space Telescope Science Institute under U.S. Government [NAG W-2166]; National Geographic Society; Sloan Foundation; Samuel Oschin Foundation; Eastman Kodak Corporation FX We would like to thank the anonymous referee for useful comments and Simona Giacintucci for useful discussions. Support for this work was provided by NASA through the Einstein Postdoctoral grant number PF2-130104 awarded by the Chandra X-ray Center, which is operated by the Smithsonian Astrophysical Observatory for NASA under contract NAS8-03060. Basic research into radio astronomy at the Naval Research Laboratory is supported by 6.1 Base funds. The scientific results reported in this article are based in part on observations made by the Chandra X-Ray Observatory. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. This work is based on data products from observations made with ESO Telescopes at the La Silla or Paranal Observatory under programme ID 070.B-0440(A). 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. The Digitized Sky Surveys were produced at the Space Telescope Science Institute under U.S. Government grant NAG W-2166. The images of these surveys are based on photographic data obtained using the Oschin Schmidt Telescope on Palomar Mountain and the UK Schmidt Telescope. The plates were processed into the present compressed digital form with the permission of these institutions. The Second Palomar Observatory Sky Survey (POSS-II) was made by the California Institute of Technology with funds from the National Science Foundation, the National Geographic Society, the Sloan Foundation, the Samuel Oschin Foundation, and the Eastman Kodak Corporation. NR 97 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 JUN 1 PY 2013 VL 769 IS 2 AR 101 DI 10.1088/0004-637X/769/2/101 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 158UM UT WOS:000319999100017 ER PT J AU Wang, ZX Kaplan, DL Slane, P Morrell, N Kaspi, VM AF Wang, Zhongxiang Kaplan, David L. Slane, Patrick Morrell, Nidia Kaspi, Victoria M. TI SERENDIPITOUS DISCOVERY OF AN INFRARED BOW SHOCK NEAR PSR J1549-4848 WITH SPITZER SO ASTROPHYSICAL JOURNAL LA English DT Article DE infrared: ISM; ISM: structure; stars: individual (PSR J1549, 4848); stars: neutron ID EXACT ANALYTIC SOLUTIONS; INTERSTELLAR DUST; SPACE-TELESCOPE; EMISSION; EXTINCTION; NEBULAE; CAMERA; GALAXY; STARS; FIELD AB We report on the discovery of an infrared cometary nebula around PSR J1549-4848 in our Spitzer survey of a few middle-aged radio pulsars. Following the discovery, multi-wavelength imaging and spectroscopic observations of the nebula were carried out. We detected the nebula in Spitzer Infrared Array Camera 8.0, Multiband Imaging Photometer for Spitzer 24 and 70 mu m imaging, and in Spitzer IRS 7.5-14.4 mu m spectroscopic observations, and also in the Wide-field Infrared Survey Explorer all-sky survey at 12 and 22 mu m. These data were analyzed in detail, and we find that the nebula can be described with a standard bow shock shape, and that its spectrum contains polycyclic aromatic hydrocarbon and H-2 emission features. However, it is not certain which object drives the nebula. We analyze the field stars and conclude that none of them can be the associated object because stars with a strong wind or mass ejection that usually produce bow shocks are much brighter than the field stars. The pulsar is approximately 15 '' away from the region in which the associated object is expected to be located. In order to resolve the discrepancy, we suggest that a highly collimated wind could be emitted from the pulsar and produce the bow shock. X-ray imaging to detect the interaction of the wind with the ambient medium-and high-spatial resolution radio imaging to determine the proper motion of the pulsar should be carried out, which will help verify the association of the pulsar with the bow shock nebula. C1 [Wang, Zhongxiang] Chinese Acad Sci, Shanghai Astron Observ, Shanghai 200030, Peoples R China. [Kaplan, David L.] Univ Wisconsin, Dept Phys, Milwaukee, WI 53211 USA. [Slane, Patrick] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Morrell, Nidia] Observ Carnegie Inst Washington, Las Campanas Observ, La Serena, Chile. [Kaspi, Victoria M.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada. RP Wang, ZX (reprint author), Chinese Acad Sci, Shanghai Astron Observ, 80 Nandan Rd, Shanghai 200030, Peoples R China. RI he, shuyi/K-2082-2014 FU National Basic Research Program of China (973 Project) [2009CB824800]; National Natural Science Foundation of China [11073042]; NASA [NAS8-03060] FX This research was supported by National Basic Research Program of China (973 Project 2009CB824800), and National Natural Science Foundation of China (11073042). Z.W. is a Research Fellow of the One-Hundred-Talents project of Chinese Academy of Sciences. P. S. acknowledges partial support from NASA Contract NAS8-03060. V. M. K. holds a Canada Research Chair and the Lorne Trottier Chair in Astrophysics and Cosmology, and is a Fellow of the Royal Society of Canada. NR 35 TC 3 Z9 3 U1 1 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 JUN 1 PY 2013 VL 769 IS 2 AR UNSP 122 DI 10.1088/0004-637X/769/2/122 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 158UM UT WOS:000319999100038 ER PT J AU Kellner, K Fernandez-Marin, H Ishak, HD Sen, R Linksvayer, TA Mueller, UG AF Kellner, K. Fernandez-Marin, H. Ishak, H. D. Sen, R. Linksvayer, T. A. Mueller, U. G. TI Co-evolutionary patterns and diversification of ant-fungus associations in the asexual fungus-farming ant Mycocepurus smithii in Panama SO JOURNAL OF EVOLUTIONARY BIOLOGY LA English DT Article DE co-evolution; host specificity; host switching; mutualism; symbiosis; thelytoky ID HOST-PARASITE COSPECIATION; GROWING ANTS; BRADYRHIZOBIUM MUTUALISM; MAXIMUM-LIKELIHOOD; FIG WASPS; COEVOLUTION; FORMICIDAE; POPULATIONS; GENETICS; AGRICULTURE AB Partner fidelity through vertical symbiont transmission is thought to be the primary mechanism stabilizing cooperation in the mutualism between fungus-farming (attine) ants and their cultivated fungal symbionts. An alternate or additional mechanism could be adaptive partner or symbiont choice mediating horizontal cultivar transmission or de novo domestication of free-living fungi. Using microsatellite genotyping for the attine ant Mycocepurus smithii and ITS rDNA sequencing for fungal cultivars, we provide the first detailed population genetic analysis of local ant-fungus associations to test for the relative importance of vertical vs. horizontal transmission in a single attine species. M.smithii is the only known asexual attine ant, and it is furthermore exceptional because it cultivates a far greater cultivar diversity than any other attine ant. Cultivar switching could permit the ants to re-acquire cultivars after garden loss, to purge inferior cultivars that are locally mal-adapted or that accumulated deleterious mutations under long-term asexuality. Compared to other attine ants, symbiont choice and local adaptation of ant-fungus combinations may play a more important role than partner-fidelity feedback in the co-evolutionary process of M.smithii and its fungal symbionts. C1 [Kellner, K.; Ishak, H. D.; Mueller, U. G.] Univ Texas Austin, Patterson Labs, Sect Integrat Biol, Austin, TX 78712 USA. [Fernandez-Marin, H.; Mueller, U. G.] Smithsonian Trop Res Inst, Balboa, Panama. [Fernandez-Marin, H.] Inst Invest Cient & Serv Alta Tecnol, Panama City, Panama. [Sen, R.] Purdue Univ, Dept Entomol, W Lafayette, IN 47907 USA. [Linksvayer, T. A.] Univ Penn, Dept Biol, Philadelphia, PA 19104 USA. RP Kellner, K (reprint author), Univ Texas Tyler, Dept Biol, 3900 Univ Blvd, Tyler, TX 75799 USA. EM antkatrina@gmail.com FU National Science Foundation [DEB-0919519]; W.M. Wheeler Lost Pines Endowment FX We thank the Autoridad Nacional del Ambiente de Panama, the Smithsonian Tropical Research Institute and Orelis Arosemena and Annette Aiello for collecting and export permits; Jon Seal, Nancy Lowe and Nicole Gerardo for help with collections; Pierre Legendre for advice on ParaFit, and Jon Seal, Christian Rabeling and Quinn McFrederick and two anonymous reviewers for helpful comments on the manuscript. The work was supported by a National Science Foundation award (DEB-0919519) to TAL and UGM, and by the W.M. Wheeler Lost Pines Endowment. NR 65 TC 7 Z9 7 U1 6 U2 74 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1010-061X J9 J EVOLUTION BIOL JI J. Evol. Biol. PD JUN PY 2013 VL 26 IS 6 BP 1353 EP 1362 DI 10.1111/jeb.12140 PG 10 WC Ecology; Evolutionary Biology; Genetics & Heredity SC Environmental Sciences & Ecology; Evolutionary Biology; Genetics & Heredity GA 161CV UT WOS:000320170100016 PM 23639137 ER PT J AU Beck, AW McSween, HY Bodnar, RJ AF Beck, Andrew W. McSween, Harry Y., Jr. Bodnar, Robert J. TI In situ laser ablation ICP-MS analyses of dimict diogenites: Further evidence for harzburgitic and orthopyroxenitic lithologies SO METEORITICS & PLANETARY SCIENCE LA English DT Article ID ASTEROID 4 VESTA; HED PARENT BODY; ORTHO-PYROXENE; STILLWATER COMPLEX; OLIVINE DIOGENITES; ELEMENT CHEMISTRY; GEOCHEMISTRY; INSIGHTS; HOWARDITES; PETROLOGY AB Trace element concentrations in pyroxene, plagioclase, and olivine were measured in five diogenite breccias previously identified as containing distinct harzburgitic (ol+opx) and orthopyroxenitic (opx) lithologies (dimict). Three samples show two distinct populations of pyroxene trace element abundances, supporting their classification as dimict. These three meteorites show increases in Y, Yb, and HREE concentrations from harzburgitic to orthopyroxenitic pyroxenes, supporting the hypothesis that the lithologies are related through fractional crystallization whereby harzburgite olivine and pyroxene crystallized from the magma first followed by orthopyroxenite pyroxene. Depletions in LREE and Eu concentrations in the orthopyroxenitic lithology are most likely due to equilibration with LREE and Eu-rich phases, likely plagioclase, which is found primarily in that lithology. Two samples do not show evidence supporting a dimict classification. Large pyroxene trace element variation in one sample indicates that it is polymict, while uniform trace element distribution in the other suggests that it may be a monomict breccia. C1 [Beck, Andrew W.] Natl Museum Nat Hist, Smithsonian Inst, Washington, DC 20560 USA. [McSween, Harry Y., Jr.] Univ Tennessee, Dept Earth & Planetary Sci, Knoxville, TN 37996 USA. [McSween, Harry Y., Jr.] Univ Tennessee, Planetary Geosci Inst, Knoxville, TN 37996 USA. [Bodnar, Robert J.] Virginia Tech, Dept Geosci, Blacksburg, VA 24061 USA. RP Beck, AW (reprint author), Natl Museum Nat Hist, Smithsonian Inst, 10th & Constitut NW, Washington, DC 20560 USA. EM becka@si.edu RI Beck, Andrew/J-7215-2015 OI Beck, Andrew/0000-0003-4455-2299 FU NASA [NNG06GG36G] FX We thank J. A. Barrat and P. Warren for their comments, and A. Ruzicka for editorial handling. We also thank L. Fedele for his assistance in both data acquisition and data reduction, the MWG for allocation of meteorite samples, and D. W. Mittlefehldt for discussions on taxonomy and geochemistry with regard to this work. This work was partially supported by NASA Cosmochemistry Grant NNG06GG36G to HYM. NR 31 TC 4 Z9 4 U1 1 U2 8 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1086-9379 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD JUN PY 2013 VL 48 IS 6 BP 1050 EP 1059 DI 10.1111/maps.12129 PG 10 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 164EQ UT WOS:000320392100008 ER PT J AU Suselbeek, L Jansen, PA Prins, HHT Steele, MA AF Suselbeek, L. Jansen, P. A. Prins, H. H. T. Steele, M. A. TI Tracking rodent-dispersed large seeds with Passive Integrated Transponder (PIT) tags SO METHODS IN ECOLOGY AND EVOLUTION LA English DT Article DE acorn; hoarding; passive integrated transponder; PIT tag; Quercus; rodents; seed dispersal; seed tracking ID QUERCUS-ROBUR SEEDLINGS; YELLOW PINE CHIPMUNKS; COTYLEDON REMOVAL; CACHE PILFERAGE; IDENTIFICATION; GROWTH; PREDATION; REGENERATION; TECHNOLOGY; MANAGEMENT AB Seed dispersal, a critical phase in the life history of many plants, is poorly understood due to the difficulty of tracking and monitoring dispersing seeds until they reach their ultimate fate. Scatter-hoarding rodents play a substantial part in the seed dispersal process of many plant species, however, existing tracking methods do not allow seed monitoring without risk of influencing the hoarding process and seed fate. Here, we describe and test the use of Passive Integrated Transponders (PIT) tags inserted into seeds for the tracking and monitoring of large seeds dispersed by rodents. Unlike other tagging methods, PIT tagging combines the advantages of leaving no external cues and being readable without disturbance of caches. Rodents cannot remove these tags. We evaluated the performance of PIT tagging through a series of trials with Quercus acorns dispersed by rodents, both in North America and in Europe, with equipment from different manufacturers. We quantified effects of tagging on seed removal and caching, cache pilferage and seed germination, by comparison between PIT-tagged and untagged acorns. We evaluated the detectability of buried tags to researchers. Minimal effects of PIT tagging on seed removal, caching, pilferage and germination were found. Buried PIT tags were retrieved with high reliability by naive researchers, even at burial depths up to 30 cm. Identification codes could be read even when multiple tags were buried at a single location, as in larder hoarding. The method was successfully applied in two field studies of dispersal of Quercus palustris and Q. rubra acorns by Eastern grey squirrels Sciurus carolinensis in North America, and Q. robur acorns by Wood mice Apodemus sylvaticus in the Netherlands. The proportion of seeds recovered was comparable to that in studies using traditional thread tags. We conclude that PIT tagging is a particularly suitable method for tracking and monitoring of seeds dispersed by scatter-hoarding rodents. PIT tagging solves most of the main problems generally encountered when following the fate of rodent-dispersed seeds over time. C1 [Suselbeek, L.; Jansen, P. A.; Prins, H. H. T.] Wageningen Univ, Dept Environm Sci, NL-6700 AA Wageningen, Netherlands. [Jansen, P. A.] Smithsonian Trop Res Inst, Balboa, Panama. [Steele, M. A.] Wilkes Univ, Dept Biol, Wilkes Barre, PA 18766 USA. RP Suselbeek, L (reprint author), Wageningen Univ, Dept Environm Sci, POB 47, NL-6700 AA Wageningen, Netherlands. EM lennart.suselbeek@wur.nl RI Jansen, Patrick/G-2545-2015; OI Jansen, Patrick/0000-0002-4660-0314; Suselbeek, Lennart/0000-0002-1896-855X FU Netherlands Organisation for Scientific Research [NWO-ALW08056]; Howard Hughes Medical Institute; H. Fenner Endowment of Wilkes University; Bullard Fellowship from Harvard Forest FX We thank Andrew Bartlow, Rachel Curtis, Daan Jacobs, Simone van Santen de Hoog, Marco Snijder, Malou van Meer, Jose van der Bijl and Jessica van der Wal for field and laboratory assistance. We also thank Frans Bongers and three anonymous reviewers for insightful comments. LS was funded by the Netherlands Organisation for Scientific Research (NWO-ALW08056). MS was supported by the Howard Hughes Medical Institute, the H. Fenner Endowment of Wilkes University, and a Bullard Fellowship from Harvard Forest. NR 50 TC 11 Z9 12 U1 8 U2 68 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 2041-210X J9 METHODS ECOL EVOL JI Methods Ecol. Evol. PD JUN PY 2013 VL 4 IS 6 BP 513 EP 519 DI 10.1111/2041-210X.12027 PG 7 WC Ecology SC Environmental Sciences & Ecology GA 160KA UT WOS:000320117200002 ER PT J AU Parchman, TL Gompert, Z Braun, MJ Brumfield, RT Mcdonald, DB Uy, JAC Zhang, G Jarvis, ED Schlinger, BA Buerkle, CA AF Parchman, T. L. Gompert, Z. Braun, M. J. Brumfield, R. T. Mcdonald, D. B. Uy, J. A. C. Zhang, G. Jarvis, E. D. Schlinger, B. A. Buerkle, C. A. TI The genomic consequences of adaptive divergence and reproductive isolation between species of manakins SO MOLECULAR ECOLOGY LA English DT Article DE genomic cline; hybrid zone; Manacus; next-generation sequencing; population genomics; speciation ID AVIAN HYBRID ZONE; ECOLOGICAL SPECIATION; GENETIC ARCHITECTURE; POPULATION-STRUCTURE; BAYESIAN-ESTIMATION; PARALLEL EVOLUTION; ANOPHELES-GAMBIAE; SOFT SWEEPS; ADAPTATION; DIFFERENTIATION AB The processes of adaptation and speciation are expected to shape genomic variation within and between diverging species. Here we analyze genomic heterogeneity of genetic differentiation and introgression in a hybrid zone between two bird species (Manacus candei and M. vitellinus) using 59100 SNPs, a whole genome assembly, and Bayesian models. Measures of genetic differentiation (FST) and introgression (genomic cline center [] and rate []) were highly heterogeneous among loci. We identified thousands of loci with elevated parameter estimates, some of which are likely to be associated with variation in fitness in Manacus populations. To analyze the genomic organization of differentiation and introgression, we mapped SNPs onto a draft assembly of the M. vitellinus genome. Estimates of FST, , and were autocorrelated at very short physical distances (<100 bp), but much less so beyond this. In addition, average statistical associations (linkage disequilibrium) between SNPs were generally low and were not higher in admixed populations than in populations of the parental species. Although they did not occur with a constant probability across the genome, loci with elevated FST, , and were not strongly co-localized in the genome. Contrary to verbal models that predict clustering of loci involved in adaptation and isolation in discrete genomic regions, these results are consistent with the hypothesis that genetic regions involved in adaptive divergence and reproductive isolation are scattered throughout the genome. We also found that many loci were characterized by both exceptional genetic differentiation and introgression, consistent with the hypothesis that loci involved in isolation are also often characterized by a history of divergent selection. However, the concordance between isolation and differentiation was only partial, indicating a complex architecture and history of loci involved in isolation. C1 [Parchman, T. L.; Gompert, Z.; Buerkle, C. A.] Univ Wyoming, Dept Bot, Laramie, WY 82071 USA. [Braun, M. J.] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC USA. [Brumfield, R. T.] Louisiana State Univ, Dept Biol Sci, Baton Rouge, LA 70803 USA. [Brumfield, R. T.] Louisiana State Univ, Museum Nat Sci, Baton Rouge, LA 70803 USA. [Mcdonald, D. B.] Univ Wyoming, Dept Zool & Physiol, Laramie, WY 82071 USA. [Uy, J. A. C.] Univ Miami, Dept Biol, Miami, FL 33146 USA. [Zhang, G.] Beijing Genome Inst, Beijing, Peoples R China. [Jarvis, E. D.] Duke Univ, Med Ctr, Dept Neurobiol, Durham, NC 27710 USA. [Schlinger, B. A.] Univ Calif Los Angeles, Dept Integrat Biol & Physiol, Los Angeles, CA 90095 USA. RP Parchman, TL (reprint author), Univ Wyoming, Dept Bot, Laramie, WY 82071 USA. EM tparchma@uwyo.edu RI Zhang, Guojie/B-6188-2014; Jarvis, Erich/A-2319-2008; OI Zhang, Guojie/0000-0001-6860-1521; Jarvis, Erich/0000-0001-8931-5049; Uy, J. Albert C./0000-0002-8437-5525; Brumfield, Robb/0000-0003-2307-0688 FU National Museum of Natural History; NSF [IOS-1137624, DEB-1146265] FX This research was funded through the Small Grants Program of the National Museum of Natural History to M. Braun and NSF grants IOS-1137624 to A. Uy and and DEB-1146265 to R. T. Brumfield. C. W. Benkman, P. Nosil, and R. Safran provided helpful comments on previous drafts of this manuscript. We thank the "International Avian Phylogenomic Community" for early access to the M. vitellinus genome data, and T. Yuri for preparing Fig. 1. We also thank T. Parsons, S. Olson, T. Glenn and J. Blake for contributions to the fieldwork. NR 83 TC 38 Z9 38 U1 9 U2 134 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0962-1083 J9 MOL ECOL JI Mol. Ecol. PD JUN PY 2013 VL 22 IS 12 BP 3304 EP 3317 DI 10.1111/mec.12201 PG 14 WC Biochemistry & Molecular Biology; Ecology; Evolutionary Biology SC Biochemistry & Molecular Biology; Environmental Sciences & Ecology; Evolutionary Biology GA 164GC UT WOS:000320396100011 PM 23441849 ER PT J AU Jangid, K Whitman, WB Condron, LM Turner, BL Williams, MA AF Jangid, Kamlesh Whitman, William B. Condron, Leo M. Turner, Benjamin L. Williams, Mark A. TI Soil bacterial community succession during long-term ecosystem development SO MOLECULAR ECOLOGY LA English DT Article DE 16S rRNA pyrosequencing; bacterial diversity; Franz Josef chronosequence; soil development; soil nutrients; vegetative succession AB The physicochemical and biological gradients of soil and vegetative succession along the Franz Josef chronosequence in New Zealand were used to test whether bacterial communities show patterns of change associated with long-term ecosystem development. Pyrosequencing was conducted on soil-derived 16S rRNA genes at nine stages of ecosystem progression and retrogression, ranging in age from 60 to c. 120000years since glacial retreat. Bray-Curtis ordination indicated that the bacterial communities showed clear patterns of change that were closely aligned with ecosystem development, pedogenesis and vegetative succession (Mantel test; r=0.58; P<0.001). Eighty per cent (80%) of the explained variability in bacterial community structure was observed during the first c. 1000years of development, when bacterial richness (Simpson's 1/D) declined from 130 to 30. The relatively high turnover of soil bacterial communities corresponded with an integrative plant-microbial successional feedback' model that predicts primarily negative feedbacks between plants and soil bacterial communities during progression and early pedogenesis. Positive feedbacks, similar to those of the plant community, could explain the long periods of community stability during later retrogressive stages of ecosystem development. This hypothesized model provides a consistent description linking belowground communities to ecosystem development and succession. The research, using deep sequencing technology, provides the first evidence for soil bacterial community change associated with the process of long-term ecosystem development. How these bacterial community changes are linked to the processes of primary ecosystem succession is not known and needs further investigation. C1 [Jangid, Kamlesh] Natl Ctr Cell Sci, Pune 411007, Maharashtra, India. [Whitman, William B.] Univ Georgia, Dept Microbiol, Athens, GA 30602 USA. [Condron, Leo M.] Lincoln Univ, Canterbury 7647, New Zealand. [Turner, Benjamin L.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. [Williams, Mark A.] Virginia Polytech & State Univ, Blacksburg, VA 24060 USA. RP Williams, MA (reprint author), Virginia Polytech & State Univ, 301 Latham Hall, Blacksburg, VA 24060 USA. EM markwill@vt.edu RI Turner, Benjamin/E-5940-2011; OI Turner, Benjamin/0000-0002-6585-0722; Williams, Mark A./0000-0002-4766-9399 FU NSF FX M.W. conceived the research. K.J. performed research. M. W., K.J. and B. W. wrote the grant and received funding from NSF. K.J. and M. W. developed figures and analyzed data. B. T. and L. C. collected samples. M. W. wrote the manuscript. All authors provided edits and intellectual expertise to manuscript. NR 0 TC 22 Z9 23 U1 4 U2 83 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0962-1083 J9 MOL ECOL JI Mol. Ecol. PD JUN PY 2013 VL 22 IS 12 BP 3415 EP 3424 DI 10.1111/mec.12325 PG 10 WC Biochemistry & Molecular Biology; Ecology; Evolutionary Biology SC Biochemistry & Molecular Biology; Environmental Sciences & Ecology; Evolutionary Biology GA 164GC UT WOS:000320396100019 PM 24624422 ER PT J AU Hollins, H AF Hollins, Hunter TI Forgotten hardware: how to urinate in a spacesuit SO ADVANCES IN PHYSIOLOGY EDUCATION LA English DT Editorial Material DE history of physiology; space physiology; urine collection AB On May 5, 1961, astronaut Alan Shepard became the first American to fly in space. Although the National Aeronautics and Space Administration (NASA) had discounted the need for him to urinate, Shepard did, in his spacesuit, short circuiting his electronic biosensors. With the development of the pressure suit needed for high-altitude and space flight during the 1950s, technicians had developed the means for urine collection. However, cultural mores, combined with a lack of inter-agency communication, and the technical difficulties of spaceflight made human waste collection a difficult task. Despite the difficulties, technicians at NASA created a successful urine collection device that John Glenn wore on the first Mercury orbital flight on February 20, 1962. With minor modifications, male astronauts used this system to collect urine until the Space Shuttle program. John Glenn's urine collection device is at the National Air and Space Museum and has been on view to the public since 1976. C1 Smithsonian Inst, Natl Air & Space Museum, Washington, DC 20013 USA. RP Hollins, H (reprint author), Smithsonian Inst, Natl Air & Space Museum, MRC 311,POB 37012, Washington, DC 20013 USA. EM hollinsh@si.edu NR 30 TC 0 Z9 0 U1 1 U2 9 PU AMER PHYSIOLOGICAL SOC PI BETHESDA PA 9650 ROCKVILLE PIKE, BETHESDA, MD 20814 USA SN 1043-4046 J9 ADV PHYSIOL EDUC JI Adv. Physiol. Educ. PD JUN PY 2013 VL 37 IS 2 BP 123 EP 128 DI 10.1152/advan.00175.2012 PG 6 WC Education, Scientific Disciplines; Physiology SC Education & Educational Research; Physiology GA 156ES UT WOS:000319805100001 PM 23728129 ER PT J AU Simpson, C AF Simpson, Carl TI SPECIES SELECTION AND THE MACROEVOLUTION OF CORAL COLONIALITY AND PHOTOSYMBIOSIS SO EVOLUTION LA English DT Article DE Diversification; multilevel selection; multivariate selection; paleobiology; phylogenetics ID PUNCTUATED EQUILIBRIUM; MOLECULAR PHYLOGENIES; DIVERSIFICATION RATES; EXTINCTION RATES; SCLERACTINIAN CORALS; PHENOTYPIC EVOLUTION; CRETACEOUS MOLLUSKS; NATURAL-SELECTION; GEOGRAPHIC RANGE; FOSSIL RECORD AB Differences in the relative diversification rates of species with variant traits are known as species selection. Species selection can produce a macroevolutionary change in the frequencies of traits by changing the relative number of species possessing each trait over time. But species selection is not the only process that can change the frequencies of traits, phyletic microevolution of traits within species and phylogenetic trait evolution among species, the tempo and mode of microevolution can also change trait frequencies. Species selection, phylogenetic, and phyletic processes can all contribute to large-scale trends, reinforcing or canceling each other out. Even more complex interactions among macroevolutionary processes are possible when multiple covarying traits are involved. Here I present a multilevel macroevolutionary framework that is useful for understanding how macroevolutionary processes interact. It is useful for empirical studies using fossils, molecular phylogenies, or both. I illustrate the framework with the macroevolution of coloniality and photosymbiosis in scleractinian corals using a time-calibrated molecular phylogeny. I find that standing phylogenetic variation in coloniality and photosymbiosis deflects the direction of macroevolution from the vector of species selection. Variation in these traits constrains species selection and results in a 200 million year macroevolutionary equilibrium. C1 [Simpson, Carl] Univ Berlin, Leibniz Inst, Museum Nat Kunde, D-10115 Berlin, Germany. RP Simpson, C (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, POB 37012,MRC 121, Washington, DC 20013 USA. EM glyptocrinus@gmail.com FU Deutsche Forschungsgemeinschaft [KI 806/7-1]; National Evolutionary Synthesis Center FX I thank M. Hopkins, W. Kiessling, D. McCandlish, and J. Spicer for discussions and G. Hunt and another anonymous reviewer for helpful comments. This work was supported by Deutsche Forschungsgemeinschaft grant KI 806/7-1 and a short-term scholar fellowship from the National Evolutionary Synthesis Center. NR 91 TC 10 Z9 10 U1 2 U2 48 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0014-3820 J9 EVOLUTION JI Evolution PD JUN PY 2013 VL 67 IS 6 BP 1607 EP 1621 DI 10.1111/evo.12083 PG 15 WC Ecology; Evolutionary Biology; Genetics & Heredity SC Environmental Sciences & Ecology; Evolutionary Biology; Genetics & Heredity GA 157DA UT WOS:000319874800008 PM 23730756 ER PT J AU Alvizu, A Diaz, MC Bastidas, C Rutzler, K Thacker, RW Marquez, LM AF Alvizu, A. Diaz, M. C. Bastidas, C. Ruetzler, K. Thacker, R. W. Marquez, L. M. TI A skeleton-less sponge of Caribbean mangroves: invasive or undescribed? SO INVERTEBRATE BIOLOGY LA English DT Article DE genetic variability; histology; Halisarca; Porifera; phylogeny ID DEMOSPONGE ASTROSCLERA-WILLEYANA; OXIDASE SUBUNIT-I; BOCAS DEL TORO; INDO-PACIFIC; HALISARCA-DUJARDINI; BIOLOGICAL INVASIONS; POPULATION-GENETICS; MEDITERRANEAN SEA; PORIFERA; MITOCHONDRIAL AB Recent surveys of sponges occurring on Caribbean mangrove roots demonstrated the presence of a skeleton-less sponge of the genus Halisarca, very similar in its morphology to the temperate H. dujardinii. This study evaluated the possibility that the mangrove sponge was actually H. dujardinii that had been introduced into the Caribbean mangroves. Detailed histology revealed differences between the mangrove sponge and H. dujardinii in cuticle thickness, and in characteristics of the choanocytes, spherulous, and granular cells. Also, phylogenetic reconstruction and genetic distance estimates based on cytochrome oxidase I gene sequences clearly differentiated the mangrove Halisarca sp. from H. dujardinii. Therefore, we rejected the hypothesis of the invasion of H. dujardinii, recognizing instead the mangrove Halisarca sp. as a new species and naming it H. restingaensis sp. nov. Estimated levels of genetic variation in the ribosomal internal transcribed spacers indicated that populations of H. restingaensis sp. nov. are highly differentiated between Venezuela and Panama (Fst=0.71). This level of population differentiation is consistent with the short larval competence period that is common in members of the genus Halisarca. C1 [Alvizu, A.; Bastidas, C.; Marquez, L. M.] Univ Simon Bolivar, Dept Biol Organismos, Caracas 1080A, Venezuela. [Diaz, M. C.] Museo Marino Margarita, Boca Del Rio, Venezuela. [Ruetzler, K.] Natl Museum Nat Hist, Smithsonian Inst, Washington, DC 20560 USA. [Thacker, R. W.] Univ Alabama Birmingham, Dept Biol, Birmingham, AL 35294 USA. [Marquez, L. M.] Fdn Inst Estudios Avanzados, Caracas 1080A, Venezuela. RP Marquez, LM (reprint author), Penn State Univ, Dept Plant Pathol & Environm Microbiol, University Pk, PA 16802 USA. EM luismarquez_gomez@yahoo.com FU Ministerio del Poder Popular para la Ciencia y la Tecnologia (Mision Ciencias); Decanato de Investigacion y Desarrollo USB; Fundacion Instituto de Estudios Avanzados IDEA; U.S. National Science Foundation [0829986] FX This project received financial support from a scholarship to AA by the Ministerio del Poder Popular para la Ciencia y la Tecnologia (Mision Ciencias), an S1 project to CB by the Decanato de Investigacion y Desarrollo USB, and an internal grant to LMM by the Fundacion Instituto de Estudios Avanzados IDEA. We thank the people at the Centro de Biotecnologia de Plantas at IDEA for logistic support. Also, we thank Dr. JL Palazon of the Instituto de Ciencias Marinas de Andalucia-CSIC for preparing the tissue sections for light microscopy, and Ms. Andrea Brothers for sectioning and processing for transmission electron microscopy. We are indebted to two reviewers and the journal editors, whose comments and suggestions for changes improved our manuscript significantly. Collections from Panama were supported by the U.S. National Science Foundation under grant 0829986 to RWT. NR 67 TC 3 Z9 4 U1 0 U2 17 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1077-8306 EI 1744-7410 J9 INVERTEBR BIOL JI Invertebr. Biol. PD JUN PY 2013 VL 132 IS 2 BP 81 EP 94 DI 10.1111/ivb.12015 PG 14 WC Marine & Freshwater Biology; Zoology SC Marine & Freshwater Biology; Zoology GA 157LH UT WOS:000319897100001 ER PT J AU Scarpignato, AL George, TL AF Scarpignato, Amy L. George, T. Luke TI Space use by Common Ravens in Marbled Murrelet nesting habitat in Northern California SO JOURNAL OF FIELD ORNITHOLOGY LA English DT Article DE Corvus corax; home range; home range overlap; resource use; resource utilization function ID WEST MOJAVE DESERT; STELLERS JAYS; POPULATION; PREDATION; CONSERVATION; DEMOGRAPHY; LANDSCAPE; SUCCESS; SEABIRD; SEX AB Little is known about space use by Common Ravens (Corvus corax) in coastal old-growth redwood (Sequoia sempervirens) forests in northern California despite their identification as nest predators of federally threatened Marbled Murrelets (Brachyramphus marmoratus). We used radio-telemetry to examine home range sizes and space use of breeding Common Ravens in Redwood National and State Parks (RNSP), California, in 2009 (N= 3) and 2010 (N= 8). Mean home range size was 182.5 ha and no home ranges were >2 km from roads or human-use areas. Ravens exhibited high site fidelity between years, and we found little overlap in the home ranges of adjacent ravens. Areas where ranges did overlap were centered on anthropogenic food sources near territory boundaries. Areas most frequently used by ravens were near roads, old-growth edge, bare ground, and in mixed hardwood and prairie habitats; areas near human-use areas and in old-growth habitat were used less by ravens. Mean perch height of ravens (52 m, N= 38) in redwood trees was similar to the mean height of Marbled Murrelet nests in RNSP (48 m). In RNSP, Marbled Murrelet nests that have been located were in old-growth forest within 2 km of roads. The attraction to anthropogenic resources with frequent use of roads and old-growth edges and their tendency to perch high in the canopy may increase the likelihood of ravens locating and predating nests of murrelets in RNSP. C1 [Scarpignato, Amy L.; George, T. Luke] Humboldt State Univ, Dept Wildlife, Arcata, CA 95521 USA. RP Scarpignato, AL (reprint author), Smithsonian Conservat Biol Inst, Migratory Bird Ctr, Natl Zool Pk, Washington, DC 20008 USA. EM amyscarp@gmail.com FU Wright Family FX We thank D. Haines for trapping expertise and CORA crews in 2009 and 2010 for data collection. We also thank the Wright Family for providing funding, the National Park Service, K. Bensen, and California State Parks for access to study sites, K. Sesser, B. Kertson, C. Rittenhouse, and J. Marzluff for help with statistical analysis, and M. Colwell, R. Golightly, three anonymous reviewers, and the editor for comments and suggestions that greatly improved our manuscript. All capture and handling methods were approved by the Humboldt State University Institutional Animal Care and Use Committee (IACUC no. 08/09.W.64.A). NR 56 TC 6 Z9 6 U1 5 U2 31 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0273-8570 J9 J FIELD ORNITHOL JI J. Field Ornithol. PD JUN PY 2013 VL 84 IS 2 BP 147 EP 159 DI 10.1111/jofo.12013 PG 13 WC Ornithology SC Zoology GA 151QU UT WOS:000319476100003 ER PT J AU Mawdsley, JR AF Mawdsley, Jonathan R. TI Taxonomy of the Goliath beetle Goliathus orientalis Moser, 1909 (Coleoptera: Scarabaeidae: Cetoniinae) SO JOURNAL OF NATURAL HISTORY LA English DT Article DE Scarabaeidae; Cetoniinae; taxonomy; Goliath beetle; Africa AB The 16 names proposed for the central and eastern African Goliath beetle Goliathus orientalis Moser, 1909, are reviewed and a complete synonymy is presented for the species. The earliest published name is Goliathus giganteus orientalis Moser, 1909, type locality Lindi, Deutsch-Ostafrika, and so the correct name for the species is Goliathus orientalis Moser, 1909. Goliathus meleagris Sjostedt, 1927a, type locality Katanga, Congo Belge, is a synonym of G.orientalis. Populations of G.orientalis in the Usambara Mountains, Tanzania, may represent a distinct subspecies. The correct subspecific name for this form would be G.orientalis usambarensis Preiss, 1933; the widely used name G.orientalis preissi Endrodi, 1951, is a junior subjective synonym of G.o.usambarensis Preiss. Goliathus orientalis is re-described and characters are presented for separation of adults of G.orientalis from adults of the partially sympatric species Goliathus goliatus (L.), 1771 and Goliathus albosignatus Boheman, 1857. C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol, Washington, DC 20560 USA. RP Mawdsley, JR (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol, Washington, DC 20560 USA. EM mawdsley@heinzctr.org NR 20 TC 1 Z9 1 U1 3 U2 17 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. PD JUN 1 PY 2013 VL 47 IS 21-22 BP 1451 EP 1461 DI 10.1080/00222933.2012.763052 PG 11 WC Biodiversity Conservation; Ecology SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 159WG UT WOS:000320077400004 ER PT J AU Adey, WH Laughinghouse, HD Miller, JB Hayek, LAC Thompson, JG Bertman, S Hampel, K Puvanendran, S AF Adey, Walter H. Laughinghouse, H. Dail Miller, John B. Hayek, Lee-Ann C. Thompson, Jesse G. Bertman, Steven Hampel, Kristin Puvanendran, Shanmugam TI Algal turf scrubber (ATS) floways on the Great Wicomico River, Chesapeake Bay: productivity, algal community structure, substrate and chemistry SO JOURNAL OF PHYCOLOGY LA English DT Article DE Algal Turf Scrubber (R); biochemistry; nutrient removal; productivity enhancement; species composition ID PHOSPHORUS; LIGHT; POLYSACCHARIDES; MICROALGAE; NUTRIENTS; BIOFUEL; CARBON AB Two Algal Turf Scrubber (ATS) units were deployed on the Great Wicomico River (GWR) for 22months to examine the role of substrate in increasing algal productivity and nutrient removal. The yearly mean productivity of flat ATS screens was 15.4 g center dot m-2 center dot d-1. This was elevated to 39.6g center dot m-2 center dot d-1 with a three-dimensional (3-D) screen, and to 47.7g center dot m-2 center dot d-1 by avoiding high summer harvest temperatures. These methods enhanced nutrient removal (N, P) in algal biomass by 3.5 times. Eighty-six algal taxa (Ochrophyta [diatoms], Chlorophyta [green algae], and Cyan-obacteria [blue-green algae]) self-seeded from the GWR and demonstrated yearly cycling. Silica (SiO2) content of the algal biomass ranged from 30% to 50% of total biomass; phosphorus, nitrogen, and carbon content of the total algal biomass ranged from 0.15% to 0.21%, 2.13% to 2.89%, and 20.0% to 25.7%, respectively. Carbohydrate content (at 10%-25% of AFDM) was dominated by glucose. Lipids (fatty acid methyl ester; FAMEs) ranged widely from 0.5% to 9% AFDM, with Omega-3 fatty acids a consistent component. Mathematical modeling of algal produ-ctivity as a function of temperature, light, and substrate showed a proportionality of 4:3:3, resp-ectively. Under landscape ATS operation, substrate manipulation provides a considerable opportunity to increase ATS productivity, water quality amelioration, and biomass coproduction for fertilizers, fermentation energy, and omega-3 products. Based on the 3-D prod-uctivity and algal chemical composition demonstrated, ATS systems used for nonpoint source water treat-ment can produce ethanol (butanol) at 5.8x per unit area of corn, and biodiesel at 12.0x per unit area of soy beans (agricultural production US). C1 [Adey, Walter H.; Laughinghouse, H. Dail] Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, Washington, DC 20013 USA. [Miller, John B.; Thompson, Jesse G.; Bertman, Steven; Hampel, Kristin; Puvanendran, Shanmugam] Western Michigan Univ, Chem Dept MS5413, Kalamazoo, MI 49008 USA. [Hayek, Lee-Ann C.] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA. RP Adey, WH (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, Washington, DC 20013 USA. EM adeyw@si.edu RI Laughinghouse, Haywood/M-5836-2016 OI Laughinghouse, Haywood/0000-0003-1018-6948 FU U.S. Department of Energy [DE-FG3608GO88049]; Smithsonian Institution [T08CC10068]; Virginia Institute of Marine Science [77263B/12683] FX Floway construction, operation, data collection, and algal analyses in this study were made possible by funding from HydroMentia, Ecological Systems Technology, The Lewis Foundation, Smithsonian Institution, and Statoil through the Virginia Institute of Marine Science. Chemical analyses were supported, in part, by funding from the U.S. Department of Energy (DE-FG3608GO88049), the Smithsonian Institution (T08CC10068), and the Virginia Institute of Marine Science (77263B/12683). We are grateful for discussions with Patrick Kangas of the University of Maryland, and Emmett Duffy and Elizabeth Canuel of the Virginia Institute of Marine Science. We thank the staff of InterfaceFLOR for their considerable efforts to simulate a manufactured version of the 3-D screen. E. Adey built the two floways studied, carried out many of the harvests, and participated in data analysis. J. Barker worked to provide excellent manuscript production. NR 32 TC 14 Z9 14 U1 4 U2 50 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0022-3646 J9 J PHYCOL JI J. Phycol. PD JUN PY 2013 VL 49 IS 3 BP 489 EP 501 DI 10.1111/jpy.12056 PG 13 WC Plant Sciences; Marine & Freshwater Biology SC Plant Sciences; Marine & Freshwater Biology GA 157DB UT WOS:000319874900007 PM 27007038 ER PT J AU Turner, BL Condron, LM AF Turner, Benjamin L. Condron, Leo M. TI Pedogenesis, nutrient dynamics, and ecosystem development: the legacy of TW Walker and JK Syers SO PLANT AND SOIL LA English DT Editorial Material ID WIND-BLOWN SAND; LONG-TERM CHRONOSEQUENCES; TEMPERATE RAIN-FOREST; NEW-ZEALAND; PHOSPHORUS TRANSFORMATIONS; ORGANIC PHOSPHORUS; SOIL DEVELOPMENT; INORGANIC PHOSPHORUS; CHRONO-TOPOSEQUENCE; FRACTIONATION C1 [Turner, Benjamin L.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. [Condron, Leo M.] Lincoln Univ, Christchurch, New Zealand. RP Turner, BL (reprint author), Smithsonian Trop Res Inst, Apartado 0843-03092, Balboa, Ancon, Panama. EM TurnerBL@si.edu RI Turner, Benjamin/E-5940-2011 OI Turner, Benjamin/0000-0002-6585-0722 NR 56 TC 14 Z9 14 U1 1 U2 72 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0032-079X J9 PLANT SOIL JI Plant Soil PD JUN PY 2013 VL 367 IS 1-2 BP 1 EP 10 DI 10.1007/s11104-013-1750-9 PG 10 WC Agronomy; Plant Sciences; Soil Science SC Agriculture; Plant Sciences GA 155TS UT WOS:000319771700001 ER PT J AU Celi, L Cerli, C Turner, BL Santoni, S Bonifacio, E AF Celi, L. Cerli, C. Turner, B. L. Santoni, S. Bonifacio, E. TI Biogeochemical cycling of soil phosphorus during natural revegetation of Pinus sylvestris on disused sand quarries in Northwestern Russia SO PLANT AND SOIL LA English DT Article DE Soil restoration; Carbon; Nitrogen; Chronosequence; Limiting nutrient ID MITIGATE CLIMATE-CHANGE; ORGANIC PHOSPHORUS; CARBON SEQUESTRATION; NUTRIENT DYNAMICS; DOUGLAS-FIR; NEW-ZEALAND; MINE SOILS; CHRONOSEQUENCE; PEDOGENESIS; MATTER AB Quarrying causes severe degradation of soils and vegetation that can be recovered partially when the quarries are abandoned and re-colonised by plants. To understand the recovery of soil functionality and nutrient cycling, we studied the development of soil phosphorus pools during Scots pine (Pinus sylvestris) revegetation in a disused sand quarry in Northwestern Russia. Sites that had been developing for different times since abandonment were compared to the parent sand and an adjacent undisturbed forest. Phosphorus speciation in genetic horizons of soil profiles was determined by sequential fractionation and solution phosphorus-31 nuclear magnetic resonance spectroscopy. Rapid transformations in soil properties occurred in 40 years, with a marked decline in pH and an accumulation of organic matter. Phosphorus transformations were shaped by geochemical processes, with a rapid release of inorganic phosphorus from primary minerals and accumulation of organic phosphorus to concentrations exceeding those found in the undisturbed site. Adsorbed and/or precipitated phosphorus increased rapidly, despite few reactive mineral colloidal surfaces. Natural succession of Scots pine in post-mining landscapes promotes ecosystem restoration through the rapid re-establishment of the biogeochemical cycles of organic matter and phosphorus. This study provides an important example of biogeochemical phosphorus cycling during the initial stages of pedogenesis. C1 [Celi, L.; Santoni, S.; Bonifacio, E.] Univ Turin, Dept Agr Forestry & Food Sci, I-10095 Turin, Italy. [Cerli, C.] Univ Amsterdam, IBED ESS, NL-1098 XH Amsterdam, Netherlands. [Turner, B. L.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. RP Celi, L (reprint author), Univ Turin, Dept Agr Forestry & Food Sci, Via Leonardo da Vinci 44, I-10095 Turin, Italy. EM luisella.celi@unito.it RI Turner, Benjamin/E-5940-2011; OI Turner, Benjamin/0000-0002-6585-0722; Bonifacio, Eleonora/0000-0003-3488-672X FU EU-INCO [013388] FX We thank Evgeniy V. Abakumov for field support and useful discussion of the Staraja Maluxa spoil-bank quarry sites. We thank also Antonio Gandino for laboratory analysis. This work was funded by the EU-INCO project no 013388. NR 70 TC 9 Z9 10 U1 3 U2 55 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0032-079X J9 PLANT SOIL JI Plant Soil PD JUN PY 2013 VL 367 IS 1-2 BP 121 EP 134 DI 10.1007/s11104-013-1627-y PG 14 WC Agronomy; Plant Sciences; Soil Science SC Agriculture; Plant Sciences GA 155TS UT WOS:000319771700008 ER PT J AU Turner, BL Lambers, H Condron, LM Cramer, MD Leake, JR Richardson, AE Smith, SE AF Turner, Benjamin L. Lambers, Hans Condron, Leo M. Cramer, Michael D. Leake, Jonathan R. Richardson, Alan E. Smith, Sally E. TI Soil microbial biomass and the fate of phosphorus during long-term ecosystem development SO PLANT AND SOIL LA English DT Article DE Chronosequence; Franz Josef; Microbial biomass; Phosphorus; Soil ID TEMPERATE RAIN-FOREST; NEW-ZEALAND; COMMUNITY COMPOSITION; EXTRACTION METHOD; TROPICAL FOREST; CHRONOSEQUENCE; CARBON; NITROGEN; RETROGRESSION; AVAILABILITY AB Soil phosphorus availability declines during long-term ecosystem development on stable land surfaces due to a gradual loss of phosphorus in runoff and transformation of primary mineral phosphate into secondary minerals and organic compounds. These changes have been linked to a reduction in plant biomass as ecosystems age, but the implications for belowground organisms remain unknown. We constructed a phosphorus budget for the well-studied 120,000 year temperate rainforest chronosequence at Franz Josef, New Zealand. The budget included the amounts of phosphorus in plant biomass, soil microbial biomass, and other soil pools. Soil microbes contained 68-78 % of the total biomass phosphorus (i.e. plant plus microbial) for the majority of the 120,000 year chronosequence. In contrast, plant phosphorus was a relatively small pool that occurred predominantly in wood. This points to the central role of the microbial biomass in determining phosphorus availability as ecosystems mature, yet also indicates the likelihood of strong competition between plants and saprotrophic microbes for soil phosphorus. This novel perspective on terrestrial biogeochemistry challenges our understanding of phosphorus cycling by identifying soil microbes as the major biological phosphorus pool during long-term ecosystem development. C1 [Turner, Benjamin L.] Smithsonian Trop Res Inst Apartado, Balboa 084303092, Ancon, Panama. [Turner, Benjamin L.; Lambers, Hans; Cramer, Michael D.; Richardson, Alan E.] Univ Western Australia, Sch Plant Biol, Crawley, WA 6009, Australia. [Condron, Leo M.] Lincoln Univ, Canterbury 7647, New Zealand. [Cramer, Michael D.] Univ Cape Town, Dept Bot, ZA-7700 Rondebosch, South Africa. [Leake, Jonathan R.] Univ Sheffield, Dept Anim & Plant Sci, Sheffield S10 2TN, S Yorkshire, England. [Richardson, Alan E.] CSIRO Plant Ind, Canberra, ACT 2601, Australia. [Smith, Sally E.] Univ Adelaide, Sch Agr Food & Wine, Adelaide, SA 5005, Australia. RP Turner, BL (reprint author), Smithsonian Trop Res Inst Apartado, Balboa 084303092, Ancon, Panama. EM TurnerBL@si.edu RI Turner, Benjamin/E-5940-2011; Richardson, Alan/I-1903-2012; Cramer, Michael/A-3213-2013; Lambers, Hans/A-1544-2008; OI Turner, Benjamin/0000-0002-6585-0722; Cramer, Michael/0000-0003-0989-3266; Lambers, Hans/0000-0002-4118-2272; Leake, Jonathan/0000-0001-8364-7616 NR 55 TC 32 Z9 34 U1 18 U2 199 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0032-079X EI 1573-5036 J9 PLANT SOIL JI Plant Soil PD JUN PY 2013 VL 367 IS 1-2 BP 225 EP 234 DI 10.1007/s11104-012-1493-z PG 10 WC Agronomy; Plant Sciences; Soil Science SC Agriculture; Plant Sciences GA 155TS UT WOS:000319771700015 ER PT J AU Jangid, K Whitman, WB Condron, LM Turner, BL Williams, MA AF Jangid, Kamlesh Whitman, William B. Condron, Leo M. Turner, Benjamin L. Williams, Mark A. TI Progressive and retrogressive ecosystem development coincide with soil bacterial community change in a dune system under lowland temperate rainforest in New Zealand SO PLANT AND SOIL LA English DT Article DE Bacterial diversity; Haast chronosequence; Pedogenesis; Soil nutrients; Vegetative succession; 16S rRNA pyrosequencing ID MICROBIAL COMMUNITIES; PALEOSEISMIC ACTIVITY; CHRONOSEQUENCE; PHOSPHORUS; SUCCESSION; DIVERSITY; PEDOGENESIS; DYNAMICS; GLACIER; LIMITATION AB It is established that plant communities show patterns of change linked to progressive and retrogressive stages of ecosystem development. It is not known, however, whether bacterial communities also show similar patterns of change associated with long-term ecosystem development. We studied soil bacterial communities along a 6,500 year dune chronosequence under lowland temperate rain forest at Haast, New Zealand. Pyrosequencing of 16S rRNA genes was used to observe structural change in bacterial communities during the process of pedogenesis and ecosystem development. Bacterial communities showed patterns of change during pedogenesis, with the largest change during the first several hundred years after dune stabilization. The most abundant bacterial taxa were Alphaproteobacteria, Actinobacteria and Acidobacteria. These include taxa most closely related to nitrogen-fixing bacteria, and suggest heterotrophic nitrogen input may be important throughout the chronosequence. Changes in bacterial community structure were related to changes in several soil properties, including total phosphorus, C:N ratio, and pH. The Bacteroidetes, Actinobacteria, Cyanobacteria, Firmicutes, and Betaproteobacteria all showed a general decline in abundance as pedogenesis proceeded, while Acidobacteria, Alphaproteobacteria, and Plantctomycetes tended to increase as soils aged. There were trends in the dynamics of bacterial community composition and structure in soil during ecosystem development. Bacterial communities changed in ways that appear to be consistent with a model of ecosystem progression and retrogression, perhaps indicating fundamental processes underpin patterns of below and above-ground community change during ecosystem development. C1 [Jangid, Kamlesh] Natl Ctr Cell Sci, Pune 411007, Maharashtra, India. [Whitman, William B.] Univ Georgia, Dept Microbiol, Athens, GA 30602 USA. [Condron, Leo M.] Lincoln Univ, Canterbury 7647, New Zealand. [Turner, Benjamin L.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. [Williams, Mark A.] Virginia Polytech & State Univ, Coll Agr & Life Sci, Blacksburg, VA 24060 USA. RP Williams, MA (reprint author), Virginia Polytech & State Univ, Coll Agr & Life Sci, 301 Latham Hall, Blacksburg, VA 24060 USA. EM markwill@vt.edu RI Turner, Benjamin/E-5940-2011 OI Turner, Benjamin/0000-0002-6585-0722 FU National Science Foundation [1216074] FX Thank you to Shankar Shanmugam who helped to create graphs and tables presented in this article. This material is based upon work supported by the National Science Foundation under Grant No. (1216074). NR 50 TC 11 Z9 12 U1 2 U2 45 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0032-079X J9 PLANT SOIL JI Plant Soil PD JUN PY 2013 VL 367 IS 1-2 BP 235 EP 247 DI 10.1007/s11104-013-1720-2 PG 13 WC Agronomy; Plant Sciences; Soil Science SC Agriculture; Plant Sciences GA 155TS UT WOS:000319771700016 ER PT J AU Bridges, N Geissler, P Silvestro, S Banks, M AF Bridges, Nathan Geissler, Paul Silvestro, Simone Banks, Maria TI Bedform migration on Mars: Current results and future plans SO AEOLIAN RESEARCH LA English DT Review DE Mars; Dunes; Ripples; Bedforms; Change detection; Sand flux ID NORTH POLAR-REGION; TRANSVERSE AEOLIAN RIDGES; MERIDIANI-PLANUM; SAND DUNES; ORBITER CAMERA; LANDING SITE; TRANSPORT PATHWAYS; OMEGA/MARS EXPRESS; LONGITUDINAL DUNES; SURFACE-ROUGHNESS AB With the advent of high resolution imaging, bedform motion can now be tracked on the Martian surface. HiRISE data, with a pixel scale as fine as 25 cm, shows displacements of sand patches, dunes, and ripples up to several meters per Earth year, demonstrating that significant landscape modification occurs in the current environment. This seems to consistently occur in the north polar erg, with variable activity at other latitudes. Volumetric dune and ripple changes indicate sand fluxes up to several cubic meters per meter per year, similar to that found in some dune fields on Earth. All "transverse aeolian ridges" are immobile. There is no relationship between bedform activity and coarse-scale global circulation models, indicating that finer scale topography and wind gusts, combined with the predicted low impact threshold on Mars, are the primary drivers. Several techniques have been developed to measure bedform changes and are largely dependent on dataset availability and the type of questions being pursued. Qualitative visual inspection can determine whether or not changes have occurred. Offsets registered to fixed tie points yield approximate migration rates of nearby crests and dune lee fronts. To compute volumetric sand flux requires precise orthorectification and registration using a digital elevation model base. Using this technique combined with sophisticated change detection software has the potential to detect changes as fine as 1/3 of a pixel (similar to 8 cm) or less. (C) 2013 Elsevier B.V. All rights reserved. C1 [Bridges, Nathan] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. [Geissler, Paul] US Geol Survey, Astrogeol Sci Ctr, Flagstaff, AZ 86001 USA. [Silvestro, Simone] SETI Inst, Mountain View, CA 94043 USA. [Banks, Maria] Smithsonian Natl Air & Space Museum, Ctr Earth & Planetary Studies, Washington, DC 20013 USA. RP Bridges, N (reprint author), Johns Hopkins Univ, Appl Phys Lab, 200-W230,11100 Johns Hopkins Rd, Laurel, MD 20723 USA. EM nathan.bridges@jhuapl.edu FU Mars Reconnaissance Orbiter Project; NASA's Mars Data Analysis Program [NNH11ZDA001N, NNH09ZDA001N] FX Detailed reviews by Mary Bourke, Matthew Chojnacki, and an anonymous reviewer substantially improved the manuscript and are gratefully acknowledged. Bradley Thomson computed the threshold frequencies from the Ames GCM, as shown in Fig. 8. Support to NTB for this research was provided the Mars Reconnaissance Orbiter Project (HiRISE co-investigator) and NASA's Mars Data Analysis Program (NNH11ZDA001N). S. Silvestro is supported by a grant from the NASA's Mars Data Analysis Program (NNH09ZDA001N). NR 143 TC 15 Z9 15 U1 4 U2 25 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 1875-9637 J9 AEOLIAN RES JI Aeolian Res. PD JUN PY 2013 VL 9 BP 133 EP 151 DI 10.1016/j.aeolia.2013.02.004 PG 19 WC Geography, Physical SC Physical Geography GA 153WF UT WOS:000319632500011 ER PT J AU Zotz, G AF Zotz, Gerhard TI Hemiepiphyte: a confusing term and its history SO ANNALS OF BOTANY LA English DT Editorial Material ID VASCULAR EPIPHYTES; RAIN-FOREST; VERTICAL-DISTRIBUTION; INCLUDING HEMIEPIPHYTES; HYDRAULIC ARCHITECTURE; AERIAL ROOTS; DIVERSITY; GROWTH; ARACEAE; EVOLUTION AB Over more than 120 years of scientific study since Schimpers seminal work, the recognized categories of structurally dependent plants have changed several times. Currently, ignoring parasitic mistletoes, it is usual to distinguish four functional groups: (1) true epiphytes; (2) primary hemiepiphytes; (3) secondary hemiepiphytes; and (4) climbing plants, i.e. lianas and vines. In this Viewpoint, it is argued that the term secondary hemiepiphytes (SHs) is misleading, that its definition is hard to impossible to apply in the field and, possibly causally related to this conceptual problem, that the use of this category in field studies is inconsistent, which now hampers interpretation and generalization. Categories will frequently fail to capture gradual biological variation, but terms and concepts should be as unambiguous as possible to facilitate productive communication. A detailed analysis of the conceptual problems associated with the term SH and its application in scientific studies clearly shows that this goal is not fulfilled in this case. Consequently, the use of SH should be abandoned. An alternative scheme to categorize structurally dependent flora is suggested. C1 [Zotz, Gerhard] Carl von Ossietzky Univ Oldenburg, Inst Biol & Environm Sci, Funct Ecol Grp, D-26111 Oldenburg, Germany. [Zotz, Gerhard] Smithsonian Trop Res Inst, Panama City, Panama. RP Zotz, G (reprint author), Carl von Ossietzky Univ Oldenburg, Inst Biol & Environm Sci, Funct Ecol Grp, Box 2503, D-26111 Oldenburg, Germany. EM gerhard.zotz@uni-oldenburg.de NR 62 TC 26 Z9 29 U1 1 U2 36 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0305-7364 J9 ANN BOT-LONDON JI Ann. Bot. PD JUN PY 2013 VL 111 IS 6 BP 1015 EP 1020 DI 10.1093/aob/mct085 PG 6 WC Plant Sciences SC Plant Sciences GA 151AP UT WOS:000319433300001 PM 23589630 ER PT J AU Aylward, FO Burnum-Johnson, KE Tringe, SG Teiling, C Tremmel, DM Moeller, JA Scott, JJ Barry, KW Piehowski, PD Nicora, CD Malfatti, SA Monroe, ME Purvine, SO Goodwin, LA Smith, RD Weinstock, GM Gerardo, NM Suen, G Lipton, MS Currie, CR AF Aylward, Frank O. Burnum-Johnson, Kristin E. Tringe, Susannah G. Teiling, Clotilde Tremmel, Daniel M. Moeller, Joseph A. Scott, Jarrod J. Barry, Kerrie W. Piehowski, Paul D. Nicora, Carrie D. Malfatti, Stephanie A. Monroe, Matthew E. Purvine, Samuel O. Goodwin, Lynne A. Smith, Richard D. Weinstock, George M. Gerardo, Nicole M. Suen, Garret Lipton, Mary S. Currie, Cameron R. TI Leucoagaricus gongylophorus Produces Diverse Enzymes for the Degradation of Recalcitrant Plant Polymers in Leaf-Cutter Ant Fungus Gardens SO APPLIED AND ENVIRONMENTAL MICROBIOLOGY LA English DT Article ID ATTA-SEXDENS-RUBROPILOSA; CUTTING ANTS; SYMBIOTIC FUNGUS; PROTEIN DATABASE; GROWING ANTS; CELLULOSE; ANNOTATION; EVOLUTION; ECOLOGY; COMMUNITIES AB Plants represent a large reservoir of organic carbon comprised primarily of recalcitrant polymers that most metazoans are unable to deconstruct. Many herbivores gain access to nutrients in this material indirectly by associating with microbial symbionts, and leaf-cutter ants are a paradigmatic example. These ants use fresh foliar biomass as manure to cultivate gardens composed primarily of Leucoagaricus gongylophorus, a basidiomycetous fungus that produces specialized hyphal swellings that serve as a food source for the host ant colony. Although leaf-cutter ants are conspicuous herbivores that contribute substantially to carbon turnover in Neotropical ecosystems, the process through which plant biomass is degraded in their fungus gardens is not well understood. Here we present the first draft genome of L. gongylophorus, and, using genomic and metaproteomic tools, we investigate its role in lignocellulose degradation in the gardens of both Atta cephalotes and Acromyrmex echinatior leaf-cutter ants. We show that L. gongylophorus produces a diversity of lignocellulases in ant gardens and is likely the primary driver of plant biomass degradation in these ecosystems. We also show that this fungus produces distinct sets of lignocellulases throughout the different stages of biomass degradation, including numerous cellulases and laccases that likely play an important role in lignocellulose degradation. Our study provides a detailed analysis of plant biomass degradation in leaf-cutter ant fungus gardens and insight into the enzymes underlying the symbiosis between these dominant herbivores and their obligate fungal cultivar. C1 [Aylward, Frank O.; Tremmel, Daniel M.; Moeller, Joseph A.; Scott, Jarrod J.; Suen, Garret; Currie, Cameron R.] Univ Wisconsin, Dept Bacteriol, Madison, WI 53706 USA. [Aylward, Frank O.; Moeller, Joseph A.; Scott, Jarrod J.; Currie, Cameron R.] Univ Wisconsin, Dept Energy Great Lakes Bioenergy, Res Ctr, Madison, WI 53706 USA. [Burnum-Johnson, Kristin E.; Piehowski, Paul D.; Nicora, Carrie D.; Monroe, Matthew E.; Purvine, Samuel O.; Smith, Richard D.; Lipton, Mary S.] Pacific NW Natl Lab, Div Biol Sci, Richland, WA 99352 USA. [Currie, Cameron R.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. [Tringe, Susannah G.; Barry, Kerrie W.; Malfatti, Stephanie A.; Goodwin, Lynne A.] Joint Genome Inst, Dept Energy, Walnut Creek, CA USA. [Gerardo, Nicole M.] Emory Univ, Dept Biol, Atlanta, GA 30322 USA. [Teiling, Clotilde] Roche Diagnost, Indianapolis, IN USA. [Weinstock, George M.] Washington Univ, Sch Med, Genome Ctr, St Louis, MO USA. RP Currie, CR (reprint author), Univ Wisconsin, Dept Bacteriol, Madison, WI 53706 USA. EM currie@bact.wisc.edu RI Piehowski, Paul/B-1108-2011; Smith, Richard/J-3664-2012; Burnum, Kristin/B-1308-2011; Lipton, Mary/H-3913-2012; OI Smith, Richard/0000-0002-2381-2349; Burnum, Kristin/0000-0002-2722-4149; Piehowski, Paul/0000-0001-5108-2227; Suen, Garret/0000-0002-6170-711X FU Roche 454 Life Sciences 10 GB grant; Office of Science of the U.S. Department of Energy [DE-AC02-05CH11231]; U.S. Department of Energy's (DOE) Office of Biological and Environmental Research (OBER) Pan-omics program at Pacific Northwest National Laboratory (PNNL); U.S. Department of Energy (DOE) Office of Biological and Environmental Research national scientific user facility on the PNNL campus; DOE [DE-AC05-76RL01830]; National Science Foundation [DEB-0747002, MCB-0702025, MCB-0731822]; DOE Great Lakes Bioenergy Research Center (DOE Office of Science BER) [DE-FC02-07ER64494] FX Fungal genome sequencing was supported by a Roche 454 Life Sciences 10 GB grant. The U.S. Department of Energy Joint Genome Institute effort was supported by the Office of Science of the U.S. Department of Energy under contract no. DE-AC02-05CH11231. Metaproteomics measurements were supported by the U.S. Department of Energy's (DOE) Office of Biological and Environmental Research (OBER) Pan-omics program at Pacific Northwest National Laboratory (PNNL) and performed in the Environmental Molecular Sciences Laboratory, a U.S. Department of Energy (DOE) Office of Biological and Environmental Research national scientific user facility on the PNNL campus. PNNL is a multiprogram national laboratory operated by Battelle for the DOE under contract DE-AC05-76RL01830. This work was also supported by National Science Foundation grants DEB-0747002, MCB-0702025, and MCB-0731822 to C.R.C. and the DOE Great Lakes Bioenergy Research Center (DOE Office of Science BER DE-FC02-07ER64494). NR 60 TC 31 Z9 31 U1 9 U2 100 PU AMER SOC MICROBIOLOGY PI WASHINGTON PA 1752 N ST NW, WASHINGTON, DC 20036-2904 USA SN 0099-2240 J9 APPL ENVIRON MICROB JI Appl. Environ. Microbiol. PD JUN PY 2013 VL 79 IS 12 BP 3770 EP 3778 DI 10.1128/AEM.03833-12 PG 9 WC Biotechnology & Applied Microbiology; Microbiology SC Biotechnology & Applied Microbiology; Microbiology GA 152CO UT WOS:000319507700026 PM 23584789 ER PT J AU Spezzano, S Brunken, S Schilke, P Caselli, P Menten, KM McCarthy, MC Bizzocchi, L Trevino-Morales, SP Aikawa, Y Schlemmer, S AF Spezzano, S. Bruenken, S. Schilke, P. Caselli, P. Menten, K. M. McCarthy, M. C. Bizzocchi, L. Trevino-Morales, S. P. Aikawa, Y. Schlemmer, S. TI INTERSTELLAR DETECTION OF c-C3D2 SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE ISM: molecules; line: identification; molecular data; molecular processes ID DEUTERIUM FRACTIONATION; DEUTERATED AMMONIA; SURFACE-CHEMISTRY; PRESTELLAR CORES; STARLESS CORES; C3H2; CLOUDS; COLD; CYCLOPROPENYLIDENE; MOLECULES AB We report the first interstellar detection of c-C3D2. Doubly deuterated cyclopropenylidene, a carbene, has been detected toward the starless cores TMC-1C and L1544 using the IRAM 30 m telescope. The J(Ka), (Kc) = 3(0,3)-2(1,2), 3(1,3)-2(0,2), and 2(2,1)-1(1,0) transitions of this species have been observed at 3 mm in both sources. The expected 1: 2 intensity ratio has been found in the 3(0,3)-2(1,2) and 3(1,3)-2(0,2) lines, belonging to the para and ortho species, respectively. We also observed lines of the main species, c-C3H2, singly deuterated c-C3HD, and the species with one C-13 off of the principal axis of the molecule, c-(HCC2H)-C-13. The lines of c-C3D2 have been observed with high signal-to-noise ratio, better than 7.5 sigma in TMC-1C and 9 sigma in L1544. The abundance of doubly deuterated cyclopropenylidene with respect to the normal species is found to be 0.4%-0.8% in TMC-1C and 1.2%-2.1% in L1544. The deuteration of this small hydrocarbon ring is analyzed with a comprehensive gas-grain model, the first including doubly deuterated species. The observed abundances of c-C3D2 can be explained solely by gas-phase processes, supporting the idea that c-C3H2 is a good indicator of gas-phase deuteration. C1 [Spezzano, S.; Bruenken, S.; Schilke, P.; Schlemmer, S.] Univ Cologne, Inst Phys, D-50937 Cologne, Germany. [Spezzano, S.; Menten, K. M.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Caselli, P.] Univ Leeds, Sch Phys & Astron, Leeds LS2 9JT, W Yorkshire, England. [McCarthy, M. C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [McCarthy, M. C.] Harvard Univ, Sch Engn & Appl Sci, Cambridge, MA 02138 USA. [Bizzocchi, L.] Observ Astron Lisboa, Ctr Astron & Astrofis, P-1349018 Lisbon, Portugal. [Trevino-Morales, S. P.] IRAM, E-18012 Granada, Spain. [Aikawa, Y.] Kobe Univ, Dept Earth & Planetary Sci, Kobe, Hyogo 6578501, Japan. RP Spezzano, S (reprint author), Univ Cologne, Inst Phys, Zulpicher Str 77, D-50937 Cologne, Germany. RI Brunken, Sandra/B-1880-2010; Schlemmer, Stephan/E-2903-2015; OI Brunken, Sandra/0000-0001-7175-4828; Schlemmer, Stephan/0000-0002-1421-7281; Bizzocchi, Luca/0000-0002-9953-8593; McCarthy, Michael/0000-0001-9142-0008 FU International Max-Planck Research School (IMPRS) for Astronomy and Astrophysics at the University of Bonn; Deutsche Forschungsgemeinschaft (DFG) [BR 4287/1-1]; Science and Technology Foundation (FCT, Portugal) [SFRH/BPD/62966/2009]; International Max-Planck Research School (IMPRS) for Astronomy and Astrophysics at the University of Cologne; [SFB956] FX The authors thank the referee for useful comments. This work has been supported by SFB956. S. Spezzano has been supported in her research with a stipend from the International Max-Planck Research School (IMPRS) for Astronomy and Astrophysics at the Universities of Bonn and Cologne. S. Schlemmer and S. B. acknowledge support by the Deutsche Forschungsgemeinschaft (DFG) through project BR 4287/1-1. L. B. acknowledges support from the Science and Technology Foundation (FCT, Portugal) through the Fellowship SFRH/BPD/62966/2009, and he is grateful to the SFB956 for the travel allowance. NR 50 TC 9 Z9 9 U1 3 U2 14 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 EI 2041-8213 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD JUN 1 PY 2013 VL 769 IS 2 AR UNSP L19 DI 10.1088/2041-8205/769/2/L19 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 151JR UT WOS:000319457300001 ER PT J AU Hietz, P Valencia, R Wright, SJ AF Hietz, Peter Valencia, Renato Joseph Wright, S. TI Strong radial variation in wood density follows a uniform pattern in two neotropical rain forests SO FUNCTIONAL ECOLOGY LA English DT Article DE biomass estimate; biomechanics; phylogenetic signal; radial wood density gradient; tropical rain forest; wood function AB Wood density (WD) affects plant biomechanics, drought and decay resistance. As a consequence, WD is an important functional trait related to plant demography and ecosystem processes, which is also used to estimate tree biomass. Radial variation in WD (changes from the centre of the stem to the cambium) affects the strength of the entire stem, but also reflects any changes in wood functional properties that might occur during a tree's lifetime. To understand how WD and radial WD gradients, which were defined as the slope of the relationship between WD and distance to the centre, are related to demographic traits of species, we investigated WD in 335 tree species from a Panamanian moist forest and 501 species from an Ecuadorian rain forest and radial density gradients in 118 and 186 species, respectively, and compared WD with tree growth, mortality and size. WD was negatively related to tree growth and mortality. WD tended to increase towards the outside in trees with low initial density and to decrease towards the outside in trees with high initial density. Radial WD gradients were largely unrelated to tree size and demographic traits, but some families had higher or lower WD gradients at a given inner WD. Inner WD was by far the best predictor of radial WD gradients (r2=0 center dot 39 for Panama and 0 center dot 45 for Ecuador) and this relationship was indistinguishable between the two rain forests. This suggests a broadly uniform function of WD variation, likely responding to mechanical requirements during ontogeny. We discuss the factors potentially driving radial increases or decreases in WD and suggest ways to elucidate the relative importance of tree mechanics, hydraulic safety or decay resistance. We also discuss that not accounting for radial WD gradients may result in substantial errors in WD of the whole stem and consequently biomass estimates, and recommend sampling density gradients when obtaining density data from tree cores. C1 [Hietz, Peter] Univ Nat Resources & Life Sci, Inst Bot, A-1180 Vienna, Austria. [Valencia, Renato] Pontificia Univ Catolica Ecuador, Escuela Ciencias Biol, Lab Ecol Plantas, Quito, Ecuador. [Joseph Wright, S.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. RP Hietz, P (reprint author), Univ Nat Resources & Life Sci, Inst Bot, Gregor Mendel Str 33, A-1180 Vienna, Austria. EM peter.hietz@boku.ac.at RI Wright, Stuart/M-3311-2013; OI Wright, Stuart/0000-0003-4260-5676; Hietz, Peter/0000-0002-0458-6593 FU F. H. Levinson Fund; Austrian Science Fund [FWF P19507-B17] FX The F. H. Levinson Fund funded the collection of wood samples. Javier Ballesteros, Salomon Aguilar and Rolando Perez collected wood samples in Panama. Pablo Alvia and Milton Zambrano collected wood samples in Ecuador. PH was supported by the Austrian Science Fund (FWF P19507-B17). We thank the editor and an anonymous reviewer for their helpful comments. NR 0 TC 12 Z9 12 U1 2 U2 38 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0269-8463 J9 FUNCT ECOL JI Funct. Ecol. PD JUN PY 2013 VL 27 IS 3 SI SI BP 684 EP 692 DI 10.1111/1365-2435.12085 PG 9 WC Ecology SC Environmental Sciences & Ecology GA 150VW UT WOS:000319420500011 ER PT J AU Hong, T Freeman, R AF Hong, Terry Freeman, Ru TI On Sal Mal Lane SO LIBRARY JOURNAL LA English DT Book Review C1 [Hong, Terry] Smithsonian BookDragon, Washington, DC USA. RP Hong, T (reprint author), Smithsonian BookDragon, Washington, DC USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU REED BUSINESS INFORMATION PI NEW YORK PA 360 PARK AVENUE SOUTH, NEW YORK, NY 10010 USA SN 0363-0277 J9 LIBR J JI Libr. J. PD JUN 1 PY 2013 VL 138 IS 10 BP 96 EP 97 PG 2 WC Information Science & Library Science SC Information Science & Library Science GA 156XC UT WOS:000319856200057 ER PT J AU Hong, T AF Hong, Terry TI Snow Hunters. SO LIBRARY JOURNAL LA English DT Book Review C1 [Hong, Terry] Smithsonian BookDragon, Washington, DC USA. RP Hong, T (reprint author), Smithsonian BookDragon, Washington, DC USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU REED BUSINESS INFORMATION PI NEW YORK PA 360 PARK AVENUE SOUTH, NEW YORK, NY 10010 USA SN 0363-0277 J9 LIBR J JI Libr. J. PD JUN 1 PY 2013 VL 138 IS 10 BP 104 EP 104 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA 156XC UT WOS:000319856200101 ER PT J AU Aiello, A AF Aiello, Annette TI Bug Music: How Insects Gave Us Rhythm and Noise SO LIBRARY JOURNAL LA English DT Book Review C1 [Aiello, Annette] Smithsonian Trop Res Inst, Balboa, Panama. RP Aiello, A (reprint author), Smithsonian Trop Res Inst, Balboa, Panama. NR 1 TC 0 Z9 0 U1 1 U2 3 PU REED BUSINESS INFORMATION PI NEW YORK PA 360 PARK AVENUE SOUTH, NEW YORK, NY 10010 USA SN 0363-0277 J9 LIBR J JI Libr. J. PD JUN 1 PY 2013 VL 138 IS 10 BP 130 EP 131 PG 2 WC Information Science & Library Science SC Information Science & Library Science GA 156XC UT WOS:000319856200203 ER PT J AU Gruppioni, C Pozzi, F Rodighiero, G Delvecchio, I Berta, S Pozzetti, L Zamorani, G Andreani, P Cimatti, A Ilbert, O Le Floc'h, E Lutz, D Magnelli, B Marchetti, L Monaco, P Nordon, R Oliver, S Popesso, P Riguccini, L Roseboom, I Rosario, DJ Sargent, M Vaccari, M Altieri, B Aussel, H Bongiovanni, A Cepa, J Daddi, E Dominguez-Sanchez, H Elbaz, D Schreiber, NF Genzel, R Iribarrem, A Magliocchetti, M Maiolino, R Poglitsch, A Garcia, AP Sanchez-Portal, M Sturm, E Tacconi, L Valtchanov, I Amblard, A Arumugam, V Bethermin, M Bock, J Boselli, A Buat, V Burgarella, D Castro-Rodriguez, N Cava, A Chanial, P Clements, DL Conley, A Cooray, A Dowell, CD Dwek, E Eales, S Franceschini, A Glenn, J Griffin, M Hatziminaoglou, E Ibar, E Isaak, K Ivison, RJ Lagache, G Levenson, L Lu, N Madden, S Maffei, B Mainetti, G Nguyen, HT O'Halloran, B Page, MJ Panuzzo, P Papageorgiou, A Pearson, CP Perez-Fournon, I Pohlen, M Rigopoulou, D Rowan-Robinson, M Schulz, B Scott, D Seymour, N Shupe, DL Smith, AJ Stevens, JA Symeonidis, M Trichas, M Tugwell, KE Vigroux, L Wang, L Wright, G Xu, CK Zemcov, M Bardelli, S Carollo, M Contini, T Le Fevre, O Lilly, S Mainieri, V Renzini, A Scodeggio, M Zucca, E AF Gruppioni, C. Pozzi, F. Rodighiero, G. Delvecchio, I. Berta, S. Pozzetti, L. Zamorani, G. Andreani, P. Cimatti, A. Ilbert, O. Le Floc'h, E. Lutz, D. Magnelli, B. Marchetti, L. Monaco, P. Nordon, R. Oliver, S. Popesso, P. Riguccini, L. Roseboom, I. Rosario, D. J. Sargent, M. Vaccari, M. Altieri, B. Aussel, H. Bongiovanni, A. Cepa, J. Daddi, E. Dominguez-Sanchez, H. Elbaz, D. Schreiber, N. Foerster Genzel, R. Iribarrem, A. Magliocchetti, M. Maiolino, R. Poglitsch, A. Perez Garcia, A. Sanchez-Portal, M. Sturm, E. Tacconi, L. Valtchanov, I. Amblard, A. Arumugam, V. Bethermin, M. Bock, J. Boselli, A. Buat, V. Burgarella, D. Castro-Rodriguez, N. Cava, A. Chanial, P. Clements, D. L. Conley, A. Cooray, A. Dowell, C. D. Dwek, E. Eales, S. Franceschini, A. Glenn, J. Griffin, M. Hatziminaoglou, E. Ibar, E. Isaak, K. Ivison, R. J. Lagache, G. Levenson, L. Lu, N. Madden, S. Maffei, B. Mainetti, G. Nguyen, H. T. O'Halloran, B. Page, M. J. Panuzzo, P. Papageorgiou, A. Pearson, C. P. Perez-Fournon, I. Pohlen, M. Rigopoulou, D. Rowan-Robinson, M. Schulz, B. Scott, D. Seymour, N. Shupe, D. L. Smith, A. J. Stevens, J. A. Symeonidis, M. Trichas, M. Tugwell, K. E. Vigroux, L. Wang, L. Wright, G. Xu, C. K. Zemcov, M. Bardelli, S. Carollo, M. Contini, T. Le Fevre, O. Lilly, S. Mainieri, V. Renzini, A. Scodeggio, M. Zucca, E. TI The Herschel* PEP/HerMES luminosity function - I. Probing the evolution of PACS selected Galaxies to z similar or equal to 4 SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies: active; galaxies: evolution; galaxies: luminosity function; mass function; galaxies: starburst; cosmology: observations; infrared: galaxies ID STAR-FORMING GALAXIES; DEEP-FIELD-SOUTH; ACTIVE GALACTIC NUCLEI; SPECTRAL ENERGY-DISTRIBUTIONS; SUPERMASSIVE BLACK-HOLES; REDSHIFT SURVEY; GOODS-SOUTH; MU-M; PHOTOMETRIC REDSHIFTS; FORMATION HISTORY AB We exploit the deep and extended far-IR data sets (at 70, 100 and 160 mu m) of the Herschel Guaranteed Time Observation (GTO) PACS Evolutionary Probe (PEP) Survey, in combination with the Herschel Multi-tiered Extragalactic Survey data at 250, 350 and 500 mu m, to derive the evolution of the rest-frame 35-, 60-, 90-and total infrared (IR) luminosity functions (LFs) up to z similar to 4. We detect very strong luminosity evolution for the total IR LF (L-IR alpha (1 + z)(3.55 +/- 0.10) up to z similar to 2, and. (1 + z) 1.62 similar to 0.51 at 2 < z less than or similar to 4) combined with a density evolution ( (1 + z)-0.57 +/- 0.22 up to z similar to 1 and. (1 + z)-3.92 +/- 0.34 at 1 < z less than or similar to 4). In agreement with previous findings, the IR luminosity density (.IR) increases steeply to z similar to 1, then flattens between z similar to 1 and z similar to 3 to decrease at z similar to 3. Galaxies with different spectral energy distributions, masses and specific star formation rates (SFRs) evolve in very different ways and this large and deep statistical sample is the first one allowing us to separately study the different evolutionary behaviours of the individual IR populations contributing to.IR. Galaxies occupying the well-established SFR-stellar mass main sequence (MS) are found to dominate both the total IR LF and.IR at all redshifts, with the contribution from off-MS sources (= 0.6 dex above MS) being nearly constant (similar to 20 per cent of the total IR) and showing no significant signs of increase with increasing z over the whole 0.8 < z < 2.2 range. Sources with mass in the range 10 = log(M/M-circle dot) = 11 are found to dominate the total IR LF, with more massive galaxies prevailing at the bright end of the high-z (greater than or similar to 2) LF. A two-fold evolutionary scheme for IR galaxies is envisaged: on the one hand, a starburst-dominated phase in which the Super Massive Black Holes (SMBH) grows and is obscured by dust (possibly triggered by a major merging event), is followed by an AGN-dominated phase, then evolving towards a local elliptical. On the other hand, moderately star-forming galaxies containing a low-luminosity AGN have various properties suggesting they are good candidates for systems in a transition phase preceding the formation of steady spiral galaxies. C1 [Gruppioni, C.; Pozzetti, L.; Zamorani, G.; Dominguez-Sanchez, H.; Bardelli, S.; Zucca, E.] INAF Osservatorio Astron Bologna, I-40127 Bologna, Italy. [Pozzi, F.; Delvecchio, I.; Cimatti, A.] Univ Bologna, Dipartimento Astron, I-40127 Bologna, Italy. [Rodighiero, G.; Marchetti, L.; Vaccari, M.; Franceschini, A.; Mainetti, G.] Univ Padua, Dipartimento Astron, I-35122 Padua, Italy. [Berta, S.; Lutz, D.; Magnelli, B.; Nordon, R.; Popesso, P.; Rosario, D. J.; Schreiber, N. Foerster; Genzel, R.; Poglitsch, A.; Sturm, E.; Tacconi, L.] Max Planck Inst Extraterr Phys MPE, D-85741 Garching, Germany. [Andreani, P.; Iribarrem, A.; Hatziminaoglou, E.; Mainieri, V.] ESO, D-85748 Garching, Germany. [Ilbert, O.; Boselli, A.; Buat, V.; Burgarella, D.; Le Fevre, O.] Univ Aix Marseille 1, CNRS, Lab Astrophys Marseille, F-13388 Marseille 13, France. [Le Floc'h, E.; Riguccini, L.; Sargent, M.; Aussel, H.; Daddi, E.; Elbaz, D.; Bethermin, M.; Chanial, P.; Madden, S.; Panuzzo, P.] CEA Saclay, Serv Astrophys, F-91191 Gif Sur Yvette, France. [Marchetti, L.] Open Univ, Dept Phys Sci, Milton Keynes MK7 6AA, Bucks, England. [Monaco, P.] Univ Trieste, Dipartimento Fis, Sez Astron, I-34131 Trieste, Italy. [Oliver, S.; Roseboom, I.; Smith, A. J.; Wang, L.] Univ Sussex, Dept Phys & Astron, Ctr Astron, Brighton BN1 9QH, E Sussex, England. [Roseboom, I.; Arumugam, V.; Ivison, R. J.] Univ Edinburgh, Inst Astron, Royal Observ, Edinburgh EH9 3HJ, Midlothian, Scotland. [Vaccari, M.] Univ Western Cape, Dept Phys, Astrophys Grp, ZA-7535 Bellville, South Africa. [Altieri, B.; Perez Garcia, A.; Sanchez-Portal, M.; Valtchanov, I.] ESA Herschel Sci Ctr, E-28692 Villafranca, Spain. [Bongiovanni, A.; Cepa, J.; Dominguez-Sanchez, H.; Castro-Rodriguez, N.; Perez-Fournon, I.] Inst Astrofis Canarias, E-38205 San Cristobal la Laguna, Spain. [Iribarrem, A.] Univ Fed Rio de Janeiro, Observ Valongo, BR-21941 Rio De Janeiro, Brazil. [Magliocchetti, M.] INAF IFSI, I-00133 Rome, Italy. [Maiolino, R.] Univ Cambridge, Cavendish Lab, Cambridge CB3 0HE, England. [Amblard, A.] NASA, Ames Res Ctr, Moett Field, CA 94035 USA. [Bock, J.; Cooray, A.; Dowell, C. D.; Levenson, L.; Lu, N.; Nguyen, H. T.; Schulz, B.; Shupe, D. L.; Xu, C. K.; Zemcov, M.] CALTECH, Pasadena, CA 91125 USA. [Bock, J.; Dowell, C. D.; Levenson, L.; Nguyen, H. T.; Zemcov, M.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Castro-Rodriguez, N.; Perez-Fournon, I.] Univ La Laguna ULL, Dept Astrofis, E-38205 San Cristobal la Laguna, Spain. [Cava, A.] Univ Complutense Madrid, Fac CC Fis, Dept Astrofis, E-28040 Madrid, Spain. [Clements, D. L.; O'Halloran, B.; Rowan-Robinson, M.] Univ London Imperial Coll Sci Technol & Med, Blackett Lab, 3Astrophys Grp, London SW7 2AZ, England. [Conley, A.; Glenn, J.] Univ Colorado, Ctr Astrophys & Space Astron UCB 389, Boulder, CO 80309 USA. [Cooray, A.] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA. [Dwek, E.] NASA, Observ Cosmol Lab, Code 665, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Eales, S.; Griffin, M.; Papageorgiou, A.; Pohlen, M.] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales. [Glenn, J.] Univ Colorado, Dept Astrophys & Planetary Sci, Boulder, CO 80309 USA. [Ibar, E.; Ivison, R. J.; Wright, G.] UK Astron Technol Ctr, Royal Observ, Edinburgh EH9 3HJ, Midlothian, Scotland. [Isaak, K.] ESTEC SRE SA, ESA Res & Sci Support Dept, NL-2201 AZ Noordwijk, Netherlands. [Lagache, G.] Univ Paris 11, Inst Astrophys Spatiale, F-91405 Orsay, France. [Lagache, G.] CNRS, UMR 8617, F-91405 Orsay, France. [Lu, N.; Schulz, B.; Shupe, D. L.; Xu, C. K.] CALTECH, Infrared Proc & Anal Ctr, JPL, Pasadena, CA 91125 USA. [Maffei, B.] Univ Manchester, Sch Phys & Astron, Manchester M13 9PL, Lancs, England. [Pearson, C. P.; Rigopoulou, D.] Univ Coll London, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England. [Pearson, C. P.] Univ Lethbridge, Inst Space Imaging Sci, Lethbridge, AB T1K 3M4, Canada. [Rigopoulou, D.] Univ Oxford, Dept Astrophys, Oxford OX1 3RH, England. [Scott, D.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada. [Seymour, N.] CSIRO Astron & Space Sci, Epping, NSW 1710, Australia. [Stevens, J. A.] Univ Hertfordshire, Ctr Astrophys Res, Hatfield AL10 9AB, Herts, England. [Trichas, M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Vigroux, L.] Univ Paris 06, CNRS, Inst Astrophys Paris, UMR 7095, F-75014 Paris, France. [Carollo, M.; Lilly, S.] Swiss Fed Inst Technol ETH Honggerberg, Inst Astron, CH-8093 Zurich, Switzerland. [Contini, T.] Univ Toulouse, CNRS, Inst Rech Astrophys & Plantol, F-31400 Toulouse, France. [Renzini, A.] INAF Osservatorio Astron Padova, I-35122 Padua, Italy. [Scodeggio, M.] INAF IASF Milano, I-20133 Milan, Italy. RP Gruppioni, C (reprint author), INAF Osservatorio Astron Bologna, Via Ranzani 1, I-40127 Bologna, Italy. EM carlotta.gruppioni@oabo.inaf.it RI Vaccari, Mattia/R-3431-2016; Cava, Antonio/C-5274-2017; Daddi, Emanuele/D-1649-2012; Bongiovanni, Angel/J-6176-2012; amblard, alexandre/L-7694-2014; Bardelli, Sandro/O-9369-2015; Zucca, Elena/O-9396-2015; Ivison, R./G-4450-2011; OI Scott, Douglas/0000-0002-6878-9840; Marchetti, Lucia/0000-0003-3948-7621; Seymour, Nicholas/0000-0003-3506-5536; Vaccari, Mattia/0000-0002-6748-0577; Cava, Antonio/0000-0002-4821-1275; Scodeggio, Marco/0000-0002-2282-5850; Pozzetti, Lucia/0000-0001-7085-0412; Magliocchetti, Manuela/0000-0001-9158-4838; Daddi, Emanuele/0000-0002-3331-9590; amblard, alexandre/0000-0002-2212-5395; Bardelli, Sandro/0000-0002-8900-0298; Zucca, Elena/0000-0002-5845-8132; Ivison, R./0000-0001-5118-1313; Gruppioni, Carlotta/0000-0002-5836-4056 FU national funding agencies: CSA (Canada); national funding agencies: NAOC (China); CEA; CNES; CNRS (France); ASI (Italy); MCINN (Spain); SNSB (Sweden); STFC; UKSA (UK); NASA (USA); University of Trieste [FRA2009]; [PRIN- INAF 1.06.09.05]; [ASI- INAF I00507/1]; [I005110] FX 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); INAFIFSI/ OAA/OAP/OAT, LENS, SISSA (Italy); and 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). SPIRE has been developed by a consortium of institutes led by CardiffUniv. (UK) and including: Univ. Lethbridge (Canada); NAOC (China); CEA, LAM(France); IFSI, Univ. Padua (Italy); IAC (Spain); StockholmObservatory (Sweden); Imperial College London, RAL, UCLMSSL, 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, UKSA (UK) and NASA (USA). CG and FP acknowledge financial contribution from the contracts PRIN- INAF 1.06.09.05 and ASI- INAF I00507/1 and I005110. PM thanks the University of Trieste for the grant FRA2009. The authors thank an anonymous referee for the helpful comments that greatly improved the quality of the paper. NR 138 TC 106 Z9 105 U1 1 U2 7 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 JUN PY 2013 VL 432 IS 1 BP 23 EP 52 DI 10.1093/mnras/stt308 PG 30 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 152IG UT WOS:000319524600023 ER PT J AU Landt, H Ward, MJ Peterson, BM Bentz, MC Elvis, M Korista, KT Karovska, M AF Landt, Hermine Ward, Martin J. Peterson, Bradley M. Bentz, Misty C. Elvis, Martin Korista, Kirk T. Karovska, Margarita TI A near-infrared relationship for estimating black hole masses in active galactic nuclei SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies: active; galaxies: nuclei; quasars: general; infrared: galaxies ID AGN MONITORING PROJECT; RADIUS-LUMINOSITY RELATIONSHIP; STAR-FORMING GALAXIES; EMISSION-LINE REGION; VELOCITY DISPERSION; HOST GALAXIES; K-CORRECTIONS; BULGE MASS; ATLAS; STARLIGHT AB Black hole masses for samples of active galactic nuclei (AGN) are currently estimated from single-epoch optical spectra using scaling relations anchored in reverberation mapping results. In particular, the two quantities needed for calculating black hole masses, namely the velocity and the radial distance of the orbiting gas are derived from the widths of the Balmer hydrogen broad emission lines and the optical continuum luminosity, respectively. We have recently presented a near-infrared (near-IR) relationship for estimating AGN black hole masses based on the widths of the Paschen hydrogen broad emission lines and the total 1 mu m continuum luminosity. The near-IR offers several advantages over the optical: it suffers less from dust extinction, the AGN continuum is observed only weakly contaminated by the host galaxy and the strongest Paschen broad emission lines Pa alpha and Pa beta are unblended. Here, we improve the calibration of the near-IR black hole mass relationship by increasing the sample from 14 to 23 reverberation-mapped AGN using additional spectroscopy obtained with the Gemini Near-Infrared Spectrograph. The additional sample improves the number statistics in particular at the high-luminosity end. C1 [Landt, Hermine; Ward, Martin J.] Univ Durham, Dept Phys, Durham DH1 3LE, England. [Landt, Hermine] Univ Melbourne, Sch Phys, Parkville, Vic 3010, Australia. [Peterson, Bradley M.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. [Peterson, Bradley M.] Ohio State Univ, Ctr Cosmol & AstroParticle Phys, Columbus, OH 43210 USA. [Bentz, Misty C.] Georgia State Univ, Dept Phys & Astron, Atlanta, GA 30303 USA. [Elvis, Martin; Karovska, Margarita] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Korista, Kirk T.] Western Michigan Univ, Dept Phys, Kalamazoo, MI 49008 USA. RP Landt, H (reprint author), Univ Durham, Dept Phys, South Rd, Durham DH1 3LE, England. EM hermine.landt@durham.ac.uk FU European Union through the COFUND scheme; National Aeronautics Space Administration FX We thank an anonymous reviewer for their thoughtful comments, which improved this paper. We also thank Chris Onken from the Australian Gemini Office for his excellent user support. HL acknowledges financial support by the European Union through the COFUND scheme. This work is based on observations obtained at the Gemini Observatory, which is operated by the Association of Universities for Research in Astronomy, Inc., under a cooperative agreement with the NSF on behalf of the Gemini partnership: the National Science Foundation (United States), the Science and Technology Facilities Council (United Kingdom), the National Research Council (Canada), CONICYT (Chile), the Australian Research Council (Australia), Ministerio da Ciencia, Tecnologia e Inovacao (Brazil) and Ministerio de Ciencia, Tecnologia e Innovacion Productiva (Argentina). 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 Space Administration. NR 51 TC 12 Z9 12 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 JUN PY 2013 VL 432 IS 1 BP 113 EP 126 DI 10.1093/mnras/stt421 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 152IG UT WOS:000319524600028 ER PT J AU Siwak, M Rucinski, SM Matthews, JM Kuschnig, R Guenther, DB Moffat, AFJ Rowe, JF Sasselov, D Weiss, WW AF Siwak, Michal Rucinski, Slavek M. Matthews, Jaymie M. Kuschnig, Rainer Guenther, David B. Moffat, Anthony F. J. Rowe, Jason F. Sasselov, Dimitar Weiss, Werner W. TI Photometric variability in FU Ori and Z CMa as observed by MOST SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE accretion, accretion discs; stars: individual: FU Ori; stars: individual: Z CMa ID Z-CANIS-MAJORIS; T TAURI STAR; SYSTEM Z CMA; AU-SCALE; ORIONIS OBJECTS; 2008 OUTBURST; DISK; SPECTROSCOPY; COMPANION; COMPONENT AB Photometric observations obtained by the MOST satellite were used to characterize optical small-scale variability of the young stars FU Ori and Z CMa. Wavelet analysis for FU Ori reveals the possible existence of several 2-9 d quasi-periodic features occurring nearly simultaneously; they may be interpreted as plasma parcels or other localized disc heterogeneities revolving at different Keplerian radii in the accretion disc. Their periods may shorten slowly which may be due to spiralling in of individual parcels towards the inner disc radius, estimated at 4.8 +/- 0.2 R-circle dot. Analysis of additional multicolour data confirms the previously obtained relation between variations in the B - V colour index and the V magnitude. In contrast to the FU Ori results, the oscillation spectrum of Z CMa does not reveal any periodicities with the wavelet spectrum possibly dominated by outburst of the Herbig Be component. C1 [Siwak, Michal] Cracov Pedag Univ, Mt Suhora Astron Observ, PL-30084 Krakow, Poland. [Rucinski, Slavek M.] Univ Toronto, Deparntment Astron & Astrophys, Toronto, ON M5S 3H4, Canada. [Matthews, Jaymie M.; Kuschnig, Rainer] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada. [Kuschnig, Rainer; Weiss, Werner W.] Univ Vienna, Inst Astron, A-1180 Vienna, Austria. [Guenther, David B.] St Marys Univ, Dept Phys & Astron, Inst Computat Astrophys, Halifax, NS B3H 3C3, Canada. [Moffat, Anthony F. J.] Univ Montreal, Dept Phys, Montreal, PQ H3C 3J7, Canada. [Rowe, Jason F.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Sasselov, Dimitar] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Siwak, M (reprint author), Cracov Pedag Univ, Mt Suhora Astron Observ, Ul Podchorazych 2, PL-30084 Krakow, Poland. EM siwak@nac.oa.uj.edu.pl FU Canadian Space Agency; Natural Sciences and Engineering Research Council of Canada; FQRNT (Quebec); Austrian Science Funds [P22691-N16] 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 Science Funds (P22691-N16). NR 37 TC 4 Z9 4 U1 0 U2 0 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 JUN PY 2013 VL 432 IS 1 BP 194 EP 199 DI 10.1093/mnras/stt441 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 152IG UT WOS:000319524600033 ER PT J AU Schmidt, KB Rix, HW da Cunha, E Brammer, GB Cox, TJ van Dokkum, P Schreiber, NMF Franx, M Fumagalli, M Jonsson, P Lundgren, B Maseda, MV Momcheva, I Nelson, EJ Skelton, RE van der Wel, A Whitaker, KE AF Schmidt, Kasper B. Rix, Hans-Walter da Cunha, Elisabete Brammer, Gabriel B. Cox, Thomas J. van Dokkum, Pieter Schreiber, Natascha M. Foerster Franx, Marijn Fumagalli, Mattia Jonsson, Patrik Lundgren, Britt Maseda, Michael V. Momcheva, Ivelina Nelson, Erica J. Skelton, Rosalind E. van der Wel, Arjen Whitaker, Katherine E. TI The spatial extent and distribution of star formation in 3D-HST mergers at z similar to 1.5 SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies: formation; galaxies: interactions; galaxies: starburst; galaxies: structure ID INTEGRAL FIELD SPECTROSCOPY; DISC GALAXY MERGERS; DARK ENERGY SURVEY; ULTRA-DEEP-FIELD; FORMING GALAXIES; MASSIVE GALAXIES; HIGH-REDSHIFT; FORMATION HISTORY; NEARBY GALAXIES; MAJOR MERGERS AB We present an analysis of the spatial distribution of star formation in a sample of 60 visually identified galaxy merger candidates at z > 1. Our sample, drawn from the 3D-HST survey, is flux limited and was selected to have high star formation rates based on fits of their broad-band, low spatial resolution spectral energy distributions. It includes plausible pre-merger (close pairs) and post-merger (single objects with tidal features) systems, with total stellar masses and star formation rates derived from multiwavelength photometry. Here we use near-infrared slitless spectra from 3D-HST which produce H alpha or [O III] emission line maps as proxies for star formation maps. This provides a first comprehensive high-resolution, empirical picture of where star formation occurred in galaxy mergers at the epoch of peak cosmic star formation rate. We find that detectable star formation can occur in one or both galaxy centres, or in tidal tails. The most common case (58 per cent) is that star formation is largely concentrated in a single, compact region, coincident with the centre of (one of) the merger components. No correlations between star formation morphology and redshift, total stellar mass or star formation rate are found. A restricted set of hydrodynamical merger simulations between similarly massive and gas-rich objects implies that star formation should be detectable in both merger components, when the gas fractions of the individual components are the same. This suggests that z similar to 1.5 mergers typically occur between galaxies whose gas fractions, masses and/or star formation rates are distinctly different from one another. C1 [Schmidt, Kasper B.; Rix, Hans-Walter; da Cunha, Elisabete; Maseda, Michael V.; van der Wel, Arjen] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Schmidt, Kasper B.] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA. [Brammer, Gabriel B.] European So Observ, Santiago 19, Chile. [Cox, Thomas J.] Carnegie Observ, Pasadena, CA 91101 USA. [van Dokkum, Pieter; Lundgren, Britt; Momcheva, Ivelina; Nelson, Erica J.; Skelton, Rosalind E.] Yale Univ, Dept Astron, New Haven, CT 06520 USA. [Schreiber, Natascha M. Foerster] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Franx, Marijn; Fumagalli, Mattia] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [Jonsson, Patrik] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Whitaker, Katherine E.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA. RP Schmidt, KB (reprint author), Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany. EM kschmidt@physics.ucsb.edu RI Skelton, Rosalind/S-1845-2016 OI Skelton, Rosalind/0000-0001-7393-3336 FU ERC grant HIGHZ [227749]; Marie Curie Initial Training Network ELIXIR of the European Commission [PITN-GA-2008-214227]; NASA [NAS5-26555] FX We acknowledge funding from ERC grant HIGHZ no. 227749. This work was funded in part by the Marie Curie Initial Training Network ELIXIR of the European Commission under contract PITN-GA-2008-214227. The work was mainly done while KBS was a member of the International Max Planck Research School for Astronomy and Cosmic Physics at the University of Heidelberg (IMPRS-HD), Germany. This work is based on observations taken by the 3D-HST Treasury Program with the NASA/ESA HST, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555. NR 96 TC 9 Z9 9 U1 1 U2 3 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 JUN PY 2013 VL 432 IS 1 BP 285 EP 300 DI 10.1093/mnras/stt459 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 152IG UT WOS:000319524600040 ER PT J AU Wetzel, AR Tinker, JL Conroy, C van den Bosch, FC AF Wetzel, Andrew R. Tinker, Jeremy L. Conroy, Charlie van den Bosch, Frank C. TI Galaxy evolution in groups and clusters: satellite star formation histories and quenching time-scales in a hierarchical Universe SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE methods: numerical; galaxies: clusters: general; galaxies: evolution; galaxies: groups: general; galaxies: haloes; galaxies: star formation ID DIGITAL-SKY-SURVEY; HALO OCCUPATION DISTRIBUTION; GALACTIC NUCLEUS FEEDBACK; DARK MATTER CONNECTION; COLOR-DENSITY RELATION; LOW-REDSHIFT UNIVERSE; AEGIS FIELD GALAXIES; ARECIBO SDSS SURVEY; IRAM LEGACY SURVEY; STELLAR MASS-LOSS AB Satellite galaxies in groups and clusters aremore likely to have low star formation rates (SFRs) and lie on the 'red sequence' than central ('field') galaxies. Using galaxy group/cluster catalogues from the Sloan Digital Sky Survey Data Release 7, together with a high-resolution, cosmological N-body simulation to track satellite orbits, we examine the star formation histories and quenching time-scales of satellites of M-star > 5 x 10(9) M-circle dot at z approximate to 0. We first explore satellite infall histories: group preprocessing and ejected orbits are critical aspects of satellite evolution, and properly accounting for these, satellite infall typically occurred at z similar to 0.5, or similar to 5 Gyr ago. To obtain accurate initial conditions for the SFRs of satellites at their time of first infall, we construct an empirical parametrization for the evolution of central galaxy SFRs and quiescent fractions. With this, we constrain the importance and efficiency of satellite quenching as a function of satellite and host halo mass, finding that satellite quenching is the dominant process for building up all quiescent galaxies at M-star < 10(10) M-circle dot. We then constrain satellite star formation histories, finding a 'delayed-then-rapid' quenching scenario: satellite SFRs evolve unaffected for 2-4 Gyr after infall, after which star formation quenches rapidly, with an e-folding time of <0.8 Gyr. These quenching time-scales are shorter for more massive satellites but do not depend on host halo mass: the observed increase in the satellite quiescent fraction with halo mass arises simply because of satellites quenching in a lower mass group prior to infall (group preprocessing), which is responsible for up to half of quenched satellites in massive clusters. Because of the long time delay before quenching starts, satellites experience significant stellar mass growth after infall, nearly identical to central galaxies. This fact provides key physical insight into the subhalo abundance matching method. C1 [Wetzel, Andrew R.; van den Bosch, Frank C.] Yale Univ, Dept Astron, New Haven, CT 06520 USA. [Tinker, Jeremy L.] NYU, Dept Phys, Ctr Cosmol & Particle Phys, New York, NY 10013 USA. [Conroy, Charlie] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Wetzel, AR (reprint author), Yale Univ, Dept Astron, New Haven, CT 06520 USA. EM andrew.wetzel@yale.edu OI Wetzel, Andrew/0000-0003-0603-8942 NR 164 TC 139 Z9 139 U1 0 U2 6 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 JUN PY 2013 VL 432 IS 1 BP 336 EP 358 DI 10.1093/mnras/stt469 PG 23 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 152IG UT WOS:000319524600045 ER PT J AU Sadowski, A Sironi, L Abarca, D Guo, XY Ozel, F Narayan, R AF Sadowski, Aleksander Sironi, Lorenzo Abarca, David Guo, Xinyi Ozel, Feryal Narayan, Ramesh TI Radio light curves during the passage of cloud G2 near Sgr A SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE acceleration of particles; accretion, accretion discs; black hole physics; radiation mechanisms: non-thermal ID SAGITTARIUS-A-ASTERISK; ADVECTION-DOMINATED ACCRETION; GENERAL-RELATIVISTIC MAGNETOHYDRODYNAMICS; BLACK-HOLE; GALACTIC-CENTER; X-RAY; PARTICLE-ACCELERATION; NUMERICAL-SIMULATION; GRMHD SIMULATIONS; SHOCKS AB We calculate radio light curves produced by the bow shock that is likely to form in front of the G2 cloud when it penetrates the accretion disc of Sgr A*. The shock acceleration of the radio-emitting electrons is captured self-consistently by means of first-principles particle-in-cell simulations. We show that the radio luminosity is expected to reach maximum in early 2013, roughly a month after the bow shock crosses the orbit pericentre. We estimate the peak radio flux at 1.4 GHz to be 1.4-22 Jy depending on the assumed orbit orientation and parameters. We show that the most promising frequencies for radio observations are in the 0.1 < nu < 1 GHz range, for which the bow shock emission will be much stronger than the intrinsic radio flux for all the models considered. C1 [Sadowski, Aleksander; Sironi, Lorenzo; Guo, Xinyi; Ozel, Feryal; Narayan, Ramesh] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Abarca, David] Harvard Univ, Cambridge, MA 02138 USA. [Ozel, Feryal] Univ Arizona, Tucson, AZ 85721 USA. RP Sadowski, A (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM asadowski@cfa.harvard.edu OI Narayan, Ramesh/0000-0002-1919-2730 FU NASA [NNX11AE16G, PF1-120090, NAS8-03060]; Chandra X-ray Center; NSF [AST-1108753]; Radcliffe Institute for Advanced Study at Harvard University; Odyssey cluster at Harvard University [TG-AST120010] FX We thank Dimitrios Psaltis for useful comments. AS and RN were supported in part by NASA grant NNX11AE16G. LS is supported by NASA through Einstein Postdoctoral Fellowship grant number PF1-120090 awarded by the Chandra X-ray Center, which is operated by the Smithsonian Astrophysical Observatory for NASA under contract NAS8-03060. FO acknowledges support from NSF grant AST-1108753 and from the Radcliffe Institute for Advanced Study at Harvard University. The particle-in-cell simulations were performed on the Odyssey cluster at Harvard University, on XSEDE resources under contract No. TG-AST120010, and on NASA High-End Computing (HEC) resources through the NASA Advanced Supercomputing (NAS) Division at Ames Research Center. NR 45 TC 29 Z9 29 U1 0 U2 3 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 JUN PY 2013 VL 432 IS 1 BP 478 EP 491 DI 10.1093/mnras/stt495 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 152IG UT WOS:000319524600054 ER PT J AU Russell, HR McNamara, BR Edge, AC Hogan, MT Main, RA Vantyghem, AN AF Russell, H. R. McNamara, B. R. Edge, A. C. Hogan, M. T. Main, R. A. Vantyghem, A. N. TI Radiative efficiency, variability and Bondi accretion on to massive black holes: the transition from radio AGN to quasars in brightest cluster galaxies SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE accretion, accretion discs; galaxies: active; galaxies: jets; X-rays: galaxies: clusters ID ACTIVE GALACTIC NUCLEI; X-RAY-EMISSION; COOLING-FLOW CLUSTERS; ADVECTION-DOMINATED ACCRETION; DEEP CHANDRA OBSERVATION; HUBBLE-SPACE-TELESCOPE; SPECTRAL ENERGY-DISTRIBUTIONS; LUMINOUS ELLIPTIC GALAXIES; COLD FEEDBACK MECHANISM; FR-I AB We examine unresolved nuclear X-ray sources in 57 brightest cluster galaxies to study the relationship between nuclear X-ray emission and accretion on to supermassive black holes. The majority of the clusters in our sample have prominent X-ray cavities embedded in the surrounding hot atmospheres, which we use to estimate mean jet power and average accretion rate on to the supermassive black holes over the past several hundred Myr. We find that roughly half of the sample have detectable nuclear X-ray emission. The nuclear X-ray luminosity is correlated with average accretion rate determined using X-ray cavities, which is consistent with the hypothesis that nuclear X-ray emission traces ongoing accretion. The results imply that jets in systems that have experienced recent active galactic nucleus (AGN) outbursts, in the last similar to 10(7) yr, are 'on' at least half of the time. Nuclear X-ray sources become more luminous with respect to the mechanical jet power as the mean accretion rate rises. We show that nuclear radiation exceeds the jet power when the mean accretion rate rises above a few per cent of the Eddington rate, or a power output of similar to 10(45) erg s(-1), where the AGN apparently transitions to a quasar. The nuclear X-ray emission from three objects (A2052, Hydra A, M84) varies by factors of 2-10 on time-scales of 6 months to 10 years. If variability at this level is a common phenomenon, it can account for much of the scatter in the relationship between mean accretion rate and nuclear X-ray luminosity. We find no significant change in the spectral energy distribution as a function of luminosity in the variable objects. The nuclear X-ray luminosity is consistent with emission from either a jet, an advection-dominated accretion flow, or a combination of the two, although other origins are possible. We also consider the longstanding problem of whether jets are powered by the accretion of cold circumnuclear gas or nearly spherical inflows of hot keV gas. For a subset of 13 nearby systems in our sample, we re-examine the relationship between the jet power and the Bondi accretion rate. The results indicate weaker evidence for a trend between Bondi accretion and jet power, due to uncertainties in the cavity volumes and gas densities at the Bondi radius. We suggest that cold gas fuelling could be a likely source of accretion power in these objects; however, we cannot rule out Bondi accretion, which could play a significant role in low-power jets. C1 [Russell, H. R.; McNamara, B. R.; Main, R. A.; Vantyghem, A. N.] Univ Waterloo, Dept Phys & Astron, Waterloo, ON N2L 3G1, Canada. [McNamara, B. R.] Perimeter Inst Theoret Phys, Waterloo, ON N2L 2Y5, Canada. [McNamara, B. R.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Edge, A. C.; Hogan, M. T.] Univ Durham, Dept Phys, Durham DH1 3LE, England. RP Russell, HR (reprint author), Univ Waterloo, Dept Phys & Astron, Waterloo, ON N2L 3G1, Canada. EM helen.russell@uwaterloo.ca OI Edge, Alastair/0000-0002-3398-6916 FU Canadian Space Agency Space Science Enhancement Program; Natural Sciences and Engineering Research Council of Canada; National Aeronautics and Space Administration; National Science Foundation FX HRR and BRM acknowledge generous financial support from the Canadian Space Agency Space Science Enhancement Program. RAM and ANV acknowledge support from the Natural Sciences and Engineering Research Council of Canada. We thank Paul Nulsen, Avery Broderick, Roderick Johnstone and James Taylor for helpful discussions. We also thank the reviewer for helpful and constructive comments. This work 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 Extra-galactic Database (NED) which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. NR 193 TC 52 Z9 52 U1 1 U2 3 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 JUN PY 2013 VL 432 IS 1 BP 530 EP 553 DI 10.1093/mnras/stt490 PG 24 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 152IG UT WOS:000319524600059 ER PT J AU Schmidt, SJ Menard, B Scranton, R Morrison, C McBride, CK AF Schmidt, Samuel J. Menard, Brice Scranton, Ryan Morrison, Christopher McBride, Cameron K. TI Recovering redshift distributions with cross-correlations: pushing the boundaries SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE methods: data analysis; methods: statistical; cosmology: observations; large-scale structure of Universe ID DIGITAL SKY SURVEY; DEEP LENS SURVEY; PHOTOMETRIC REDSHIFT; GALAXIES; EVOLUTION; QUASARS; TESTS AB Determining accurate redshift distributions for very large samples of objects has become increasingly important in cosmology. We investigate the impact of extending cross-correlation based redshift distribution recovery methods to include small-scale clustering information. The major concern in such work is the ability to disentangle the amplitude of the underlying redshift distribution from the influence of evolving galaxy bias. Using multiple simulations covering a variety of galaxy bias evolution scenarios, we demonstrate reliable redshift recoveries using linear clustering assumptions well into the non-linear regime for redshift distributions of narrow redshift width. Including information from intermediate physical scales balances the increased information available from clustering and the residual bias incurred from relaxing of linear constraints. We discuss how breaking a broad sample into tomographic bins can improve estimates of the redshift distribution, and present a simple bias removal technique using clustering information from the spectroscopic sample alone. C1 [Schmidt, Samuel J.; Scranton, Ryan; Morrison, Christopher] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA. [Menard, Brice] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [McBride, Cameron K.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Schmidt, SJ (reprint author), Univ Calif Davis, Dept Phys, 1 Shields Ave, Davis, CA 95616 USA. EM sschmidt@physics.ucdavis.edu FU NSF [AST-1009514]; Alfred P. Sloan foundation FX This work was supported by NSF Grant AST-1009514. Brice Menard is supported by the NSF and the Alfred P. Sloan foundation. We thank the anonymous referee for suggestions that improved the content of the paper. We used mock catalogues based on the LasDamas project; we thank the LasDamas collaboration for providing us with these data. We thank Darren Croton for making the Millennium simulation light cones used in this work publicly available. NR 26 TC 11 Z9 12 U1 1 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 JUN PY 2013 VL 431 IS 4 BP 3307 EP 3318 DI 10.1093/mnras/stt410 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 151RX UT WOS:000319479000028 ER PT J AU Villaescusa-Navarro, F Vogelsberger, M Viel, M Loeb, A AF Villaescusa-Navarro, F. Vogelsberger, M. Viel, M. Loeb, A. TI Neutrino signatures on the high-transmission regions of the Lyman alpha forest SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE neutrinos; intergalactic medium; quasars: absorption lines; cosmology: theory; large-scale structure of Universe ID LARGE-SCALE STRUCTURE; MASSIVE NEUTRINOS; INTERGALACTIC MEDIUM; POWER SPECTRUM; SIMULATION; COSMOLOGY; UNIVERSE; VOIDS; FLUX AB We quantify the impact of massive neutrinos on the statistics of low-density regions in the intergalactic medium as probed by the Lyman alpha forest at redshifts z = 2.2-4. Based on mock but realistic quasar (QSO) spectra extracted from hydrodynamic simulations with cold dark matter, baryons and neutrinos, we find that the probability distribution of weak Lyman alpha absorption features, as sampled by Lyman alpha flux regions at high transmissivity, is strongly affected by the presence of massive neutrinos. We show that systematic errors affecting the Lyman alpha forest reduce but do not erase the neutrino signal. Using the Fisher matrix formalism, we conclude that the sum of the neutrino masses can be measured, using the method proposed in this paper, with a precision smaller than 0.4 eV using a catalogue of 200 high-resolution (signal-to-noise ratio similar to 100) QSO spectra. This number reduces to 0.27 eV by making use of reasonable priors in the other parameters that also affect the statistics of the high-transitivity regions of the Lyman alpha forest. The constraints obtained with this method can be combined with independent bounds from the cosmic microwave background, large-scale structures and measurements of the matter power spectrum from the Lyman alpha forest to produce tighter upper limits on the sum of the masses of the neutrinos. C1 [Villaescusa-Navarro, F.] Univ Valencia, IFIC, CSIC, E-46071 Valencia, Spain. [Villaescusa-Navarro, F.; Vogelsberger, M.; Loeb, A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Viel, M.] Osserv Astron Trieste, INAF, I-34131 Trieste, Italy. [Viel, M.] Ist Nazl Fis Nucl, Sez Trieste, I-34127 Trieste, Italy. RP Villaescusa-Navarro, F (reprint author), Univ Valencia, IFIC, CSIC, E-46071 Valencia, Spain. EM viel@oats.inaf.it OI Viel, Matteo/0000-0002-2642-5707 FU CSIC; ASI/AAE; INFN/PD51; ASI/EUCLID; PRIN-INAF; PRIN-MIUR; NSF [AST-0907890]; NASA [NNX08AL43G, NNA09DB30A]; ERC FX We thank the referee for the very helpful report. We thank Enzo Branchini, Olga Mena, Jordi Miralda-Escude, Carlos Pena-Garay, Khee-Gan Lee, Jonathan Pritchard and Jesus Zavala for discussions and helpful comments on the manuscript and Volker Springel for providing us with GADGET-3. The simulations were run on the Darwin Supercomputer Centre HPCF in Cambridge (UK) and at the research computing centre of Harvard University. FV-N was supported by the CSIC under the JAE-pre-doc program when this work started. This work was supported in part by grants: ASI/AAE, INFN/PD51, ASI/EUCLID, PRIN-INAF 2009, PRIN-MIUR (for MVi), as well as NSF grant AST-0907890 and NASA grants NNX08AL43G and NNA09DB30A (for AL). MVi and FV-N are supported by the ERC Starting Grant 'CosmoIGM'. NR 44 TC 5 Z9 5 U1 1 U2 5 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 JUN PY 2013 VL 431 IS 4 BP 3670 EP 3677 DI 10.1093/mnras/stt452 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 151RX UT WOS:000319479000057 ER PT J AU McKellar, AE Marra, PP Hannon, SJ Studds, CE Ratcliffe, LM AF McKellar, Ann E. Marra, Peter P. Hannon, Susan J. Studds, Colin E. Ratcliffe, Laurene M. TI Winter rainfall predicts phenology in widely separated populations of a migrant songbird SO OECOLOGIA LA English DT Article DE American redstart; Climate change; Migration; Migratory connectivity; Setophaga ruticilla ID SAHARAN MIGRATORY BIRDS; CLIMATE-CHANGE; ECOLOGICAL CONDITIONS; NONBREEDING-SEASON; AMERICAN REDSTARTS; SPRING MIGRATION; ARRIVAL DATE; SETOPHAGA-RUTICILLA; PASSAGE AREAS; BREEDING DATE AB Climate change is affecting behaviour and phenology in many animals. In migratory birds, weather patterns both at breeding and at non-breeding sites can influence the timing of spring migration and breeding. However, variation in responses to weather across a species range has rarely been studied, particularly among populations that may winter in different locations. We used prior knowledge of migratory connectivity to test the influence of weather from predicted non-breeding sites on bird phenology in two breeding populations of a long-distance migratory bird species separated by 3,000 km. We found that winter rainfall showed similar associations with arrival and egg-laying dates in separate breeding populations on an east-west axis: greater rainfall in Jamaica and eastern Mexico was generally associated with advanced American redstart (Setophaga ruticilla) phenology in Ontario and Alberta, respectively. In Ontario, these patterns of response could largely be explained by changes in the behaviour of individual birds, i.e., phenotypic plasticity. By explicitly incorporating migratory connectivity into responses to climate, our data suggest that widely separated breeding populations can show independent and geographically specific associations with changing weather conditions. The tendency of individuals to delay migration and breeding following dry winters could result in population declines due to predicted drying trends in tropical areas and the tight linkage between early arrival/breeding and reproductive success in long-distance migrants. C1 [McKellar, Ann E.; Ratcliffe, Laurene M.] Queens Univ, Dept Biol, Kingston, ON K7L 3N6, Canada. [Marra, Peter P.; Studds, Colin E.] Smithsonian Conservat Biol Inst, Migratory Bird Ctr, Natl Zool Pk, Washington, DC 20008 USA. [Hannon, Susan J.] Univ Alberta, Dept Biol Sci, Edmonton, AB T6G 2E9, Canada. RP McKellar, AE (reprint author), Univ Missouri, Dept Fisheries & Wildlife Sci, Columbia, MO 65211 USA. EM mckellara@missouri.edu RI Studds, Colin/C-3701-2012 FU Queen's University; Natural Sciences and Engineering Research Council of Canada; Canadian Foundation for Innovation; National Science Foundation; Smithsonian Institution; Ontario Innovation Trust; Sigma Xi; American Ornithologists' Union; Society of Canadian Ornithologists; American Museum of Natural History FX We thank all of the field assistants who contributed to this study. C. Eckert helped with data analysis. Funding was provided by Queen's University, the Natural Sciences and Engineering Research Council of Canada, the Canadian Foundation for Innovation, the National Science Foundation, the Smithsonian Institution, the Ontario Innovation Trust, Sigma Xi, the American Ornithologists' Union, the Society of Canadian Ornithologists, and the American Museum of Natural History. Procedures were performed in accordance with permits from the Queen's University Animal Care Committee (Ratcliffe-2010-009) and the Canadian Wildlife Services (banding permit 10771E and collection permit CA0233). All methods used in this study comply with current laws of the country in which they were performed. NR 55 TC 20 Z9 22 U1 9 U2 106 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0029-8549 J9 OECOLOGIA JI Oecologia PD JUN PY 2013 VL 172 IS 2 BP 595 EP 605 DI 10.1007/s00442-012-2520-8 PG 11 WC Ecology SC Environmental Sciences & Ecology GA 146GE UT WOS:000319077100028 PM 23161154 ER PT J AU Jiang, ZB Chen, ZW Wang, Y Yang, J Huang, JS Zhang, QZ Fazio, G AF Jiang, Zhi-Bo Chen, Zhi-Wei Wang, Yuan Yang, Ji Huang, Jia-Sheng Zhang, Qi-Zhou Fazio, Giovani TI AFGL 5157 NH3: a new stellar cluster in the forming process SO RESEARCH IN ASTRONOMY AND ASTROPHYSICS LA English DT Article DE ISM: individual (AFGL 5157); ISM: jets and outflows; ISM: lines and bands; stars: formation ID SPECTRAL ENERGY-DISTRIBUTION; FAR-INFRARED SOURCES; PROTOSTELLAR CANDIDATES; OUTER GALAXY; OBJECTS; REGION; OUTFLOWS; EMISSION; AFGL-5157; SAMPLE AB We present the analysis of Spitzer/IRAC and near infrared imaging observation of AFGL 5157, an active star forming region. In the IRAC images, this region shows strong emissions of polycyclic aromatic hydrocarbons in channel 4 and emissions of H-2 in channel 2. Many of the H-2 features are aligned to form jet-like structures. Three bipolar jets in the NH3 core region and a couple of jets northwest of the core have been identified. We identify the possible driving agents of the bipolar jets and show them to be very young. An embedded cluster has been detected in the NH3 core; many members in the cluster have spectral energy distributions that increase from JHK bands toward longer wavelengths, indicative of their early evolutionary stages. Millimeter and submillimeter continuum emissions in the NH3 core and the northwest subregion are found to coincide spatially with these presumable Class 0/I sources. The existence of H-2 bipolar jets and very young stellar objects suggests that star formation is continuing at the present epoch in these subregions. Combining information from previous studies, we propose a sequential star formation scenario in the whole AFGL 5157 region. C1 [Jiang, Zhi-Bo; Chen, Zhi-Wei; Wang, Yuan; Yang, Ji] Chinese Acad Sci, Purple Mt Observ, Nanjing 210008, Jiangsu, Peoples R China. [Jiang, Zhi-Bo; Chen, Zhi-Wei; Wang, Yuan] Chinese Acad Sci, Key Lab Radio Astron, Nanjing 210008, Jiangsu, Peoples R China. [Chen, Zhi-Wei] Chinese Acad Sci, Grad Univ, Beijing 100049, Peoples R China. [Huang, Jia-Sheng; Zhang, Qi-Zhou; Fazio, Giovani] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Jiang, ZB (reprint author), Chinese Acad Sci, Purple Mt Observ, Nanjing 210008, Jiangsu, Peoples R China. EM zbjiang@pmo.ac.cn FU National Aeronautics and Space Administration; National Science Foundation; JCMT data archive; National Natural Science Foundation of China [10873037, 10921063]; National Basic Research Program of China (973 Program) [2007CB815406] FX Z. J. is grateful to M. Ashby and K. Qiu for their assistance in reducing the data and making the mosaic, and Y. Chen for providing the NIR H2 image. This work makes use of 2MASS, 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, and the JCMT data archive, which is operated by the Joint Astronomy Centre on behalf of the Science and Technology Facilities Council of the UK, the Netherlands Organisation for Scientific Research, and the National Research Council of Canada. This publication makes use of data products from the Wide-field Infrared Survey Explorer, which is a joint project of the University of California, Los Angeles, and the Jet Propulsion Laboratory/California Institute of Technology, funded by the National Aeronautics and Space Administration. The project is supported by the National Natural Science Foundation of China (Grant Nos. 10873037 and 10921063), and partially supported by the National Basic Research Program of China (973 Program, 2007CB815406). NR 22 TC 0 Z9 0 U1 1 U2 6 PU NATL ASTRONOMICAL OBSERVATORIES, CHIN ACAD SCIENCES PI BEIJING PA 20A DATUN RD, CHAOYANG, BEIJING, 100012, PEOPLES R CHINA SN 1674-4527 J9 RES ASTRON ASTROPHYS JI Res. Astron. Astrophys. PD JUN PY 2013 VL 13 IS 6 BP 695 EP 704 DI 10.1088/1674-4527/13/6/009 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 154VP UT WOS:000319704300009 ER PT J AU Lintott, CJ Schwamb, ME Barclay, T Sharzer, C Fischer, DA Brewer, J Giguere, M Lynn, S Parrish, M Batalha, N Bryson, S Jenkins, J Ragozzine, D Rowe, JF Schwainski, K Gagliano, R Gilardi, J Jek, KJ Paakkonen, JP Smits, T AF Lintott, Chris J. Schwamb, Megan E. Barclay, Thomas Sharzer, Charlie Fischer, Debra A. Brewer, John Giguere, Matthew Lynn, Stuart Parrish, Michael Batalha, Natalie Bryson, Steve Jenkins, Jon Ragozzine, Darin Rowe, Jason F. Schwainski, Kevin Gagliano, Robert Gilardi, Joe Jek, Kian J. Paeaekkoenen, Jari-Pekka Smits, Tjapko TI PLANET HUNTERS: NEW KEPLER PLANET CANDIDATES FROM ANALYSIS OF QUARTER 2 SO ASTRONOMICAL JOURNAL LA English DT Article DE planets and satellites: detection; planets and satellites: individual (KIC 4552729b, KIC 10005758b, KIC 10005758c) ID GALAXY ZOO; SYSTEMS; STELLAR AB We present new planet candidates identified in NASA Kepler Quarter 2 public release data by volunteers engaged in the Planet Hunters citizen science project. The two candidates presented here survive checks for false positives, including examination of the pixel offset to constrain the possibility of a background eclipsing binary. The orbital periods of the planet candidates are 97.46 days (KIC 4552729) and 284.03 (KIC 10005758) days and the modeled planet radii are 5.3 and 3.8R(circle plus). The latter star has an additional known planet candidate with a radius of 5.05R(circle plus) and a period of 134.49 days, which was detected by the Kepler pipeline. The discovery of these candidates illustrates the value of massively distributed volunteer review of the Kepler database to recover candidates which were otherwise uncataloged. C1 [Lintott, Chris J.] Oxford Astrophys, Oxford OX1 3RH, England. [Lintott, Chris J.; Lynn, Stuart; Parrish, Michael] Adler Planetarium, Chicago, IL 60605 USA. [Schwamb, Megan E.; Schwainski, Kevin] Yale Univ, Dept Phys, New Haven, CT 06520 USA. [Schwamb, Megan E.] Yale Univ, Yale Ctr Astron & Astrophys, New Haven, CT 06520 USA. [Barclay, Thomas; Batalha, Natalie; Bryson, Steve; Rowe, Jason F.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Barclay, Thomas] Bay Area Environm Res Inst, Sonoma, CA 95476 USA. [Sharzer, Charlie; Fischer, Debra A.; Brewer, John; Giguere, Matthew] Yale Univ, Dept Astron, New Haven, CT 06511 USA. [Jenkins, Jon] SETI Inst, Mountain View, CA 94043 USA. [Ragozzine, Darin] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Lintott, CJ (reprint author), Oxford Astrophys, Denys Wilkinson Bldg,Keble Rd, Oxford OX1 3RH, England. EM cjl@astro.ox.ac.uk OI Brewer, John/0000-0002-9873-1471; Schwamb, Megan/0000-0003-4365-1455; Fischer, Debra/0000-0003-2221-0861 FU Yale University; NASA [10-OUTRCH.210-0001, NAS5-26555]; NSF Astronomy and Astrophysics Postdoctoral Fellowship [AST-100325]; Leverhulme Trust; National Science Foundation [DRL-0941610]; National Aeronautics and Space Administration; NASA Office of Space Science [NNX09AF08G] FX D.F. acknowledges funding support from Yale University and support from the NASA Supplemental Outreach Award, 10-OUTRCH.210-0001. M.E.S. is supported by an NSF Astronomy and Astrophysics Postdoctoral Fellowship under award AST-100325. The Zooniverse is supported by The Leverhulme Trust. The Talk system used by Planet Hunters was built during work supported by the National Science Foundation under grant No. DRL-0941610. We gratefully acknowledge the dedication and achievements of Kepler Science Team and all those who contributed to the success of the mission. We acknowledge use of public release data served by the NASA/IPAC/NExScI Star and Exoplanet Database, which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. This research has made use of NASA's Astrophysics Data System Bibliographic Services. This paper includes data collected by the Kepler spacecraft, and we gratefully acknowledge the entire Kepler mission team's efforts in obtaining and providing the light curves used in this analysis. Funding for the Kepler mission is provided by the NASA Science Mission directorate. The publicly released Kepler light curves were obtained from the Mikulski Archive for Space Telescopes at the Space Telescope Science Institute (MAST). STScI is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555. Support for MAST for non-HST data is provided by the NASA Office of Space Science via grant NNX09AF08G and by other grants and contracts. NR 26 TC 10 Z9 10 U1 0 U2 12 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 J9 ASTRON J JI Astron. J. PD JUN PY 2013 VL 145 IS 6 AR 151 DI 10.1088/0004-6256/145/6/151 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 147LC UT WOS:000319167400008 ER PT J AU Littlefield, C Garnavich, P Applegate, A Magno, K Pogge, R Irwin, J Marion, GH Vinko, J Kirshner, R AF Littlefield, C. Garnavich, P. Applegate, A. Magno, K. Pogge, R. Irwin, J. Marion, G. H. Vinko, J. Kirshner, R. TI A NEW SUB-PERIOD-MINIMUM CATACLYSMIC VARIABLE WITH PARTIAL HYDROGEN DEPLETION AND EVIDENCE OF SPIRAL DISK STRUCTURE SO ASTRONOMICAL JOURNAL LA English DT Article DE novae, cataclysmic variables; stars: dwarf novae; stars: evolution; stars: individual (CSS 120422:111127+571239, SBS 1108+574) ID AM CVN STARS; ACCRETION DISKS; DWARF NOVA; ORBITAL PERIOD; INTERACTING BINARIES; CLOSE BINARIES; WHITE-DWARF; EVOLUTION; SECONDARIES; SIMULATIONS AB We present time-resolved spectroscopy and photometry of CSS 120422:111127+571239 (=SBS 1108+574), a recently discovered SU UMa-type dwarf nova whose 55 minute orbital period is well below the cataclysmic variable (CV) period minimum of similar to 78 minutes. In contrast with most other known CVs, its spectrum features He I emission of comparable strength to the Balmer lines, implying a hydrogen abundance less than 0.1 of long-period CVs-but still at least 10 times higher than that in AM CVn stars. Together, the short orbital period and remarkable helium-to-hydrogen ratio suggest that mass transfer in CSS 120422 began near the end of the donor star's main-sequence lifetime, meaning that this CV is a strong candidate progenitor of an AM CVn system as described by Podsiadlowski et al. Moreover, a Doppler tomogram of the Ha line reveals two distinct regions of enhanced emission. While one is the result of the stream-disk impact, the other is probably attributable to spiral disk structure generated when material in the outer disk achieves a 2:1 orbital resonance with respect to the donor. C1 [Littlefield, C.; Garnavich, P.; Magno, K.] Univ Notre Dame, Dept Phys, Notre Dame, IN 46556 USA. [Applegate, A.] Georgian Court Univ, Dept Phys, Lakewood, NJ 08701 USA. [Pogge, R.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. [Irwin, J.; Marion, G. H.; Kirshner, R.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Vinko, J.] Univ Szeged, Dept Opt, H-6720 Szeged, Hungary. [Vinko, J.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA. RP Littlefield, C (reprint author), Univ Notre Dame, Dept Phys, Notre Dame, IN 46556 USA. FU NSF [AST-1211196, AST-9987045]; Department of Physics at the University of Notre Dame; NSF Telescope System Instrumentation Program (TSIP); Ohio Board of Regents; Ohio State University Office of Research FX R.P.K. received support from NSF grant AST-1211196.; K.M. and A.A. received funding for this research through the Research Experience for Undergraduates program offered by the Department of Physics at the University of Notre Dame.; The MODS spectrographs were built with funding from the NSF grant AST-9987045 and the NSF Telescope System Instrumentation Program (TSIP), with additional funds from the Ohio Board of Regents and the Ohio State University Office of Research. NR 42 TC 10 Z9 10 U1 0 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 EI 1538-3881 J9 ASTRON J JI Astron. J. PD JUN PY 2013 VL 145 IS 6 AR 145 DI 10.1088/0004-6256/145/6/145 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 147LC UT WOS:000319167400002 ER PT J AU Ahlering, MA Maldonado, JE Eggert, LS Fleischer, RC Western, D Brown, JL AF Ahlering, M. A. Maldonado, J. E. Eggert, L. S. Fleischer, R. C. Western, D. Brown, J. L. TI Conservation outside Protected Areas and the Effect of Human-Dominated Landscapes on Stress Hormones in Savannah Elephants SO CONSERVATION BIOLOGY LA English DT Article DE community-based conservation; fecal DNA; fecal glucocorticoids; Loxodonta africana; noninvasive hormone analysis; protected areas ID LOXODONTA-AFRICANA; REPRODUCTIVE OUTPUT; MICROSATELLITE LOCI; RELATEDNESS; KENYA; POPULATIONS; DEMOGRAPHY; RESPONSES; CONFLICT; PATTERNS AB Biodiversity conservation strategies are increasingly focused on regions outside national protected areas, where animals face numerous anthropogenic threats and must coexist with human settlements, livestock, and agriculture. The effects of these potential threats are not always clear, but they could have profound implications for population viability. We used savannah elephants (Loxodonta africana) as a case study to assess the physiological stress associated with living in a human-livestock-dominated landscape. We collected samples over two 3-month periods in 2007 and 2008. We used fecal DNA to identify 96 individual elephants in a community conservation area (CCA) and measured fecal glucocorticoid metabolite (FGM) concentrations as a proxy for stress. The CCA is community Maasai land managed for livestock and wildlife. We compared the FGM concentrations from the CCA to FGM concentrations of 40 elephants in Amboseli National Park and 32 elephants in the Maasai Mara National Reserve, where human settlements and intense livestock grazing were absent. In the CCA, we found no significant individual differences in FGM concentrations among the elephants in 2007 (p = 0.312) or 2008 (p = 0.412) and no difference between years (p = 0.616). The elephants in the CCA had similar FGM concentrations to the Maasai Mara population, but Amboseli elephants had significantly lower FGM concentrations than those in either Maasai Mara or the CCA (Tukey pairwise test, p < 0.001), due primarily to females excreting significantly lower FGM relative to males (p = 0.025). In the CCA, there was no relation among female group size, average pairwise group relatedness, and average group FGM concentration. We found no clear evidence of chronic stress in elephants living on CCA communal land, which is encouraging for conservation strategies promoting the protection of animals living outside protected areas. C1 [Ahlering, M. A.; Eggert, L. S.] Univ Missouri, Div Biol Sci, Columbia, MO 65211 USA. [Ahlering, M. A.; Maldonado, J. E.; Fleischer, R. C.] Smithsonian Conservat Biol Inst, Ctr Conservat & Evolutionary Genet, Washington, DC 20008 USA. [Maldonado, J. E.] Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Washington, DC 20013 USA. [Ahlering, M. A.; Western, D.] African Conservat Ctr, Nairobi, Kenya. [Brown, J. L.] Smithsonian Conservat Biol Inst, Ctr Species Survival, Front Royal, VA 22630 USA. RP Ahlering, MA (reprint author), Nature Conservancy, 10 Cornell St Stop 9019, Grand Forks, ND 58202 USA. EM mahlering@tnc.org FU African Conservation Centre; South Rift Association of Land Owners; University of Missouri Research Board; Center for Conservation and Evolutionary Genetics at the Smithsonian Conservation Biology Institute; Center for Species Survival at the Smithsonian Conservation Biology Institute; Smithsonian Postdoctoral Fellowship Program; Friends of the National Zoo; American Philosophical Society; Liz Claiborne and Art Ortenberg Foundation FX We thank staff at the African Conservation Centre and the South Rift Association of Land Owners for support, especially A. Muchiru, K. Mwathe, J. Kamanga, J. Muriuki, J. Nyamu, and J. Worden. We especially thank A. Kuseyo, P. Meiponyi, and S. Russell for field help and A. Johnson and the Eggert lab for lab assistance. This study was supported by the University of Missouri Research Board, the Center for Conservation and Evolutionary Genetics, and the Center for Species Survival at the Smithsonian Conservation Biology Institute, the Smithsonian Postdoctoral Fellowship Program, Friends of the National Zoo, the American Philosophical Society, and the Liz Claiborne and Art Ortenberg Foundation. NR 41 TC 7 Z9 7 U1 17 U2 121 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0888-8892 J9 CONSERV BIOL JI Conserv. Biol. PD JUN PY 2013 VL 27 IS 3 BP 569 EP 575 DI 10.1111/cobi.12061 PG 7 WC Biodiversity Conservation; Ecology; Environmental Sciences SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 150OD UT WOS:000319399600017 PM 23692020 ER PT J AU Freeman, CJ Thacker, RW Baker, DM Fogel, ML AF Freeman, Christopher J. Thacker, Robert W. Baker, David M. Fogel, Marilyn L. TI Quality or quantity: is nutrient transfer driven more by symbiont identity and productivity than by symbiont abundance? SO ISME JOURNAL LA English DT Article DE cyanobacteria; microbial symbionts; nutrient exchange; porifera; stable isotopes; symbiosis ID MARINE SPONGES; CYANOBACTERIAL SYMBIONTS; MICROBIAL COMMUNITIES; CORAL; DIVERSITY; EVOLUTION; HOST; MICROORGANISMS; ANIMALS; ECOLOGY AB By forming symbiotic interactions with microbes, many animals and plants gain access to the products of novel metabolic pathways. We investigated the transfer of symbiont-derived carbon and nitrogen to the sponges Aplysina cauliformis, Aplysina fulva, Chondrilla caribensis, Neopetrosia subtriangularis and Xestospongia bocatorensis, all of which host abundant microbial populations, and Niphates erecta, which hosts a sparse symbiont community. We incubated sponges in light and dark bottles containing seawater spiked with C-13-and N-15-enriched inorganic compounds and then measured C-13 and N-15 enrichment in the microbial (nutrient assimilation) and sponge (nutrient transfer) fractions. Surprisingly, although most sponges hosting abundant microbial communities were more enriched in C-13 than N. erecta, only N. subtriangularis was more enriched in N-15 than N. erecta. Although photosymbiont abundance varied substantially across species, C-13 and N-15 enrichment was not significantly correlated with photosymbiont abundance. Enrichment was significantly correlated with the ratio of gross productivity to respiration (P:R), which varied across host species and symbiont phylotype. Because irradiance impacts P:R ratios, we also incubated A. cauliformis in C-13-enriched seawater under different irradiances to determine whether symbiont carbon fixation and transfer are dependent on irradiance. Carbon fixation and transfer to the sponge host occurred in all treatments, but was greatest at higher irradiances and was significantly correlated with P:R ratios. Taken together, these results demonstrate that nutrient transfer from microbial symbionts to host sponges is influenced more by host-symbiont identities and P:R ratios than by symbiont abundance. C1 [Freeman, Christopher J.; Thacker, Robert W.] Univ Alabama Birmingham, Dept Biol, Birmingham, AL 35294 USA. [Baker, David M.; Fogel, Marilyn L.] Carnegie Inst Sci, Geophys Lab, Washington, DC USA. [Baker, David M.] Natl Museum Nat Hist, Smithsonian Inst, Washington, DC 20560 USA. RP Freeman, CJ (reprint author), Smithsonian Marine Stn Ft Pierce, 701 Seaway Dr, Ft Pierce, FL 34949 USA. EM cjfre_freeman@yahoo.com FU Smithsonian Tropical Research Institute Short-Term Fellowship; US National Science Foundation [0726944, 0829986]; Smithsonian Institution Marine Science Network Postdoctoral Fellowship; Carnegie Institution of Washington; WM Keck Foundation [072000] FX We thank R Collin, G Jacome and P Gondola at the Smithsonian Tropical Research Institute Bocas Research Station and Roxane Bowden, Geophysical Laboratory for technical assistance. Financial support for this project came from a Smithsonian Tropical Research Institute Short-Term Fellowship, a Sigma Xi Grants-in-Aid of Research to CJF, US National Science Foundation Grants 0726944 and 0829986 to RWT and a Smithsonian Institution Marine Science Network Postdoctoral Fellowship awarded to DMB; the Carnegie Institution of Washington to DMB and MLF, and the WM Keck Foundation (072000) to MLF. NR 37 TC 21 Z9 21 U1 5 U2 65 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 1751-7362 J9 ISME J JI ISME J. PD JUN PY 2013 VL 7 IS 6 BP 1116 EP 1125 DI 10.1038/ismej.2013.7 PG 10 WC Ecology; Microbiology SC Environmental Sciences & Ecology; Microbiology GA 149PP UT WOS:000319333600006 PM 23407307 ER PT J AU Campbell, JE Fourqurean, JW AF Campbell, Justin E. Fourqurean, James W. TI Effects of in situ CO2 enrichment on the structural and chemical characteristics of the seagrass Thalassia testudinum SO MARINE BIOLOGY LA English DT Article ID BANKS EX KONIG; CARBON-DIOXIDE; OCEAN ACIDIFICATION; TURTLE GRASS; ELEVATED CO2; NITROGEN LIMITATION; POSIDONIA-OCEANICA; ZOSTERA-MARINA; CLIMATE-CHANGE; SOUTH FLORIDA AB Seagrasses commonly display carbon-limited photosynthetic rates. Thus, increases in atmospheric pCO(2), and consequentially oceanic CO2(aq) concentrations, may prove beneficial. While addressed in mesocosms, these hypotheses have not been tested in the field with manipulative experimentation. This study examines the effects of in situ CO2(aq) enrichment on the structural and chemical characteristics of the tropical seagrass, Thalassia testudinum. CO2(aq) availability was manipulated for 6 months in clear, open-top chambers within a shallow seagrass meadow in the Florida Keys (USA), reproducing forecasts for the year 2100. Structural characteristics (leaf area, leaf growth, shoot mass, and shoot density) were unresponsive to CO2(aq) enrichment. However, leaf nitrogen and phosphorus content declined on average by 11 and 21 %, respectively. Belowground, non-structural carbohydrates increased by 29 %. These results indicate that increased CO2(aq) availability may primarily alter the chemical composition of seagrasses, influencing both the nutrient status and resilience of these systems. C1 [Campbell, Justin E.; Fourqurean, James W.] Florida Int Univ, Marine Sci Program, Dept Biol Sci, North Miami, FL 33181 USA. [Campbell, Justin E.; Fourqurean, James W.] Florida Int Univ, Southeast Environm Res Ctr, North Miami, FL 33181 USA. RP Campbell, JE (reprint author), Smithsonian Marine Stn, 701 Seaway Dr, Ft Pierce, FL 34949 USA. EM campbellju@si.edu RI Fourqurean, James/B-4606-2008 OI Fourqurean, James/0000-0002-0811-8500 FU National Science Foundation through the Florida Coastal Everglades Long-Term Ecological Research Program [DBI-0620409]; Florida International University FX We thank Dr. Patrick Rice and the Florida Keys Community College for logistical support. Rebecca Bernard, Jeana Drake, Pamela Parker, and Bryan Dewsbury provided assistance in the field. This work was supported by the National Science Foundation through the Florida Coastal Everglades Long-Term Ecological Research Program under Grant No. DBI-0620409, and a Graduate School Doctoral Evidence Acquisition Fellowship awarded by Florida International University. This is contribution number 603 from the Southeast Environmental Research Center at FIU. NR 58 TC 20 Z9 20 U1 2 U2 71 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0025-3162 EI 1432-1793 J9 MAR BIOL JI Mar. Biol. PD JUN PY 2013 VL 160 IS 6 BP 1465 EP 1475 DI 10.1007/s00227-013-2199-3 PG 11 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA 149ZN UT WOS:000319360100015 ER PT J AU Zabin, CJ Danner, EM Baumgartner, EP Spafford, D Miller, KA Pearse, JS AF Zabin, Chela J. Danner, Eric M. Baumgartner, Erin P. Spafford, David Miller, Kathy Ann Pearse, John S. TI A comparison of intertidal species richness and composition between Central California and Oahu, Hawaii SO MARINE ECOLOGY-AN EVOLUTIONARY PERSPECTIVE LA English DT Review DE Climate change; range shifts; rocky shores; temporal comparisons; tropical islands; tropical versus temperate ID TROPICAL ROCKY SHORE; CLIMATE-CHANGE; CITIZEN SCIENCE; COMMUNITY ORGANIZATION; LATITUDINAL GRADIENTS; NORTHEAST PACIFIC; PHYSICAL STRESS; TIME SCALES; DIVERSITY; PATTERNS AB The intertidal zone of tropical islands is particularly poorly known. In contrast, temperate locations such as California's Monterey Bay are fairly well studied. However, even in these locations, studies have tended to focus on a few species or locations. Here we present the results of the first broadscale surveys of invertebrate, fish and algal species richness from a tropical island, Oahu, Hawaii, and a temperate mainland coast, Central California. Data were gathered through surveys of 10 sites in the early 1970s and again in the mid-1990s in San Mateo and Santa Cruz counties, California, and of nine sites in 20012005 on Oahu. Surveys were conducted in a similar manner allowing for a comparison between Oahu and Central California and, for California, a comparison between time periods 24years apart. We report a previously undocumented richness of intertidal species in both locations: 516 for Oahu and 801 for Central California. Surprisingly, when differences in search efforts are controlled, overall (alpha) diversity appears to be similar between locations, although site level (beta) diversity is much higher in California. Species richness in California generally increased along a wave exposure gradient and distance from an urban area. Much higher numbers of both invasive and endemic species were found on Oahu. In California, more invertebrate species were found in the 1990s, likely due to an improvement in taxonomic resources since the 1970s, and species composition was different in the two surveys due to the high incidence of rare species. Although some southern species increased in number between the two time periods and some northern species decreased, we detected little evidence of change favoring southern or northern species. These results are in line with recent findings that water temperatures in the Monterey Bay have been in a cooling trend since the 1980s, in contrast to many locations elsewhere in the world. C1 [Zabin, Chela J.] Smithsonian Environm Res Ctr, Tiburon, CA 94920 USA. [Zabin, Chela J.] Univ Calif Davis, Dept Environm Sci & Policy, Davis, CA 95616 USA. [Danner, Eric M.] SW Fisheries Sci Ctr, Santa Cruz, CA USA. [Baumgartner, Erin P.] Western Oregon Univ, Dept Biol, Monmouth, OR USA. [Spafford, David] Univ Hawaii, Dept Bot, Manoa, HI USA. [Miller, Kathy Ann] Univ Calif Berkeley, Univ Herbarium, Berkeley, CA 94720 USA. [Pearse, John S.] Univ Calif Santa Cruz, Dept Ecol & Evolutionary Biol, Santa Cruz, CA 95064 USA. RP Zabin, CJ (reprint author), Smithsonian Environm Res Ctr, 3152 Paradise Dr, Tiburon, CA 94920 USA. EM zabinc@si.edu FU California Sea Grant [R/CA-8, R/CA-10]; NOAA [NA36RG0537]; California Sea Grant through NOAA's National Sea Grant College Program, U.S. Department of Commerce [R/CZ-132]; California Natural Resources Agency [OCA61588]; National Science Foundation [0232016] FX The Central California surveys in the 1970s were supported by California Sea Grant #R/CA-8 and R/CA-10 to W. T. Doyle, and those in the 1990s by NOAA Grant #NA36RG0537, California Sea Grant Project #R/CZ-132 to J. S. Pearse through NOAA's National Sea Grant College Program, U.S. Department of Commerce; and was supported in part by OCA61588 (e.g. the California Natural Resources Agency). The Oahu surveys were supported by the National Science Foundation Graduate Fellowship in K-12 Teaching program (NSF Training Grants 0232016). The statements, findings, conclusions and recommendations are those of the authors and do not necessarily reflect the views of the aforementioned organizations. NR 136 TC 2 Z9 2 U1 5 U2 57 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0173-9565 J9 MAR ECOL-EVOL PERSP JI Mar. Ecol.-Evol. Persp. PD JUN PY 2013 VL 34 IS 2 BP 131 EP 156 DI 10.1111/maec.12007 PG 26 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA 150VV UT WOS:000319420400001 ER PT J AU Carvalho, JC Cardoso, P Borges, PAV Schmera, D Podani, J AF Carvalho, Jose C. Cardoso, Pedro Borges, Paulo A. V. Schmera, Dnes Podani, Janos TI Measuring fractions of beta diversity and their relationships to nestedness: a theoretical and empirical comparison of novel approaches SO OIKOS LA English DT Article ID PRESENCE-ABSENCE DATA; TURNOVER; ARTHROPODS; COMPONENTS; GRADIENTS; RICHNESS; PATTERNS; DRIVERS; MAMMALS; AZORES AB Beta diversity and nestedness are central concepts of ecology and biogeography and evaluation of their relationships is in the focus of contemporary ecological and conservation research. Beta diversity patterns are originated from two distinct processes: the replacement (or turnover) of species and the loss (or gain) of species leading to richness differences. Nested distributional patterns are generally thought to have a component deriving from beta diversity which is independent of replacement processes. Quantification of these phenomena is often made by calculating a measure of beta diversity, and the resulting value being subsequently partitioned into a contribution by species replacement plus a fraction shared by beta diversity and nestedness. Three methods have been recently proposed for such partitioning, all of them based on pairwise comparisons of sites. In this paper, the performance of these methods was evaluated on theoretical grounds and tested by a simulation study in which different gradients of dissimilarity, with known degrees of species replacement and species loss, were created. Performance was also tested using empirical data addressing land-use induced changes in endemic arthropod communities of the Terceira Island in the Azores. We found that the partitioning of cc (dissimilarity in terms of the Jaccard index) into two additive fractions, -3 (dissimilarity due to species replacement) plus rich (dissimilarity due to richness differences) reflects the species replacement and species loss processes across the simulated gradients in an ecologically and mathematically meaningful way, whilst the other two methods lack mathematical consistency and prove conceptually self-contradictory. Moreover, the first method identified a selective local extinction process for endemic arthropods, triggered by land-use changes, while the latter two methods overweighted the replacement component and led to false conclusions. Their basic flaw derives from the fact that the proposed replacement and nestedness components (deemed to account for species loss) are not scaled in the same way as the measure that accounts for the total dissimilarity (SOrensen and Jaccard indices). We therefore recommend the use of cc=-3+rich, since its components are scaled in the same units and their responses are proportional to the replacement and the gain/loss of species. C1 [Carvalho, Jose C.; Cardoso, Pedro; Borges, Paulo A. V.] Univ Acores, Azorean Biodivers Grp CITA A, PT-9700042 Terceira, Azores, Portugal. [Carvalho, Jose C.] Univ Minho, Dept Biol, CBMA Mol & Environm Ctr, PT-4710057 Braga, Portugal. [Cardoso, Pedro] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA. [Schmera, Dnes] Univ Basel, Sect Conservat Biol, CH-4056 Basel, Switzerland. [Schmera, Dnes] Hungarian Acad Sci, Ctr Ecol Res, Balaton Limnol Inst, HU-8237 Tihany, Hungary. [Podani, Janos] Eotvos Lorand Univ, Dept Plant Systemat Ecol & Theoret Biol, Inst Biol, HU-1117 Budapest, Hungary. [Podani, Janos] Hungarian Acad Sci, Ecol Res Grp, HU-1117 Budapest, Hungary. RP Carvalho, JC (reprint author), Univ Acores, Azorean Biodivers Grp CITA A, Rua Capitao Joao d'Avila, PT-9700042 Terceira, Azores, Portugal. EM josecarvalho@bio.uminho.pt RI Schmera, Denes/B-1617-2010; Borges, Paulo/B-2780-2008; Podani, Janos/G-3074-2014; Cardoso, Pedro/A-8820-2008 OI Schmera, Denes/0000-0003-1248-8413; Borges, Paulo/0000-0002-8448-7623; Podani, Janos/0000-0002-1452-1486; Cardoso, Pedro/0000-0001-8119-9960 FU Luso-American Foundation; Portuguese Foundation for Science and Technology [SFRH/BPD/40688/2007]; project 'Reservas Florestais dos Acores: Cartografia e Inventariacao dos Artropodes Endemicos dos Acores' [17.01 - 080203]; project 'Consequences of land-use change on Azorean fauna and flora - the Target' [DRCT M.2.1.2/I/003/2008] FX We thank D. Bonte and C. Ricotta for helpful comments. JCC expresses his gratitude to the Luso-American Foundation for its support (FLAD CandT Links 2010 grant). PC was supported by the Portuguese Foundation for Science and Technology (SFRH/BPD/40688/2007). Data used in this study were obtained in projects 'Reservas Florestais dos Acores: Cartografia e Inventariacao dos Artropodes Endemicos dos Acores' (PROJ. 17.01 - 080203) and 'Consequences of land-use change on Azorean fauna and flora - the 2010 Target' (Ref: DRCT M.2.1.2/I/003/2008). NR 35 TC 41 Z9 43 U1 6 U2 90 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0030-1299 J9 OIKOS JI Oikos PD JUN PY 2013 VL 122 IS 6 BP 825 EP 834 DI 10.1111/j.1600-0706.2012.20980.x PG 10 WC Ecology SC Environmental Sciences & Ecology GA 150RJ UT WOS:000319408300003 ER PT J AU Clough, GW AF Clough, G. Wayne TI Untitled 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 JUN PY 2013 VL 44 IS 3 BP 6 EP 6 PG 1 WC Humanities, Multidisciplinary SC Arts & Humanities - Other Topics GA 154CS UT WOS:000319649700002 ER PT J AU Craven, D Hall, JS Ashton, MS Berlyn, GP AF Craven, D. Hall, J. S. Ashton, M. S. Berlyn, G. P. TI Water-use efficiency and whole-plant performance of nine tropical tree species at two sites with contrasting water availability in Panama SO TREES-STRUCTURE AND FUNCTION LA English DT Article DE Carbon isotope; Wood traits; Wood density; WUE; Plasticity; Functional traits; Central America ID CARBON-ISOTOPE DISCRIMINATION; WOOD SPECIFIC-GRAVITY; RAIN-FOREST; PHENOTYPIC PLASTICITY; DRY FOREST; SHADE TOLERANCE; INTERSPECIFIC VARIABILITY; ECOPHYSIOLOGICAL TRAITS; FUNCTIONAL TRAITS; ADULT STATURE AB Across their natural distributions, tropical tree species are regularly exposed to seasonal droughts of varying intensities. Their ability to tolerate drought stress plays a vital role in determining growth and mortality rates, as well as shaping the functional composition of tropical forests. In order to assess the ability of species to acclimate to contrasting levels of drought stress, physiological and structural traits involved in drought adaptation-wood C isotope discrimination (delta C-13), wood specific gravity, and wood C content-of 2-year-old saplings of nine tropical tree species were evaluated in common garden experiments at two study sites in Panama with contrasting seasonality. We assessed co-variation in wood traits with relative growth rates (RGR(BD)), aboveground biomass, and basal diameter and the plasticity of wood traits across study sites. Overall, species responded to lower water availability by increasing intrinsic water-use efficiency, i.e., less negative wood delta C-13, but did not exhibit a uniform, directional response for wood specific gravity or wood C content. Trait plasticity for all wood traits was independent of RGR(BD) and tree size. We found that the adaptive value of intrinsic water-use efficiency varied with water availability. Intrinsic water-use efficiency increased with decreasing RGR(BD) at the more seasonal site, facilitating higher survival of slower growing species. Conversely, intrinsic water-use efficiency increased with tree size at the less seasonal site, which conferred a competitive advantage to larger individuals at the cost of greater susceptibility to drought-induced mortality. Our results illustrate that acclimation to water availability has negligible impacts on tree growth over short periods, but eventually could favor slow-growing species with conservative water-use strategies in tropical regions experiencing increasingly frequent and severe droughts. C1 [Craven, D.; Ashton, M. S.; Berlyn, G. P.] Yale Univ, Sch Forestry & Environm Studies, New Haven, CT 06511 USA. [Craven, D.; Hall, J. S.] Smithsonian Trop Res Inst, Ctr Trop Forest Sci, Native Species Reforestn Project PRORENA, Panama City, Panama. RP Craven, D (reprint author), Yale Univ, Sch Forestry & Environm Studies, 370 Prospect St, New Haven, CT 06511 USA. EM dylan.craven@aya.yale.edu RI Craven, Dylan/K-2717-2012 OI Craven, Dylan/0000-0003-3940-833X FU Frank Levinson Family Foundation; Frank Levinson Donor-Advised Fund at the Peninsula Community Foundation, Yale University; STRI; Lewis B. Cullman Fellowship for Dissertation Research; Tropical Research Institute FX This article is a scientific contribution of the Native Species Reforestation Project (PRORENA), a collaborative research program of the Center for Tropical Forest Science (CTFS) at the Smithsonian Tropical Research Institute (STRI) and the School of Forestry and Environmental Studies at Yale University. The species selection trial at Rio Hato was managed by PRORENA through an agreement with Panama's National Environmental Authority (ANAM) and the land at Las Lajas was made available by Forest Finance. Export permits for wood and leaf samples were obtained from ANAM. We thank the field technicians and support staff of PRORENA and CTFS for their considerable efforts in establishing and maintaining the species selection trials at Rio Hato and Las Lajas. We are especially grateful for the help of the following people at different stages of this study: Yael Camacho, Mark Wishnie, Marcos Garcia, Julio Nunez, Leidy Martinez, Anabel Rivas, Norma Cedeno, Rivieth de Leon, Adriana Sautu, Marla Diaz, Rolando Perez, Gerard Olack, Helmut Ernstberger, Jonas Karosas, Mark Bradford, Christian Salas, Charles Nock, and Nathaly Guerrero. This research was made possible through the generous financial support of the Frank Levinson Family Foundation, the Frank Levinson Donor-Advised Fund at the Peninsula Community Foundation, Yale University, and STRI. DC was supported by the Lewis B. Cullman Fellowship for Dissertation Research and the Tropical Research Institute. NR 106 TC 10 Z9 11 U1 2 U2 106 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0931-1890 J9 TREES-STRUCT FUNCT JI Trees-Struct. Funct. PD JUN PY 2013 VL 27 IS 3 BP 639 EP 653 DI 10.1007/s00468-012-0818-0 PG 15 WC Forestry SC Forestry GA 145KX UT WOS:000319015800015 ER PT J AU Gowaty, PA Hubbell, SP AF Gowaty, Patricia Adair Hubbell, Stephen P. TI Bayesian animals sense ecological constraints to predict fitness and organize individually flexible reproductive decisions SO BEHAVIORAL AND BRAIN SCIENCES LA English DT Editorial Material ID TIME AB A quantitative theory of reproductive decisions (Gowaty & Hubbell 2009) says that individuals use updated priors from constantly changing demographic circumstances to predict their futures to adjust actions flexibly and adaptively. Our ecological/evolutionary models of ultimate causes seem consistent with Clark's ideas and thus suggest an opportunity for a unified proximate and ultimate theory of Bayesian animal brains, senses, and actions. C1 [Gowaty, Patricia Adair] Dept Ecol & Evolutionary Biol, Los Angeles, CA 90095 USA. Inst Environm & Sustainabil, Los Angeles, CA 90095 USA. Smithsonian Trop Res Inst, Unit 9100, Dpo, AA 34002 USA. RP Gowaty, PA (reprint author), Dept Ecol & Evolutionary Biol, Los Angeles, CA 90095 USA. EM gowaty@eeb.ucla.edu; shubbell@eeb.ucla.edu NR 4 TC 2 Z9 2 U1 0 U2 13 PU CAMBRIDGE UNIV PRESS PI NEW YORK PA 32 AVENUE OF THE AMERICAS, NEW YORK, NY 10013-2473 USA SN 0140-525X EI 1469-1825 J9 BEHAV BRAIN SCI JI Behav. Brain Sci. PD JUN PY 2013 VL 36 IS 3 BP 215 EP 216 DI 10.1017/S0140525X12002385 PG 2 WC Psychology, Biological; Behavioral Sciences; Neurosciences SC Psychology; Behavioral Sciences; Neurosciences & Neurology GA 143ZT UT WOS:000318909200013 PM 23663591 ER PT J AU Stoffolano, JG Rice, M Murphy, WL AF Stoffolano, John G., Jr. Rice, Marian Murphy, William L. TI The importance of antennal mechanosensilla of Sepedon fuscipennis (Diptera: Sciomyzidae) SO CANADIAN ENTOMOLOGIST LA English DT Article ID BIOLOGICAL-CONTROL; LEPIDOPTERA; TORTRICIDAE AB The styli, often called the aristae, of the antennae of adult Sepedon fuscipennis Loew (Diptera: Sciomyzidae) are shown to possess mechanosensilla, the number and arrangement of which differ between the sexes. It is suggested that the mechanosensilla provide sensory input to the female regarding the touching, or appositioning, of her styli by the male with his forelegs during copulation. Among the Sciomyzidae, S. fuscipennis males are unique in appositioning the antennae of the female during mating. Large clusters of pollen found on the styli of both sexes suggest that mechanosensilla and chemosensilla also provide sensory information about potential sources of food such as nectar (i.e., carbohydrates). C1 [Stoffolano, John G., Jr.] Univ Massachusetts, Div Entomol, Dept Plant Soil & Insect Sci, Amherst, MA 01003 USA. [Rice, Marian] Mt Holyoke Coll, Dept Biol Sci, S Hadley, MA 01075 USA. [Murphy, William L.] Smithsonian Inst, Fishers, IN 46038 USA. RP Stoffolano, JG (reprint author), Univ Massachusetts, Div Entomol, Dept Plant Soil & Insect Sci, Amherst, MA 01003 USA. EM stoff@ent.umass.edu FU Massachusetts Agricultural Experiment Station [MAS-00983] FX This research was supported by the Massachusetts Agricultural Experiment Station (MAS-00983 to J.G.S.) and is published as Contribution No. 3482 from the Massachusetts Agricultural Experiment Station. Funds from the Crampton Fund from the Division of Entomology, Department of Plant, Soil, and Insect Sciences, helped defray the cost of publication. Thanks to Ray Miller, Pietermaritzburg, University of KwaZulu-Natal, Scottsville, South Africa, for collecting and assisting in getting the SEM of S. testacea. Appreciation is extended to Elyssa Longo and Emily Errico for collecting and maintaining flies during the summer of 2009. Thanks to Lloyd Knutson for encouraging this study and to Rory McDonnell and Amnon Freidberg for reading the manuscript and making suggestions. Finally, thanks to all reviewers for important suggestions and editorial comments. NR 28 TC 1 Z9 1 U1 0 U2 5 PU CAMBRIDGE UNIV PRESS PI NEW YORK PA 32 AVENUE OF THE AMERICAS, NEW YORK, NY 10013-2473 USA SN 0008-347X J9 CAN ENTOMOL JI Can. Entomol. PD JUN PY 2013 VL 145 IS 3 BP 265 EP 272 DI 10.4039/tce.2012.103 PG 8 WC Entomology SC Entomology GA 143ZM UT WOS:000318908400003 ER PT J AU Riedel, J Dorn, S Plath, M Potvin, C Mody, K AF Riedel, Judith Dorn, Silvia Plath, Mirco Potvin, Catherine Mody, Karsten TI Time matters: Temporally changing effects of planting schemes and insecticide treatment on native timber tree performance on former pasture SO FOREST ECOLOGY AND MANAGEMENT LA English DT Article DE Canopy stratification; Edge effects; Herbivory; Restoration; Smallholder forestry; Tree protection ID RAIN-FOREST; AGRICULTURAL LANDSCAPES; MIXED PLANTATIONS; TROPICAL PASTURE; NEOTROPICAL TREE; EARLY GROWTH; PANAMA; REFORESTATION; ACCUMULATION; BIODIVERSITY AB Reforestation of former pastures with native timber trees holds potential to improve small-scale farmers livelihoods while supporting ecosystem functioning and biological diversity. To promote successful reforestation with native tree species, more knowledge is needed, particularly on effects of species identity, tree diversity, and insecticide application on tree survival and growth at different time periods after plantation establishment. We assessed these effects for three native Central American timber species and compared results gained 2 and 5 years after tree establishment. Survival, stem diameter, and tree height were quantified for Tabebuia rosea, Anacardium excelsum, and Cedrela odorata, planted in (1) monocultures, (2) three-species mixtures, and (3) three-species mixtures treated with insecticides during the first 2 years of seedling establishment. We further tested how survival and growth performance were affected by the individual tree position within reforestation tree stands to account for border effects in small-scale tree patches in pasture-afforestations. Survival was significantly affected by tree species identity with the highest survival in T. rosea and the lowest survival in C. odorata. Tree growth was affected by tree species identity, tree diversity, insecticide treatment, environmental heterogeneity, and border effects, but these effects varied across the individual tree species. Interspecific analyses revealed significant differences between species. A. excelsum trees attained the largest and C. odorata the smallest size after 5 years of growth. Across species, tree growth in years 3-5 after tree planting was highest in mixtures treated with insecticides during tree establishment, followed by monocultures and then unprotected mixtures. Enhanced growth in monocultures compared to unprotected mixtures was particularly found in T. rosea during early establishment, and in A. excelsum at a later stage of tree stand development. Growth-enhancing effects of planting schemes may be related to differential responses to herbivore damage and to tree-tree competition. Positive border effects, i.e. a significantly enhanced growth at the border of a tree stand, were found for T. rosea in all three planting schemes and for A. excelsum in protected mixtures. Our results suggest that besides early, restricted insecticide application, tree diversity within stands should be considered as management measure to enhance timber tree growth on former pasture. The finding of enhanced growth of native timber trees at the border of small tree stands suggests small patches of native timber trees planted on former pasture as a promising reforestation strategy in Latin America. (C) 2013 Elsevier B.V. All rights reserved. C1 [Riedel, Judith; Dorn, Silvia; Plath, Mirco; Mody, Karsten] Swiss Fed Inst Technol, Inst Agr Sci, CH-8092 Zurich, Switzerland. [Potvin, Catherine] McGill Univ, Dept Biol, Montreal, PQ H3A 1B1, Canada. [Potvin, Catherine] Smithsonian Trop Res Inst, Ancon 084303092, Apartado, Panama. RP Mody, K (reprint author), Tech Univ Darmstadt, Inst Biol, Schnittspahnstr 3, D-64287 Darmstadt, Germany. EM mody@bio.tu-darmstadt.de FU ETH North-South Centre FX We thank Hector Barrios (University of Panama and Smithsonian Tropical Research Institute) for support with the project management, which was also granted by the Panamanian National Environmental Authority (ANAM), and Jose Monteza and Sardinilla personnel for assistance with fieldwork. We thank Heather Kirk (ETH Zurich) and two anonymous reviewers for useful comments on the manuscript. This study has been supported by the Research Fellow Partnership Program (RFPP) of the ETH North-South Centre. NR 57 TC 7 Z9 7 U1 5 U2 48 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 JUN 1 PY 2013 VL 297 BP 49 EP 56 DI 10.1016/j.foreco.2013.02.003 PG 8 WC Forestry SC Forestry GA 142ZH UT WOS:000318835600005 ER PT J AU Schweizer, D Gilbert, GS Holl, KD AF Schweizer, Daniella Gilbert, Gregory S. Holl, Karen D. TI Phylogenetic ecology applied to enrichment planting of tropical native tree species SO FOREST ECOLOGY AND MANAGEMENT LA English DT Article DE Seedling performance; Restoration ecology; Tropical rain forest; Phylogenetic ecology; Enrichment planting; Herbivores ID DEPENDENT SEEDLING MORTALITY; RAIN-FOREST TREE; DENSITY-DEPENDENCE; LOCAL ADAPTATION; PATHOGEN INTERACTIONS; ENHANCED SPECIFICITY; NICHE CONSERVATISM; DISPERSAL DISTANCE; HOST-SPECIFICITY; COMMUNITY AB Enrichment planting within established plantations or secondary forests is a common strategy to enhance forest recovery, given that later successional forest species tend to have low dispersal and limited recruitment into these sites. It is difficult, however, to predict how species of seedlings will perform when planted under different overstory species. The field of phylogenetic ecology offers tools to help guide the selection of seedlings, drawing on the evolutionary conservatism of important functional traits. We evaluated the survival, growth, foliar disease, and herbivory of various native tropical tree seedlings at different evolutionary distances from monospecific stands of trees beneath which they were planted. We expected that seedlings planted under conspecific overstory trees would have low survival and growth and high percent foliar damage (as predicted by the Janzen-Connell Hypothesis), and that seedling performance would improve steadily with phylogenetic distance between seedling and overstory species. We found that seedlings planted under conspecific canopies had lower survivorship, reduced growth, and greater foliar damage than seedlings planted under canopies of different tree species. An overall increase in seedling performance with greater phylogenetic distance between seedling and overstory species was dominated by the contrast in performance between conspecific pairs and seedlings planted beneath extra-familial overstory species; but lack of available congeneric pairing limited inference about interactions among close relatives. Most pathogenic fungi isolated from enrichment-planted seedlings also caused disease when inoculated on the overstory tree species where the seedlings had been planted; this is consistent with overstory trees being an important reservoir of pathogens that affect seedlings. We conclude that enrichment planting with species more distantly related to those that dominate the canopy should enhance seedling's performance. Closer analysis at the congeneric level is warranted because of expected strong biotic interactions at close phylogenetic distances. (C) 2013 Elsevier B.V. All rights reserved. C1 [Schweizer, Daniella; Gilbert, Gregory S.; Holl, Karen D.] Univ Calif Santa Cruz, Dept Environm Studies, Santa Cruz, CA 95064 USA. [Gilbert, Gregory S.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. RP Schweizer, D (reprint author), Univ Calif Santa Cruz, Dept Environm Studies, 1156 High St, Santa Cruz, CA 95064 USA. EM daniellaschweizer@gmail.com RI Holl, Karen/D-8033-2014 OI Holl, Karen/0000-0003-2893-6161 FU STEPS Institute for Innovation in Environmental Research at UC Santa Cruz; Smithsonian Tropical Research Institute; UCSC Environmental Studies Department; Center for Tropical Research in Ecology, Agriculture, and Development (CenTREAD); NSF [DEB-0515520, DEB-0842059] FX The authors thank the Smithsonian Tropical Research Institute (STRI) for logistical support and ANAM for granting us permission to conduct research in the republic of Panama. We thank the Native Species Reforestation Project (PRORENA), a collaborative research program led by the Center for Tropical Forest Science at the Smithsonian Tropical Research Institute and the Tropical Resources Institute at the Yale School of Forestry and Environmental Studies, for allowing us the use of their experimental plantation, their nursery, and logistical support. Special thanks to Jose Deago, former PRORENA staff, for his valuable assistance at the beginning of the project and to our field assistants for their hard work. This research was made possible through the financial support to Daniella Schweizer from the STEPS Institute for Innovation in Environmental Research at UC Santa Cruz the Smithsonian Tropical Research Institute, the UCSC Environmental Studies Department, and the Center for Tropical Research in Ecology, Agriculture, and Development (CenTREAD), and to Gregory S. Gilbert from NSF DEB-0515520 and DEB-0842059. NR 81 TC 12 Z9 12 U1 5 U2 72 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 JUN 1 PY 2013 VL 297 BP 57 EP 66 DI 10.1016/j.foreco.2013.02.012 PG 10 WC Forestry SC Forestry GA 142ZH UT WOS:000318835600006 ER PT J AU Watson, R Munro, C Edwards, KL Norton, V Brown, JL Walker, SL AF Watson, Rebecca Munro, Coralie Edwards, Katie L. Norton, Vicki Brown, Janine L. Walker, Susan L. TI Development of a versatile enzyme immunoassay for non-invasive assessment of glucocorticoid metabolites in a diversity of taxonomic species SO GENERAL AND COMPARATIVE ENDOCRINOLOGY LA English DT Article DE Assay development; Biological validation; Enzyme immunoassay; EIA; Glucocorticoids ID CONSERVATION PHYSIOLOGY; STRESS; PLATES; ASSAY; ADSORPTION; INDICATORS; HORMONES; MAMMALS; ELISA; ZOO AB Endocrinology is a useful tool for conservation biologists and animal managers, and measuring glucocorticoids can help understand biological mechanisms associated with species decline and animal welfare. The current study describes the development and optimization of a glucocorticoid enzyme immunoassay (EIA) to non-invasively assess adrenal activity in a variety of taxa. The antiserum (CJM006) was raised in rabbits to a corticosterone-3-CMO-BSA immunogen and used in a standard competitive EIA system. However, the EIA initially produced results with unacceptably high inter-assay variation, attributed to consistent patterns observed within the optical density of developing plates. To determine the cause of this variability, a number of factors were examined using synthetic corticosterone standard and endogenous faecal extract, including: plate type (Nunc MaxiSorp (R) II versus Immulon IB plates); the use of non-specific secondary antibody; type (artificial versus natural) and presence (light versus dark) of light during incubation; plate loading temperature (4 degrees C versus room temperature); and substrate reagent temperature (4 degrees C versus room temperature). Results indicated that variability was associated with plate location effects, which were not initially detected because control samples were always run in the same positions across plates. Light and temperature were the two major factors that affected EIA reliability. For this assay, the standard protocol required slight modification, with the optimal protocol using Nunc MaxiSorp (R) plates, room temperature substrate reagents and dark incubation conditions. Following optimization, this EIA was then validated biochemically for 38 species, through parallel displacement curves and interference assessment tests of faecal and urine samples. Additionally, biological validation was performed opportunistically in a subset of species, with use of this EIA demonstrating significant elevations in faecal glucocorticoid metabolites following potentially challenging events. In summary, this glucocorticoid EIA cross-reacts with excreted glucocorticoid metabolites across a wide range of taxa, including ungulates, primates, felids, birds, rodents and amphibians. We conclude that when used with optimal reagent and incubation conditions, this EIA will be useful for non-invasive monitoring of adrenal activity in a wide range of wildlife species. (C) 2013 Elsevier Inc. All rights reserved. C1 [Watson, Rebecca; Edwards, Katie L.; Norton, Vicki; Walker, Susan L.] Chester Zoo, North England Zool Soc, Chester CH2 1LH, Cheshire, England. [Watson, Rebecca] Univ Glasgow, Glasgow G12 8QQ, Lanark, Scotland. [Munro, Coralie] Univ Calif Davis, Davis, CA 95616 USA. [Edwards, Katie L.] Univ Liverpool, Inst Integrat Biol, Liverpool L69 7ZB, Merseyside, England. [Brown, Janine L.] Smithsonian Conservat Biol Inst, Ctr Species Survival, Front Royal, VA 22630 USA. RP Walker, SL (reprint author), Chester Zoo, North England Zool Soc, Caughall Rd, Chester CH2 1LH, Cheshire, England. EM s.walker@chesterzoo.org RI Edwards, Katie/K-5559-2015 OI Edwards, Katie/0000-0001-6736-1183 NR 33 TC 21 Z9 21 U1 8 U2 79 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0016-6480 J9 GEN COMP ENDOCR JI Gen. Comp. Endocrinol. PD JUN 1 PY 2013 VL 186 BP 16 EP 24 DI 10.1016/j.ygcen.2013.02.001 PG 9 WC Endocrinology & Metabolism SC Endocrinology & Metabolism GA 141UC UT WOS:000318751000003 PM 23462197 ER PT J AU Shurakov, A Tong, CYE Blundell, R Kaurova, N Voronov, B Gol'tsman, G AF Shurakov, Alexander Tong, Cheuk-yu E. Blundell, Raymond Kaurova, Natalia Voronov, Boris Gol'tsman, Gregory TI Microwave Stabilization of a HEB Mixer in a Pulse-Tube Cryocooler SO IEEE TRANSACTIONS ON APPLIED SUPERCONDUCTIVITY LA English DT Article DE Allan variance; hot electron bolometer (HEB) mixer; pulse-tube cryocooler AB We report the results of our study of the stability of an 800 GHz hot electron bolometer (HEB) mixer cooled with a pulse-tube cryocooler. Pulse-tube cryocoolers introduce temperature fluctuations as well as mechanical vibrations at a frequency of similar to 1 Hz, both of which can cause receiver gain fluctuations at that frequency. In our system, the motor of the cryocooler was separated from the cryostat to minimize mechanical vibrations, leaving thermal effects as the dominant source of the receiver gain fluctuations. We measured root mean square temperature variations of the 4 K stage of similar to 7 mK. The HEB mixer was pumped by a solid state local oscillator at 810 GHz. The root mean square current fluctuations at the low noise operating point (1.50 mV, 56.5 mu A) were similar to 0.12 mu A, and were predominantly due to thermal fluctuations. To stabilize the bias current, microwave radiation was injected to the HEB mixer. The injected power level was set by a proportional-integral-derivative controller, which completely compensates for the bias current oscillations induced by the pulse-tube cryocooler. Significant improvement in the Allan variance of the receiver output power was obtained, and an Allan time of 5 s was measured. C1 [Shurakov, Alexander; Tong, Cheuk-yu E.; Blundell, Raymond] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Kaurova, Natalia; Voronov, Boris; Gol'tsman, Gregory] Moscow State Pedag Univ, Moscow 119991, Russia. RP Shurakov, A (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM ashurako@cfa.harvard.edu; etong@cfa.harvard.edu; rblundell@cfa.harvard.edu; nkaurova@yandex.ru; bmvoronov@mail.ru; goltsman@mspu-phys.ru OI Tong, Edward/0000-0002-7736-4203 FU Russian Foundation for Basic Research [12-02-01291-a] FX This work was supported in part by the Russian Foundation for Basic Research under Grant 12-02-01291-a. NR 15 TC 3 Z9 3 U1 0 U2 8 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 1051-8223 EI 1558-2515 J9 IEEE T APPL SUPERCON JI IEEE Trans. Appl. Supercond. PD JUN PY 2013 VL 23 IS 3 AR 1501504 DI 10.1109/TASC.2013.2241591 PN 1 PG 4 WC Engineering, Electrical & Electronic; Physics, Applied SC Engineering; Physics GA 143KT UT WOS:000318867100020 ER PT J AU Tong, CYE Grimes, PK Barbier, A Schuster, K Wang, MJ AF Tong, Cheuk-yu Edward Grimes, Paul K. Barbier, Arnaud Schuster, Karl Wang, Ming-jye TI Design and Performance of a 3-Junction Series Distributed SIS Mixer for Wide IF Applications SO IEEE TRANSACTIONS ON APPLIED SUPERCONDUCTIVITY LA English DT Article DE Distributed mixer; IF bandwidth; SIS mixer ID BANDWIDTH AB Series distributed superconductor-insulator-superconductor mixers have been used to provide very wide instantaneous bandwidth of operation. In this paper, we explore a design based on a 3-junction array in which the junctions themselves form part of the RF tuning network of the mixer. We have developed mixers based on these designs for use in the 200 and 300 GHz bands. Receivers incorporating these wideband mixers demonstrate very low noise temperature. At a local oscillator frequency of 300 GHz, the lowest measured intermediate frequency noise temperature is about 42 K and the usable intermediate frequency bandwidth extends from 6 to 16.5 GHz. Both the design theory and experimental results are presented. C1 [Tong, Cheuk-yu Edward; Grimes, Paul K.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Barbier, Arnaud; Schuster, Karl] Inst Radio Astron Millimetr, F-38406 St Martin Dheres, France. [Wang, Ming-jye] Acad Sinica, Inst Astron & Astrophys, Taipei 10617, Taiwan. RP Tong, CYE (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM etong@cfa.harvard.edu; pgrimes@cfa.harvard.edu; barbier@iram.fr; schuster@iram.fr; mingjye@asiaa.sinica.edu.tw OI Tong, Edward/0000-0002-7736-4203 NR 10 TC 4 Z9 4 U1 1 U2 5 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 1051-8223 EI 1558-2515 J9 IEEE T APPL SUPERCON JI IEEE Trans. Appl. Supercond. PD JUN PY 2013 VL 23 IS 3 AR 1400404 DI 10.1109/TASC.2012.2235517 PN 1 PG 4 WC Engineering, Electrical & Electronic; Physics, Applied SC Engineering; Physics GA 143KT UT WOS:000318867100011 ER PT J AU Garcia-Verdugo, C Friar, E Santiago, LS AF Garcia-Verdugo, Carlos Friar, Elizabeth Santiago, Louis S. TI ECOLOGICAL ROLE OF HYBRIDIZATION IN ADAPTIVE RADIATIONS: A CASE STUDY IN THE DUBAUTIA ARBOREA-DUBAUTIA CILIOLATA (ASTERACEAE) COMPLEX SO INTERNATIONAL JOURNAL OF PLANT SCIENCES LA English DT Article DE habitat colonization; hybrid swarm; leaf size; phenotypic novelty; silverswords; water use efficiency ID SILVERSWORD ALLIANCE ASTERACEAE; EUROPAEA SUBSP GUANCHICA; CHLOROPLAST DNA EVIDENCE; OLEA-EUROPAEA; GENE FLOW; HYBRID SPECIATION; MAUNA-KEA; TRAITS; POPULATIONS; EVOLUTION AB Premise of research. Hybridization is a mechanism frequently invoked to account for the spectacular radiations observed in oceanic islands, but, surprisingly, there is little empirical support for its ecological role in island plant radiations. Theory predicts that hybridization should provide individuals with the phenotypic novelty required for habitat shifts, thus promoting conditions for subsequent speciation. In this article, we studied the first stages of this process using two hybridizing species of Dubautia (Asteraceae), the most diversified genus of the Hawaiian silversword radiation. Methodology. Phenotypic and habitat differentiation were investigated in two recently derived species (Dubautia arborea and Dubautia ciliolata) and a hybrid zone. Morphological trait expression and physiological trait expression under field and common garden conditions and microclimatic variation were analyzed to address the patterns of differentiation among parental species and hybrids. Pivotal results. Our analyses showed that parental species occupied contrasting habitats and represented the extremes of phenotypic variation. Conversely, hybrids displayed novel phenotypes outside parental ranges, generating a continuum of intermediate phenotypes in the study system. We also found a strong relationship between morphological and physiological variation and plant performance, which suggests that broad phenotypic variation in hybrids could be favored by the environmental heterogeneity of the hybrid zone. Conclusions. The initial expectations for the ecological role of hybridization in adaptive radiations are confirmed in this Dubautia system, in which hybrids of closely related species display novel morphological and physiological variation associated with the colonization of a new habitat. To understand the evolutionary processes creating an unusual degree of variation within particular lineages, molecular C1 [Garcia-Verdugo, Carlos; Friar, Elizabeth] Rancho Santa Ana Bot Garden, Claremont, CA 91711 USA. [Garcia-Verdugo, Carlos] Univ Calif Berkeley, Dept Integrat Biol, Berkeley, CA 94720 USA. [Garcia-Verdugo, Carlos] Univ Calif Berkeley, Jepson Herbarium, Berkeley, CA 94720 USA. [Friar, Elizabeth] Natl Sci Fdn, Div Environm Biol, Arlington, VA 22230 USA. [Santiago, Louis S.] Univ Calif Riverside, Dept Bot & Plant Sci, Riverside, CA 92521 USA. [Santiago, Louis S.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. RP Garcia-Verdugo, C (reprint author), Rancho Santa Ana Bot Garden, Claremont, CA 91711 USA. EM carlosgarciaverdugo@gmail.com RI Santiago, Louis/E-3185-2016; OI Santiago, Louis/0000-0001-5994-6122; Garcia-Verdugo, Carlos/0000-0003-0332-5583 NR 48 TC 4 Z9 4 U1 1 U2 66 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 JUN PY 2013 VL 174 IS 5 BP 749 EP 759 DI 10.1086/669929 PG 11 WC Plant Sciences SC Plant Sciences GA 145YN UT WOS:000319056100003 ER PT J AU Ballantine, DL Ruiz, H AF Ballantine, D. L. Ruiz, H. TI A unique red algal reef formation in Puerto Rico SO CORAL REEFS LA English DT Editorial Material C1 [Ballantine, D. L.; Ruiz, H.] Univ Puerto Rico, Dept Marine Sci, Mayaguez, PR 00709 USA. [Ballantine, D. L.] Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, Washington, DC 20560 USA. RP Ballantine, DL (reprint author), Univ Puerto Rico, Dept Marine Sci, Mayaguez, PR 00709 USA. EM david.ballantine@upr.edu NR 3 TC 1 Z9 1 U1 0 U2 6 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0722-4028 J9 CORAL REEFS JI Coral Reefs PD JUN PY 2013 VL 32 IS 2 BP 411 EP 411 DI 10.1007/s00338-013-1016-2 PG 1 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA 139FR UT WOS:000318567900010 ER PT J AU Langguth, T Honnen, AC Hailer, F Mizera, T Skoric, S Vali, U Zachos, FE AF Langguth, Tobias Honnen, Ann-Christin Hailer, Frank Mizera, Tadeusz Skoric, Stefan Vali, Ulo Zachos, Frank E. TI Genetic structure and phylogeography of a European flagship species, the white-tailed sea eagle Haliaeetus albicilla SO JOURNAL OF AVIAN BIOLOGY LA English DT Article ID RECENT POPULATION BOTTLENECKS; MITOCHONDRIAL-DNA; MICROSATELLITE DATA; CONTROL REGION; DIVERSITY; SOFTWARE; FALCONIFORMES; HYBRIDIZATION; ACCIPITRIDAE; POLYMORPHISM AB We analysed 120 white-tailed sea eagles Haliaeetus albicilla from eastern (Poland and Estonia) and southeastern (Serbian Danube population) Europe for genetic variability and structuring at the mitochondrial control region and seven nuclear microsatellite loci. We combined this new dataset with sequence and genotype data from previous analyses covering Greenland and Eurasia (total sample sizes of 420 and 186 individuals for mtDNA and microsatellites, respectively) to address the following questions: 1) does the large eastern population in Europe add significantly to the species overall genetic diversity? 2) Do the new sequence data match the clinal distribution pattern (west to east) of the two major mtDNA lineages? 3) Does the preliminary hypothesis of two nuclear genetic clusters recently found in this species hold for the whole of Europe, and do these clusters show a geographic pattern? Our results confirmed Europe as a stronghold of genetic diversity in white-tailed sea eagles, and the east of the continent contributed disproportionately to this, the reason being the admixture of eagles with different genetic background. As hypothesised, both mitochondrial lineages were recovered also in eastern Europe, but the globally more eastern lineage was dominant. The presence of two microsatellite clusters was also confirmed, and these groups, too, show a non-random geographic distribution, with, except for Poland, a high proportion of eastern-type' eagles in the populations of eastcentral and eastern Europe. C1 [Langguth, Tobias] Queens Univ, Dept Biol, Kingston, ON K7L 3N6, Canada. [Langguth, Tobias; Zachos, Frank E.] Univ Kiel, Inst Zool, DE-24118 Kiel, Germany. [Zachos, Frank E.] Nat Hist Museum Vienna, AT-1010 Vienna, Austria. [Honnen, Ann-Christin] Inst Freshwater Ecol & Inland Fisheries Berlin, DE-12587 Berlin, Germany. [Hailer, Frank] Senckenberg Gesell Nat Forsch, BiK F, LOEWE Biodivers & Climate Res Ctr, DE-62325 Frankfurt, Germany. [Hailer, Frank] Goethe Univ Frankfurt, DE-62325 Frankfurt, Germany. [Hailer, Frank] Natl Zool Pk, Smithsonian Conservat Biol Inst, Ctr Conservat & Evolutionary Genet, Washington, DC 20013 USA. [Mizera, Tadeusz] Poznan Univ Life Sci, Dept Zool, PL-60625 Poznan, Poland. [Skoric, Stefan] Univ Belgrade, Inst Multidisciplinary Res, Belgrade 11030, Serbia. [Vali, Ulo] Estonian Univ Life Sci, Inst Agr & Environm Sci, EE-51014 Tartu, Estonia. RP Langguth, T (reprint author), Queens Univ, Dept Biol, Kingston, ON K7L 3N6, Canada. EM frank.zachos@nhm-wien.ac.at RI Hailer, Frank/C-9114-2012; OI Hailer, Frank/0000-0002-2340-1726; Honnen, Ann-Christin/0000-0003-4355-7231 FU 'LOEWE - Landes-Offensive zur Entwicklung Wissenschaftlich-okonomischer Exzellenz' of Hesse, Germany; Smithsonian Conservation Biology Center FX FH was partly supported by the 'LOEWE - Landes-Offensive zur Entwicklung Wissenschaftlich-okonomischer Exzellenz' of Hesse, Germany, and by the Smithsonian Conservation Biology Center. We thank Martin Paeckert for helpful criticisms and comments on an earlier version of this manuscript. NR 49 TC 7 Z9 7 U1 5 U2 48 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0908-8857 J9 J AVIAN BIOL JI J. Avian Biol. PD JUN PY 2013 VL 44 IS 3 BP 263 EP 271 DI 10.1111/j.1600-048X.2012.00075.x PG 9 WC Ornithology SC Zoology GA 142QC UT WOS:000318811100008 ER PT J AU Larjavaara, M Muller-Landau, HC AF Larjavaara, Markku Muller-Landau, Helene C. TI Temperature explains global variation in biomass among humid old-growth forests (vol 21, pg 998, 2012) SO GLOBAL ECOLOGY AND BIOGEOGRAPHY LA English DT Correction C1 [Larjavaara, Markku] Metla, Finnish Forest Res Inst, FI-01301 Vantaa, Finland. [Muller-Landau, Helene C.] Smithsonian Trop Res Inst, Panama City, Panama. RP Larjavaara, M (reprint author), Metla, Finnish Forest Res Inst, Jokiniemenkuja 1,Box 18, FI-01301 Vantaa, Finland. EM markku.larjavaara@gmail.com NR 1 TC 1 Z9 1 U1 1 U2 12 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1466-822X J9 GLOBAL ECOL BIOGEOGR JI Glob. Ecol. Biogeogr. PD JUN PY 2013 VL 22 IS 6 BP 772 EP 772 DI 10.1111/geb.12037 PG 1 WC Ecology; Geography, Physical SC Environmental Sciences & Ecology; Physical Geography GA 138MO UT WOS:000318512900013 ER PT J AU Seeger, A AF Seeger, Anthony TI Burst of Breath: Indigenous Ritual Wind Instruments in Lowland South America. SO JOURNAL OF ANTHROPOLOGICAL RESEARCH LA English DT Book Review C1 [Seeger, Anthony] Univ Calif Los Angeles, Los Angeles, CA 90024 USA. [Seeger, Anthony] Smithsonian Inst, Washington, DC 20560 USA. RP Seeger, A (reprint author), Univ Calif Los Angeles, Los Angeles, CA 90024 USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU UNIV NEW MEXICO, DEPT ANTHROPOL PI ALBUQUERQUE PA MSC01 1040, ANTHROPOLOGY 1, UNIV NEW MEXICO, ALBUQUERQUE, NM 87131 USA SN 0091-7710 EI 2153-3806 J9 J ANTHROPOL RES JI J. Anthropol. Res. PD SUM PY 2013 VL 69 IS 2 BP 289 EP 292 PG 4 WC Anthropology SC Anthropology GA AP7MW UT WOS:000342262400018 ER PT J AU Green, RD AF Green, Rayna D. TI Introduction Miss Indian Pageants in the West SO JOURNAL OF THE WEST LA English DT Editorial Material C1 Amer Museum Nat Hist, Smithsonian Inst, Amer Indian Program, New York, NY 10024 USA. RP Green, RD (reprint author), Amer Museum Nat Hist, Smithsonian Inst, Amer Indian Program, New York, NY 10024 USA. NR 2 TC 0 Z9 0 U1 0 U2 0 PU ABC-CLIO PI SANTA BARBARA PA 130 CREMONA DR, SANTA BARBARA, CA 93117 USA SN 0022-5169 EI 1930-0115 J9 J WEST JI J. West PD SUM PY 2013 VL 52 IS 3 BP 5 EP 9 PG 5 WC History SC History GA V39AN UT WOS:000209384000002 ER PT J AU Siegal-Willott, JL Harr, KE Hall, JO Hayek, LAC Auil-Gomez, N Powell, JA Bonde, RK Heard, D AF Siegal-Willott, Jessica L. Harr, Kendal E. Hall, Jeffery O. Hayek, Lee-Ann C. Auil-Gomez, Nicole Powell, James A. Bonde, Robert K. Heard, Darryl TI BLOOD MINERAL CONCENTRATIONS IN MANATEES (TRICHECHUS MANATUS LATIROSTRIS AND TRICHECHUS MANATUS MANATUS) SO JOURNAL OF ZOO AND WILDLIFE MEDICINE LA English DT Article DE Blood; manatee; mineral; serum; Trichechus manatus ID DUGONG DUGONG-DUGON; BASE-LINE LEVELS; TRACE-METALS; CONTAMINANT CONCENTRATIONS; FLORIDA MANATEE; MARINE MAMMALS; LIVER-TISSUE; FRESH-WATER; SEDIMENTS; ORGANOCHLORINE AB Limited information is available regarding the role of minerals and heavy metals in the morbidity and mortality of manatees. Whole-blood and serum mineral concentrations were evaluated in apparently healthy, free-ranging Florida (Trichechus manatus latirostris, n = 31) and Belize (Trichechus manatus manatus, n 14) manatees. Toxicologic statuses of the animals and of their environment had not been previously determined. Mean mineral whole-blood (WB) and serum values in Florida (FL) and Belize (BZ) manatees were determined, and evaluated for differences with respect to geographic location, relative age, and sex. Mean WB and serum silver, boron, cobalt, magnesium, molybdenum, and WB cadmium concentrations were significantly higher in BZ versus FL manatees (P <= 0.05). Mean WB aluminum, calcium, manganese, sodium, phosphorus, vanadium, and serum zinc concentrations were significantly lower in BZ versus FL manatees. Adult manatees had significant and higher mean WB aluminum, manganese, sodium, antimony, vanadium, and serum manganese and zinc concentrations compared to juvenile animals. Significant and lower mean WB and serum silver, boron, cobalt, and serum copper and strontium concentrations were present in adults compared to juveniles (P <= 0.05). Females had significant and higher mean WB nickel and serum barium compared to males (P <= 0.05). Mean WB arsenic and zinc, and mean serum iron, magnesium, and zinc concentrations fell within toxic ranges reported for domestic species. Results reveal manatee blood mineral concentrations differ with location, age, and sex. Influence from diet, sediment, water, and anthropogenic sources on manatee mineral concentration warrant further investigation. C1 [Siegal-Willott, Jessica L.; Harr, Kendal E.; Heard, Darryl] Univ Florida, Coll Vet Med, Gainesville, FL 32610 USA. [Hall, Jeffery O.] Utah State Univ, Utah Vet Diagnost Lab, Logan, UT 84341 USA. [Hayek, Lee-Ann C.] Smithsonian Inst, NHB MRC 121, Washington, DC 20560 USA. [Auil-Gomez, Nicole] Wildlife Trust, Belize City, Belize. [Bonde, Robert K.] US Geol Survey, Southeast Ecol Sci Ctr, Gainesville, FL 32653 USA. [Powell, James A.] Sea Shore Alliance, St Petersburg, FL 33701 USA. RP Siegal-Willott, JL (reprint author), Smithsonian Natl Zool Pk, Dept Anim Hlth, 3001 Connecticut Ave NW, Washington, DC 20008 USA. EM jess_sw24@hotmail.com OI Harr, Kendal/0000-0001-5390-3586; Bonde, Robert/0000-0001-9179-4376 FU Zoological Medicine Department at the College of Veterinary Medicine, University of Florida; U.S. Fish and Wildlife Service [MA79172-4] FX The authors thank Dr. Adrienne Atkins, James Reid, Andy Garrett, and the expert research teams in Belize and Florida for their help in manatee capture, handling, and data collection. The authors also thank the Florida Fish and Wildlife Conservation Commission for assistance in the field and the Zoological Medicine Department at the College of Veterinary Medicine, University of Florida, for financial assistance. Lastly, the authors thank Dr. Karen Bischoff at Cornell University Veterinary Diagnostic Laboratory and Dr. David Crewz for consultation on this project. This work was conducted under U.S. Fish and Wildlife Service research permit MA79172-4 issued to the U.S. Geological Survey Sirenia Project. All sampling was conducted in accordance with IACUC standards and samples imported under valid CITES permits. Any use of trade, product, or firm names is for descriptive purposes only and does not imply endorsement by the U.S. Government. NR 37 TC 2 Z9 2 U1 1 U2 8 PU AMER ASSOC ZOO VETERINARIANS PI YULEE PA 581705 WHITE OAK ROAD, YULEE, FL 32097 USA SN 1042-7260 EI 1937-2825 J9 J ZOO WILDLIFE MED JI J. Zoo Wildl. Med. PD JUN PY 2013 VL 44 IS 2 BP 285 EP 294 DI 10.1638/2012-0093R PG 10 WC Veterinary Sciences SC Veterinary Sciences GA AM1PS UT WOS:000339620500007 PM 23805546 ER PT J AU Clancy, MM Woc-Colburn, M Viner, T Sanchez, C Murray, S AF Clancy, Meredith M. Woc-Colburn, Margarita Viner, Tabitha Sanchez, Carlos Murray, Suzan TI RETROSPECTIVE ANALYSIS OF MORTALITIES IN ELEPHANT SHREWS (MACROSCELIDIDAE) AND TREE SHREWS (TUPAIIDAE) AT THE SMITHSONIAN NATIONAL ZOOLOGICAL PARK, USA SO JOURNAL OF ZOO AND WILDLIFE MEDICINE LA English DT Article DE elephant shrew; tree shrew; Macroscelididae; Tupaiidae; Cryptococcus spp.; Gongylonema spp.; arteriosclerosis ID INFECTION AB Investigations into the cause of mortality and other important findings at necropsy were made into two families of small mammals at the Smithsonian National Zoological Park (SNZP; USA). Necropsy reports from 1976 through 2008 were reviewed for all elephant shrews in family Macroscelididae (n = 118) and all tree shrews in family Tupaiidae (n = 90) that lived for greater than 30 days at the SNZP. Causes of mortality were classified by body system and etiology to identify prevalent diseases and trends across demographics for each family. In elephant shrews, gastrointestinal disease (n = 18) and respiratory disease (n = 22) were important causes of mortality with an increased prevalence of pneumonia in adult males. Trauma was a common cause of mortality in tree shrews (n = 22). Cryptococcosis was an important cause of mortality in both families (n = 8 elephant shrews; n = 13 tree shrews). Bacterial infections, often systemic at time of mortality, were also common (n = 16 elephant shrews; n = 17 tree shrews). Arteriosclerosis was a common comorbid pathology noted at necropsy in certain populations, seen only in Elephantulus rufescens in the family Macroscelididae (n = 22) and in only males in the family Tupaiidae (n = 11). Gongylonemiasis was seen commonly in tree shrews (n = 15), as a comorbid finding, or in 5 cases directly leading to mortality. Awareness of the prevalence of these diseases can help guide prevention and intervention strategies. C1 [Clancy, Meredith M.; Woc-Colburn, Margarita; Viner, Tabitha; Sanchez, Carlos; Murray, Suzan] Smithsonian Natl Zool Pk, Washington, DC 20008 USA. RP Clancy, MM (reprint author), Wildlife Conservat Soc, Zool Hlth Program, 2300 Southern Blvd, Bronx, NY 10460 USA. EM mclancy@wcs.org NR 20 TC 2 Z9 2 U1 1 U2 7 PU AMER ASSOC ZOO VETERINARIANS PI YULEE PA 581705 WHITE OAK ROAD, YULEE, FL 32097 USA SN 1042-7260 EI 1937-2825 J9 J ZOO WILDLIFE MED JI J. Zoo Wildl. Med. PD JUN PY 2013 VL 44 IS 2 BP 302 EP 309 DI 10.1638/2012-0115R1.1 PG 8 WC Veterinary Sciences SC Veterinary Sciences GA AM1PS UT WOS:000339620500009 PM 23805548 ER PT J AU Sommanustweechai, A Kasantikul, T Somsa, W Wongratanacheewin, S Sermswan, RW Kongmakee, P Thomas, W Kamolnorranath, S Siriaroonrat, B Bush, M Banlunara, W AF Sommanustweechai, Angkana Kasantikul, Tanit Somsa, Wachirawit Wongratanacheewin, Surasakdi Sermswan, Rasana W. Kongmakee, Piyaporn Thomas, Warissara Kamolnorranath, Sumate Siriaroonrat, Boripat Bush, Mitchell Banlunara, Wijit TI ENVIRONMENTAL MANAGEMENT PROCEDURES FOLLOWING FATAL MELIOIDOSIS IN A CAPTIVE CHIMPANZEE (PAN TROGLODYTES) SO JOURNAL OF ZOO AND WILDLIFE MEDICINE LA English DT Article DE Burkholderia pseudomallei; chimpanzee; environment; melioidosis; Pan troglodytes ID BURKHOLDERIA-PSEUDOMALLEI; EPIDEMIOLOGY AB A 40-yr-old male captive chimpanzee (Pan troglodytes) presented with depression and anorexia for 7 days. The tentative diagnosis, following a physical examination under anesthesia, was pneumonia with sepsis. Despite antibiotic treatment and supportive care the chimpanzee died a week following presentation. Gross pathology confirmed severe purulent pneumonia and diffuse hepatosplenic abscesses. Detected in serum at the time of the initial examination, the melioidosis serum antibody titer was elevated (>1: 512). Soil samples were collected from three sites in the exhibit at three depths of 5, 15, and 30 cm. By direct and enrichment culture, positive cultures for Burkholderia pseudomallei were found at 5 and 15 cm in one site. The other two sites were positive by enrichment culture at the depth of 5 cm. To prevent disease in the remaining seven troop members, they were relocated to permit a soil treatment with calcium oxide. The exhibit remained empty for approximately 1 yr before the chimpanzees were returned. During that period, the soil in the exhibit area was again cultured as before and all samples were negative for B. pseudomallei. Following the soil treatment in the exhibit, all chimpanzees have remained free of clinical signs consistent with melioidosis. C1 [Sommanustweechai, Angkana; Kasantikul, Tanit; Kongmakee, Piyaporn; Kamolnorranath, Sumate; Siriaroonrat, Boripat] Zool Pk Org, Bur Res Conservat & Educ, Bangkok 10300, Thailand. [Somsa, Wachirawit; Thomas, Warissara] Zool Pk Org, Nakornratchasrima Zoo, Nakornratchasrima 30000, Thailand. [Wongratanacheewin, Surasakdi; Sermswan, Rasana W.] Khon Kaen Univ, Melioidosis Res Ctr, Khon Kaen 40002, Thailand. [Bush, Mitchell] Natl Zool Pk, Smithsonian Conservat Biol Inst, Front Royal, VA 22630 USA. [Banlunara, Wijit] Chulalongkorn Univ, Fac Vet Sci, Dept Pathol, Bangkok 10300, Thailand. [Sommanustweechai, Angkana] Khon Kaen Univ, Fac Med, Dept Biochem, Khon Kaen 40002, Thailand. RP Sommanustweechai, A (reprint author), Zool Pk Org, Bur Res Conservat & Educ, Bangkok 10300, Thailand. EM angangkana@yahoo.com NR 12 TC 2 Z9 2 U1 1 U2 6 PU AMER ASSOC ZOO VETERINARIANS PI YULEE PA 581705 WHITE OAK ROAD, YULEE, FL 32097 USA SN 1042-7260 EI 1937-2825 J9 J ZOO WILDLIFE MED JI J. Zoo Wildl. Med. PD JUN PY 2013 VL 44 IS 2 BP 475 EP 479 DI 10.1638/2012-0025R5.1 PG 5 WC Veterinary Sciences SC Veterinary Sciences GA AM1PS UT WOS:000339620500031 PM 23805570 ER PT J AU Spearman, LA AF Spearman, Lauren A. TI Taxonomic Revision of the South African Grasshopper Genus Euloryma (Orthoptera: Acrididae) SO TRANSACTIONS OF THE AMERICAN ENTOMOLOGICAL SOCIETY LA English DT Article DE Acrididae; Dirshacris; Hemiacridinae; Hemiloryma; Labioloryma; Loryma; South Africa AB The South African flightless hemiacridine genus Euloryma is revised for the first time, with 21 new species described. The genus name Euloryma is a nomen novum, proposed because the genus Loryma Stal, 1878 (Orthoptera: Acrididae) is a junior homonym of the genus Loryma Walker, 1859 (Lepidoptera: Pyralidae). A detailed discussion of the rationale for this new name is provided. Species keys, a reference chart of species, extensive photography of external and internal morphology, and distribution maps are provided. Morphology figures labeled with internal and external terminology are included. Two provisional Euloryma species-groups are proposed: karoo species-group and the cederbergensis species-group. The majority of the karoo species-group members are found in succulent karoo biome, with one species in the grassland biome, whereas the majority of the cederbergensis species-group members are found in the fynbos biome. The new tribe name Dirshacrini is proposed, due to proposed changes in nomenclature; tribe members Hemiloryma, Dirshacris and Labidioloryma are photographed, a list of diagnostic differences is provided, and a key to the genera is given. The following new species are proposed: karoo species-group: ashleyi sp. nov.; carolynae sp. nov.; magna sp. nov.; browni sp. nov.; khoi sp. nov.; namaqua sp. nov.; san sp. nov.; mayi sp. nov.; zebrata sp. nov.; bonteboki sp. nov.; karoo sp. nov.; cederbergensis species-group: mirabunda sp. nov.; cederbergensis, sp. nov.; lapollai sp. nov.; tsitsikamma sp. nov.; waboom sp. nov.; solveigae sp. nov.; larsenorum sp. nov.; umoja sp. nov.; lyra sp. nov.; ottei sp. nov. C1 [Spearman, Lauren A.] Rutgers State Univ, Grad Program Ecol Evolut & Nat Resources, New Brunswick, NJ 08901 USA. RP Spearman, LA (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20013 USA. EM SpearmanL@si.edu FU U.S. Government Fulbright IIE Scholarship; NSF [DEB-0542775]; Rutgers University Graduate School; Orthopterists' Society FX This research was supported in-part by a U.S. Government Fulbright IIE Scholarship (2005-2006), an NSF grant awarded to Dr. Daniel Otte (DEB-0542775), Dr. Michael L. May, and the Rutgers University Graduate School which assisted with supplemental travel funds. Before all others, the Orthopterists' Society provided grant support that helped fund critical preliminary fieldwork needed for gathering further funding. NR 22 TC 3 Z9 3 U1 1 U2 6 PU AMER ENTOMOL SOC PI PHILADELPHIA PA 1900 BENJ FRANKLIN PARKWAY, PHILADELPHIA, PA 19103-1195 USA SN 0002-8320 EI 2162-3139 J9 T AM ENTOMOL SOC JI Trans. Am. Entomol. Soc. PD JUN PY 2013 VL 139 IS 1 BP 1 EP + DI 10.3157/061.139.0101 PG 101 WC Entomology SC Entomology GA AM8SQ UT WOS:000340147800001 ER PT J AU Lovely, KR McShea, WJ Lafon, NW Carr, DE AF Lovely, Karen R. McShea, William J. Lafon, Nelson W. Carr, David E. TI Land Parcelization and Deer Population Densities in a Rural County of Virginia SO WILDLIFE SOCIETY BULLETIN LA English DT Article DE density estimation; human-wildlife conflict; modeling; Odocoileus virginianus; parcelization; population management; Virginia; white-tailed deer AB The parcelization of exurban landscapes creates a matrix of intermediately sized and privately managed land parcels, presenting a unique challenge to wildlife managers. During 2010-2011, we studied the correlates between land parcelization, deer density, and hunting patterns in exurban northwestern Virginia, USA. We estimated October deer densities (no. deer/km(2)) and conducted landowner surveys of deer harvest in 13 study blocks of mean size 34.8 km(2). The extent of parcelization varied between study blocks; mean parcel size ranged from 2.00 ha to 26.12 ha. We used distance-sampling techniques to survey pre-harvest deer densities in each section, with estimated densities ranging from 9.4 deer/km(2) to 30.1 deer/km(2). We quantified deer harvest through calculations of harvest density and the percentage of land hunted. As parcel size increased, the percentage of land hunted increased. Harvest densities reported by landowners, however, remained constant with the exception of 2.0-4.0-ha parcels, which had higher harvest densities than 60.8-161.8-ha parcels. We used linear regression analysis to model the response of deer density (natural log) to landscape metrics, and the best-fit model predicted deer density from mean parcel size with equivalent models including habitat with mean parcel size. Our results suggest that development processes that subdivide rural lands can significantly increase deer populations. The mechanism for this increase may be restricted hunter access to smaller property parcels and-or increased probability of deer refuges nearby. (C) 2013 The Wildlife Society. C1 [Lovely, Karen R.; McShea, William J.] Natl Zool Pk, Smithsonian Conservat Biol Inst, Front Royal, VA 22630 USA. [Lafon, Nelson W.] Virginia Dept Game & Inland Fisheries, Forest, VA 24551 USA. [Carr, David E.] Univ Virginia, Blandy Expt Farm, Boyce, VA 22620 USA. RP Lovely, KR (reprint author), Natl Zool Pk, Smithsonian Conservat Biol Inst, 1500 Remount Rd, Front Royal, VA 22630 USA. EM mcsheaw@si.edu FU U.S. Department of Agriculture; Virginia Department of Game and Inland Fisheries; University of Virginia FX This project was funded under a U.S. Department of Agriculture cooperative agreement with the Virginia Department of Game and Inland Fisheries. Virginia Department of Game and Inland Fisheries and the University of Virginia provided financial and logistical support for this study. We thank M. Williamson, M. Kline, and D. Kozel for their help with data collection; F. Frenzel, M. Knox, D. Kocka, T. Urgo, H. Tomlinson, C. Grady, R. Hanger, M. Dye and all the others at Virginia Department of Game and Inland Fisheries who provided support; J. McCarthy and C. Wroth from the Rappahannock County administrative offices; A. Cahill from the Frederick County administrative office; the interns at the Smithsonian Conservation Biology Institute; and all the volunteers who assisted with spotlighting. NR 46 TC 3 Z9 3 U1 2 U2 7 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1938-5463 J9 WILDLIFE SOC B JI Wildl. Soc. Bull. PD JUN PY 2013 VL 37 IS 2 BP 360 EP 367 DI 10.1002/wsb.244 PG 8 WC Biodiversity Conservation SC Biodiversity & Conservation GA V38HP UT WOS:000209334800016 ER PT J AU Donoso, DA Johnston, MK Clay, NA Kaspari, ME AF Donoso, David A. Johnston, Mary K. Clay, Natalie A. Kaspari, Michael E. TI Trees as templates for trophic structure of tropical litter arthropod fauna SO SOIL BIOLOGY & BIOCHEMISTRY LA English DT Article DE Tree hypothesis; Species hypothesis; Seasonality hypothesis; Ecosystem size hypothesis; Brown food web; Litter arthropods; Predator to prey ratios ID FOOD-CHAIN LENGTH; ECOSYSTEM SIZE; COMMUNITY STRUCTURE; STABLE-ISOTOPES; FOREST-FLOOR; BOTTOM-UP; DIVERSITY; WEB; DECOMPOSITION; DISTURBANCE AB Litter arthropod abundance in tropical forests is patchily distributed in space and time. This patchiness can be described by three general hypotheses relating plant-based effects to litter arthropod distribution. The tree hypothesis (H1) posits that environments maintained underneath tree canopies are different from those between canopies in ways that shape arthropod abundance. The species hypothesis (H2) refines this scenario, positing that different plant species might maintain distinct litter environments to which arthropod abundances respond. Without regard to specific plant effects, seasonal changes in litter profiles (H3) can account for temporal patchiness in arthropod abundance. The ecosystem size hypothesis provides a mechanism for tree, species and seasonal effects. It links increasing food chain length with habitat availability and its heterogeneity. In a Panamanian rainforest we sampled litter arthropods in quadrats located near (1 m) and far away (30 m) from the parent trunk of 93 tree individuals (to test the tree hypothesis) from 10 tree species (to test the species hypothesis) in the early wet season, when litter is deepest. To test for effects of seasonal changes of litter profiles, we then resampled 25 trees (i.e., five individuals from each of five species) in the late wet season, when climatic conditions are similar, but litter is shallowest. We found weak support for all tree, species and seasonality hypotheses. With few exceptions, trees and species did not sustain different arthropod abundances, neither early nor late in the wet season. Collembola abundance increased late in the wet season, when litter is shallowest. Supporting the ecosystem size hypothesis, accumulated litter either due to trees, species and seasonality sustained higher predator abundance and higher predator to prey ratios. Our results suggest that plants may account for detrital, brown, food web structure; but these effects are mostly through plant-based provision of structural support. This study adds to growing evidence relating the ecosystem size hypothesis to litter environments and suggest a framework to understand plant-based bottom-up forces in structuring litter communities. (C) 2013 Elsevier Ltd. All rights reserved. C1 [Donoso, David A.; Johnston, Mary K.; Clay, Natalie A.; Kaspari, Michael E.] Univ Oklahoma, Dept Zool, Grad Program Ecol & Evolutionary Biol, Norman, OK 73019 USA. [Donoso, David A.] Univ Tecn Particular Loja, Dept Ciencias Nat, Loja, Ecuador. [Johnston, Mary K.] Concordia Univ, Austin, TX 78726 USA. [Kaspari, Michael E.] Smithsonian Trop Res Inst, Balboa, Panama. RP Donoso, DA (reprint author), Univ Oklahoma, Dept Zool, Grad Program Ecol & Evolutionary Biol, Norman, OK 73019 USA. EM david.donosov@gmail.com OI Kaspari, Michael/0000-0002-9717-5768 FU NSF [0212386, 090221] FX We kindly acknowledge the assistance of L Vitt, M. Yuan, R. Broughton, Y. Luo, L. Weider, and G. Wellborn in our graduate committees. We thank S. Hubbel, R. Foster, R. Condit, and J. Wright for allowing access to the CTFS plot. We thank the ZEEB Journal Club for comments on this manuscript. NSF Grants No. 0212386 and No. 090221 to MK supported this research. O. Acevedo, B. Jimenez, and H. Castaneda provided valuable support at BCI. NR 49 TC 3 Z9 3 U1 2 U2 53 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0038-0717 J9 SOIL BIOL BIOCHEM JI Soil Biol. Biochem. PD JUN PY 2013 VL 61 BP 45 EP 51 DI 10.1016/j.soilbio.2013.02.004 PG 7 WC Soil Science SC Agriculture GA 133LQ UT WOS:000318140300005 ER PT J AU Temkin, A Shertzer, J AF Temkin, A. Shertzer, J. TI Electron scattering from excited states of hydrogen: Implications for the ionization threshold law SO PHYSICAL REVIEW A LA English DT Article ID ATOM IMPACT-IONIZATION; TEMKIN-POET MODEL AB The elastic scattering wave function for electrons scattered from the Nth excited state of hydrogen is the final state of the matrix element for excitation of that state. This paper deals with the solution of that problem primarily in the context of the Temkin-Poet (TP) model [A. Temkin, Phys. Rev. 126, 130 (1962); R. Poet, J. Phys. B 11, 3081 (1978)], wherein only the radial parts of the interaction are included. The relevant potential for the outer electron is dominated by the Hartree potential, V-N(H)(r). In the first part of the paper, V-N(H)(r) is approximated by a potential W-N(r), for which the scattering equation can be analytically solved. The results allow formal analytical continuation of N into the continuum, so that the ionization threshold law can be deduced. Because the analytic continuation involves going fromN to an imaginary function of the momentum of the inner electron, the threshold law turns out to be an exponentially damped function of the available energy E, in qualitative accord with the result of Macek and Ihra [J. H. Macek and W. Ihra, Phys. Rev. A 55, 2024 (1997)] for the TP model. Thereafter, the scattering equation for the Hartree potential V-N(H)(r) is solved numerically. The numerical aspects of these calculations have proven to be challenging and required several developments for the difficulties to be overcome. The results for V-N(H)(r) show only a simple energy-dependent shift from the approximate potential W-N(r), which therefore does not change the analytic continuation and the form of the threshold law. It is concluded that the relevant optical potential must be included in order to compare directly with the analytic result of Macek and Ihra. The paper concludes with discussions of (a) a quantum mechanical interpretation of the result, and (b) the outlook of this approach for the complete problem. C1 [Temkin, A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Shertzer, J.] Coll Holy Cross, Worcester, MA 01610 USA. [Shertzer, J.] Harvard Smithsonian Ctr Astrophys, ITAMP, Cambridge, MA 02138 USA. RP Temkin, A (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. NR 25 TC 0 Z9 0 U1 1 U2 5 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 MAY 30 PY 2013 VL 87 IS 5 AR 052718 DI 10.1103/PhysRevA.87.052718 PG 8 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA 155EF UT WOS:000319728500004 ER PT J AU Bartos, I Haiman, Z Kocsis, B Marka, S AF Bartos, Imre Haiman, Zoltan Kocsis, Bence Marka, Szabolcs TI Gas Cloud G2 Can Illuminate the Black Hole Population Near the Galactic Center SO PHYSICAL REVIEW LETTERS LA English DT Article ID ADVECTION-DOMINATED ACCRETION; DENSE STAR-CLUSTERS; GRAVITATIONAL-WAVES; MASS SEGREGATION; STELLAR REMNANTS; BONDI ACCRETION; NEUTRON-STARS; X-RAYS; CHANDRA; GROWTH AB Galactic nuclei are expected to be densely populated with stellar- and intermediate-mass black holes. Exploring this population will have important consequences for the observation prospects of gravitational waves as well as understanding galactic evolution. The gas cloud G2 currently approaching Sgr A* provides an unprecedented opportunity to probe the black hole and neutron star population of the Galactic nucleus. We examine the possibility of a G2-cloud-black-hole encounter and its detectability with current x-ray satellites, such as Chandra and NuSTAR. We find that multiple encounters are likely to occur close to the pericenter, which may be detectable upon favorable circumstances. This opportunity provides an additional important science case for leading x-ray observatories to closely follow G2 on its way to the nucleus. C1 [Bartos, Imre; Marka, Szabolcs] Columbia Univ, Dept Phys, New York, NY 10027 USA. [Bartos, Imre; Haiman, Zoltan; Marka, Szabolcs] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA. [Haiman, Zoltan] Columbia Univ, Dept Astron, New York, NY 10027 USA. [Kocsis, Bence] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Bartos, I (reprint author), Columbia Univ, Dept Phys, 538 W 120th St, New York, NY 10027 USA. EM ibartos@phys.columbia.edu RI Kocsis, Bence/C-3061-2013; Bartos, Imre/A-2592-2017 OI Kocsis, Bence/0000-0002-4865-7517; FU Columbia University in the City of New York; National Science Foundation [PHY-0847182]; NASA [NNX11AE05G]; Columbia University FX The authors thank Akos Bogdan, Charles Hailey, Jules Halpern, Avi Loeb, Brian Metzger, Jeremiah Ostriker, and Frits Paerels for helpful discussions. The Columbia Experimental Gravity group is grateful for the generous support from Columbia University in the City of New York and from the National Science Foundation under cooperative agreement PHY-0847182. Z. H. acknowledges support from NASA Grant No. NNX11AE05G. I. B. received fellowship support from Columbia University. NR 40 TC 8 Z9 8 U1 0 U2 0 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 MAY 30 PY 2013 VL 110 IS 22 AR 221102 DI 10.1103/PhysRevLett.110.221102 PG 5 WC Physics, Multidisciplinary SC Physics GA 155HK UT WOS:000319738400002 PM 23767710 ER PT J AU Smith, BD AF Smith, Bruce D. TI Modifying landscapes and mass kills: Human niche construction and communal ungulate harvests SO QUATERNARY INTERNATIONAL LA English DT Article ID MANAGEMENT; PLANT AB This special issue of Quaternary International includes case study consideration of communal ungulate hunting structures situated in open alpine, tundra, grassland, and desert settings in North America and the Near East. Along with being constructed in a variety of different environments, the mass kill structures described in this issue of QI also exhibit variation in design, as each was specifically tailored to capture a particular prey species, with target species including bighorn sheep (Ovis canadensis), bison (Bison bison), caribou (Rangifer tarandus), pronghorn (Antilocapra americana) gazelle (Gazella spp.), and onager (Equus hemionus). In this introductory article I employ the interrelated concepts of niche construction and traditional ecological knowledge to provide a broader frame of reference for consideration of the underlying similarities and sophistication of these diverse ungulate drive structures, and bring them into clearer focus as comprising important and integral components in the overall socio-economic systems of the small-scale human societies that constructed them. Requiring detailed understanding of local landscapes and patterns of seasonal movement and flight behavior of prey species, such structures were constructed to reduce acquisition effort and increase the predictability of prey species by channeling and constraining their movement for easier harvesting. This was accomplished by creating structural modifications to the landscape designed to direct the prey into killing zones or enclosures. (C) 2013 Elsevier Ltd and INQUA. All rights reserved. C1 Smithsonian Inst, Natl Museum Nat Hist, Program Human Ecol & Archaeobiol, Dept Anthropol, Washington, DC 20560 USA. RP Smith, BD (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Program Human Ecol & Archaeobiol, Dept Anthropol, 10th & Constitut Ave, Washington, DC 20560 USA. EM smithb@si.edu NR 25 TC 7 Z9 7 U1 5 U2 25 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 1040-6182 J9 QUATERN INT JI Quat. Int. PD MAY 29 PY 2013 VL 297 BP 8 EP 12 DI 10.1016/j.quaint.2012.12.006 PG 5 WC Geography, Physical; Geosciences, Multidisciplinary SC Physical Geography; Geology GA 154XZ UT WOS:000319711300002 ER PT J AU Zeder, MA Bar-Oz, G Rufolo, SJ Hole, F AF Zeder, Melinda A. Bar-Oz, Guy Rufolo, Scott J. Hole, Frank TI New perspectives on the use of kites in mass-kills of Levantine gazelle: A view from northeastern Syria SO QUATERNARY INTERNATIONAL LA English DT Article ID SOUTHERN LEVANT; DESERT KITES; HOLOCENE; STRATEGIES; BEHAVIOR; ORIGINS; ISRAEL; JORDAN; NEGEV AB A deposit of gazelle bones at Tell Kuran in the Khabur Basin of northeastern Syria provides evidence for the use of desert kites in the mass-slaughter of steppic game. The deposit's late 4th millennium BCE date, long after livestock had replaced game as primary meat sources, suggests that this practice was directed toward social rather than economic ends. Evidence for the use of kites in the mass killing of steppe animals in the Khabur Basin is examined and the possibility that not only gazelle, but also onagers and possibly other steppe animals' were hunted in this way is explored. The role of such socially driven practices in the local extirpation of steppe species is discussed. (C) 2013 Elsevier Ltd and INQUA. All rights reserved. C1 [Zeder, Melinda A.; Rufolo, Scott J.] Smithsonian Inst, Program Human Ecol & Archaeobiol, Dept Anthropol, Natl Museum Nat Hist, Washington, DC 20560 USA. [Bar-Oz, Guy] Univ Haifa, Dept Archaeol, IL-31999 Haifa, Israel. [Hole, Frank] Yale Univ, Dept Anthropol, New Haven, CT 06520 USA. RP Zeder, MA (reprint author), Smithsonian Inst, Program Human Ecol & Archaeobiol, Dept Anthropol, Natl Museum Nat Hist, Washington, DC 20560 USA. EM Zederm@si.edu NR 84 TC 18 Z9 18 U1 1 U2 9 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 1040-6182 J9 QUATERN INT JI Quat. Int. PD MAY 29 PY 2013 VL 297 BP 110 EP 125 DI 10.1016/j.quaint.2012.12.045 PG 16 WC Geography, Physical; Geosciences, Multidisciplinary SC Physical Geography; Geology GA 154XZ UT WOS:000319711300011 ER PT J AU Wiley, AE Ostrom, PH Welch, AJ Fleischer, RC Gandhi, H Southon, JR Stafford, TW Penniman, JF Hu, D Duvall, FP James, HF AF Wiley, Anne E. Ostrom, Peggy H. Welch, Andreanna J. Fleischer, Robert C. Gandhi, Hasand Southon, John R. Stafford, Thomas W., Jr. Penniman, Jay F. Hu, Darcy Duvall, Fern P. James, Helen F. TI Millennial-scale isotope records from a wide-ranging predator show evidence of recent human impact to oceanic food webs SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA LA English DT Article DE fishing; seabird; stable isotope ID HIGHLY MOBILE SEABIRD; COLLAGEN EXTRACTION; FISH COMMUNITIES; HAWAIIAN PETREL; TROPHIC LEVEL; RADIOCARBON; RATIOS; SIZE; ERADICATION; DIVERGENCE AB Human exploitation of marine ecosystems is more recent in oceanic than near shore regions, yet our understanding of human impacts on oceanic food webs is comparatively poor. Few records of species that live beyond the continental shelves date back more than 60 y, and the sheer size of oceanic regions makes their food webs difficult to study, even in modern times. Here, we use stable carbon and nitrogen isotopes to study the foraging history of a generalist, oceanic predator, the Hawaiian petrel (Pterodroma sandwichensis), which ranges broadly in the Pacific from the equator to near the Aleutian Islands. Our isotope records from modern and ancient, radiocarbon-dated bones provide evidence of over 3,000 y of dietary stasis followed by a decline of ca. 1.8 parts per thousand in delta N-15 over the past 100 y. Fishery-induced trophic decline is the most likely explanation for this sudden shift, which occurs in genetically distinct populations with disparate foraging locations. Our isotope records also show that coincident with the apparent decline in trophic level, foraging segregation among petrel populations decreased markedly. Because variation in the diet of generalist predators can reflect changing availability of their prey, a foraging shift in wide-ranging Hawaiian petrel populations suggests a relatively rapid change in the composition of oceanic food webs in the Northeast Pacific. Understanding and mitigating widespread shifts in prey availability may be a critical step in the conservation of endangered marine predators such as the Hawaiian petrel. C1 [Wiley, Anne E.; Ostrom, Peggy H.; Gandhi, Hasand; Stafford, Thomas W., Jr.] Michigan State Univ, Dept Zool, E Lansing, MI 48824 USA. [Wiley, Anne E.; James, Helen F.] Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Div Birds, Washington, DC 20004 USA. [Welch, Andreanna J.; Fleischer, Robert C.] Smithsonian Inst, Natl Zool Pk, Smithsonian Conservat Biol Inst, Ctr Conservat & Evolutionary Genet, Washington, DC 20008 USA. [Welch, Andreanna J.] Univ Maryland, Behav Ecol Evolut & Systemat Program, College Pk, MD USA. [Welch, Andreanna J.] SUNY Buffalo, Dept Biol Sci, Buffalo, NY 14260 USA. [Stafford, Thomas W., Jr.] Univ Calif Irvine, Dept Earth Syst Sci, Irvine, CA 92617 USA. [Stafford, Thomas W., Jr.] Aarhus Univ, Dept Phys & Astron, DK-8000 Aarhus, Denmark. [Stafford, Thomas W., Jr.] Nat Hist Museum Denmark, Ctr GeoGenet, DK-1350 Copenhagen, Denmark. [Penniman, Jay F.] Univ Hawaii, Pacific Cooperat Studies Unit, Honolulu, HI 96822 USA. [Hu, Darcy] Natl Pk Serv, Pacific West Reg Off, Honolulu, HI 96850 USA. [Duvall, Fern P.] Dept Land & Nat Resources, Wailuku, HI 96793 USA. RP Wiley, AE (reprint author), Michigan State Univ, Dept Zool, E Lansing, MI 48824 USA. EM wileyann@msu.edu FU National Science Foundation (Division of Environmental Biology) [0745604]; Geological Society of America; Michigan State University; National Museum of Natural History, Smithsonian Institution FX For access to museum specimens, we thank the Bird Division and Paleobiology Department, National Museum of Natural History, the Natural History Museum of Los Angeles County, the Bernice Bishop Museum, and M. Spitzer, C. Gebhard, K. Garrett, K. Campbell, L. Garetano, and C. Kishinami for their assistance. We also thank N. Holmes, S. Judge, K. Swindle, D. Ainley, and J. Adams for sharing their expertise and D. Johnson for the use of his photography equipment. We are also grateful to J. Mead and N. Ostrom for helpful comments on the manuscript. Funding was provided by the National Science Foundation (Division of Environmental Biology-0745604), Geological Society of America, Michigan State University, and the National Museum of Natural History, Smithsonian Institution. NR 58 TC 20 Z9 20 U1 6 U2 58 PU NATL ACAD SCIENCES PI WASHINGTON PA 2101 CONSTITUTION AVE NW, WASHINGTON, DC 20418 USA SN 0027-8424 J9 P NATL ACAD SCI USA JI Proc. Natl. Acad. Sci. U. S. A. PD MAY 28 PY 2013 VL 110 IS 22 BP 8972 EP 8977 DI 10.1073/pnas.1300213110 PG 6 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 165RC UT WOS:000320500000059 PM 23671094 ER PT J AU Moss, J Behringer, D Shields, JD Baeza, A Aguilar-Perera, A Bush, PG Dromer, C Herrera-Moreno, A Gittens, L Matthews, TR McCord, MR Scharer, MT Reynal, L Truelove, N Butler, MJ AF Moss, Jessica Behringer, Donald Shields, Jeffrey D. Baeza, Antonio Aguilar-Perera, Alfonso Bush, Phillippe G. Dromer, Clement Herrera-Moreno, Alejandro Gittens, Lester Matthews, Thomas R. McCord, Michael R. Schaerer, Michelle T. Reynal, Lionel Truelove, Nathanial Butler, Mark J. TI Distribution, prevalence, and genetic analysis of Panulirus argus virus 1 (PaV1) from the Caribbean Sea SO DISEASES OF AQUATIC ORGANISMS LA English DT Article DE Spiny lobster; Disease; Epidemiology; Connectivity ID SPINY LOBSTER; PANULIRUS-ARGUS-VIRUS-1 PAV1; POPULATION-STRUCTURE; PARASITE PREVALENCE; SAMPLE-SIZE; LATREILLE; TRANSMISSION; INFECTION; PATTERNS; MEXICO AB The pathogenic virus Panulirus argus virus 1 (PaV1) was first discovered in Caribbean spiny lobsters Panulirus argus from the Florida Keys (USA) in 1999 and has since been reported in Belize, Mexico, and Cuba; its distribution in the wider Caribbean is unknown. We collected tissue samples from adult spiny lobsters from 30 locations in 14 countries bordering the Caribbean Sea and used molecular diagnostics to assay for the presence of PaV1. PaV1 occurred primarily in the northern areas of the Caribbean, where its prevalence was highest. The virus was not found in lobsters from the southeastern Caribbean, and its prevalence was lowest in the southwestern Caribbean. DNA sequence analysis was performed on a fragment of the viral DNA to examine the genetic diversity of PaV1 on a Caribbean-wide scale. Sequence variation in the viral DNA fragment was high, with 61 unique alleles identified from 9 areas. The sharing of viral alleles in lobsters from distant locations supports the hypothesis of a strong genetic connectivity among lobsters within the Caribbean, and further supports the hypothesis that postlarvae infected with PaV1 may serve to disperse the virus over long distances. C1 [Moss, Jessica; Shields, Jeffrey D.] Virginia Inst Marine Sci, Dept Environm & Aquat Anim Hlth, Coll William & Mary, Gloucester Point, VA 23062 USA. [Behringer, Donald] Univ Florida, Sch Forest Resources & Conservat, Gainesville, FL 32653 USA. [Behringer, Donald] Univ Florida, Emerging Pathogens Inst, Gainesville, FL 32610 USA. [Baeza, Antonio; Gittens, Lester; Butler, Mark J.] Old Dominion Univ, Dept Biol Sci, Norfolk, VA 23529 USA. [Baeza, Antonio] Smithsonian Marine Stn Ft Pierce, Ft Pierce, FL 34949 USA. [Aguilar-Perera, Alfonso] Univ Autonoma Yucatan, Fac Med Vet & Zootecnia, Dep Biol Marina, Merida, Mexico. [Dromer, Clement; Reynal, Lionel] Ifremer, F-97231 Le Robert, Martinique, France. [Herrera-Moreno, Alejandro] Programa EcoMar Inc, Santo Domingo 1070011999, Dominican Rep. [Gittens, Lester] Govt Bahamas, Minist Agr & Marine Fisheries, Dept Marine Resources, Nassau 3028, Bahamas. [Matthews, Thomas R.] Fish & Wildlife Res Inst, Florida Fish & Wildlife Conservat Commiss, Marathon, FL 33050 USA. [Schaerer, Michelle T.] US Naval Base, Naval Facil Engn Command NAVFAC, Environm Div, Guantanamo Bay, Cuba. [Schaerer, Michelle T.] Univ Puerto Rico, Dept Marine Sci, Mayaguez, PR 00681 USA. [Truelove, Nathanial] Univ Manchester, Fac Life Sci, Manchester M13 9PL, Lancs, England. RP Moss, J (reprint author), Virginia Inst Marine Sci, Dept Environm & Aquat Anim Hlth, Coll William & Mary, Greate Rd, Gloucester Point, VA 23062 USA. EM jamoss@vims.edu RI Aguilar-Perera, Alfonso/D-6327-2012; OI Aguilar-Perera, Alfonso/0000-0002-7579-2183 FU National Science Foundation (NSF) [OCE0136894, OCE0929086] FX We thank K. Wheeler, P. Coffey, P. O'Leary, and S. Katsuki for assistance with sample processing. We thank D. Parthree for assistance with GIS mapping of sample locations. Sampling of lobsters was also aided greatly by assistance from E. Wederforte (Curacao), J. Azueta (Belize), T. Trott (Bermuda), and R. Wilkens (St. Kitts). This work was funded by National Science Foundation (NSF) grants OCE0136894 and OCE0929086. This is Virginia Institute of Marine Science (VIMS) contribution #3261. NR 36 TC 7 Z9 7 U1 2 U2 14 PU INTER-RESEARCH PI OLDENDORF LUHE PA NORDBUNTE 23, D-21385 OLDENDORF LUHE, GERMANY SN 0177-5103 J9 DIS AQUAT ORGAN JI Dis. Aquat. Org. PD MAY 27 PY 2013 VL 104 IS 2 BP 129 EP 140 DI 10.3354/dao02589 PG 12 WC Fisheries; Veterinary Sciences SC Fisheries; Veterinary Sciences GA 151OJ UT WOS:000319469600005 PM 23709466 ER PT J AU Duval, BD Dijkstra, P Drake, BG Johnson, DW Ketterer, ME Megonigal, JP Hungate, BA AF Duval, Benjamin D. Dijkstra, Paul Drake, Bert G. Johnson, Dale W. Ketterer, Michael E. Megonigal, J. Patrick Hungate, Bruce A. TI Element Pool Changes within a Scrub-Oak Ecosystem after 11 Years of Exposure to Elevated CO2 SO PLOS ONE LA English DT Article ID ROTATION POPLAR PLANTATION; PROGRESSIVE NITROGEN LIMITATION; ATMOSPHERIC CO2; SOIL CARBON; PHOSPHORUS-AVAILABILITY; ABOVEGROUND BIOMASS; N-FERTILIZATION; ENRICHMENT; FOREST; RESPONSES AB The effects of elevated CO2 on ecosystem element stocks are equivocal, in part because cumulative effects of CO2 on element pools are difficult to detect. We conducted a complete above and belowground inventory of non-nitrogen macro- and micronutrient stocks in a subtropical woodland exposed to twice-ambient CO2 concentrations for 11 years. We analyzed a suite of nutrient elements and metals important for nutrient cycling in soils to a depth of similar to 2 m, in leaves and stems of the dominant oaks, in fine and coarse roots, and in litter. In conjunction with large biomass stimulation, elevated CO2 increased oak stem stocks of Na, Mg, P, K, V, Zn and Mo, and the aboveground pool of K and S. Elevated CO2 increased root pools of most elements, except Zn. CO2-stimulation of plant Ca was larger than the decline in the extractable Ca pool in soils, whereas for other elements, increased plant uptake matched the decline in the extractable pool in soil. We conclude that elevated CO2 caused a net transfer of a subset of nutrients from soil to plants, suggesting that ecosystems with a positive plant growth response under high CO2 will likely cause mobilization of elements from soil pools to plant biomass. C1 [Duval, Benjamin D.; Dijkstra, Paul; Hungate, Bruce A.] No Arizona Univ, Dept Biol Sci, Flagstaff, AZ 86011 USA. [Duval, Benjamin D.; Dijkstra, Paul; Hungate, Bruce A.] No Arizona Univ, Merriam Powell Ctr Environm Res, Flagstaff, AZ 86011 USA. [Drake, Bert G.; Megonigal, J. Patrick] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. [Johnson, Dale W.] Univ Nevada, Dept Nat Resources, Reno, NV 89557 USA. [Ketterer, Michael E.] No Arizona Univ, Dept Chem & Biochem, Flagstaff, AZ 86011 USA. RP Duval, BD (reprint author), USDA ARS, US Dairy Forage Res Ctr, Madison, WI 53706 USA. EM Benjamin.Duval@ars.usda.gov FU NSF [DEB-0092642, DEB-0543218] FX Research was funded by NSF grants DEB-0092642 and DEB-0543218. The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 41 TC 3 Z9 3 U1 0 U2 56 PU PUBLIC LIBRARY SCIENCE PI SAN FRANCISCO PA 1160 BATTERY STREET, STE 100, SAN FRANCISCO, CA 94111 USA SN 1932-6203 J9 PLOS ONE JI PLoS One PD MAY 23 PY 2013 VL 8 IS 5 AR e64386 DI 10.1371/journal.pone.0064386 PG 9 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 151BM UT WOS:000319435600063 PM 23717607 ER PT J AU Ashby, MLN Willner, SP Fazio, GG Huang, JS Arendt, R Barmby, P Barro, G Bell, EF Bouwens, R Cattaneo, A Croton, D Dave, R Dunlop, JS Egami, E Faber, S Finlator, K Grogin, NA Guhathakurta, P Hernquist, L Hora, JL Illingworth, G Kashlinsky, A Koekemoer, AM Koo, DC Labbe, I Li, Y Lin, L Moseley, H Nandra, K Newman, J Noeske, K Ouchi, M Peth, M Rigopoulou, D Robertson, B Sarajedini, V Simard, L Smith, HA Wang, Z Wechsler, R Weiner, B Wilson, G Wuyts, S Yamada, T Yan, H AF Ashby, M. L. N. Willner, S. P. Fazio, G. G. Huang, J. -S. Arendt, R. Barmby, P. Barro, G. Bell, E. F. Bouwens, R. Cattaneo, A. Croton, D. Dave, R. Dunlop, J. S. Egami, E. Faber, S. Finlator, K. Grogin, N. A. Guhathakurta, P. Hernquist, L. Hora, J. L. Illingworth, G. Kashlinsky, A. Koekemoer, A. M. Koo, D. C. Labbe, I. Li, Y. Lin, L. Moseley, H. Nandra, K. Newman, J. Noeske, K. Ouchi, M. Peth, M. Rigopoulou, D. Robertson, B. Sarajedini, V. Simard, L. Smith, H. A. Wang, Z. Wechsler, R. Weiner, B. Wilson, G. Wuyts, S. Yamada, T. Yan, H. TI SEDS: THE SPITZER EXTENDED DEEP SURVEY. SURVEY DESIGN, PHOTOMETRY, AND DEEP IRAC SOURCE COUNTS SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: high-redshift; infrared: galaxies; surveys ID EXTRAGALACTIC LEGACY SURVEY; LYMAN-BREAK GALAXIES; INFRARED BACKGROUND FLUCTUATIONS; SPACE-TELESCOPE OBSERVATIONS; UV LUMINOSITY FUNCTIONS; STAR-FORMATION HISTORY; EXTREMELY RED OBJECTS; CLUSTERING PROPERTIES; REDSHIFT SURVEY; MU-M AB The Spitzer Extended Deep Survey (SEDS) is a very deep infrared survey within five well-known extragalactic science fields: the UKIDSS Ultra-Deep Survey, the Extended Chandra Deep Field South, COSMOS, the Hubble Deep Field North, and the Extended Groth Strip. SEDS covers a total area of 1.46 deg(2) to a depth of 26 AB mag (3s) in both of the warm Infrared Array Camera (IRAC) bands at 3.6 and 4.5 mu m. Because of its uniform depth of coverage in so many widely-separated fields, SEDS is subject to roughly 25% smaller errors due to cosmic variance than a single-field survey of the same size. SEDS was designed to detect and characterize galaxies from intermediate to high redshifts (z = 2-7) with a built-in means of assessing the impact of cosmic variance on the individual fields. Because the full SEDS depth was accumulated in at least three separate visits to each field, typically with six- month intervals between visits, SEDS also furnishes an opportunity to assess the infrared variability of faint objects. This paper describes the SEDS survey design, processing, and publicly-available data products. Deep IRAC counts for the more than 300,000 galaxies detected by SEDS are consistent with models based on known galaxy populations. Discrete IRAC sources contribute 5.6 +/- 1.0 and 4.4 +/- 0.8 nW m(-2) sr(-1) at 3.6 and 4.5 mu m to the diffuse cosmic infrared background (CIB). IRAC sources cannot contribute more than half of the total CIB flux estimated from DIRBE data. Barring an unexpected error in the DIRBE flux estimates, half the CIB flux must therefore come from a diffuse component. C1 [Ashby, M. L. N.; Willner, S. P.; Fazio, G. G.; Huang, J. -S.; Hernquist, L.; Hora, J. L.; Smith, H. A.; Wang, Z.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Arendt, R.; Kashlinsky, A.; Moseley, H.] NASA, Goddard Space Flight Ctr, Observat Cosmol Lab, Greenbelt, MD 20771 USA. [Arendt, R.] Univ Maryland Baltimore Cty, CRESST, Baltimore, MD 21250 USA. [Barmby, P.] Univ Western Ontario, London, ON N6A 3K7, Canada. [Barro, G.; Faber, S.; Guhathakurta, P.; Illingworth, G.; Koo, D. C.] Univ Calif Santa Cruz, Lick Observ, Univ Calif Observ, Santa Cruz, CA 95064 USA. [Barro, G.; Faber, S.; Guhathakurta, P.; Illingworth, G.; Koo, D. C.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. [Bell, E. F.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Bouwens, R.; Labbe, I.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [Cattaneo, A.] Aix Marseille Univ, CNRS, Lab Astrophys Marseille, UMR 7326, F-13388 Marseille, France. [Croton, D.] Swinburne Univ Technol, Ctr Astrophys & Supercomp, Hawthorn, Vic 3122, Australia. [Dave, R.; Robertson, B.] Univ Arizona, Dept Astron, Tucson, AZ 85721 USA. [Dunlop, J. S.] Univ Edinburgh, Royal Observ, Inst Astron, Scottish Univ Phys Alliance, Edinburgh EH9 3HJ, Midlothian, Scotland. [Egami, E.; Robertson, B.; Weiner, B.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Finlator, K.] Univ Copenhagen, Niels Bohr Inst, Dark Cosmol Ctr, DK-2100 Copenhagen O, Denmark. [Grogin, N. A.; Koekemoer, A. M.; Noeske, K.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Kashlinsky, A.] SSAI, Lanham, MD 20706 USA. [Li, Y.] Penn State Univ, Dept Phys & Astron, University Pk, PA 16802 USA. [Li, Y.] Penn State Univ, Inst Gravitat & Cosmos, University Pk, PA 16802 USA. [Lin, L.] Acad Sinica, Inst Astron & Astrophys, Taipei 106, Taiwan. [Nandra, K.; Wuyts, S.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Newman, J.] Univ Pittsburgh, Dept Phys & Astron, Pittsburgh, PA 15260 USA. [Ouchi, M.] Univ Tokyo, Inst Cosm Ray Res, Kashiwa, Chiba 2778582, Japan. [Ouchi, M.] Univ Tokyo, Kavli Inst Phys & Math Universe WPI, Kashiwa, Chiba 2778583, Japan. [Peth, M.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Rigopoulou, D.] Univ Oxford, Oxford OX1 3RH, England. [Rigopoulou, D.] Rutherford Appleton Lab, Space Sci & Technol Dept, Didcot OX11 0QX, Oxon, England. [Sarajedini, V.] Univ Florida, Dept Astron, Gainesville, FL 32611 USA. [Simard, L.] Natl Res Council Canada, Herzberg Inst Astrophys, Victoria, BC, Canada. [Wechsler, R.] Stanford Univ, Dept Phys, Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94305 USA. [Wechsler, R.] SLAC Natl Accelerator Lab, Menlo Pk, CA 94025 USA. [Wilson, G.] Univ Calif Riverside, Dept Phys & Astron, Riverside, CA 92521 USA. [Yamada, T.] Tohoku Univ, Astron Inst, Sendai, Miyagi 980, Japan. [Yan, H.] Univ Missouri, Dept Phys & Astron, Columbia, MO 65211 USA. RP Ashby, MLN (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM mashby@cfa.harvard.edu RI Finlator, Kristian/M-4809-2014; Barmby, Pauline/I-7194-2016 OI Finlator, Kristian/0000-0002-0496-1656; Hora, Joseph/0000-0002-5599-4650; Koekemoer, Anton/0000-0002-6610-2048; Arendt, Richard/0000-0001-8403-8548; Bell, Eric/0000-0002-5564-9873; Barmby, Pauline/0000-0003-2767-0090 FU National Aeronautics and Space Administration (NASA); NASA [1367335, 1367411, 1367412]; European Research Council; Royal Society via a Wolfson Research Merit Award; National Science Foundation FX The authors are grateful to E. Diolaiti for helpful advice on the optimal use of StarFinder. 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 the National Aeronautics and Space Administration (NASA). Support for this work was provided by NASA through contract numbers 1367335, 1367411 and 1367412 issued by JPL/Caltech. J.S.D. acknowledges the support of the European Research Council via an Advanced Grant, and the support of the Royal Society via a Wolfson Research Merit Award. IRAF is distributed by the National Optical Astronomy Observatory, which is operated by the Association of Universities for Research in Astronomy (AURA) under cooperative agreement with the National Science Foundation. NR 69 TC 83 Z9 83 U1 2 U2 7 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAY 20 PY 2013 VL 769 IS 1 AR 80 DI 10.1088/0004-637X/769/1/80 PG 27 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 157NL UT WOS:000319904500080 ER PT J AU Bai, XN Stone, JM AF Bai, Xue-Ning Stone, James M. TI WIND-DRIVEN ACCRETION IN PROTOPLANETARY DISKS. I. SUPPRESSION OF THE MAGNETOROTATIONAL INSTABILITY AND LAUNCHING OF THE MAGNETOCENTRIFUGAL WIND SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; instabilities; magnetohydrodynamics (MHD); methods: numerical; protoplanetary disks; turbulence ID YOUNG STELLAR OBJECTS; X-RAY IONIZATION; 3-DIMENSIONAL MAGNETOHYDRODYNAMIC SIMULATIONS; SURFACE-LAYER ACCRETION; T TAURI DISKS; PROTOSTELLAR DISKS; MAGNETIZED ACCRETION; DEAD ZONES; NONLINEAR EVOLUTION; AMBIPOLAR DIFFUSION AB We perform local, vertically stratified shearing-box MHD simulations of protoplanetary disks (PPDs) at a fiducial radius of 1 AU that take into account the effects of both Ohmic resistivity and ambipolar diffusion (AD). The magnetic diffusion coefficients are evaluated self-consistently from a look-up table based on equilibrium chemistry. We first show that the inclusion of AD dramatically changes the conventional picture of layered accretion. Without net vertical magnetic field, the system evolves into a toroidal field dominated configuration with extremely weak turbulence in the far-UV ionization layer that is far too inefficient to drive rapid accretion. In the presence of a weak net vertical field (plasma beta similar to 10(5) at midplane), we find that the magnetorotational instability (MRI) is completely suppressed, resulting in a fully laminar flow throughout the vertical extent of the disk. A strong magnetocentrifugal wind is launched that efficiently carries away disk angular momentum and easily accounts for the observed accretion rate in PPDs. Moreover, under a physical disk wind geometry, all the accretion flow proceeds through a strong current layer with a thickness of similar to 0.3H that is offset from disk midplane with radial velocity of up to 0.4 times the sound speed. Both Ohmic resistivity and AD are essential for the suppression of the MRI and wind launching. The efficiency of wind transport increases with increasing net vertical magnetic flux and the penetration depth of the FUV ionization. Our laminar wind solution has important implications on planet formation and global evolution of PPDs. C1 [Bai, Xue-Ning; Stone, James M.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. [Bai, Xue-Ning] Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, Cambridge, MA 02138 USA. RP Bai, XN (reprint author), Princeton Univ, Dept Astrophys Sci, Peyton Hall, Princeton, NJ 08544 USA. EM xbai@cfa.harvard.edu FU NASA through a Hubble Fellowship grant from the Space Telescope Science Institute [HST-HF-51301.01-A]; NASA [NAS5-26555]; National Science Foundation [AST-0908269]; Kraken and Nautilus at the National Institute for Computational Sciences through XSEDE [TG-AST090106] FX We thank Jeremy Goodman, Arieh Konigl, and Neal Turner for useful discussions. X.N.B. acknowledges support for program number HST-HF-51301.01-A provided by NASA through a Hubble Fellowship 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. J.M.S. acknowledges support from the National Science Foundation through grant AST-0908269. This work used computational facilities provided by PICSciE at Princeton University. Part of the computation is performed on Kraken and Nautilus at the National Institute for Computational Sciences through XSEDE grant TG-AST090106. NR 127 TC 87 Z9 88 U1 0 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 MAY 20 PY 2013 VL 769 IS 1 AR 76 DI 10.1088/0004-637X/769/1/76 PG 21 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 157NL UT WOS:000319904500076 ER PT J AU Brown, WR Kilic, M Prieto, CA Gianninas, A Kenyon, SJ AF Brown, Warren R. Kilic, Mukremin Allende Prieto, Carlos Gianninas, A. Kenyon, Scott J. TI THE ELM SURVEY. V. MERGING MASSIVE WHITE DWARF BINARIES SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries: close; Galaxy: stellar content; stars: individual (SDSS J0751-0141, SDSS J0811+0225); stars: neutron; white dwarfs ID DIGITAL SKY SURVEY; DOUBLE DEGENERATE SYSTEM; HOT SUBDWARF STARS; HYPERVELOCITY STARS; NLTT 11748; THEORETICAL ISOCHRONES; SPECTROSCOPIC SURVEY; PHOTOMETRIC SYSTEMS; MILLISECOND PULSAR; ECLIPSING BINARY AB We present the discovery of 17 low-mass white dwarfs (WDs) in short-period (P <= 1 day) binaries. Our sample includes four objects with remarkable log g similar or equal to 5 surface gravities and orbital solutions that require them to be double degenerate binaries. All of the lowest surface gravity WDs have metal lines in their spectra implying long gravitational settling times or ongoing accretion. Notably, six of the WDs in our sample have binary merger times < 10 Gyr. Four have greater than or similar to 0.9M(circle dot) companions. If the companions are massive WDs, these four binaries will evolve into stable mass transfer AM CVn systems and possibly explode as underluminous supernovae. If the companions are neutron stars, then these may be millisecond pulsar binaries. These discoveries increase the number of detached, double degenerate binaries in the ELM Survey to 54; 31 of these binaries will merge within a Hubble time. C1 [Brown, Warren R.; Kenyon, Scott J.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. [Kilic, Mukremin; Gianninas, A.] Univ Oklahoma, Homer L Dodge Dept Phys & Astron, Norman, OK 73019 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; kilic@ou.edu; callende@iac.es; alexg@nhn.ou.edu; skenyon@cfa.harvard.edu RI Alexandros, Gianninas/B-8352-2016; OI Alexandros, Gianninas/0000-0002-8655-4308; Kenyon, Scott/0000-0003-0214-609X FU Alfred P. Sloan Foundation; National Science Foundation; U.S. Department of Energy Office of Science; Smithsonian Institution FX We thank M. Alegria, P. Canton, S. Gotilla, J. McAfee, E. Martin, A. Milone, and R. Ortiz for their assistance with observations obtained at the MMT Observatory, and P. Berlind and M. Calkins for their assistance with observations obtained at the Fred Lawrence Whipple Observatory. We also thank P. Bergeron and D. Koester for their invaluable assistance in the computation of our stellar atmosphere model grids. This research makes use of the SAO/NASA Astrophysics Data System Bibliographic Service. This project makes use of data products from the Sloan Digital Sky Survey, which has been funded by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, and the U.S. Department of Energy Office of Science. This work was supported in part by the Smithsonian Institution. NR 73 TC 42 Z9 42 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAY 20 PY 2013 VL 769 IS 1 AR 66 DI 10.1088/0004-637X/769/1/66 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 157NL UT WOS:000319904500066 ER PT J AU Cappelluti, N Kashlinsky, A Arendt, RG Comastri, A Fazio, GG Finoguenov, A Hasinger, G Mather, JC Miyaji, T Moseley, SH AF Cappelluti, N. Kashlinsky, A. Arendt, R. G. Comastri, A. Fazio, G. G. Finoguenov, A. Hasinger, G. Mather, J. C. Miyaji, T. Moseley, S. H. TI CROSS-CORRELATING COSMIC INFRARED AND X-RAY BACKGROUND FLUCTUATIONS: EVIDENCE OF SIGNIFICANT BLACK HOLE POPULATIONS AMONG THE CIB SOURCES SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology: observations; dark ages, reionization, first stars; infrared: diffuse background; stars: Population III; X-rays: diffuse background ID ACTIVE GALACTIC NUCLEI; COBE DIRBE MAPS; SPITZER-SPACE-TELESCOPE; WIDE-FIELD SURVEY; ALL-SKY SURVEY; NUMBER COUNTS; SOURCE CATALOG; POWER SPECTRUM; GOODS FIELDS; III STARS AB In order to understand the nature of the sources producing the recently uncovered cosmic infrared background (CIB) fluctuations, we study cross-correlations between the fluctuations in the source-subtracted CIB from Spitzer/IRAC data and the unresolved cosmic X-ray background from deep Chandra observations. Our study uses data from the EGS/AEGIS field, where both data sets cover an similar or equal to 8' x 45' region of the sky. Our measurement is the cross-power spectrum between the IR and X-ray data. The cross-power signal between the IRAC maps at 3.6 mu m and 4.5 mu m and the Chandra [0.5-2] keV data has been detected, at angular scales greater than or similar to 20 '', with an overall significance of similar or equal to 3.8 sigma and similar or equal to 5.6 sigma, respectively. At the same time we find no evidence of significant cross-correlations at the harder Chandra bands. The cross-correlation signal is produced by individual IR sources with 3.6 mu m and 4.5 mu m magnitudes m(AB) greater than or similar to 25-26 and [0.5-2] keV X-ray fluxes << 7 x 10(-17) erg cm(2) s(-1). We determine that at least 15%-25% of the large scale power of the CIB fluctuations is correlated with the spatial power spectrum of the X-ray fluctuations. If this correlation is attributed to emission from accretion processes at both IR and X-ray wavelengths, this implies a much higher fraction of accreting black holes than among the known populations. We discuss the various possible origins for the cross-power signal and show that neither local foregrounds nor the known remaining normal galaxies and active galactic nuclei can reproduce the measurements. These observational results are an important new constraint on theoretical modeling of the near-IR CIB fluctuations. C1 [Cappelluti, N.; Comastri, A.] INAF Osservatorio Astron Bologna, I-40127 Bologna, Italy. [Cappelluti, N.; Arendt, R. G.; Finoguenov, A.] Univ Maryland Baltimore Cty, Baltimore, MD 21250 USA. [Kashlinsky, A.; Arendt, R. G.; Mather, J. C.; Moseley, S. H.] NASA, Goddard Space Flight Ctr, Observat Cosmol Lab, Greenbelt, MD 20771 USA. [Kashlinsky, A.] SSAI, Lanham, MD 20706 USA. [Fazio, G. G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Finoguenov, A.] Univ Helsinki, Dept Phys, FI-00014 Helsinki, Finland. [Hasinger, G.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Mather, J. C.; Moseley, S. H.] NASA, Greenbelt, MD 20771 USA. [Miyaji, T.] Univ Nacl Autonoma Mexico, Inst Astron, Ensenada 22860, BC, Mexico. RP Cappelluti, N (reprint author), INAF Osservatorio Astron Bologna, Via Ranzani 1, I-40127 Bologna, Italy. RI Comastri, Andrea/O-9543-2015; OI Comastri, Andrea/0000-0003-3451-9970; Cappelluti, Nico/0000-0002-1697-186X; Arendt, Richard/0000-0001-8403-8548 FU NASA Chandra Archival research grant [AR2-13014B]; INAF fellowship program; Della Riccia foundation; [ASI-INAFI/009/10/0] FX N.C., A.K., and R.A. acknowledge NASA Chandra Archival research grant No. AR2-13014B for partial support. N.C. acknowledges the INAF fellowship program. We acknowledge financial contribution from the agreement ASI-INAFI/009/10/0. N.C. acknowledges the Della Riccia foundation for partially funding this project. NR 57 TC 24 Z9 24 U1 1 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAY 20 PY 2013 VL 769 IS 1 AR 68 DI 10.1088/0004-637X/769/1/68 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 157NL UT WOS:000319904500068 ER PT J AU Fong, W Berger, E Chornock, R Margutti, R Levan, AJ Tanvir, NR Tunnicliffe, RL Czekala, I Fox, DB Perley, DA Cenko, SB Zauderer, BA Laskar, T Persson, SE Monson, AJ Kelson, DD Birk, C Murphy, D Servillat, M Anglada, G AF Fong, W. Berger, E. Chornock, R. Margutti, R. Levan, A. J. Tanvir, N. R. Tunnicliffe, R. L. Czekala, I. Fox, D. B. Perley, D. A. Cenko, S. B. Zauderer, B. A. Laskar, T. Persson, S. E. Monson, A. J. Kelson, D. D. Birk, C. Murphy, D. Servillat, M. Anglada, G. TI DEMOGRAPHICS OF THE GALAXIES HOSTING SHORT-DURATION GAMMA-RAY BURSTS SO ASTROPHYSICAL JOURNAL LA English DT Article DE gamma-ray burst: general ID CORE-COLLAPSE SUPERNOVAE; DELAY-TIME DISTRIBUTION; STAR-FORMATION RATES; SHORT GRB 111117A; OPTICAL AFTERGLOW; POPULATION SYNTHESIS; INTERSTELLAR-MEDIUM; EXTENDED EMISSION; IA SUPERNOVAE; NEUTRON-STARS AB We present observations of the afterglows and host galaxies of three short-duration gamma-ray bursts (GRBs): 100625A, 101219A, and 110112A. We find that GRB 100625A occurred in a z = 0.452 early-type galaxy with a stellar mass of approximate to 4.6 x 10(9) M-circle dot and a stellar population age of approximate to 0.7 Gyr, and GRB 101219A originated in a star-forming galaxy at z = 0.718 with a stellar mass of approximate to 1.4 x 10(9) M-circle dot, a star formation rate of approximate to 16 M-circle dot yr(-1), and a stellar population age of approximate to 50 Myr. We also report the discovery of the optical afterglow of GRB 110112A, which lacks a coincident host galaxy to i greater than or similar to 26 mag, and we cannot conclusively identify any field galaxy as a possible host. From afterglow modeling, the bursts have inferred circumburst densities of approximate to 10(-4)-1 cm(-3) and isotropic-equivalent gamma-ray and kinetic energies of approximate to 10(50)-10(51) erg. These three events highlight the diversity of galactic environments that host short GRBs. To quantify this diversity, we use the sample of 36 Swift short GRBs with robust associations to an environment (similar to 1/2 of 68 short bursts detected by Swift to 2012 May) and classify bursts originating from four types of environments: late-type (approximate to 50%), early-type (approximate to 15%), inconclusive (approximate to 20%), and "host-less" (lacking a coincident host galaxy to limits of greater than or similar to 26 mag; approximate to 15%). To find likely ranges for the true late- and early-type fractions, we assign each of the host-less bursts to either the late- or early-type category using probabilistic arguments and consider the scenario that all hosts in the inconclusive category are early-type galaxies to set an upper bound on the early-type fraction. We calculate most likely ranges for the late- and early-type fractions of approximate to 60%-80% and approximate to 20%-40%, respectively. We find no clear trend between gamma- ray duration and host type. We also find no change to the fractions when excluding events recently claimed as possible contaminants from the long GRB/collapsar population. Our reported demographics are consistent with a short GRB rate driven by both stellar mass and star formation. C1 [Fong, W.; Berger, E.; Chornock, R.; Margutti, R.; Czekala, I.; Zauderer, B. A.; Laskar, T.; Servillat, M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Levan, A. J.; Tunnicliffe, R. L.] Univ Warwick, Dept Phys, Coventry CV4 7AL, W Midlands, England. [Tanvir, N. R.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. [Fox, D. B.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Perley, D. A.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA. [Cenko, S. B.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Persson, S. E.; Monson, A. J.; Kelson, D. D.; Birk, C.; Murphy, D.] Observ Carnegie Inst Sci, Pasadena, CA 91101 USA. [Servillat, M.] Univ Paris Diderot, CEA Saclay, Lab AIM, CEA,DSM,IRFU,SAp,CNRS, F-91191 Gif Sur Yvette, France. [Anglada, G.] Univ Gottingen, Inst Astrophys, D-37077 Gottingen, Germany. RP Fong, W (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. OI Czekala, Ian/0000-0002-1483-8811 FU National Science Foundation [AST-1107973]; NASA/Swift AO6 [NNX10AI24G]; NASA/Swift A07 [NNX12AD69G]; National Aeronautics and Space Administration through Chandra Award [GO1-12072X]; National Aeronautics Space Administration [NAS8-03060]; NSF [AST-0908886, AST-1211916] FX We thank F. di Mille for observing on behalf of the Berger GRB group at Harvard. The Berger GRB group is supported by the National Science Foundation under grant AST-1107973, and by NASA/Swift AO6 grant NNX10AI24G and A07 grant NNX12AD69G. Partial support was also provided by the National Aeronautics and Space Administration through Chandra Award Number GO1-12072X 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 NAS8-03060. This paper includes data gathered with the 6.5 m Magellan Telescopes located at Las Campanas Observatory, Chile. This work is based in part on observations obtained at the Gemini Observatory, which is operated by the Association of Universities for Research in Astronomy, Inc., under a cooperative agreement with the NSF on behalf of the Gemini partnership: the National Science Foundation (United States), the Science and Technology Facilities Council (United Kingdom), the National Research Council (Canada), CONICYT (Chile), the Australian Research Council (Australia), Ministerio da Ciencia, Tecnologia e Inovacao (Brazil), and Ministerio de Ciencia, Tecnologia e Innovacion Productiva (Argentina). This work made use of data supplied by the UK Swift Science Data Centre at the University of Leicester. S.B.C. acknowledges generous support from Gary & Cynthia Bengier, the Richard & Rhoda Goldman Fund, the Christopher R. Redlich Fund, the TABASGO Foundation, and NSF grants AST-0908886 and AST-1211916. NR 154 TC 45 Z9 46 U1 1 U2 12 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAY 20 PY 2013 VL 769 IS 1 AR 56 DI 10.1088/0004-637X/769/1/56 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 157NL UT WOS:000319904500056 ER PT J AU Jacoby, GH Ciardullo, R De Marco, O Lee, MG Herrmann, KA Hwang, HS Kaplan, E Davies, JE AF Jacoby, George H. Ciardullo, Robin De Marco, Orsola Lee, Myung Gyoon Herrmann, Kimberly A. Hwang, Ho Seong Kaplan, Evan Davies, James E. TI A SURVEY FOR PLANETARY NEBULAE IN M31 GLOBULAR CLUSTERS SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: individual (M31); globular clusters: general; planetary nebulae: general; stars: evolution ID INTERMEDIATE-MASS STARS; HUBBLE-SPACE-TELESCOPE; LOCAL GROUP GALAXIES; DIFFUSE IONIZED-GAS; WIDE-FIELD SURVEY; X-RAY SOURCES; LEO-I GROUP; STRUCTURAL PARAMETERS; LUMINOSITY FUNCTION; STANDARD CANDLES AB We report the results of an [O III] lambda 5007 spectroscopic survey for planetary nebulae (PNe) located within the star clusters of M31. By examining R similar to 5000 spectra taken with the WIYN+Hydra spectrograph, we identify 3 PN candidates in a sample of 274 likely globular clusters, 2 candidates in objects which may be globular clusters, and 5 candidates in a set of 85 younger systems. The possible PNe are all faint, between similar to 2.5 and similar to 6.8 mag down the PN luminosity function, and, partly as a consequence of our selection criteria, have high excitation, with [O III] lambda 5007 to H beta ratios ranging from 2 to greater than or similar to 12. We discuss the individual candidates, their likelihood of cluster membership, and the possibility that they were formed via binary interactions within the clusters. Our data are consistent with the suggestion that PN formation within globular clusters correlates with binary encounter frequency, though, due to the small numbers and large uncertainties in the candidate list, this study does not provide sufficient evidence to confirm the hypothesis. C1 [Jacoby, George H.] Giant Magellan Telescope Carnegie Observ, Pasadena, CA 91101 USA. [Ciardullo, Robin] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [De Marco, Orsola] Macquarie Univ, Dept Phys & Astron, Sydney, NSW 2109, Australia. [Lee, Myung Gyoon] Seoul Natl Univ, Dept Phys & Astron, Astron Program, Seoul 151742, South Korea. [Herrmann, Kimberly A.] Lowell Observ, Flagstaff, AZ 86001 USA. [Hwang, Ho Seong; Davies, James E.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. [Kaplan, Evan] Vassar Coll, Poughkeepsie, NY 12604 USA. RP Jacoby, GH (reprint author), Giant Magellan Telescope Carnegie Observ, 813 Santa Barbara St, Pasadena, CA 91101 USA. EM gjacoby@gmto.org; rbc@astro.psu.edu; orsola.demarco@mq.edu.au; mglee@astrog.snu.ac.kr; herrmann@lowell.edu; hhwang@cfa.harvard.edu; evanskaplan@gmail.com; jdavies@cfa.harvard.edu FU Mid-career Researcher Program through an NRF grant; MEST [2010-0013875]; NOAO/KPNO Research Experiences for Undergraduates (REU) Program; National Science Foundation (NSF) Research Experience for Undergraduates Program; Department of Defense ASSURE program through Scientific Program [AST-0754223, AST-0132798] FX We thank Laura Fullton for early discussions about this project, and Nelson Caldwell for helpful insights and providing access to his M31 cluster Web site http://www.cfa.harvard.edu/oir/eg/m31clusters/M31_Hectospec.html. M.G.L. is supported in part by the Mid-career Researcher Program through an NRF grant funded by the MEST (No. 2010-0013875). E.K. was supported by the NOAO/KPNO Research Experiences for Undergraduates (REU) Program, which is funded by the National Science Foundation (NSF) Research Experience for Undergraduates Program and the Department of Defense ASSURE program through Scientific Program Order No. 13 (AST-0754223) of the Cooperative Agreement No. AST-0132798 between the Association of Universities for Research in Astronomy (AURA) and the NSF. NR 87 TC 8 Z9 9 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAY 20 PY 2013 VL 769 IS 1 AR 10 DI 10.1088/0004-637X/769/1/10 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 157NL UT WOS:000319904500010 ER PT J AU Jerjen, H Da Costa, GS Willman, B Tisserand, P Arimoto, N Okamoto, S Mateo, M Saviane, I Walsh, S Geha, M Jordan, A Olszewski, E Walker, M Zoccali, M Kroupa, P AF Jerjen, H. Da Costa, G. S. Willman, B. Tisserand, P. Arimoto, N. Okamoto, S. Mateo, M. Saviane, I. Walsh, S. Geha, M. Jordan, A. Olszewski, E. Walker, M. Zoccali, M. Kroupa, P. TI MAIN-SEQUENCE STAR POPULATIONS IN THE VIRGO OVERDENSITY REGION SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies; individual (Sagittarius) - galaxies; stellar content - Galaxy; abundances - Galaxy; halo - Galaxy; structure ID SAGITTARIUS DWARF GALAXY; RR-LYRAE STARS; DIGITAL SKY SURVEY; MILKY-WAY; TIDAL STREAM; SPHEROIDAL GALAXY; SURVEY VIEW; LUMINOSITY FUNCTIONS; STELLAR OVERDENSITY; HALO SUBSTRUCTURE AB We present deep color-magnitude diagrams (CMDs) for two Subaru Suprime-Cam fields in the Virgo Stellar Stream (VSS)/Virgo Overdensity (VOD) and compare them to a field centered on the highest concentration of Sagittarius (Sgr) Tidal Stream stars in the leading arm, Branch A of the bifurcation. A prominent population of main-sequence stars is detected in all three fields and can be traced as faint as g approximate to 24 mag. Using theoretical isochrone fitting, we derive an age of 9.1(-1.1)(+1.0) Gyr, a median abundance of [Fe/H] = -0.70(-0.20)(+0.15) dex, and a heliocentric distance of 30.9 +/- 3.0 kpc for the main sequence of the Sgr Stream Branch A. The dominant main-sequence populations in the two VSS/VOD fields (A circle dot approximate to 265 degrees, B circle dot approximate to 13 degrees) are located at a mean distance of 23.3 +/- 1.6 kpc and have an age of similar to 8.2 Gyr, and an abundance of [Fe/H] approximate to -0.67(-0.12)(+0.16) dex, similar to the Sgr Stream stars. These statistically robust parameters, derived from the photometry of 260 main-sequence stars, are also in good agreement with the age of the main population in the Sgr dwarf galaxy (8.0 +/- 1.5 Gyr). They also agree with the peak in the metallicity distribution of 2-3 Gyr oldMgiants, [Fe/H] approximate to -0.6 dex, in the Sgr north leading arm. We then compare the results from the VSS/VOD fields with the Sgr Tidal Stream model by Law & Majewski based on a triaxial Galactic halo shape that is empirically calibrated with Sloan Digital Sky Survey Sgr A-branch and Two Micron All Sky Survey M-giant stars. We find that the most prominent feature in the CMDs, the main-sequence population at 23 kpc, is not explained by the model. Instead the model predicts in these directions a low-density filamentary structure of Sgr debris stars at similar to 9 kpc and a slightly higher concentration of Sgr stars spread over a heliocentric distance range of 42-53 kpc. At best there is only marginal evidence for the presence of these populations in our data. Our findings then suggest that while there are probably some Sgr debris stars present, the dominant stellar population in the VOD originates from a different halo structure that has an almost identical age and metallicity as some sections of the Sgr tidal stream. C1 [Jerjen, H.; Da Costa, G. S.; Tisserand, P.] Australian Natl Univ, Mt Stromlo Observ, Res Sch Astron & Astrophys, Weston, ACT 2611, Australia. [Willman, B.] Haverford Coll, Dept Astron, Haverford, PA 19041 USA. [Arimoto, N.] Natl Inst Nat Sci, Natl Astron Observ Japan, Subaru Telescope, Hilo, HI 96720 USA. [Arimoto, N.] Grad Univ Adv Studies, Dept Astron Sci, Mitaka, Tokyo, Japan. [Okamoto, S.] Peking Univ, Kavli Inst Astron & Astrophys, Beijing 100871, Peoples R China. [Mateo, M.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Saviane, I.] European So Observ, Santiago 19, Chile. [Walsh, S.] Australian Astron Observ, N Ryde, NSW 1670, Australia. [Geha, M.] Yale Univ, Dept Astron, New Haven, CT 06520 USA. [Jordan, A.; Zoccali, M.] Pontificia Univ Catolica Chile, Dept Astron & Astrofis, Santiago 7820436, Chile. [Jordan, A.; Zoccali, M.] Milky Way Millennium Nucleus, Santiago 7820436, Chile. [Olszewski, E.] Univ Arizona, Steward Observ, Tucson, AZ USA. [Walker, M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Kroupa, P.] Univ Bonn, Argelander Inst Astron, D-53121 Bonn, Germany. RP Jerjen, H (reprint author), Australian Natl Univ, Mt Stromlo Observ, Res Sch Astron & Astrophys, Via Cotter Rd, Weston, ACT 2611, Australia. RI Walker, Matthew/P-1777-2014; OI Walker, Matthew/0000-0003-2496-1925; Jordan, Andres/0000-0002-5389-3944 FU Go8-DAAD-Australia/Germany Joint Research Cooperation Scheme; Access to Major Research Facilities Programme, a component of the International Science Linkages established under the Australian Government innovation statement, Backing Australia's Ability; Australian Research Council [DP0878137, DP120100475]; NSF [AST-0908446, AST-0807498]; BASAL [CATA PFB-06]; FONDAP [CFA 15010003,]; Chilean Ministry for the Economy, Development, and Tourisms Programa Iniciativa Cientifica Milenio [P07-021-F]; Fondecyt [REGULAR 1110393] FX Renee Kraan-Korteweg for reading the early versions of the manuscript. H.J. and P.K. acknowledge financial support from the Go8-DAAD-Australia/Germany Joint Research Cooperation Scheme and H.J. and P.T. acknowledge financial support from the Access to Major Research Facilities Programme, which is a component of the International Science Linkages established under the Australian Government innovation statement, Backing Australia's Ability. This research is also supported in part by the Australian Research Council through Discovery Projects grants DP0878137 and DP120100475. B.W. thanks NSF AST-0908446. A.J. and M.Z. acknowledge support from BASAL CATA PFB-06, FONDAP CFA 15010003, the Chilean Ministry for the Economy, Development, and Tourisms Programa Iniciativa Cientifica Milenio through grant P07-021-F, awarded to The Milky Way Millennium Nucleus, and Fondecyt REGULAR 1110393. E.O. acknowledges American NSF support through grant AST-0807498. The authors are grateful to David Law and Steven Majewski for making the details of their model data publicly available. NR 58 TC 5 Z9 5 U1 1 U2 7 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAY 20 PY 2013 VL 769 IS 1 AR 14 DI 10.1088/0004-637X/769/1/14 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 157NL UT WOS:000319904500014 ER PT J AU Levi, A Sasselov, D Podolak, M AF Levi, A. Sasselov, D. Podolak, M. TI VOLATILE TRANSPORT INSIDE SUPER-EARTHS BY ENTRAPMENT IN THE WATER-ICE MATRIX SO ASTROPHYSICAL JOURNAL LA English DT Article DE planets and satellites: composition; planets and satellites: interiors ID HIGH-PRESSURE; METHANE HYDRATE; TRANSMISSION SPECTRUM; ATMOSPHERIC METHANE; THERMAL EXPANSIVITY; ROOM-TEMPERATURE; SOLID METHANE; LOW-MASS; GPA; PLANETS AB Whether volatiles can be entrapped in a background matrix composing planetary envelopes and be dragged via convection to the surface is a key question in understanding atmospheric fluxes, cycles, and composition. In this paper, we consider super-Earths with an extensive water mantle (i.e., water planets), and the possibility of entrapment of methane in their extensive water-ice envelopes. We adopt the theory developed by van der Waals & Platteeuw for modeling solid solutions, often used for modeling clathrate hydrates, and modify it in order to estimate the thermodynamic stability field of a new phase called methane filled ice Ih. We find that in comparison to water ice VII the filled ice Ih structure may be stable not only at the high pressures but also at the high temperatures expected at the core-water mantle transition boundary of water planets. C1 [Levi, A.; Podolak, M.] Tel Aviv Univ, Dept Geophys & Planetary Sci, IL-69978 Tel Aviv, Israel. [Levi, A.; Sasselov, D.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Levi, A (reprint author), Tel Aviv Univ, Dept Geophys & Planetary Sci, IL-69978 Tel Aviv, Israel. EM amitlevi.planetphys@gmail.com OI LEVI, AMIT/0000-0003-1080-1007 NR 45 TC 12 Z9 12 U1 1 U2 11 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAY 20 PY 2013 VL 769 IS 1 AR 29 DI 10.1088/0004-637X/769/1/29 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 157NL UT WOS:000319904500029 ER PT J AU Liao, YW Lin, KY Huang, YD Wu, JHP Ho, PTP Chen, MT Huang, CWL Koch, PM Nishioka, H Cheng, TA Fu, SY Liu, GC Molnar, SM Umetsu, K Wang, FC Chang, YY Han, CC Li, CT Martin-Cocher, P Oshiro, P AF Liao, Yu-Wei Lin, Kai-Yang Huang, Yau-De Wu, Jiun-Huei Proty Ho, Paul T. P. Chen, Ming-Tang Huang, Chih-Wei Locutus Koch, Patrick M. Nishioka, Hiroaki Cheng, Tai-An Fu, Szu-Yuan Liu, Guo-Chin Molnar, Sandor M. Umetsu, Keiichi Wang, Fu-Cheng Chang, Yu-Yen Han, Chih-Chiang Li, Chao-Te Martin-Cocher, Pierre Oshiro, Peter TI PLATFORM DEFORMATION PHASE CORRECTION FOR THE AMiBA-13 COPLANAR INTERFEROMETER SO ASTROPHYSICAL JOURNAL LA English DT Article DE instrumentation: interferometers ID MICROWAVE BACKGROUND ANISOTROPY; MASSIVE GALAXY CLUSTERS; SCALING RELATIONS; ARRAY AB We present a new way to solve the platform deformation problem of coplanar interferometers. The platform of a coplanar interferometer can be deformed due to driving forces and gravity. A deformed platform will induce extra components into the geometric delay of each baseline and change the phases of observed visibilities. The reconstructed images will also be diluted due to the errors of the phases. The platform deformations of The Yuan-Tseh Lee Array for Microwave Background Anisotropy (AMiBA) were modeled based on photogrammetry data with about 20 mount pointing positions. We then used the differential optical pointing error between two optical telescopes to fit the model parameters in the entire horizontal coordinate space. With the platform deformation model, we can predict the errors of the geometric phase delays due to platform deformation with a given azimuth and elevation of the targets and calibrators. After correcting the phases of the radio point sources in the AMiBA interferometric data, we recover 50%-70% flux loss due to phase errors. This allows us to restore more than 90% of a source flux. The method outlined in this work is not only applicable to the correction of deformation for other coplanar telescopes but also to single-dish telescopes with deformation problems. This work also forms the basis of the upcoming science results of AMiBA-13. C1 [Liao, Yu-Wei; Lin, Kai-Yang; Huang, Yau-De; Ho, Paul T. P.; Chen, Ming-Tang; Huang, Chih-Wei Locutus; Koch, Patrick M.; Nishioka, Hiroaki; Umetsu, Keiichi; Han, Chih-Chiang; Li, Chao-Te; Martin-Cocher, Pierre; Oshiro, Peter] Acad Sinica, Inst Astron & Astrophys, Taipei 10617, Taiwan. [Wu, Jiun-Huei Proty; Huang, Chih-Wei Locutus; Cheng, Tai-An; Fu, Szu-Yuan; Wang, Fu-Cheng] Natl Taiwan Univ, Inst Astrophys, Dept Phys, Taipei 10617, Taiwan. [Wu, Jiun-Huei Proty; Huang, Chih-Wei Locutus; Cheng, Tai-An; Fu, Szu-Yuan; Wang, Fu-Cheng] Natl Taiwan Univ, Ctr Theoret Sci, Taipei 10617, Taiwan. [Ho, Paul T. P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Liu, Guo-Chin] Tamkang Univ, Dept Phys, Tamsui 25137, New Taipei City, Taiwan. [Molnar, Sandor M.] Natl Taiwan Univ, Leung Ctr Cosmol & Particle Astrophys, Taipei 10617, Taiwan. [Chang, Yu-Yen] Max Planck Inst Astron, D-69117 Heidelberg, Germany. RP Liao, YW (reprint author), Acad Sinica, Inst Astron & Astrophys, POB 23-141, Taipei 10617, Taiwan. EM ywliao@asiaa.sinica.edu.tw; jhpw@phys.ntu.edu.tw OI WU, JIUN-HUEI/0000-0001-9608-7662; Umetsu, Keiichi/0000-0002-7196-4822 FU Ministry of Education; National Science Council (NSC) [NSC 98-2119-M-001-024-MY4]; Academia Sinica, Taiwan; AMiBA project FX We thank the Ministry of Education, the National Science Council (NSC; NSC code: NSC 98-2119-M-001-024-MY4), and the Academia Sinica, Taiwan, for their funding and supporting of the AMiBA project. Y.W.L. thanks M. Birkinshaw for helpful suggestions. The guiding, supporting, hard working, and helpful discussions of the entire AMiBA team are also acknowledged. NR 19 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 MAY 20 PY 2013 VL 769 IS 1 AR 71 DI 10.1088/0004-637X/769/1/71 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 157NL UT WOS:000319904500071 ER PT J AU Neufeld, DA Wu, YW Kraus, A Menten, KM Tolls, V Melnick, GJ Nagy, Z AF Neufeld, David A. Wu, Yuanwei Kraus, Alex Menten, Karl M. Tolls, Volker Melnick, Gary J. Nagy, Zsofia TI HERSCHEL*/HIFI OBSERVATIONS OF A NEW INTERSTELLAR WATER MASER: THE 5(32)-4(41) TRANSITION AT 620.701 GHz SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM: molecules; masers; molecular processes; submillimeter: ISM ID EXTRAORDINARY SOURCES HEXOS; VY CANIS MAJORIS; ORION SOURCE I; H2O MASERS; RATE COEFFICIENTS; EMISSION; HIFI; W49N; KL; EXCITATION AB Using the Herschel Space Observatory's Heterodyne Instrument for the Far-Infrared, we have performed mapping observations of the 620.701 GHz 5(32)-4(41) transition of ortho-H2O within a similar to 1'.5 x 1'.5 region encompassing the Kleinmann-Low nebula in Orion (Orion-KL), and pointed observations of that transition toward the Orion South condensation and the W49N region of high-mass star formation. Using the Effelsberg 100 m radio telescope, we obtained ancillary observations of the 22.23508 GHz 6(16)-5(23) water maser transition; in the case of Orion-KL, the 621 GHz and 22 GHz observations were carried out within 10 days of each other. The 621 GHz water line emission shows clear evidence for strong maser amplification in all three sources, exhibiting narrow (similar to 1 km s(-1) FWHM) emission features that are coincident (kinematically and/or spatially) with observed 22 GHz features. Moreover, in the case of W49N-for which observations were available at three epochs spanning a 2 yr period-the spectra exhibited variability. The observed 621 GHz/22 GHz line ratios are consistent with a maser pumping model in which the population inversions arise from the combined effects of collisional excitation and spontaneous radiative decay, and the inferred physical conditions can plausibly arise in gas heated by either dissociative or non-dissociative shocks. The collisional excitation model also predicts that the 22 GHz population inversion will be quenched at higher densities than that of the 621 GHz transition, providing a natural explanation for the observational fact that 22 GHz maser emission appears to be a necessary but insufficient condition for 621 GHz maser emission. C1 [Neufeld, David A.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Wu, Yuanwei; Kraus, Alex; Menten, Karl M.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Tolls, Volker; Melnick, Gary J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Nagy, Zsofia] Univ Groningen, Kapteyn Astron Inst, NL-9747 AD Groningen, Netherlands. RP Neufeld, DA (reprint author), Johns Hopkins Univ, Dept Phys & Astron, 3400 North Charles St, Baltimore, MD 21218 USA. FU NASA FX Support for this work was provided by NASA through an award issued by JPL/Caltech. This study was partly based on observations with the 100 m telescope of the MPIfR (Max-Planck-Institut fur Radioastronomie) at Effelsberg. We are grateful to M. Gerin for useful comments on the manuscript. We thank S. Jones and collaborators for providing us with a draft of their results prior to publication. NR 47 TC 8 Z9 8 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 MAY 20 PY 2013 VL 769 IS 1 AR 48 DI 10.1088/0004-637X/769/1/48 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 157NL UT WOS:000319904500048 ER PT J AU Salyk, C Herczeg, GJ Brown, JM Blake, GA Pontoppidan, KM van Dishoeck, EF AF Salyk, Colette Herczeg, Gregory J. Brown, Joanna M. Blake, Geoffrey A. Pontoppidan, Klaus M. van Dishoeck, Ewine F. TI MEASURING PROTOPLANETARY DISK ACCRETION WITH HI PFUND beta SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; protoplanetary disks; stars: formation; stars: pre-main sequence ID T-TAURI-STARS; HERBIG AE/BE STARS; MAIN-SEQUENCE STARS; YOUNG STELLAR OBJECTS; INTERMEDIATE-MASS STARS; SPITZER C2D SURVEY; SPECTRAL ENERGY-DISTRIBUTIONS; CO ROVIBRATIONAL EMISSION; AURIGA MOLECULAR CLOUD; RHO-OPHIUCHI CLOUD AB In this work, we introduce the use of HI Pfund beta (Pf beta; 4.6538 mu m) as a tracer of mass accretion from protoplanetary disks onto young stars. Pf beta was serendipitously observed in NIRSPEC and CRIRES surveys of CO fundamental emission, amounting to a sample size of 120 young stars with detected Pf beta emission. Using a subsample of disks with previously measured accretion luminosities, we show that Pf beta line luminosity is well correlated with accretion luminosity over a range of at least three orders of magnitude. We use this correlation to derive accretion luminosities for all 120 targets, 65 of which are previously unreported in the literature. The conversion from accretion luminosity to accretion rate is limited by the availability of stellar mass and radius measurements; nevertheless, we also report accretion rates for 67 targets, 16 previously unmeasured. Our large sample size and our ability to probe high extinction values allow for relatively unbiased comparisons between different types of disks. We find that the transitional disks in our sample have lower than average Pf beta line luminosities, and thus accretion luminosities, at a marginally significant level. We also show that high Pf beta equivalent width is a signature of transitional disks with high inner disk gas/dust ratios. In contrast, we find that disks with signatures of slow disk winds have Pf beta luminosities comparable to those of other disks in our sample. Finally, we investigate accretion rates for stage I disks, including significantly embedded targets. We find that stage I and stage II disks have statistically indistinguishable Pf beta line luminosities, implying similar accretion rates, and that the accretion rates of stage I disks are too low to be consistent with quiescent accretion. Our results are instead consistent with both observational and theoretical evidence that stage I objects experience episodic, rather than quiescent, accretion. C1 [Salyk, Colette] Natl Opt Astron Observ, Tucson, AZ 85719 USA. [Herczeg, Gregory J.] Peking Univ, Kavli Inst Astron & Astrophys, Beijing 100871, Peoples R China. [Brown, Joanna M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Blake, Geoffrey A.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. [Pontoppidan, Klaus M.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [van Dishoeck, Ewine F.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [van Dishoeck, Ewine F.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. RP Salyk, C (reprint author), Natl Opt Astron Observ, 950 North Cherry Ave, Tucson, AZ 85719 USA. EM csalyk@noao.edu FU NOAO Leo Goldberg Fellowship; University of Texas at Austin McDonald Observatory Harlan J. Smith Postdoctoral Fellowship; EU A-ERC [291141]; National Aeronautics and Space Administration; W. M. Keck Foundation FX C.S. thanks Casey Deen and Chris Sneden for providing an introduction to MOOG. C.S. also acknowledges the financial support of the NOAO Leo Goldberg Fellowship program and the University of Texas at Austin McDonald Observatory Harlan J. Smith Postdoctoral Fellowship. E.v.D. is supported by EU A-ERC grant 291141. This publication makes use of data products from the Wide-field Infrared Survey Explorer, which is a joint project of the University of California, Los Angeles, and the Jet Propulsion Laboratory/California Institute of Technology, funded by the National Aeronautics and Space Administration. 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. NR 189 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 EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAY 20 PY 2013 VL 769 IS 1 AR 21 DI 10.1088/0004-637X/769/1/21 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 157NL UT WOS:000319904500021 ER PT J AU Sanders, NE Soderberg, AM Foley, RJ Chornock, R Milisavljevic, D Margutti, R Drout, MR Moe, M Berger, E Brown, WR Lunnan, R Smartt, SJ Fraser, M Kotak, R Magill, L Smith, KW Wright, D Huang, K Urata, Y Mulchaey, JS Rest, A Sand, DJ Chomiuk, L Friedman, AS Kirshner, RP Marion, GH Tonry, JL Burgett, WS Chambers, KC Hodapp, KW Kudritzki, RP Price, PA AF Sanders, N. E. Soderberg, A. M. Foley, R. J. Chornock, R. Milisavljevic, D. Margutti, R. Drout, M. R. Moe, M. Berger, E. Brown, W. R. Lunnan, R. Smartt, S. J. Fraser, M. Kotak, R. Magill, L. Smith, K. W. Wright, D. Huang, K. Urata, Y. Mulchaey, J. S. Rest, A. Sand, D. J. Chomiuk, L. Friedman, A. S. Kirshner, R. P. Marion, G. H. Tonry, J. L. Burgett, W. S. Chambers, K. C. Hodapp, K. W. Kudritzki, R. P. Price, P. A. TI PS1-12sk IS A PECULIAR SUPERNOVA FROM A He-RICH PROGENITOR SYSTEM IN A BRIGHTEST CLUSTER GALAXY ENVIRONMENT SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: clusters: general; galaxies: star formation; stars: winds, outflows; supernovae: general; supernovae: individual (PS1-12sk) ID CORE-COLLAPSE SUPERNOVAE; DIGITAL SKY SURVEY; SWIFT ULTRAVIOLET/OPTICAL TELESCOPE; DELAY-TIME DISTRIBUTION; ACCRETING WHITE-DWARFS; STAR-FORMATION RATES; GAMMA-RAY BURSTS; IA SUPERNOVA; CIRCUMSTELLAR MEDIUM; HOST GALAXIES AB We report on our discovery and observations of the Pan-STARRS1 supernova (SN) PS1-12sk, a transient with properties that indicate atypical star formation in its host galaxy cluster or pose a challenge to popular progenitor system models for this class of explosion. The optical spectra of PS1-12sk classify it as a Type Ibn SN (SN Ibn; cf. SN 2006jc), dominated by intermediate-width (3 x 10(3) km s(-1)) and time variable He I emission. Our multi-wavelength monitoring establishes the rise time dt similar to 9-23 days and shows an NUV-NIR spectral energy distribution with temperature greater than or similar to 17x10(3) K and a peak magnitude of M-z = -18.88 +/- 0.02 mag. SN Ibn spectroscopic properties are commonly interpreted as the signature of a massive star (17-100M(circle dot)) explosion within an He-enriched circumstellar medium. However, unlike previous SNe Ibn, PS1-12sk is associated with an elliptical brightest cluster galaxy, CGCG 208-042 (z = 0.054) in cluster RXC J0844.9+4258. The expected probability of an event like PS1-12sk in such environments is low given the measured infrequency of core-collapse SNe in red-sequence galaxies compounded by the low volumetric rate of SN Ibn. Furthermore, we find no evidence of star formation at the explosion site to sensitive limits (Sigma(H alpha) less than or similar to 2 x 10(-3) M-circle dot yr(-1) kpc(-2)). We therefore discuss white dwarf binary systems as a possible progenitor channel for SNe Ibn. We conclude that PS1-12sk represents either a fortuitous and statistically unlikely discovery, evidence for a top-heavy initial mass function in galaxy cluster cooling flow filaments, or the first clue suggesting an alternate progenitor channel for SNe Ibn. C1 [Sanders, N. E.; Soderberg, A. M.; Foley, R. J.; Chornock, R.; Milisavljevic, D.; Margutti, R.; Drout, M. R.; Moe, M.; Berger, E.; Brown, W. R.; Lunnan, R.; Friedman, A. S.; Kirshner, R. P.; Marion, G. H.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Smartt, S. J.; Fraser, M.; Kotak, R.; Magill, L.; Smith, K. W.; Wright, D.] Queens Univ Belfast, Astrophys Res Ctr, Sch Maths & Phys, Belfast BT7 1NN, Antrim, North Ireland. [Huang, K.] Acad Sinica, Inst Astron & Astrophys, Taipei 106, Taiwan. [Urata, Y.] Natl Cent Univ, Inst Astron, Chungli 32054, Taiwan. [Mulchaey, J. S.] Carnegie Observ, Pasadena, CA 91101 USA. [Rest, A.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Sand, D. J.] Texas Tech Univ, Dept Phys, Lubbock, TX 79409 USA. [Chomiuk, L.] Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA. [Friedman, A. S.] MIT, Cambridge, MA 02138 USA. [Tonry, J. L.; Burgett, W. S.; Chambers, K. C.; Hodapp, K. W.; Kudritzki, R. P.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Price, P. A.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. RP Sanders, NE (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM nsanders@cfa.harvard.edu RI Friedman, Andrew/I-4691-2013; OI Friedman, Andrew/0000-0003-1334-039X; Lunnan, Ragnhild/0000-0001-9454-4639; Kotak, Rubina/0000-0001-5455-3653; Fraser, Morgan/0000-0003-2191-1674; Chambers, Kenneth /0000-0001-6965-7789 FU National Science Foundation [NSF PHY11-25915, AST-1009749]; David and Lucile Packard Foundation Fellowship for Science and Engineering; NSF STS postdoctoral fellowship; National Aeronautics and Space Administration through the Planetary Science Division of the NASA Science Mission Directorate [NNX08AR22G]; NSF [AST-1211196]; NASA; US National Science Foundation (NSF); National Aeronautics and Space Administration FX This work was supported by the National Science Foundation through a Graduate Research Fellowship provided to N.E.S. Support for this work was provided by the David and Lucile Packard Foundation Fellowship for Science and Engineering awarded to A.M.S. A.S.F. acknowledges support through an NSF STS postdoctoral fellowship. R.P.K. was supported in part by the National Science Foundation under grant NSF PHY11-25915 to the Kavli Institute for Theoretical Physics.; The Pan-STARRS1 Surveys (PS1) have been made possible through contributions of the Institute for Astronomy, the University of Hawaii, the Pan-STARRS Project Office, the Max-Planck Society and its participating institutes, the Max Planck Institute for Astronomy, Heidelberg and the Max Planck Institute for Extraterrestrial Physics, Garching, The Johns Hopkins University, Durham University, the University of Edinburgh, Queen's University Belfast, the Harvard-Smithsonian Center for Astrophysics, the Las Cumbres Observatory Global Telescope Network Incorporated, the National Central University of Taiwan, the Space Telescope Science Institute, and the National Aeronautics and Space Administration under grant No. NNX08AR22G issued through the Planetary Science Division of the NASA Science Mission Directorate.; Partial support for this work was provided by National Science Foundation grant AST-1009749. The CfA Supernova Program is supported in part by NSF grant AST-1211196. This publication makes use of data products from the 2MASS survey, funded by NASA and the US National Science Foundation (NSF). Computations were run on machines in the Harvard Astronomy Computation Facility supported by the Optical and Infrared Astronomy Division of the Harvard-Smithsonian Center for Astrophysics. Other computations were performed on the Harvard Odyssey cluster, supported by the FAS Science Division Research Computing Group at Harvard University.; This research made use of APLpy, an open-source plotting package for Python hosted at http://aplpy.github.com, 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 152 TC 14 Z9 16 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 MAY 20 PY 2013 VL 769 IS 1 AR 39 DI 10.1088/0004-637X/769/1/39 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 157NL UT WOS:000319904500039 ER PT J AU Seward, FD Smith, RK AF Seward, F. D. Smith, R. K. TI AZIMUTHAL STRUCTURE OF THE Cyg X-2 X-RAY DUST HALO SO ASTROPHYSICAL JOURNAL LA English DT Article DE dust; extinction - X-rays; individual (CygX-2) ID INTERSTELLAR DUST; CHANDRA OBSERVATIONS; SCATTERING HALO; GRAINS; PERSEI; ROSAT AB There is little information concerning the azimuthal distribution of X-rays in dust-scattering halos. This paper describes a Chandra observation of the bright source Cyg X-2 designed specifically for this purpose. After measuring and subtracting approximate to 10% instrument effects, we find the scattering halo to be rather uniform with possible fluctuations in the surface brightness of only 2%. Observations and data processing are discussed in detail. Some information about the dust distribution is derived. C1 [Seward, F. D.; Smith, R. K.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Seward, FD (reprint author), Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA. FU National Aeronautics and Space Administration [NNX10AD10G, NAS8-03060]; Chandra X-Ray Observatory Center [GO7-8141X] FX Support for this work was provided by the National Aeronautics and Space Administration through grant NNX10AD10G and by Chandra Award Number GO7-8141X 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 NAS8-03060. We thank Bruce Draine for suggesting that measurements of dust grain structure might be accomplished with Chandra observations. NR 26 TC 5 Z9 5 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAY 20 PY 2013 VL 769 IS 1 AR 17 DI 10.1088/0004-637X/769/1/17 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 157NL UT WOS:000319904500017 ER PT J AU Townsend, RHD Rivinius, T Rowe, JF Moffat, AFJ Matthews, JM Bohlender, D Neiner, C Telting, JH Guenther, DB Kallinger, T Kuschnig, R Rucinski, SM Sasselov, D Weiss, WW AF Townsend, R. H. D. Rivinius, Th. Rowe, J. F. Moffat, A. F. J. Matthews, J. M. Bohlender, D. Neiner, C. Telting, J. H. Guenther, D. B. Kallinger, T. Kuschnig, R. Rucinski, S. M. Sasselov, D. Weiss, W. W. TI MOST OBSERVATIONS OF sigma Ori E: CHALLENGING THE CENTRIFUGAL BREAKOUT NARRATIVE SO ASTROPHYSICAL JOURNAL LA English DT Article DE circumstellar matter; stars: chemically peculiar; stars: early-type; stars: individual (HD 37479); stars: magnetic field; stars: rotation ID RIGIDLY ROTATING MAGNETOSPHERE; HELIUM-STRONG STARS; ORIONIS-E; MAGNETIC-FIELD; HR 7355-STAR; PHOTOMETRY; DISCOVERY; CLUSTER; SPACE; MODEL AB We present results from three weeks' photometric monitoring of the magnetic helium-strong star sigma Ori E using the Microvariability and Oscillations of Stars microsatellite. The star's light curve is dominated by twice-per-rotation eclipse-like dimmings arising when magnetospheric clouds transit across and occult the stellar disk. However, no evidence is found for any abrupt centrifugal breakout of plasma from the magnetosphere, either in the residual flux or in the depths of the light minima. Motivated by this finding we compare the observationally inferred magnetospheric mass against that predicted by a breakout analysis. The large discrepancy between the values leads us to argue that centrifugal breakout does not play a significant role in establishing the magnetospheric mass budget of sigma Ori E. C1 [Townsend, R. H. D.] Univ Wisconsin, Dept Astron, Madison, WI 53706 USA. [Rivinius, Th.] ESO European Org Astron Res Southern Hamisphere, Santiago 19001, Casilla, Chile. [Rowe, J. F.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Moffat, A. F. J.] Univ Montreal, Dept Phys, Montreal, PQ H3C 3J7, Canada. [Matthews, J. M.; Kallinger, T.; Kuschnig, R.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada. [Bohlender, D.] Natl Res Council Canada, Herzberg Inst Astrophys, Victoria, BC V9E 2E7, Canada. [Neiner, C.] Univ Paris Diderot, UPMC, Observatoire Paris, UMR 8109,CNRS,LESIA, F-92195 Meudon, France. [Guenther, D. B.] St Marys Univ, Dept Phys & Astron, Halifax, NS B3H 3C3, Canada. [Kallinger, T.; Kuschnig, R.; Weiss, W. W.] Univ Vienna, Inst Astron, A-1180 Vienna, Austria. [Rucinski, S. M.] Univ Toronto, Dept Astron & Astrophys, Toronto, ON M5S 3H4, Canada. [Sasselov, D.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Townsend, RHD (reprint author), Univ Wisconsin, Dept Astron, 2535 Sterling Hall,475 N Charter St, Madison, WI 53706 USA. EM townsend@astro.wisc.edu OI Kallinger, Thomas/0000-0003-3627-2561 FU NSF [AST-0908688, AST-0904607]; NASA [NNX12AC72G]; NSERC (Canada); Austrian Science Fund [P22691-N16] FX R.H.D.T. acknowledges support from NSF awards AST-0908688 and AST-0904607, and NASA award NNX12AC72G. A.F.J.M., D.B.G., J.M.M., and S.M.R. are grateful for financial support from NSERC (Canada). R.K. and W.W. acknowledge support by the Austrian Science Fund P22691-N16. NR 45 TC 11 Z9 11 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAY 20 PY 2013 VL 769 IS 1 AR 33 DI 10.1088/0004-637X/769/1/33 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 157NL UT WOS:000319904500033 ER PT J AU Visser, R Jorgensen, JK Kristensen, LE van Dishoeck, EF Bergin, EA AF Visser, Ruud Jorgensen, Jes K. Kristensen, Lars E. van Dishoeck, Ewine F. Bergin, Edwin A. TI HOT WATER IN THE INNER 100 AU OF THE CLASS 0 PROTOSTAR NGC 1333 IRAS2A SO ASTROPHYSICAL JOURNAL LA English DT Article DE astrochemistry - circumstellar matter - stars; formation - stars; protostars - techniques; spectroscopic ID STAR-FORMING REGIONS; LOW-MASS PROTOSTARS; YOUNG STELLAR OBJECTS; ROTATIONAL-EXCITATION; HERSCHEL-HIFI; SUBMILLIMETER ARRAY; CIRCUMSTELLAR DISKS; CHEMICAL EVOLUTION; HIGH-TEMPERATURE; LINE EMISSION AB Evaporation of water ice above 100 K in the inner few 100 AU of low-mass embedded protostars (the so-called hot core) should produce quiescent water vapor abundances of similar to 10(-4) relative to H-2. Observational evidence so far points at abundances of only a few 10(-6). However, these values are based on spherical models, which are known from interferometric studies to be inaccurate on the relevant spatial scales. Are hot cores really that much drier than expected, or are the lowabundances an artifact of the inaccurate physical models? We present deep velocity-resolved Herschel-HIFI spectra of the 3(12)-3(03) lines of (H2O)-O-16 and (H2O)-O-18 (1097 GHz, E-u/k = 249 K) in the low-mass Class 0 protostar NGC 1333 IRAS2A. A spherical radiative transfer model with a power-law density profile is unable to reproduce both the HIFI data and existing interferometric data on the (H2O)-O-18 3(13)-2(20) line (203 GHz, Eu/k = 204 K). Instead, the HIFI spectra likely show optically thick emission from a hot core with a radius of about 100 AU. The mass of the hot core is estimated from the (CO)-O-18 J = 9-8 and 10-9 lines. We derive a lower limit to the hot water abundance of 2 x 10(-5), consistent with the theoretical predictions of similar to 10(-4). The revised HDO/H2O abundance ratio is 1 x 10(-3), an order of magnitude lower than previously estimated. C1 [Visser, Ruud; Bergin, Edwin A.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Jorgensen, Jes K.] Univ Copenhagen, Niels Bohr Inst, DK-2100 Copenhagen O, Denmark. [Jorgensen, Jes K.] Univ Copenhagen, Nat Hist Museum Denmark, Ctr Star & Planet Format, DK-1350 Copenhagen K, Denmark. [Kristensen, Lars E.; van Dishoeck, Ewine F.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [Kristensen, Lars E.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [van Dishoeck, Ewine F.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. RP Visser, R (reprint author), Univ Michigan, Dept Astron, 500 Church St, Ann Arbor, MI 48109 USA. EM visserr@umich.edu RI Jorgensen, Jes Kristian/L-7936-2014; Kristensen, Lars/F-4774-2011 OI Jorgensen, Jes Kristian/0000-0001-9133-8047; Kristensen, Lars/0000-0003-1159-3721 FU NASA; Lundbeck Foundation Junior Group Leader Fellowship; Danish National Research Foundation; Netherlands Research School for Astronomy (NOVA); Spinoza grant [614.001.008]; Netherlands Organisation for Scientific Research (NWO); European Community's Seventh Framework Programme FX The authors thank the entire WISH team-in particular the internal referees Asuncion Fuente and Silvia Leurini-for valuable discussions. Magnus Persson kindly helped with the PdBI/HIFI comparison and Sebastien Maret was quick to fix a bug in CLASS. We thank Friedrich Wyrowski and the APEX Arnold Benz likewise for the 1894 GHz line. Support for this work was provided by NASA through an award issued by JPL/Caltech. J.K.J. is supported by a Lundbeck Foundation Junior Group Leader Fellowship as well as the Centre of Star and Planet Formation funded by the Danish National Research Foundation. Astrochemistry in Leiden is supported by the Netherlands Research School for Astronomy (NOVA), by a Spinoza grant and grant 614.001.008 from the Netherlands Organisation for Scientific Research (NWO), and by the European Community's Seventh Framework Programme FP7/2007-2013 under grant agreement 238258 (LASSIE). 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 USA. 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); Netherlands: SRON, TUD; Poland: CAMK, CBK; Spain: Observatorio Astronomico Nacional (IGN), Centro de Astrobiologia (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. NR 61 TC 17 Z9 17 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAY 20 PY 2013 VL 769 IS 1 AR 19 DI 10.1088/0004-637X/769/1/19 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 157NL UT WOS:000319904500019 ER PT J AU Xu, Y Li, JJ Reid, MJ Menten, KM Zheng, XW Brunthaler, A Moscadelli, L Dame, TM Zhang, B AF Xu, Y. Li, J. J. Reid, M. J. Menten, K. M. Zheng, X. W. Brunthaler, A. Moscadelli, L. Dame, T. M. Zhang, B. TI ON THE NATURE OF THE LOCAL SPIRAL ARM OF THE MILKY WAY SO ASTROPHYSICAL JOURNAL LA English DT Article DE astrometry - Galaxy; kinematics and dynamics - masers - stars; formation - techniques; high angular resolution ID STAR-FORMING REGIONS; H-II REGIONS; ULTRACOMPACT HII-REGIONS; BASE-LINE INTERFEROMETRY; VLBA CALIBRATOR SURVEY; YOUNG STELLAR OBJECTS; LUMINOUS IRAS SOURCES; H2O MASERS; TRIGONOMETRIC PARALLAXES; MOLECULAR CLOUDS AB Trigonometric parallax measurements of nine water masers associated with the Local Arm of the Milky Way were carried out as part of the BeSSeL Survey using the Very Long Baseline Array. When combined with 21 other parallax measurements from the literature, the data allow us to study the distribution and three-dimensional motions of star forming regions in the spiral arm over the entire northern sky. Our results suggest that the Local Arm does not have the large pitch angle characteristic of a short spur. Instead its active star formation, overall length (> 5 kpc), and shallow pitch angle (similar to 10 degrees) suggest that it is more like the adjacent Perseus and Sagittarius Arms; perhaps it is a branch of one of these arms. Contrary to previous results, we find the Local Arm to be closer to the Perseus than to the Sagittarius Arm, suggesting that a branching from the former may be more likely. An average peculiar motion of near zero toward both the Galactic center and north Galactic pole, and counter rotation of similar to 5 km s(-1) were observed, indicating that the Local Arm has similar kinematic properties as found for other major spiral arms. C1 [Xu, Y.; Li, J. J.] Chinese Acad Sci, Purple Mt Observ, Nanjing 210008, Jiangsu, Peoples R China. [Li, J. J.; Menten, K. M.; Brunthaler, A.; Zhang, B.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Reid, M. J.; Dame, T. M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Zheng, X. W.] Nanjing Univ, Nanjing 20093, Jiangsu, Peoples R China. [Moscadelli, L.] INAF Osservatorio Astrofis Arcetri, I-50125 Florence, Italy. RP Xu, Y (reprint author), Chinese Acad Sci, Purple Mt Observ, Nanjing 210008, Jiangsu, Peoples R China. EM xuye@pmo.ac.cn OI Moscadelli, Luca/0000-0002-8517-8881 NR 96 TC 72 Z9 73 U1 3 U2 9 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAY 20 PY 2013 VL 769 IS 1 AR 15 DI 10.1088/0004-637X/769/1/15 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 157NL UT WOS:000319904500015 ER PT J AU Kuang, S Newchurch, MJ Burris, J Liu, X AF Kuang, Shi Newchurch, Michael J. Burris, John Liu, Xiong TI Ground-based lidar for atmospheric boundary layer ozone measurements SO APPLIED OPTICS LA English DT Article ID ABSORPTION CROSS-SECTIONS; TROPOSPHERIC OZONE; VERTICAL-DISTRIBUTION; DIAL MEASUREMENTS; AEROSOL LIDAR; RAMAN LIDAR; TEMPERATURE; ULTRAVIOLET; ALGORITHM; PROFILES AB Ground-based lidars are suitable for long-term ozone monitoring as a complement to satellite and ozonesonde measurements. However, current ground-based lidars are unable to consistently measure ozone below 500 m above ground level (AGL) due to both engineering issues and high retrieval sensitivity to various measurement errors. In this paper, we present our instrument design, retrieval techniques, and preliminary results that focus on the high-temporal profiling of ozone within the atmospheric boundary layer (ABL) achieved by the addition of an inexpensive and compact mini-receiver to the previous system. For the first time, to the best of our knowledge, the lowest, consistently achievable observation height has been extended down to 125 m AGL for a ground-based ozone lidar system. Both the analysis and preliminary measurements demonstrate that this lidar measures ozone with a precision generally better than +/- 10% at a temporal resolution of 10 min and a vertical resolution from 150 m at the bottom of the ABL to 550 m at the top. A measurement example from summertime shows that inhomogeneous ozone aloft was affected by both surface emissions and the evolution of ABL structures. (C) 2013 Optical Society of America C1 [Kuang, Shi; Newchurch, Michael J.] Univ Alabama, Dept Atmospher Sci, Huntsville, AL 35805 USA. [Burris, John] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Liu, Xiong] Harvard Smithsonian Ctr Astrophys, Atom & Mol Phys Div, Cambridge, MA 02138 USA. RP Kuang, S (reprint author), Univ Alabama, Dept Atmospher Sci, 320 Sparkman Dr, Huntsville, AL 35805 USA. EM kuang@nsstc.uah.edu RI Liu, Xiong/P-7186-2014 OI Liu, Xiong/0000-0003-2939-574X FU NASA's Science Mission Directorate; NOAA's National Environmental Satellite, Data, and Information Service (NESDIS) FX The authors thank Tom McGee of NASA/GSFC, Stuart McDermid, and Thierry Leblanc of NASA/JPL for extensive discussions about lidar instrumentation, Jack Kaye and Jay Al-Saadi of NASA/headquarters for continuing support, Wesley Cantrell and Guanyu Huang of UAHuntsville for providing the ozonesonde data, and Debra Hopson of the Huntsville Department of Natural Resources and Environmental Management for providing the surface ozone data. This work was supported by NASA's Science Mission Directorate and NOAA's National Environmental Satellite, Data, and Information Service (NESDIS). The UAHuntsville ozone lidar is affiliated with the Tropospheric Ozone Lidar NETwork (TOLNET) and the Network for Detection of Atmospheric Composition Change (NDACC). NR 53 TC 9 Z9 9 U1 1 U2 25 PU OPTICAL SOC AMER PI WASHINGTON PA 2010 MASSACHUSETTS AVE NW, WASHINGTON, DC 20036 USA SN 1559-128X J9 APPL OPTICS JI Appl. Optics PD MAY 20 PY 2013 VL 52 IS 15 BP 3557 EP 3566 DI 10.1364/AO.52.003557 PG 10 WC Optics SC Optics GA 149SP UT WOS:000319341800014 PM 23736241 ER PT J AU Batygin, K Stevenson, DJ AF Batygin, Konstantin Stevenson, David J. TI MASS-RADIUS RELATIONSHIPS FOR VERY LOW MASS GASEOUS PLANETS SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE planets and satellites: interiors; planets and satellites: physical evolution ID GIANT PLANETS; EXTRASOLAR PLANETS; HOT JUPITERS; SUPER-EARTHS; EVOLUTION; INTERIORS; NEPTUNES; KEPLER; SYSTEM; GAS AB Recently, the Kepler spacecraft has detected a sizable aggregate of objects, characterized by giant-planet-like radii and modest levels of stellar irradiation. With the exception of a handful of objects, the physical nature, and specifically the average densities, of these bodies remain unknown. Here, we propose that the detected giant planet radii may partially belong to planets somewhat less massive than Uranus and Neptune. Accordingly, in this work, we seek to identify a physically sound upper limit to planetary radii at low masses and moderate equilibrium temperatures. As a guiding example, we analyze the interior structure of the Neptune-mass planet Kepler-30d and show that it is acutely deficient in heavy elements, especially compared with its solar system counterparts. Subsequently, we perform numerical simulations of planetary thermal evolution and in agreement with previous studies, show that generally, 10-20 M-circle plus, multi-billion year old planets, composed of high density cores and extended H/He envelopes can have radii that firmly reside in the giant planet range. We subject our results to stability criteria based on extreme ultraviolet radiation, as well as Roche-lobe overflow driven mass-loss and construct mass-radius relationships for the considered objects. We conclude by discussing observational avenues that may be used to confirm or repudiate the existence of putative low mass, gas-dominated planets. C1 [Batygin, Konstantin] Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, Cambridge, MA 02138 USA. [Batygin, Konstantin; Stevenson, David J.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. RP Batygin, K (reprint author), Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, 60 Garden St, Cambridge, MA 02138 USA. EM kbatygin@cfa.harvard.edu FU Institute for Theory and Computation, Harvard-Smithsonian Center for Astrophysics FX We thank Tristan Guillot, Geoff Blake, Ruth Murray-Clay, Adam Burrows, and David Kipping for numerous useful conversations. We are grateful to the referee for a careful and insightful report that has greatly increased the quality of the manuscript. K.B. acknowledges the generous support from the ITC Prize Postdoctoral Fellowship at the Institute for Theory and Computation, Harvard-Smithsonian Center for Astrophysics. NR 40 TC 7 Z9 7 U1 1 U2 9 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 MAY 20 PY 2013 VL 769 IS 1 AR L9 DI 10.1088/2041-8205/769/1/L9 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 151HN UT WOS:000319451400009 ER PT J AU Foley, RJ Kirshner, RP AF Foley, Ryan J. Kirshner, Robert P. TI METALLICITY DIFFERENCES IN TYPE Ia SUPERNOVA PROGENITORS INFERRED FROM ULTRAVIOLET SPECTRA SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE supernovae: general; supernovae: individual (SN 2011by, SN 2011fe) ID HUBBLE-SPACE-TELESCOPE; HOST GALAXIES; SN 2011FE; LIGHT-CURVE; LUMINOSITIES; EXTINCTION; INDICATORS; REDSHIFT; DISTANCE; LAMBDA AB Two "twin" Type Ia supernovae (SNe Ia), SNe 2011by and 2011fe, have extremely similar optical light-curve shapes, colors, and spectra, yet have different ultraviolet (UV) continua as measured in Hubble Space Telescope spectra and measurably different peak luminosities. We attribute the difference in the UV continua to significantly different progenitor metallicities. This is the first robust detection of different metallicities for SN Ia progenitors. Theoretical reasoning suggests that differences in metallicity also lead to differences in luminosity. SNe Ia with higher progenitor metallicities have lower Ni-56 yields and lower luminosities for the same light-curve shape. SNe 2011by and 2011fe have different peak luminosities (Delta M-V approximate to 0.6 mag), which correspond to different Ni-56 yields: M-11fe(Ni-56)/M-11by(Ni-56) = 1.7(-0.5)(+ 0.7). From theoretical models that account for different neutron-to-proton ratios in progenitors, the differences in Ni-56 yields for SNe 2011by and 2011fe imply that their progenitor stars were above and below solar metallicity, respectively. Although we can distinguish progenitor metallicities in a qualitative way from UV data, the quantitative interpretation in terms of abundances is limited by the present state of theoretical models. C1 [Foley, Ryan J.; Kirshner, Robert P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Foley, RJ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. FU NSF [AST-1211196, PHY11-25915]; NASA; NASA through a grant from the Space Telescope Science Institute [12592]; Association of Universities for Research in Astronomy, Incorporated, under NASA [NAS5-26555] FX Supernova research at Harvard is supported by NSF grant AST-1211196. We thank the KITP for hospitality, where this research was supported in part by NSF grant PHY11-25915.; 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 NASA. Support for GO Program number 12592 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. NR 49 TC 28 Z9 28 U1 0 U2 1 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 MAY 20 PY 2013 VL 769 IS 1 AR UNSP L1 DI 10.1088/2041-8205/769/1/L1 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 151HN UT WOS:000319451400001 ER PT J AU Takei, D Drake, JJ Tsujimoto, M Ness, JU Osborne, JP Starrfield, S Kitamoto, S AF Takei, D. Drake, J. J. Tsujimoto, M. Ness, J. -U. Osborne, J. P. Starrfield, S. Kitamoto, S. TI X-RAY ECLIPSE DIAGNOSIS OF THE EVOLVING MASS LOSS IN THE RECURRENT NOVA U SCORPII 2010 SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE novae, cataclysmic variables; stars: individual (U Scorpii); X-rays: stars ID CLASSICAL NOVAE; OUTBURST; SUZAKU; MODEL; ERUPTION; WINDS; DISK AB We report the Suzaku detection of the earliest X-ray eclipse seen in the recurrent nova U Scorpii 2010. A target-of-opportunity observation 15 days after the outburst found a 27% +/- 5% dimming in the 0.2-1.0 keV energy band at the predicted center of an eclipse. In comparison with the X-ray eclipse depths seen at two later epochs by XMM-Newton, the source region shrank by about 10%-20% between days 15 and 35 after the outburst. The X-ray eclipses appear to be deeper than or similar to contemporaneous optical eclipses, suggesting the X-ray and optical source region extents are comparable on day 15. We raise the possibility of the energy dependency in the photon escape regions, and that this would be a result of the supersoft X-ray opacity being higher than the Thomson scattering opacity at the photosphere due to bound-free transitions in abundant metals that are not fully ionized. Assuming a spherically symmetric model, we constrain the mass-loss rate as a function of time. For a ratio of actual to Thomson opacity of 10-100 in supersoft X-rays, we find an ejecta mass of about 10(-7)-10(-6) M-circle dot. C1 [Takei, D.; Drake, J. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Tsujimoto, M.] Japan Aerosp Explorat Agcy, Inst Space & Astronaut Sci, Chuo Ku, Sagamihara, Kanagawa 2525210, Japan. [Ness, J. -U.] SRE OAX, European Space Agcy, XMM Newton Observ SOC, E-28691 Madrid, Spain. [Osborne, J. P.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. [Starrfield, S.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA. [Kitamoto, S.] Rikkyo Univ, Dept Phys, Toshima Ku, Tokyo 1718501, Japan. RP Takei, D (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM dtakei@head.cfa.harvard.edu RI XRAY, SUZAKU/A-1808-2009 FU JSPS; NASA [NAS8-03060]; UK Space Agency; NSF FX We thank Suzaku for undertaking our target-of-opportunity program, and B. E. Schaefer for organizing the U Scorpii 2010 collaboration. Optical data are from AAVSO and VSOLJ databases. We acknowledge support from the JSPS (D.T.), NASA contract NAS8-03060 to the CXC (J.J.D.), the UK Space Agency (J.O.), and NSF and NASA grants to ASU (S.S.). NR 36 TC 2 Z9 2 U1 0 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 MAY 20 PY 2013 VL 769 IS 1 AR L4 DI 10.1088/2041-8205/769/1/L4 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 151HN UT WOS:000319451400004 ER PT J AU Ngo, KM Turner, BL Muller-Landau, HC Davies, SJ Larjavaara, M Hassan, NFB Lum, S AF Kang Min Ngo Turner, Benjamin L. Muller-Landau, Helene C. Davies, Stuart J. Larjavaara, Markku Hassan, Nik Faizu bin Nik Lum, Shawn TI Carbon stocks in primary and secondary tropical forests in Singapore SO FOREST ECOLOGY AND MANAGEMENT LA English DT Article DE Aboveground and belowground biomass; Carbon pools; Coastal hill dipterocarp forest; Ecosystem carbon; Necromass; Tropical rain forest ID COARSE WOODY DEBRIS; HILL DIPTEROCARP FOREST; MINERAL NUTRIENT STATUS; ADINANDRA-BELUKAR; AMAZONIAN FORESTS; EASTERN AMAZONIA; SOIL CARBON; STORAGE; BIOMASS; LANDSCAPE AB Tropical forests contain large reserves of carbon that are vulnerable to perturbation linked to human activities, including deforestation and climate change. Accurate estimates of forest carbon are therefore required urgently to support efforts to conserve tropical forests. We quantified carbon stocks in primary and 60-year-old secondary forest plots located on infertile Ultisols in Bukit Timah Nature Reserve, one of the few remaining areas of forest in Singapore. We used tree census data for 24.2 ha of primary forest and 23 ha of secondary forest, together with allometric equations, to estimate aboveground and coarse root biomass. Coarse woody debris stocks were censused along 2.44 km and 2.12 km of transects in primary and secondary forest, respectively. Soil carbon and fine root carbon stocks were assessed from soil samples taken to 3 m depth in a 2-ha secondary forest plot and a 2-ha primary forest plot, combined with bulk density measured in a nearby soil profile pit. Total estimated carbon stock in the primary forest, which was located on the hilltop and upper slopes (80-115 m elevation), was 337 Mg C ha(-1), of which 50% was aboveground biomass, 33% in soil, 12% in coarse roots, 4.6% in coarse woody debris, and 0.8% in fine roots. In the secondary forest, located on lower slopes and valley (50-85 m elevation), the total carbon stock was 274 Mg C ha(-1) and the relative importance of aboveground biomass and soil were reversed, with 38% in aboveground biomass, 52% in soil, 6.9% in coarse roots, 1.5% in coarse woody debris, and 1.3% in fine roots. Including carbon in deep subsoil (i.e. to 3 m) increased soil carbon stocks by similar to 40% compared to 1 m depth. Overall, the 60-year-old secondary forest contained 60% as much biomass as the primary forest, while the primary forest had lower carbon stocks than other primary forests in the region. (c) 2013 Elsevier B.V. All rights reserved. C1 [Kang Min Ngo; Hassan, Nik Faizu bin Nik] Natl Inst Educ, Ctr Trop Forest Sci, Singapore 637616, Singapore. [Turner, Benjamin L.; Muller-Landau, Helene C.; Larjavaara, Markku] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. [Davies, Stuart J.] Smithsonian Inst, Dept Bot, SIGEO CTFS, Washington, DC 20013 USA. [Lum, Shawn] Nanyang Technol Univ, Natl Inst Educ, Nat Sci & Sci Educ Acad Grp, Singapore 637616, Singapore. RP Ngo, KM (reprint author), Natl Inst Educ, Ctr Trop Forest Sci, 1 Nanyang Walk, Singapore 637616, Singapore. EM ngokangmin@gmail.com RI Turner, Benjamin/E-5940-2011; OI Turner, Benjamin/0000-0002-6585-0722; Larjavaara, Markku/0000-0002-3484-889X; Ngo, Kang Min/0000-0001-8273-6158 FU HSBC Carbon Initiative; CTFS grant FX We thank Mohamad Fairoz bin Mohamed and other assistants for help in the field, Ryan Chisholm for help with data analysis, and Dayana Agudo for laboratory support. The research was funded by the HSBC Carbon Initiative and a CTFS grant to K.M.N. NR 55 TC 34 Z9 37 U1 8 U2 108 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0378-1127 J9 FOREST ECOL MANAG JI For. Ecol. Manage. PD MAY 15 PY 2013 VL 296 BP 81 EP 89 DI 10.1016/j.foreco.2013.02.004 PG 9 WC Forestry SC Forestry GA 134LE UT WOS:000318210900009 ER PT J AU Riley, SM AF Riley, Sheila M. TI On the Floor SO LIBRARY JOURNAL LA English DT Book Review C1 [Riley, Sheila M.] Smithsonian Inst Libs, Washington, DC USA. RP Riley, SM (reprint author), Smithsonian Inst Libs, Washington, DC USA. NR 1 TC 0 Z9 0 U1 0 U2 1 PU REED BUSINESS INFORMATION PI NEW YORK PA 360 PARK AVENUE SOUTH, NEW YORK, NY 10010 USA SN 0363-0277 J9 LIBR J JI Libr. J. PD MAY 15 PY 2013 VL 138 IS 9 BP 69 EP 69 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA 143TJ UT WOS:000318890800053 ER PT J AU Argenti, L Pazourek, R Feist, J Nagele, S Liertzer, M Persson, E Burgdorfer, J Lindroth, E AF Argenti, Luca Pazourek, Renate Feist, Johannes Nagele, Stefan Liertzer, Matthias Persson, Emil Burgdoerfer, Joachim Lindroth, Eva TI Photoionization of helium by attosecond pulses: Extraction of spectra from correlated wave functions SO PHYSICAL REVIEW A LA English DT Article ID DOUBLY EXCITED-STATES; DEPENDENT SCHRODINGER-EQUATION; DIFFERENTIAL CROSS-SECTIONS; CONFIGURATION-INTERACTION; ANGULAR-DISTRIBUTION; FINAL-STATE; MULTIELECTRON DYNAMICS; HE PHOTOIONIZATION; 2-ELECTRON ATOMS; 2 THRESHOLD AB We investigate the photoionization spectrum of helium by attosecond XUV pulses both in the spectral region of doubly excited resonances as well as above the double ionization threshold. In order to probe for convergence, we compare three techniques to extract photoelectron spectra from the wave packet resulting from the integration of the time-dependent Schrodinger equation in a finite-element discrete variable representation basis. These techniques are projection on products of hydrogenic bound and continuum states, projection onto multichannel scattering states computed in a B-spline close-coupling basis, and a technique based on exterior complex scaling implemented in the same basis used for the time propagation. These methods allow one to monitor the population of continuum states in wave packets created with ultrashort pulses in different regimes. Applications include photo cross sections and anisotropy parameters in the spectral region of doubly excited resonances, time-resolved photoexcitation of autoionizing resonances in an attosecond pump-probe setting, and the energy and angular distribution of correlated wave packets for two-photon double ionization. C1 [Argenti, Luca] Univ Autonoma Madrid, Dept Quim, E-28049 Madrid, Spain. [Pazourek, Renate; Nagele, Stefan; Liertzer, Matthias; Persson, Emil; Burgdoerfer, Joachim] Vienna Univ Technol, Inst Theoret Phys, A-1040 Vienna, Austria. [Feist, Johannes] Harvard Smithsonian Ctr Astrophys, ITAMP, Cambridge, MA 02138 USA. [Feist, Johannes] Univ Autonoma Madrid, Dept Fis Teor Mat Condensada, E-28049 Madrid, Spain. [Lindroth, Eva] Stockholm Univ, AlbaNova Univ Ctr, Dept Phys, SE-10691 Stockholm, Sweden. RP Argenti, L (reprint author), Univ Autonoma Madrid, Dept Quim, Modulo 13, E-28049 Madrid, Spain. EM luca.argenti@uam.es RI Feist, Johannes/J-7394-2012; Nagele, Stefan/E-6938-2011; Lindroth, Eva/I-2715-2013; OI Feist, Johannes/0000-0002-7972-0646; Nagele, Stefan/0000-0003-1213-0294; Lindroth, Eva/0000-0003-3444-1317; Argenti, Luca/0000-0003-1093-4379 FU Goran Gustafsson Foundation; Swedish Science Research Council (VR); European COST Action [CM0702]; FWF-Austria [P21141-N16, P23359-N16]; SFB ViCoM, SFB NextLite; National Science Foundation; NICS; TACC [TG-PHY090031]; European Research Council under the European Union [290853]; MICINN [FIS2010-15127]; NSF; European Research Council [290981 (PLASMONANOQUANTA)]; TU Vienna Doctoral Program Functional Matter; Vienna Science and Technology Fund (WWTF) [MA09-030] FX The authors thank Dr. Alicia Palacios for fruitful discussions. Special thanks are due to Professor Mariusz Zubek and Professor Alexander Menzel for providing us with original experimental data. This work was supported by the Goran Gustafsson Foundation, the Swedish Science Research Council (VR), the European COST Action CM0702, the FWF-Austria, Grants No. P21141-N16 and No. P23359-N16, the SFB ViCoM, SFB NextLite, and in part by the National Science Foundation through XSEDE resources provided by NICS and TACC under Grant No. TG-PHY090031. The computational results presented have also been achieved in part using the Vienna Scientific Cluster (VSC). L.A. acknowledges support from the European Research Council under the European Union's Seventh Framework Programme (FP7/2007-2013)/ERC Grant Agreement No. 290853, and the MICINN Project No. FIS2010-15127. J.F. acknowledges support from the NSF through a grant to ITAMP and by the European Research Council under Grant No. 290981 (PLASMONANOQUANTA). R.P. acknowledges support by the TU Vienna Doctoral Program Functional Matter. M.L. acknowledges funding by the Vienna Science and Technology Fund (WWTF) through Project No. MA09-030. NR 109 TC 29 Z9 29 U1 1 U2 61 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 2469-9926 EI 2469-9934 J9 PHYS REV A JI Phys. Rev. A PD MAY 13 PY 2013 VL 87 IS 5 AR 053405 DI 10.1103/PhysRevA.87.053405 PG 17 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA 145XU UT WOS:000319054000011 ER PT J AU Fernandez-Perea, M Pivovaroff, MJ Soufli, R Alameda, J Mirkarimi, P Descalle, MA Baker, SL McCarville, T Ziock, K Hornback, D Romaine, S Bruni, R Zhong, Z Honkimaki, V Ziegler, E Christensen, FE Jakobsen, AC AF Fernandez-Perea, Monica Pivovaroff, Mike J. Soufli, Regina Alameda, Jennifer Mirkarimi, Paul Descalle, Marie-Anne Baker, Sherry L. McCarville, Tom Ziock, Klaus Hornback, Donald Romaine, Suzanne Bruni, Ric Zhong, Zhong Honkimaeki, Veijo Ziegler, Eric Christensen, Finn E. Jakobsen, Anders C. TI Ultra-short-period WC/SiC multilayer coatings for x-ray applications SO NUCLEAR INSTRUMENTS & METHODS IN PHYSICS RESEARCH SECTION A-ACCELERATORS SPECTROMETERS DETECTORS AND ASSOCIATED EQUIPMENT LA English DT Article; Proceedings Paper CT 4th International Workshop on Metrology for X-ray Optics, Mirror Design and Fabrication CY JUL 04-06, 2012 CL Barcelona, SPAIN DE Multilayer coatings; Thin films; Tungsten carbide; Silicon carbide; Hard x-ray mirrors; Gamma-ray mirrors ID FILMS; ATTENUATION; TABULATION AB Multilayer coatings enhance x-ray mirror performance at incidence angles steeper than the critical angle, allowing for improved flux, design flexibility and facilitating alignment. In an attempt to extend the use of multilayer coatings to photon energies higher than previously achieved, we have developed multilayers with ultra-short periods between 1 and 2 nm based on the material system WC/SiC. This material system was selected because it possesses very sharp and stable interfaces. In this article, we show highlights from a series of experiments performed in order to characterize the stress, microstructure and morphology of the multilayer films, as well as their reflective performance at photon energies from 8 to 384 keV. Published by Elsevier B.V. C1 [Fernandez-Perea, Monica; Pivovaroff, Mike J.; Soufli, Regina; Alameda, Jennifer; Mirkarimi, Paul; Descalle, Marie-Anne; Baker, Sherry L.; McCarville, Tom] Lawrence Livermore Natl Lab, Livermore, CA 94550 USA. [Ziock, Klaus; Hornback, Donald] Oak Ridge Natl Lab, Oak Ridge, TN 37831 USA. [Romaine, Suzanne; Bruni, Ric] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Zhong, Zhong] Brookhaven Natl Lab, Natl Synchrotron Light Source, Upton, NY 11973 USA. [Honkimaeki, Veijo; Ziegler, Eric] European Synchrotron Radiat Facil, F-38043 Grenoble, France. [Christensen, Finn E.; Jakobsen, Anders C.] Danish Tech Univ DTU Space, DK-2800 Lyngby, Denmark. RP Fernandez-Perea, M (reprint author), Lawrence Livermore Natl Lab, 7000 East Ave, Livermore, CA 94550 USA. EM fernandezper1@llnl.gov RI Pivovaroff, Michael/M-7998-2014 OI Pivovaroff, Michael/0000-0001-6780-6816 FU U.S. Department of Energy by Lawrence Livermore National Laboratory [DE-AC52-07NA27344]; Oak Ridge National Laboratory [DE-AC05-00OR22725]; National Nuclear Security Administration's Office of Non-proliferation and Verification Research Development FX This work was performed under the auspices of theU.S. Department of Energy by Lawrence Livermore National Laboratory under Contract DE-AC52-07NA27344 and by Oak Ridge National Laboratory, managed by UT-Battelle, under contract DE-AC05-00OR22725. Funding for this research was provided by the National Nuclear Security Administration's Office of Non-proliferation and Verification Research & Development. We acknowledge the European Synchrotron Radiation Facility for provision of synchrotron radiation facilities and the MPI-Stuttgart for access to the High Energy Micro-Diffraction apparatus at ESRF. The contributions of Cynthia Gonsalves and Harry Kawayoshi (Evans Analytical Labs, Sunnyvale, California) in the sample preparation and acquisition of the TEM images is gratefully acknowledged. NR 16 TC 10 Z9 10 U1 3 U2 29 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0168-9002 EI 1872-9576 J9 NUCL INSTRUM METH A JI Nucl. Instrum. Methods Phys. Res. Sect. A-Accel. Spectrom. Dect. Assoc. Equip. PD MAY 11 PY 2013 VL 710 BP 114 EP 119 DI 10.1016/j.nima.2012.10.066 PG 6 WC Instruments & Instrumentation; Nuclear Science & Technology; Physics, Nuclear; Physics, Particles & Fields SC Instruments & Instrumentation; Nuclear Science & Technology; Physics GA 133HD UT WOS:000318128600022 ER PT J AU Wilke, RHT Johnson-Wilke, RL Cotroneo, V Davis, WN Reid, PB Schwartz, DA Trolier-McKinstry, S AF Wilke, Rudeger H. T. Johnson-Wilke, Raegan L. Cotroneo, Vincenzo Davis, William N. Reid, Paul B. Schwartz, Daniel A. Trolier-McKinstry, Susan TI Sputter deposition of PZT piezoelectric films on thin glass substrates for adjustable x-ray optics SO APPLIED OPTICS LA English DT Article ID TRANSMISSION ELECTRON-MICROSCOPY; ZIRCONATE-TITANATE FILMS; CRYSTALLIZATION BEHAVIOR; DEFORMABLE MIRROR; LEAD; GEL; MICROSTRUCTURE; EVOLUTION; KINETICS; GROWTH AB Piezoelectric PbZr0.52Ti0.48O3 (PZT) thin films deposited on thin glass substrates have been proposed for adjustable optics in future x-ray telescopes. The light weight of these x-ray optics enables large collecting areas, while the capability to correct mirror figure errors with the PZT thin film will allow much higher imaging resolution than possible with conventional lightweight optics. However, the low strain temperature and flexible nature of the thin glass complicate the use of chemical-solution deposition due to warping of the substrate at typical crystallization temperatures for the PZT. RF magnetron sputtering enabled preparation of PZT films with thicknesses up to 3 mu m on Schott D263 glass substrates with much less deformation. X-ray diffraction analysis indicated that the films crystallized with the perovskite phase and showed no indication of secondary phases. Films with 1 cm(2) electrodes exhibited relative permittivity values near 1100 and loss tangents below 0.05. In addition, the remanent polarization was 26 mu C/cm(2) with coercive fields of 33 kV/cm. The transverse piezoelectric coefficient was as high as -6.1 +/- 0.6 C/m(2). To assess influence functions for the x-ray optics application, the piezoelectrically induced deflection of individual cells was measured and compared with finite-element-analysis calculations. The good agreement between the results suggests that actuation of PZT thin films can control mirror figure errors to a precision of about 5 nm, allowing sub-arcsecond imaging. (c) 2013 Optical Society of America C1 [Wilke, Rudeger H. T.; Johnson-Wilke, Raegan L.; Trolier-McKinstry, Susan] Penn State Univ, Mat Res Inst, University Pk, PA 16802 USA. [Cotroneo, Vincenzo; Davis, William N.; Reid, Paul B.; Schwartz, Daniel A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Wilke, RHT (reprint author), Penn State Univ, Mat Res Inst, University Pk, PA 16802 USA. EM rhw11@psu.edu OI Trolier-McKinstry, Susan/0000-0002-7267-9281 FU Gordon and Betty Moore Foundation; NASA APRA [NNX09AE87G] FX This work was supported by grants from the Gordon and Betty Moore Foundation and from NASA APRA contract NNX09AE87G. The authors also gratefully acknowledge the usage of facilities in the W. M. Keck Smart Materials Integration Laboratory and the National Nanofabrication Infrastructure Network site at Penn State. The authors would like to thank Glen Fox for the numerous discussions and his invaluable advice in optimizing the deposition parameters for the PZT films. NR 48 TC 27 Z9 27 U1 3 U2 59 PU OPTICAL SOC AMER PI WASHINGTON PA 2010 MASSACHUSETTS AVE NW, WASHINGTON, DC 20036 USA SN 1559-128X J9 APPL OPTICS JI Appl. Optics PD MAY 10 PY 2013 VL 52 IS 14 BP 3412 EP 3419 DI 10.1364/AO.52.003412 PG 8 WC Optics SC Optics GA 145DP UT WOS:000318994500036 PM 23669858 ER PT J AU Palacios, A Feist, J Gonzalez-Castrillo, A Sanz-Vicario, JL Martin, F AF Palacios, Alicia Feist, Johannes Gonzalez-Castrillo, Alberto Luis Sanz-Vicario, Jose Martin, Fernando TI Autoionization of Molecular Hydrogen: Where do the Fano Lineshapes Go? SO CHEMPHYSCHEM LA English DT Article DE ab initio calculations; autoionization; electronelectron correlation; molecular hydrogen; photochemistry ID DOUBLY-EXCITED STATES; DISSOCIATIVE PHOTOIONIZATION; ATTOSECOND PULSES; LASER-PULSES; H-2; D-2; SPECTROSCOPY; IONIZATION; GENERATION; EXCITATION AB Atomic autoionization following photoabsorption is a typical example of quantum interferences governed by electronelectron correlation. Coherence between direct photoionization and autoionization paths results in Fano profiles, widely explored in atoms in the last 60 years. The advent of femto- and attosecond laser technology made time-resolved images of the delayed electron ejection in autoionization accessible, leading to the reemergence of such studies in atomic systems. The counterpart molecular phenomena show the richness, as well as the complexity, added by nuclear motion, which may proceed on similar time scales. However, Fano profiles are usually absent in measured molecular photoionization cross sections and an unequivocal parametrization of molecular autoionization signatures, similar to that introduced by Fano in atoms [U. Fano, Phys. Rev. 1961, 124, 1866] has not yet been achieved. In this work we introduce a simple semiclassical model that accounts for all the features observed in H2 photoionization and demonstrate that the interference structures observed in dissociative ionization spectra are almost exclusively due to the phase accumulated in the nuclear motion. Furthermore, we show that the temporal build-up of these structures in the energy-differential cross sections is also determined by nuclear motion. We validate our models by comparing with full-dimensional ab initio calculations solving the time-dependent Schrodinger equation. C1 [Palacios, Alicia; Gonzalez-Castrillo, Alberto; Martin, Fernando] Univ Autonoma Madrid, Dept Quim, E-28049 Madrid, Spain. [Feist, Johannes] Harvard Smithsonian Ctr Astrophys, ITAMP, Cambridge, MA 02138 USA. [Luis Sanz-Vicario, Jose] Univ Antioquia, Inst Fis, Grp Fis Atom & Mol, Medellin, Colombia. [Martin, Fernando] Inst Madrileno Estudios Avanzados Nanociencia, Madrid 28049, Spain. RP Palacios, A (reprint author), Univ Autonoma Madrid, Dept Quim, Modulo 13, E-28049 Madrid, Spain. EM alicia.palacios@uam.es RI Palacios, Alicia/J-6823-2012; Martin, Fernando/C-3972-2014; Feist, Johannes/J-7394-2012 OI Palacios, Alicia/0000-0001-6531-9926; Martin, Fernando/0000-0002-7529-925X; Feist, Johannes/0000-0002-7972-0646 FU European Research Council [XCHEM 290853]; European grant MC-ITN CORINF; European grant MC-RG ATTOTREND; European COST Action [CM0702]; MICINN [FIS2010-15127, ACI2008-0777, CSD 2007-00010]; ERA-Chemistry project [PIM2010EEC-00751]; Juan de la Cierva Contract grant from MICINN; NSF; Vicerrectoria de Investigacion at Universidad de Antioquia [E01538] FX We thank Mare Nostrum BSC and CCC-UAM for allocation of computer time. Work supported by the Advanced Grant of the European Research Council XCHEM 290853, the European grants MC-ITN CORINF and MC-RG ATTOTREND, the European COST Action CM0702, the MICINN project Nos. FIS2010-15127, ACI2008-0777 and CSD 2007-00010 (Spain), and the ERA-Chemistry project PIM2010EEC-00751. A. P. acknowledges a Juan de la Cierva Contract grant from MICINN. J.F. thanks the NSF for support through a grant to ITAMP. J.L.S.-V. acknowledges financial support from Vicerrectoria de Investigacion (contract number E01538 and Estrategia de Sostenibilidad 2013-2014) at Universidad de Antioquia. NR 56 TC 8 Z9 8 U1 2 U2 27 PU WILEY-V C H VERLAG GMBH PI WEINHEIM PA BOSCHSTRASSE 12, D-69469 WEINHEIM, GERMANY SN 1439-4235 J9 CHEMPHYSCHEM JI ChemPhysChem PD MAY 10 PY 2013 VL 14 IS 7 SI SI BP 1456 EP 1463 DI 10.1002/cphc.201200974 PG 8 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA 135IV UT WOS:000318282700015 PM 23494906 ER PT J AU Ward, DC AF Ward, David C. TI Wrong Sinclair SO TLS-THE TIMES LITERARY SUPPLEMENT LA English DT Letter C1 Smithsonian Inst, Natl Portrait Gallery, Washington, DC 20560 USA. RP Ward, DC (reprint author), Smithsonian Inst, Natl Portrait Gallery, Washington, DC 20560 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU TIMES SUPPLEMENTS LIMITED PI MARKET HARBOROUGH PA TOWER HOUSE, SOVEREIGN PARK, MARKET HARBOROUGH LE87 4JJ, ENGLAND SN 0307-661X J9 TLS-TIMES LIT SUPPL JI TLS-Times Lit. Suppl. PD MAY 10 PY 2013 IS 5745 BP 6 EP 6 PG 1 WC Humanities, Multidisciplinary SC Arts & Humanities - Other Topics GA 143TI UT WOS:000318890700010 ER PT J AU Chen, XP Arce, HG Zhang, QZ Bourke, TL Launhardt, R Jorgensen, JK Lee, CF Foster, JB Dunham, MM Pineda, JE Henning, T AF Chen, Xuepeng Arce, Hector G. Zhang, Qizhou Bourke, Tyler L. Launhardt, Ralf Jorgensen, Jes K. Lee, Chin-Fei Foster, Jonathan B. Dunham, Michael M. Pineda, Jaime E. Henning, Thomas TI SMA OBSERVATIONS OF CLASS 0 PROTOSTARS: A HIGH ANGULAR RESOLUTION SURVEY OF PROTOSTELLAR BINARY SYSTEMS SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries: general; dust, extinction; ISM: clouds; stars: formation; techniques: interferometric ID STAR-FORMING REGIONS; SPITZER C2D SURVEY; INITIAL MASS FUNCTION; MAIN-SEQUENCE STARS; NEARBY DENSE CORES; SUBMILLIMETER CONTINUUM OBSERVATIONS; QUADRUPOLAR MOLECULAR OUTFLOW; 1ST HYDROSTATIC CORE; BARNARD-1 DARK CLOUD; SOLAR-TYPE STARS AB We present high angular resolution 1.3 mm and 850 mu m dust continuum data obtained with the Submillimeter Array toward 33 Class 0 protostars in nearby clouds (distance < 500 pc), which represents so far the largest survey toward protostellar binary/multiple systems. The median angular resolution in the survey is 2 ''.5, while the median linear resolution is approximately 600 AU. Compact dust continuum emission is observed from all sources in the sample. Twenty-one sources in the sample show signatures of binarity/multiplicity, with separations ranging from 50 AU to 5000 AU. The numbers of singles, binaries, triples, and quadruples in the sample are 12, 14, 5, and 2, respectively. The derived multiplicity frequency (MF) and companion star fraction (CSF) for Class 0 protostars are 0.64 +/- 0.08 and 0.91 +/- 0.05, respectively, with no correction for completeness. The derived MF and CSF in this survey are approximately two times higher than the values found in the binary surveys toward Class I young stellar objects, and approximately three (for MF) and four (for CSF) times larger than the values found among main-sequence stars, with a similar range of separations. Furthermore, the observed fraction of high-order multiple systems to binary systems in Class 0 protostars (0.50 +/- 0.09) is also larger than the fractions found in Class I young stellar objects (0.31 +/- 0.07) and main-sequence stars (<= 0.2). These results suggest that binary properties evolve as protostars evolve, as predicted by numerical simulations. The distribution of separations for Class 0 protostellar binary/multiple systems shows a general trend in which CSF increases with decreasing companion separation. We find that 67% +/- 8% of the protobinary systems have circumstellar mass ratios below 0.5, implying that unequal-mass systems are preferred in the process of binary star formation. We suggest an empirical sequential fragmentation picture for binary star formation, based on this work and existing lower resolution single-dish observations. C1 [Chen, Xuepeng] Chinese Acad Sci, Purple Mt Observ, Nanjing 210008, Jiangsu, Peoples R China. [Chen, Xuepeng; Arce, Hector G.; Dunham, Michael M.] Yale Univ, Dept Astron, New Haven, CT 06520 USA. [Zhang, Qizhou; Bourke, Tyler L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Launhardt, Ralf; Henning, Thomas] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Jorgensen, Jes K.] Univ Copenhagen, Niels Bohr Inst, DK-2100 Copenhagen O, Denmark. [Jorgensen, Jes K.] Univ Copenhagen, Ctr Star & Planet Format, DK-2100 Copenhagen O, Denmark. [Lee, Chin-Fei] Acad Sinica, Inst Astron & Astrophys, Taipei 106, Taiwan. [Foster, Jonathan B.] Boston Univ, Inst Astrophys Res, Boston, MA 02215 USA. [Pineda, Jaime E.] ESO, D-85748 Garching, Germany. [Pineda, Jaime E.] Univ Manchester, Sch Phys & Astron, Jodrell Bank Ctr Astrophys, Manchester M13 9PL, Lancs, England. RP Chen, XP (reprint author), Chinese Acad Sci, Purple Mt Observ, 2 West Beijing Rd, Nanjing 210008, Jiangsu, Peoples R China. EM xpchen@pmo.ac.cn RI Pineda, Jaime/J-7405-2013; OI Pineda, Jaime/0000-0002-3972-1978; Zhang, Qizhou/0000-0003-2384-6589 FU Thousand Young Talents Program of China; NSF [AST-0845619]; European Community [229517] FX We thank the anonymous referee for providing many insightful suggestions and comments, which helped us improve this work greatly. We thank the SMA staff for technical support during the observations and their maintenance of the SMA archival data. X.C. acknowledges the support of the Thousand Young Talents Program of China. This material is based on work supported by NSF grant AST-0845619 to H.G.A. J.E.P. has received funding from the European Community's Seventh Framework Programme (/FP7/2007-2013/) under grant agreement No 229517. NR 191 TC 43 Z9 43 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 MAY 10 PY 2013 VL 768 IS 2 AR 110 DI 10.1088/0004-637X/768/2/110 PG 31 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 134QK UT WOS:000318228400013 ER PT J AU Demory, BO Torres, G Neves, V Rogers, L Gillon, M Horch, E Sullivan, P Bonfils, X Delfosse, X Forveille, T Lovis, C Mayor, M Santos, N Seager, S Smalley, B Udry, S AF Demory, Brice-Olivier Torres, Guillermo Neves, Vasco Rogers, Leslie Gillon, Michael Horch, Elliott Sullivan, Peter Bonfils, Xavier Delfosse, Xavier Forveille, Thierry Lovis, Christophe Mayor, Michel Santos, Nuno Seager, Sara Smalley, Barry Udry, Stephane TI SPITZER OBSERVATIONS OF GJ 3470 b: A VERY LOW-DENSITY NEPTUNE-SIZE PLANET ORBITING A METAL-RICH M DWARF SO ASTROPHYSICAL JOURNAL LA English DT Article DE planetary systems; stars: individual (GJ 3470); techniques: photometric; techniques: spectroscopic ID TRANSIT LIGHT-CURVE; LOW-MASS; SUPER-EARTHS; SOLID EXOPLANETS; BULK COMPOSITION; BINARY STARS; HOT NEPTUNE; METALLICITY; TELESCOPE; III. AB We present Spitzer/IRAC 4.5 mu m transit photometry of GJ 3470 b, a Neptune-size planet orbiting an M1.5 dwarf star with a 3.3 day period recently discovered in the course of the HARPS M-dwarf survey. We refine the stellar parameters by employing purely empirical mass-luminosity and surface brightness relations constrained by our updated value for the mean stellar density, and additional information from new near-infrared spectroscopic observations. We derive a stellar mass of M-star = 0.539(-0.043)(+0.047) M-circle dot and a radius of R-star = 0.568(-0.031)(+0.037) R-circle dot. We determine the host star of GJ 3470 b to bemetal-rich, with ametallicity of [Fe/H] = +0.20 +/- 0.10 and an effective temperature of T-eff = 3600 +/- 100 K. The revised stellar parameters yield a planetary radius R-p = 4.83(-0.21)(+0.22) R-circle plus that is 13% larger than the value previously reported in the literature. We find a planetary mass M-p = 13.9(-1.4)(+1.5) M-circle plus that translates to a very low planetary density rho(p) = 0.72(-0.12)(+0.13) g cm(-3), which is 33% smaller than the original value. With a mean density half of that of GJ 436 b, GJ 3470 b is an example of a very low-density low-mass planet, similar to Kepler-11 d, Kepler-11 e, and Kepler-18 c, but orbiting a much brighter nearby star that is more conducive to follow-up studies. C1 [Demory, Brice-Olivier; Seager, Sara] MIT, Dept Earth Atmospher & Planetary Sci, Cambridge, MA 02139 USA. [Torres, Guillermo] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Neves, Vasco; Santos, Nuno] Univ Porto, Ctr Astrofis, P-4150762 Oporto, Portugal. [Neves, Vasco; Santos, Nuno] Univ Porto, Fac Ciencias, Dept Fis & Astron, P-4169007 Oporto, Portugal. [Neves, Vasco; Bonfils, Xavier; Delfosse, Xavier; Forveille, Thierry] UJF Grenoble 1, CNRS INSU, IPAG UMR 5274, F-38041 Grenoble, France. [Rogers, Leslie] CALTECH, Dept Astrophys, Pasadena, CA 91125 USA. [Gillon, Michael] Univ Liege, Inst Astrophys & Geophys, Liege 1, Belgium. [Horch, Elliott] So Connecticut State Univ, Dept Phys, New Haven, CT 06515 USA. [Sullivan, Peter; Seager, Sara] MIT, Dept Phys, Cambridge, MA 02138 USA. [Sullivan, Peter; Seager, Sara] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02138 USA. [Lovis, Christophe; Mayor, Michel; Udry, Stephane] Univ Geneva, Observ Geneve, CH-1290 Versoix, Switzerland. [Smalley, Barry] Keele Univ, Astrophys Grp, Keele ST5 5BG, Staffs, England. RP Demory, BO (reprint author), MIT, Dept Earth Atmospher & Planetary Sci, 77 Massachusetts Ave, Cambridge, MA 02139 USA. EM demory@mit.edu RI Santos, Nuno/E-9957-2011; OI Santos, Nuno/0000-0003-4422-2919; Bonfils, Xavier/0000-0001-9003-8894; Demory, Brice-Olivier/0000-0002-9355-5165 FU NASA; NASA through Hubble Fellowship grant [HF-51313.01-A, NAS 5-26555]; JPL/Caltech; Space Telescope Science Institute; European Research Council/European Community under the FP7 [239953]; Fundacao para a Ciencia e a Tecnologia (FCT) [PTDC/CTE-AST/098528/2008, PTDC/CTE-AST/120251/2010]; "Programme National de Planetologie" (PNP) of CNRS/INSU, France; NSF grant [AST-1007992]; FCT [SFRH/BD/60688/2009] FX We thank Zach Berta and Elisabeth Newton for helpful discussions regarding near-IR M-dwarf spectral characterization. We are grateful to Rob Simcoe, Paul Schechter, Elisabeth Adams, and David Ciardi for their help in obtaining the ground-based observations presented in this paper. We thank the anonymous referee for a report that improved the paper. We thank the Spitzer Science Center staff, and especially Nancy Silbermann, for the efficient scheduling of our observations. We also wish to thank the staff of the Magellan Telescopes and Las Campanas Observatory for their assistance in obtaining the FIRE observations. 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. The WIYN Observatory is a joint facility of the University of Wisconsin-Madison, Indiana University, Yale University, and the National Optical Astronomy Observatory. Support for LAR was provided by NASA through Hubble Fellowship grant HF-51313.01-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 by the European Research Council/European Community under the FP7 through Starting Grant agreement number 239953 and by Fundacao para a Ciencia e a Tecnologia (FCT) in the form of grants PTDC/CTE-AST/098528/2008 and PTDC/CTE-AST/120251/2010. The financial support from the "Programme National de Planetologie" (PNP) of CNRS/INSU, France, is gratefully acknowledged. G.T. acknowledges partial support for this work through NSF grant AST-1007992. V.N. also acknowledges the support from the FCT in the form of the fellowship SFRH/BD/60688/2009. M.G. is Research Associate at the Belgian Fonds National de la Recherche Scientifique (FNRS). NR 58 TC 17 Z9 17 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 MAY 10 PY 2013 VL 768 IS 2 AR 154 DI 10.1088/0004-637X/768/2/154 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 134QK UT WOS:000318228400057 ER PT J AU Garcia, J Dauser, T Reynolds, CS Kallman, TR McClintock, JE Wilms, J Eikmann, W AF Garcia, J. Dauser, T. Reynolds, C. S. Kallman, T. R. McClintock, J. E. Wilms, J. Eikmann, W. TI X-RAY REFLECTED SPECTRA FROM ACCRETION DISK MODELS. III. A COMPLETE GRID OF IONIZED REFLECTION CALCULATIONS SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; atomic processes; black hole physics; line: formation; radiative transfer; X-rays: general ID ACTIVE GALACTIC NUCLEI; K-SHELL PHOTOIONIZATION; RESONANT AUGER DESTRUCTION; PLANE-PARALLEL GEOMETRY; FINITE-DENSITY PLASMAS; BLACK-HOLE SYSTEMS; ATOMIC DECAY DATA; COLD MATTER; IRON LINES; DIELECTRONIC RECOMBINATION AB We present a new and complete library of synthetic spectra for modeling the component of emission that is reflected from an illuminated accretion disk. The spectra were computed using an updated version of our code XILLVER that incorporates new routines and a richer atomic database. We offer in the form of a table model an extensive grid of reflection models that cover a wide range of parameters. Each individual model is characterized by the photon index G of the illuminating radiation, the ionization parameter xi at the surface of the disk (i.e., the ratio of the X-ray flux to the gas density), and the iron abundance A(Fe) relative to the solar value. The ranges of the parameters covered are 1.2 <= Gamma <= 3.4, 1 <= xi <= 10(4), and 0.5 <= A(Fe) <= 10. These ranges capture the physical conditions typically inferred from observations of active galactic nuclei, and also stellar-mass black holes in the hard state. This library is intended for use when the thermal disk flux is faint compared to the incident power-law flux. The models are expected to provide an accurate description of the Fe K emission line, which is the crucial spectral feature used to measure black hole spin. A total of 720 reflection spectra are provided in a single FITS file (http://hea-www.cfa.harvard.edu/similar to javier/xillver/) suitable for the analysis of X-ray observations via the atable model in XSPEC. Detailed comparisons with previous reflection models illustrate the improvements incorporated in this version of XILLVER. C1 [Garcia, J.; McClintock, J. E.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Garcia, J.; Reynolds, C. S.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Dauser, T.; Wilms, J.; Eikmann, W.] Dr Karl Remeis Observ, D-96049 Bamberg, Germany. [Dauser, T.; Wilms, J.; Eikmann, W.] Erlangen Ctr Astroparticle Phys, D-96049 Bamberg, Germany. [Reynolds, C. S.] Univ Maryland, Joint Space Sci Inst, College Pk, MD 20742 USA. [Kallman, T. R.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Garcia, J (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM javier@head.cfa.harvard.edu; thomas.dauser@sternwarte.uni-erlangen.de; chris@astro.umd.edu; timothy.r.kallman@nasa.gov; jem@cfa.harvard.edu; joern.wilms@sternwarte.uni-erlangen.de; wiebke.eikmann@sternwarte.uni-erlangen.de RI Wilms, Joern/C-8116-2013 OI Wilms, Joern/0000-0003-2065-5410 NR 96 TC 82 Z9 82 U1 1 U2 7 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAY 10 PY 2013 VL 768 IS 2 AR 146 DI 10.1088/0004-637X/768/2/146 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 134QK UT WOS:000318228400049 ER PT J AU Gupta, A Mathur, S Krongold, Y Nicastro, F AF Gupta, A. Mathur, S. Krongold, Y. Nicastro, F. TI A TWO-PHASE LOW-VELOCITY OUTFLOW IN THE SEYFERT 1 GALAXY Ark 564 SO ASTROPHYSICAL JOURNAL LA English DT Article DE black hole physics; galaxies: Seyfert; quasars: absorption lines; X-rays: galaxies ID ACTIVE GALACTIC NUCLEI; SUPERSOLAR METAL ABUNDANCES; XMM-NEWTON OBSERVATION; X-RAY; EMISSION-LINE; IONIZED-GAS; INTERSTELLAR-MEDIUM; ABSORBING OUTFLOW; SPECTRAL-ANALYSIS; QUASAR FEEDBACK AB The Seyfert 1 galaxy Ark 564 was observed with Chandra high-energy transmission gratings for 250 ks. We present the high-resolution X-ray spectrum that shows several associated absorption lines. The photoionization model requires two warm absorbers (WAs) with two different ionization states (log U = 0.39 +/- 0.03 and log U = -0.99 +/- 0.13), both with moderate outflow velocities (similar to 100 km s(-1)) and relatively low line of sight column densities (log N-H = 20.94 and 20.11 cm(-2)). The high-ionization phase produces absorption lines of O VII, O VIII, Ne IX, Ne X, Mg XI, Fe XVII, and Fe XVIII, while the low-ionization phase produces lines at lower energies (O VI and O VII). The pressure-temperature equilibrium curve for the Ark 564 absorber does not have the typical "S" shape, even if the metallicity is super-solar; as a result, the two WA phases do not appear to be in pressure balance. This suggests that the continuum incident on the absorbing gas is perhaps different from the observed continuum. We also estimated the mass outflow rate and the associated kinetic energy and find it to be at most 0.009% of the bolometric luminosity of Ark 564. Thus, it is highly unlikely that these outflows provide significant feedback required by the galaxy formation models. C1 [Gupta, A.; Mathur, S.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. [Krongold, Y.] Univ Nacl Autonoma Mexico, Inst Astron, Mexico City 04510, DF, Mexico. [Nicastro, F.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Nicastro, F.] Osservatorio Astron Roma INAF, I-00040 Monte Porzio Catone, RM, Italy. [Mathur, S.] Ohio State Univ, Ctr Cosmol & Astroparticle Phys, Columbus, OH 43210 USA. RP Gupta, A (reprint author), Ohio State Univ, Dept Astron, 174 W 18th Ave, Columbus, OH 43210 USA. EM agupta@astronomy.ohio-state.edu OI Nicastro, Fabrizio/0000-0002-6896-1364 FU National Aeronautics and Space Administration, Chandra X-ray Observatory Center [TM9-0010X]; National Aeronautics Space Administration [NAS8-03060]; CONACyT [168519]; UNAM-DGAPA PAPIIT [IN103712] FX Support for this work was provided by the National Aeronautics and Space Administration through Chandra Award No. TM9-0010X 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 NAS8-03060. Y.K. acknowledges support from CONACyT 168519 grant and UNAM-DGAPA PAPIIT IN103712 grant. The authors thank the anonymous reviewer for valuable comments and suggestions to improve the quality of the paper. NR 59 TC 9 Z9 9 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAY 10 PY 2013 VL 768 IS 2 AR 141 DI 10.1088/0004-637X/768/2/141 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 134QK UT WOS:000318228400044 ER PT J AU Jones, DO Rodney, SA Riess, AG Mobasher, B Dahlen, T McCully, C Frederiksen, TF Casertano, S Hjorth, J Keeton, CR Koekemoer, A Strolger, LG Wiklind, TG Challis, P Graur, O Hayden, B Patel, B Weiner, BJ Filippenko, AV Garnavich, P Jha, SW Kirshner, RP Ferguson, HC Grogin, NA Kocevski, D AF Jones, David O. Rodney, Steven A. Riess, Adam G. Mobasher, Bahram Dahlen, Tomas McCully, Curtis Frederiksen, Teddy F. Casertano, Stefano Hjorth, Jens Keeton, Charles R. Koekemoer, Anton Strolger, Louis-Gregory Wiklind, Tommy G. Challis, Peter Graur, Or Hayden, Brian Patel, Brandon Weiner, Benjamin J. Filippenko, Alexei V. Garnavich, Peter Jha, Saurabh W. Kirshner, Robert P. Ferguson, Henry C. Grogin, Norman A. Kocevski, Dale TI THE DISCOVERY OF THE MOST DISTANT KNOWN TYPE Ia SUPERNOVA AT REDSHIFT 1.914 SO ASTROPHYSICAL JOURNAL LA English DT Article DE supernovae: general ID HUBBLE-SPACE-TELESCOPE; EXTRAGALACTIC LEGACY SURVEY; INITIAL MASS FUNCTION; DARK-ENERGY; PHOTOMETRIC CLASSIFICATION; LUMINOSITY FUNCTIONS; ULTRAVIOLET-SPECTRA; SNE-IA; CONSTRAINTS; GALAXY AB We present the discovery of a Type Ia supernova (SN) at redshift z = 1.914 from the CANDELS multi-cycle treasury program on the Hubble Space Telescope (HST). This SN was discovered in the infrared using the Wide-Field Camera 3, and it is the highest-redshift Type Ia SN yet observed. We classify this object as a SN Ia by comparing its light curve and spectrum with those of a large sample of Type Ia and core-collapse SNe. Its apparent magnitude is consistent with that expected from the Lambda CDM concordance cosmology. We discuss the use of spectral evidence for classification of z > 1.5 SNe Ia using HST grism simulations, finding that spectral data alone can frequently rule out SNe II, but distinguishing between SNe Ia and SNe Ib/c can require prohibitively long exposures. In such cases, a quantitative analysis of the light curve may be necessary for classification. Our photometric and spectroscopic classification methods can aid the determination of SN rates and cosmological parameters from the full high-redshift CANDELS SN sample. C1 [Jones, David O.; Rodney, Steven A.; Riess, Adam G.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Riess, Adam G.; Dahlen, Tomas; Casertano, Stefano; Koekemoer, Anton; Ferguson, Henry C.; Grogin, Norman A.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Mobasher, Bahram] Univ Calif Riverside, Dept Phys & Astron, Riverside, CA 92521 USA. [McCully, Curtis; Keeton, Charles R.; Patel, Brandon; Jha, Saurabh W.] Rutgers State Univ, Dept Phys & Astron, Piscataway, NJ 08854 USA. [Frederiksen, Teddy F.; Hjorth, Jens] Univ Copenhagen, Niels Bohr Inst, Dark Cosmol Ctr, DK-2100 Copenhagen, Denmark. [Strolger, Louis-Gregory] Western Kentucky Univ, Dept Phys, Bowling Green, KY 42101 USA. [Wiklind, Tommy G.] ESO, Joint ALMA Observ, Santiago, Chile. [Challis, Peter; Kirshner, Robert P.; Kocevski, Dale] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Graur, Or] Tel Aviv Univ, Sch Phys & Astron, IL-69978 Tel Aviv, Israel. [Graur, Or] Amer Museum Nat Hist, Dept Astrophys, New York, NY 10024 USA. [Hayden, Brian; Garnavich, Peter] Univ Notre Dame, Dept Phys, Notre Dame, IN 46556 USA. [Weiner, Benjamin J.] Univ Arizona, Dept Astron, Tucson, AZ 85721 USA. [Filippenko, Alexei V.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. RP Jones, DO (reprint author), Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. RI Hjorth, Jens/M-5787-2014; OI Hjorth, Jens/0000-0002-4571-2306; Graur, Or/0000-0002-4391-6137; Weiner, Benjamin/0000-0001-6065-7483; Koekemoer, Anton/0000-0002-6610-2048 FU NASA from the Space Telescope Science Institute [HST-GO-12060, HST-GO-12099]; NASA [NAS 5-26555]; NASA through Hubble Fellowship [HST-HF-51312]; National Science Foundation (NSF) [AST-1211916]; TABASGO Foundation; Christopher R. Redlich Fund; DNRF; NSF [PHY11-25915]; Israeli Science Foundation FX We thank the anonymous referee for many helpful comments, and Masao Sako and Rick Kessler for their invaluable assistance with SNANA and PSNID. In addition, our aXe and aXeSim analysis was made possible by help from Jeremy Walsh, Harold Kuntschner, Martin Kummel, Howard Bushouse, and Nor Pirzkal. We also thank Daniel Scolnic for many useful discussions. Financial support for this work was provided by NASA through grants HST-GO-12060 and HST-GO-12099 from the Space Telescope Science Institute, which is operated by Associated Universities for Research in Astronomy, Inc., under NASA contract NAS 5-26555. Additional support for S.R. was provided by NASA through Hubble Fellowship grant HST-HF-51312. A.V.F. is also grateful for the support of National Science Foundation (NSF) grant AST-1211916, the TABASGO Foundation, and the Christopher R. Redlich Fund. The Dark Cosmology Centre is funded by the DNRF. R.P.K. was supported in part by NSF grant PHY11-25915 to the Kavli Institute for Theoretical Physics at the University of California, Santa Barbara. O.G. acknowledges support by a grant from the Israeli Science Foundation. NR 53 TC 30 Z9 30 U1 2 U2 14 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAY 10 PY 2013 VL 768 IS 2 AR 166 DI 10.1088/0004-637X/768/2/166 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 134QK UT WOS:000318228400069 ER PT J AU McCauley, PI Saar, SH Raymond, JC Ko, YK Saint-Hilaire, P AF McCauley, Patrick I. Saar, Steven H. Raymond, John C. Ko, Yuan-Kuen Saint-Hilaire, Pascal TI EXTREME-ULTRAVIOLET AND X-RAY OBSERVATIONS OF COMET LOVEJOY (C/2011 W3) IN THE LOWER CORONA SO ASTROPHYSICAL JOURNAL LA English DT Article DE comets: general; comets: individual (C/2011 W3); Sun: corona ID BRIGHT SUNGRAZING COMETS; ATOMIC DATABASE; ORBITAL EVOLUTION; UVCS OBSERVATION; EMISSION-LINES; KREUTZ SYSTEM; SOLAR-WIND; FRAGMENTATION; MISSION; CHIANTI AB We present an analysis of extreme-ultraviolet and soft X-ray emission detected toward Comet Lovejoy (C/2011 W3) during its post-perihelion traverse of the solar corona on 2011 December 16. Observations were recorded by the Atmospheric Imaging Assembly (AIA) aboard the Solar Dynamics Observatory and the X-Ray Telescope (XRT) aboard Hinode. A single set of contemporaneous images is explored in detail, along with prefatory consideration for time evolution using only the 171 angstrom data. For each of the eight passbands, we characterize the emission and derive outgassing rates where applicable. As material sublimates from the nucleus and is immersed in coronal plasma, it rapidly ionizes through charge states seldom seen in this environment. The AIA data show four stages of oxygen ionization (O III-O VI) along with C IV, while XRT likely captured emission from O VII, a line typical of the corona. With a nucleus of at least several hundred meters upon approach to a perihelion that brought the comet to within 0.2 R-circle dot of the photosphere, Lovejoy was the most significant sungrazer in recent history. Correspondingly high outgassing rates on the order of 10(32.5) oxygen atoms per second are estimated. Assuming that the neutral oxygen comes from water, this translates to a mass-loss rate of similar to 9.5 x 10(9) g s(-1), and based only on the 171 angstrom observations, we find a total mass loss of similar to 10(13) g over the AIA egress. Additional and supporting analyses include a differential emission measure to characterize the coronal environment, consideration for the opening angle, and a comparison of the emission's leading edge with the expected position of the nucleus. C1 [McCauley, Patrick I.; Saar, Steven H.; Raymond, John C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Ko, Yuan-Kuen] USN, Res Lab, Div Space Sci, Washington, DC 20375 USA. [Saint-Hilaire, Pascal] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. RP McCauley, PI (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI McCauley, Patrick/P-7747-2015 OI McCauley, Patrick/0000-0002-1450-7350 FU Smithsonian Astrophysical Observatory (SAO) via Hinode/XRT [NNM07AB07C]; SDO/AIA [SP02H1701R] FX Support for this work was provided by the Smithsonian Astrophysical Observatory (SAO) via funding from Hinode/XRT through grant NNM07AB07C and SDO/AIA through grant SP02H1701R. 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). SDO is a NASA satellite, and the AIA instrument team is led by Lockheed Martin, with SAO as the major subcontractor. We gratefully acknowledge Ted Tarbell for his work in aligning the SOT and SDO data, which was important for Figure 6. P.I.M. thanks the SSXG members at SAO for being characteristically helpful and welcoming. NR 39 TC 14 Z9 14 U1 0 U2 10 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAY 10 PY 2013 VL 768 IS 2 AR 161 DI 10.1088/0004-637X/768/2/161 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 134QK UT WOS:000318228400064 ER PT J AU McGreer, ID Jiang, LH Fan, XH Richards, GT Strauss, MA Ross, NP White, M Shen, Y Schneider, DP Myers, AD Brandt, WN DeGraf, C Glikman, E Ge, J Streblyanska, A AF McGreer, Ian D. Jiang, Linhua Fan, Xiaohui Richards, Gordon T. Strauss, Michael A. Ross, Nicholas P. White, Martin Shen, Yue Schneider, Donald P. Myers, Adam D. Brandt, W. Niel DeGraf, Colin Glikman, Eilat Ge, Jian Streblyanska, Alina TI THE z=5 QUASAR LUMINOSITY FUNCTION FROM SDSS STRIPE 82 SO ASTROPHYSICAL JOURNAL LA English DT Article DE quasars: general ID DIGITAL-SKY-SURVEY; HIGH-REDSHIFT QUASARS; SUPERMASSIVE BLACK-HOLES; OSCILLATION SPECTROSCOPIC SURVEY; SIMILAR-TO 4; SURVEY PHOTOMETRIC SYSTEM; SURVEY COMMISSIONING DATA; ACTIVE GALACTIC NUCLEI; BROAD ABSORPTION-LINE; EARLY DATA RELEASE AB We present ameasurement of the Type I quasar luminosity function at z = 5 using a large sample of spectroscopically confirmed quasars selected from optical imaging data. We measure the bright end (M-1450 < -26) with Sloan Digital Sky Survey (SDSS) data covering similar to 6000 deg(2), then extend to lower luminosities (M-1450 < -24) with newly discovered, faint z similar to 5 quasars selected from 235 deg(2) of deep, coadded imaging in the SDSS Stripe 82 region (the celestial equator in the Southern Galactic Cap). The faint sample includes 14 quasars with spectra obtained as ancillary science targets in the SDSS-III Baryon Oscillation Spectroscopic Survey, and 59 quasars observed at the MMT and Magellan telescopes. We construct a well-defined sample of 4.7 < z < 5.1 quasars that is highly complete, with 73 spectroscopic identifications out of 92 candidates. Our color selection method is also highly efficient: of the 73 spectra obtained, 71 are high-redshift quasars. These observations reach below the break in the luminosity function (M*(1450) approximate to -27). The bright-end slope is steep (beta less than or similar to -4), with a constraint of beta < -3.1 at 95% confidence. The break luminosity appears to evolve strongly at high redshift, providing an explanation for the flattening of the bright-end slope reported previously. We find a factor of similar to 2 greater decrease in the number density of luminous quasars (M-1450 < -26) from z = 5 to z = 6 than from z = 4 to z = 5, suggesting a more rapid decline in quasar activity at high redshift than found in previous surveys. Our model for the quasar luminosity function predicts that quasars generate similar to 30% of the ionizing photons required to keep hydrogen in the universe ionized at z = 5. C1 [McGreer, Ian D.; Fan, Xiaohui] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Jiang, Linhua] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA. [Richards, Gordon T.] Drexel Univ, Dept Phys, Philadelphia, PA 19104 USA. [Strauss, Michael A.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. [Ross, Nicholas P.; White, Martin] Lawrence Berkeley Natl Lab, Berkeley, CA 92420 USA. [White, Martin] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. [Shen, Yue] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Schneider, Donald P.; Brandt, W. Niel] Penn State Univ, Dept Astron & Astrophys, Davey Lab 525, University Pk, PA 16802 USA. [Schneider, Donald P.] Penn State Univ, Inst Gravitat & Cosmos, University Pk, PA 16802 USA. [Myers, Adam D.] Univ Wyoming, Dept Phys & Astron, Laramie, WY 82071 USA. [DeGraf, Colin] Carnegie Mellon Univ, McWilliams Ctr Cosmol, Pittsburgh, PA 15213 USA. [Glikman, Eilat] Yale Univ, Dept Phys, New Haven, CT 06520 USA. [Glikman, Eilat] Yale Univ, Yale Ctr Astron & Astrophys, New Haven, CT 06520 USA. [Ge, Jian] Univ Florida, Bryant Space Sci Ctr 211, Dept Astron, Gainesville, FL 32611 USA. [Streblyanska, Alina] IAC, E-38200 Tenerife, Spain. [Streblyanska, Alina] ULL, Dept Astrofis, E-38206 Tenerife, Spain. RP McGreer, ID (reprint author), Univ Arizona, Steward Observ, 933 North Cherry Ave, Tucson, AZ 85721 USA. EM imcgreer@as.arizona.edu RI White, Martin/I-3880-2015; Brandt, William/N-2844-2015; Jiang, Linhua/H-5485-2016 OI White, Martin/0000-0001-9912-5070; Brandt, William/0000-0002-0167-2453; Jiang, Linhua/0000-0003-4176-6486 FU David and Lucile Packard Fellowship; NSF [AST 08-06861, AST 11-07682]; NASA [HST-HF-51291.01]; STSci; Alfred P. Sloan Foundation; National Science Foundation; U.S. Department of Energy Office of Science; University of Arizona; Brookhaven National Laboratory; University of Cambridge; Carnegie Mellon University; University of Florida; Harvard University; Instituto de Astrofisica de Canarias; Johns Hopkins University; Lawrence Berkeley National Laboratory; Max Planck Institute for Astrophysics; Max Planck Institute for Extraterrestrial Physics; New Mexico State University; New York University; Ohio State University; Pennsylvania State University; University of Portsmouth; Princeton University; University of Tokyo; University of Utah; Vanderbilt University; University of Virginia; University of Washington; Yale University FX The authors thank the staffs of the MMT and Magellan telescopes, particularly the recently retired John McAfee, for enabling many of the observations presented here. I.D.M., L.J., and X.F. acknowledge support from a David and Lucile Packard Fellowship, and NSF Grants AST 08-06861 and AST 11-07682. L.J. acknowledges support from NASA through Hubble Fellowship grant HST-HF-51291.01 awarded by the STSci.; Funding for SDSS-III has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, and the U.S. Department of Energy Office of Science. The SDSS-III Web site is http://www.sdss3.org/.; SDSS-III is managed by the Astrophysical Research Consortium for the Participating Institutions of the SDSS-III Collaboration including the University of Arizona, the Brazilian Participation Group, Brookhaven National Laboratory, University of Cambridge, Carnegie Mellon University, University of Florida, the French Participation Group, the German Participation Group, Harvard University, the Instituto de Astrofisica de Canarias, the Michigan State/Notre Dame/JINA Participation Group, Johns Hopkins University, Lawrence Berkeley National Laboratory, Max Planck Institute for Astrophysics, Max Planck Institute for Extraterrestrial Physics, New Mexico State University, New York University, Ohio State University, Pennsylvania State University, University of Portsmouth, Princeton University, the Spanish Participation Group, University of Tokyo, University of Utah, Vanderbilt University, University of Virginia, University of Washington, and Yale University. NR 146 TC 61 Z9 61 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAY 10 PY 2013 VL 768 IS 2 AR 105 DI 10.1088/0004-637X/768/2/105 PG 25 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 134QK UT WOS:000318228400008 ER PT J AU Schwamb, ME Orosz, JA Carter, JA Welsh, WF Fischer, DA Torres, G Howard, AW Crepp, JR Keel, WC Lintott, CJ Kaib, NA Terrell, D Gagliano, R Jek, KJ Parrish, M Smith, AM Lynn, S Simpson, RJ Giguere, MJ Schawinski, K AF Schwamb, Megan E. Orosz, Jerome A. Carter, Joshua A. Welsh, William F. Fischer, Debra A. Torres, Guillermo Howard, Andrew W. Crepp, Justin R. Keel, William C. Lintott, Chris J. Kaib, Nathan A. Terrell, Dirk Gagliano, Robert Jek, Kian J. Parrish, Michael Smith, Arfon M. Lynn, Stuart Simpson, Robert J. Giguere, Matthew J. Schawinski, Kevin TI PLANET HUNTERS: A TRANSITING CIRCUMBINARY PLANET IN A QUADRUPLE STAR SYSTEM SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries: eclipsing; planets and satellites: detection; planets and satellites: general; stars: individual (KIC 4862625) ID WIDE BINARY STARS; ECLIPSING BINARY; CM DRACONIS; ABSOLUTE DIMENSIONS; EVOLUTIONARY MODELS; ACCURATE MASSES; STELLAR ORBITS; MAIN-SEQUENCE; DATA RELEASE; HW VIRGINIS AB We report the discovery and confirmation of a transiting circumbinary planet (PH1b) around KIC 4862625, an eclipsing binary in the Kepler field. The planet was discovered by volunteers searching the first six Quarters of publicly available Kepler data as part of the Planet Hunters citizen science project. Transits of the planet across the larger and brighter of the eclipsing stars are detectable by visual inspection every similar to 137 days, with seven transits identified in Quarters 1-11. The physical and orbital parameters of both the host stars and planet were obtained via a photometric-dynamical model, simultaneously fitting both the measured radial velocities and the Kepler light curve of KIC 4862625. The 6.18 +/- 0.17 R-circle plus planet orbits outside the 20 day orbit of an eclipsing binary consisting of an F dwarf (1.734 +/- 0.044 R-circle dot, 1.528 +/- 0.087 M-circle dot) and M dwarf (0.378 +/- 0.023 R-circle dot, 0.408 +/- 0.024 M-circle dot). For the planet, we find an upper mass limit of 169 M-circle plus (0.531 Jupiter masses) at the 99.7% confidence level. With a radius and mass less than that of Jupiter, PH1b is well within the planetary regime. Outside the planet's orbit, at similar to 1000 AU, a previously unknown visual binary has been identified that is likely bound to the planetary system, making this the first known case of a quadruple star system with a transiting planet. C1 [Schwamb, Megan E.; Schawinski, Kevin] Yale Univ, Yale Ctr Astron & Astrophys, New Haven, CT 06520 USA. [Schwamb, Megan E.; Schawinski, Kevin] Yale Univ, Dept Phys, New Haven, CT 06511 USA. [Orosz, Jerome A.; Welsh, William F.] San Diego State Univ, Dept Astron, San Diego, CA 92182 USA. [Carter, Joshua A.; Torres, Guillermo] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Fischer, Debra A.; Giguere, Matthew J.] Yale Univ, Dept Astron, New Haven, CT 06511 USA. [Howard, Andrew W.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Crepp, Justin R.] CALTECH, Dept Astron, Pasadena, CA 91125 USA. [Crepp, Justin R.] Univ Notre Dame, Dept Phys, Notre Dame, IN 46556 USA. [Keel, William C.] Univ Alabama, Dept Phys & Astron, Tuscaloosa, AL 35487 USA. [Keel, William C.] Florida Inst Technol, Dept Phys & Space Sci, SARA Observ, Melbourne, FL USA. [Lintott, Chris J.; Simpson, Robert J.] Oxford Astrophys, Oxford OX1 3RH, England. [Lintott, Chris J.; Parrish, Michael; Smith, Arfon M.; Lynn, Stuart] Adler Planetarium, Chicago, IL 60605 USA. [Kaib, Nathan A.] Northwestern Univ, Evanston, IL 60208 USA. [Terrell, Dirk] SW Res Inst, Dept Space Studies, Boulder, CO 80302 USA. [Schawinski, Kevin] Swiss Fed Inst Technol, Dept Phys, Inst Astron, CH-8093 Zurich, Switzerland. RP Schwamb, ME (reprint author), Yale Univ, Yale Ctr Astron & Astrophys, POB 208121, New Haven, CT 06520 USA. EM megan.schwamb@yale.edu RI Howard, Andrew/D-4148-2015; OI Howard, Andrew/0000-0001-8638-0320; Smith, Arfon/0000-0002-3957-2474; Schwamb, Megan/0000-0003-4365-1455; Schawinski, Kevin/0000-0001-5464-0888 FU National Science Foundation (NSF) Astronomy and Astrophysics Postdoctoral Fellowship [AST-1003258]; American Philosophical Society; Kepler Participating Scientist Program via NASA [NNX12AD23G]; NSF [AST-1109928, AST-1007992]; NASA [10-OUTRCH.210-0001, NAS8-03060, NAS5-26555]; STScI; Yale University; Leverhulme Trust; NASA Einstein Postdoctoral Fellowship, the Chandra X-ray Observatory Center [PF9-00069]; NSF CDI [DRL-0941610]; W. M. Keck Foundation; NASA Science Mission directorate; NASA Office of Space Science [NNX09AF08G] FX M.E.S. is supported by a National Science Foundation (NSF) Astronomy and Astrophysics Postdoctoral Fellowship under award AST-1003258 and in part by an American Philosophical Society Franklin Grant. J.A.O. and W.F.W. acknowledge support from the Kepler Participating Scientist Program via NASA grant NNX12AD23G and the NSF via grant AST-1109928. J.A.C. acknowledges NASA support through Hubble Fellowship grants, awarded by STScI, operated by AURA. D. A. F. acknowledges funding support from Yale University and support from the NASA Supplemental Outreach Award, 10-OUTRCH.210-0001. G. T. also acknowledges support from NSF through grant AST-1007992. C.J.L. acknowledges support from The Leverhulme Trust. K. S. acknowledges support from a NASA Einstein Postdoctoral Fellowship grant number PF9-00069, 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. The Planet Hunters "Talk" discussion tool used was developed at the Adler Planetarium with support from the NSF CDI grant: DRL-0941610.; The data presented herein were partly 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. We thank the observers from the California Planet Survey collaboration for their efforts. We thank Mike Brown and Emily Schaller for their assistance in obtaining NGS AO observations. We thank Tom Barclay, Gibor Basri, Luke Dones, Hans Kjeldsen, Hal Levison, and Andrej Prsa for useful discussions.; This paper includes data collected by the Kepler spacecraft, and we gratefully acknowledge the entire Kepler mission team's efforts in obtaining and providing the light curves used in this analysis. Funding for the Kepler mission is provided by the NASA Science Mission directorate. The publicly released Kepler light curves were obtained from the Mikulski Archive for Space Telescopes (MAST). STScI is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555. Support for MAST for non-HST data is provided by the NASA Office of Space Science via grant NNX09AF08G and by other grants and contracts. NR 75 TC 76 Z9 76 U1 0 U2 14 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAY 10 PY 2013 VL 768 IS 2 AR 127 DI 10.1088/0004-637X/768/2/127 PG 21 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 134QK UT WOS:000318228400030 ER PT J AU Snyder, GF Hayward, CC Sajina, A Jonsson, P Cox, TJ Hernquist, L Hopkins, PF Yan, L AF Snyder, Gregory F. Hayward, Christopher C. Sajina, Anna Jonsson, Patrik Cox, Thomas J. Hernquist, Lars Hopkins, Philip F. Yan, Lin TI MODELING MID-INFRARED DIAGNOSTICS OF OBSCURED QUASARS AND STARBURSTS SO ASTROPHYSICAL JOURNAL LA English DT Article DE dust, extinction; galaxies: interactions; galaxies: starburst; infrared: galaxies; quasars: general; radiative transfer ID ULTRALUMINOUS INFRARED GALAXIES; ACTIVE GALACTIC NUCLEI; SPITZER-SPACE-TELESCOPE; SIMILAR-TO 2; SUPERMASSIVE BLACK-HOLES; STAR-FORMING GALAXIES; SPECTRAL ENERGY-DISTRIBUTIONS; SMALL-MAGELLANIC-CLOUD; PARTICLE HYDRODYNAMICS SIMULATIONS; HOST GALAXIES AB We analyze the link between active galactic nuclei (AGNs) and mid-infrared flux using dust radiative transfer calculations of starbursts realized in hydrodynamical simulations. Focusing on the effects of galaxy dust, we evaluate diagnostics commonly used to disentangle AGN and star formation in ultraluminous infrared galaxies (ULIRGs). We examine these quantities as a function of time, viewing angle, dust model, AGN spectrum, and AGN strength in merger simulations representing two possible extremes of the ULIRG population: one is a typical gas-rich merger at z similar to 0, and the other is characteristic of extremely obscured starbursts at z similar to 2-4. This highly obscured burst begins star-formation-dominated with significant polycyclic aromatic hydrocarbon (PAH) emission, and ends with a similar to 10(9) yr period of red near-IR colors. At coalescence, when the AGN is most luminous, dust obscures the near-infrared AGN signature, reduces the relative emission from PAHs, and enhances the 9.7 mu m absorption by silicate grains. Although generally consistent with previous interpretations, our results imply none of these indicators can unambiguously estimate the AGN luminosity fraction in all cases. Motivated by the simulations, we show that a combination of the extinction feature at 9.7 mu m, the PAH strength, and a near-infrared slope can simultaneously constrain the AGN fraction and dust grain distribution for a wide range of obscuration. We find that this indicator, accessible to the James Webb Space Telescope, may estimate the AGN power as tightly as the hard X-ray flux alone, thereby providing a valuable future cross-check and constraint for large samples of distant ULIRGs. C1 [Snyder, Gregory F.; Jonsson, Patrik; Hernquist, Lars] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Hayward, Christopher C.] Heidelberger Inst Theoret Studien, D-69118 Heidelberg, Germany. [Sajina, Anna] Tufts Univ, Dept Phys & Astron, Medford, MA 02155 USA. [Cox, Thomas J.] Carnegie Observ, Pasadena, CA 91101 USA. [Hopkins, Philip F.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Yan, Lin] CALTECH, Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA. RP Snyder, GF (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM gsnyder@cfa.harvard.edu RI Hayward, Christopher/I-4756-2012 OI Hayward, Christopher/0000-0003-4073-3236 NR 123 TC 21 Z9 21 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 MAY 10 PY 2013 VL 768 IS 2 AR 168 DI 10.1088/0004-637X/768/2/168 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 134QK UT WOS:000318228400071 ER PT J AU Steeghs, D McClintock, JE Parsons, SG Reid, MJ Littlefair, S Dhillon, VS AF Steeghs, D. McClintock, J. E. Parsons, S. G. Reid, M. J. Littlefair, S. Dhillon, V. S. TI THE NOT-SO-MASSIVE BLACK HOLE IN THE MICROQUASAR GRS1915+105 SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries: close; stars: individual (GRS1915+105); techniques: radial velocities; X-rays: binaries ID GRS 1915+105; RADIAL-VELOCITIES; GRS-1915+105; GALAXY; STAR; VARIABILITY; DISTANCE; ENERGY; SPIN AB We present a new dynamical study of the black hole X-ray transient GRS1915+105 making use of near-infrared spectroscopy obtained with X-shooter at the Very Large Telescope. We detect a large number of donor star absorption features across a wide range of wavelengths spanning the H and K bands. Our 24 epochs covering a baseline of over 1 yr permit us to determine a new binary ephemeris including a refined orbital period of P = 33.85 +/- 0.16 days. The donor star radial velocity curves deliver a significantly improved determination of the donor semi-amplitude which is both accurate (K-2 = 126 +/- 1 km s(-1)) and robust against choice of donor star template and spectral features used. We furthermore constrain the donor star's rotational broadening to v sin i = 21 +/- 4 km s(-1), delivering a binary mass ratio of q = 0.042 +/- 0.024. If we combine these new constraints with distance and inclination estimates derived from modeling the radio emission, a black hole mass of M-BH = 10.1 +/- 0.6 M-circle dot is inferred, paired with an evolved mass donor of M-2 = 0.47 +/- 0.27 M-circle dot. Our analysis suggests a more typical black hole mass for GRS1915+105 rather than the unusually high values derived in the pioneering dynamical study by Greiner et al. Our data demonstrate that high-resolution infrared spectroscopy of obscured accreting binaries can deliver dynamical mass determinations with a precision on par with optical studies. C1 [Steeghs, D.; Parsons, S. G.] Univ Warwick, Dept Phys, Astron & Astrophys Grp, Coventry CV4 7AL, W Midlands, England. [Steeghs, D.; McClintock, J. E.; Reid, M. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Parsons, S. G.] Univ Valparaiso, Fac Ciencias, Dept Fis & Astron, Valparaiso, Chile. [Littlefair, S.; Dhillon, V. S.] Univ Sheffield, Dept Phys & Astron, Sheffield S3 7RH, S Yorkshire, England. RP Steeghs, D (reprint author), Univ Warwick, Dept Phys, Astron & Astrophys Grp, Coventry CV4 7AL, W Midlands, England. RI Steeghs, Danny/C-5468-2009; OI Steeghs, Danny/0000-0003-0771-4746; Littlefair, Stuart/0000-0001-7221-855X FU STFC [PP/D005914/1, ST/I001719/1]; NASA [NNX11AD08G]; ESO at the La Silla Paranal Observatory [085.D-0497] FX D.S. acknowledges support from STFC through an Advanced Fellowship (PP/D005914/1) as well as grant ST/I001719/1. J.E.M. acknowledges the support of NASA grant NNX11AD08G. Based on observations made with ESO Telescopes at the La Silla Paranal Observatory under program ID 085.D-0497. We thank Tom Marsh for the use of his Molly spectral analysis package. NR 28 TC 35 Z9 35 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 MAY 10 PY 2013 VL 768 IS 2 AR 185 DI 10.1088/0004-637X/768/2/185 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 134QK UT WOS:000318228400088 ER PT J AU Rando, JC Alcover, JA Olson, SL Pieper, H AF Carlos Rando, Juan Antoni Alcover, Josep Olson, Storrs L. Pieper, Harald TI A new species of extinct scops owl (Aves: Strigiformes: Strigidae: Otus) from Sao Miguel Island (Azores Archipelago, North Atlantic Ocean) SO ZOOTAXA LA English DT Article DE AMS 14C; extinction; evolution of island biotas; Macaronesia; Otus frutuosoi n. sp.; Quaternary; Sao Miguel Scops Owl ID CANARY-ISLANDS; BIRDS; GENUS AB The extinct Sao Miguel Scops Owl Otus frutuosoi n. sp. is described from fossil bones found in Gruta de Agua de Pau, a volcanic tube in Sao Miguel Island (Azores Archipelago, North Atlantic Ocean). It is the first extinct bird described from the Azores and, after the Madeiran Scops Owl (O. mauli Rando, Pieper, Alcover & Olson 2012a), the second extinct species of Strigiformes known in Macaronesia. The forelimb elements of the new taxon are shorter, the hindlimb elements are longer, and the pelvis is shorter and broader than in the Eurasian Scops Owl (O. scops Linnaeus). The new species differs from O. mauli in the smaller size of many of its bones, especially the ulna and tibiotarsus. Its measurements (estimated weight, wing area, and wing loading, and the ratio of humerus + ulna + carpometacarpus length/femur length) indicate weak powers of flight and ground-dwelling habits. The latest occurrence of the new species, as evidenced by a radiocarbon date of 1970 +/- 40 BP from bone collagen, indicates a Late Holocene extinction event subsequent to 49 cal BC, and was probably linked to human arrival and subsequent habitat alterations. C1 [Carlos Rando, Juan] Univ La Laguna, Dept Biol Anim UDI Zool, E-38206 Tenerife, Canary Islands, Spain. [Antoni Alcover, Josep] Inst Mediterrani Estudis Avancats, Dept Biodiversitat & Conservacio, Mallorca 07190, Balearic Island, Spain. [Olson, Storrs L.] Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Div Birds, Washington, DC 20560 USA. RP Alcover, JA (reprint author), Inst Mediterrani Estudis Avancats, Dept Biodiversitat & Conservacio, Mallorca 07190, Balearic Island, Spain. EM canariomys@yahoo.es; jaalcover@imedea.uib-csic.es; olsons@si.edu; orunzehpieper@condaservices.com NR 46 TC 1 Z9 1 U1 2 U2 11 PU MAGNOLIA PRESS PI AUCKLAND PA PO BOX 41383, AUCKLAND, ST LUKES 1030, NEW ZEALAND SN 1175-5326 EI 1175-5334 J9 ZOOTAXA JI Zootaxa PD MAY 9 PY 2013 VL 3647 IS 2 BP 343 EP 357 DI 10.11646/zootaxa.3647.2.6 PG 15 WC Zoology SC Zoology GA 138WU UT WOS:000318542900006 PM 26295111 ER PT J AU Keith, DA Rodriguez, JP Rodriguez-Clark, KM Nicholson, E Aapala, K Alonso, A Asmussen, M Bachman, S Basset, A Barrow, EG Benson, JS Bishop, MJ Bonifacio, R Brooks, TM Burgman, MA Comer, P Comin, FA Essl, F Faber-Langendoen, D Fairweather, PG Holdaway, RJ Jennings, M Kingsford, RT Lester, RE Mac Nally, R McCarthy, MA Moat, J Oliveira-Miranda, MA Pisanu, P Poulin, B Regan, TJ Riecken, U Spalding, MD Zambrano-Martinez, S AF Keith, David A. Rodriguez, Jon Paul Rodriguez-Clark, Kathryn M. Nicholson, Emily Aapala, Kaisu Alonso, Alfonso Asmussen, Marianne Bachman, Steven Basset, Alberto Barrow, Edmund G. Benson, John S. Bishop, Melanie J. Bonifacio, Ronald Brooks, Thomas M. Burgman, Mark A. Comer, Patrick Comin, Francisco A. Essl, Franz Faber-Langendoen, Don Fairweather, Peter G. Holdaway, Robert J. Jennings, Michael Kingsford, Richard T. Lester, Rebecca E. Mac Nally, Ralph McCarthy, Michael A. Moat, Justin Oliveira-Miranda, Maria A. Pisanu, Phil Poulin, Brigitte Regan, Tracey J. Riecken, Uwe Spalding, Mark D. Zambrano-Martinez, Sergio TI Scientific Foundations for an IUCN Red List of Ecosystems SO PLOS ONE LA English DT Article ID FOOD-WEB PERSPECTIVE; BIODIVERSITY LOSS; EXTINCTION RISK; HABITAT LOSS; VEGETATION CLASSIFICATION; ECOLOGICAL COMMUNITIES; CONSERVATION BIOLOGY; ENVIRONMENTAL-CHANGE; RELATIVE RESILIENCE; GLOBAL SYNTHESIS AB An understanding of risks to biodiversity is needed for planning action to slow current rates of decline and secure ecosystem services for future human use. Although the IUCN Red List criteria provide an effective assessment protocol for species, a standard global assessment of risks to higher levels of biodiversity is currently limited. In 2008, IUCN initiated development of risk assessment criteria to support a global Red List of ecosystems. We present a new conceptual model for ecosystem risk assessment founded on a synthesis of relevant ecological theories. To support the model, we review key elements of ecosystem definition and introduce the concept of ecosystem collapse, an analogue of species extinction. The model identifies four distributional and functional symptoms of ecosystem risk as a basis for assessment criteria: A) rates of decline in ecosystem distribution; B) restricted distributions with continuing declines or threats; C) rates of environmental (abiotic) degradation; and D) rates of disruption to biotic processes. A fifth criterion, E) quantitative estimates of the risk of ecosystem collapse, enables integrated assessment of multiple processes and provides a conceptual anchor for the other criteria. We present the theoretical rationale for the construction and interpretation of each criterion. The assessment protocol and threat categories mirror those of the IUCN Red List of species. A trial of the protocol on terrestrial, subterranean, freshwater and marine ecosystems from around the world shows that its concepts are workable and its outcomes are robust, that required data are available, and that results are consistent with assessments carried out by local experts and authorities. The new protocol provides a consistent, practical and theoretically grounded framework for establishing a systematic Red List of the world's ecosystems. This will complement the Red List of species and strengthen global capacity to report on and monitor the status of biodiversity C1 [Keith, David A.; Kingsford, Richard T.] Univ New S Wales, Australian Wetlands Rivers & Landscapes Ctr, Sydney, NSW, Australia. [Keith, David A.] New South Wales Off Environm & Heritage, Hurstville, NSW, Australia. [Rodriguez, Jon Paul; Rodriguez-Clark, Kathryn M.; Asmussen, Marianne; Zambrano-Martinez, Sergio] Inst Venezolano Invest Cient, Ctr Ecol, Caracas, Venezuela. [Rodriguez, Jon Paul; Oliveira-Miranda, Maria A.] Provita, Caracas, Venezuela. [Rodriguez, Jon Paul; Asmussen, Marianne] EcoHlth Alliance, New York, NY USA. [Rodriguez, Jon Paul; Brooks, Thomas M.] IUCN Commiss Ecosyst Management, Gland, Switzerland. [Rodriguez, Jon Paul; Brooks, Thomas M.] IUCN Species Survival Commiss, Gland, Switzerland. [Nicholson, Emily; McCarthy, Michael A.; Regan, Tracey J.] Univ Melbourne, Ctr Excellence Environm Decis, Melbourne, Vic 3010, Australia. [Aapala, Kaisu] Finnish Environm Inst, Helsinki, Finland. [Alonso, Alfonso] Smithsonian Inst, Natl Zool Pk, Smithsonian Conservat Biol Inst, Washington, DC 20008 USA. [Bachman, Steven; Moat, Justin] Royal Bot Gardens, Richmond, England. [Basset, Alberto] Univ Salento, Ecotekne Ctr, Dept Biol & Environm Sci, Lecce, Italy. [Barrow, Edmund G.] IUCN Global Ecosyst Management Programme, Nairobi, Kenya. [Benson, John S.] Royal Bot Gardens Trust, Sydney, NSW, Australia. [Bishop, Melanie J.] Macquarie Univ, Dept Biol Sci, N Ryde, NSW 2109, Australia. [Bonifacio, Ronald; Pisanu, Phil] Sci Resource Ctr, Dept Environm & Nat Resources, Adelaide, SA, Australia. [Brooks, Thomas M.; Faber-Langendoen, Don] NatureServe, Arlington, VA USA. [Burgman, Mark A.] Univ Melbourne, Australian Ctr Excellence Risk Assessment, Melbourne, Vic 3010, Australia. [Comer, Patrick] NatureServe, Boulder, CO USA. [Comin, Francisco A.] Pyrenean Inst Ecol, Zaragoza, Spain. [Essl, Franz] Environm Agcy Austria, Vienna, Austria. [Essl, Franz] Univ Vienna, Dept Conservat Biol Vegetat & Landscape Ecol, Vienna, Austria. [Fairweather, Peter G.] Flinders Univ S Australia, Sch Biol Sci, Adelaide, SA 5001, Australia. [Holdaway, Robert J.] Landcare Res, Lincoln, New Zealand. [Jennings, Michael] Univ Idaho, Dept Geog, Moscow, ID 83843 USA. [Lester, Rebecca E.] Deakin Univ, Sch Life & Environm Sci, Warrnambool, Vic, Australia. [Mac Nally, Ralph] Monash Univ, Sch Biol Sci, Australian Ctr Biodivers, Clayton, Vic 3800, Australia. [Poulin, Brigitte] Tour du Valat Res Ctr, Arles, France. [Riecken, Uwe] German Fed Agcy Nat Conservat, Bonn, Germany. [Spalding, Mark D.] Univ Cambridge, Dept Zool, Nat Conservancy & Conservat Sci Grp, Cambridge, England. RP Keith, DA (reprint author), Univ New S Wales, Australian Wetlands Rivers & Landscapes Ctr, Sydney, NSW, Australia. EM david.keith@unsw.edu.au RI Rodriguez, Jon Paul/A-1491-2009; Nicholson, Emily/H-9001-2013; Lester, Rebecca/H-3907-2011; OI Rodriguez, Jon Paul/0000-0001-5019-2870; Nicholson, Emily/0000-0003-2199-3446; Lester, Rebecca/0000-0003-2682-6495; Brooks, Thomas/0000-0001-8159-3116; Essl, Franz/0000-0001-8253-2112; Bishop, Melanie/0000-0001-8210-6500; McCarthy, Michael/0000-0003-1039-7980 FU MAVA Foundation; Gordon and Betty Moore Foundation; Smithsonian Institution; EcoHealth Alliance, Provita; Fulbright Program; Tour du Valat,; Australian Centre of Excellence for Environmental Decisions and Centre de Suive Ecologique FX The authors gratefully acknowledge funding support from the MAVA Foundation, Gordon and Betty Moore Foundation, Smithsonian Institution, EcoHealth Alliance, Provita, the Fulbright Program, Tour du Valat, the Australian Centre of Excellence for Environmental Decisions and Centre de Suive Ecologique. The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 175 TC 88 Z9 92 U1 15 U2 179 PU PUBLIC LIBRARY SCIENCE PI SAN FRANCISCO PA 1160 BATTERY STREET, STE 100, SAN FRANCISCO, CA 94111 USA SN 1932-6203 J9 PLOS ONE JI PLoS One PD MAY 8 PY 2013 VL 8 IS 5 AR e62111 DI 10.1371/journal.pone.0062111 PG 25 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 145YI UT WOS:000319055600016 PM 23667454 ER PT J AU First, MR Robbins-Wamsley, SH Riley, SC Moser, CS Smith, GE Tamburri, MN Drake, LA AF First, Matthew R. Robbins-Wamsley, Stephanie H. Riley, Scott C. Moser, Cameron S. Smith, George E. Tamburri, Mario N. Drake, Lisa A. TI Stratification of Living Organisms in Ballast Tanks: How Do Organism Concentrations Vary as Ballast Water Is Discharged? SO ENVIRONMENTAL SCIENCE & TECHNOLOGY LA English DT Article ID MARINE SNOW; TRANSPORT; DYNAMICS AB Vertical migrations of living organisms and settling of particle-attached organisms lead to uneven distributions of biota at different depths in the water column. In ballast tanks, heterogeneity could lead to different population estimates depending on the portion of the discharge sampled. For example, concentrations of organisms exceeding a discharge standard may not be detected if sampling occurs during periods of the discharge when concentrations are low. To determine the degree of stratification, water from ballast tanks was sampled at two experimental facilities as the tanks were drained after water was held for 1 or 5 days. Living organisms >= 50 mu m were counted in discrete segments of the drain (e.g., the first 20 min of the drain operation, the second 20 min interval, etc.), thus representing different strata in the tank. In 1 and 5 day trials at both facilities, concentrations of organisms varied among drain segments, and the patterns of stratification varied among replicate trials. From numerical simulations, the optimal sampling strategy for stratified tanks is to collect multiple time-integrated samples spaced relatively evenly throughout the discharge event. C1 [First, Matthew R.; Robbins-Wamsley, Stephanie H.; Riley, Scott C.] SAIC Inc, Key West, FL 33041 USA. [Moser, Cameron S.] EXCET Inc, Key West, FL 33041 USA. [Smith, George E.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. [Tamburri, Mario N.] Univ Maryland, Chesapeake Biol Lab, Ctr Environm Sci, Solomons, MD 20688 USA. [Drake, Lisa A.] USN, Div Chem, Res Lab, Key West, FL 33041 USA. RP First, MR (reprint author), SAIC Inc, Key West, FL 33041 USA. EM matthew.first.ctr@nrl.navy.mil RI Tamburri, Mario/F-7193-2013; OI First, Matthew/0000-0003-1330-3353; First, Matt/0000-0003-3465-2376 FU United States Coast Guard Environmental (USCG) Standards Division [CG-5224, HSCG23-10-X-MMS192, HSCG23-11-X-MMS154]; Maryland Port Administration; US Maritime Administration FX This work was supported by the United States Coast Guard Environmental (USCG) Standards Division (CG-5224, contracts HSCG23-10-X-MMS192 and HSCG23-11-X-MMS154), although this work does not reflect official USCG policy. Support for the work conducted at MERC was provided by the Maryland Port Administration and US Maritime Administration. The research conducted at the Naval Research Laboratory in Key West was supported by Diane Lysogorski (Section Head of NRL Code 6136 and Director of the Center for Corrosion Science and Engineering, Key West, Florida). We are grateful to Richard Everett (USCG) for his input and advice with this effort. We also appreciate the comments and suggestions provided by two anonymous reviewers, Ms. Lysogorski, and Richard Colton (Superintendent, Chemistry Division, Naval Research Laboratory), which improved and clarified earlier drafts of this manuscript. NR 29 TC 9 Z9 9 U1 1 U2 27 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0013-936X J9 ENVIRON SCI TECHNOL JI Environ. Sci. Technol. PD MAY 7 PY 2013 VL 47 IS 9 BP 4442 EP 4448 DI 10.1021/es400033z PG 7 WC Engineering, Environmental; Environmental Sciences SC Engineering; Environmental Sciences & Ecology GA 141WA UT WOS:000318756000062 PM 23614690 ER PT J AU Borucki, WJ Agol, E Fressin, F Kaltenegger, L Rowe, J Isaacson, H Fischer, D Batalha, N Lissauer, JJ Marcy, GW Fabrycky, D Desert, JM Bryson, ST Barclay, T Bastien, F Boss, A Brugamyer, E Buchhave, LA Burke, C Caldwell, DA Carter, J Charbonneau, D Crepp, JR Christensen-Dalsgaard, J Christiansen, JL Ciardi, D Cochran, WD DeVore, E Doyle, L Dupree, AK Endl, M Everett, ME Ford, EB Fortney, J Gautier, TN Geary, JC Gould, A Haas, M Henze, C Howard, AW Howell, SB Huber, D Jenkins, JM Kjeldsen, H Kolbl, R Kolodziejczak, J Latham, DW Lee, BL Lopez, E Mullally, F Orosz, JA Prsa, A Quintana, EV Sanchis-Ojeda, R Sasselov, D Seader, S Shporer, A Steffen, JH Still, M Tenenbaum, P Thompson, SE Torres, G Twicken, JD Welsh, WF Winn, JN AF Borucki, William J. Agol, Eric Fressin, Francois Kaltenegger, Lisa Rowe, Jason Isaacson, Howard Fischer, Debra Batalha, Natalie Lissauer, Jack J. Marcy, Geoffrey W. Fabrycky, Daniel Desert, Jean-Michel Bryson, Stephen T. Barclay, Thomas Bastien, Fabienne Boss, Alan Brugamyer, Erik Buchhave, Lars A. Burke, Chris Caldwell, Douglas A. Carter, Josh Charbonneau, David Crepp, Justin R. Christensen-Dalsgaard, Jorgen Christiansen, Jessie L. Ciardi, David Cochran, William D. DeVore, Edna Doyle, Laurance Dupree, Andrea K. Endl, Michael Everett, Mark E. Ford, Eric B. Fortney, Jonathan Gautier, Thomas N., III Geary, John C. Gould, Alan Haas, Michael Henze, Christopher Howard, Andrew W. Howell, Steve B. Huber, Daniel Jenkins, Jon M. Kjeldsen, Hans Kolbl, Rea Kolodziejczak, Jeffery Latham, David W. Lee, Brian L. Lopez, Eric Mullally, Fergal Orosz, Jerome A. Prsa, Andrej Quintana, Elisa V. Sanchis-Ojeda, Roberto Sasselov, Dimitar Seader, Shawn Shporer, Avi Steffen, Jason H. Still, Martin Tenenbaum, Peter Thompson, Susan E. Torres, Guillermo Twicken, Joseph D. Welsh, William F. Winn, Joshua N. TI Kepler-62: A Five-Planet System with Planets of 1.4 and 1.6 Earth Radii in the Habitable Zone SO SCIENCE LA English DT Article ID SUN-LIKE STAR; TRANSITING PLANET; CANDIDATES; SCIENCE; MASS; II. AB We present the detection of five planets-Kepler-62b, c, d, e, and f-of size 1.31, 0.54, 1.95, 1.61 and 1.41 Earth radii (R-circle plus), orbiting a K2V star at periods of 5.7, 12.4, 18.2, 122.4, and 267.3 days, respectively. The outermost planets, Kepler-62e and -62f, are super-Earth-size (1.25 R-circle plus < planet radius <= 2.0 R-circle plus) planets in the habitable zone of their host star, respectively receiving 1.2 +/- 0.2 times and 0.41 +/- 0.05 times the solar flux at Earth's orbit. Theoretical models of Kepler-62e and -62f for a stellar age of similar to 7 billion years suggest that both planets could be solid, either with a rocky composition or composed of mostly solid water in their bulk. C1 [Borucki, William J.; Batalha, Natalie; Lissauer, Jack J.; Bryson, Stephen T.; Haas, Michael; Henze, Christopher; Howell, Steve B.; Huber, Daniel] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Agol, Eric; Lee, Brian L.] Univ Washington, Dept Astron, Seattle, WA 98195 USA. [Fressin, Francois; Kaltenegger, Lisa; Desert, Jean-Michel; Carter, Josh; Charbonneau, David; Dupree, Andrea K.; Geary, John C.; Latham, David W.; Sasselov, Dimitar; Torres, Guillermo] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Kaltenegger, Lisa] Max Planck Inst Astron, D-69115 Heidelberg, Germany. [Rowe, Jason; Burke, Chris; Caldwell, Douglas A.; Christiansen, Jessie L.; DeVore, Edna; Doyle, Laurance; Jenkins, Jon M.; Mullally, Fergal; Quintana, Elisa V.; Seader, Shawn; Tenenbaum, Peter; Thompson, Susan E.; Twicken, Joseph D.] SETI Inst, Mountain View, CA 94043 USA. [Isaacson, Howard; Marcy, Geoffrey W.; Kolbl, Rea] Univ Calif Berkeley, Berkeley, CA 94720 USA. [Fischer, Debra] Yale Univ, New Haven, CT 06520 USA. [Fabrycky, Daniel; Fortney, Jonathan; Lopez, Eric; Shporer, Avi] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. [Fabrycky, Daniel] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. [Barclay, Thomas; Still, Martin] Bay Area Environm Res Inst, Moffett Field, CA 94035 USA. [Bastien, Fabienne] Vanderbilt Univ, Nashville, TN 37235 USA. [Boss, Alan] Carnegie Inst Sci, Washington, DC 20015 USA. [Brugamyer, Erik; Cochran, William D.; Endl, Michael] Univ Texas Austin, McDonald Observ, Austin, TX 78712 USA. [Buchhave, Lars A.] Univ Copenhagen, Niels Bohr Inst, DK-2100 Copenhagen, Denmark. [Buchhave, Lars A.] Univ Copenhagen, Nat Hist Museum Denmark, Ctr Star & Planet Format, DK-1350 Copenhagen, Denmark. [Crepp, Justin R.] CALTECH, Dept Astron, Pasadena, CA 91125 USA. [Crepp, Justin R.] Univ Notre Dame, Dept Phys, Notre Dame, IN 46556 USA. [Christensen-Dalsgaard, Jorgen; Kjeldsen, Hans] Aarhus Univ, Dept Phys & Astron, Aarhus, Denmark. [Ciardi, David] CALTECH, Exoplanet Sci Inst, Pasadena, CA 91125 USA. [Everett, Mark E.] Natl Opt Astron Observ, Tucson, AZ 85719 USA. [Ford, Eric B.] Univ Florida, Gainesville, FL 32611 USA. [Gautier, Thomas N., III] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Gould, Alan] Lawrence Hall Sci, Berkeley, CA 94720 USA. [Howard, Andrew W.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Kolodziejczak, Jeffery] George C Marshall Space Flight Ctr, Huntsville, AL 35805 USA. [Orosz, Jerome A.; Welsh, William F.] San Diego State Univ, San Diego, CA 92182 USA. [Prsa, Andrej] Villanova Univ, Villanova, PA 19085 USA. [Shporer, Avi] Las Cumbres Observ Global Telescope, Goleta, CA 93117 USA. [Steffen, Jason H.] Northwestern Univ, Evanston, IL 60208 USA. [Sanchis-Ojeda, Roberto; Winn, Joshua N.] MIT, Cambridge, MA 02139 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; /0000-0002-0802-9145; Buchhave, Lars A./0000-0003-1605-5666; Ciardi, David/0000-0002-5741-3047; Fischer, Debra/0000-0003-2221-0861; Fabrycky, Daniel/0000-0003-3750-0183 FU NASA's Science Mission Directorate; W. M. Keck Foundation; Deutsche Forschungsgemeinschaft [ENP Ka 3142/1-1]; NASA Astrobiology Institute; Danish National Research Foundation; ASTERISK project; European Research Council [267864]; NASA through the Kepler Participating Scientist Program (PSP); NSF [AST-1109928, AST-0645416]; NASA [ADAP12-0172]; NASA PSP [NNX08AR04G, NNX12AF73G]; NASA 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 of the California Institute of Technology, the University of California, and NASA. The Keck Observatory was made possible by the generous financial support of the W. M. Keck Foundation. L.K. acknowledges support from Deutsche Forschungsgemeinschaft grants ENP Ka 3142/1-1 and NASA Astrobiology Institute. Funding for the Stellar Astrophysics Centre is provided by the Danish National Research Foundation. The research is supported by the ASTERISK project (Asteroseismic Investigations with SONG and Kepler) funded by European Research Council grant 267864. W. F. W. and J.A.O. acknowledge support from NASA through the Kepler Participating Scientist Program (PSP) and from NSF grant AST-1109928. D.F. acknowledges support from NASA ADAP12-0172. O.R.S.-O. and J.N.W. are supported by the Kepler PSP through grant NNX12AC76G. E.F. is partially supported by NASA PSP grants NNX08AR04G and NNX12AF73G. E.A. acknowledges NSF career grant AST-0645416. We also thank the Spitzer staff at IPAC and in particular N. Silbermann for checking and scheduling the Spitzer observations. The Spitzer Space Telescope is operated by the Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA. We thank the many people who gave so generously of their time to make this mission a success. All data products are available to the public at the Mikulski Archive for Space Telescopes, http://stdatu.stsci.edu/kepler. NR 26 TC 98 Z9 99 U1 90 U2 290 PU AMER ASSOC ADVANCEMENT SCIENCE PI WASHINGTON PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA SN 0036-8075 J9 SCIENCE JI Science PD MAY 3 PY 2013 VL 340 IS 6132 BP 587 EP 590 DI 10.1126/science.1234702 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 135EA UT WOS:000318268900042 PM 23599262 ER PT J AU Morgan, GA Campbell, BA Carter, LM Plaut, JJ Phillips, RJ AF Morgan, Gareth A. Campbell, Bruce A. Carter, Lynn M. Plaut, Jeffrey J. Phillips, Roger J. TI 3D Reconstruction of the Source and Scale of Buried Young Flood Channels on Mars SO SCIENCE LA English DT Article ID CERBERUS FOSSAE; STRATIGRAPHY; PLAINS; WATER; LAVA AB Outflow channels on Mars are interpreted as the product of gigantic floods due to the catastrophic eruption of groundwater that may also have initiated episodes of climate change. Marte Vallis, the largest of the young martian outflow channels (<500 million years old), is embayed by lava flows that hinder detailed studies and comparisons with older channel systems. Understanding Marte Vallis is essential to our assessment of recent Mars hydrologic activity during a period otherwise considered to be cold and dry. Using data from the Shallow Radar sounder on the Mars Reconnaissance Orbiter, we present a three-dimensional (3D) reconstruction of buried channels on Mars and provide estimates of paleohydrologic parameters. Our work shows that Cerberus Fossae provided the waters that carved Marte Vallis, and it extended an additional 180 kilometers to the east before the emplacement of the younger lava flows. We identified two stages of channel incision and determined that channel depths were more than twice those of previous estimates. C1 [Morgan, Gareth A.; Campbell, Bruce A.] Smithsonian Inst, Ctr Earth & Planetary Studies, Washington, DC 20560 USA. [Carter, Lynn M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Plaut, Jeffrey J.] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Phillips, Roger J.] SW Res Inst, Planetary Sci Directorate, Boulder, CO USA. RP Morgan, GA (reprint author), Smithsonian Inst, Ctr Earth & Planetary Studies, Washington, DC 20560 USA. EM morganga@si.edu RI Carter, Lynn/D-2937-2012 FU NASA Mars Reconnaissance Orbiter Project FX C. Chazen and T. Watters provided very helpful reviews of earlier versions of the paper. Comments and suggestions by four anonymous referees were extremely beneficial. Thanks are also extended to P. Russell for his technical assistance. Funding for this work was provided by the NASA Mars Reconnaissance Orbiter Project. The SHARAD data and MOLA altimetry are available through NASA's Planetary Data system. NR 22 TC 5 Z9 5 U1 0 U2 24 PU AMER ASSOC ADVANCEMENT SCIENCE PI WASHINGTON PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA SN 0036-8075 EI 1095-9203 J9 SCIENCE JI Science PD MAY 3 PY 2013 VL 340 IS 6132 BP 607 EP 610 DI 10.1126/science.1234787 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 135EA UT WOS:000318268900047 PM 23470730 ER PT J AU Priede, IG Bergstad, OA Miller, PI Vecchione, M Gebruk, A Falkenhaug, T Billett, DSM Craig, J Dale, AC Shields, MA Tilstone, GH Sutton, TT Gooday, AJ Inall, ME Jones, DOB Martinez-Vicente, V Menezes, GM Niedzielski, T Sigurosson, P Rothe, N Rogacheva, A Alt, CHS Brand, T Abell, R Brierley, AS Cousins, NJ Crockard, D Hoelzel, AR Hoines, A Letessier, TB Read, JF Shimmield, T Cox, MJ Galbraith, JK Gordon, JDM Horton, T Neat, F Lorance, P AF Priede, Imants G. Bergstad, Odd Aksel Miller, Peter I. Vecchione, Michael Gebruk, Andrey Falkenhaug, Tone Billett, David S. M. Craig, Jessica Dale, Andrew C. Shields, Mark A. Tilstone, Gavin H. Sutton, Tracey T. Gooday, Andrew J. Inall, Mark E. Jones, Daniel O. B. Martinez-Vicente, Victor Menezes, Gui M. Niedzielski, Tomasz Sigurosson, Porsteinn Rothe, Nina Rogacheva, Antonina Alt, Claudia H. S. Brand, Timothy Abell, Richard Brierley, Andrew S. Cousins, Nicola J. Crockard, Deborah Hoelzel, A. Rus Hoines, Age Letessier, Tom B. Read, Jane F. Shimmield, Tracy Cox, Martin J. Galbraith, John K. Gordon, John D. M. Horton, Tammy Neat, Francis Lorance, Pascal TI Does Presence of a Mid-Ocean Ridge Enhance Biomass and Biodiversity? SO PLOS ONE LA English DT Article ID MID-ATLANTIC RIDGE; TEMPERATE NE ATLANTIC; DEEP-WATER FISH; NORTH-ATLANTIC; SEA-FLOOR; CORYPHAENOIDES-RUPESTRIS; DEMERSAL FISH; OCEAN; SEAMOUNTS; PATTERNS AB In contrast to generally sparse biological communities in open-ocean settings, seamounts and ridges are perceived as areas of elevated productivity and biodiversity capable of supporting commercial fisheries. We investigated the origin of this apparent biological enhancement over a segment of the North Mid-Atlantic Ridge (MAR) using sonar, corers, trawls, traps, and a remotely operated vehicle to survey habitat, biomass, and biodiversity. Satellite remote sensing provided information on flow patterns, thermal fronts, and primary production, while sediment traps measured export flux during 2007-2010. The MAR, 3,704,404 km 2 in area, accounts for 44.7% lower bathyal habitat (800-3500 m depth) in the North Atlantic and is dominated by fine soft sediment substrate (95% of area) on a series of flat terraces with intervening slopes either side of the ridge axis contributing to habitat heterogeneity. The MAR fauna comprises mainly species known from continental margins with no evidence of greater biodiversity. Primary production and export flux over the MAR were not enhanced compared with a nearby reference station over the Porcupine Abyssal Plain. Biomasses of benthic macrofauna and megafauna were similar to global averages at the same depths totalling an estimated 258.9 kt C over the entire lower bathyal north MAR. A hypothetical flat plain at 3500 m depth in place of the MAR would contain 85.6 kt C, implying an increase of 173.3 kt C attributable to the presence of the Ridge. This is approximately equal to 167 kt C of estimated pelagic biomass displaced by the volume of the MAR. There is no enhancement of biological productivity over the MAR; oceanic bathypelagic species are replaced by benthic fauna otherwise unable to survive in the mid ocean. We propose that globally sea floor elevation has no effect on deep sea biomass; pelagic plus benthic biomass is constant within a given surface productivity regime. C1 [Priede, Imants G.; Craig, Jessica; Shields, Mark A.; Cousins, Nicola J.; Crockard, Deborah] Univ Aberdeen, Inst Biol & Environm Sci, Oceanlab, Aberdeen, Scotland. [Bergstad, Odd Aksel; Falkenhaug, Tone] Inst Marine Res, Flodevigen, His, Norway. [Miller, Peter I.; Tilstone, Gavin H.; Martinez-Vicente, Victor] Plymouth Marine Lab, Remote Sensing Grp, Plymouth, Devon, England. [Vecchione, Michael] Smithsonian Inst, Natl Museum Nat Hist, Natl Systemat Lab, Natl Marine Fisheries Serv,NOAA, Washington, DC 20560 USA. [Gebruk, Andrey; Rogacheva, Antonina] Russian Acad Sci, PP Shirshov Inst Oceanol, Moscow, Russia. [Billett, David S. M.; Gooday, Andrew J.; Jones, Daniel O. B.; Rothe, Nina; Alt, Claudia H. S.; Read, Jane F.; Horton, Tammy] Natl Oceanog Ctr, Southampton, Hants, England. [Dale, Andrew C.; Inall, Mark E.; Brand, Timothy; Abell, Richard; Shimmield, Tracy; Gordon, John D. M.] Scottish Marine Inst, Scottish Assoc Marine Sci, Oban, Argyll, Scotland. [Sutton, Tracey T.] Coll William & Mary, Virginia Inst Marine Sci, Gloucester Point, VA USA. [Menezes, Gui M.] Univ Azores, Dept Oceanog & Fisheries, Horta, Faial, Portugal. [Niedzielski, Tomasz] Univ Wroclaw, Inst Geog & Reg Dev, Dept Geoinformat & Cartog, PL-50138 Wroclaw, Poland. [Sigurosson, Porsteinn] Marine Res Inst, IS-121 Reykjavik, Iceland. [Brierley, Andrew S.] Univ St Andrews, Scottish Oceans Inst, St Andrews KY16 9AJ, Fife, Scotland. [Hoelzel, A. Rus] Univ Durham, Sch Biol & Biomed Sci, Durham, England. [Hoines, Age] Inst Marine Res, N-5024 Bergen, Norway. [Letessier, Tom B.] Univ Western Australia, Oceans Inst, Ctr Marine Futures, Perth, WA 6009, Australia. [Cox, Martin J.] Australian Antarctic Div, Southern Ocean Ecosyst Change Dept, Kingston, Tas, Australia. [Galbraith, John K.] NOAA, Northeast Fisheries Sci Ctr, Woods Hole, MA USA. [Neat, Francis] Marine Scotland Sci, Marine Lab, Aberdeen, Scotland. [Lorance, Pascal] IFREMER, Ctr Atlantique, F-44311 Nantes 03, France. RP Priede, IG (reprint author), Univ Aberdeen, Inst Biol & Environm Sci, Oceanlab, Aberdeen, Scotland. EM i.g.priede@abdn.ac.uk RI Miller, Peter/E-4525-2013; Jones, Daniel/A-3412-2009; Horton, Tammy/G-3590-2010; Alt, Claudia/B-5439-2014; Dale, Andrew/H-4847-2012; Inall, Mark/I-4835-2014; Menezes, Gui/A-3956-2009; Martinez-Vicente, Victor/F-5131-2010; OI Miller, Peter/0000-0002-5292-8789; Jones, Daniel/0000-0001-5218-1649; Horton, Tammy/0000-0003-4250-1068; Dale, Andrew/0000-0002-9256-7770; Inall, Mark/0000-0002-1624-4275; Menezes, Gui/0000-0003-0781-4579; Martinez-Vicente, Victor/0000-0003-3492-583X; Priede, Imants/0000-0002-5064-9751; Bergstad, Odd Aksel/0000-0002-4096-0896; Lorance, Pascal/0000-0002-6453-2925; Tilstone, Gavin/0000-0002-9347-1682 FU UK Natural Environment Research Council [NE/C512961/1]; Census of Marine Life FX The research was funded by the UK Natural Environment Research Council (http://www.nerc.ac.uk/) consortium grant number NE/C512961/1 for a project entitled: ECOMAR; Ecosystem of the Mid Atlantic Ridge at the Sub-Polar Front and Charlie Gibbs Fracture Zone. Funding was also provided by the Census of Marine Life (http://www.coml.org/). Other than selecting the project for funding and approving the resources required, the funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 55 TC 19 Z9 19 U1 2 U2 69 PU PUBLIC LIBRARY SCIENCE PI SAN FRANCISCO PA 1160 BATTERY STREET, STE 100, SAN FRANCISCO, CA 94111 USA SN 1932-6203 J9 PLOS ONE JI PLoS One PD MAY 2 PY 2013 VL 8 IS 5 AR e61550 DI 10.1371/journal.pone.0061550 PG 10 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 175AF UT WOS:000321200500009 PM 23658696 ER PT J AU Crabtree, KN Martinez, O Barreau, L Thorwirth, S McCarthy, MC AF Crabtree, Kyle N. Martinez, Oscar, Jr. Barreau, Lou Thorwirth, Sven McCarthy, Michael C. TI Microwave Detection of Sulfoxylic Acid (HOSOH) SO JOURNAL OF PHYSICAL CHEMISTRY A LA English DT Article ID GAS-PHASE; SULFINIC ACID; AB-INITIO; SULFUR-COMPOUNDS; 2ND DERIVATIVES; COUPLED-CLUSTER; MOLECULES; SPECTRA; H2S; PERTURBATION AB Sulfoxylic acid (HOSOH), a chemical intermediate roughly midway along the path between highly reduced (H2S) and highly oxidized sulfur (H2SO4), has been detected using Fourier transform microwave spectroscopy and double resonance techniques, guided by new high-level CCSD(T) quantum chemical calculations of its molecular structure. Rotational spectra of the two most stable isomers of HOSOH, the putative ground state with C-2 symmetry and the low-lying C-5 rotamer, have been measured to high precision up to 71 GHz, allowing accurate spectroscopic parameters to be derived for both isomers. HOSOH may play a role in atmospheric and interstellar chemistry, and the present work provides the essential data to enable remote sensing and/or radioastronomical searches for these species. Spectroscopic characterization of HOSOH suggests that other transient intermediates in the oxidation of SO2 to H2SO4 may be amenable to laboratory detection as Well. C1 [Crabtree, Kyle N.; Martinez, Oscar, Jr.; Barreau, Lou; McCarthy, Michael C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Thorwirth, Sven] Univ Cologne, Inst Phys 1, D-50937 Cologne, Germany. RP McCarthy, MC (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM mccarthy@cfa.harvard.edu RI Thorwirth, Sven/C-6217-2011; OI Thorwirth, Sven/0000-0001-8200-6710; McCarthy, Michael/0000-0001-9142-0008; Crabtree, Kyle/0000-0001-5629-5192; Barreau, Lou/0000-0002-1312-2600 FU NSF [CHE-1058063]; CfA Postdoctoral Fellowship from the Smithsonian Astrophysical Observatory; Deutsche Forschungsgemeinschaft (DFG) [TH 1301/3-1, TH 1301/3-2] FX The work in Cambridge is supported by NSF grant no. CHE-1058063. K.N.C. has been supported by a CfA Postdoctoral Fellowship from the Smithsonian Astrophysical Observatory. S.T. gratefully acknowledges funding by the Deutsche Forschungsgemeinschaft (DFG) through grants TH 1301/3-1 and TH 1301/3-2. NR 42 TC 12 Z9 12 U1 2 U2 12 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 1089-5639 J9 J PHYS CHEM A JI J. Phys. Chem. A PD MAY 2 PY 2013 VL 117 IS 17 BP 3608 EP 3613 DI 10.1021/jp400742q PG 6 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA 138UZ UT WOS:000318536800005 PM 23534485 ER PT J AU Hetzinger, S Halfar, J Zack, T Mecking, JV Kunz, BE Jacob, DE Adey, WH AF Hetzinger, S. Halfar, J. Zack, T. Mecking, J. V. Kunz, B. E. Jacob, D. E. Adey, W. H. TI Coralline algal Barium as indicator for 20th century northwestern North Atlantic surface ocean freshwater variability SO SCIENTIFIC REPORTS LA English DT Article ID MARGINAL ICE-ZONE; GREAT-BARRIER-REEF; PAST 4 DECADES; NEWFOUNDLAND SHELF; SALINITY VARIABILITY; EQUATORIAL PACIFIC; SEA ICE; CIRCULATION; CLIMATE; FORAMINIFERA AB During the past decades climate and freshwater dynamics in the northwestern North Atlantic have undergone major changes. Large-scale freshening episodes, related to polar freshwater pulses, have had a strong influence on ocean variability in this climatically important region. However, little is known about variability before 1950, mainly due to the lack of long-term high-resolution marine proxy archives. Here we present the first multidecadal-length records of annually resolved Ba/Ca variations from Northwest Atlantic coralline algae. We observe positive relationships between algal Ba/Ca ratios from two Newfoundland sites and salinity observations back to 1950. Both records capture episodical multi-year freshening events during the 20th century. Variability in algal Ba/Ca is sensitive to freshwater-induced changes in upper ocean stratification, which affect the transport of cold, Ba-enriched deep waters onto the shelf (highly stratified equals less Ba/Ca). Algal Ba/Ca ratios therefore may serve as a new resource for reconstructing past surface ocean freshwater changes. C1 [Hetzinger, S.; Halfar, J.] Univ Toronto, CPS Dept, Mississauga, ON L5L 1C6, Canada. [Hetzinger, S.] GEOMAR Helmholtz Zentrum Ozeanforsch Kiel, D-24148 Kiel, Germany. [Zack, T.; Kunz, B. E.; Jacob, D. E.] Johannes Gutenberg Univ Mainz, Dept Geosci, Earth Syst Sci Res Ctr, D-55099 Mainz, Germany. [Zack, T.] Univ Gothenburg, Dept Earth Sci, S-40530 Gothenburg, Sweden. [Mecking, J. V.] GEOMAR Helmholtz Zentrum Ozeanforsch Kiel, D-24105 Kiel, Germany. [Mecking, J. V.] Univ Bergen, Inst Geophys, N-5007 Bergen, Norway. [Jacob, D. E.] Macquarie Univ, N Ryde, NSW 2109, Australia. [Adey, W. H.] Smithsonian Inst, Dept Bot, Washington, DC 20560 USA. RP Hetzinger, S (reprint author), Univ Toronto, CPS Dept, 3359 Mississauga Rd N, Mississauga, ON L5L 1C6, Canada. EM shetzinger@geomar.de RI Jacob, Dorrit/F-8617-2010; Halfar, Jochen/C-7317-2014; Zack, Thomas/K-7228-2013; Hetzinger, Steffen/B-5778-2016 OI Jacob, Dorrit/0000-0003-4744-6627; Zack, Thomas/0000-0003-4747-4134; FU Alexander von Humboldt Foundation; Natural Sciences and Engineering Research Council of Canada Discovery Grant; Canadian Foundation for Climate and Atmospheric Science Grant; Canadian Foundation for Innovation and Research and Ontario Research Fund Grant FX We thank B. Williams for discussion and helpful comments. We also thank B. Hooper for support during field work and G. Gamboa and A. Omar for lab assistance. This research was funded by the Alexander von Humboldt Foundation (Feodor Lynen Fellowship to S.H.), a Natural Sciences and Engineering Research Council of Canada Discovery Grant, a Canadian Foundation for Climate and Atmospheric Science Grant, and a Canadian Foundation for Innovation and Research and Ontario Research Fund Grant (all J.H.). NR 58 TC 5 Z9 5 U1 2 U2 25 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 2045-2322 J9 SCI REP-UK JI Sci Rep PD MAY 2 PY 2013 VL 3 AR 1761 DI 10.1038/srep01761 PG 8 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 134UZ UT WOS:000318242000003 PM 23636135 ER PT J AU Coblentz, KE Van Bael, SA AF Coblentz, Kyle E. Van Bael, Sunshine A. TI Field colonies of leaf-cutting ants select plant materials containing low abundances of endophytic fungi SO ECOSPHERE LA English DT Article DE Atta colombica; fungal endophytes; interactions; mutualism; Neotropics; Panama; symbiosis ID ARGENTINE STEM WEEVIL; ATTA-CEPHALOTES; NEOTYPHODIUM ENDOPHYTES; HERBIVORY; PATHOGENS; INSECTS; GRASSES; FOREST; HOST; TREE AB Endophytic fungi live symbiotically in the tissues of plants. Although a large amount of evidence suggests a mutualistic role for vertically transmitted endophytic fungi in agronomic grasses, the role of horizontally transmitted endophytic fungi as mutualists has been challenged. Recent studies, however, have shown that horizontally transmitted endophytic fungi can act as mutualists to their plant hosts by providing defense against pathogens and defoliators. In particular, several experimental studies have shown that endophytic fungi interact negatively with leaf-cutting ants and their fungal cultivar, but these studies were performed under laboratory conditions. Using field colonies of Atta colombica in Central Panama, we measured the fungal endophyte content in the forage material of leaf-cutting ants and compared it to ambient endophyte levels. We then used the collected data to model the area of plant material containing endophytes that enters a mature colony daily. We found that mature colonies collect leaf material that is 20% lower in endophyte abundance than surrounding leaves. A similar pattern was observed for newly emerged colonies. Our model suggests that via ant foraging preferences, leaf-cutting ants reduce the possible area of material containing endophytes entering the colony by 33%. Our results provide further evidence for a negative interaction between leaf-cutting ants and horizontally transmitted endophytes, suggesting that fungal endophytes have a defensive role in tropical plants by influencing leaf-cutting ant foraging preferences. C1 [Coblentz, Kyle E.; Van Bael, Sunshine A.] Tulane Univ, Dept Ecol & Evolutionary Biol, New Orleans, LA 70118 USA. [Van Bael, Sunshine A.] Smithsonian Trop Res Inst, Balboa, Panama. RP Coblentz, KE (reprint author), Tulane Univ, Dept Ecol & Evolutionary Biol, 400 Lindy Boggs, New Orleans, LA 70118 USA. EM svanbael@tulane.edu FU NSF [DEB-0949602]; REU supplement [DEB-1207260] FX We thank several students, including Franz Brock-mann, Laura Avila-Segura, Dani Moore, and the members of the McGill NEO program Tropical Biology course (2009 and 2011) for collecting pilot data and discussing ideas about leaf-cutting ants and endophytes. For help in the field, we thank K. Mighell and A. Kudla. This work was funded by NSF DEB-0949602 to SAV and an REU supplement DEB-1207260. NR 47 TC 4 Z9 4 U1 0 U2 21 PU ECOLOGICAL SOC AMER PI WASHINGTON PA 1990 M STREET NW, STE 700, WASHINGTON, DC 20036 USA SN 2150-8925 J9 ECOSPHERE JI Ecosphere PD MAY PY 2013 VL 4 IS 5 AR UNSP 66 DI 10.1890/ES13-00012.1 PG 10 WC Ecology SC Environmental Sciences & Ecology GA 256KF UT WOS:000327308300015 ER PT J AU Rottgering, H van Weeren, R Bruggen, M Croston, J Hoeft, M Ogrean, G Barthel, P Best, P Bonafede, A Brunetti, G Cassano, R Chyzy, K Conway, J De Gasperin, F Ferrari, C Heald, G Jackson, N Jarvis, M Lehnert, M Macario, G Miley, G Orru, E Pizzo, R Rafferty, D Stroe, A Tasse, C van der Tol, S White, G Wise, M AF Rottgering, H. van Weeren, R. Brueggen, M. Croston, J. Hoeft, M. Ogrean, G. Barthel, P. Best, P. Bonafede, A. Brunetti, G. Cassano, R. Chyzy, K. Conway, J. De Gasperin, F. Ferrari, C. Heald, G. Jackson, N. Jarvis, M. Lehnert, M. Macario, G. Miley, G. Orru, E. Pizzo, R. Rafferty, D. Stroe, A. Tasse, C. van der Tol, S. White, G. Wise, M. CA LOFAR Collaboration TI The "Sausage" and "Toothbrush" clusters of galaxies and the prospects of LOFAR observations of clusters of galaxies SO ASTRONOMISCHE NACHRICHTEN LA English DT Article; Proceedings Paper CT Workshop on Galaxy Clusters as Giant Cosmic Laboratories CY MAY 21-23, 2012 CL Madrid, SPAIN DE galaxies: clusters: general; galaxies: clusters: individual(CIZA J2242.8+5301, 1RXS J0603.3+4214); telescopes ID CIZA J2242.8+5301; CALIBRATION; MERGERS AB LOFAR, the Low Frequency Radio Array, is a new pan-European radio telescope that is almost fully operational. One of its main drivers is to make deep images of the low frequency radio sky. To be able to do this a number of challenges need to be addressed. These include the high data rates, removal of radio frequency interference, calibration of the beams and correcting for the corrupting influence of the ionosphere. One of the key science goals is to study merger shocks, particle acceleration mechanisms and the structure of magnetic fields in nearby and distant merging clusters. Recent studies with the GMRT and WSRT radio telescopes of the "Sausage" and the "Toothbrush" clusters have given a very good demonstration of the power of radio observations to study merging clusters. Recently we discovered that both clusters contain relic and halo sources, large diffuse regions of radio emission not associated with individual galaxies. The 2 Mpc northern relic in the Sausage cluster displays highly aligned magnetic fields and and exhibits a strong spectral index gradient that is a consequence of cooling of the synchrotron emitting particles in the post-shock region. We have argued that these observations provide strong evidence that shocks in merging clusters are capable of accelerating particles. For the Toothbrush cluster we observe a puzzling linear relic that extends over 2 Mpc. The proposed scenario is that a triple-merger can lead to such a structure. With LOFAR's sensitivity it will not only be possible to trace much weaker shocks, but also to study those shocks due to merging clusters up to redshifts of at least one. (C) 2013 WILEY-VCH Verlag GmbH & Co. KGaA, Weinheim C1 [Rottgering, H.; Miley, G.; Rafferty, D.; Stroe, A.; van der Tol, S.] Sterrewacht Leiden, NL-2300 RA Leiden, Netherlands. [van Weeren, R.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. [Brueggen, M.; Ogrean, G.; Bonafede, A.; De Gasperin, F.] Univ Hamburg, Hamburger Sternwarte, D-21029 Hamburg, Germany. [Croston, J.] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England. [Hoeft, M.] Thuringer Landessternwarte, Tautenburg, Germany. [Barthel, P.] Univ Groningen, Kapteyn Inst, NL-9747 AD Groningen, Netherlands. [Best, P.] Royal Observ, Edinburgh EH9 3HJ, Midlothian, Scotland. [Brunetti, G.; Cassano, R.] Ist Radioastron, INAF, IT-40129 Bologna, Italy. [Chyzy, K.] Uniwersytetu Jagiellonskiego, Obserwatorium Astron, PL-30244 Krakow, Poland. [Conway, J.] Chalmers, Onsala Space Observ, SE-43992 Onsala, Sweden. [Ferrari, C.; Macario, G.] Univ Nice Sophia Antipolis, CNRS, Observ Cote Azur, Lab Lagrange,UMR7293, F-06300 Nice, France. [Heald, G.; Orru, E.; Pizzo, R.; Wise, M.] ASTRON, NL-7990 AA Dwingeloo, Netherlands. [Jarvis, M.] Univ Oxford Astrophys, Dept Phys, Oxford OX1 3RH, England. [Jarvis, M.] Univ Western Cape, Dept Phys, ZA-7535 Bellville, South Africa. [Jackson, N.] Univ Manchester, Jodrell Bank, Ctr Astrophys, Manchester M13 9PL, Lancs, England. [Lehnert, M.] Observ Paris, F-92195 Meudon, France. [Tasse, C.] Rhodes Univ, ZA-6140 Grahamstown, South Africa. [White, G.] Open Univ, Dept Phys & Astron, Milton Keynes MK7 6AA, Bucks, England. [White, G.] STFC Rutherford Appleton Lab, Space Sci & Technol Dept, Didcot OX11 0QX, Oxon, England. RP Rottgering, H (reprint author), Sterrewacht Leiden, POB 9513, NL-2300 RA Leiden, Netherlands. EM rottgering@strw.leidenuniv.nl OI Brunetti, Gianfranco/0000-0003-4195-8613; Cassano, Rossella/0000-0003-4046-0637; de Gasperin, Francesco/0000-0003-4439-2627; van Weeren, Reinout/0000-0002-0587-1660 FU Agence Nationale de la Recherche [ANR-09-JCJC-0001-01]; NASA [PF2-130104, NAS8-03060]; Chandra X-ray Center FX C. Ferrari and G. Macario acknowledge financial support by the "Agence Nationale de la Recherche" through grant ANR-09-JCJC-0001-01. R. van Weeren was supported for this work by NASA through Einstein Postdoctoral grant number PF2-130104 awarded by the Chandra X-ray Center, which is operated by the Smithsonian Astrophysical Observatory for NASA under contract NAS8-03060. NR 19 TC 2 Z9 2 U1 0 U2 6 PU WILEY-V C H VERLAG GMBH PI WEINHEIM PA POSTFACH 101161, 69451 WEINHEIM, GERMANY SN 0004-6337 EI 1521-3994 J9 ASTRON NACHR JI Astro. Nachr. PD MAY PY 2013 VL 334 IS 4-5 SI SI BP 333 EP 337 DI 10.1002/asna.201211847 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 237IF UT WOS:000325862000006 ER PT J AU Nulsen, PEJ McNamara, BR AF Nulsen, P. E. J. McNamara, B. R. TI AGN feedback in clusters: Shock and sound heating SO ASTRONOMISCHE NACHRICHTEN LA English DT Article; Proceedings Paper CT Workshop on Galaxy Clusters as Giant Cosmic Laboratories CY MAY 21-23, 2012 CL Madrid, SPAIN DE galaxies: clusters: general; galaxies: clusters: intracluster medium; galaxies: jets; intergalactic medium ID ACTIVE GALACTIC NUCLEI; LARGE-SCALE SHOCK; X-RAY CAVITIES; GALAXY CLUSTER; INTRACLUSTER MEDIUM; GASEOUS ATMOSPHERE; BLACK-HOLES; GAS; SIMULATIONS; M87 AB Observations support the view that feedback, in the form of radio outbursts from active nuclei in central galaxies, prevents catastrophic cooling of gas and rapid star formation in many groups and clusters of galaxies. Variations in jet power drive a succession of weak shocks that can heat regions close to the active galactic nuclei (AGN). On larger scales, shocks fade into sound waves. The Braginskii viscosity determines a well-defined sound damping rate in the weakly magnetised intracluster medium (ICM) that can provide sufficient heating on larger scales. It is argued that weak shocks and sound dissipation are the main means by which radio AGN heat the ICM, in which case, the power spectrum of AGN outbursts plays a central role in AGN feedback. (C) 2013 WILEY-VCH Verlag GmbH & Co. KGaA, Weinheim C1 [Nulsen, P. E. J.; McNamara, B. R.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [McNamara, B. R.] Univ Waterloo, Dept Phys & Astron, Waterloo, ON N2L 3G1, Canada. [McNamara, B. R.] Perimeter Inst Theoret Phys, Waterloo, ON, Canada. RP Nulsen, PEJ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM pnulsen@cfa.harvard.edu OI Nulsen, Paul/0000-0003-0297-4493 FU NASA [NAS8-03060] FX This work was supported by NASA grant NAS8-03060. NR 30 TC 7 Z9 7 U1 0 U2 1 PU WILEY-V C H VERLAG GMBH PI WEINHEIM PA POSTFACH 101161, 69451 WEINHEIM, GERMANY SN 0004-6337 EI 1521-3994 J9 ASTRON NACHR JI Astro. Nachr. PD MAY PY 2013 VL 334 IS 4-5 SI SI BP 386 EP 389 DI 10.1002/asna.201211863 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 237IF UT WOS:000325862000018 ER PT J AU Birzan, L Rafferty, DA Nulsen, PEJ McNamara, BR Rottgering, HJA Wise, MW AF Birzan, L. Rafferty, D. A. Nulsen, P. E. J. McNamara, B. R. Rottgering, H. J. A. Wise, M. W. TI The duty cycle of the radio mode feedback SO ASTRONOMISCHE NACHRICHTEN LA English DT Article; Proceedings Paper CT Workshop on Galaxy Clusters as Giant Cosmic Laboratories CY MAY 21-23, 2012 CL Madrid, SPAIN DE cooling flows; galaxies: clusters: intracluster medium; radio continuum: galaxies; X-rays: galaxies: clusters ID FLUX-LIMITED SAMPLE; X-RAY CAVITIES; GALAXY CLUSTERS; COOLING FLOWS; CORE; GAS; THRESHOLD; PROFILES; AGN AB The Chandra X-ray Observatory has revealed X-ray bubbles in the intracluster medium (ICM) of many nearby clusters, which are thought to be created by the central active galactic nucleus (AGN). However, the duty cycle of such AGN outbursts is not well understood. In order to further understand how cooling is balanced by bubble heating we studied complete samples of cooling flow clusters (from the Brightest 55 clusters of galaxies sample, B55, and the HIghest X-ray FLUx Galaxy Cluster Sample, HIFLUGCS). We found that there is a radio luminosity cut-off of 2.5x10(30) erg s(-1) Hz(-1) for the cooling flow clusters. Furthermore, we find a duty cycle for radio mode feedback, the fraction of time that a system possesses bubbles inflated by its central radio source, of greater than or similar to 69% for the B55 sample and greater than or similar to 63% for the HIFLUGCS sample. These duty cycles are lower limits since some bubbles are likely missed in existing images. We used simulations to constrain the bubble power that might be present and remain undetected in the cooling flow systems without detected bubbles. Among theses systems, almost all could have significant bubble power. Therefore, our results imply that the duty cycle of AGN outbursts with the potential to heat the gas significantly in cooling flow clusters is at least 60% and could approach 100 %. (C) 2013 WILEY-VCH Verlag GmbH & Co. KGaA, Weinheim C1 [Birzan, L.; Rafferty, D. A.; Rottgering, H. J. A.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [Nulsen, P. E. J.; McNamara, B. R.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [McNamara, B. R.] Univ Waterloo, Dept Phys & Astron, Waterloo, ON N2L 2G1, Canada. [McNamara, B. R.] Perimeter Inst Theoret Phys, Waterloo, ON N2L 2Y5, Canada. [Wise, M. W.] Netherlands Inst Radio Astron ASTRON, NL-7990 AA Dwingeloo, Netherlands. RP Birzan, L (reprint author), Leiden Univ, Leiden Observ, POB 9513, NL-2300 RA Leiden, Netherlands. EM birzan@strw.leidenuniv.nl OI Nulsen, Paul/0000-0003-0297-4493 NR 33 TC 3 Z9 3 U1 0 U2 1 PU WILEY-V C H VERLAG GMBH PI WEINHEIM PA POSTFACH 101161, 69451 WEINHEIM, GERMANY SN 0004-6337 EI 1521-3994 J9 ASTRON NACHR JI Astro. Nachr. PD MAY PY 2013 VL 334 IS 4-5 SI SI BP 390 EP 393 DI 10.1002/asna.201211864 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 237IF UT WOS:000325862000019 ER PT J AU Grissom, CA Grabow, N Riley, CS Charola, AE AF Grissom, Carol A. Grabow, Nicole Riley, Corey Smith Charola, A. Elena TI EVALUATION OF COATING PERFORMANCE ON SILVER EXPOSED TO HYDROGEN SULFIDE SO JOURNAL OF THE AMERICAN INSTITUTE FOR CONSERVATION LA English DT Article DE silver; coatings; hydrogen sulfide; thickness; gloss; colorimetry AB Twelve coatings applied to sterling silver coupons were subjected to high levels of hydrogen sulfide to test their effectiveness in preventing tarnish in indoor environments. Silver coupons were assessed over the course of the experiment using visual observation, image analysis of digital photographs, gloss measurement, and colorimetry. Acrysol WS-24, Agateen Air Dry Lacquer No. 27, HMG Heat and Waterproof Adhesive, and PVAc AYAT generally performed best. Mowiol 28-99 performed very well on some areas but was mediocre otherwise. Butvar B-98 and Acryloid B-48N were generally less effective in retarding tarnish. Acryloid B-72 and Butvar B-76 performed less well. Aquazol 500, Aquazol 500 topped with Renaissance Wax, and Renaissance Wax were least effective. Coating thickness proved to be a significant factor in coating performance. C1 [Grissom, Carol A.; Charola, A. Elena] Smithsonian Inst, Museum Conservat Inst, Suitland, MD 20746 USA. [Grabow, Nicole] Midwest Art Conservat Ctr, Minneapolis, MN 55404 USA. [Riley, Corey Smith] Caryatid Conservat Serv, Miami, FL USA. RP Grissom, CA (reprint author), Smithsonian Inst, Museum Conservat Inst, 4210 Silver Hill Rd, Suitland, MD 20746 USA. EM grissomc@si.edu; ngrabow@preserveart.org; jcoreys@gmail.com; Charola_ae@yahoo.com NR 18 TC 2 Z9 2 U1 1 U2 7 PU MANEY PUBLISHING PI LEEDS PA STE 1C, JOSEPHS WELL, HANOVER WALK, LEEDS LS3 1AB, W YORKS, ENGLAND SN 0197-1360 EI 1945-2330 J9 J AM INST CONSERV JI J. Am. Inst. Conserv. PD MAY PY 2013 VL 52 IS 2 BP 82 EP 96 DI 10.1179/0197136013Z.0000000007 PG 15 WC Humanities, Multidisciplinary SC Arts & Humanities - Other Topics GA 227IJ UT WOS:000325105600002 ER PT J AU Campbell, JE Fourqurean, JW AF Campbell, Justin E. Fourqurean, James W. TI Mechanisms of bicarbonate use influence the photosynthetic carbon dioxide sensitivity of tropical seagrasses SO LIMNOLOGY AND OCEANOGRAPHY LA English DT Article ID INORGANIC CARBON; ZOSTERA-MARINA; THALASSIA-TESTUDINUM; OCEAN ACIDIFICATION; CYMODOCEA-NODOSA; ULVA-LACTUCA; IN-SITU; CO2; METABOLISM; LIGHT AB The photosynthetic bicarbonate (HCO3-) use properties of three widely distributed tropical seagrasses were compared using a series of laboratory experiments. Photosynthetic rates of Thalassia testudinum, Halodule wrightii, and Syringodium filiforme were monitored in an enclosed chamber while being subjected to shifts in pH and dissolved inorganic carbon. Specific mechanisms of seagrass HCO3- use were compared by examining the photosynthetic effects of the carbonic anhydrase inhibitor acetazolamide (AZ). All seagrasses increased photosynthetic rates with reduced pH, suggesting a large effect of dissolved aqueous carbon dioxide (CO2(aq)). However, there was considerable interspecific variation in pH response. T. testudinum was highly sensitive, increasing photosynthetic rates by 100% as the pH was reduced from 8.2 to 7.4, whereas rates in H. wrightii and S. filiforme increased by only 20% over a similar range, and displayed prominent photosynthetic plateaus, indicating an increased capacity for HCO3- use. Additional incubations that manipulated [HCO3-] under constant [CO2(aq)] support these findings, as only H. wrightii and S. filiforme increased photosynthetic rates with increasing [HCO3-]. T. testudinum responded to AZ addition, indicating that carbonic anhydrase enzymes facilitate limited HCO3- use. H. wrightii and S. filiforme showed no response to AZ, suggesting alternate, more efficient mechanisms of HCO3- use. Estimated kinetic parameters, K-s(CO2) and V-max, revealed interspecific variation and further support these conclusions. Variation in photosynthetic pH responses and AZ sensitivity indicate distinctions in the carbon use properties of seagrasses exposed to similar environmental conditions. These results suggest that not all seagrasses will similarly respond to future increases in CO2(aq) availability. Attention towards potential shifts in competitive interactions within multispecific seagrass beds is warranted. C1 Florida Int Univ, Dept Biol Sci, Marine Sci Program, N Miami, FL USA. Florida Int Univ, Southeast Environm Res Ctr, N Miami, FL USA. RP Campbell, JE (reprint author), Smithsonian Marine Stn, Ft Pierce, FL USA. EM campbellju@si.edu RI Fourqurean, James/B-4606-2008 OI Fourqurean, James/0000-0002-0811-8500 FU Dissertation Evidence Acquisition Fellowship; Florida International University (FIU); Florida Coastal Everglades Long-Term Ecological Research Program (National Science Foundation-Division of biological infrastructure) [0620409] FX A special thanks to Michael Durako, who provided valuable insight on the experimental methods and final manuscript. Two anonymous reviewers also improved the quality of this work. Support for this project was provided by a Dissertation Evidence Acquisition Fellowship awarded by Florida International University (FIU) and by the Florida Coastal Everglades Long-Term Ecological Research Program (National Science Foundation-Division of biological infrastructure grant-0620409). This is Contribution Number 594 from the Southeast Environmental Research Center at FIU. NR 38 TC 9 Z9 9 U1 2 U2 34 PU AMER SOC LIMNOLOGY OCEANOGRAPHY PI WACO PA 5400 BOSQUE BLVD, STE 680, WACO, TX 76710-4446 USA SN 0024-3590 J9 LIMNOL OCEANOGR JI Limnol. Oceanogr. PD MAY PY 2013 VL 58 IS 3 BP 839 EP 848 DI 10.4319/lo.2013.58.3.0839 PG 10 WC Limnology; Oceanography SC Marine & Freshwater Biology; Oceanography GA 192NG UT WOS:000322491100007 ER PT J AU Solomon, CT Bruesewitz, DA Richardson, DC Rose, KC Van de Bogert, MC Hanson, PC Kratz, TK Larget, B Adrian, R Babin, BL Chiu, CY Hamilton, DP Gaiser, EE Hendricks, S Istvanovics, V Laas, A O'Donnell, DM Pace, ML Ryder, E Staehr, PA Torgersen, T Vanni, MJ Weathers, KC Zhu, GW AF Solomon, Christopher T. Bruesewitz, Denise A. Richardson, David C. Rose, Kevin C. Van de Bogert, Matthew C. Hanson, Paul C. Kratz, Timothy K. Larget, Bret Adrian, Rita Babin, Brenda Leroux Chiu, Chih-Yu Hamilton, David P. Gaiser, Evelyn E. Hendricks, Susan Istvanovics, Vera Laas, Alo O'Donnell, David M. Pace, Michael L. Ryder, Elizabeth Staehr, Peter A. Torgersen, Thomas Vanni, Michael J. Weathers, Kathleen C. Zhu, Guangwei TI Ecosystem respiration: Drivers of daily variability and background respiration in lakes around the globe SO LIMNOLOGY AND OCEANOGRAPHY LA English DT Article ID DISSOLVED ORGANIC-CARBON; NET HETEROTROPHY; TEMPERATE LAKES; WATER LAKE; METABOLISM; OXYGEN; DYNAMICS; TERRESTRIAL; PATTERNS; BALANCE AB We assembled data from a global network of automated lake observatories to test hypotheses regarding the drivers of ecosystem metabolism. We estimated daily rates of respiration and gross primary production (GPP) for up to a full year in each lake, via maximum likelihood fits of a free-water metabolism model to continuous high-frequency measurements of dissolved oxygen concentrations. Uncertainties were determined by a bootstrap analysis, allowing lake-days with poorly constrained rate estimates to be down-weighted in subsequent analyses. GPP and respiration varied considerably among lakes and at seasonal and daily timescales. Mean annual GPP and respiration ranged from 0.1 to 5.0 mg O-2 L-1 d(-1) and were positively related to total phosphorus but not dissolved organic carbon concentration. Within lakes, significant day-to-day differences in respiration were common despite large uncertainties in estimated rates on some lake-days. Daily variation in GPP explained 5% to 85% of the daily variation in respiration after temperature correction. Respiration was tightly coupled to GPP at a daily scale in oligotrophic and dystrophic lakes, and more weakly coupled in mesotrophic and eutrophic lakes. Background respiration ranged from 0.017 to 2.1 mg O-2 L-1 d(-1) and was positively related to indicators of recalcitrant allochthonous and autochthonous organic matter loads, but was not clearly related to an indicator of the quality of allochthonous organic matter inputs. C1 [Solomon, Christopher T.] McGill Univ, Dept Nat Resource Sci, Ste Anne De Bellevue, PQ, Canada. [Bruesewitz, Denise A.] Univ Texas, Inst Marine Sci, Port Aransas, TX USA. [Richardson, David C.] SUNY Coll New Paltz, Dept Biol, New Paltz, NY USA. [Rose, Kevin C.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. [Van de Bogert, Matthew C.; Hanson, Paul C.] Univ Wisconsin, Ctr Limnol, Madison, WI 53706 USA. [Kratz, Timothy K.] Univ Wisconsin, Ctr Limnol, Trout Lake Stn, Boulder Junction, CO USA. [Larget, Bret] Univ Wisconsin, Dept Bot, Madison, WI USA. [Larget, Bret] Univ Wisconsin, Dept Stat, Madison, WI 53706 USA. [Adrian, Rita] Leibniz Inst Freshwater Ecol & Inland Fisheries, Berlin, Germany. [Babin, Brenda Leroux] Louisiana State Univ, Dept Oceanog & Coastal Sci, Baton Rouge, LA 70803 USA. [Chiu, Chih-Yu] Acad Sinica, Biodivers Res Ctr, Taipei 115, Taiwan. [Hamilton, David P.] Univ Waikato, Environm Res Inst, Hamilton, New Zealand. [Gaiser, Evelyn E.] Florida Int Univ, Dept Biol Sci, Miami, FL 33199 USA. [Gaiser, Evelyn E.] Florida Int Univ, Southeast Environm Res Ctr, Miami, FL 33199 USA. [Hendricks, Susan] Murray State Univ, Hancock Biol Stn, Murray, KY 42071 USA. [Istvanovics, Vera] Hungarian Acad Sci, Water Qual Management Grp, Budapest, Hungary. [Laas, Alo] Estonian Univ Life Sci, Inst Agr & Environm Sci, Ctr Limnol, Tartumaa, Estonia. [O'Donnell, David M.] Upstate Freshwater Inst, Syracuse, NY USA. [Pace, Michael L.] Univ Virginia, Dept Environm Sci, Charlottesville, VA 22903 USA. [Ryder, Elizabeth] Inst Marine, Newport, County Mayo, Ireland. [Staehr, Peter A.] Aarhus Univ, Dept Biosci, Roskilde, Denmark. [Torgersen, Thomas] Univ Connecticut, Dept Marine Sci, Groton, CT 06340 USA. [Vanni, Michael J.] Miami Univ, Dept Zool, Oxford, OH 45056 USA. [Vanni, Michael J.] Miami Univ, Grad Program Ecol Evolut & Environm Biol, Oxford, OH 45056 USA. [Weathers, Kathleen C.] Cary Inst Ecosyst Studies, Millbrook, NY USA. [Zhu, Guangwei] Chinese Acad Sci, Nanjing Inst Geog & Limnol, Nanjing, Peoples R China. RP Solomon, CT (reprint author), McGill Univ, Dept Nat Resource Sci, Ste Anne De Bellevue, PQ, Canada. EM chris.solomon@mcgill.ca RI Chen, Mei-Chu/C-7532-2014; Solomon, Chris/E-6284-2014; Staehr, Peter /J-3693-2013; Laas, Alo/G-7992-2016; OI Chen, Mei-Chu/0000-0003-0997-2298; Solomon, Chris/0000-0002-2850-4257; Laas, Alo/0000-0002-4801-0377; Pace, Michael/0000-0001-5945-6131 FU Research Coordination Network grant from the U.S. National Science Foundation (NSF); Gordon and Betty Moore Foundation; U.S. NSF Integrative Graduate Education and Research Traineeship [0903560]; Long-Term Research in Environmental Biology [0743192]; Archbold Biological Station; U.S. NSF [0446017, 0639229, 0822700, OCI-0936174]; Gordon and Betty Moore Foundation [1182, 2735]; Irish Marine Institute; Danish Centre for Lake Restoration and Danish Council for Independent Research, Natural Sciences [272-05-0277, 10-085238]; Hancock Biological Station long-term monitoring program; U.S. NSF Experimental Program to Stimulate Competitive Research [0918856]; long-term research program at the Leibniz-Instutite of Freshwater Ecology and Inland Fisheries in Berlin, Germany; U.S. Environmental Protection Agency, Environmental Monitoring for Public Access and Community Tracking; Louisiana Universities Marine Consortium, Environmental Monitoring Program; New Zealand Ministry of Science and Innovation [UOWX0505]; Bay of Plenty Regional Council; Lake Sunapee Protective Association; Division of Biological Infrastructure [0434684, 0842125]; Estonian Science Foundation [8729]; Estonian target funding project [SF 0170011508]; Academia Sinica FX Network-level activities of GLEON are funded in part by a Research Coordination Network grant from the U.S. National Science Foundation (NSF). C.T.S. was funded in part by a grant from the Gordon and Betty Moore Foundation. Financial and logistical support for the individual observatories contributing to this analysis came from local and national sources including: U.S. NSF Integrative Graduate Education and Research Traineeship 0903560 and Long-Term Research in Environmental Biology 0743192; Archbold Biological Station; U.S. NSF 0446017, 0639229, and 0822700 and Gordon and Betty Moore Foundation 1182 and 2735; Irish Marine Institute; Danish Centre for Lake Restoration and Danish Council for Independent Research, Natural Sciences 272-05-0277 and 10-085238; Hancock Biological Station long-term monitoring program and U.S. NSF Experimental Program to Stimulate Competitive Research 0918856; the long-term research program at the Leibniz-Instutite of Freshwater Ecology and Inland Fisheries in Berlin, Germany; U.S. Environmental Protection Agency, Environmental Monitoring for Public Access and Community Tracking; Louisiana Universities Marine Consortium, Environmental Monitoring Program; New Zealand Ministry of Science and Innovation, contract UOWX0505 and Bay of Plenty Regional Council; Lake Sunapee Protective Association and U.S. NSF OCI-0936174, Division of Biological Infrastructure 0434684, and Emerging Frontiers 0842125; Estonian Science Foundation 8729 and Estonian target funding project SF 0170011508; and Academia Sinica. NR 48 TC 63 Z9 65 U1 11 U2 116 PU AMER SOC LIMNOLOGY OCEANOGRAPHY PI WACO PA 5400 BOSQUE BLVD, STE 680, WACO, TX 76710-4446 USA SN 0024-3590 J9 LIMNOL OCEANOGR JI Limnol. Oceanogr. PD MAY PY 2013 VL 58 IS 3 BP 849 EP 866 DI 10.4319/lo.2013.58.3.0849 PG 18 WC Limnology; Oceanography SC Marine & Freshwater Biology; Oceanography GA 192NG UT WOS:000322491100008 ER PT J AU Read, JS Rose, KC AF Read, Jordan S. Rose, Kevin C. TI Physical responses of small temperate lakes to variation in dissolved organic carbon concentrations SO LIMNOLOGY AND OCEANOGRAPHY LA English DT Article ID THERMAL STRUCTURE; WATER CLARITY; SHIELD LAKES; CLIMATE; SIZE; RADIATION; ABUNDANCE; PLANKTON; TRENDS; EXPORT AB We used a mechanistic physical model to examine the effect of variability in dissolved organic carbon (DOC) concentrations on the physical properties of small temperate lakes. The model was validated on eight small (6 X 10(-4) to 3.8 X 10(-2) km(2)) lakes in Wisconsin and Michigan, with a standard error < 1 degrees C for seven of eight lakes. Attenuation of photosynthetically active radiation (400-700 nm) in these lakes was regulated by DOC concentrations and was important in the vertical structuring of water temperatures. Heat exchange below the surface mixed layer was near the molecular rate, increasing the importance of water clarity as a control on the heat content of deeper waters. To understand the thermal effects of changing DOC concentrations, we applied scenarios of a 50% increase and 50% decrease in DOC concentrations for one lake (Trout Bog) and found water temperatures to vary in response, with the seasonally averaged temperatures in the increased DOC scenario being > 2 degrees C colder than the reduced scenario. We found a nonlinear relationship between DOC and temperature, with clearer (lower DOC) simulations being more sensitive to climate variability, suggesting that DOC may act as a buffer against a warming climate. Our model showed that DOC also influenced epilimnetic depths, as nocturnal mixing (related to the vertical partitioning of heat) was more important than wind-driven mixing. Small lakes are globally important regulators of biogeochemical cycles and are structurally different from larger lakes. Important feedbacks to physical processes must be accounted for when understanding the effects of changing DOC and climate on small lakes. C1 [Read, Jordan S.] Univ Wisconsin, Dept Civil & Environm Engn, Madison, WI 53706 USA. [Rose, Kevin C.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. RP Read, JS (reprint author), US Geol Survey, Ctr Integrated Data Analyt, Middleton, WI USA. EM jread@usgs.gov OI Read, Jordan/0000-0002-3888-6631 FU Division of Environmental Biology and Molecular and Cellular Biology [0822700, 0702395]; Environmental Aquatic Resource Sensing (EARS) Integrative Graduate Education and Research Traineeship (IGERT) program; NSF Division of Graduate Education grant [0903560]; Smithsonian Institution postdoctoral fellowship; EARS IGERT; Gordon and Betty Moore Foundation [1182] FX J.S.R. was supported by National Science Foundation (NSF) North Temperate Lakes Long-Term Ecological Research grants from the Division of Environmental Biology and Molecular and Cellular Biology (grants 0822700 and 0702395, respectively). These grants also funded buoys on Crystal Bog, North Sparkling Bog, Trout Bog, and Mouser Bog. K.C.R. was supported by the Environmental Aquatic Resource Sensing (EARS) Integrative Graduate Education and Research Traineeship (IGERT) program, NSF Division of Graduate Education grant 0903560, and a Smithsonian Institution postdoctoral fellowship. The EARS IGERT grant supplied buoys for Timber and Jekl Bogs. This research could not have been completed without the intellectual and logistical support of the C. Williamson Lab of Miami University and the support, discussion, and/or fieldwork of K. McMahon, E. Stanley, L. Winslow, P. Hanson, E. K. Read, A. Shade, T. Meinke, K. Morrison, S. Yeo, and C. Watras. This article was improved by incorporating valuable feedback received at the 11th Global Lakes Ecological Observatory (GLEON) meeting, where travel and lodging costs for JSR and KCR were covered by the Gordon and Betty Moore Foundation (award 1182). We thank J. Cole and S. Carpenter from the Tropic Cascade Project for providing buoy data from Peter and Ward Lakes and M. Pace and R. Batt for thoughtful discussion on this topic. C. Williamson and two anonymous reviewers helped improve earlier versions of this article. NR 34 TC 35 Z9 35 U1 3 U2 41 PU AMER SOC LIMNOLOGY OCEANOGRAPHY PI WACO PA 5400 BOSQUE BLVD, STE 680, WACO, TX 76710-4446 USA SN 0024-3590 J9 LIMNOL OCEANOGR JI Limnol. Oceanogr. PD MAY PY 2013 VL 58 IS 3 BP 921 EP 931 DI 10.4319/lo.2013.58.3.0921 PG 11 WC Limnology; Oceanography SC Marine & Freshwater Biology; Oceanography GA 192NG UT WOS:000322491100013 ER PT J AU Denevi, BW Ernst, CM Meyer, HM Robinson, MS Murchie, SL Whitten, JL Head, JW Watters, TR Solomon, SC Ostrach, LR Chapman, CR Byrne, PK Klimczak, C Peplowski, PN AF Denevi, Brett W. Ernst, Carolyn M. Meyer, Heather M. Robinson, Mark S. Murchie, Scott L. Whitten, Jennifer L. Head, James W. Watters, Thomas R. Solomon, Sean C. Ostrach, Lillian R. Chapman, Clark R. Byrne, Paul K. Klimczak, Christian Peplowski, Patrick N. TI The distribution and origin of smooth plains on Mercury SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article DE Mercury; Volcanism; Smooth Plains ID 1ST MESSENGER FLYBY; CALORIS BASIN; TERRESTRIAL PLANETS; ERUPTION CONDITIONS; GLOBAL PERSPECTIVE; MARE VOLCANISM; IMPACT MELT; MARINER 10; LUNAR; STRATIGRAPHY AB Orbital images from the MESSENGER spacecraft show that similar to 27% of Mercury's surface is covered by smooth plains, the majority (>65%) of which are interpreted to be volcanic in origin. Most smooth plains share the spectral characteristics of Mercury's northern smooth plains, suggesting they also share their magnesian alkali-basalt-like composition. A smaller fraction of smooth plains interpreted to be volcanic in nature have a lower reflectance and shallower spectral slope, suggesting more ultramafic compositions, an inference that implies high temperatures and high degrees of partial melting in magma source regions persisted through most of the duration of smooth plains formation. The knobby and hummocky plains surrounding the Caloris basin, known as Odin-type plains, occupy an additional 2% of Mercury's surface. The morphology of these plains and their color and stratigraphic relationships suggest that they formed as Caloris ejecta, although such an origin is in conflict with a straightforward interpretation of crater size-frequency distributions. If some fraction is volcanic, this added area would substantially increase the abundance of relatively young effusive deposits inferred to have more mafic compositions. Smooth plains are widespread on Mercury, but they are more heavily concentrated in the north and in the hemisphere surrounding Caloris. No simple relationship between plains distribution and crustal thickness or radioactive element distribution is observed. A likely volcanic origin for some older terrain on Mercury suggests that the uneven distribution of smooth plains may indicate differences in the emplacement age of large-scale volcanic deposits rather than differences in crustal formational process. C1 [Denevi, Brett W.; Ernst, Carolyn M.; Meyer, Heather M.; Murchie, Scott L.; Peplowski, Patrick N.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. [Robinson, Mark S.; Ostrach, Lillian R.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ USA. [Whitten, Jennifer L.; Head, James W.] Brown Univ, Dept Geol Sci, Providence, RI 02912 USA. [Watters, Thomas R.] Smithsonian Inst, Ctr Earth & Planetary Studies, Natl Air & Space Museum, Washington, DC 20560 USA. [Solomon, Sean C.; Byrne, Paul K.; Klimczak, Christian] Carnegie Inst Sci, Dept Terr Magnetism, Washington, DC USA. [Solomon, Sean C.] Columbia Univ, Lamont Doherty Earth Observ, Palisades, NY USA. [Chapman, Clark R.] SW Res Inst, Boulder, CO USA. RP Denevi, BW (reprint author), Johns Hopkins Univ, Appl Phys Lab, Dept Space, 11100 Johns Hopkins Rd, Laurel, MD 20723 USA. EM Brett.Denevi@jhuapl.edu RI Ernst, Carolyn/I-4902-2012; Denevi, Brett/I-6502-2012; Murchie, Scott/E-8030-2015; Peplowski, Patrick/I-7254-2012 OI Denevi, Brett/0000-0001-7837-6663; Murchie, Scott/0000-0002-1616-8751; Peplowski, Patrick/0000-0001-7154-8143 FU NASA Discovery Program [NAS5-97271, NASW-00002] FX We thank Aileen Yingst and an anonymous reviewer for constructive reviews. This research has made use of the Integrated Software for Imagers and Spectometers (ISIS) of the U.S. Geological Survey. The MESSENGER project is supported by the NASA Discovery Program under contracts NAS5-97271 to The Johns Hopkins University Applied Physics Laboratory and NASW-00002 to the Carnegie Institution of Washington. NR 78 TC 70 Z9 71 U1 1 U2 16 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9097 EI 2169-9100 J9 J GEOPHYS RES-PLANET JI J. Geophys. Res.-Planets PD MAY PY 2013 VL 118 IS 5 BP 891 EP 907 DI 10.1002/jgre.20075 PG 17 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 224TN UT WOS:000324912400002 ER PT J AU McFarlin, SC Barks, SK Tocheri, MW Massey, JS Eriksen, AB Fawcett, KA Stoinski, TS Hof, PR Bromage, TG Mudakikwa, A Cranfield, MR Sherwood, CC AF McFarlin, Shannon C. Barks, Sarah K. Tocheri, Matthew W. Massey, Jason S. Eriksen, Amandine B. Fawcett, Katie A. Stoinski, Tara S. Hof, Patrick R. Bromage, Timothy G. Mudakikwa, Antoine Cranfield, Michael R. Sherwood, Chet C. TI Early Brain Growth Cessation in Wild Virunga Mountain Gorillas (Gorilla beringei beringei) SO AMERICAN JOURNAL OF PRIMATOLOGY LA English DT Article DE brain growth; mountain gorillas; life history ID FATTY-ACID-COMPOSITION; LIFE-HISTORY; HUMAN-EVOLUTION; ENDOCRANIAL VOLUMES; MATERNAL INVESTMENT; NATIONAL-PARK; AFRICAN APES; TOOL-USE; PRIMATE; CHIMPANZEES AB Understanding the life history correlates of ontogenetic differences in hominoid brain growth requires information from multiple species. At present, however, data on how brain size changes over the course of development are only available from chimpanzees and modern humans. In this study, we examined brain growth in wild Virunga mountain gorillas using data derived from necropsy reports (N = 34) and endocranial volume (EV) measurements (N = 86). The youngest individual in our sample was a 10-day-old neonatal male with a brain mass of 208 g, representing 42% of the adult male average. Our results demonstrate that Virunga mountain gorillas reach maximum adult-like brain mass by 3-4 years of age; adult-sized EV is reached by the time the first permanent molars emerge. This is in contrast to the pattern observed in chimpanzees, which despite their smaller absolute brain size, reportedly attain adult brain mass approximately 1 year later than Virunga mountain gorillas. Our findings demonstrate that brain growth is completed early in Virunga mountain gorillas compared to other great apes studied thus far, in a manner that appears to be linked with other life history characteristics of this population. Am. J. Primatol. 75:450-463, 2013. (c) 2012 Wiley Periodicals, Inc. C1 [McFarlin, Shannon C.; Barks, Sarah K.; Sherwood, Chet C.] George Washington Univ, Dept Anthropol, Ctr Adv Study Hominid Paleobiol, Washington, DC 20052 USA. [Tocheri, Matthew W.] Smithsonian Inst, Dept Anthropol, Natl Museum Nat Hist, Human Origins Program, Washington, DC 20560 USA. [Massey, Jason S.] Univ Minnesota, Dept Anthropol, Minneapolis, MN USA. [Eriksen, Amandine B.] Univ Indianapolis, Archeol & Forens Lab, Indianapolis, IN 46227 USA. [Fawcett, Katie A.; Stoinski, Tara S.] Dian Fossey Gorilla Fund Int, Atlanta, GA USA. [Stoinski, Tara S.] Zoo Atlanta, Atlanta, GA USA. [Hof, Patrick R.] Mt Sinai Sch Med, Fishberg Dept Neurosci, New York, NY USA. [Hof, Patrick R.] Mt Sinai Sch Med, Friedman Brain Inst, New York, NY USA. [Bromage, Timothy G.] NYU, Coll Dent, Dept Biomat & Biomimet, New York, NY USA. [Mudakikwa, Antoine] Rwanda Dev Board, Dept Tourism & Conservat, Kigali, Rwanda. [Cranfield, Michael R.] Univ Calif Davis, Sch Vet Med, Mt Gorilla Vet Program, Davis, CA 95616 USA. RP McFarlin, SC (reprint author), George Washington Univ, Dept Anthropol, Ctr Adv Study Hominid Paleobiol, Washington, DC 20052 USA. EM mcfarlin@gwu.edu; sherwood@gwu.edu OI Tocheri, Matthew/0000-0001-7600-8998 FU National Science Foundation [BCS-0827531, BCS-0964944]; Leakey Foundation; James S. McDonnell Foundation [22002078, 220020293]; George Washington University Academic Excellence; Max Planck Society; Alexander von Foundation FX Contract grant sponsor: National Science Foundation; Contract grant numbers: BCS-0827531, BCS-0964944; Contract grant sponsor: Leakey Foundation; Contract grant sponsor: James S. McDonnell Foundation; Contract grant numbers: 22002078, 220020293; Contract grant sponsor: The George Washington University Academic Excellence support to CASHP; Contract grant sponsor: Max Planck Society; Contract grant sponsor: Alexander von Foundation. NR 96 TC 13 Z9 13 U1 3 U2 25 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0275-2565 EI 1098-2345 J9 AM J PRIMATOL JI Am. J. Primatol. PD MAY PY 2013 VL 75 IS 5 SI SI BP 450 EP 463 DI 10.1002/ajp.22100 PG 14 WC Zoology SC Zoology GA 115LY UT WOS:000316814900007 PM 23208801 ER PT J AU Freeman, RL Dattilo, BF Morse, A Blair, M Felton, S Pojeta, J AF Freeman, Rebecca L. Dattilo, Benjamin F. Morse, Aaron Blair, Michael Felton, Steve Pojeta, John, Jr. TI THE "CURSE OF RAFINESQUINA:" NEGATIVE TAPHONOMIC FEEDBACK EXERTED BY STROPHOMENID SHELLS ON STORM-BURIED LINGULIDS IN THE CINCINNATIAN SERIES (KATIAN, ORDOVICIAN) OF OHIO SO PALAIOS LA English DT Article ID BRACHIOPOD GLOTTIDIA-PYRAMIDATA; PALEOECOLOGICAL SIGNIFICANCE; ECOSYSTEM ENGINEERS; FOSSIL; MIDDLE; BEDS; REGION; USA; INVERTEBRATES; INARTICULATA AB Thousands of lingulid brachiopods were found clustered beneath hundreds of individual valves of the strophomenid brachiopod Rafinesquina in the Upper Ordovician of Ohio. This association suggested a relationship between the two brachiopods, but the nature of this relationship was unclear. We utilized serial thin sectioning to examine these brachiopods and to determine the origin of the bed in which they were found. Sedimentary structures, mixed taphonomies, and stratigraphic and paleogeographic setting suggest that the lingulids occupied a hiatal concentration that had previously been reworked, but not significantly transported, by tropical storms. The final burial event was a storm that exhumed living lingulids along with disarticulated Rafinesquina shells from the same sediments. Neither living nor dead shells were transported, but were reworked locally, then reburied together. The lingulids then burrowed upward to escape, but most were trapped by the concave-downward Rafinesquina shells that had been redeposited above them. This finding offers the first documented example of negative ecosystem engineering and taphonomic feedback in the fossil record, as well as the oldest documented lingulid escape traces. It also suggests that taphonomic feedback can be subdivided into live-dead interactions that occur under normal background depositional conditions and those that occur during periodic short-lived sediment-reworking events, such as storms and tsunamis. C1 [Freeman, Rebecca L.] Univ Kentucky, Dept Earth & Environm Sci, Lexington, KY 40506 USA. [Dattilo, Benjamin F.; Blair, Michael] Indiana Univ Purdue Univ, Dept Geosci, Ft Wayne, IN 46805 USA. [Morse, Aaron] Ball State Univ, Dept Geol Sci, Muncie, IN 47306 USA. [Pojeta, John, Jr.] US Geol Survey, Dept Paleobiol, Museum Nat Hist, Smithsonian Inst, Washington, DC 20013 USA. RP Freeman, RL (reprint author), Univ Kentucky, Dept Earth & Environm Sci, Lexington, KY 40506 USA. EM rebecca.freeman@uky.edu; dattilob@ipfw.edu; apmorse@bsu.edu; pojetaj@si.edu FU University of Kentucky College of Arts and Sciences; American Chemical Society Petroleum Research Fund [50242-UNI8] FX The U.S. Army Corps of Engineers provided access to the "Curse of Rafinesquina" tombs study site. The Dry Dredgers of Cincinnati, Ohio and the Cincinnati Museum Center helped with the excavation of the material. Transylvania University Campus Security, Lexington, Kentucky provided access to the tomb of Rafinesque. Freeman thanks the University of Kentucky College of Arts and Sciences for a College Research Activity Award and Peter Idstein of UK's Department of Earth and Environmental Science for helpful discussion and support. Dattilo acknowledges support by American Chemical Society Petroleum Research Fund Grant 50242-UNI8, and thanks Chancellor Michael Wartell and Indiana University-Purdue University Fort Wayne for transportation to the U.S. National Museum. Kate Bulinski of Bellarmine University collected additional material at a different outcrop. Bryan Utesch prepared many of the thin sections. Parts of this work were carried out in the Argast Family Instrumentation and Analysis Lab at IPFW. We thank Carlton Brett and two anonymous reviewers, as well as two anonymous reviewers at the U.S. Geological Survey, and editor John-Paul Zonneveld for helpful suggestions that improved the manuscript. This paper is a contribution to the International Geoscience Programme (IGCP) Project 591: The Early to Middle Paleozoic Revolution. NR 75 TC 3 Z9 3 U1 0 U2 4 PU SEPM-SOC SEDIMENTARY GEOLOGY PI TULSA PA 6128 EAST 38TH ST, STE 308, TULSA, OK 74135-5814 USA SN 0883-1351 EI 1938-5323 J9 PALAIOS JI Palaios PD MAY-JUN PY 2013 VL 28 IS 5-6 BP 359 EP 372 DI 10.2110/palo.2012.p12-094r PG 14 WC Geology; Paleontology SC Geology; Paleontology GA 197NB UT WOS:000322856800010 ER PT J AU Lukowiak, M Pisera, A O'Dea, A AF Lukowiak, Magdalena Pisera, Andrzej O'Dea, Aaron TI DO SPICULES IN SEDIMENTS REFLECT THE LIVING SPONGE COMMUNITY? A TEST IN A CARIBBEAN SHALLOW-WATER LAGOON SO PALAIOS LA English DT Article ID BOCAS DEL TORO; CORAL-REEFS; DEMOSPONGIAE; PANAMA; PORIFERA; RECORD; ISLANDS; BRAZIL; RIVER AB We compared sponge spicules occurring in surface sediments with those of a living sponge community in a shallow-water reef environment of Bocas del Toro archipelago, Panama, with the goal of evaluating how faithfully spicular analysis reflects the living sponge community. Most megasclere morphotypes present in living species are also found in sediment. On the contrary, microscleres are underrepresented in the sediment samples. Apart from spicules that belong to taxa that live at present in the area, some morphotypes found in the sediment have no equivalent in the known living community. Forty species of living sponges have been recognized in the study area, but 9 (22%) do not produce mineral spicules and, therefore, are not recorded in sediment. Sediment spicules suggest the presence of 22 taxa, thus, loss of information in the process of fossilization is average to considerable, with most living taxa identified also with sediment spicules. Some morphotypes are abundant in sediment (i.e., ovoid spicules) even though the sponges bearing them are rare or absent, thus suggesting either preferential preservation or recent disappearances of taxa producing them. As transport did not play a significant role during the fossilization process, spicular analysis when all limitations and constraints are considered is a tenable tool in the reconstruction of former sponge communities, but not of the share of various sponge species. Spicular analysis may also help reveal the presence of cryptic and excavating species that are often overlooked in traditional studies. C1 [Lukowiak, Magdalena; Pisera, Andrzej] Polish Acad Sci, Inst Paleobiol, PL-00818 Warsaw, Poland. [O'Dea, Aaron] Smithsonian Trop Res Inst, Ctr Trop Paleoecol & Archeol, Balboa, Panama. RP Lukowiak, M (reprint author), Polish Acad Sci, Inst Paleobiol, Ul Twarda 51155, PL-00818 Warsaw, Poland. EM mlukowiak@twarda.pan.pl; apis@twarda.pan.pl; odeaa@si.edu FU Smithsonian Tropical Research Institute; PalSIRP Sepkoski Grant; Institute of Paleobiology; National System of Investigators of the National Research of the National Secretariat for Science, Technology and Innovation of Panama (SENACYT) FX This paper is a part of the Ph.D. project of ML and was possible thanks to support of the Institute of Paleobiology, Polish Academy of Sciences, a Short Term Fellowship from the Smithsonian Tropical Research Institute, and a PalSIRP Sepkoski Grant to ML. The Institute of Paleobiology also funded AP. The National System of Investigators (SNI) of the National Research of the National Secretariat for Science, Technology and Innovation of Panama (SENACYT) funded AO. Recursos Minerales kindly gave permission to collect sediments. We would like to thank Gabriel Jacome, Plinio Gondola, Felix Rodriguez, Alexa Fredston-Hermann, Brigida de Gracia, and all the team at the Bocas Research Station for their support. Special thanks are to Alexander Wolfe, University of Alberta (Canada), for linguistic improvements of the manuscript. The authors appreciate also comments and helpful suggestions by Susan Kidwell and the anonymous reviewer. NR 104 TC 5 Z9 5 U1 1 U2 8 PU SEPM-SOC SEDIMENTARY GEOLOGY PI TULSA PA 6128 EAST 38TH ST, STE 308, TULSA, OK 74135-5814 USA SN 0883-1351 EI 1938-5323 J9 PALAIOS JI Palaios PD MAY-JUN PY 2013 VL 28 IS 5-6 BP 373 EP 385 DI 10.2110/palo.2012.p12-082r PG 13 WC Geology; Paleontology SC Geology; Paleontology GA 197NB UT WOS:000322856800011 ER PT J AU Scheyer, TM Aguilera, OA Delfino, M Fortier, DC Carlini, AA Sanchez, R Carrillo-Briceno, JD Quiroz, L Sanchez-Villagra, MR AF Scheyer, T. M. Aguilera, O. A. Delfino, M. Fortier, D. C. Carlini, A. A. Sanchez, R. Carrillo-Briceno, J. D. Quiroz, L. Sanchez-Villagra, M. R. TI Crocodylian diversity peak and extinction in the late Cenozoic of the northern Neotropics SO NATURE COMMUNICATIONS LA English DT Article ID MIOCENE URUMACO FORMATION; SEXUAL SIZE DIMORPHISM; PHYLOGENETIC-RELATIONSHIPS; FALCON STATE; VENEZUELA; CROCODILE; NEOGENE; AFRICA; TIME; PLIOPLEISTOCENE AB Northern South America and South East Asia are today's hotspots of crocodylian diversity with up to six (mainly alligatorid) and four (mainly crocodylid) living species respectively, of which usually no more than two or three occur sympatrically. In contrast, during the late Miocene, 14 species existed in South America. Here we show a diversity peak in sympatric occurrence of at least seven species, based on detailed stratigraphic sequence sampling and correlation, involving four geological formations from the middle Miocene to the Pliocene, and on the discovery of two new species and a new occurrence. This degree of crocodylian sympatry is unique in the world and shows that at least several members of Alligatoroidea and Gavialoidea coexisted. By the Pliocene, all these species became extinct, and their extinction was probably related to hydrographic changes linked to the Andean uplift. The extant fauna is first recorded with the oldest Crocodylus species from South America. C1 [Scheyer, T. M.; Sanchez-Villagra, M. R.] Univ Zurich, Palaeontol Inst & Museum, CH-8006 Zurich, Switzerland. [Aguilera, O. A.] Univ Fed Fluminense, Programa Posgrad Biol Marinha, Inst Biol, BR-2402014 Rio De Janeiro, Brazil. [Delfino, M.] Univ Turin, Dipartimento Sci Terra, I-10125 Turin, Italy. [Delfino, M.] Univ Autonoma Barcelona, Inst Catala Paleontol Miquel Crusafont, E-08193 Barcelona, Spain. [Fortier, D. C.] Univ Fed Rio Grande do Sul, Dept Paleontol & Estratig, IGeo, BR-15001 Porto Alegre, RS, Brazil. [Carlini, A. A.] Museo La Plata, Dept Cient Paleontol Vertebrados, La Plata, Buenos Aires, Argentina. [Sanchez, R.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. [Carrillo-Briceno, J. D.] Alcaldia Bolivariana Municipio Urumaco, Urumaco, Estado Falcon, Venezuela. [Quiroz, L.] Univ Saskatchewan, Dept Geol Sci, Saskatoon, SK S7N 5E2, Canada. RP Sanchez-Villagra, MR (reprint author), Univ Zurich, Palaeontol Inst & Museum, Karl Schmid Str 4, CH-8006 Zurich, Switzerland. EM m.sanchez@pim.uzh.ch OI Carrillo Briceno, Jorge Domingo/0000-0002-8652-7692 FU Swiss National Science Foundation [31003 A 127053, 146440, Sinergia CRSII3-136293]; Spanish Ministerio de Economia y Competitividad [CGL2011-28681]; Florida Museum of the Natural History; CAPES; CNPq FX p Specimens are deposited at The Alcaldia del Municipio Urumaco (AMU), Falcon, Venezuela. J. Hernandez provided access to the specimens. We thank the authorities at the Instituto del Patrimonio Cultural of the Republica Bolivariana de Venezuela for generous support to conduct this research. M. Reisser (ETHZ) and C. Colucci (UZH) are thanked for preparation and discussions. This work was funded by the Swiss National Science Foundation (grant 31003 A 127053 and 146440 to TMS; and Sinergia CRSII3-136293 to MRS-V) and Spanish Ministerio de Economia y Competitividad (CGL2011-28681 to MD). Collections visits to DCF funded by The Florida Museum of the Natural History and Brazilian agencies CAPES and CNPq. NR 53 TC 33 Z9 34 U1 0 U2 21 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 MAY PY 2013 VL 4 AR 1907 DI 10.1038/ncomms2940 PG 9 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 166WI UT WOS:000320589900103 PM 23695701 ER PT J AU Kawashima, T Thorington, RW Murakami, K Sato, F AF Kawashima, Tomokazu Thorington, Richard W., Jr. Murakami, Kunio Sato, Fumi TI Evolutionary Anatomy and Phyletic Implication of the Extrinsic Cardiac Nervous System in the Philippine Tarsier (Tarsius syrichta, Primates) in Comparisons With Strepsirrhines and New World Monkeys SO ANATOMICAL RECORD-ADVANCES IN INTEGRATIVE ANATOMY AND EVOLUTIONARY BIOLOGY LA English DT Article DE tarsier; cardiac innervation; comparative anatomy; evolution; primate phylogeny ID INNERVATION; MORPHOLOGY; POSITION; BANCANUS; PATTERN; APES; EYES AB To provide information on evolutionary morphological differences and similarities between Tarsiformes (tarsiers) and other primates (Strepsirrhini and Platyrrhini), we examined the previously undescribed extrinsic cardiac nervous system (ECNS) and surrounding structures in three Philippine tarsiers (Tarsius syrichta). We found that the complicated ECNS morphology shows little variation in contrast to significant anatomical diversity of the surrounding somatic structures in tarsiers as reported in our previous primate studies. Further, our comparative morphological data on the ECNS show the following aspects of evolutionary anatomical significance; (1) the traits of the general relationship between the superior cervical ganglion and the spinal nerves are common to the Tarsii and Strepsirrhini, (2) the traits of the general composition of the cervicothoracic ganglion, its communicating branches to spinal nerves, and its cardiac nerve are common to the Tarsii and Platyrrhini, and (3) the traits of the general relationship between the middle cervical ganglion and the spinal nerves and its cardiac nerve are common among Strepsirrhini, Tarsii, and Platyrrhini. Therefore, the general anatomical characteristics of the ECNS in tarsiers retain a primitive state for some traits and exhibit a derived state for others. These characteristics of the ECNS also reflect an evolutionary history without the modification and specialization as seen in the surrounding somatic structures. It may play a key role in unifying future studies on molecular phylogeny and updating evolutionary anatomical information. (C) 2013 Wiley Periodicals, Inc. C1 [Kawashima, Tomokazu; Murakami, Kunio; Sato, Fumi] Toho Univ, Sch Med, Dept Anat, Tokyo 1438540, Japan. [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), Toho Univ, Sch Med, Dept Anat, Ota Ku, 5-21-16 Omori Nishi, Tokyo 1438540, Japan. EM tomokazu.kawashima@med.toho-u.ac.jp FU Japanese Ministry of Education, Culture, Sports, Science, and Technology [16790804, 19790985, 23791579]; Field Museum of Natural History FX Grant sponsor: Scientific Research from the Japanese Ministry of Education, Culture, Sports, Science, and Technology (2004-2006, 2007-2009, and 2011-2014); Grant numbers: 16790804; 19790985; 23791579. Grant sponsor: International Research Program by the Japanese Ministry of Education, Culture, Sports, Science, and Technology (2008-2009); Grant sponsor: Visiting Research from the Field Museum of Natural History (2008-2009). NR 35 TC 1 Z9 1 U1 3 U2 26 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1932-8486 J9 ANAT REC JI Anat. Rec. PD MAY PY 2013 VL 296 IS 5 BP 798 EP 806 DI 10.1002/ar.22680 PG 9 WC Anatomy & Morphology SC Anatomy & Morphology GA 164CU UT WOS:000320387200008 PM 23444325 ER PT J AU Janiak, DS Osman, RW Whitlatch, RB AF Janiak, Dean S. Osman, Richard W. Whitlatch, Robert B. TI The role of species richness and spatial resources in the invasion success of the colonial ascidian Didemnum vexillum Kott, 2002 in eastern Long Island Sound SO JOURNAL OF EXPERIMENTAL MARINE BIOLOGY AND ECOLOGY LA English DT Article DE Didemnum vexillum; Fouling communities; Invasion; Long Island Sound; Spatial resources; Species richness ID MARINE COMMUNITIES; PROPAGULE PRESSURE; ECOLOGICAL OBSERVATIONS; EPIFAUNAL COMMUNITY; BIOTIC RESISTANCE; HARD-SUBSTRATE; NORTH-AMERICA; PREDATION; HABITAT; RECRUITMENT AB Since it was first discovered in the northwest Atlantic in the late 1980s, the non-indigenous colonial ascidian Didemnum vexillum Kott, 2002 has become a common inhabitant of coastal marinas as well as deeper water sites. This species has also been found to have an expanding global distribution leading to questions about its ability to successfully invade into a variety of communities. The goal of the present study was to build on previous knowledge and to examine the possible mechanisms that allow Didemnum to successfully invade fouling communities in eastern Long Island Sound. In separate experiments, we examined whether species richness and spatial resources (i.e. open space) influenced invasion success. Communities at 2 sites, a protected marina and an open coast site, were compared. In the first experiment, small colonies of Didemnum were transplanted into communities that contained different species richness levels (0, 2,4, 6 spp.) and in the second, small colonies of Didemnum were transplanted into communities that varied in the amount of species cover (0, 60, 50, 100%) that was present. The growth of Didemnum, as well as species initially present and any new species from recruitment was measured each week for approximately 10 weeks. Communities with high amounts of initial open space, regardless of species richness, tended to result in increased abundances of Didemnum at the open coast site and initially at the protected marina. At the marina site, growth of recruits and resident species resulted in the rapid loss of space in all treatments in both experiments, which reduced the success of Didemnum. At the open coast site, without increased competition from recruiting species, Didemnum became more abundant and eventually dominated many of the communities in all treatments. Despite being a global invader, Didemnum appears to be a relatively poor competitor for spatial resources. Its dominance seems to depend on the amount of unoccupied space present within communities it's invading. That, coupled with high recruitment from a diverse community, can overwhelm the potential invasion success of this species. Published by Elsevier B.V. C1 [Janiak, Dean S.; Osman, Richard W.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. [Whitlatch, Robert B.] Univ Connecticut, Dept Marine Sci, Groton, CT 06340 USA. RP Janiak, DS (reprint author), Smithsonian Environm Res Ctr, POB 28,647 Contees Wharf Rd, Edgewater, MD 21037 USA. EM janiakd@si.edu; osmanr@si.edu; robert.whitlatch@uconn.edu FU Connecticut Sea Grant College program; US EPA STAR program FX Funding for this project was provided by grants to R. Osman and R. Whitlatch from the Connecticut Sea Grant College program and the US EPA STAR program. Thanks to L Stefaniak, K. Bostrom, J. Godfrey, J. Hamilton, J. Mangiafico, R Patrylak, J. Reinhardt and A. Watson for their assistance with field work Gary Grenier and Bob Dziomba designed and constructed the donut panels. [ST] NR 46 TC 5 Z9 5 U1 3 U2 52 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 MAY PY 2013 VL 443 BP 12 EP 20 DI 10.1016/j.jembe.2013.02.030 PG 9 WC Ecology; Marine & Freshwater Biology SC Environmental Sciences & Ecology; Marine & Freshwater Biology GA 164QX UT WOS:000320425700002 ER PT J AU Dent, WRF Thi, WF Kamp, I Williams, JP Menard, F Andrews, S Ardila, D Aresu, G Augereau, JC Navascues, DBY Brittain, S Carmona, A Ciardi, D Danchi, W Donaldson, J Duchene, G Eiroa, C Fedele, D Grady, C de Gregorio-Molsalvo, I Howard, C Huelamo, N Krivov, A Lebreton, J Liseau, R Martin-Zaidi, C Mathews, G Meeus, G Mendigutia, I Montesinos, B Morales-Calderon, M Mora, A Nomura, H Pantin, E Pascucci, I Phillips, N Pinte, C Podio, L Ramsay, SK Riaz, B Riviere-Marichalar, P Roberge, A Sandell, G Solano, E Tilling, I Torrelles, JM Vandenbusche, B Vicente, S White, GJ Woitke, P AF Dent, W. R. F. Thi, W. F. Kamp, I. Williams, J. P. Menard, F. Andrews, S. Ardila, D. Aresu, G. Augereau, J. -C. Barrado y Navascues, D. Brittain, S. Carmona, A. Ciardi, D. Danchi, W. Donaldson, J. Duchene, G. Eiroa, C. Fedele, D. Grady, C. de Gregorio-Molsalvo, I. Howard, C. Huelamo, N. Krivov, A. Lebreton, J. Liseau, R. Martin-Zaidi, C. Mathews, G. Meeus, G. Mendigutia, I. Montesinos, B. Morales-Calderon, M. Mora, A. Nomura, H. Pantin, E. Pascucci, I. Phillips, N. Pinte, C. Podio, L. Ramsay, S. K. Riaz, B. Riviere-Marichalar, P. Roberge, A. Sandell, G. Solano, E. Tilling, I. Torrelles, J. M. Vandenbusche, B. Vicente, S. White, G. J. Woitke, P. TI GASPS-A Herschel Survey of Gas and Dust in Protoplanetary Disks: Summary and Initial Statistics SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC LA English DT Article ID TW-HYDRAE ASSOCIATION; ETA-CHAMAELEONTIS CLUSTER; PICTORIS MOVING GROUP; HERBIG AE/BE SYSTEMS; TUCANA-HOROLOGIUM ASSOCIATION; SPITZER-MIPS OBSERVATIONS; AURIGA MOLECULAR CLOUD; MAIN-SEQUENCE STARS; LOW-MASS PROTOSTARS; X-RAY-EMISSION AB We describe a large-scale far-infrared line and continuum survey of protoplanetary disk through to young debris disk systems carried out using the ACS instrument on the Herschel Space Observatory. This Open Time Key program, known as GASPS (Gas Survey of Protoplanetary Systems), targeted similar to 250 young stars in narrow wavelength regions covering the [OI] fine structure line at 63 mu m the brightest far-infrared line in such objects. A subset of the brightest targets were also surveyed in [OI]145 mu m, [CII] at 157 mu m, as well as several transitions of H2O and high-excitation CO lines at selected wavelengths between 78 and 180 mu m. Additionally, GASPS included continuum photometry at 70, 100 and 160 mu m, around the peak of the dust emission. The targets were SED Class II-III T Tauri stars and debris disks from seven nearby young associations, along with a comparable sample of isolated Herbig AeBe stars. The aim was to study the global gas and dust content in a wide sample of circumstellar disks, combining the results with models in a systematic way. In this overview paper we review the scientific aims, target selection and observing strategy of the program. We summarise some of the initial results, showing line identifications, listing the detections, and giving a first statistical study of line detectability. The [OI] line at 63 mu m was the brightest line seen in almost all objects, by a factor of similar to 10. Overall [OI]63 mu m detection rates were 49%, with 100% of HAeBe stars and 43% of T Tauri stars detected. A comparison with published disk dust masses (derived mainly from sub-mm continuum, assuming standard values of the mm mass opacity) shows a dust mass threshold for [OI] 63 mu m detection of similar to 10(-5) M-circle dot. Normalising to a distance of 140 pc, 84% of objects with dust masses >= 10(-5) M-circle dot can be detected in this line in the present survey; 32% of those of mass 10(-6)-10(-5) M-circle dot, and only a very small number of unusual objects with lower masses can be detected. This is consistent with models with a moderate UV excess and disk flaring. For a given disk mass, [OI] detectability is lower for M stars compared with earlier spectral types. Both the continuum and line emission was, in most systems, spatially and spectrally unresolved and centred on the star, suggesting that emission in most cases was from the disk. Approximately 10 objects showed resolved emission, most likely from outflows. In the GASPS sample, [OI] detection rates in T Tauri associations in the 0.3-4 Myr age range were similar to 50%. For each association in the 5-20 Myr age range, similar to 2 stars remain detectable in [OI]63 mu m, and no systems were detected in associations with age >20 Myr. Comparing with the total number of young stars in each association, and assuming a ISM-like gas/dust ratio, this indicates that similar to 18% of stars retain a gas-rich disk of total mass similar to 1 M-Jupiter for 1-4 Myr, 1-7% keep such disks for 5-10 Myr, but none are detected beyond 10-20 Myr. The brightest [OI] objects from GASPS were also observed in [OI]145 mu m, [CII]157 mu m and CO J = 18 - 17, with detection rates of 20-40%. Detection of the [CII] line was not correlated with disk mass, suggesting it arises more commonly from a compact remnant envelope. C1 [Dent, W. R. F.; de Gregorio-Molsalvo, I.; Phillips, N.; Podio, L.] ALMA SCO, Santiago, Chile. [Thi, W. F.; Kamp, I.; Aresu, G.; Vicente, S.] Univ Groningen, Kapteyn Astron Inst, NL-9700 AV Groningen, Netherlands. [Thi, W. F.; Menard, F.; Augereau, J. -C.; Carmona, A.; Duchene, G.; Lebreton, J.; Martin-Zaidi, C.; Pinte, C.] IPAG, UJF Grenoble 1, CNRS INSU, UMR 5274, F-38041 Grenoble, France. [Williams, J. P.; Mathews, G.] Univ Hawaii Manoa, Inst Astron, Honolulu, HI 96822 USA. [Andrews, S.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Ardila, D.] CALTECH, NASA Herschel Sci Ctr, Pasadena, CA 91125 USA. [Barrado y Navascues, D.; Huelamo, N.; Mendigutia, I.; Montesinos, B.; Morales-Calderon, M.; Riviere-Marichalar, P.; Solano, E.] CSIC INTA, Ctr Astrobiol, Dept Astrofis, E-28691 Villanueva De La Canada, Spain. [Barrado y Navascues, D.] Ctr Astron Hispano Aleman, Calar Alto Observ, E-04004 Almera, Spain. [Brittain, S.] Clemson Univ, Dept Phys & Astron, Kinard Lab 118, Clemson, SC 29634 USA. [Ciardi, D.] CALTECH, NASA Exoplanet Sci Inst, Pasadena, CA 91125 USA. [Danchi, W.; Roberge, A.] NASA, Goddard Space Flight Ctr, Exoplanets & Stellar Astrophys Lab, Greenbelt, MD 20771 USA. [Donaldson, J.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Duchene, G.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Eiroa, C.; Meeus, G.] UAM Campus Cantoblanco, Fac Ciencias, Dep Fis, Madrid, Spain. [Fedele, D.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Grady, C.] Eureka Sci, Oakland, CA USA. [Howard, C.; Sandell, G.] NASA, Ames Res Ctr, SOFIA USRA, Moffett Field, CA 94035 USA. [Krivov, A.] Univ Jena, Inst Astrophys, Jena, Germany. [Liseau, R.] Chalmers, Onsala Space Observ, Dept Earth & Space Sci, S-43900 Onsala, Sweden. [Mora, A.] ESA ESAC Gaia SOC, Madrid 28691, Spain. [Nomura, H.] Kyoto Univ, Grad Sch Sci, Dept Astron, Kyoto 6068502, Japan. [Pantin, E.] Univ Paris Diderot, IRFU SAp, CNRS, CEA DSM,Lab AIM,CE Saclay, Paris, France. [Pascucci, I.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA. [Ramsay, S. K.] European So Observ, D-85748 Garching, Germany. [Riaz, B.] Univ Hertfordshire, Ctr Astrophys Res, Hatfield AL10 9AB, Herts, England. [Tilling, I.] Univ Edinburgh, Royal Observ, Edinburgh, Midlothian, Scotland. [Torrelles, J. M.] Univ Barcelona, CSIC UB IEEC, Barcelona, Spain. [Vandenbusche, B.] Katholieke Univ Leuven, Inst Sterrenkunde, B-3001 Heverlee, Belgium. [White, G. J.] Open Univ, Dept Phys Sci, Milton Keynes MK7 6AA, Bucks, England. [White, G. J.] Rutherford Appleton Lab, RALSpace, Didcot OX11 0NL, Oxon, England. [Woitke, P.] Univ St Andrews, Sch Phys & Astron, SUPA, St Andrews KY16 9SS, Fife, Scotland. RP Dent, WRF (reprint author), ALMA SCO, Alonso Cordova 3107, Santiago, Chile. RI Fedele, Davide/L-8688-2013; Roberge, Aki/D-2782-2012; Barrado Navascues, David/C-1439-2017; Solano, Enrique/C-2895-2017; Huelamo, Nuria/C-3042-2017; Montesinos, Benjamin/C-3493-2017; Morales-Calderon, Maria/C-8384-2017; OI Fedele, Davide/0000-0001-6156-0034; Roberge, Aki/0000-0002-2989-3725; Barrado Navascues, David/0000-0002-5971-9242; Huelamo, Nuria/0000-0002-2711-8143; Montesinos, Benjamin/0000-0002-7982-2095; Morales-Calderon, Maria/0000-0001-9526-9499; Torrelles, Jose Maria/0000-0002-6896-6085; Mendigutia, Ignacio/0000-0002-0233-5328; Ciardi, David/0000-0002-5741-3047 FU ANR [BLAN-0221, 0504-01, 0505-01]; European Commission's 7th Framework program [pERG06-GA-2009-256513]; CNES; PNPS of CNRS/INSU, France; EU FP7 [284405]; Scottish University physics Alliance fellowship; BMVIT (Austria); ESA-PRODEX (Belgium); CEA/CNES (France); DLR (Germany); ASI/INAF (Italy); CICYT/MCYT (Spain) FX We wish to acknowledge the Herschel Helpdesk for their timely and useful responses. The Grenoble group thanks ANR (contracts BLAN-0221, 0504-01 and 0505-01), European Commission's 7th Framework program (contract pERG06-GA-2009-256513), CNES, and PNPS of CNRS/INSU, France for support. PW, IK, and WFT acknowledge funding from the EU FP7-2011 under Grant Agreement nr. 284405. WFT acknowledges a Scottish University physics Alliance fellowship (2006-2009).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). NR 173 TC 41 Z9 42 U1 0 U2 10 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 MAY PY 2013 VL 125 IS 927 BP 477 EP 505 DI 10.1086/670826 PG 29 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 162CK UT WOS:000320241800001 ER PT J AU Zeitlin, C Case, AW Spence, HE Schwadron, NA Golightly, M Wilson, JK Kasper, JC Blake, JB Looper, MD Mazur, JE Townsend, LW Iwata, Y AF Zeitlin, C. Case, A. W. Spence, H. E. Schwadron, N. A. Golightly, M. Wilson, J. K. Kasper, J. C. Blake, J. B. Looper, M. D. Mazur, J. E. Townsend, L. W. Iwata, Y. TI Measurements of galactic cosmic ray shielding with the CRaTER instrument SO SPACE WEATHER-THE INTERNATIONAL JOURNAL OF RESEARCH AND APPLICATIONS LA English DT Article DE galactic cosmic rays; shielding; CRaTER ID SPACE RADIATION; FRAGMENTATION; NUCFRG2; FE-56; MODEL AB The Cosmic Ray Telescope for the Effects of Radiation (CRaTER) instrument aboard the Lunar Reconnaissance Orbiter has been measuring energetic charged particles from the galactic cosmic rays (GCRs) and solar particle events in lunar orbit since 2009. CRaTER includes three pairs of silicon detectors, separated by pieces of tissue-equivalent plastic that shield two of the three pairs from particles incident at the zenith-facing end of the telescope. Heavy-ion beams studied in previous ground-based work have been shown to be reasonable proxies for the GCRs when their energies are sufficiently high. That work, which included GCR simulations, led to predictions for the amount of dose reduction that would be observed by CRaTER. Those predictions are compared to flight data obtained by CRaTER in 2010-2011. C1 [Zeitlin, C.] SW Res Inst, Boulder, CO 80302 USA. [Case, A. W.; Kasper, J. C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Spence, H. E.; Schwadron, N. A.; Golightly, M.; Wilson, J. K.] Univ New Hampshire, Inst Study Earth Oceans & Space, Durham, NH 03824 USA. [Blake, J. B.; Looper, M. D.; Mazur, J. E.] Aerosp Corp, El Segundo, CA 90245 USA. [Townsend, L. W.] Univ Tennessee, Dept Nucl Engn, Knoxville, TN 37996 USA. [Iwata, Y.] Natl Inst Radiol Sci, Chiba 260, Japan. RP Zeitlin, C (reprint author), SW Res Inst, 1050 Walnut St, Boulder, CO 80302 USA. EM zeitlin@boulder.swri.edu RI Kasper, Justin/D-1152-2010; OI Kasper, Justin/0000-0002-7077-930X; Spence, Harlan/0000-0002-2526-2205 FU Southwest Research Institute [12-053]; University of New Hampshire; University of New Hampshire under the NASA [NNG11PA03C] FX This work was supported by Southwest Research Institute under Agreement 12-053 with the University of New Hampshire, and by the University of New Hampshire under the NASA CRaTER contract NNG11PA03C. NR 25 TC 6 Z9 6 U1 0 U2 5 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 1542-7390 J9 SPACE WEATHER JI Space Weather PD MAY PY 2013 VL 11 IS 5 BP 284 EP 296 DI 10.1002/swe.20043 PG 13 WC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology & Atmospheric Sciences SC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology & Atmospheric Sciences GA 166MR UT WOS:000320559400011 ER PT J AU Abe, L Goncalves, I Agabi, A Alapini, A Guillot, T Mekarnia, D Rivet, JP Schmider, FX Crouzet, N Fortney, J Pont, F Barbieri, M Daban, JB Fantei-Caujolle, Y Gouvret, C Bresson, Y Roussel, A Bonhomme, S Robini, A Dugue, M Bondoux, E Peron, S Petit, PY Szulagyi, J Fruth, T Erikson, A Rauer, H Fressin, F Valbousquet, F Blanc, PE Le van Suu, A Aigrain, S AF Abe, L. Goncalves, I. Agabi, A. Alapini, A. Guillot, T. Mekarnia, D. Rivet, J-P Schmider, F-X Crouzet, N. Fortney, J. Pont, F. Barbieri, M. Daban, J-B. Fantei-Caujolle, Y. Gouvret, C. Bresson, Y. Roussel, A. Bonhomme, S. Robini, A. Dugue, M. Bondoux, E. Peron, S. Petit, P-Y Szulagyi, J. Fruth, T. Erikson, A. Rauer, H. Fressin, F. Valbousquet, F. Blanc, P-E Le van Suu, A. Aigrain, S. TI The secondary eclipses of WASP-19b as seen by the ASTEP 400 telescope from Antarctica SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE instrumentation: photometers; stars: individual: WASP-19; planetary systems; planets and satellites: atmospheres; starspots ID OPTIMAL IMAGE SUBTRACTION; GROUND-BASED DETECTION; EXTRASOLAR PLANET; TIDAL DISSIPATION; TRANSITING EXOPLANET; HOT JUPITERS; PHOTOMETRY; EVOLUTION; CONSTRAINTS; ATMOSPHERES AB Aims. The Antarctica Search for Transiting ExoPlanets (ASTEP) program was originally aimed at probing the quality of the Dome C, Antarctica for the discovery and characterization of exoplanets by photometry. In the first year of operation of the 40 cm ASTEP 400 telescope (austral winter 2010), we targeted the known transiting planet WASP-19b in order to try to detect its secondary transits in the visible. This is made possible by the excellent sub-millimagnitude precision of the binned data. Methods. The WASP-19 system was observed during 24 nights in May 2010. Once brought back from Antarctica, the data were processed using various methods, and the best results were with an implementation of the optimal image subtraction (OIS) algorithm. Results. The photometric variability level due to starspots is about 1.8% (peak-to-peak), in line with the SuperWASP data from 2007 (1.4%) and higher than in 2008 (0.07%). We find a rotation period of WASP-19 of 10.7 +/- 0.5 days, in agreement with the SuperWASP determination of 10.5 +/- 0.2 days. Theoretical models show that this can only be explained if tidal dissipation in the star is weak, i.e. the tidal dissipation factor Q'(*) > 3 x 10(7). Separately, we find evidence of a secondary eclipse of depth 390 +/- 190 ppm with a 2.0 sigma significance, a phase that is consistent with a circular orbit and a 3% false positive probability. Given the wavelength range of the observations (420 to 950 nm), the secondary transit depth translates into a day-side brightness temperature of 2690(-220)(+150) K, in line with measurements in the z' and K bands. The day-side emission observed in the visible could be due either to thermal emission of an extremely hot day side with very little redistribution of heat to the night side or to direct reflection of stellar light with a maximum geometrical albedo A(g) = 0.27 +/- 0.13. We also report a low-frequency oscillation in phase at the planet orbital period, but with a lower limit amplitude that could not be attributed to the planet phase alone and that was possibly contaminated with residual lightcurve trends. Conclusions. This first evidence of a secondary eclipse in the visible from the ground demonstrates the high potential of Dome C, Antarctica, for continuous photometric observations of stars with exoplanets. These continuous observations are required to understand star-planet interactions and the dynamical properties of exoplanetary atmospheres. C1 [Abe, L.; Goncalves, I.; Agabi, A.; Guillot, T.; Mekarnia, D.; Rivet, J-P; Schmider, F-X; Barbieri, M.; Daban, J-B.; Fantei-Caujolle, Y.; Gouvret, C.; Bresson, Y.; Roussel, A.; Bonhomme, S.; Robini, A.; Dugue, M.; Bondoux, E.; Peron, S.; Petit, P-Y; Szulagyi, J.] Univ Nice Sophia Antipolis, Observ Cote Azur, CNRS UMR 7293, F-06108 Nice 2, France. [Alapini, A.; Pont, F.] Univ Exeter, Sch Phys, Exeter EX4 4QL, Devon, England. [Guillot, T.; Fortney, J.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. [Crouzet, N.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Fruth, T.; Erikson, A.; Rauer, H.] DLR Inst Planetary Res, D-12489 Berlin, Germany. [Fressin, F.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Valbousquet, F.] Opt & Vis, F-06162 Juan Les Pins, France. [Blanc, P-E; Le van Suu, A.] Univ Aix Marseille, Observ Haute Provence, F-04870 St Michel lObservatoire, France. [Blanc, P-E; Le van Suu, A.] CNRS, F-04870 St Michel lObservatoire, France. [Aigrain, S.] Univ Oxford, Dept Phys, Oxford OX1 3RH, England. RP Abe, L (reprint author), Univ Nice Sophia Antipolis, Observ Cote Azur, CNRS UMR 7293, F-06108 Nice 2, France. EM Lyu.Abe@unice.fr OI Barbieri, Mauro/0000-0001-8362-3462; Fortney, Jonathan/0000-0002-9843-4354 FU French Agence Nationale de la Recherche (ANR); Institut des Sciences de l'Univers (INSU); Programme National de Planetologie; Institut Paul-Emile Victor (IPEV); Plan Pluri-Formation OPERA between Observatoire de la Cote d'Azur and Universite de Nice Sophia Antipolis (UNS); INSU/CNRS; Fulbright fellowship while at UCSC FX The ASTEP project has been funded by the French Agence Nationale de la Recherche (ANR), Institut des Sciences de l'Univers (INSU), Programme National de Planetologie, Institut Paul-Emile Victor (IPEV), and the Plan Pluri-Formation OPERA between Observatoire de la Cote d'Azur and Universite de Nice Sophia Antipolis (UNS). Ivan Goncalves is funded by INSU/CNRS. T.G. acknowledges support from a Fulbright fellowship while at UCSC. NR 47 TC 13 Z9 13 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 MAY PY 2013 VL 553 AR A49 DI 10.1051/0004-6361/201220351 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 156YA UT WOS:000319858700049 ER PT J AU Casassus, S Hales, A de Gregorio, I Dent, B Belloche, A Gusten, R Menard, F Hughes, AM Wilner, D Salinas, V AF Casassus, S. Hales, A. de Gregorio, I. Dent, B. Belloche, A. Guesten, R. Menard, F. Hughes, A. M. Wilner, D. Salinas, V. TI CO(6-5) and [C I](2-1) pointed observations of five protoplanetary disks: Warm gas in HD 142527 (Research Note) SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE protoplanetary disks; stars: emission-line, Be ID MAIN-SEQUENCE STARS; T TAURI STARS; CIRCUMSTELLAR DISKS; SURROUNDING HD-142527; PLANET FORMATION; IMAGING SURVEY; YOUNG STARS; CO EMISSION; CHEMISTRY; DUST AB Context. The molecular gas in protoplanetary disks can be traced with single-dish instruments in low J rotational lines of CO, in systems clear of coincident extended emission. Other rotational lines of CO also sample the gas-phase CO reservoir, albeit with different biases; CO(6-5) traces warmer molecular gas. A rarefied atomic gas could be traced in [C I](2-1), but no C I detections in disks exist. Aims. Our goals are to identify gas-rich systems that are bright in CO(6-5), for subsequent ALMA observations, and search for C I. Methods. We follow-up a CO(3-2) survey in protoplanetary disks with APEX/CHAMP+ maps in CO(6-5) 691.4 GHz and [C I](2-1) 809.3 GHz. Results. We obtain one compact CO(6-5) detection in HD 142 527, three upper limits, and extended CO(6-5) emission in HD 37389. Given the CO(2-1) flux, the CO(6-5) line in HD 142527 would imply a temperature of 19 K if the CO ladder was isothermal, for a common solid angle, which is close to CO freezeout. This low temperature, together with a modulated CO(6-5) line profile, can be explained by a 4 '' pointing off set. The C I observations yield upper limits on the mass of rarefied gas phase neutral carbon. Conclusions. The CO(6-5) detection in HD 142527 adds to the other two southern systems with known CO(6-5) signal (HD 100546 and TW Hya). The CO(6-5)/CO(3-2) flux ratio varies from 2 to 24 among seven sources with bona-fide CO(6-5) detections, and is uncorrelated with spectral type in this sample. The upper limits on CI emission constrain the fraction of carbon in low-density (<10(3) cm(-3)) atomic gas to <4 x 10(-3) (3 sigma). C1 [Casassus, S.; Salinas, V.] Univ Chile, Dept Astron, Santiago, Chile. [Casassus, S.] LUTH, Observ Paris, F-92190 Meudon, France. [Casassus, S.] Univ Paris 07, F-92190 Meudon, France. [Hales, A.; de Gregorio, I.; Dent, B.] Joint ALMA Observ, Santiago 7630355, Chile. [de Gregorio, I.] European So Observ, Santiago 19, Chile. [Belloche, A.; Guesten, R.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Menard, F.] Univ Chile, UMI FCA, CNRS INSU France UMI 3386, Santiago, Chile. [Menard, F.] Univ Chile, Dept Astron, Santiago, Chile. [Menard, F.] IPAG, CNRS UJF Grenoble 1, UMR 5274, F-38041 Grenoble 9, France. [Hughes, A. M.] Wesleyan Univ, Dept Astron, Van Vleck Observ, Middletown, CT 06459 USA. [Wilner, D.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Casassus, S (reprint author), Univ Chile, Dept Astron, Santiago, Chile. EM simon@das.uchile.cl RI Casassus, Simon/I-8609-2016 FU Millennium Science Initiative (Chilean Ministry of Economy) [Nucleus P10-022-F]; Marie Curie International Incoming Fellowship [REA-236176]; FONDECYT [1100221]; CATA (CONICYT) [Fondo Basal PFB-06]; Ministerio de Ciencia e Innovacion (Spain) [AYA2008-06189-C03-01] FX We thank the referee for a thorough review with constructive comments that improved this research note. S.C., A.H., B.D., & F.M. acknowledge support from the Millennium Science Initiative (Chilean Ministry of Economy), through grant "Nucleus P10-022-F". S.C. acknowledges support from a Marie Curie International Incoming Fellowship (REA-236176), from FONDECYT grant 1100221, and the CATA ("Fondo Basal PFB-06, CONICYT"). I.d.G. acknowledges partial support from Ministerio de Ciencia e Innovacion (Spain), grant AYA2008-06189-C03-01. NR 35 TC 9 Z9 9 U1 0 U2 1 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD MAY PY 2013 VL 553 AR UNSP A64 DI 10.1051/0004-6361/201219644 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 156YA UT WOS:000319858700064 ER PT J AU Immer, K Reid, MJ Menten, KM Brunthaler, A Dame, TM AF Immer, K. Reid, M. J. Menten, K. M. Brunthaler, A. Dame, T. M. TI Trigonometric parallaxes of massive star forming regions: G012.88+0.48 and W33 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE astrometry; masers; parallaxes; proper motions; stars: distances; stars: formation ID MILKY-WAY; PROTOSTELLAR CANDIDATES; GALACTIC PLANE; BESSEL SURVEY; SPIRAL ARM; COMPLEX; MASERS; PARAMETERS; EMISSION; DISTANCE AB We report trigonometric parallaxes for water masers in the G012.88+0.48 region and in the massive star forming complex W33 (containing G012.68-0.18, G012.81-0.19, G012.90-0.24, G012.90-0.26), from the Bar and Spiral Structure Legacy (BeSSeL) survey using the Very Long Baseline Array. The parallax distances to all these masers are consistent with 2.40(-0.15)(+0.17) kpc, which locates the W33 complex and G012.88+0.48 in the Scutum spiral arm. Our results show that W33 is a single star forming complex at about two-thirds the kinematic distance of 3.7 kpc. The luminosity and mass of this region, based on the kinematic distance, have therefore been overestimated by more than a factor of two. The spectral types in the star cluster in W33 Main have to be changed by 1.5 points to later types. C1 [Immer, K.; Menten, K. M.; Brunthaler, A.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Immer, K.; Reid, M. J.; Dame, T. M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02140 USA. RP Immer, K (reprint author), Max Planck Inst Radioastron, Hugel 69, D-53121 Bonn, Germany. EM kimmer@mpifr-bonn.mpg.de FU ERC Advanced Investigator Grant GLOSTAR [247078] FX The authors would like to thank Koichiro Sugiyama for providing the 6.7 GHz methanol maser results of G012.88+0.48 from the Japanese VLBI Network survey. This work was partially funded by the ERC Advanced Investigator Grant GLOSTAR (247078). This work made use of the Swinburne University of Technology software correlator, developed as part of the Australian Major National Research Facilities Programme and operated under licence (Deller et al. 2007). NR 36 TC 18 Z9 18 U1 0 U2 0 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD MAY PY 2013 VL 553 AR UNSP A117 DI 10.1051/0004-6361/201220793 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 156YA UT WOS:000319858700117 ER PT J AU in 't Zand, JJM Galloway, DK Marshall, HL Ballantyne, DR Jonker, PG Paerels, FBS Palmer, DM Patruno, A Weinberg, NN AF in 't Zand, J. J. M. Galloway, D. K. Marshall, H. L. Ballantyne, D. R. Jonker, P. G. Paerels, F. B. S. Palmer, D. M. Patruno, A. Weinberg, N. N. TI A bright thermonuclear X-ray burst simultaneously observed with Chandra and RXTE SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE accretion, accretion disks; X-rays: binaries; X-rays: bursts; stars: neutron; X-rays: individuals: SAX J1808.4-3658 ID REDSHIFTED ABSORPTION-LINES; COMPTON HEATED WINDS; BINARY EXO 0748-676; NEUTRON-STAR; MILLISECOND PULSAR; SAX J1808.4-3658; ACCRETION DISKS; MODEL ATMOSPHERES; TIMING-EXPLORER; SPECTRA AB The prototypical accretion-powered millisecond pulsar SAX J1808.4-3658 was observed simultaneously with Chandra-LETGS and RXTE-PCA near the peak of a transient outburst in November 2011. A single thermonuclear (type-I) burst was detected, the brightest yet observed by Chandra from any source, and the second-brightest observed by RXTE. We found no evidence for discrete spectral features during the burst; absorption edges have been predicted to be present in such bursts, but may require a greater degree of photospheric expansion than the rather moderate expansion seen in this event (a factor of a few). These observations provide a unique data set to study an X-ray burst over a broad bandpass and at high spectral resolution (lambda/Delta lambda = 200-400). We find a significant excess of photons at high and low energies compared to the standard black body spectrum. This excess is well described by a 20-fold increase of the persistent flux during the burst. We speculate that this results from burst photons being scattered in the accretion disk corona. These and other recent observations of X-ray bursts point out the need for detailed theoretical modeling of the radiative and hydrodynamical interaction between thermonuclear X-ray bursts and accretion disks. C1 [in 't Zand, J. J. M.; Jonker, P. G.] SRON Netherlands Inst Space Res, NL-3584 CA Utrecht, Netherlands. [Galloway, D. K.] Monash Univ, Sch Math Sci, Monash Ctr Astrophys, Clayton, Vic 3800, Australia. [Galloway, D. K.] Monash Univ, Sch Phys, Clayton, Vic 3800, Australia. [Marshall, H. L.; Weinberg, N. N.] MIT, Dept Phys, Cambridge, MA 02139 USA. [Marshall, H. L.; Weinberg, N. N.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Ballantyne, D. R.] Georgia Inst Technol, Sch Phys, Ctr Relativist Astrophys, Atlanta, GA 30332 USA. [Jonker, P. G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Jonker, P. G.] Radboud Univ Nijmegen, Dept Astrophys IMAPP, NL-6500 GL Nijmegen, Netherlands. [Paerels, F. B. S.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA. [Palmer, D. M.] Los Alamos Natl Lab, Los Alamos, NM 87545 USA. [Patruno, A.] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 XH Amsterdam, Netherlands. RP in 't Zand, JJM (reprint author), SRON Netherlands Inst Space Res, Sorbonnelaan 2, NL-3584 CA Utrecht, Netherlands. EM jeanz@sron.nl OI Galloway, Duncan/0000-0002-6558-5121 NR 56 TC 12 Z9 12 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 MAY PY 2013 VL 553 AR UNSP A83 DI 10.1051/0004-6361/201321056 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 156YA UT WOS:000319858700083 ER PT J AU Kovacs, G Kovacs, T Hartman, JD Bakos, GA Bieryla, A Latham, D Noyes, RW Regaly, Z Esquerdo, GA AF Kovacs, G. Kovacs, T. Hartman, J. D. Bakos, G. A. Bieryla, A. Latham, D. Noyes, R. W. Regaly, Zs Esquerdo, G. A. TI Comprehensive time series analysis of the transiting extrasolar planet WASP-33b SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE planets and satellites: individual: WASP-33b; stars: variables: delta Scuti; methods: data analysis ID EXOPLANETARY SYSTEM; KEPLER OBSERVATIONS; LIGHT CURVES; STAR; ORBIT; FIELD; PARAMETERS; STARSPOTS; ALGORITHM; STELLAR AB Context. HD 15082 (WASP-33) is the hottest and fastest rotating star known to harbor a transiting extrasolar planet (WASP-33b). The lack of high precision radial velocity (RV) data stresses the need for precise light curve analysis and gathering further RV data. Aims. By using available photometric and RV data, we perform a blend analysis, compute more accurate system parameters, confine the planetary mass, and, attempt to cast light on the observed transit anomalies. Methods. We combined the original HATNet observations and various followup data to jointly analyze the signal content and extract the transit component and used our RV data to aid the global parameter determination. Results. The blend analysis of the combination of multicolor light curves yields the first independent confirmation of the planetary nature of WASP-33b. We clearly identify three frequency components in the 15-21 d(-1) regime with amplitudes 7-5 mmag. These frequencies correspond to the delta Scuti-type pulsation of the host star. None of these pulsation frequencies or their low-order linear combinations are in close resonance with the orbital frequency. We show that these pulsation components explain some but not all of the observed transit anomalies. The grand-averaged transit light curve shows that there is a similar to 1.5 mmag brightening shortly after the planet passes the mid-transit phase. Although the duration and amplitude of this brightening varies, it is visible even through the direct inspections of the individual transit events (some 40-60% of the followup light curves show this phenomenon). We suggest that the most likely explanation of this feature is the presence of a well-populated spot belt which is highly inclined to the orbital plane. This geometry is consistent with the inference from the spectroscopic anomalies. Finally, we constrain the planetary mass to M-p = 3.27 +/- 0.73 M-J by using our RV data collected by the TRES spectrograph. C1 [Kovacs, G.; Kovacs, T.; Regaly, Zs] Konkoly Observ Budapest, H-1121 Budapest, Hungary. [Kovacs, G.] Univ N Dakota, Dept Phys & Astrophys, Grand Forks, ND 58202 USA. [Hartman, J. D.; Bakos, G. A.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. [Bieryla, A.; Latham, D.; Noyes, R. W.; Esquerdo, G. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Kovacs, G (reprint author), Konkoly Observ Budapest, H-1121 Budapest, Hungary. EM kovacs@konkoly.hu OI Hartman, Joel/0000-0001-8732-6166 FU Hungarian Scientific Research Foundation (OTKA) [K-81373]; NSF [AST-1108686]; Hungarian OTKA [K-83790, MB08C-81013]; Hungarian Academy of Science FX The results presented in this paper have been greatly benefited from the archive of Exoplanet Transit Database (ETD) maintained by Stanislav Poddany, Lubos Brat and Ondrej Pejcha. We thank for their prompt and helpful feedback on our questions occurring during the analysis. We also thank to the numerous professional amateur observers who feed this site. Useful correspondence on the transit anomalies with ETD contributors Ramon Naves and Eugene Sokov are appreciated. Thanks are due to Pedro Valdes Sada, who sent us the data on WASP-33 gathered at Kitt Peak. We thank Attila Szing for performing the observations on November 24/25, 2011 and Andras Pal for making his astrometric routine available to us. Thanks are also due to Katalin Olah for discussions on stellar activity, to Jan Budaj for helping us to revisit the Roche-filling factor and to the referee whose thorough review helped us substantially in revising the paper. G.K. and T.K. acknowledge the support of the Hungarian Scientific Research Foundation (OTKA) through grant K-81373. G.A.B. and J.D.H. acknowledges partial support from NSF grant AST-1108686. Zs.R. has been supported by the Hungarian OTKA Grants K-83790 and MB08C-81013, and the "Lendulet" Program of the Hungarian Academy of Science. This research has made use of the SIMBAD database, operated at CDS, Strasbourg, France. NR 51 TC 13 Z9 13 U1 1 U2 2 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD MAY PY 2013 VL 553 AR A44 DI 10.1051/0004-6361/201219642 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 156YA UT WOS:000319858700044 ER PT J AU Magnelli, B Popesso, P Berta, S Pozzi, F Elbaz, D Lutz, D Dickinson, M Altieri, B Andreani, P Aussel, H Bethermin, M Bongiovanni, A Cepa, J Charmandaris, V Chary, RR Cimatti, A Daddi, E Schreiber, NMF Genzel, R Gruppioni, C Harwit, M Hwang, HS Ivison, RJ Magdis, G Maiolino, R Murphy, E Nordon, R Pannella, M Garcia, AP Poglitsch, A Rosario, D Sanchez-Portal, M Santini, P Scott, D Sturm, E Tacconi, LJ Valtchanov, I AF Magnelli, B. Popesso, P. Berta, S. Pozzi, F. Elbaz, D. Lutz, D. Dickinson, M. Altieri, B. Andreani, P. Aussel, H. Bethermin, M. Bongiovanni, A. Cepa, J. Charmandaris, V. Chary, R. -R. Cimatti, A. Daddi, E. Schreiber, N. M. Foerster Genzel, R. Gruppioni, C. Harwit, M. Hwang, H. S. Ivison, R. J. Magdis, G. Maiolino, R. Murphy, E. Nordon, R. Pannella, M. Perez Garcia, A. Poglitsch, A. Rosario, D. Sanchez-Portal, M. Santini, P. Scott, D. Sturm, E. Tacconi, L. J. Valtchanov, I. TI The deepest Herschel-PACS far-infrared survey: number counts and infrared luminosity functions from combined PEP/GOODS-H observations SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE galaxies: evolution; infrared: galaxies; galaxies: starburst; galaxies: statistics ID STAR-FORMATION HISTORY; SPECTRAL ENERGY-DISTRIBUTIONS; MULTIBAND IMAGING PHOTOMETER; SPACE-TELESCOPE OBSERVATIONS; EXTRAGALACTIC LEGACY SURVEY; FIELD-SOUTH SURVEY; FORMING GALAXIES; SOURCE CATALOGS; GOODS-NORTH; EVOLUTION AB We present results from the deepest Herschel-Photodetector Array Camera and Spectrometer (PACS) far-infrared blank field extragalactic survey, obtained by combining observations of the Great Observatories Origins Deep Survey (GOODS) fields from the PACS Evolutionary Probe (PEP) and GOODS-Herschel key programmes. We describe data reduction and the construction of images and catalogues. In the deepest parts of the GOODS-S field, the catalogues reach 3 sigma depths of 0.9, 0.6 and 1.3 mJy at 70, 100 and 160 mu m, respectively, and resolve similar to 75% of the cosmic infrared background at 100 mu m and 160 mu m into individually detected sources. We use these data to estimate the PACS confusion noise, to derive the PACS number counts down to unprecedented depths, and to determine the infrared luminosity function of galaxies down to L-IR = 10(11) L-circle dot at z similar to 1 and L-IR = 10(12) L-circle dot at z similar to 2, respectively. For the infrared luminosity function of galaxies, our deep Herschel far-infrared observations are fundamental because they provide more accurate infrared luminosity estimates than those previously obtained from mid-infrared observations. Maps and source catalogues (>3 sigma) are now publicly released. Combined with the large wealth of multi-wavelength data available for the GOODS fields, these data provide a powerful new tool for studying galaxy evolution over a broad range of redshifts. C1 [Magnelli, B.; Popesso, P.; Berta, S.; Lutz, D.; Schreiber, N. M. Foerster; Genzel, R.; Poglitsch, A.; Rosario, D.; Sturm, E.; Tacconi, L. J.] Max Planck Inst Extraterr Phys MPE, D-85741 Garching, Germany. [Magnelli, B.] Univ Bonn, Argelander Inst Astron, D-53121 Bonn, Germany. [Pozzi, F.; Cimatti, A.] Univ Bologna, Dipartimento Astron, I-40127 Bologna, Italy. [Elbaz, D.; Aussel, H.; Bethermin, M.; Daddi, E.; Pannella, M.] Univ Paris Diderot, CNRS, CEA, Lab AIM,CEA Saclay,IRFU,Serv Astrophys,DSM, F-91191 Gif Sur Yvette, France. [Dickinson, M.] Natl Opt Astron Observ, Tucson, AZ 85719 USA. [Altieri, B.; Sanchez-Portal, M.; Valtchanov, I.] ESAC, Herschel Sci Ctr, Madrid 28691, Spain. [Andreani, P.] ESO, D-85748 Garching, Germany. [Andreani, P.] INAF, Osservatorio Astron Trieste, I-34143 Trieste, Italy. [Bongiovanni, A.; Cepa, J.; Perez Garcia, A.] Inst Astrofis Canarias, E-38200 San Cristobal la Laguna, Spain. [Bongiovanni, A.; Cepa, J.; Perez Garcia, A.] Univ la Laguna, Dept Astrofis, E-38207 San Cristobal de la Laguna, Spain. [Charmandaris, V.] Univ Crete, Dept Phys, Iraklion 71002, Greece. [Charmandaris, V.] Univ Crete, Inst Theoret & Computat Phys, Iraklion 71002, Greece. [Charmandaris, V.] Observ Paris, F-75014 Paris, France. [Charmandaris, V.] IESL Fdn Res & Technol Hellas, Iraklion 71110, Greece. [Chary, R. -R.] CALTECH, Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA. [Gruppioni, C.] Osservatorio Astron Bologna, INAF, I-40127 Bologna, Italy. [Harwit, M.] Cornell Univ, Ctr Radiophys & Space Res, Ithaca, NY 14853 USA. [Hwang, H. S.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. [Ivison, R. J.] Royal Observ, UK Astron Technol Ctr, Edinburgh EH9 3HJ, Midlothian, Scotland. [Magdis, G.] Univ Oxford, Dept Phys, Oxford OX1 3RH, England. [Maiolino, R.] Univ Cambridge, Cavendish Lab, Cambridge CB3 0HE, England. [Murphy, E.] Observ Carnegie Inst Sci, Pasadena, CA 91101 USA. [Nordon, R.] Tel Aviv Univ, Raymond & Beverly Sackler Fac Exact Sci, Sch Phys & Astron, IL-69978 Tel Aviv, Israel. [Santini, P.] Osserv Astron Roma, INAF, I-00040 Monte Porzio Catone, Italy. [Scott, D.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada. RP Magnelli, B (reprint author), Max Planck Inst Extraterr Phys MPE, Postfach 1312, D-85741 Garching, Germany. EM magnelli@astro.uni-bonn.de RI Charmandaris, Vassilis/A-7196-2008; Magdis, Georgios/C-7295-2014; Daddi, Emanuele/D-1649-2012; Bongiovanni, Angel/J-6176-2012; Ivison, R./G-4450-2011; OI Bethermin, Matthieu/0000-0002-3915-2015; Santini, Paola/0000-0002-9334-8705; Charmandaris, Vassilis/0000-0002-2688-1956; Magdis, Georgios/0000-0002-4872-2294; Daddi, Emanuele/0000-0002-3331-9590; Ivison, R./0000-0001-5118-1313; Gruppioni, Carlotta/0000-0002-5836-4056; Scott, Douglas/0000-0002-6878-9840; Altieri, Bruno/0000-0003-3936-0284 FU BMVIT (Austria); ESA-PRODEX (Belgium); CEA/CNES (France); DLR (Germany); ASI/INAF (Italy); CICYT/MCYT (Spain); NASA through JPL/Caltech FX We thank the anonymous referee for suggestions which greatly enhanced this work. 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); and 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). Support for this work was provided by the NASA through an award issued by JPL/Caltech NR 84 TC 114 Z9 113 U1 1 U2 9 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 MAY PY 2013 VL 553 AR UNSP A132 DI 10.1051/0004-6361/201321371 PG 22 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 156YA UT WOS:000319858700132 ER PT J AU Basset, Y Eastwood, R Sam, L Lohman, DJ Novotny, V Treuer, T Miller, SE Weiblen, GD Pierce, NE Bunyavejchewin, S Sakchoowong, W Kongnoo, P Osorio-Arenas, MA AF Basset, Yves Eastwood, Rod Sam, Legi Lohman, David J. Novotny, Vojtech Treuer, Tim Miller, Scott E. Weiblen, George D. Pierce, Naomi E. Bunyavejchewin, Sarayudh Sakchoowong, Watana Kongnoo, Pitoon Osorio-Arenas, Miguel A. TI Cross-continental comparisons of butterfly assemblages in tropical rainforests: implications for biological monitoring SO INSECT CONSERVATION AND DIVERSITY LA English DT Article DE Barro Colorado Island; biological monitoring; Center for Tropical Forest Science; Lepidoptera; Panama; Papua New Guinea; Pollard Walks; Thailand; tropical rainforest ID SPECIES-DIVERSITY; INSECT DIVERSITY; DRY FOREST; CLIMATE; TEMPERATURE; COMMUNITY; ECOLOGY; CONSERVATION; DISTURBANCE; ABUNDANCE AB . 1.Standardised transect counts of butterflies in old-growth rainforests in different biogeographical regions are lacking. Such data are needed to mitigate the influence of methodological and environmental factors within and between sites and, ultimately, to discriminate between long-term trends and short-term stochastic changes in abundance and community composition. 2.We compared butterfly assemblages using standardised Pollard Walks in the understory of closed-canopy lowland tropical rainforests across three biogeographical regions: Barro Colorado Island (BCI), Panama; Khao Chong (KHC), Thailand; and Wanang (WAN), Papua New Guinea. 3.The length and duration of transects, their spatial autocorrelation, and number of surveys per year represented important methodological factors that strongly influenced estimates of butterfly abundance. Of these, the effect of spatial autocorrelation was most difficult to mitigate across study sites. 4.Butterfly abundance and faunal composition were best explained by air temperature, elevation, rainfall, wind velocity, and human disturbance at BCI and KHC. In the absence of weather data at WAN, duration of transects and number of forest gaps accounted for most of the explained variance, which was rather low in all cases (<33%). 5.Adequate monitoring of the abundance of common butterflies was achieved at the 50ha BCI plot, with three observers walking each of 10 transects of 500m for 30min each, during each of four surveys per year. These data may be standardised further after removing outliers of temperature and rainfall. Practical procedures are suggested to implement global monitoring of rainforest butterflies with Pollard Walks. C1 [Basset, Yves; Osorio-Arenas, Miguel A.] Smithsonian Trop Res Inst, Panama City, Panama. [Eastwood, Rod; Lohman, David J.; Treuer, Tim; Pierce, Naomi E.] Harvard Univ, Museum Comparat Zool, Cambridge, MA 02138 USA. [Sam, Legi] New Guinea Binatang Res Ctr, Madang, Papua N Guinea. [Lohman, David J.] CUNY City Coll, Dept Biol, New York, NY USA. [Novotny, Vojtech] Acad Sci Czech Republic, Biol Ctr, Ceske Budejovice, Czech Republic. [Novotny, Vojtech] Univ South Bohemia, Sch Biol Sci, Ceske Budejovice, Czech Republic. [Miller, Scott E.] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA. [Weiblen, George D.] Univ Minnesota, Bell Museum Nat Hist, St Paul, MN 55108 USA. [Bunyavejchewin, Sarayudh; Sakchoowong, Watana] Thai Natl Pk Wildlife & Plant Conservat Dept, Bangkok, Thailand. [Kongnoo, Pitoon] Khao Chong Bot Garden, Ctr Trop Forest Sci, Trang, Thailand. RP Basset, Y (reprint author), Smithsonian Trop Res Inst, Apartado 0843-03092, Panama City, Panama. EM bassety@si.edu RI Basset, Yves/B-6642-2014; Novotny, Vojtech/G-9434-2014; OI Novotny, Vojtech/0000-0001-7918-8023; Miller, Scott/0000-0002-4138-1378; Sam, Legi/0000-0003-2351-9529 FU CTFS; Arnold Arboretum of Harvard University; Harvard University Center for the Environment; Darwin Initiative for the Survival of Species, US National Science Foundation [DEB0816749]; Czech National Science Foundation [206/09/0115, P505/10/0673]; Czech Ministry of Education [ME09082, LC06073]; International Foundation For Science [D/4986-1] FX Work at BCI and KHC was funded by the CTFS, the Arnold Arboretum of Harvard University, and grants from the Harvard University Center for the Environment to N.E.P. and from CTFS to D.J.L. Research at WAN was funded by the Darwin Initiative for the Survival of Species, US National Science Foundation grant DEB0816749, Czech National Science Foundation grants 206/09/0115 and P505/10/0673, Czech Ministry of Education ME09082 and LC06073 grants, and International Foundation For Science grant D/4986-1. S. Kiratiprayoon and S. Davies helped us to implement our protocols at KHC. Y. Gonzalez, I. Rivas, C. DeLeon, F. Perez, R. Bobadilla (BCI), T. Tongrod, M. Reinkaw (KHC), and F. Kimbeng (WAN) recorded butterflies in transects. J. Tennent assisted with species identifications at WAN. Comments by O. Lewis and three anonymous reviewers greatly improved the text. NR 52 TC 8 Z9 8 U1 6 U2 48 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1752-458X J9 INSECT CONSERV DIVER JI Insect. Conserv. Divers. PD MAY PY 2013 VL 6 IS 3 BP 223 EP 233 DI 10.1111/j.1752-4598.2012.00205.x PG 11 WC Biodiversity Conservation; Entomology SC Biodiversity & Conservation; Entomology GA 150QR UT WOS:000319406400003 ER PT J AU Boel, LWT Ortner, DJ AF Boel, L. W. T. Ortner, D. J. TI Skeletal Manifestations of Skin Ulcer in the Lower Leg SO INTERNATIONAL JOURNAL OF OSTEOARCHAEOLOGY LA English DT Article DE bone pathology; palaeopathology; periostitis; ulcer ID PATHOLOGY; DISEASE AB Skin ulcers of the lower leg are known to cause both destructive and, more commonly, bone-forming lesions. Typically, bone-forming lesions in this disorder have clearly defined margins although there may be extensive reactive bone formation involving much or all of the adjacent diaphysis. These lesions are best described in patients from tropical areas, and in these environmental contexts, these are known as tropical ulcers, but leg ulcers can be caused by a variety of diseases and conditions, of which vascular insufficiency plays an important role among the elderly. The lesions are important clinically because of the disability associated with the ulcer and because of complications that can develop including osteomyelitis and cancer. In most cases, the bone lesions caused by ulcer are easily diagnosed in archaeological human skeletal remains and provide some insight into the prevalence of this disorder in antiquity.In this paper, we review the gross and radiological manifestations of bone lesions resulting from overlying skin ulcer in tibiae of 13 cases including archaeological and modern medically documented skeletons. In two of the cases, there is medical documentation regarding the presence of a chronic ulcer on the lower leg. The objectives of this paper were to explore the diversity of bone lesions associated with ulcers of the tibia and to provide an improved basis for the diagnosis of this disorder in human skeletal remains. Copyright (c) 2011 John Wiley & Sons, Ltd. C1 [Boel, L. W. T.] Univ Aarhus, Dept Forens Med, DK-8200 Aarhus N, Denmark. [Ortner, D. J.] Smithsonian Inst, Dept Anthropol, Washington, DC 20560 USA. RP Boel, LWT (reprint author), Univ Aarhus, Dept Forens Med, Brendstrupgaardsvej 100, DK-8200 Aarhus N, Denmark. EM lwb@forensic.au.dk NR 17 TC 3 Z9 3 U1 1 U2 26 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1047-482X J9 INT J OSTEOARCHAEOL JI Int. J. Osteoarchaeol. PD MAY-JUN PY 2013 VL 23 IS 3 BP 303 EP 309 DI 10.1002/oa.1248 PG 7 WC Anthropology; Archaeology SC Anthropology; Archaeology GA 160JH UT WOS:000320115200005 ER PT J AU Abbondanza, FN Power, ML Dickson, MA Brown, J Oftedal, OT AF Abbondanza, Frances N. Power, Michael L. Dickson, Melissa A. Brown, Janine Oftedal, Olav T. TI Variation in the Composition of Milk of Asian Elephants (Elephas maximus) Throughout Lactation SO ZOO BIOLOGY LA English DT Article DE lactation; milk constituents; milk replacers ID AFRICAN ELEPHANT; LOXODONTA-AFRICANA; MAMMARY-GLAND; OLIGOSACCHARIDES; COLOSTRUM; LACTOSE; GROWTH AB We investigated milk nutrient composition from three Asian elephant cows over the first 3 years of lactation, including two consecutive lactations in one cow. Body mass gain is presented for three calves during the first year. Milk samples (n = 74) were analyzed for dry matter (DM), fat, crude protein (CP), sugar, ash, calcium (Ca), phosphorus (P), and potassium (K); gross energy (GE) was calculated. Concentrations of most nutrients changed over lactation: DM, fat, CP, Ca, P, and GE were positively correlated to calf age; sugar was negatively correlated to calf age. GE doubled between birth (1 kcal/g) and 2 years of age (2 kcal/g). After accounting for calf age, GE, fat, Ca, and P concentrations differed among the cows. Milk composition also differed between two lactations from the same cow. When milk nutrients were expressed on a mg per kcal basis, the pattern changes: CP, Ca, and P remained relatively constant over lactation on a per energy basis. Calf mass quadrupled over the first year of life; mass gain was linear at 0.9 kg/day. Asian elephant milk composition is variable, both across lactations and between cows, complicating efforts to determine representative values for comparative studies and for the formulation of elephant milk formulas. The fact that CP, Ca, and P were all relatively constant when expressed on a per energy basis may be of biological significance. The increase in nutrient density over lactation undoubtedly limits maternal water loss, reducing the volume of milk necessary to support the calf. Zoo Biol 32:291-298, 2013. (c) 2012 Wiley Periodicals, Inc. C1 [Abbondanza, Frances N.; Brown, Janine] Smithsonian Conservat Biol Inst, Dept Ctr Species Survival, Front Royal, VA 22630 USA. [Power, Michael L.] Smithsonian Conservat Biol Inst, Natl Zool Pk, Conservat Ecol Ctr, Nutr Lab, Washington, DC USA. [Power, Michael L.] Amer Coll Obstetricians & Gynecologists, Res Dept, Washington, DC 20024 USA. [Dickson, Melissa A.] Dickerson Pk Zoo, Springfield, MO USA. [Oftedal, Olav T.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. RP Abbondanza, FN (reprint author), Smithsonian Conservat Biol Inst, 1500 Remount Rd, Front Royal, VA 22630 USA. EM Parkern@si.edu OI Power, Michael/0000-0002-6120-3528 NR 43 TC 3 Z9 3 U1 1 U2 30 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0733-3188 J9 ZOO BIOL JI Zoo Biol. PD MAY-JUN PY 2013 VL 32 IS 3 BP 291 EP 298 DI 10.1002/zoo.21022 PG 8 WC Veterinary Sciences; Zoology SC Veterinary Sciences; Zoology GA 160SG UT WOS:000320139100009 PM 22588804 ER PT J AU Ballance, CP Loch, SD Foster, AR Smith, RK Witthoeft, MC Kallman, TR AF Ballance, C. P. Loch, S. D. Foster, A. R. Smith, R. K. Witthoeft, M. C. Kallman, T. R. TI UNCERTAINTIES ON ATOMIC DATA SO FUSION SCIENCE AND TECHNOLOGY LA English DT Article; Proceedings Paper CT Technical Meeting on Data Evaluation for Atomic, Molecular and Plasma-Material Interaction Processes in Fusion CY SEP 04-07, 2012 CL Daejeon, SOUTH KOREA DE uncertainty estimates on atomic data; collisional radiative modeling; R-matrix ID ELECTRON-IMPACT EXCITATION; RECOMBINATION; PLASMAS; IONS AB There have been long outstanding requests from the modeling community for uncertainty estimates on atomic data. This paper outlines a systematic approach from fundamental atomic structure and collisional calculations, through to well-known spectral diagnostic lines, correlating the uncertainties from each contributing process. C1 [Ballance, C. P.; Loch, S. D.] Auburn Univ, Dept Phys, Allison Lab 206, Auburn, AL 36849 USA. [Foster, A. R.; Smith, R. K.] Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom & Mol Phys, Cambridge, MA 02138 USA. [Witthoeft, M. C.; Kallman, T. R.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Ballance, CP (reprint author), Auburn Univ, Dept Phys, Allison Lab 206, Auburn, AL 36849 USA. EM ballance@physics.auburn.edu FU U.S. Department of Energy FX C. P. B. acknowledges the invitation by the International Atomic Energy Agency (IAEA) and the support of the National Fusion Research Institute (NFRI) for his participation in the Joint IAEA-NFRI Technical Meeting on Data Evaluation. A part of this work was funded by the U.S. Department of Energy, and the O VII calculations were carried out at the National Energy Research Scientific Computing Center computing facilities in Berkeley, California. NR 7 TC 1 Z9 1 U1 0 U2 8 PU AMER NUCLEAR SOC PI LA GRANGE PK PA 555 N KENSINGTON AVE, LA GRANGE PK, IL 60526 USA SN 1536-1055 EI 1943-7641 J9 FUSION SCI TECHNOL JI Fusion Sci. Technol. PD MAY PY 2013 VL 63 IS 3 BP 358 EP 362 PG 5 WC Nuclear Science & Technology SC Nuclear Science & Technology GA 148KX UT WOS:000319244600007 ER PT J AU Zamora, S Darroch, S Rahman, IA AF Zamora, Samuel Darroch, Simon Rahman, Imran A. TI Taphonomy and ontogeny of early pelmatozoan echinoderms: A case study of a mass-mortality assemblage of Gogia from the Cambrian of North America SO PALAEOGEOGRAPHY PALAEOCLIMATOLOGY PALAEOECOLOGY LA English DT Article DE Gogia; Echinoderms; Cambrian; Population; Taphonomy; Ontogeny ID GUIZHOU PROVINCE; SPENCE SHALE; BLASTOZOAN ECHINODERMS; PALEOZOIC ECHINODERMS; STALKED ECHINODERMS; KAILI BIOTA; DEEP-SEA; CRINOIDS; UTAH; CHINA AB During the Palaeozoic, pelmatozoan echinoderms were substantially more diverse than they are in modern oceans; however, the taphonomy and ontogeny of many of these extinct groups is poorly known. Here, we report an exceptional mass-mortality assemblage of the basal pelmatozoan Gogia sp., which consists of 106 articulated and nearly complete specimens preserved on a single bedding plane. This slab was collected from the middle Cambrian Spence Shale of Utah, USA, which is characterized by a high-diversity echinoderm fauna that inhabited relatively deepwater distal-ramp settings on a subsiding passive margin of Laurentia. The preferential orientation of specimens strongly suggests that all the animals were entombed by a single unidirectional obrution event; the specimens were most likely derived from a nearby area and represent a single population that was living under the same environmental conditions. Statistical analysis of the thecal heights of specimens, taken as a proxy for age, reveals a bimodal distribution, suggesting that there were at least two episodes of larval settling in the original population. This implies that gogiids displayed seasonal cycles of reproduction, as do many modern echinoderms in equivalent environmental settings. During ontogeny, the theca and stem of Gogia sp. grew by increasing the size of plates, as well as through the incorporation of new plates (e.g., in the sutures between existing ones). The brachioles, by contrast, were more conservative developmentally, and the size of plates was maintained through ontogeny; they grew exclusively through the distal addition of new plates. The epispires, which were used for respiration, are more numerous in adults, as are the brachioles, indicating a degree of metabolic control on the development of these structures. This study demonstrates that taxonomic studies of gogiids should, wherever possible, consider a large number of specimens encompassing a range of sizes in order to clearly distinguish between ontogenetic and interspecific morphological variation. Published by Elsevier B.V. C1 [Zamora, Samuel] Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20013 USA. [Darroch, Simon] Yale Univ, New Haven, CT 06520 USA. [Rahman, Imran A.] Univ Bristol, Sch Earth Sci, Bristol BS8 1RJ, Avon, England. RP Zamora, S (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20013 USA. EM samuel@unizar.es; simon.darroch@yale.edu; imran.rahman@bristol.ac.uk RI Rahman, Imran/F-4224-2012 OI Rahman, Imran/0000-0001-6598-6534 FU Spanish Ministry of Science and Education MEC-FEDER-EU [CGL2011-24516]; Smithsonian Institution; Yale Peabody Museum of Natural History; Natural Environment Research Council [NE/H015817/1] FX The authors would like to thank Tatsuo Oji, Colin Sumrall and Aaron Hunter for their valuable discussions on the structure and ecology of echinoderm meadows. Pincelli Hull and Gene Hunt provided advice on the uses and applications of BIC. Isabel Perez provided assistance in the preparation of the photographs, plates and video. Special thanks are due to Val and Glade Gunther for collecting the slab, and for providing crucial locality and stratigraphic information that made this study possible. We are grateful to two anonymous reviewers whose insightful comments helped improve the final manuscript. S.Z. was funded by the Spanish Ministry of Science and Education MEC-FEDER-EU (project CGL2011-24516) and a Post Doctoral grant at the Smithsonian Institution. S.D. was supported by the Yale Peabody Museum of Natural History. I.A.R. was funded by the Natural Environment Research Council (grant number NE/H015817/1). NR 67 TC 10 Z9 10 U1 1 U2 12 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0031-0182 EI 1872-616X J9 PALAEOGEOGR PALAEOCL JI Paleogeogr. Paleoclimatol. Paleoecol. PD MAY 1 PY 2013 VL 377 BP 62 EP 72 DI 10.1016/j.palaeo.2013.03.009 PG 11 WC Geography, Physical; Geosciences, Multidisciplinary; Paleontology SC Physical Geography; Geology; Paleontology GA 143SV UT WOS:000318889400006 ER PT J AU Tiansawat, P Dalling, JW AF Tiansawat, Pimonrat Dalling, James W. TI Differential seed germination responses to the ratio of red to far-red light in temperate and tropical species SO PLANT ECOLOGY LA English DT Article DE Regeneration niche; Light dependence; Light quality; Seed mass; Lambir Hill National Park ID NEOTROPICAL PIONEERS; LEAF-LITTER; SOIL; SIZE; FOREST; PERSISTENCE; TREE; DISPERSAL; SHAPE; CANOPY AB Variation in vegetation density creates a range of red to far-red ratios of irradiance (R:FR) potentially permitting fine-scale discrimination of light conditions for seed germination. However, remarkably few studies have explored whether R:FR responses of germination vary among species that differ in distribution and life-history traits. In this study, we explored the relationships between R:FR requirements and four species characteristics: seed mass, latitudinal distribution (tropical vs. temperate), seed dormancy (dormant vs. nondormant), and plant growth form (woody vs. nonwoody). We obtained data on germination response to R:FR of 62 species from published literature and added new data for ten species from aseasonal tropical forests in Borneo. First, we analyzed whether species characteristics influenced overall light dependency of germination using phylogenetic logistic regression. We found that seed mass had a strong negative effect on light dependency, but that the seed mass at which tropical taxa had a 50 % probability of light dependency was 40 times that of temperate taxa. For light-dependent species, we found that the threshold R:FR that stimulates 50 % of maximum germination (R:FR50) was also related to seed mass and latitudinal distribution. In agreement with an earlier study, we found that for temperate taxa, the R:FR50 was significantly negatively correlated with seed mass. In contrast, for 22 tropical taxa, we found a significant positive correlation. These opposing relationships suggest contrasting selection pressures on germination responses of tropical taxa (mostly trees) and temperate herbaceous plants, and which are likely related to differences in seed longevity, seed burial rates, and reproductive output. C1 [Tiansawat, Pimonrat; Dalling, James W.] Univ Illinois, Dept Plant Biol, Urbana, IL 61801 USA. [Dalling, James W.] Smithsonian Trop Res Inst, Ancon, Panama. RP Tiansawat, P (reprint author), Univ Illinois, Dept Plant Biol, 265 Morrill Hall 505 South Goodwin Ave, Urbana, IL 61801 USA. EM ptiansa2@illinois.edu OI Tiansawat, Pimonrat/0000-0003-1354-1247 FU Center for Tropical Forest Science; Royal Thai Government Scholarship FX The authors thank Yuji Tokumoto for help in providing Dillenia suffruticosa seeds. The authors express their gratitude to Carol Augspurger, Adam Davis, and two anonymous reviewers for helpful comments on the study. This study is partly funded by the 2010 grant program of the Center for Tropical Forest Science and Royal Thai Government Scholarship. NR 63 TC 0 Z9 1 U1 2 U2 58 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 1385-0237 J9 PLANT ECOL JI Plant Ecol. PD MAY PY 2013 VL 214 IS 5 BP 751 EP 764 DI 10.1007/s11258-013-0205-y PG 14 WC Plant Sciences; Ecology; Forestry SC Plant Sciences; Environmental Sciences & Ecology; Forestry GA 146DN UT WOS:000319069600007 ER PT J AU Yang, J Swenson, NG Cao, M Chuyong, GB Ewango, CEN Howe, R Kenfack, D Thomas, D Wolf, A Lin, LX AF Yang, Jie Swenson, Nathan G. Cao, Min Chuyong, George B. Ewango, Corneille E. N. Howe, Robert Kenfack, David Thomas, Duncan Wolf, Amy Lin, Luxiang TI A Phylogenetic Perspective on the Individual Species-Area Relationship in Temperate and Tropical Tree Communities SO PLOS ONE LA English DT Article ID NEUTRAL THEORY; NULL MODELS; RAIN-FOREST; DIVERSITY; ECOLOGY; BIODIVERSITY; EQUIVALENCE; EVOLUTION; TRAITS; CHINA AB Ecologists have historically used species-area relationships (SARs) as a tool to understand the spatial distribution of species. Recent work has extended SARs to focus on individual-level distributions to generate individual species area relationships (ISARs). The ISAR approach quantifies whether individuals of a species tend have more or less species richness surrounding them than expected by chance. By identifying richness 'accumulators' and 'repellers', respectively, the ISAR approach has been used to infer the relative importance of abiotic and biotic interactions and neutrality. A clear limitation of the SAR and ISAR approaches is that all species are treated as evolutionarily independent and that a large amount of work has now shown that local tree neighborhoods exhibit non-random phylogenetic structure given the species richness. Here, we use nine tropical and temperate forest dynamics plots to ask: (i) do ISARs change predictably across latitude?; (ii) is the phylogenetic diversity in the neighborhood of species accumulators and repellers higher or lower than that expected given the observed species richness?; and (iii) do species accumulators, repellers distributed non-randomly on the community phylogenetic tree? The results indicate no clear trend in ISARs from the temperate zone to the tropics and that the phylogenetic diversity surrounding the individuals of species is generally only non-random on very local scales. Interestingly the distribution of species accumulators and repellers was non-random on the community phylogenies suggesting the presence of phylogenetic signal in the ISAR across latitude. C1 [Yang, Jie; Cao, Min; Lin, Luxiang] Chinese Acad Sci, Xishuangbanna Trop Bot Garden, Key Lab Trop Forest Ecol, Kunming, Peoples R China. [Yang, Jie] Chinese Acad Sci, Grad Univ, Beijing, Peoples R China. [Swenson, Nathan G.] Michigan State Univ, Dept Plant Biol, E Lansing, MI 48824 USA. [Chuyong, George B.] Univ Buea, Dept Bot & Plant Physiol, Buea, Cameroon. [Ewango, Corneille E. N.] Ctr Format & Rech Conservat Forestiere CEFRECOF E, Reserve De Faune A Okapi, Zaire. [Howe, Robert; Wolf, Amy] Univ Wisconsin, Dept Nat & Appl Sci, Green Bay, WI 54302 USA. [Kenfack, David] Smithsonian Inst, Smithsonian Global Earth Observ Network, Washington, DC USA. [Thomas, Duncan] Oregon State Univ, Dept Bot & Plant Pathol, Corvallis, OR 97331 USA. RP Lin, LX (reprint author), Chinese Acad Sci, Xishuangbanna Trop Bot Garden, Key Lab Trop Forest Ecol, Kunming, Peoples R China. EM linluxa@xtbg.ac.cn FU United States National Science Foundation [DEB - 1046113]; National Science Foundation of China [31061160188, 31000201]; Queensland-Chinese Academy of Science Joint Biotechnology Projects [GJHZ1130] FX This work was conducted as a part of a Dimensions of Biodiversity IRCN workshop in Changbaishan, China, funded by the United States National Science Foundation (DEB - 1046113). This study was supported by the National Science Foundation of China (31061160188 and 31000201) and the Queensland-Chinese Academy of Science Joint Biotechnology Projects (GJHZ1130). The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 40 TC 4 Z9 9 U1 2 U2 54 PU PUBLIC LIBRARY SCIENCE PI SAN FRANCISCO PA 1160 BATTERY STREET, STE 100, SAN FRANCISCO, CA 94111 USA SN 1932-6203 J9 PLOS ONE JI PLoS One PD MAY 1 PY 2013 VL 8 IS 5 AR UNSP e63192 DI 10.1371/journal.pone.0063192 PG 10 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 147KY UT WOS:000319167000098 PM 23650553 ER PT J AU Stinchcomb, GE Messner, TC Williamson, FC Driese, SG Nordt, LC AF Stinchcomb, Gary E. Messner, Timothy C. Williamson, Forrest C. Driese, Steven G. Nordt, Lee C. TI Climatic and human controls on Holocene floodplain vegetation changes in eastern Pennsylvania based on the isotopic composition of soil organic matter SO QUATERNARY RESEARCH LA English DT Article DE delta C-13 of soil organic matter; Alluvial deposit; Buried soil; Holocene paleoclimate; Eastern North America ID NORTHEASTERN UNITED-STATES; LATE QUATERNARY VEGETATION; C-4 PLANT PRODUCTIVITY; AMERICAN GREAT-PLAINS; NORTH-AMERICA; NATURAL-ABUNDANCE; NEW-YORK; ECOLOGICAL CHANGE; CENTRAL TEXAS; RIVER-BASIN AB A paleoenvironmental time-series spanning the Holocene was constructed using 29 radiocarbon ages and 149 standardized delta C-13(som) values from alluvial terrace profiles along the middle Delaware River valley. There is good agreement between increasing delta C-13(som) and Panicoideae phytolith concentrations, suggesting that variations in C-4 biomass are a major contributor to changes in the soil delta C-13. A measurement error deconvolution curve over time reveals two isotope stages (II-I), with nine sub-stages exhibiting variations in average delta C-13(som) (average %C-4). Stage II, similar to 10.7-4.3 Ica, shows above-average delta C-13(som) (increase %C-4) values with evidence of an early Holocene warming and dry interval (sub-stage IIb, 9.8-83 ka) that coincides with rapid warming and cool-dry abrupt climate-change events. Sub-stage IId, 7.0-4.3 ka, is an above average delta C-13(som) (increase %C-4) interval associated with the mid-Holocene warm-dry hypsithermal. The Stage II-I shift at 4.3 ka documents a transition toward below average delta C-13(som) (decrease %C-4) values and coincides with decreasing insolation and hydroclimatic change. Sub-stages Ib and Id (above average %C.4) coincide with the first documented occurrence of maize in the northeastern USA and a substantial increase in human population during the Late Woodland. These associations suggest that people influenced delta C-13(som) during the late Holocene. (C) 2013 University of Washington. Published by Elsevier Inc. All rights reserved. C1 [Stinchcomb, Gary E.; Driese, Steven G.; Nordt, Lee C.] Baylor Univ, Dept Geol, Terr Paleoclimatol Res Grp, Waco, TX 76798 USA. [Messner, Timothy C.] Smithsonian Natl Museum Nat Hist, Dept Anthropol, Archaeobiol Program, Washington, DC USA. [Messner, Timothy C.] SUNY Coll Potsdam, Dept Anthropol, Potsdam, NY USA. [Williamson, Forrest C.] Baylor Univ, Dept Stat Sci, Waco, TX 76798 USA. RP Stinchcomb, GE (reprint author), Baylor Univ, Dept Geol, Terr Paleoclimatol Res Grp, Waco, TX 76798 USA. OI Stinchcomb, Gary/0000-0003-3220-7762 FU NSF [EAR 0823131]; Baylor research grant FX Support for this study was provided by NSF EAR 0823131 awarded to S.G. Driese, which supported radiocarbon dating, thin-sections, and delta13C analysis, and a GSA student-aid-in research grant and Baylor research grant awarded to G.E. Stinchcomb which supported radiocarbon dating. We thank Brinnen Carter and the Delaware Water Gap National Recreation Area for providing additional funds for radiocarbon dating, Chase Gerken, John McFadden, Steve Dworkin, Ren Zhang, Lauren Michel, Sally Horn, Zheng-Hua Li, and Jason Mintz for field and lab assistance, James Lee, Michael Stewart, and John Stiteler for introducing us to the Browning Site, and Jane Harvill and Jack Tubbs for statistical assistance. Derek Booth, John Dodson, and two anonymous reviewers provided comments and suggestions that greatly improved an earlier version of this manuscript. NR 109 TC 2 Z9 2 U1 4 U2 30 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0033-5894 J9 QUATERNARY RES JI Quat. Res. PD MAY PY 2013 VL 79 IS 3 BP 377 EP 390 DI 10.1016/j.yqres.2013.02.004 PG 14 WC Geography, Physical; Geosciences, Multidisciplinary SC Physical Geography; Geology GA 149GX UT WOS:000319308100007 ER PT J AU Slot, M Wright, SJ Kitajima, K AF Slot, Martijn Wright, S. Joseph Kitajima, Kaoru TI Foliar respiration and its temperature sensitivity in trees and lianas: in situ measurements in the upper canopy of a tropical forest SO TREE PHYSIOLOGY LA English DT Article DE canopy crane; carbon balance; climate change; lianas; Panama; respiration; Q(10); temperature response of respiration; tropical forest ID LEAF DARK RESPIRATION; GLOBAL VEGETATION MODELS; RAIN-FOREST; AMAZONIAN FOREST; DRY FOREST; PLANT RESPIRATION; FUNCTIONAL-GROUPS; CLIMATE-CHANGE; ECOSYSTEM; CARBON AB Leaf dark respiration (R) and its temperature sensitivity are essential for efforts to model carbon fluxes in tropical forests under current and future temperature regimes, but insufficient data exist to generalize patterns of R in species-rich tropical forests. Here, we tested the hypothesis that R and its temperature sensitivity (expressed as Q(10), the proportional increase in R with a 10 degrees C rise in temperature) vary in relation to leaf functional traits, and among plant functional types (PFTs). We conducted in situ measurements of R of 461 leaves of 26 species of tree and liana in the upper canopy of a tropical forest in Panama. A construction crane allowed repeated non-destructive access to measure leaves kept in the dark since the previous night and equilibrated to the ambient temperature of 23-31 degrees C in the morning. R at 25 degrees C (R-25) varied among species (mean 1.11 mu mol m(-2) s(-1); range 0.72-1.79 mu mol m(-2) s(-1)) but did not differ significantly among PFTs. R-25 correlated positively with photosynthetic capacity, leaf mass per unit area, concentrations of nitrogen and phosphorus, and negatively with leaf lifespan. Q(10) estimated for each species was on average higher than the 2.0 often assumed in coupled climate-vegetation models (mean 2.19; range 1.24-3.66). Early-successional tree species had higher Q(10) values than other functional types, but interspecific variation in Q(10) values was not correlated with other leaf traits. Similarity in respiration characteristics across PFTs, and relatively strong correlations of R with other leaf functional traits offer potential for trait-based vegetation modeling in species-rich tropical forests. C1 [Slot, Martijn; Kitajima, Kaoru] Univ Florida, Dept Biol, Gainesville, FL 32611 USA. [Wright, S. Joseph; Kitajima, Kaoru] Smithsonian Trop Res Inst, Balboa, Panama. RP Slot, M (reprint author), Univ Florida, Dept Biol, Gainesville, FL 32611 USA. EM mslot@ufl.edu RI Wright, Stuart/M-3311-2013 OI Wright, Stuart/0000-0003-4260-5676 FU Smithsonian Tropical Research Institute (STRI) FX M.S. was supported by a Smithsonian Tropical Research Institute (STRI) Short-term Fellowship. NR 51 TC 19 Z9 19 U1 4 U2 50 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0829-318X J9 TREE PHYSIOL JI Tree Physiol. PD MAY PY 2013 VL 33 IS 5 BP 505 EP 515 DI 10.1093/treephys/tpt026 PG 11 WC Forestry SC Forestry GA 150ZR UT WOS:000319430900006 PM 23592296 ER PT J AU Clough, GW AF Clough, G. Wayne TI Untitled 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 MAY PY 2013 VL 44 IS 2 BP 6 EP 6 PG 1 WC Humanities, Multidisciplinary SC Arts & Humanities - Other Topics GA 134DC UT WOS:000318189100002 ER PT J AU Parker, JD Torchin, ME Hufbauer, RA Lemoine, NP Alba, C Blumenthal, DM Bossdorf, O Byers, JE Dunn, AM Heckman, RW Hejda, M Jarosik, V Kanarek, AR Martin, LB Perkins, SE Pysek, P Schierenbeck, K Schloder, C van Klinken, R Vaughn, KJ Williams, W Wolfe, LM AF Parker, John D. Torchin, Mark E. Hufbauer, Ruth A. Lemoine, Nathan P. Alba, Christina Blumenthal, Dana M. Bossdorf, Oliver Byers, James E. Dunn, Alison M. Heckman, Robert W. Hejda, Martin Jarosik, Vojtech Kanarek, Andrew R. Martin, Lynn B. Perkins, Sarah E. Pysek, Petr Schierenbeck, Kristina Schloeder, Carmen van Klinken, Rieks Vaughn, Kurt J. Williams, Wyatt Wolfe, Lorne M. TI Do invasive species perform better in their new ranges? SO ECOLOGY LA English DT Article DE animal invasion; biogeography; comparative demography; invasion paradox; invasive species; plant invasion ID INCREASED COMPETITIVE ABILITY; ENEMY RELEASE HYPOTHESIS; BIOLOGICAL INVASIONS; PLANT INVASIONS; INTRODUCED POPULATIONS; NORTH-AMERICA; NATIVE RANGE; SIZE; EVOLUTION; SUCCESS AB A fundamental assumption in invasion biology is that most invasive species exhibit enhanced performance in their introduced range relative to their home ranges. This idea has given rise to numerous hypotheses explaining "invasion success" by virtue of altered ecological and evolutionary pressures. There are surprisingly few data, however, testing the underlying assumption that the performance of introduced populations, including organism size, reproductive output, and abundance, is enhanced in their introduced compared to their native range. Here, we combined data from published studies to test this hypothesis for 26 plant and 27 animal species that are considered to be invasive. On average, individuals of these 53 species were indeed larger, more fecund, and more abundant in their introduced ranges. The overall mean, however, belied significant variability among species, as roughly half of the investigated species (N = 27) performed similarly when compared to conspecific populations in their native range. Thus, although some invasive species are performing better in their new ranges, the pattern is not universal, and just as many are performing largely the same across ranges. C1 [Parker, John D.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. [Torchin, Mark E.; Schloeder, Carmen] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. [Hufbauer, Ruth A.; Williams, Wyatt] Colorado State Univ, Dept Bioagr Sci & Pest Management, Ft Collins, CO 80523 USA. [Hufbauer, Ruth A.; Williams, Wyatt] Colorado State Univ, Grad Degree Program Ecol, Ft Collins, CO 80523 USA. [Lemoine, Nathan P.] Florida Int Univ, Dept Biol, North Miami, FL 33181 USA. [Alba, Christina; Hejda, Martin; Jarosik, Vojtech; Pysek, Petr] Acad Sci Czech Republic, Inst Bot, Dept Invas Ecol, CZ-25243 Pruhonice, Czech Republic. [Blumenthal, Dana M.] USDA ARS, Ft Collins, CO 80526 USA. [Bossdorf, Oliver] Univ Bern, Inst Plant Sci, CH-3013 Bern, Switzerland. [Byers, James E.] Univ Georgia, Odum Sch Ecol, Athens, GA 30602 USA. [Dunn, Alison M.] Univ Leeds, Fac Biol Sci, Sch Biol, Leeds LS2 9JT, W Yorkshire, England. [Heckman, Robert W.] Univ N Carolina, Dept Biol, Chapel Hill, NC 27599 USA. [Jarosik, Vojtech; Pysek, Petr] Charles Univ Prague, Fac Sci, Dept Ecol, CZ-12844 Prague 2, Czech Republic. [Kanarek, Andrew R.] Univ Tennessee, Natl Inst Math & Biol Synth, Knoxville, TN 37996 USA. [Martin, Lynn B.] Univ S Florida, Dept Integrat Biol, Tampa, FL 33620 USA. [Perkins, Sarah E.] Cardiff Sch Biosci, Cardiff CF10 3AX, S Glam, Wales. [Schierenbeck, Kristina] Calif State Univ Chico, Dept Biol Sci, Chico, CA 95929 USA. [van Klinken, Rieks] CSIRO Ecosyst Sci, Brisbane, Qld 4102, Australia. [Vaughn, Kurt J.] Landowner Stewardship Program Audubon Calif, Winters, CA 95694 USA. [Wolfe, Lorne M.] Georgia So Univ, Dept Biol, Statesboro, GA 30460 USA. RP Parker, JD (reprint author), Smithsonian Environm Res Ctr, 647 Contees Wharf Rd, Edgewater, MD 21037 USA. EM parkerj@si.edu RI van Klinken, Rieks/B-1772-2009; Perkins, Sarah/B-1817-2010; Pysek, Petr/B-1957-2012; Bossdorf, Oliver/A-8328-2008; Alba, Christina/H-1579-2014; Hejda, Martin/H-1589-2014; Heckman, Robert/J-2640-2015; Parker, John/F-9761-2010; OI van Klinken, Rieks/0000-0002-7578-8977; Perkins, Sarah/0000-0002-7457-2699; Bossdorf, Oliver/0000-0001-7504-6511; Alba, Christina/0000-0001-7040-8480; Heckman, Robert/0000-0002-2281-3091; Parker, John/0000-0002-3632-7625; Dunn, Alison/0000-0002-4855-1077; Martin, Lynn/0000-0002-5887-4937 FU Global Invasions Network NSF RCN [DEB-0541673]; NSF REU site grant [NSF-DBI 0851303]; Czech Science Foundation [P505/11/1112, 206/09/0563]; long-term research development project (Academy of Sciences of the Czech Republic) [RVO 67985939]; institutional resources of the Ministry of Education, Youth and Sports of the Czech Republic; Praemium Academiae award from the Academy of Sciences of the Czech Republic; NERC [NE/G015201/1]; NSF [EF-0832858]; SNF grant [31003A_122408]; Colorado Agricultural Experiment Station; NSF RCN [DEB-0541673] FX We thank Jess Shue, Christian Latimer, Emily Myron, Madalin Parepa, Lauren Richie, and Hannah Wilbur for data entry and verification. This work was supported in part by the Global Invasions Network NSF RCN DEB-0541673 and an NSF REU site grant (NSF-DBI 0851303). Petr Pysek and Vojtech Jarosik were supported by grants no. P505/11/1112 and 206/09/0563 (Czech Science Foundation), long-term research development project no. RVO 67985939 (Academy of Sciences of the Czech Republic), and institutional resources of the Ministry of Education, Youth and Sports of the Czech Republic. Petr Pysek acknowledges the support by Praemium Academiae award from the Academy of Sciences of the Czech Republic. Alison Dunn acknowledges support from NERC (NE/G015201/1). Andrew R. Kanarek acknowledges support from NSF Award #EF-0832858. Lynn B. Martin acknowledges NSF-IOS 0940275. Oliver Bossdorf was supported by the SNF grant 31003A_122408. Ruth A. Hufbauer acknowledges support from the Colorado Agricultural Experiment Station and NSF RCN DEB-0541673. NR 56 TC 56 Z9 57 U1 12 U2 250 PU ECOLOGICAL SOC AMER PI WASHINGTON PA 1990 M STREET NW, STE 700, WASHINGTON, DC 20036 USA SN 0012-9658 EI 1939-9170 J9 ECOLOGY JI Ecology PD MAY PY 2013 VL 94 IS 5 BP 985 EP 994 PG 10 WC Ecology SC Environmental Sciences & Ecology GA 144VQ UT WOS:000318969800001 PM 23858639 ER PT J AU Chanchani, N AF Chanchani, Nachiket TI The Camera Work of Ananda Kentish Coomaraswamy and Alfred Stieglitz SO HISTORY OF PHOTOGRAPHY LA English DT Article DE Ananda Kentish Coomaraswamy (18771947); Alfred Stieglitz (18661946); Auguste Rodin (18401917); artistic exchange; ethics; Georgia O'Keeffe (18871986); labour; modernisms; modern dance; mudra; Museum of Fine Arts; Boston; straight photography; pictorialist photography; reception of South Asian art; repetition; South Asian art collections; Stella Bloch (18971999) AB In the 1920s art museums in the United States began to collect and display photographs by Alfred Stieglitz and other leading photographers as works of art. Previous scholars have acknowledged this movement's significance in Stieglitz's struggle for the institutional recognition of photography. They have, however, scarcely queried the conditions under which this movement began. This article scrutinises the circumstances under which the Museum of Fine Arts, Boston, MA, accepted prints from Stieglitz and other practitioners of the medium. It posits that the Boston Museum's decision to accept these prints was motivated by its protean curator Ananda Kentish Coomaraswamy's interest in pictorialist and photo-secessionist photography's creative and political possibilities as well as in Stieglitz's life and work. Stieglitz's pictures appealed to Coomaraswamy because he recognised in them ways in which the American photographer was referencing strands of classical South Asian aesthetics to develop more inclusive and more symbolic works of American art. One of these filaments was Stieglitz's absorption of a codified language of hand gestures assumed by dancers and deities that Coomaraswamy was concurrently documenting and interpreting in his writings, photographs and films to elevate maligned traditions of South Asian sculpture and performance as Art. In recovering this narrative of Coomraswamy and Stieglitz's overlapping lives and works, this article begins to disentangle histories of collecting, of modernist photography and of the crystallisation of South Asian art history as a scholarly discipline. C1 [Chanchani, Nachiket] Univ Michigan, Ann Arbor, MI 48109 USA. RP Chanchani, N (reprint author), Smithsonian Inst, Washington, DC 20560 USA. EM nachiket@umich.edu NR 23 TC 2 Z9 2 U1 0 U2 12 PU TAYLOR & FRANCIS LTD PI ABINGDON PA 4 PARK SQUARE, MILTON PARK, ABINGDON OX14 4RN, OXON, ENGLAND SN 0308-7298 J9 HIST PHOTOGR JI Hist. Photogr. PD MAY 1 PY 2013 VL 37 IS 2 BP 204 EP 220 DI 10.1080/03087298.2012.711903 PG 17 WC Art SC Art GA 143LB UT WOS:000318867900006 ER PT J AU Dick, SJ AF Dick, Steven J. TI The Stardust Revolution: The New Story of Our Origin in the Stars SO JOURNAL FOR THE HISTORY OF ASTRONOMY LA English DT Book Review C1 [Dick, Steven J.] NASA, Washington, DC USA. [Dick, Steven J.] Smithsonian Inst, Natl Air & Space Museum, Washington, DC 20560 USA. EM stevedick1@comcast.net NR 1 TC 0 Z9 0 U1 0 U2 1 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 MAY PY 2013 VL 44 BP 219 EP 220 PN 2 PG 2 WC History & Philosophy Of Science SC History & Philosophy of Science GA 145PH UT WOS:000319028600011 ER PT J AU Hunt, G AF Hunt, Gene TI PRESENTATION OF THE 2012 CHARLES SCHUCHERT AWARD OF THE PALEONTOLOGICAL SOCIETY TO GENE HUNT RESPONSE SO JOURNAL OF PALEONTOLOGY LA English DT Editorial Material C1 Natl Museum Nat Hist, Smithsonian Inst, Washington, DC 20013 USA. RP Hunt, G (reprint author), Natl Museum Nat Hist, Smithsonian Inst, Washington, DC 20013 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU PALEONTOLOGICAL SOC INC PI LAWRENCE PA 810 EAST 10TH ST, LAWRENCE, KS 66044 USA SN 0022-3360 J9 J PALEONTOL JI J. Paleontol. PD MAY PY 2013 VL 87 IS 3 BP 532 EP 533 PG 2 WC Paleontology SC Paleontology GA 144SL UT WOS:000318960600018 ER PT J AU Ando, A Woodard, SC Evans, HF Littler, K Herrman, S Macleod, KG Kim, S Khim, BK Robinson, SA Huber, BT AF Ando, A. Woodard, S. C. Evans, H. F. Littler, K. Herrman, S. Macleod, K. G. Kim, S. Khim, B. -K. Robinson, S. A. Huber, B. T. TI An emerging palaeoceanographic 'missing link': multidisciplinary study of rarely recovered parts of deep-sea Santonian-Campanian transition from Shatsky Rise SO JOURNAL OF THE GEOLOGICAL SOCIETY LA English DT Editorial Material ID FORAMINIFERA; CLIMATE; ATLANTIC; ISOTOPES; RECORD; OCEAN C1 [Ando, A.; Kim, S.; Khim, B. -K.] Pusan Natl Univ, Dept Oceanog, Coastal Environm Syst Sch BK21, Pusan 609735, South Korea. [Ando, A.; Huber, B. T.] Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20013 USA. [Woodard, S. C.] Texas A&M Univ, Dept Oceanog, College Stn, TX 77843 USA. [Evans, H. F.] Columbia Univ, Lamont Doherty Earth Observ, Palisades, NY 10964 USA. [Littler, K.; Robinson, S. A.] UCL, Dept Earth Sci, London WC1E 6BT, England. [Herrman, S.] ETH, Inst Geol, Dept Earth Sci, CH-8092 Zurich, Switzerland. [Macleod, K. G.] Univ Missouri, Dept Geol Sci, Columbia, MO 65211 USA. RP Ando, A (reprint author), Pusan Natl Univ, Dept Oceanog, Coastal Environm Syst Sch BK21, Pusan 609735, South Korea. EM AndoA@si.edu RI Robinson, Stuart/C-4808-2011; MacLeod, Kenneth/C-4042-2017 OI Robinson, Stuart/0000-0003-4329-1058; MacLeod, Kenneth/0000-0002-6016-0837 NR 22 TC 8 Z9 8 U1 0 U2 8 PU GEOLOGICAL SOC PUBL HOUSE PI BATH PA UNIT 7, BRASSMILL ENTERPRISE CENTRE, BRASSMILL LANE, BATH BA1 3JN, AVON, ENGLAND SN 0016-7649 J9 J GEOL SOC LONDON JI J. Geol. Soc. PD MAY PY 2013 VL 170 IS 3 BP 381 EP 384 DI 10.1144/jgs2012-137 PG 4 WC Geosciences, Multidisciplinary SC Geology GA 143VE UT WOS:000318895500001 ER PT J AU Singerling, SA McSween, HY Taylor, LA AF Singerling, Sheryl A. McSween, Harry Y., Jr. Taylor, Larry A. TI Glasses in howardites: Impact melts or pyroclasts? SO METEORITICS & PLANETARY SCIENCE LA English DT Article ID ASTEROID 4 VESTA; PARENT BODY; EXPLOSIVE ERUPTIONS; ORIGIN; MOON; METAMORPHISM; EUCRITE; CLASSIFICATION; CONSTRAINTS; PERSPECTIVE AB We have analyzed glasses in eight howardites with the aim of distinguishing their origins as impact melts or pyroclasts. Although theoretical calculations predict that pyroclastic eruptions could have taken place on Vesta, the occurrence of pyroclastic glasses in HED meteorites has not been documented. This study involved petrographic examination of textures, electron microprobe analysis of major and minor elements, and LA-ICP-MS analysis for selected trace elements. Previously documented textural and compositional differences between lunar impact-melt and pyroclastic glasses partly guided this study. This work yielded no positive identification of pyroclastic glasses. The most likely explanation is that pyroclastic glasses never formed, either because Vesta contains insufficient volatiles to have powered explosive eruptions, or because eruptive conditions produced optically dense fire-fountains that allowed melt drops to collect as lava ponds. The impact-melt glasses were grouped (low-alkali, Ca-rich, and K-rich) based on compositions. We suggest that these glasses are the result of impacts onto known HED lithologies. The low-alkali glasses are impact melts of bulk HED lithologies. We hypothesize that the Ca-rich and K-rich glasses result from oversampling of plagioclase and of mesostasis that experienced liquid immiscibility, respectively, during micrometeorite impacts into eucrite targets. C1 [Singerling, Sheryl A.; McSween, Harry Y., Jr.; Taylor, Larry A.] Univ Tennessee, Dept Earth & Planetary Sci, Planetary Geosci Inst, Knoxville, TN 37996 USA. RP Singerling, SA (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Mineral Sci, Washington, DC 20560 USA. EM singerlings@si.edu FU NASA Cosmochemistry grants [NNX10AH48G, NNX11AG58G] FX We thank the following individuals for useful discussions: Arya Udry, Adam Sarafian, Andrew Beck, Brian Balta, Allan Patchen, Andrea Patzer, and Yang Liu. In addition, we thank Tim McCoy for use of the SEM in the NMNH Department of Mineral Sciences. Paul Buchanan and Rhiannon Mayne provided thorough reviews. This work was partly funded by NASA Cosmochemistry grants NNX10AH48G to HYM and NNX11AG58G to LAT. NR 62 TC 9 Z9 9 U1 0 U2 13 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1086-9379 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD MAY PY 2013 VL 48 IS 5 BP 715 EP 729 DI 10.1111/maps.12099 PG 15 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 143OP UT WOS:000318877300001 ER PT J AU Nie, ZL Deng, T Meng, Y Sun, H Wen, J AF Nie, Ze-Long Deng, Tao Meng, Ying Sun, Hang Wen, Jun TI Post-Boreotropical dispersals explain the pantropical disjunction in Paederia (Rubiaceae) SO ANNALS OF BOTANY LA English DT Article DE Intercontinental disjunction; long-distance dispersal; Paederia; pantropical; post-Boreotropical; Rubiaceae ID LONG-DISTANCE DISPERSAL; OUT-OF-AFRICA; HISTORICAL BIOGEOGRAPHY; CHLOROPLAST DNA; MOLECULAR PHYLOGENETICS; TRANSOCEANIC DISPERSAL; NORTHERN HEMISPHERE; OCEANIC DISPERSAL; GEOGRAPHIC RANGE; TIBETAN PLATEAU AB Pantropical intercontinental disjunction is a common biogeographical pattern in flowering plants exhibiting a discontinuous distribution primarily in tropical Asia, Africa and the Americas. Only a few plant groups with this pattern have been investigated at the generic level with molecular phylogenetic and biogeographical methods. Paederia (Rubiaceae) is a pantropical genus of 31 species of woody lianas, with the greatest species diversity in continental Asia and Madagascar and only two species from tropical America. The aim of this study was to reconstruct the biogeographical history of Paederia based on phylogenetic analyses to explore how the genus attained its pantropical distribution. Maximum parsimony and Bayesian inference were used for phylogenetic analyses using sequences of five plastid markers (the rbcL gene, rps16 intron, trnT-F region, atpB-rbcL spacer and psbA-trnH spacer). Biogeographical inferences were based on a Bayesian uncorrelated lognormal relaxed molecular clock together with both Bayesian and likelihood ancestral area reconstructions. The data suggest an early diverged Asian lineage sister to the clade of the remaining species consisting of a predominantly Asian sub-clade and a primarily Malagasy sub-clade. Paederia is inferred to have originated in the Oligocene in tropical continental Asia. It then reached Africa in the early to middle Miocene, most probably via long-distance dispersal across the Indian Ocean. The two Neotropical species are inferred to have derived independently in the late Miocene from ancestors of Asia and East Africa, respectively. The results demonstrate the importance of post-Boreotropical long-distance dispersals (across three major oceans) in shaping the global pantropical disjunction in some plants, such as Paederia, with small, winged diaspores adapted to long-distance dispersal by various agents including wind, ocean currents or birds. Overland migration is less likely to explain its palaeotropical disjunction between Asia and Africa. C1 [Nie, Ze-Long; Deng, Tao; Meng, Ying; Sun, Hang] Chinese Acad Sci, Kunming Inst Bot, Key Lab Biodivers & Biogeog, Kunming 650201, Yunnan, Peoples R China. [Meng, Ying] Chinese Acad Sci, Inst Tibetan Plateau Res Kunming, Kunming 650201, Peoples R China. [Wen, Jun] Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, MRC 166, Washington, DC 20013 USA. RP Sun, H (reprint author), Chinese Acad Sci, Kunming Inst Bot, Key Lab Biodivers & Biogeog, Kunming 650201, Yunnan, Peoples R China. EM hsun@mail.kib.ac.cn; wenj@si.edu RI Nie, Ze-Long/N-8471-2015 OI Nie, Ze-Long/0000-0001-8065-3981 FU Natural Sciences Foundation of China [NSFC 30970193]; Chinese Academy of Sciences [2011312D11022, XDB03030112]; NSFC; Yunnan Natural Science Foundation [U1136601]; NSFC-International (Region) Cooperation Project [31061160184]; John D. and Catherine T. MacArthur Foundation; Laboratory of Analytical Biology of the National Museum of Natural History, Smithsonian Institution; National Museum of Natural History, the Smithsonian Institution FX This study was supported by grants from Natural Sciences Foundation of China (NSFC 30970193 to Z.-L.N.), the One Hundred Talents Program of the Chinese Academy of Sciences (2011312D11022 to H.S.), United Fund of the NSFC and Yunnan Natural Science Foundation (U1136601 to H.S.), NSFC-International (Region) Cooperation Project (31061160184 to H.S.), the "Strategic Priority Research Program (B)" of the Chinese Academy of Sciences, XDB03030112 to H.S.) and the John D. and Catherine T. MacArthur Foundation to J. Wen, R. Ree and G. Mueller. Laboratory work was done at and partially supported by the Laboratory of Analytical Biology of the National Museum of Natural History, Smithsonian Institution. Fieldwork in North America was supported by the Small Grants Program of the National Museum of Natural History, the Smithsonian Institution. We thank Michael Nee, Fernando Chang, Ruth Kiew, Tze Leong Yao, Richard Chung, Leng Guan Saw, Elizabeth Widjaja, Zhiduan Chen, Tieyao Tu, Yumin Shui and Wenhong Chen for field assistance and sample collection. NR 110 TC 8 Z9 8 U1 3 U2 48 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0305-7364 J9 ANN BOT-LONDON JI Ann. Bot. PD MAY PY 2013 VL 111 IS 5 BP 873 EP 886 DI 10.1093/aob/mct053 PG 14 WC Plant Sciences SC Plant Sciences GA 140DA UT WOS:000318633300011 PM 23478944 ER PT J AU Hoyos, N Escobar, J Restrepo, JC Arango, AM Ortiz, JC AF Hoyos, N. Escobar, J. Restrepo, J. C. Arango, A. M. Ortiz, J. C. TI Impact of the 2010-2011 La Nina phenomenon in Colombia, South America: The human toll of an extreme weather event SO APPLIED GEOGRAPHY LA English DT Article DE ENSO; Extreme weather events; Spatial autocorrelation; Spatial error; Natural hazard; Vulnerability ID SOCIAL VULNERABILITY; NATURAL HAZARDS; WATER DISCHARGE; CLIMATE; PACIFIC; RIVER AB The 2010-2011 La Nina (positive phase of El Nino) phenomenon affected four million Colombians, similar to 9% of the total population, and caused economic losses of approximately US $7.8 billion, related to destruction of infrastructure, flooding of agricultural lands and payment of government subsidies. We analyzed the spatial patterns of effects on the population, measured as the number of affected persons in each municipality normalized to the total municipal population for 2011, using global (Moran's I index) and local (LISA) spatial autocorrelation indicators, and multiple regression analyses (OLS and ML spatial error model). The spatial autocorrelation analysis revealed two regional clusters or "hotspots" with high autocorrelation values, in the lower Magdalena River Valley (Caribbean plains) and lower Atrato Valley (Pacific lowlands). The regression analyses emphasized the importance of the spatial component as well as the variables related to hazard exposure and social vulnerability. Municipalities in "hotspots" show: (1) a high degree of flooding, as they are located on the Magdalena and Atrato River floodplains, and (2) high social vulnerability, suggested by low values of the ICV (national living conditions index). (C) 2012 Elsevier Ltd. All rights reserved. C1 [Hoyos, N.; Escobar, J.] Smithsonian Trop Res Inst, Ctr Trop Paleoecol & Archaeol, Balboa, Panama. [Hoyos, N.] Corp Geol ARES, Bogota, Colombia. [Escobar, J.] Univ Norte, Dept Ingn Civil & Ambiental, Barranquilla, Colombia. [Restrepo, J. C.; Ortiz, J. C.] Univ Norte, Dept Fis, Grp Fis Aplicada, Area Oceano & Atmosfera, Barranquilla, Colombia. [Arango, A. M.] iMMAP, Bogota, Colombia. RP Hoyos, N (reprint author), Corp Geol ARES, Calle 44A 53-96, Bogota, Colombia. EM natahoyos2011@gmail.com OI Restrepo, Juan Camilo/0000-0001-5696-8625 NR 58 TC 23 Z9 25 U1 2 U2 47 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 0143-6228 J9 APPL GEOGR JI Appl. Geogr. PD MAY PY 2013 VL 39 BP 16 EP 25 DI 10.1016/j.apgeog.2012.11.018 PG 10 WC Geography SC Geography GA 128VD UT WOS:000317796900003 ER PT J AU Swenson, NG Mi, XC Kress, WJ Thompson, J Uriarte, M Zimmerman, JK AF Swenson, Nathan G. Mi, Xiangcheng Kress, W. John Thompson, Jill Uriarte, Maria Zimmerman, Jess K. TI Species-time-area and phylogenetic-time-area relationships in tropical tree communities SO ECOLOGY AND EVOLUTION LA English DT Article DE Community ecology; phylogenetic diversity; scaling; species-time-area relationship ID FOREST; DIVERSITY; ECOLOGY; SCALE; BIOLOGY AB The species-area relationship (SAR) has proven to be one of the few strong generalities in ecology. The temporal analog of the SAR, the species-time relationship (STR), has received considerably less attention. Recent work primarily from the temperate zone has aimed to merge the SAR and the STR into a synthetic and unified species-time-area relationship (STAR) as originally envisioned by Preston (1960). Here we test this framework using two tropical tree communities and extend it by deriving a phylogenetic-time-area relationship (PTAR). The work finds some support for Preston's prediction that diversity-time relationships, both species and phylogenetic, are sensitive to the spatial scale of the sampling. Contrary to the Preston's predictions we find a decoupling of diversity-area and diversity-time relationships in both forests as the time period used to quantify the diversity-area relationship changes. In particular, diversity-area and diversity-time relationships are positively correlated using the initial census to quantify the diversity-area relationship, but weakly or even negatively correlated when using the most recent census. Thus, diversity-area relationships could forecast the temporal accumulation of biodiversity of the forests, but they failed to back-cast the temporal accumulation of biodiversity suggesting a decoupling of space and time. C1 [Swenson, Nathan G.] Michigan State Univ, Dept Plant Biol, E Lansing, MI 48824 USA. [Mi, Xiangcheng] Chinese Acad Sci, Inst Bot, State Key Lab Vegetat & Environm Change, Beijing 100093, Peoples R China. [Kress, W. John] Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, Washington, DC 20013 USA. [Thompson, Jill; Zimmerman, Jess K.] Univ Puerto Rico, Inst Ecosyst Studies, Rio Piedras, PR 00781 USA. [Thompson, Jill] Ctr Ecol & Hydrol, Penicuik EH26 0QB, Midlothian, Scotland. [Uriarte, Maria] Columbia Univ, Dept Ecol Evolut & Environm Biol, New York, NY 10027 USA. RP Swenson, NG (reprint author), Michigan State Univ, Dept Plant Biol, E Lansing, MI 48824 USA. EM swensonn@msu.edu RI Uriarte, Maria/L-8944-2013; Thompson, Jill/K-2200-2012 OI Thompson, Jill/0000-0002-4370-2593 FU Michigan State University; Center for Tropical Forest Science Research Grant; U.S. National Science Foundation; University of Puerto Rico; International Institute of Tropical Forestry; Andrew Mellon Foundation FX N. G. S was supported by Michigan State University and a Center for Tropical Forest Science Research Grant. The LFDP is part of the Luquillo Long- Term Ecological Research Program, supported by the U.S. National Science Foundation, the University of Puerto Rico, the International Institute of Tropical Forestry, and the Andrew Mellon Foundation. The Forest Dynamics Plot of Barro Colorado Island has been made possible through the generous support of the U.S. National Science Foundation, the John D. and Catherine T. MacArthur Foundation, and the Smithsonian Tropical Research Institute. We gratefully acknowledge the hard work of hundreds of people from over 10 countries who have censused these FDPs over the past two decades. The Luquillo and BCI Forest Dynamics Plots are part the Center for Tropical Forest Science, a global network of large-scale demographic tree plots. NR 34 TC 0 Z9 0 U1 1 U2 45 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 2045-7758 J9 ECOL EVOL JI Ecol. Evol. PD MAY PY 2013 VL 3 IS 5 BP 1173 EP 1183 DI 10.1002/ece3.526 PG 11 WC Ecology; Evolutionary Biology SC Environmental Sciences & Ecology; Evolutionary Biology GA 142MW UT WOS:000318802500004 PM 23762505 ER PT J AU Li, G Gordon, IE Le Roy, RJ Hajigeorgiou, PG Coxon, JA Bernath, PF Rothman, LS AF Li, Gang Gordon, Iouli E. Le Roy, Robert J. Hajigeorgiou, Photos G. Coxon, John A. Bernath, Peter F. Rothman, Laurence S. TI Reference spectroscopic data for hydrogen halides. Part I: Construction and validation of the ro-vibrational dipole moment functions SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER LA English DT Article DE Hydrogen fluoride; Hydrogen chloride; Hydrogen bromide; Hydrogen iodide; Dipole moment function; Intensity ID RADIATIVE TRANSITION-PROBABILITIES; FREQUENCY-MODULATION SPECTROSCOPY; SPECTRAL-LINE PARAMETERS; TUNABLE DIODE-LASERS; 1ST OVERTONE BAND; FUNDAMENTAL-BAND; MATRIX-ELEMENTS; DIATOMIC-MOLECULES; ROTATION INTERACTION; BROADENED WIDTHS AB Knowledge of the infrared transition moments of hydrogen halides, namely HF, HCl, HBr, and HI, is essential for atmospheric, astrophysical, and laser applications. Recently, a new polynomial empirical dipole moment function (DMF) for HCl has been constructed using an efficient approach that involves a direct fit of experimental ro-vibrational intensities [Li et al. J Quant Spectrosc Radiat Transfer 2011;112:1543-50]. In the present study, this method was extended to the use of Fade approximation representations of the DMF and applied to all four hydrogen halides. To carry out the fits, the best available experimental data were collected and critically evaluated. Combining dipole moment functions with the wavefunctions obtained from highly-accurate empirical potential energy curves, line intensities were computed numerically for numerous ro-vibrational bands, and compared with the experimental values and with intensities calculated using the most recent ab initio dipole moment functions. Results obtained in this work form basis for calculating intensities of spectral lines of hydrogen halides and their isotopologues in the HITRAN 2012 database. (C) 2013 Elsevier Ltd. All rights reserved. C1 [Li, Gang; Gordon, Iouli E.; Rothman, Laurence S.] Harvard Smithsonian Ctr Astrophys, Atom & Mol Phys Div, Cambridge, MA 02138 USA. [Le Roy, Robert J.] Univ Waterloo, Dept Chem, Waterloo, ON N2L 3G1, Canada. [Hajigeorgiou, Photos G.] Univ Nicosia, Dept Life & Hlth Sci, CY-1700 Nicosia, Cyprus. [Coxon, John A.] Dalhousie Univ, Dept Chem, Halifax, NS B3H 4J3, Canada. [Bernath, Peter F.] Old Dominion Univ, Dept Chem & Biochem, Norfolk, VA 23529 USA. RP Gordon, IE (reprint author), Harvard Smithsonian Ctr Astrophys, Atom & Mol Phys Div, 60 Garden St, Cambridge, MA 02138 USA. EM igordon@cfa.harvard.edu RI Bernath, Peter/B-6567-2012; Li, Gang/P-2272-2015; OI Bernath, Peter/0000-0002-1255-396X; Li, Gang/0000-0002-5605-7896; Gordon, Iouli/0000-0003-4763-2841; Rothman, Laurence/0000-0002-3837-4847 FU NASA [NNX10AB94G]; University of Nicosia FX We thank R. Tipping for stimulating discussions. We are grateful to A. Domanskaya for providing us the uncertainties of the line intensity measurements of HI. Thanks to J.F. Harrison for providing us his dipole moment functions for the hydrogen halides. Support from NASA Planetary Atmospheres Grant NNX10AB94G for this study is gratefully acknowledged. PGH acknowledges the University of Nicosia for financial support of research activities. NR 74 TC 13 Z9 13 U1 0 U2 46 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0022-4073 J9 J QUANT SPECTROSC RA JI J. Quant. Spectrosc. Radiat. Transf. PD MAY PY 2013 VL 121 BP 78 EP 90 DI 10.1016/j.jqsrt.2013.02.005 PG 13 WC Optics; Spectroscopy SC Optics; Spectroscopy GA 136TO UT WOS:000318386500008 ER PT J AU Ma, YN Filley, TR Johnston, CT Crow, SE Szlavecz, K McCormick, MK AF Ma, Yini Filley, Timothy R. Johnston, Cliff T. Crow, Susan E. Szlavecz, Katalin McCormick, Melissa K. TI The combined controls of land use legacy and earthworm activity on soil organic matter chemistry and particle association during afforestation SO ORGANIC GEOCHEMISTRY LA English DT Article ID CARBON SEQUESTRATION; FOREST-FLOOR; PHYSICAL FRACTIONATION; LUMBRICUS-TERRESTRIS; MICROBIAL BIOMASS; GRASSLAND SOILS; NITROUS-OXIDE; STABILIZATION; DYNAMICS; TURNOVER AB The chemistry and physical association of soil organic matter in the patchwork of successional forest stands in the eastern US is strongly controlled by past land use. Invasive earthworm activity in these same systems, however, may impart a chemical and physical disturbance exceeding that of land use legacy. We established eight plots within forests of the Smithsonian Environmental Research Center (SERC) (Edgewater, MD), to compare sites with no record of significant agricultural disturbance or earthworm activity and successional mixed hardwood forests recovering from past agriculture (60-132 yr) that contained both native and non-native earthworms. Soils (0-15 cm) were separated into physical fractions by size (microaggregates) and density (light and heavy particulate organic matter) and investigated for organic carbon (C) and nitrogen (N) partitioning. In addition, molecular composition was analyzed using FTIR spectroscopy and lignin phenol and substituted fatty acid (SFA) extraction. Even after 132 yr of recovery, the successional forests were nearly devoid of Oa+e horizons; a condition we attribute to high activity of invasive earthworms. Additionally, soil organic carbon (SOC) concentration profiles, and C-14 derived mean residence times indicated mixing of the surface soils and fresh input of carbon to 10 cm, distinct from the undisturbed, mature sites. The proportion of microaggregated particulate organic matter (iPOM) and silt + clay (iSC) was significantly higher in successional than undisturbed forests, which we attribute to the combined influence of past agricultural land use and high earthworm activity. Among the successional sites, older forests exhibited a significant decrease in the proportion of C and N in iSC but an increase in their proportion in iPOM, suggesting selective incorporation of iPOM with earthworm activity over great periods of time. In addition, continual consumption and mixing activities of the earthworm population could also be a primary control of the higher concentration and less oxidized lignin phenols as well as a higher proportion of lignin phenols to SFA in all soil fractions in the successional sites. Using partial least squares (PLS) regression of FTIR spectra, we also demonstrated a strong correlation between soil C physical distribution (microaggregated vs. non-microaggregated) and chemical aspects of specific FTIR regions which confirmed our findings from the lignin and SFA and showed distinct chemical dominance among the different sites. Our results indicated that while past agricultural practice may have been the primary initial influence on C and N stock and soil physical distribution in the successional sites, the prolonged legacy and trajectory of recovery from the past land disturbance can be controlled by the nature of the invasive and native earthworm activity during afforestation. (c) 2013 Elsevier Ltd. All rights reserved. C1 [Ma, Yini; Filley, Timothy R.] Purdue Univ, Dept Earth Atmospher & Planetary Sci, W Lafayette, IN 47907 USA. [Ma, Yini; Filley, Timothy R.; Johnston, Cliff T.] Purdue Climate Change Res Ctr, W Lafayette, IN 47907 USA. [Johnston, Cliff T.] Purdue Univ, Dept Agron, W Lafayette, IN 47907 USA. [Crow, Susan E.] Univ Hawaii, Dept Nat Resources & Environm Management, Honolulu, HI 96822 USA. [Szlavecz, Katalin] Johns Hopkins Univ, Dept Earth & Planetary Sci, Baltimore, MD 21216 USA. [McCormick, Melissa K.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. RP Ma, YN (reprint author), Purdue Univ, Dept Earth Atmospher & Planetary Sci, W Lafayette, IN 47907 USA. EM ma25@purdue.edu OI Szlavecz, Katalin/0000-0003-2504-0298 FU National Science Foundation [EAR-0748746] FX This research was supported by Grant EAR-0748746 from the National Science Foundation. We would like to thank Seth L. King and Grace Conyers for helping physical separation of soil samples; David Gamblin and Ian Schaller for helping lignin and SFA extraction and analysis; Kira Albright and Gnanasiri S. Premachandra for performing the FTIR analysis of samples. We thank two anonymous reviewers for valuable comments, which led to a considerable improvement of the manuscript. NR 89 TC 6 Z9 6 U1 9 U2 92 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0146-6380 J9 ORG GEOCHEM JI Org. Geochem. PD MAY PY 2013 VL 58 BP 56 EP 68 DI 10.1016/j.orggeochem.2013.02.010 PG 13 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 140VL UT WOS:000318684200005 ER PT J AU Massaro, F Harris, DE Tremblay, GR Liuzzo, E Bonafede, A Paggi, A AF Massaro, F. Harris, D. E. Tremblay, G. R. Liuzzo, E. Bonafede, A. Paggi, A. TI A CHANDRA SNAPSHOT SURVEY FOR 3C RADIO GALAXIES WITH REDSHIFTS BETWEEN 0.3 AND 0.5 SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE galaxies: active; radio continuum: galaxies; X-rays: general ID X-RAY-EMISSION; MAGNETIC-FIELD STRENGTHS; DIGITAL SKY SURVEY; INVERSE-COMPTON EMISSION; HUBBLE-SPACE-TELESCOPE; HOT-SPOTS; CLUSTER ENVIRONMENTS; INTRACLUSTER MEDIUM; COMPLETE SAMPLE; FR-I AB This paper contains an analysis of short Chandra observations of 19 3C sources with redshifts between 0.3 and 0.5 not previously observed in the X-rays. This sample is part of a project to obtain Chandra data for all of the extragalactic sources in the 3C catalog. Nuclear X-ray intensities as well as any X-ray emission associated with radio jet knots, hotspots, or lobes have been measured in three energy bands: soft, medium, and hard. Standard X-ray spectral analysis for the four brightest nuclei has also been performed. X-ray emission was detected for all the nuclei of the radio sources in the current sample with the exception of 3C 435A. There is one compact steep spectrum source while all the others are FR II radio galaxies. X-ray emission from two galaxy clusters (3C 19 and 3C 320), from six hotspots in four radio galaxies (3C 16, 3C 19, 3C 268.2, 3C 313), and extended X-ray emission on kiloparsec scales in 3C 187 and 3C 313, has been detected. C1 [Massaro, F.] SLAC Natl Lab, Menlo Pk, CA 94025 USA. [Massaro, F.] Kavli Inst Particle Astrophys & Cosmol, Menlo Pk, CA 94025 USA. [Harris, D. E.; Paggi, A.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. [Tremblay, G. R.] European So Observ, D-85748 Garching, Germany. [Liuzzo, E.] INAF, Ist Radioastron, I-40129 Bologna, Italy. [Bonafede, A.] Univ Hamburg, Hamburger Sternwarte, D-21029 Hamburg, Germany. RP Massaro, F (reprint author), SLAC Natl Lab, 2575 Sand Hill Rd, Menlo Pk, CA 94025 USA. RI Massaro, Francesco/L-9102-2016; Paggi, Alessandro/C-1219-2017; OI Massaro, Francesco/0000-0002-1704-9850; Paggi, Alessandro/0000-0002-5646-2410; Tremblay, Grant/0000-0002-5445-5401 FU National Aeronautics and Space Administration; National Science Foundation; NASA [GO1-12125A, GO2-13115X]; European Union; Valle DAosta Region; Italian Minister for Work and Welfare; FOR [1254]; Deutsche Forschungsgemeinschaft: Magnetization of inter-stellar and intergalactic media: the prospect of low-frequency radio observations; European Community's Seventh Framework Programme (FP7) [229517] FX We thank the anonymous referee for useful comments that led to improvements in the paper. We are grateful to R. Morganti, M. Hardcastle, and C. C. Cheung for providing several radio maps of the 3C sources and for helpful discussions. This research has made use of NASA's Astrophysics Data System. TOPCAT8 (Taylor 2005) and SAOImage DS9 were used extensively in this work for the preparation and manipulation of the tabular data and the images. SAOImage DS9 was developed by the Smithsonian Astrophysical Observatory. The NASA/IPAC Extragalactic Database (NED) is provided by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. Several radio maps were downloaded from the NVAS and from the DRAGN Web site.9 The National Radio Astronomy Observatory is operated by Associated Universities, Inc., under contract with the National Science Foundation. The work at SAO is supported by NASA-GRANTS GO1-12125A and GO2-13115X. This work was also supported by contributions from the European Union, Valle DAosta Region, and the Italian Minister for Work and Welfare. A.B. acknowledges support from the research group FOR 1254 funded by the Deutsche Forschungsgemeinschaft: Magnetization of inter-stellar and intergalactic media: the prospect of low-frequency radio observations. G.R.T. acknowledges support from the European Community's Seventh Framework Programme (/FP7/2007-2013/) under grant agreement No. 229517. NR 110 TC 5 Z9 5 U1 0 U2 4 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 MAY PY 2013 VL 206 IS 1 AR 7 DI 10.1088/0067-0049/206/1/7 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 139BK UT WOS:000318556300007 ER PT J AU Scoville, N Arnouts, S Aussel, H Benson, A Bongiorno, A Bundy, K Calvo, MAA Capak, P Carollo, M Civano, F Dunlop, J Elvis, M Faisst, A Finoguenov, A Fu, H Giavalisco, M Guo, Q Ilbert, O Iovino, A Kajisawa, M Kartaltepe, J Leauthaud, A Le Fevre, O LeFloch, E Lilly, SJ Liu, CTC Manohar, S Massey, R Masters, D McCracken, HJ Mobasher, B Peng, YJ Renzini, A Rhodes, J Salvato, M Sanders, DB Sarvestani, BD Scarlata, C Schinnerer, E Sheth, K Shopbell, PL Smolcic, V Taniguchi, Y Taylor, JE White, SDM Yan, L AF Scoville, N. Arnouts, S. Aussel, H. Benson, A. Bongiorno, A. Bundy, K. Calvo, M. A. A. Capak, P. Carollo, M. Civano, F. Dunlop, J. Elvis, M. Faisst, A. Finoguenov, A. Fu, Hai Giavalisco, M. Guo, Q. Ilbert, O. Iovino, A. Kajisawa, M. Kartaltepe, J. Leauthaud, A. Le Fevre, O. LeFloch, E. Lilly, S. J. Liu, C. T. -C. Manohar, S. Massey, R. Masters, D. McCracken, H. J. Mobasher, B. Peng, Y. -J. Renzini, A. Rhodes, J. Salvato, M. Sanders, D. B. Sarvestani, B. D. Scarlata, C. Schinnerer, E. Sheth, K. Shopbell, P. L. Smolcic, V. Taniguchi, Y. Taylor, J. E. White, S. D. M. Yan, L. TI EVOLUTION OF GALAXIES AND THEIR ENVIRONMENTS AT z=0.1-3 IN COSMOS SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE galaxies: evolution; large-scale structure of universe ID VLT DEEP SURVEY; STAR-FORMATION HISTORY; SIMILAR-TO 1.4; REDSHIFT SURVEY; STELLAR MASS; PHOTOMETRIC REDSHIFTS; FORMING GALAXIES; DENSITY RELATION; CLUSTER SURVEY; LEGACY SURVEY AB Large-scale structures (LSSs) out to z < 3.0 are measured in the Cosmic Evolution Survey (COSMOS) using extremely accurate photometric redshifts (photoz). The K-s-band-selected sample (from Ultra-Vista) is comprised of 155,954 galaxies. Two techniques-adaptive smoothing and Voronoi tessellation-are used to estimate the environmental densities within 127 redshift slices. Approximately 250 statistically significant overdense structures are identified out to z = 3.0 with shapes varying from elongated filamentary structures to more circularly symmetric concentrations. We also compare the densities derived for COSMOS with those based on semi-analytic predictions for Lambda CDM simulation and find excellent overall agreement between the mean densities as a function of redshift and the range of densities. The galaxy properties (stellar mass, spectral energy distributions (SEDs), and star formation rates (SFRs)) are strongly correlated with environmental density and redshift, particularly at z < 1.0-1.2. Classifying the spectral type of each galaxy using the rest-frame b - i color (from the photoz SED fitting), we find a strong correlation of early-type galaxies (E-Sa) with high-density environments, while the degree of environmental segregation varies systematically with redshift out to z similar to 1.3. In the highest density regions, 80% of the galaxies are early types at z = 0.2 compared to only 20% at z = 1.5. The SFRs and the star formation timescales exhibit clear environmental correlations. At z > 0.8, the SFR density is uniformly distributed over all environmental density percentiles, while at lower redshifts the dominant contribution is shifted to galaxies in lower density environments. C1 [Scoville, N.; Benson, A.; Fu, Hai; Manohar, S.; Rhodes, J.; Salvato, M.; Shopbell, P. L.; Smolcic, V.] CALTECH, Pasadena, CA 91125 USA. [Arnouts, S.] Canada France Hawaii Telescope Corp, Kamuela, HI 96743 USA. [Arnouts, S.; Kartaltepe, J.] Aix Marseille Univ, CNRS, Lab Astrophys Marseille, UMR 7326, F-13388 Marseille, France. [Aussel, H.; LeFloch, E.] Univ Paris 07, CNRS, AIM Unite Mixte Rech CEA, UMR 158, Paris, France. [Benson, A.] Carnegie Observ, Pasadena, CA USA. [Bongiorno, A.] Osserv Astron Roma, INAF, I-00040 Pomezia, Italy. [Bundy, K.; Leauthaud, A.] Univ Tokyo, Inst Phys & Math Universe, Kashiwa, Chiba 2778582, Japan. [Calvo, M. A. A.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Capak, P.; Yan, L.] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. [Carollo, M.; Faisst, A.; Lilly, S. J.; Peng, Y. -J.] ETH, Inst Astron, CH-8093 Zurich, Switzerland. [Civano, F.; Elvis, M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Dunlop, J.] Univ Edinburgh, Royal Observ, Inst Astron, Edinburgh EH9 3HJ, Midlothian, Scotland. [Finoguenov, A.; Guo, Q.; Salvato, M.; White, S. D. M.] Max Planck Inst Extraterr Phys, D-85478 Garching, Germany. [Fu, Hai] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA USA. [Giavalisco, M.] Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA. [Guo, Q.] Chinese Acad Sci, Natl Astron Observ, Beijing 100012, Peoples R China. [Ilbert, O.; Le Fevre, O.] Lab Astrophys Marseille, F-13376 Marseille 12, France. [Iovino, A.] Osserv Astron Brera, INAF, I-20159 Milan, Italy. [Kajisawa, M.; Taniguchi, Y.] Ehime Univ, Grad Sch Sci, Dept Phys, Matsuyama, Ehime 7908577, Japan. [Liu, C. T. -C.] CUNY Coll Staten Isl, Dept Engn Sci & Phys, Astrophys Observ, Staten Isl, NY 10314 USA. [Liu, C. T. -C.] Amer Museum Nat Hist, Dept Astrophys, New York, NY 10024 USA. [Liu, C. T. -C.] Amer Museum Nat Hist, Hayden Planetarium, New York, NY 10024 USA. [Massey, R.] Inst Astron, Edinburgh EH9 3HJ, Midlothian, Scotland. [Masters, D.; Mobasher, B.; Sarvestani, B. D.] Univ Calif Riverside, Dept Phys & Astron, Riverside, CA 92521 USA. [McCracken, H. J.] Univ Paris 06, CNRS, UMR7095, Inst Astrophys Paris, F-75014 Paris, France. [Renzini, A.] Osserv Astron Padova, INAF, I-35122 Padua, Italy. [Rhodes, J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Sanders, D. B.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Scarlata, C.] Univ Minnesota, Dept Phys & Astron, Minneapolis, MN 55455 USA. [Schinnerer, E.] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Sheth, K.] Natl Radio Astron Observ, Charlottesville, VA 22903 USA. [Smolcic, V.] Argelander Inst Astron, D-53121 Bonn, Germany. [Taylor, J. E.] Univ Waterloo, Dept Phys & Astron, Waterloo, ON N2L 3G1, Canada. RP Scoville, N (reprint author), CALTECH, MC 249-17,1200 East Calif Blvd, Pasadena, CA 91125 USA. OI Iovino, Angela/0000-0001-6958-0304; Bongiorno, Angela/0000-0002-0101-6624; Schinnerer, Eva/0000-0002-3933-7677 FU NASA [12712786]; National Radio Astronomy Observatory; National basic research program of China (program 973) [2009CB24901]; Young Researcher Grant of National Astronomical Observatories, CAS; NSFC [11143005]; Partner Group program of the Max Planck Society FX We thank the referee for helpful suggestions that have very much improved this work and we thank Zara Scoville for proof-reading of the manuscript. Support for this work was provided by NASA through Contract Number 12712786 issued by JPL. Additional information on the COSMOS survey is available from the main COSMOS Web site at http://www.astro.caltech.edu/cosmos. It is a pleasure to acknowledge the excellent services provided by the NASA IPAC/IRSA staff in providing online archive and server capabilities for the COSMOS data sets. The environmental densities and mpeg versions with all 127 redshift slices of the maps shown in Figures 6-8 will be available in FITS format from the NASA IPAC/IRSA archive at http://irsa.ipac.caltech.edu/data/COSMOS/. K.S. acknowledges support from the National Radio Astronomy Observatory which is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. G.Q. acknowledges support from the National basic research program of China (program 973 under grant No. 2009CB24901), the Young Researcher Grant of National Astronomical Observatories, CAS, the NSFC grants program (No. 11143005), and the Partner Group program of the Max Planck Society. NR 70 TC 61 Z9 61 U1 1 U2 5 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 MAY PY 2013 VL 206 IS 1 AR 3 DI 10.1088/0067-0049/206/1/3 PG 26 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 139BK UT WOS:000318556300003 ER PT J AU Krasnopolsky, VA Belyaev, DA Gordon, IE Li, G Rothman, LS AF Krasnopolsky, V. A. Belyaev, D. A. Gordon, I. E. Li, G. Rothman, L. S. TI Observations of D/H ratios in H2O, HCl, and HF on Venus and new DCl and DF line strengths SO ICARUS LA English DT Article DE Venus, Atmosphere; Spectroscopy; Atmospheres, Chemistry; Atmospheres, Composition ID HIGH-RESOLUTION SPECTROSCOPY; DIPOLE-MOMENT FUNCTION; WATER-VAPOR; UPPER LIMIT; CLOUD TOPS; ATMOSPHERE; DEUTERIUM; MESOSPHERE; DEPENDENCE; PRESSURE AB Intensities of the spectral lines in the fundamental bands of (DCl)-Cl-35 and DF were calculated using the semi-empirical dipole moment functions derived from the most accurate and precise measurements of intensities of the to-vibrational lines of (HCl)-Cl-35 and HF. Values obtained in this way for the deuterated species are superior to any available measured or calculated data to date. Our study of the D/H ratios in H2O, HCl, and HF on Venus is based on spatially-resolved high-resolution spectroscopy using the CSHELL spectrograph at NASA IRTF. Search for DF on Venus using its R5 (1-0) line at 3024.054 cm(-1) results in a DF mixing ratio of 0.23 +/- 0.11 ppb that corresponds to (D/H)(HF) = 420 +/- 200 times that in the Standard Mean Ocean Water (SMOW). H2O abundances on Venus were retrieved using lines at 3022.366 and 3025.761 cm(-1) that were observed at an exceptionally low overhead telluric water abundance of 03 pr. mm. The measured H2O mixing ratios at 74 km vary insignificantly between 55 degrees S and 55 degrees N with a mean value of 3.2 ppm. When compared with simultaneous observations of HDO near 2722 cm(-1), this results in (D/H)(H2O) = 95 +/- 15 times SMOW. Reanalysis of the observation of the (DCl)-Cl-35 R4 (1-0) line at 2141.540 cm(-1) (Krasnopolsky, V.A. [2012b]. Icarus 219, 244-249) using the improved line strength and more thorough averaging of the spectra gives (D/H)(HCI) = 190 +/- 50 times SMOW. The similarity of the measured (D/H)(H2O) = 95 +/- 15 at 74 km with 120 +/- 40 observed by De Bergh et al. (De Bergh, C., Bezard, B., Owen, T., Crisp, D., Maillard, J.P., Lutz, B.L. [1991]. Science 251, 547-549) below the clouds favors the constant (D/H)(H2O) from the surface to the mesosphere, in accord with the prediction by theory. D/H approximate to 100 removes a difference of a factor of 2 between H2O abundances in the observations by Krasnopolsky (Krasnopolsky, V.A. [2010b]. Icarus 209, 314-322) and the Venus Express nadir observations (Cottini, V., Ignatiev, Piccioni, G., Drossart, P., Grassi, D., Markiewicz, W.J. [2012]. Icarus 217, 561-569). Equivalent widths of the HDO and H2O lines are similar in our observations; therefore some errors cancel out in their ratios. Photochemistry of HCl in the mesosphere tends to enrich D in HCI and deplete it in H2O. This may be an explanation of the twofold difference between the observed D/H in HCl and H2O. An alternative explanation is based on (D/H)(H2O) approximate to 200 observed in the mesosphere by Bjoraker et al. (Bjoraker, G.L., Larson, H.P., Mumma, M.J., Timmermann, R., Montani, J.L. [1992]. Bull. Am. Astron. Soc. 24, 995) and Fedorova et al. (Fedorova, A. et al. J. Geophys. Res. 113, E00B22). This means an effective exchange of D between H2O and HCl and almost equal D/H in both species. However, this requires a twofold increase in D/H from the lower atmosphere to the mesosphere. This increase is not supported by theory; furthermore, condensation processes usually deplete D/H above the clouds. Photochemistry of HF has not been studied; it proceeds mostly in the lower thermosphere, and D/H in HF may be very different from that in H2O. Overall, the observational data on D/H in all hydrogen-bearing species on Venus are helpful to solve the problem of deuterium fractionation on Venus. (C) 2013 Elsevier Inc. All rights reserved. C1 [Krasnopolsky, V. A.] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA. [Krasnopolsky, V. A.] Moscow Inst Phys & Technol, Dolgoprudnyy, Russia. [Belyaev, D. A.] Russian Acad Sci, Space Res Inst, Moscow, Russia. [Gordon, I. E.; Li, G.; Rothman, L. S.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Krasnopolsky, VA (reprint author), Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA. EM vlad.krasn@verizon.net RI Krasnopolsky, Vladimir/L-5085-2013; Belyaev, Denis/A-5404-2015; Li, Gang/P-2272-2015; OI Li, Gang/0000-0002-5605-7896; Gordon, Iouli/0000-0003-4763-2841; Rothman, Laurence/0000-0002-3837-4847 FU NASA [NNX10AB94G]; Russian Government; RF President Grant [MK-3820.2012.2]; National Aeronautic and Space Administration, Science Mission Directorate, Planetary Astronomy Program [NCC 5-538] FX This work is supported by a NASA Planetary Astronomy grant to V.A. Krasnopolsky, a grant of the Russian Government to MIPT and V.A. Krasnopolsky, and the RF President Grant MK-3820.2012.2 to D. Belyaev. The effort at the Harvard-Smithsonian Center for Astrophysics has been supported by NASA through the Planetary Atmospheres Grant NNX10AB94G.; Visiting Astronomer at the Infrared Telescope Facility, which is operated by the University of Hawaii under Cooperative Agreement No. NCC 5-538 with the National Aeronautic and Space Administration, Science Mission Directorate, Planetary Astronomy Program. NR 48 TC 18 Z9 18 U1 0 U2 18 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 J9 ICARUS JI Icarus PD MAY PY 2013 VL 224 IS 1 BP 57 EP 65 DI 10.1016/j.icarus.2013.02.010 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 133HC UT WOS:000318128500006 ER PT J AU Stanley, JD Corwin, KA AF Stanley, Jean-Daniel Corwin, Kimberley A. TI Measuring Strata Thicknesses in Cores to Assess Recent Sediment Compaction and Subsidence of Egypt's Nile Delta Coastal Margin SO JOURNAL OF COASTAL RESEARCH LA English DT Article DE Coastal protection; coastline shifts; compaction; cores; Egypt; eustatic sea level; geotechnical properties; Holocene; human activity; Nile Delta; relative sea level; sediment color; sediment deprivation; strata thickness; subsidence ID COLORADO RIVER DELTA; SEA-LEVEL RISE; MISSISSIPPI DELTA; HOLOCENE; IRON; MINERALOGY; REWORKING; FUTURE; PERIOD; RATES AB This study develops a method to determine compaction and subsidence of Holocene fluviomarine sections along Egypt's northern Nile Delta coastal margin based on variations of strata thickness with depth. Thicknesses of 3183 oxidized layers in 85 long cores (10 to 45 m) are examined to determine the nature of down-section and spatial patterns. The thickest layers are at depths of 1 to 2 m (dating to <1000 y BP) and become significantly reduced within the next meter due to (1) rapid expulsion of interstitial pore water from overburden compression of sediment and (2) evaporation in near-surface deposits in this hyperarid setting. Thicknesses decrease more irregularly to depths of 5 to 6 in and then more gently to the base of the sections. The more gradual compaction of strata at mid- and lower-core depths accounts for more than 50% of total Holocene compaction. The derivatives of regression curves determine the strata thickness reduction rate, which is treated as a proxy for compaction rate. Average compaction rates for Holocene sections vary along the approximately 225-km-long coastal margin: about 8.4 mm/yin the NE, about 7.7 mm/y in the NC, and about 3.7 mm/y in the NW sectors. These rates, somewhat higher than those previously proposed for this delta, are within the range for land subsidence obtained from recent satellite surveys. The interaction of natural factors, such as moderate to high compaction rates and rising global sea level, with human activities, especially those reducing sediment supplied to the lower delta, presents serious concerns for the delta's future. Without emplacement of a continuous network of protective structures along the coast, a marked landward retreat of about 30 km by the Mediterranean coast is projected in little more than a century, resulting in submergence and loss of agricultural and wetland terrains vital to Egypt's rapidly expanding population. C1 [Stanley, Jean-Daniel; Corwin, Kimberley A.] Smithsonian Inst, Natl Museum Nat Hist E 205, Dept Paleobiol, CUSP, Washington, DC 20013 USA. RP Stanley, JD (reprint author), Smithsonian Inst, Natl Museum Nat Hist E 205, Dept Paleobiol, CUSP, Washington, DC 20013 USA. EM stanleyd@si.edu NR 88 TC 4 Z9 4 U1 0 U2 10 PU COASTAL EDUCATION & RESEARCH FOUNDATION PI LAWRENCE PA 810 EAST 10TH STREET, LAWRENCE, KS 66044 USA SN 0749-0208 J9 J COASTAL RES JI J. Coast. Res. PD MAY PY 2013 VL 29 IS 3 BP 657 EP 670 DI 10.2112/JCOASTRES-D-12A-00011.1 PG 14 WC Environmental Sciences; Geography, Physical; Geosciences, Multidisciplinary SC Environmental Sciences & Ecology; Physical Geography; Geology GA 137SI UT WOS:000318457300015 ER PT J AU Sabin, L Parker, QA Contreras, ME Olguin, L Frew, DJ Stupar, M Vazquez, R Wright, NJ Corradi, RLM Morris, RAH AF Sabin, L. Parker, Q. A. Contreras, M. E. Olguin, L. Frew, D. J. Stupar, M. Vazquez, R. Wright, N. J. Corradi, R. L. M. Morris, R. A. H. TI New Galactic supernova remnants discovered with IPHAS SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE ISM: supernova remnants ID H-ALPHA SURVEY; LARGE-MAGELLANIC-CLOUD; CANDIDATE PLANETARY-NEBULAE; EMISSION-LINE PROPERTIES; DIFFUSE IONIZED-GAS; WOLF-RAYET STARS; GHZ SKY SURVEY; NOVA REMNANT; CRAB-NEBULA; INTERSTELLAR-MEDIUM AB As part of a systematic search programme of a 10 degrees wide strip of the northern Galactic plane, we present preliminary evidence for the discovery of four (and possibly five) new supernova remnants (SNRs). The pilot search area covered the 19-20 h right ascension zone sampling from +20 degrees to +55 degrees in declination using binned mosaic images from the Isaac Newton Telescope Photometric H alpha Survey (IPHAS). The optical identification of the candidate SNRs was based mainly on their filamentary and arc-like emission morphologies, their apparently coherent, even if fractured, structure and clear disconnection from any diffuse neighbouring H II region type nebulosity. Follow-up optical spectroscopy was undertaken, sampling carefully across prominent features of these faint sources. The resulting spectra revealed typical emission-line ratios for shock-excited nebulae which are characteristic of SNRs, which, along with the latest diagnostic diagrams, strongly support the likely SNR nature of these sources: G038.7-1.3 (IPHASX J190640.5+042819), G067.6+0.9 (IPHASX J195744.9+305306), G066.0-0.0 (IPHASX J195749.2+290259) and G065.8-0.5 (IPHASX J195920.4+283740). A fifth possible younger, higher density nebula SNR candidate, G067.8+0.5 (IPHASX J200002.4+305035), was discovered similar to 5 arcmin to the west of IPHASX J195744.9+305306, and it warrants further study. A multiwavelength cross-check from available archived data in the regions of these candidates was also performed with a focus on possible radio counterparts. A close positional match between previously unrecognized radio structures at several frequencies and across various components of the H alpha optical image data was found for all SNR candidates. This lends further direct support for the SNR nature of these objects. Evolved SNRs may have very weak and/or highly fragmented radio emission which could explain why they had not been previously recognized, but the association becomes clear in combination with the optical emission. C1 [Sabin, L.; Contreras, M. E.; Vazquez, R.] Univ Nacl Autonoma Mexico, Inst Astron, Ensenada 22800, Baja California, Mexico. [Sabin, L.] Univ Guadalajara, CUCEI, Dept Fis, Inst Aston & Meteorol, Guadalajara 44130, Jalisco, Mexico. [Parker, Q. A.; Frew, D. J.; Stupar, M.] Macquarie Univ, Res Ctr Astron Astrophys & Astrophoton, Sydney, NSW 2109, Australia. [Parker, Q. A.; Frew, D. J.; Stupar, M.] Macquarie Univ, Dept Phys & Astron, Sydney, NSW 2109, Australia. [Parker, Q. A.; Stupar, M.] Australian Astron Observ, Epping, NSW 1710, Australia. [Olguin, L.] Univ Sonora, Dept Invest Fis, Hermosillo 83190, Sonora, Mexico. [Wright, N. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Corradi, R. L. M.] Inst Astrofis Canarias, E-38200 Tenerife, Spain. [Corradi, R. L. M.] Univ La Laguna, Dept Astrofis, E-38200 Tenerife, Spain. [Morris, R. A. H.] Univ Bristol, Dept Phys, Astrophys Grp, Bristol BS8 1TL, Avon, England. RP Sabin, L (reprint author), Univ Nacl Autonoma Mexico, Inst Astron, Apdo Postal 877, Ensenada 22800, Baja California, Mexico. EM laurence.sabin@gmail.com RI Vazquez, Roberto/L-3613-2016; OI Morris, Rhys/0000-0002-9210-1567; Vazquez, Roberto/0000-0002-3279-9764; Frew, David/0000-0002-3108-5284 FU PAPIIT-UNAM [IN109509]; National Aeronautics and Space Administration; National Aeronautics and Space Administration's Earth Science Technology Office [NCC5-626]; ARC; Macquarie University FX We thank both the anonymous referee and P. Boumis for valuable comments and suggestions that have contributed to significantly improving the quality of the paper. This project has been supported by PAPIIT-UNAM grant IN109509. This paper makes use of data obtained as part of the INT Photometric H alpha Survey (IPHAS) of the northern Galactic plane carried out at the Isaac Newton Telescope (INT). The INT is operated on the island of La Palma by the Isaac Newton Group at the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias. All IPHAS data are processed by the Cambridge Astronomical Survey Unit, at the Institute of Astronomy in Cambridge. The investigation is based on observations collected at the 2.1 m telescope at the Observatorio Astronomico Nacional at San Pedro Martir (Baja California, Mexico) operated by the Instituto de Astronomia of the Universidad Nacional Autonoma de Mexico and at the 2.5 m INT telescope operated on the island of La Palma by the Isaac Newton Group in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias. Special thanks is given to the technical staff and night assistants of the San Pedro Martir Observatory. This research has made use of the ALADIN data base operated at the 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. This research also made use of Montage, funded by the National Aeronautics and Space Administration's Earth Science Technology Office, Computation Technologies Project, under Cooperative Agreement Number NCC5-626 between NASA and the California Institute of Technology. Montage is maintained by the NASA/IPAC Infrared Science Archive. MS thanks the ARC for provision of Discovery project funding while DJF thanks Macquarie University for a university research fellowship. NR 71 TC 14 Z9 15 U1 0 U2 7 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 MAY PY 2013 VL 431 IS 1 BP 279 EP 291 DI 10.1093/mnras/stt160 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 136EE UT WOS:000318343600042 ER PT J AU Carter, PJ Steeghs, D de Miguel, E Goff, W Koff, RA Krajci, T Marsh, TR Gansicke, BT Breedt, E Groot, PJ Nelemans, G Roelofs, GHA Rau, A Koester, D Kupfer, T AF Carter, P. J. Steeghs, D. de Miguel, E. Goff, W. Koff, R. A. Krajci, T. Marsh, T. R. Gaensicke, B. T. Breedt, E. Groot, P. J. Nelemans, G. Roelofs, G. H. A. Rau, A. Koester, D. Kupfer, T. TI The helium-rich cataclysmic variable SBSS 1108+574 SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE accretion, accretion discs; binaries: close; stars: individual: SBSS 1108+574; novae, cataclysmic variables; white dwarfs ID AM CVN STARS; MINIMUM ORBITAL PERIOD; X-RAY BINARIES; WHITE-DWARF; WZ SAGITTAE; EFFECTIVE TEMPERATURES; COMPACT BINARIES; ACCRETION DISKS; CLOSE BINARIES; URSAE MAJORIS AB We present time-resolved spectroscopy and photometry of the dwarf nova SBSS 1108+574, obtained during the 2012 outburst. Its quiescent spectrum is unusually rich in helium, showing broad, double-peaked emission lines from the accretion disc. We measure a line flux ratio He I 5875/H alpha = 0.81 +/- 0.04, a much higher ratio than typically observed in cataclysmic variable stars (CVs). The outburst spectrum shows hydrogen and helium in absorption, with weak emission of Ha and He I 6678, as well as strong He II emission. From our photometry, we find the superhump period to be 56.34 +/- 0.18 min, in agreement with the previously published result. The spectroscopic period, derived from the radial velocities of the emission lines, is found to be 55.3 +/- 0.8 min, consistent with a previously identified photometric orbital period, and significantly below the normal CV period minimum. This indicates that the donor in SBSS 1108+574 is highly evolved. The superhump excess derived from our photometry implies a mass ratio of q = 0.086 +/- 0.014. Our spectroscopy reveals a grazing eclipse of the large outbursting disc. As the disc is significantly larger during outburst, it is unlikely that an eclipse will be detectable in quiescence. The relatively high accretion rate implied by the detection of outbursts, together with the large mass ratio, suggests that SBSS 1108+574 is still evolving towards its period minimum. C1 [Carter, P. J.; Steeghs, D.; Marsh, T. R.; Gaensicke, B. T.; Breedt, E.] Univ Warwick, Dept Phys, Coventry CV4 7AL, W Midlands, England. [de Miguel, E.] Univ Huelva, Dept Fis Aplicada, Huelva 21071, Spain. [de Miguel, E.] Observ CIECEM, CBA Huelva, Huelva, Spain. [Goff, W.] CBA Sutter Creek, Sutter Creek, CA 95685 USA. [Koff, R. A.] CBA Colorado, Antelope Hils Observ, Bennet, CO 80102 USA. [Krajci, T.] CBA New Mexico, Cloudcroft, NM 88317 USA. [Groot, P. J.; Nelemans, G.; Kupfer, T.] Radboud Univ Nijmegen, Dept Astrophys, IMAPP, NL-6500 GL Nijmegen, Netherlands. [Nelemans, G.] Katholieke Univ Leuven, Inst Astron, B-3001 Louvain, Belgium. [Roelofs, G. H. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Rau, A.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Koester, D.] Univ Kiel, Inst Theoret Phys & Astrophys, D-24098 Kiel, Germany. RP Carter, PJ (reprint author), Univ Warwick, Dept Phys, Coventry CV4 7AL, W Midlands, England. EM philip.carter@warwick.ac.uk RI Steeghs, Danny/C-5468-2009; Gaensicke, Boris/A-9421-2012; Nelemans, Gijs/D-3177-2012; de Miguel, Enrique/F-3734-2016; Groot, Paul/K-4391-2016 OI Steeghs, Danny/0000-0003-0771-4746; Gaensicke, Boris/0000-0002-2761-3005; Nelemans, Gijs/0000-0002-0752-2974; de Miguel, Enrique/0000-0002-1381-8843; Groot, Paul/0000-0002-4488-726X FU Science and Technology Facilities Council (STFC) [ST/F002599/1]; Netherlands Research School for Astronomy (NOVA); NWO-Rubicon grant; NWO-VIDI grant; 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 We thank the anonymous referee for useful comments and suggestions. PJC acknowledges the support of a Science and Technology Facilities Council (STFC) studentship. DS, TRM, BTG and EB acknowledge support from the STFC grant no. ST/F002599/1. TK acknowledges support by the Netherlands Research School for Astronomy (NOVA). GHAR acknowledges an NWO-Rubicon grant. GN acknowledges an NWO-VIDI grant.; 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/. NR 62 TC 10 Z9 10 U1 0 U2 3 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 MAY PY 2013 VL 431 IS 1 BP 372 EP 382 DI 10.1093/mnras/stt169 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 136EE UT WOS:000318343600051 ER PT J AU Jardine, M Vidotto, AA van Ballegooijen, A Donati, JF Morin, J Fares, R Gombosi, TI AF Jardine, M. Vidotto, A. A. van Ballegooijen, A. Donati, J. -F. Morin, J. Fares, R. Gombosi, T. I. TI Influence of surface stressing on stellar coronae and winds SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE magnetic fields; stars: coronae; stars: winds, outflows ID SCALE MAGNETIC TOPOLOGIES; 3-DIMENSIONAL MHD SIMULATION; LOW-MASS STARS; DIFFERENTIAL ROTATION; AB-DORADUS; M DWARFS; SOLAR-SYSTEM; FIELD; MODEL; FLUX AB The large-scale field of the Sun is well represented by its lowest energy (or potential) state. Recent observations, by comparison, reveal that many solar-type stars show large-scale surface magnetic fields that are highly non-potential - that is, they have been stressed above their lowest energy state. This non-potential component of the surface field is neglected by current stellar wind models. The aim of this paper is to determine its effect on the coronal structure and wind. We use Zeeman-Doppler surface magnetograms of two stars - one with an almost potential, one with a non-potential surface field - to extrapolate a static model of the coronal structure for each star. We find that the stresses are carried almost exclusively in a band of unidirectional azimuthal field that is confined to mid-latitudes. Using this static solution as an initial state for a magnetohydrodynamic (MHD) wind model, we then find that the final state is determined primarily by the potential component of the surface magnetic field. The band of azimuthal field must be confined close to the stellar surface, as it is not compatible with a steady-state wind. By artificially increasing the stellar rotation rate, we demonstrate that the observed azimuthal fields cannot be produced by the action of the wind but must be due to processes at or below the stellar surface. We conclude that the background winds of solar-like stars are largely unaffected by these highly stressed surface fields. Nonetheless, the increased flare activity and associated coronal mass ejections that may be expected to accompany such highly stressed fields may have a significant impact on any surrounding planets. C1 [Jardine, M.; Vidotto, A. A.; Fares, R.] Univ St Andrews, Sch Phys & Astron, SUPA, St Andrews KY16 9SS, Fife, Scotland. [van Ballegooijen, A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Donati, J. -F.] Observ Midi Pyrenees, Lab dOAstrophys, F-31400 Toulouse, France. [Morin, J.] Univ Gottingen, Inst Astrophys, D-37077 Gottingen, Germany. [Gombosi, T. I.] Univ Michigan, Ann Arbor, MI 48109 USA. RP Jardine, M (reprint author), Univ St Andrews, Sch Phys & Astron, SUPA, St Andrews KY16 9SS, Fife, Scotland. EM mmj@st-andrews.ac.uk RI Gombosi, Tamas/G-4238-2011; OI Gombosi, Tamas/0000-0001-9360-4951; Morin, Julien/0000-0002-4996-6901; Vidotto, Aline/0000-0001-5371-2675 FU STFC; Royal Astronomical Society; Alexander von Humboldt foundation FX The authors acknowledge support from STFC. AAV acknowledges support from the Royal Astronomical Society. JM acknowledges support from a fellowship of the Alexander von Humboldt foundation. NR 56 TC 16 Z9 16 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 MAY PY 2013 VL 431 IS 1 BP 528 EP 538 DI 10.1093/mnras/stt181 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 136EE UT WOS:000318343600064 ER PT J AU Lanzuisi, G Civano, F Elvis, M Salvato, M Hasinger, G Vignali, C Zamorani, G Aldcroft, T Brusa, M Comastri, A Fiore, F Fruscione, A Gilli, R Ho, LC Mainieri, V Merloni, A Siemiginowska, A AF Lanzuisi, G. Civano, F. Elvis, M. Salvato, M. Hasinger, G. Vignali, C. Zamorani, G. Aldcroft, T. Brusa, M. Comastri, A. Fiore, F. Fruscione, A. Gilli, R. Ho, L. C. Mainieri, V. Merloni, A. Siemiginowska, A. TI The Chandra-COSMOS survey - IV. X-ray spectra of the bright sample SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies: active; galaxies: high-redshift; galaxies: nuclei; X-rays: galaxies ID ACTIVE GALACTIC NUCLEI; WIDE-FIELD SURVEY; SUPERMASSIVE BLACK-HOLES; ROSAT DEEP SURVEY; STAR-FORMATION; LUMINOSITY FUNCTION; HELLAS2XMM SURVEY; MULTIWAVELENGTH PROJECT; OPTICAL IDENTIFICATIONS; SEYFERT-GALAXIES AB We present the X-ray spectral analysis of the 390 brightest extragalactic sources in the Chandra-Cosmic Evolution Survey catalogue, showing at least 70 net counts in the 0.5-7 keV band. This sample has a 100 per cent completeness in optical-infrared identification, with similar to 75 per cent of the sample having a spectroscopic redshift and similar to 25 per cent a photometric redshift. Our analysis allows us to accurately determine the intrinsic absorption, the broad-band continuum shape (Gamma) and intrinsic L2-10 distributions, with an accuracy better than 30 per cent on the spectral parameters for 95 per cent of the sample. The sample is equally divided in type 1 (49.7 per cent) and type 2 active galactic nuclei (48.7 per cent) plus few passive galaxies at low z. We found a significant difference in the distribution of Gamma of type 1 and type 2, with small intrinsic dispersion, a weak correlation of Gamma with L2-10 and a large population (15 per cent of the sample) of high luminosity, highly obscured (QSO2) sources. The distribution of the X-ray/Optical flux ratio (Log(F-X/F-i)) for type 1 is narrow (0 < X/O < 1), while type 2 are spread up to X/O = 2. The X/O correlates well with the amount of X-ray obscuration. Finally, a small sample of Compton-thick candidates and peculiar sources is presented. In the appendix, we discuss the comparison between Chandra and XMM-Newton spectra for 280 sources in common. We found a small systematic difference, with XMM-Newton spectra that tend to have softer power laws and lower obscuration. C1 [Lanzuisi, G.; Salvato, M.; Brusa, M.; Merloni, A.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Lanzuisi, G.; Civano, F.; Elvis, M.; Aldcroft, T.; Fruscione, A.; Siemiginowska, A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Lanzuisi, G.] Tech Univ Munich, Fak Phys, D-85748 Garching, Germany. [Hasinger, G.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Vignali, C.; Zamorani, G.] Univ Bologna, Dipartimento Astron, I-40127 Bologna, Italy. [Comastri, A.; Gilli, R.] INAF Osservatorio Astron Bologna, I-40127 Bologna, Italy. [Fiore, F.] Osservatorio Astron Roma INAF, I-00040 Monte Porzio Catone, Italy. [Ho, L. C.] Observ Carnegie Inst Sci, Pasadena, CA 91101 USA. [Mainieri, V.] ESO Headquarters, D-85748 Garching, Germany. RP Lanzuisi, G (reprint author), Max Planck Inst Extraterr Phys, Giessenbachstr, D-85748 Garching, Germany. EM giolanzu@mpe.mpg.de RI Vignali, Cristian/J-4974-2012; Lanzuisi, Giorgio/K-4378-2013; Comastri, Andrea/O-9543-2015; Gilli, Roberto/P-1110-2015; OI Vignali, Cristian/0000-0002-8853-9611; Lanzuisi, Giorgio/0000-0001-9094-0984; Brusa, Marcella/0000-0002-5059-6848; Comastri, Andrea/0000-0003-3451-9970; Gilli, Roberto/0000-0001-8121-6177; Fiore, Fabrizio/0000-0002-4031-4157; Zamorani, Giovanni/0000-0002-2318-301X FU ASI-INAF [I/009/10/0]; NASA Chandra grant [GO7-8136A]; Blancheflor Boncompagni Ludovisi foundation; Smithsonian Scholarly Studies; ESA Member States; NASA FX We thank the anonymous referee for providing constructive comments and help in improving the contents of this paper. We acknowledge financial contribution from the agreement ASI-INAF I/009/10/0. This work was supported in part by NASA Chandra grant number GO7-8136A (ME, FC), the Blancheflor Boncompagni Ludovisi foundation (FC) and the Smithsonian Scholarly Studies (FC). This work is based on observations made with the Chandra X-ray satellite. Also based on observations obtained with XMM-Newton, an ESA science mission with instruments and contributions directly funded by ESA Member States and NASA. This research has made use of data and/or software provided by the High Energy Astrophysics Science Archive Research Center (HEASARC), which is a service of the Astrophysics Science Division at NASA/GSFC and the High Energy Astrophysics Division of the Smithsonian Astrophysical Observatory. NR 112 TC 30 Z9 30 U1 0 U2 1 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 MAY PY 2013 VL 431 IS 1 BP 978 EP 996 DI 10.1093/mnras/stt222 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 136EE UT WOS:000318343600098 ER PT J AU Chen, Z Shu, CG Burgarella, D Buat, V Huang, JS Luo, ZJ AF Chen, Z. Shu, C. G. Burgarella, D. Buat, V. Huang, J. -S. Luo, Z. J. TI Properties and morphologies of Lyman break galaxies at z similar to 1 in the Chandra Deep Field South, inferred from spectral energy distributions SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies: evolution; galaxies: formation; galaxies: luminosity function, mass function; galaxies: statistics; galaxies: structure ID STAR-FORMING GALAXIES; DIGITAL SKY SURVEY; HUBBLE-SPACE-TELESCOPE; HIGH-REDSHIFT GALAXIES; ULTRAVIOLET-LUMINOUS GALAXIES; FRAME OPTICAL-PROPERTIES; MASS-SIZE RELATION; YALE-CHILE MUSYC; STELLAR MASS; FORMATION HISTORY AB After carefully cross-identifying previously discovered - and selected by the Galaxy Evolution Explorer (GALEX) - Lyman break galaxy (LBG) candidates one-to-one with their optical counterparts in the field of the Chandra Deep Field South (CDF-S), we re-estimate their photometric redshifts using multiwavelength data from ultraviolet and optical to near-infrared. Considering their re-estimated photometric redshifts and spectral energy distributions, we refine a new updated sample of 383 LBGs at 0.7 less than or similar to z less than or similar to 1.4, with two confirmed active galactic nuclei being excluded. There are 260 and 111 LBGs classified as starburst and irregular types, respectively. The ages of the LBGs span from several Myr to 1.5 Gyr with a median of similar to 50 Myr. Their dust-corrected star formation rates (SFRs) and stellar masses (M-*) are 4-220 M-circle dot yr(-1) and from 2.3 x 10(8) to 4 x 10(11) M-circle dot, with median values of similar to 25 M-circle dot yr(-1) and similar to 10(10) M-circle dot. The rest-frame far-ultraviolet luminosity function of the LBGs is presented with the best-fitting Schechter parameters of alpha = -1.61 +/- 0.40, M* = -20.40 +/- 0.22 and phi* = (0.89 +/- 0.30) x 10(-3) Mpc(-3) dex(-1). LBGs of irregular types are mainly distributed along the main sequence of star-forming galaxies, while most LBGs of starburst types are located in the starburst region. Together with previous studies, we suggest that the star formation mode for LBGs at z > 3 is mainly starburst, and that it evolves to be more significant to the quenching mode after z similar to 3. A downsizing effect is clearly found, and we discuss the physical implications and comparisons with previous studies in detail. LBGs with larger SFRs are, on average, more compact. In the rest-frame colour (U - B)-M-* diagram, LBGs are distributed in the 'blue' cloud. We suggest that LBGs might evolve along the blue cloud from later to earlier types. The Hubble Space Telescope images in F606W (V band) and F850LP (z band) are taken from the Galaxy Evolution from Morphology and SEDs (GEMS) survey and the Great Observatories Origins Deep Survey South (GOODS-S) for morphological studies of LBGs. SEXTRACTOR and GALFIT are applied in order to obtain their morphological parameters. We establish an image gallery of 277 LBGs, commonly detected in both bands, by visually classifying individual LBGs into the following types: chain, spiral, tadpole, bulge and clump. We define a morphological sample of 142 LBGs with reliable results of Sersic indices and sizes in both bands. We find that LBGs at z similar to 1 are dominated by disc-like galaxies, with median sizes of 2.34 and 2.68 kpc in F606W and F850LP, respectively. The correlations between the photometric and morphological properties of LBGs are investigated. Strong correlations between their half-light radii and M-* (i.e. size-stellar mass relations) are found in both bands. We discuss the physical connections between the correlations and the downsizing effect. C1 [Chen, Z.; Shu, C. G.] Shanghai Astron Observ, Shanghai 200030, Peoples R China. [Chen, Z.; Shu, C. G.; Luo, Z. J.] Shanghai Normal Univ, Shanghai Key Lab Astrophys, Shanghai 200234, Peoples R China. [Chen, Z.; Burgarella, D.; Buat, V.] Observ Astron Marseille Provence, Lab Astrophys Marseille, F-13012 Marseille, France. [Huang, J. -S.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Chen, Z (reprint author), Shanghai Astron Observ, 80 Nandan Rd, Shanghai 200030, Peoples R China. EM cgshu@shao.ac.cn FU DB; Laboratoire d'Astrophysique de Marseille; Chinese National Nature Science Foundation [10878003, 10833005, 10778725]; Shanghai Science Foundation; Leading Academic Discipline Project of Shanghai Normal University [DZL805]; NASA [NAS5-26555]; NASA Office of Space Science [NNX09AF08G] FX We are grateful to an anonymous referee for a thorough review of the manuscript and for valuable comments. ZC is very grateful for the financial support provided by DB and to the Laboratoire d'Astrophysique de Marseille for a visit. ZC is also grateful to DB and VB for their hospitality during the stay in Marseille. This work is partly supported by the Chinese National Nature Science Foundation (Nos 10878003, 10833005 and 10778725), the Shanghai Science Foundation and the Leading Academic Discipline Project of Shanghai Normal University (DZL805). Some/all of the data presented in this paper were obtained from the Multimission Archive at the Space Telescope Science Institute (MAST). STScI is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555. Support for MAST for non-HST data is provided by the NASA Office of Space Science via grant NNX09AF08G and by other grants and contracts. NR 165 TC 4 Z9 4 U1 0 U2 7 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 MAY PY 2013 VL 431 IS 3 BP 2080 EP 2105 DI 10.1093/mnras/stt230 PG 26 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 136FL UT WOS:000318347500006 ER PT J AU Naoz, S Farr, WM Lithwick, Y Rasio, FA Teyssandier, J AF Naoz, Smadar Farr, Will M. Lithwick, Yoram Rasio, Frederic A. Teyssandier, Jean TI Secular dynamics in hierarchical three-body systems SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE minor planets, asteroids: general; planets and satellites: dynamical evolution and stability; binaries: close ID BINARY MINOR PLANETS; TRIPLE STAR SYSTEMS; KOZAI MECHANISM; TIDAL FRICTION; HOT JUPITERS; CH CYGNI; IRREGULAR SATELLITES; ORBITAL EVOLUTION; GLOBULAR-CLUSTERS; INCLINED SYSTEMS AB The secular approximation for the evolution of hierarchical triple configurations has proven to be very useful in many astrophysical contexts, from planetary to triple-star systems. In this approximation the orbits may change shape and orientation, on time-scales longer than the orbital time-scales, but the semimajor axes are constant. For example, for highly inclined triple systems, the Kozai-Lidov mechanism can produce large-amplitude oscillations of the eccentricities and inclinations. Here we revisit the secular dynamics of hierarchical triple systems. We derive the secular evolution equations to octupole order in Hamiltonian perturbation theory. Our derivation corrects an error in some previous treatments of the problem that implicitly assumed a conservation of the z-component of the angular momentum of the inner orbit (i.e. parallel to the total angular momentum of the system). Already to quadrupole order, our results show new behaviours including the possibility for a system to oscillate from prograde to retrograde orbits. At the octupole order, for an eccentric outer orbit, the inner orbit can reach extremely high eccentricities and undergo chaotic flips in its orientation. We discuss applications to a variety of astrophysical systems, from stellar triples to merging compact binaries and planetary systems. Our results agree with those of previous studies done to quadrupole order only in the limit in which one of the inner two bodies is a massless test particle and the outer orbit is circular; our results agree with previous studies at octupole order for the eccentricity evolution, but not for the inclination evolution. C1 [Naoz, Smadar; Farr, Will M.; Lithwick, Yoram; Rasio, Frederic A.; Teyssandier, Jean] Northwestern Univ, CIERA, Evanston, IL 60208 USA. [Naoz, Smadar] Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, Cambridge, MA 02138 USA. [Lithwick, Yoram; Rasio, Frederic A.] Northwestern Univ, Dept Phys & Astron, Evanston, IL 60208 USA. [Teyssandier, Jean] UPMC, CNRS, UMR 7095, Inst Astrophys Paris, F-75014 Paris, France. RP Naoz, S (reprint author), Northwestern Univ, CIERA, Evanston, IL 60208 USA. EM snaoz@cfa.harvard.edu OI Naoz, Smadar/0000-0002-9802-9279 FU NASA [PF2-130096]; Chandra X-ray Center; NSF [AST-1109776]; NSF MRI award FX We thank Boaz Katz, Rosemary Mardling and Eugene Chiang for useful discussions. We thank Staffan Soderhjelm, our referee, for very useful comments that improved the manuscript in great deal. We also thank Keren Sharon and Paul Kiel for comments on the manuscript. SN supported by NASA through an Einstein Post-doctoral Fellowship awarded by the Chandra X-ray Center, which is operated by the Smithsonian Astrophysical Observatory for NASA under contract PF2-130096. YL acknowledges support from NSF grant AST-1109776. Simulations for this project were performed on the HPC cluster fugu funded by an NSF MRI award. NR 92 TC 79 Z9 79 U1 0 U2 6 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD MAY PY 2013 VL 431 IS 3 BP 2155 EP 2171 DI 10.1093/mnras/stt302 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 136FL UT WOS:000318347500011 ER PT J AU Symeonidis, M Vaccari, M Berta, S Page, MJ Lutz, D Arumugam, V Aussel, H Bock, J Boselli, A Buat, V Capak, PL Clements, DL Conley, A Conversi, L Cooray, A Dowell, CD Farrah, D Franceschini, A Giovannoli, E Glenn, J Griffin, M Hatziminaoglou, E Hwang, HS Ibar, E Ilbert, O Ivison, RJ Le Floc'h, E Lilly, S Kartaltepe, JS Magnelli, B Magdis, G Marchetti, L Nguyen, HT Nordon, R O'Halloran, B Oliver, SJ Omont, A Papageorgiou, A Patel, H Pearson, CP Perez-Fournon, I Pohlen, M Popesso, P Pozzi, F Rigopoulou, D Riguccini, L Rosario, D Roseboom, IG Rowan-Robinson, M Salvato, M Schulz, B Scott, D Seymour, N Shupe, DL Smith, AJ Valtchanov, I Wang, L Xu, CK Zemcov, M Wuyts, S AF Symeonidis, M. Vaccari, M. Berta, S. Page, M. J. Lutz, D. Arumugam, V. Aussel, H. Bock, J. Boselli, A. Buat, V. Capak, P. L. Clements, D. L. Conley, A. Conversi, L. Cooray, A. Dowell, C. D. Farrah, D. Franceschini, A. Giovannoli, E. Glenn, J. Griffin, M. Hatziminaoglou, E. Hwang, H. -S. Ibar, E. Ilbert, O. Ivison, R. J. Le Floc'h, E. Lilly, S. Kartaltepe, J. S. Magnelli, B. Magdis, G. Marchetti, L. Nguyen, H. T. Nordon, R. O'Halloran, B. Oliver, S. J. Omont, A. Papageorgiou, A. Patel, H. Pearson, C. P. Perez-Fournon, I. Pohlen, M. Popesso, P. Pozzi, F. Rigopoulou, D. Riguccini, L. Rosario, D. Roseboom, I. G. Rowan-Robinson, M. Salvato, M. Schulz, B. Scott, Douglas Seymour, N. Shupe, D. L. Smith, A. J. Valtchanov, I. Wang, L. Xu, C. K. Zemcov, M. Wuyts, S. TI The Herschel census of infrared SEDs through cosmic time SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies: evolution; galaxies: high-redshift; galaxies: starburst; infrared: galaxies; submillimetre: galaxies ID SPECTRAL ENERGY-DISTRIBUTIONS; STAR-FORMING GALAXIES; ACTIVE GALACTIC NUCLEI; SPITZER-SPACE-TELESCOPE; SIMILAR-TO 2; HUBBLE-DEEP-FIELD; DEGREE EXTRAGALACTIC SURVEY; HIGH-REDSHIFT GALAXIES; MU-M OBSERVATIONS; SUBMILLIMETER GALAXIES AB Using Herschel data from the deepest SPIRE and PACS surveys (HerMES and PEP) in COSMOS, GOODS-S and GOODS-N, we examine the dust properties of infrared (IR)-luminous (L-IR > 10(10) L-circle dot) galaxies at 0.1 < z < 2 and determine how these evolve with cosmic time. The unique angle of this work is the rigorous analysis of survey selection effects, making this the first study of the star-formation-dominated, IR-luminous population within a framework almost entirely free of selection biases. We find that IR-luminous galaxies have spectral energy distributions (SEDs) with broad far-IR peaks characterized by cool/extended dust emission and average dust temperatures in the 25-45 K range. Hot (T > 45 K) SEDs and cold (T < 25 K), cirrus-dominated SEDs are rare, with most sources being within the range occupied by warm starbursts such as M82 and cool spirals such as M51. We observe a luminosity-temperature (L-T) relation, where the average dust temperature of log [L-IR/L-circle dot] similar to 12.5 galaxies is about 10 K higher than that of their log [L-IR/L-circle dot] similar to 10.5 counterparts. However, although the increased dust heating in more luminous systems is the driving factor behind the L-T relation, the increase in dust mass and/or starburst size with luminosity plays a dominant role in shaping it. Our results show that the dust conditions in IR-luminous sources evolve with cosmic time: at high redshift, dust temperatures are on average up to 10 K lower than what is measured locally (z less than or similar to 0.1). This is manifested as a flattening of the L-T relation, suggesting that (ultra) luminous infrared galaxies [(U)LIRGs] in the early Universe are typically characterized by a more extended dust distribution and/or higher dust masses than local equivalent sources. Interestingly, the evolution in dust temperature is luminosity dependent, with the fraction of LIRGs with T < 35 K showing a two-fold increase from z similar to 0 to z similar to 2, whereas that of ULIRGs with T < 35 K shows a six-fold increase. Our results suggest a greater diversity in the IR-luminous population at high redshift, particularly for ULIRGs. C1 [Symeonidis, M.; Page, M. J.] Univ Coll London, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England. [Vaccari, M.; Franceschini, A.; Marchetti, L.] Univ Padua, Dipartimento Astron, I-35122 Padua, Italy. [Vaccari, M.; Giovannoli, E.] Univ Western Cape, Dept Phys, Astrophys Grp, ZA-7535 Cape Town, South Africa. [Berta, S.; Lutz, D.; Magnelli, B.; Popesso, P.; Rosario, D.; Wuyts, S.] Max Planck Inst Extraterr Phys MPE, D-85741 Garching, Germany. [Arumugam, V.; Ivison, R. J.; Roseboom, I. G.] Inst Astron, Edinburgh EH9 3HJ, Midlothian, Scotland. [Aussel, H.; Boselli, A.; Le Floc'h, E.] Univ Paris Diderot, CNRS, CE Saclay, Lab AIM Paris Saclay,CEA DSM Irfu, F-91191 Gif Sur Yvette, France. [Bock, J.; Capak, P. L.; Cooray, A.; Dowell, C. D.; Nguyen, H. T.; Schulz, B.; Shupe, D. L.; Xu, C. K.; Zemcov, M.] CALTECH, Pasadena, CA 91125 USA. [Bock, J.; Dowell, C. D.; Nguyen, H. T.; Zemcov, M.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Buat, V.] Univ Aix Marseille, CNRS, OAMP, Lab Astrophys Marseille, F-13388 Marseille 13, France. [Clements, D. L.; O'Halloran, B.; Patel, H.; Rowan-Robinson, M.] Univ London Imperial Coll Sci Technol & Med, Blackett Lab, Astrophys Grp, London SW7 2AZ, England. [Conley, A.; Glenn, J.] Univ Colorado, Ctr Astrophys & Space Astron UCB 389, Boulder, CO 80309 USA. [Riguccini, L.; Valtchanov, I.] Villanueva Canada, European Space Astron Ctr, Herschel Sci Ctr, E-28691 Madrid, Spain. [Cooray, A.] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA. [Farrah, D.] Virginia Tech, Dept Phys, Blacksburg, VA 24061 USA. [Glenn, J.] Univ Colorado, CASA UCB 389, Dept Astrophys & Planetary Sci, Boulder, CO 80309 USA. [Griffin, M.; Papageorgiou, A.; Pohlen, M.] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales. [Hatziminaoglou, E.] ESO, D-85748 Garching, Germany. [Hwang, H. -S.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. [Ibar, E.; Ivison, R. J.] Royal Observ, UK Astron Technol Ctr, Edinburgh EH9 3HJ, Midlothian, Scotland. [Ilbert, O.] Univ Aix Marseille 1, CNRS, Lab Astrophys Marseille, F-13376 Marseille 12, France. [Lilly, S.] Inst Astron, CH-8093 Zurich, Switzerland. [Kartaltepe, J. S.] Natl Opt Astron Observ, Tucson, AZ 85719 USA. [Magdis, G.; Rigopoulou, D.] Univ Oxford, Dept Astrophys, Oxford OX1 3RH, England. [Nordon, R.] Tel Aviv Univ, Raymond & Beverly Sackler Fac Exact Sci, Sch Phys & Astron, IL-69978 Tel Aviv, Israel. [Oliver, S. J.; Smith, A. J.; Wang, L.] Univ Sussex, Dept Phys & Astron, Ctr Astron, Brighton BN1 9QH, E Sussex, England. [Omont, A.] Univ Paris 06, CNRS, UMR 7095, Inst Astrophys Paris, F-75014 Paris, France. [Pearson, C. P.; Rigopoulou, D.] Rutherford Appleton Lab, RAL Space, Didcot OX11 0QX, Oxon, England. [Pearson, C. P.] Univ Lethbridge, Inst Space Imaging Sci, Lethbridge, AB T1K 3M4, Canada. [Perez-Fournon, I.] IAC, E-38200 Tenerife, Spain. [Perez-Fournon, I.] ULL, Departamento Astrofis, E-38205 Tenerife, Spain. [Pozzi, F.] INAF Osservatorio Astron Roma, I-00040 Monte Porzio Catone, Italy. [Riguccini, L.] NASA, Astrophys Branch, Ames Res Ctr, Moffett Field, CA 94035 USA. [Salvato, M.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Schulz, B.; Shupe, D. L.; Xu, C. K.] CALTECH, JPL, Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA. [Scott, Douglas] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada. [Seymour, N.] CSIRO Astron & Space Sci, Epping, NSW 1710, Australia. RP Symeonidis, M (reprint author), Univ Coll London, Mullard Space Sci Lab, Holmbury St Mary, Dorking RH5 6NT, Surrey, England. EM m.symeonidis@ucl.ac.uk RI Magdis, Georgios/C-7295-2014; Ivison, R./G-4450-2011; Vaccari, Mattia/R-3431-2016; OI Magdis, Georgios/0000-0002-4872-2294; Ivison, R./0000-0001-5118-1313; Vaccari, Mattia/0000-0002-6748-0577; Scott, Douglas/0000-0002-6878-9840; Marchetti, Lucia/0000-0003-3948-7621; Seymour, Nicholas/0000-0003-3506-5536 FU CSA (Canada); NAOC (China); CEA (France); CNES (France); CNRS (France); ASI (Italy); MCINN (Spain); SNSB (Sweden); STFC (UK); UKSA (UK); NASA (USA); BMVIT (Austria); ESA-PRODEX (Belgium); CEA/CNES (France); DLR (Germany); ASI/INAF (Italy); CICYT/MCYT (Spain) FX This paper uses data from Herschel's photometers SPIRE and PACS. SPIRE has been developed by a consortium of institutes led by Cardiff Univ. (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, UKSA (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). NR 161 TC 78 Z9 78 U1 0 U2 5 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 MAY PY 2013 VL 431 IS 3 BP 2317 EP 2340 DI 10.1093/mnras/stt330 PG 24 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 136FL UT WOS:000318347500024 ER PT J AU D'Ammando, F Antolini, E Tosti, G Finke, J Ciprini, S Larsson, S Ajello, M Covino, S Gasparrini, D Gurwell, M Hauser, M Romano, P Schinzel, F Wagner, SJ Impiombato, D Perri, M Persic, M Pian, E Polenta, G Sbarufatti, B Treves, A Vercellone, S Wehrle, A Zook, A AF D'Ammando, F. Antolini, E. Tosti, G. Finke, J. Ciprini, S. Larsson, S. Ajello, M. Covino, S. Gasparrini, D. Gurwell, M. Hauser, M. Romano, P. Schinzel, F. Wagner, S. J. Impiombato, D. Perri, M. Persic, M. Pian, E. Polenta, G. Sbarufatti, B. Treves, A. Vercellone, S. Wehrle, A. Zook, A. TI Long-term monitoring of PKS 0537-441 with Fermi-LAT and multiwavelength observations SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies: active; BL Lacertae objects: general; BL Lacertae objects: individual: PKS 0537-441; galaxies: quasars: general ID BL-LACERTAE OBJECTS; LARGE-AREA TELESCOPE; ACTIVE GALACTIC NUCLEI; X-RAY-SPECTRA; SOUTHERN RADIO-SOURCES; BLAZAR 3C 454.3; GAMMA-RAY; COMPLETE SAMPLE; MULTIFREQUENCY OBSERVATIONS; ENERGY-DISTRIBUTION AB We report on multiwavelength observations of the blazar PKS 0537-441 (z = 0.896) obtained from microwaves through gamma-rays by Submillimeter Array, Rapid Eye Mounting, Automatic Telescope for Optical Monitoring (ATOM), Swift and Fermi mostly during 2008 August-2010 April. Strong variability has been observed in gamma-rays, with two major flaring episodes (2009 July and 2010 March) and a harder-when-brighter behaviour, quite common for flat spectrum radio quasars and low-synchrotron-peaked BL Lacertae objects (BL Lacs), in 2010 March. In the same way, the spectral energy distribution (SED) of the source cannot be modelled by a simple synchrotron self-Compton model, as opposed to many BL Lacs, but the addition of an external Compton component of seed photons from a dust torus is needed. The 230 GHz light curve showed an increase simultaneous with the gamma-ray one, indicating co-spatiality of the mm and gamma-ray emission region likely at large distance from the central engine. The low, average, and high activity SED of the source could be fit changing only the electron distribution parameters, but two breaks in the electron distribution are necessary. The ensuing extra spectral break, located at near-infrared (NIR)-optical frequencies, together with that in gamma-rays seem to indicate a common origin, most likely due to an intrinsic feature in the underlying electron distribution. An overall correlation between the gamma-ray band with the R band and K band has been observed with no significant time lag. On the other hand, when inspecting the light curves on short time-scales some differences are evident. In particular, flaring activity has been detected in NIR and optical bands with no evident gamma-ray counterparts in 2009 September and November. Moderate variability has been observed in X-rays with no correlation between flux and photon index. An increase of the detected X-ray flux with no counterpart at the other wavelengths has been observed in 2008 October, suggesting once more a complex correlation between the emission at different energy bands. C1 [D'Ammando, F.; Antolini, E.; Tosti, G.] Univ Perugia, Dipartimento Fis, I-06123 Perugia, Italy. [D'Ammando, F.; Antolini, E.; Tosti, G.] Ist Nazl Fis Nucl, Sez Perugia, I-06123 Perugia, Italy. [Finke, J.] USN, Res Lab, Washington, DC 20375 USA. [Ciprini, S.; Gasparrini, D.; Perri, M.; Polenta, G.] ASI, Sci Data Ctr, I-00044 Rome, Italy. [Larsson, S.] Stockholm Univ, Albanova, Dept Phys, SE-10691 Stockholm, Sweden. [Larsson, S.] Albanova, Oskar Klein Ctr Cosmoparticle Phys, SE-10691 Stockholm, Sweden. [Larsson, S.] Stockholm Univ, Dept Astron, SE-10691 Stockholm, Sweden. [Ajello, M.] Stanford Univ, Dept Phys, Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94305 USA. [Ajello, M.] Stanford Univ, SLAC Natl Accelerator Lab, Stanford, CA 94305 USA. [Ajello, M.; Sbarufatti, B.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Covino, S.] Oss Astron Brera, INAF, I-23807 Merate, LC, Italy. [Gurwell, M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Hauser, M.; Wagner, S. J.] Heidelberg Univ, Landerssternwarte, D-69117 Heidelberg, Germany. [Romano, P.; Impiombato, D.; Vercellone, S.] IASF Palermo, INAF, I-90146 Palermo, Italy. [Schinzel, F.] Univ New Mexico, Dept Phys & Astron, Albuquerque, NM 87131 USA. [Persic, M.; Pian, E.] OA Trieste, INAF, I-34127 Trieste, Italy. [Persic, M.] Ist Nazl Fis Nucl, Sez Trieste, I-34127 Trieste, Italy. [Pian, E.] Scuola Normale Super Pisa, I-56126 Pisa, Italy. [Polenta, G.] Oss Astron Roma, INAF, I-00040 Monte Porzio Catone, Italy. [Sbarufatti, B.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Treves, A.] Univ Insubria, Dept Math & Phys, I-22100 Como, Italy. [Wehrle, A.] Space Sci Inst, Boulder, CO 80301 USA. [Zook, A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP D'Ammando, F (reprint author), Univ Perugia, Dipartimento Fis, I-06123 Perugia, Italy. EM dammando@ira.inaf.it OI Vercellone, Stefano/0000-0003-1163-1396; Perri, Matteo/0000-0003-3613-4409; Polenta, Gianluca/0000-0003-4067-9196; Persic, Massimo/0000-0003-1853-4900; Sbarufatti, Boris/0000-0001-6620-8347; Covino, Stefano/0000-0001-9078-5507; Gasparrini, Dario/0000-0002-5064-9495; Pian, Elena/0000-0001-8646-4858 FU Smithsonian Institution; Academia Sinica; National Aeronautics and Space Administration; ESA Member States; NASA; PRIN-INAF FX The Fermi-LAT Collaboration acknowledges generous ongoing support from a number of agencies and institutes that have supported both the development and the operation of the LAT as well as scientific data analysis. These include the National Aeronautics and Space Administration and the Department of Energy in the United States, the Commissariat a l'Energie Atomique and the Centre National de la Recherche Scientifique / Institut National de Physique Nucleaire et de Physique des Particules in France, the Agenzia Spaziale Italiana and the Istituto Nazionale di Fisica Nucleare in Italy, the Ministry of Education, Culture, Sports, Science and Technology (MEXT), High Energy Accelerator Research Organization (KEK) and Japan Aerospace Exploration Agency (JAXA) in Japan and the K. A. Wallenberg Foundation, the Swedish Research Council and the Swedish National Space Board in Sweden. Additional support for science analysis during the operations phase is gratefully acknowledged from the Istituto Nazionale di Astrofisica in Italy and the Centre National d'Etudes Spatiales in France. 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. We thank the Swift team for making these observations possible, the duty scientists and science planners. This publication makes use of data products from the Wide-field Infrared Survey Explorer, which is a joint project of the University of California, Los Angeles, and the Jet Propulsion Laboratory/California Institute of Technology, funded by the National Aeronautics and Space Administration. This paper is partly based on observations obtained with Planck (http://www.esa.int/Planck), an ESA science mission with instruments and contributions directly funded by ESA Member States, NASA, and Canada. We thank the anonymous referee, Y. Tanaka, C. Dermer, S. Digel, and E. Charles for useful comments and suggestions. Some authors acknowledge financial contribution from grant PRIN-INAF-2011. NR 93 TC 21 Z9 21 U1 1 U2 5 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 MAY PY 2013 VL 431 IS 3 BP 2481 EP 2492 DI 10.1093/mnras/stt344 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 136FL UT WOS:000318347500038 ER PT J AU Bietenholz, MF Kondratiev, V Ransom, S Slane, P Bartel, N Buchner, S AF Bietenholz, M. F. Kondratiev, V. Ransom, S. Slane, P. Bartel, N. Buchner, S. TI The proper motion of PSR J0205+6449 in 3C 58 SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE pulsars: individual: PSR J0205+6449; supernovae: general; ISM: supernova remnants ID FREQUENCY VARIABLE SOURCES; SUPERNOVA REMNANT 3C-58; EPOCH VLBI OBSERVATIONS; ACTIVE GALACTIC NUCLEI; COMPACT RADIO-SOURCES; GREEN-BANK-TELESCOPE; PULSAR J0205+6449; SPECTRAL INDEX; DISCOVERY; PULSATIONS AB We report on sensitive phase referenced and gated 1.4 GHz very long baseline interferometry (VLBI) radio observations of the pulsar PSR J0205+6449 in the young pulsar wind nebula 3C 58, made in 2007 and 2010. We employed a novel technique where the similar to 105-m Green Bank telescope is used simultaneously to obtain single-dish data used to determine the pulsar's period as well as to obtain VLBI data, allowing the VLBI correlation to be gated synchronously with the pulse to increase the signal-to-noise ratio. The high timing noise of this young pulsar precludes the determination of the proper motion from the pulsar timing. We derive the position of the pulsar accurate at the milliarcsecond level, which is consistent with a re-determined position from the Chandra X-ray observations. We reject the original tentative optical identification of the pulsar by Shearer & Neustroev in 2008, but rather identify a different optical counterpart on their images, with R-band magnitude similar to 24. We also determine an accurate proper motion for PSR J0205+6449 of (2.3 +/- 0.3) mas yr(-1), corresponding to a projected velocity of only (35 +/- 6) km s(-1) for a distance of 3.2 kpc, at position angle -38 degrees. This projected velocity is quite low compared to the velocity dispersion of known pulsars of similar to 200 km s(-1). Our measured proper motion does not suggest any particular kinematic age for the pulsar. C1 [Bietenholz, M. F.; Buchner, S.] Hartebeesthoek Radio Observ, ZA-1740 Krugersdrop, South Africa. [Bietenholz, M. F.; Bartel, N.] York Univ, Dept Phys & Astron, Toronto, ON M3J 1P3, Canada. [Kondratiev, V.] Netherlands Inst Radio Astron, ASTRON, NL-7990 AA Dwingeloo, Netherlands. [Kondratiev, V.] PN Lebedev Phys Inst, Ctr Astro Space, Moscow 117997, Russia. [Ransom, S.] Natl Radio Astron Observ, Charlottesville, VA 22903 USA. [Slane, P.] Harvard Smithsonian Ctr Astrophys, Div Theory, Cambridge, MA 02138 USA. RP Bietenholz, MF (reprint author), Hartebeesthoek Radio Observ, POB 443, ZA-1740 Krugersdrop, South Africa. EM mbieten@yorku.ca RI Kondratiev, Vladislav/N-1105-2015; OI Kondratiev, Vladislav/0000-0001-8864-7471; Ransom, Scott/0000-0001-5799-9714 FU National Sciences and Engineering Research Council of Canada; NASA [NAS8-03060]; National Aeronautics and Space Administration; National Science Foundation FX The research at York University was supported by the National Sciences and Engineering Research Council of Canada. PS acknowledges partial support from NASA contract NAS8-03060. The National Radio Astronomy Observatory, NRAO, is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. The telescope at Effelsberg is operated by the Max-Planck-Institut fur Radioastronomie in Bonn, Germany. 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 have made use of NASA's Astrophysics Data System Bibliographic Services. NR 44 TC 4 Z9 4 U1 0 U2 1 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 MAY PY 2013 VL 431 IS 3 BP 2590 EP 2598 DI 10.1093/mnras/stt353 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 136FL UT WOS:000318347500047 ER PT J AU Xu, XY Cuesta, AJ Padmanabhan, N Eisenstein, DJ McBride, CK AF Xu, Xiaoying Cuesta, Antonio J. Padmanabhan, Nikhil Eisenstein, Daniel J. McBride, Cameron K. TI Measuring D-A and H at z=0.35 from the SDSS DR7 LRGs using baryon acoustic oscillations SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE cosmological parameters; cosmology: observations; cosmology: theory; dark energy; distance scale; large-scale structure of Universe ID DIGITAL SKY SURVEY; GALAXY REDSHIFT SURVEY; MATTER POWER SPECTRUM; LUMINOUS RED GALAXIES; LARGE-SCALE STRUCTURE; PROBING DARK ENERGY; SPECTROSCOPIC TARGET SELECTION; COSMOLOGICAL CONSTANT; CENT DISTANCE; DATA RELEASE AB We present measurements of the angular diameter distance D-A(z) and the Hubble parameter H(z) at z = 0.35 using the anisotropy of the baryon acoustic oscillation (BAO) signal measured in the galaxy clustering distribution of the Sloan Digital Sky Survey (SDSS) Data Release 7 (DR7) luminous red galaxy (LRG) sample. Our work is the first to apply density-field reconstruction to an anisotropic analysis of the acoustic peak. Reconstruction partially removes the effects of non-linear evolution and redshift-space distortions in order to sharpen the acoustic signal. We present the theoretical framework behind the anisotropic BAO signal and give a detailed account of the fitting model we use to extract this signal from the data. Our method focuses only on the acoustic peak anisotropy, rather than the more model-dependent anisotropic information from the broad-band power. We test the robustness of our analysis methods on 160 Large Suite of Dark Matter Simulation DR7 mock catalogues and find that our models are unbiased at the similar to 0.2 per cent level in measuring the BAO anisotropy. After reconstruction we measure D-A(z = 0.35) = 1050 +/- 38 Mpc and H(z = 0.35) = 84.4 +/- 7.0 km s(-1) Mpc(-1) assuming a sound horizon of r(s) = 152.76 Mpc. Note that these measurements are correlated with a correlation coefficient of 0.57. This represents a factor of 1.4 improvement in the error on D-A relative to the pre-reconstruction case; a factor of 1.2 improvement is seen for H. C1 [Xu, Xiaoying] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Cuesta, Antonio J.; Padmanabhan, Nikhil] Yale Univ, Dept Phys, New Haven, CT 06511 USA. [Eisenstein, Daniel J.; McBride, Cameron K.] Harvard Univ, Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Xu, XY (reprint author), Univ Arizona, Steward Observ, 933 N Cherry Ave, Tucson, AZ 85721 USA. EM xxu@as.arizona.edu FU Alfred P. Sloan Foundation; National Science Foundation; US Department of Energy; National Aeronautics and Space Administration; Japanese Monbukagakusho; Max Planck Society; Higher Education Funding Council for England; American Museum of Natural History; Astrophysical Institute Potsdam; University of Basel; University of Chicago; Drexel University; Fermilab; Institute for Advanced Study; Johns Hopkins University; Joint Institute for Nuclear Astrophysics; Kavli Institute for Particle Astrophysics and Cosmology; Chinese Academy of Sciences (LAMOST); Los Alamos National Laboratory; Max-Planck-Institute for Astronomy (MPIA); New Mexico State University; Ohio State University; University of Pittsburgh; University of Portsmouth; Princeton University; United States Naval Observatory; University of Washington; NSF [AST-0707725]; NASA [NNX07AH11G, NNX11AF43G] FX Funding for the Sloan Digital Sky Survey (SDSS) and SDSS-II has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, the US 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 website is http://www.sdss.org/.; The SDSS is managed by the Astrophysical Research Consortium (ARC) for the Participating Institutions. The Participating Institutions are the American Museum of Natural History, Astrophysical Institute Potsdam, University of Basel, University of Chicago, Drexel University, Fermilab, the Institute for Advanced Study, the Japan Participation Group, the Johns Hopkins University, the Joint Institute for Nuclear Astrophysics, the Kavli Institute for Particle Astrophysics and Cosmology, the Korean Scientist Group, the Chinese Academy of Sciences (LAMOST), Los Alamos National Laboratory, the Max-Planck-Institute for Astronomy (MPIA), New Mexico State University, Ohio State University, University of Pittsburgh, University of Portsmouth, Princeton University, the United States Naval Observatory and the University of Washington.; We thank the LasDamas collaboration for making their galaxy mock catalogues public. XX thanks Kushal Mehta for useful conversations. XX and DJE were supported by NSF grant AST-0707725 and NASA grant NNX07AH11G. NP and AJC are partially supported by NASA grant NNX11AF43G. This work was supported in part by the facilities and staff of the Yale University Faculty of Arts and Sciences High Performance Computing Center. NR 95 TC 50 Z9 51 U1 0 U2 4 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 MAY PY 2013 VL 431 IS 3 BP 2834 EP 2860 DI 10.1093/mnras/stt379 PG 27 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 136FL UT WOS:000318347500070 ER PT J AU Ratti, EM van Grunsven, TFJ Torres, MAP Jonker, PG Miller-Jones, JCA Hessels, JWT Van Winckel, H van der Sluys, M Nelemans, G AF Ratti, E. M. van Grunsven, T. F. J. Torres, M. A. P. Jonker, P. G. Miller-Jones, J. C. A. Hessels, J. W. T. Van Winckel, H. van der Sluys, M. Nelemans, G. TI IGR J19308+0530: Roche lobe overflow on to a compact object from a donor 1.8 times as massive SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE accretion: accretion discs; stars: individual: IGR J19308+0530; X-rays: binaries; novae, cataclysmic variables; stars: mass loss ID X-RAY BINARIES; CATACLYSMIC VARIABLES; FOLLOW-UP; CATALOG; STARS; GALAXY; TELESCOPE; EVOLUTION; EDITION; MODEL AB We present phase-resolved spectroscopy and photometry of the optical counterpart to the X-ray binary IGR J19308+0530. Ellipsoidal modulations in the light curve show that the F-type companion star in the system is Roche lobe filling. The optical spectra are dominated by absorption features from the donor star, with similar to 10-20 per cent disc contribution to the optical continuum. We measure an orbital period of 14.662 +/- 0.001 h, a radial velocity semiamplitude for the companion star of K-2 = 91.4 +/- 1.4 kms(-1) and a rotational broadening of v sin i = 108.9 +/- 0.6 kms(-1). FromK(2) and v sin i, given that the donor star is filling its Roche lobe, we derive a mass ratio of q = M-2/M-1 = 1.78 +/- 0.04, which is typically considered to be too large for stable Roche lobe overflow. Our observations support an inclination of similar to 50 degrees. The accretor in IGR J19308+0530 is most likely a white dwarf, although a neutron star cannot entirely be excluded. C1 [Ratti, E. M.; van Grunsven, T. F. J.; Torres, M. A. P.; Jonker, P. G.] SRON Netherlands Inst Space Res, SRON, NL-3584 CA Utrecht, Netherlands. [van Grunsven, T. F. J.; Jonker, P. G.; van der Sluys, M.; Nelemans, G.] Radboud Univ Nijmegen, IMAPP, Dept Astrophys, NL-6525 AJ Nijmegen, Netherlands. [Torres, M. A. P.; Jonker, P. G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Miller-Jones, J. C. A.] Curtin Univ Technol, Int Ctr Radio Astron Res, Perth, WA 6845, Australia. [Hessels, J. W. T.] ASTRON, NL-7990 AA Dwingeloo, Netherlands. [Hessels, J. W. T.] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 XH Amsterdam, Netherlands. [Van Winckel, H.; Nelemans, G.] Katholieke Univ Leuven, Inst Sterrenkunde, B-3001 Louvain, Belgium. [van der Sluys, M.] Nikhef Natl Inst Subat Phys, NL-1098 XG Amsterdam, Netherlands. RP Ratti, EM (reprint author), SRON Netherlands Inst Space Res, SRON, Sorbonnelaan 2, NL-3584 CA Utrecht, Netherlands. EM e.m.ratti@sron.nl RI Van Winckel, Hans/I-7863-2013; Nelemans, Gijs/D-3177-2012; Miller-Jones, James/B-2411-2013 OI Van Winckel, Hans/0000-0001-5158-9327; Nelemans, Gijs/0000-0002-0752-2974; Miller-Jones, James/0000-0003-3124-2814 FU Netherlands Organization for Scientific Research FX PGJ and GN acknowledge support from a VIDI grant from the Netherlands Organization for Scientific Research. We thank T. Marsh for MOLLY, E. L. Robinson for his XRbinary code and F. Verbunt for useful discussion. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. NR 33 TC 3 Z9 3 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 MAY PY 2013 VL 431 IS 1 BP L10 EP L14 DI 10.1093/mnrasl/sls052 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 136EE UT WOS:000318343600003 ER PT J AU Zavala, J Vogelsberger, M Walker, MG AF Zavala, Jesus Vogelsberger, Mark Walker, Matthew G. TI Constraining self-interacting dark matter with the Milky Way's dwarf spheroidals SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE methods: numerical; galaxies: haloes; dark matter ID LAMBDA-CDM; GALAXY HALOES; SATELLITES; SUBHALOES; CLUSTER; CORES; SIMULATIONS; OUTFLOWS AB Self-interacting dark matter is an attractive alternative to the cold dark matter paradigm only if it is able to substantially reduce the central densities of dwarf-size haloes while keeping the densities and shapes of cluster-size haloes within current constraints. Given the seemingly stringent nature of the latter, it was thought for nearly a decade that self-interacting dark matter would be viable only if the cross-section for self-scattering was strongly velocity dependent. However, it has recently been suggested that a constant cross-section per unit mass of sigma(T)/m similar to 0.1 cm(2) g(-1) is sufficient to accomplish the desired effect. We explicitly investigate this claim using high-resolution cosmological simulations of a Milky Way-size halo and find that, similarly to the cold dark matter case, such cross-section produces a population of massive subhaloes that is inconsistent with the kinematics of the classical dwarf spheroidals, in particular with the inferred slopes of the mass profiles of Fornax and Sculptor. This problem is resolved if sigma(T)/m similar to 0.1 cm(2) g(-1) at the dwarf spheroidal scales. Since this value is likely inconsistent with the halo shapes of several clusters, our results leave only a small window open for a velocity-independent self-interacting dark matter model to work as a distinct alternative to cold dark matter. C1 [Zavala, Jesus] Perimeter Inst Theoret Phys, Waterloo, ON N2L 2Y5, Canada. [Zavala, Jesus] Univ Waterloo, Dept Phys & Astron, Waterloo, ON N2L 3G1, Canada. [Vogelsberger, Mark; Walker, Matthew G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Zavala, J (reprint author), Perimeter Inst Theoret Phys, 31 Caroline St N, Waterloo, ON N2L 2Y5, Canada. EM jzavalaf@uwaterloo.ca RI Walker, Matthew/P-1777-2014; Zavala Franco, Jesus/M-5152-2014 OI Walker, Matthew/0000-0003-2496-1925; Zavala Franco, Jesus/0000-0003-4442-908X FU University of Waterloo; Perimeter Institute for Theoretical Physics; Government of Canada through Industry Canada; Province of Ontario through the Ministry of Research and Innovation; CITA National Fellowship; NASA through Hubble Fellowship [HST-HF-51283.01-A, HST-HF-51317.01]; Space Telescope Science Institute; NASA [NAS5-26555] FX We thank Volker Springel for giving us access to GADGET-3, Niayesh Afshordi, Manoj Kaplinghat and Paul Steinhardt for fruitful discussions, Mike Boylan-Kolchin, Fabio Governato, Lars Hernquist, Avi Loeb, Jorge Penarrubia and Simon White for useful suggestions. JZ is supported by the University of Waterloo and the Perimeter Institute for Theoretical Physics. Research at Perimeter Institute is supported by the Government of Canada through Industry Canada and by the Province of Ontario through the Ministry of Research and Innovation. JZ acknowledges financial support by a CITA National Fellowship. MGW is currently supported by NASA through Hubble Fellowship grant HST-HF-51283.01-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 NAS5-26555. MV acknowledges support from NASA through Hubble Fellowship grant HST-HF-51317.01. NR 46 TC 103 Z9 103 U1 0 U2 0 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 MAY PY 2013 VL 431 IS 1 BP L20 EP L24 DI 10.1093/mnrasl/sls053 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 136EE UT WOS:000318343600005 ER PT J AU Kwiatkowski, L Cox, PM Economou, T Halloran, PR Mumby, PJ Booth, BBB Carilli, J Guzman, HM AF Kwiatkowski, Lester Cox, Peter M. Economou, Theo Halloran, Paul R. Mumby, Peter J. Booth, Ben B. B. Carilli, Jessica Guzman, Hector M. TI Caribbean coral growth influenced by anthropogenic aerosol emissions SO NATURE GEOSCIENCE LA English DT Article ID ATLANTIC MULTIDECADAL OSCILLATION; SEA-SURFACE TEMPERATURE; NORTH-ATLANTIC; CLIMATE-CHANGE; REEF ECOSYSTEMS; VARIABILITY; PORITES; CALCIFICATION; CENTURIES; DECLINE AB Coral growth rates are highly dependent on environmental variables such as sea surface temperature(1,2) and solar irradiance(3,4). Multi-decadal variability in coral growth rates has been documented throughout the Caribbean over the past 150-200 years(5,6), and linked to variations in Atlantic sea surface temperatures(5). Multi-decadal variability in sea surface temperatures in the North Atlantic, in turn, has been linked to volcanic and anthropogenic aerosol forcing(7). Here, we examine the drivers of changes in coral growth rates in the western Caribbean between 1880 and 2000, using previously published coral growth chronologies from two sites in the region, and a numerical model. Changes in coral growth rates over this period coincided with variations in sea surface temperature and incoming short-wave radiation. Our model simulations show that variations in the concentration of anthropogenic aerosols caused variations in sea surface temperature and incoming radiation in the second half of the twentieth century. Before this, variations in volcanic aerosols may have played a more important role. With the exception of extreme mass bleaching events, we suggest that neither climate change from greenhouse-gas emissions nor ocean acidification is necessarily the driver of multi-decadal variations in growth rates at some Caribbean locations. Rather, the cause may be regional climate change due to volcanic and anthropogenic aerosol emissions. C1 [Kwiatkowski, Lester; Cox, Peter M.; Economou, Theo] Univ Exeter, Coll Engn Math & Phys Sci, Exeter EX4 4QF, Devon, England. [Halloran, Paul R.; Booth, Ben B. B.] Met Off Hadley Ctr, Exeter EX1 3PB, Devon, England. [Mumby, Peter J.] Univ Queensland, Sch Biol Sci, Brisbane, Qld 4072, Australia. [Carilli, Jessica] Australian Nucl Sci & Technol Org, Lucas Heights, NSW 2234, Australia. [Guzman, Hector M.] Smithsonian Trop Res Inst, Panama City, Panama. RP Kwiatkowski, L (reprint author), Univ Exeter, Coll Engn Math & Phys Sci, Exeter EX4 4QF, Devon, England. EM lk244@exeter.ac.uk RI Halloran, Paul/G-3965-2012; Cox, Peter/B-3299-2012 OI Halloran, Paul/0000-0002-9227-0678; FU NERC grant; University of Exeter; EU FORCE project; Joint DECC/Defra Met Office Hadley Centre Climate Programme [GA01101] FX We thank R. Williams, C. Luke, A. Hunter, D. Long, C. Saenger, J. P. Carricart-Ganivet and R. Iglesias-Prieto for helpful insight. We also thank J. Hughes for undertaking the all-forcings model simulations. The study was financially supported by a NERC grant to P.J.M. and P.M.C., the University of Exeter and the EU FORCE project. P.R.H. was supported by the Joint DECC/Defra Met Office Hadley Centre Climate Programme (GA01101). NR 30 TC 10 Z9 11 U1 1 U2 61 PU NATURE PUBLISHING GROUP PI NEW YORK PA 75 VARICK ST, 9TH FLR, NEW YORK, NY 10013-1917 USA SN 1752-0894 EI 1752-0908 J9 NAT GEOSCI JI Nat. Geosci. PD MAY PY 2013 VL 6 IS 5 BP 362 EP 366 DI 10.1038/NGEO1780 PG 5 WC Geosciences, Multidisciplinary SC Geology GA 134QA UT WOS:000318227000015 ER PT J AU Piao, T Comita, LS Jin, GZ Kim, JH AF Piao, Tiefeng Comita, Liza S. Jin, Guangze Kim, Ji Hong TI Density dependence across multiple life stages in a temperate old-growth forest of northeast China SO OECOLOGIA LA English DT Article DE Species coexistence; Janzen-Connell hypothesis; Liangshui FDP; Pinus koraiensis; Habitat heterogeneity ID SPECIES SHADE TOLERANCE; BORNEAN RAIN-FOREST; TROPICAL TREE; SEEDLING MORTALITY; SPATIAL-PATTERNS; NEOTROPICAL FOREST; PLANT DIVERSITY; NEIGHBORHOOD; COEXISTENCE; SURVIVAL AB Recent studies on species coexistence suggest that density dependence is an important mechanism regulating plant populations. However, there have been few studies of density dependence conducted for more than one life-history stage or that control for habitat heterogeneity, which may influence spatial patterns of survival and mask density dependence. We explored the prevalence of density dependence across multiple life stages, and the effects of controlling for habitat heterogeneity, in a temperate forest in northeast China. We used generalized linear mixed-effects models to test for density-dependent mortality of seedlings and spatial point pattern analysis to detect density dependence for sapling-to-juvenile transitions. Conspecific neighbors had a negative effect on survival of plants in both life stages. At the seedling stage, we found a negative effect of conspecific seedling neighbors on survival when analyzing all species combined. However, in species-level analyses, only 2 of 11 focal species were negatively impacted by conspecific neighbors, indicating wide variation among species in the strength of density dependence. Controlling for habitat heterogeneity did not alter our findings of density dependence at the seedling stage. For the sapling-to-juvenile transition stage, 11 of 15 focal species showed patterns of local scale (< 10 m) conspecific thinning, consistent with negative density dependence. The results varied depending on whether we controlled for habitat heterogeneity, indicating that a failure to account for habitat heterogeneity can obscure patterns of density dependence. We conclude that density dependence may promote tree species coexistence by acting across multiple life-history stages in this temperate forest. C1 [Piao, Tiefeng; Jin, Guangze] Northeast Forestry Univ, Ctr Ecol Res, Harbin 150040, Peoples R China. [Comita, Liza S.] Ohio State Univ, Dept Ecol Evolut & Organismal Biol, Columbus, OH 43210 USA. [Comita, Liza S.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. [Kim, Ji Hong] Kangwon Natl Univ, Coll Forest & Environm Sci, Chunchon 200701, South Korea. RP Jin, GZ (reprint author), Northeast Forestry Univ, Ctr Ecol Res, Harbin 150040, Peoples R China. EM taxus@126.com RI Jin, Guangze/F-5271-2017; OI Jin, Guangze/0000-0002-9852-0965; Comita, Liza/0000-0002-9169-1331 FU National Natural Science Foundation of China [30770350, 31270473]; Natural Science Foundation of Heilongjiang Province, China [ZJN0706]; US NSF [DEB-1046113] FX This study was financially supported by the National Natural Science Foundation of China (No. 30770350, 31270473), and the Natural Science Foundation of Heilongjiang Province, China (No. ZJN0706). Many critical comments on the manuscript were received in the 2011 Smithsonian CTFS/SIGEO and CForBio Workshop in Changbaishan (US NSF grant DEB-1046113). We are grateful to Keping Ma and Zhanqing Hao for their efforts in organizing that workshop, and the technological support from Smithsonian Tropical Research Institute. We also thank Thorsten Wiegand, Stephan Getzin and Yan Zhu for providing useful suggestions. The conduction of this study complied with the current laws of China. NR 58 TC 30 Z9 38 U1 7 U2 95 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0029-8549 EI 1432-1939 J9 OECOLOGIA JI Oecologia PD MAY PY 2013 VL 172 IS 1 BP 207 EP 217 DI 10.1007/s00442-012-2481-y PG 11 WC Ecology SC Environmental Sciences & Ecology GA 127GU UT WOS:000317686800019 PM 23053238 ER PT J AU Bischoff, C Brizius, A Buder, I Chinone, Y Cleary, K Dumoulin, RN Kusaka, A Monsalve, R Naess, SK Newburgh, LB Nixon, G Reeves, R Smith, KM Vanderlinde, K Wehus, IK Bogdan, M Bustos, R Church, SE Davis, R Dickinson, C Eriksen, HK Gaier, T Gundersen, JO Hasegawa, M Hazumi, M Holler, C Huffenberger, KM Imbriale, WA Ishidoshiro, K Jones, ME Kangaslahti, P Kapner, DJ Lawrence, CR Leitch, EM Limon, M McMahon, JJ Miller, AD Nagai, M Nguyen, H Pearson, TJ Piccirillo, L Radford, SJE Readhead, ACS Richards, JL Samtleben, D Seiffert, M Shepherd, MC Staggs, ST Tajima, O Thompson, KL Williamson, R Winstein, B Wollack, EJ Zwart, JTL AF Bischoff, C. Brizius, A. Buder, I. Chinone, Y. Cleary, K. Dumoulin, R. N. Kusaka, A. Monsalve, R. Naess, S. K. Newburgh, L. B. Nixon, G. Reeves, R. Smith, K. M. Vanderlinde, K. Wehus, I. K. Bogdan, M. Bustos, R. Church, S. E. Davis, R. Dickinson, C. Eriksen, H. K. Gaier, T. Gundersen, J. O. Hasegawa, M. Hazumi, M. Holler, C. Huffenberger, K. M. Imbriale, W. A. Ishidoshiro, K. Jones, M. E. Kangaslahti, P. Kapner, D. J. Lawrence, C. R. Leitch, E. M. Limon, M. McMahon, J. J. Miller, A. D. Nagai, M. Nguyen, H. Pearson, T. J. Piccirillo, L. Radford, S. J. E. Readhead, A. C. S. Richards, J. L. Samtleben, D. Seiffert, M. Shepherd, M. C. Staggs, S. T. Tajima, O. Thompson, K. L. Williamson, R. Winstein, B. Wollack, E. J. Zwart, J. T. L. CA QUIET Collaboration TI THE Q/U IMAGING EXPERIMENT INSTRUMENT SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmic background radiation; cosmology: observations; instrumentation: detectors; instrumentation: polarimeters; telescopes ID MICROWAVE-ANISOTROPY-PROBE; BACKGROUND POLARIZATION; WMAP OBSERVATIONS; QUIET EXPERIMENT; ANGULAR SCALE; SUBMILLIMETER; MILLIMETER; DESIGN; RADIOMETERS; POLARIMETRY AB The Q/U Imaging ExperimenT (QUIET) is designed to measure polarization in the cosmic microwave background, targeting the imprint of inflationary gravitational waves at large angular scales(similar to 1 degrees). Between 2008 October and 2010 December, two independent receiver arrays were deployed sequentially on a 1.4 m side-fed Dragonian telescope. The polarimeters that form the focal planes use a compact design based on high electron mobility transistors (HEMTs) that provides simultaneous measurements of the Stokes parameters Q, U, and I in a single module. The 17-element Q-band polarimeter array, with a central frequency of 43.1 GHz, has the best sensitivity (69 mu Ks(1/2)) and the lowest instrumental systematic errors ever achieved in this band, contributing to the tensor-to-scalar ratio at r < 0.1. The 84-element W-band polarimeter array has a sensitivity of 87 mu Ks(1/2) at a central frequency of 94.5 GHz. It has the lowest systematic errors to date, contributing at r < 0.01. The two arrays together cover multipoles in the range l similar to 25-975. These are the largest HEMT-based arrays deployed to date. This article describes the design, calibration, performance, and sources of systematic error of the instrument. C1 [Bischoff, C.; Brizius, A.; Buder, I.; Kusaka, A.; Smith, K. M.; Bogdan, M.; Kapner, D. J.; Tajima, O.; Williamson, R.; Winstein, B.] Univ Chicago, Enrico Fermi Inst, Dept Phys, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Bischoff, C.; Buder, I.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Brizius, A.; Samtleben, D.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Chinone, Y.; Hasegawa, M.; Hazumi, M.; Ishidoshiro, K.; Nagai, M.; Tajima, O.] High Energy Accelerator Res Org KEK, Tsukuba, Ibaraki 3050801, Japan. [Chinone, Y.] Tohoku Univ, Grad Sch Sci, Astron Inst, Aoba Ku, Sendai, Miyagi 9808578, Japan. [Cleary, K.; Reeves, R.; Gaier, T.; Pearson, T. J.; Radford, S. J. E.; Readhead, A. C. S.; Richards, J. L.; Shepherd, M. C.; Williamson, R.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA. [Dumoulin, R. N.; Newburgh, L. B.; Limon, M.; Miller, A. D.; Williamson, R.; Zwart, J. T. L.] Columbia Univ, Dept Phys, New York, NY 10027 USA. [Dumoulin, R. N.; Newburgh, L. B.; Limon, M.; Miller, A. D.; Williamson, R.; Zwart, J. T. L.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA. [Kusaka, A.; Newburgh, L. B.; Nixon, G.; Smith, K. M.; Staggs, S. T.] Princeton Univ, Joseph Henry Labs Phys, Princeton, NJ 08544 USA. [Monsalve, R.; Bustos, R.; Gundersen, J. O.; Huffenberger, K. M.] Univ Miami, Dept Phys, Coral Gables, FL 33146 USA. [Monsalve, R.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA. [Naess, S. K.; Eriksen, H. K.] Univ Oslo, Inst Theoret Astrophys, N-0315 Oslo, Norway. [Vanderlinde, K.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada. [Vanderlinde, K.] Univ Toronto, Dunlap Inst Astron & Astrophys, Toronto, ON, Canada. [Vanderlinde, K.] Univ Toronto, Dept Astron & Astrophys, Toronto, ON, Canada. [Wehus, I. K.] Univ Oslo, Dept Phys, N-0316 Oslo, Norway. [Wehus, I. K.; Holler, C.; Jones, M. E.] Univ Oxford, Dept Astrophys, Oxford OX1 3RH, England. [Bustos, R.] Univ Chile, Dept Astron, Santiago, Chile. [Bustos, R.] Univ Concepcion, Dept Astron, Concepcion, Chile. [Church, S. E.; Thompson, K. L.] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94305 USA. [Church, S. E.; Thompson, K. L.] Stanford Univ, Dept Phys, Stanford, CA 94305 USA. [Davis, R.; Dickinson, C.; Piccirillo, L.] Univ Manchester, Ctr Astrophys, Jodrell Bank, Sch Phys & Astron, Manchester M13 9PL, Lancs, England. [Eriksen, H. K.] Univ Oslo, Ctr Math Applicat, N-0316 Oslo, Norway. [Gaier, T.; Imbriale, W. A.; Kangaslahti, P.; Lawrence, C. R.; Leitch, E. M.; Seiffert, M.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Kapner, D. J.] Micro Encoder Inc, Kirkland, WA 98034 USA. [McMahon, J. J.] Univ Michigan, Dept Phys, Ann Arbor, MI 48109 USA. [Nguyen, H.] Fermilab Natl Accelerator Lab, Batavia, IL 60510 USA. [Samtleben, D.] Nikhef, Amsterdam, Netherlands. [Wollack, E. J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Zwart, J. T. L.] Univ Western Cape, Dept Phys, ZA-7535 Bellville, South Africa. RP Bischoff, C (reprint author), Univ Chicago, Enrico Fermi Inst, Dept Phys, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. EM newburgh@princeton.edu RI Reeves, Rodrigo/H-2812-2014; Williamson, Ross/H-1734-2015; Pearson, Timothy/N-2376-2015; Wollack, Edward/D-4467-2012; OI Reeves, Rodrigo/0000-0001-5704-271X; Williamson, Ross/0000-0002-6945-2975; Huffenberger, Kevin/0000-0001-7109-0099; Bischoff, Colin/0000-0001-9185-6514; Zwart, Jonathan/0000-0002-4967-946X; Pearson, Timothy/0000-0001-5213-6231; Wollack, Edward/0000-0002-7567-4451; Limon, Michele/0000-0002-5900-2698; radford, simon/0000-0001-9113-1660 FU NSF [AST-0506648, PHY-0855887, PHY-0355328, AST-0448909, AST-1010016, PHY-0551142]; KAKENHI [20244041, 20740158, 21111002]; KIPAC Enterprise; Strategic Alliance for the Implementation of New Technologies (SAINT); Office of Science of the U.S. Department of Energy [DE-AC02-05CH11231]; Fermilab; Kavli Institute for Cosmological Physics; University of Chicago; JPL RTD program; STFC Advanced Fellowship; ERC IRG; CONICYT [PFB-06]; ALMA-Conicyt [31070015]; Sloan foundation; ERC; [PRODEX C90284] FX Support for the QUIET instrument and operation comes through the NSF cooperative agreement AST-0506648. Support was also provided by NSF awards PHY-0855887, PHY-0355328, AST-0448909, AST-1010016, and PHY-0551142; KAKENHI 20244041, 20740158, and 21111002; PRODEX C90284; a KIPAC Enterprise grant; and by the Strategic Alliance for the Implementation of New Technologies (SAINT). This research used resources of the National Energy Research Scientific Computing Center, which is supported by the Office of Science of the U.S. Department of Energy under Contract No. DE-AC02-05CH11231.; Some work was performed on the Joint Fermilab-KICP Supercomputing Cluster, supported by grants from Fermilab, the Kavli Institute for Cosmological Physics, and the University of Chicago. Some work was performed on the Titan Cluster, owned and maintained by the University of Oslo and NOTUR (the Norwegian High Performance Computing Consortium), and on the Central Computing System, owned and operated by the Computing Research Center at KEK. Portions of this work were performed at the Jet Propulsion Laboratory (JPL) and California Institute of Technology, operating under a contract with the National Aeronautics and Space Administration. The Q-band modules were developed using funding from the JPL R&TD program. We acknowledge the Northrop Grumman Corporation for collaboration in the development and fabrication of HEMT-based cryogenic temperature-compatible MMICs.; C.D. acknowledges an STFC Advanced Fellowship and an ERC IRG grant under FP7. R. B. acknowledges support from CONICYT project Basal PFB-06 and ALMA-Conicyt 31070015. A. D. M. acknowledges a Sloan foundation fellowship. H. K. E. acknowledges an ERC Starting Grant under FP7. NR 54 TC 14 Z9 14 U1 1 U2 7 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAY 1 PY 2013 VL 768 IS 1 AR 9 DI 10.1088/0004-637X/768/1/9 PG 28 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 130ZT UT WOS:000317960500009 ER PT J AU Chitta, LP Kariyappa, R van Ballegooijen, AA DeLuca, EE Hasan, SS Hanslmeier, A AF Chitta, L. P. Kariyappa, R. van Ballegooijen, A. A. DeLuca, E. E. Hasan, S. S. Hanslmeier, A. TI OBSERVATIONS AND MODELING OF THE EMERGING EXTREME-ULTRAVIOLET LOOPS IN THE QUIET SUN AS SEEN WITH THE SOLAR DYNAMICS OBSERVATORY SO ASTROPHYSICAL JOURNAL LA English DT Article DE Sun: atmosphere; Sun: corona; Sun: photosphere; Sun: surface magnetism ID ACTIVE-REGION CORE; DIFFERENTIAL EMISSION MEASURE; CORONAL LOOPS; BRIGHT POINTS; HEATING MODEL; HINODE; SDO; PLASMA; TRACE AB We used data from the Helioseismic and Magnetic Imager (HMI) and the Atmospheric Imaging Assembly (AIA) on the Solar Dynamics Observatory (SDO) to study coronal loops at small scales, emerging in the quiet Sun. With HMI line-of-sight magnetograms, we derive the integrated and unsigned photospheric magnetic flux at the loop footpoints in the photosphere. These loops are bright in the EUV channels of AIA. Using the six AIA EUV filters, we construct the differential emission measure (DEM) in the temperature range 5.7-6.5 in log T (K) for several hours of observations. The observed DEMs have a peak distribution around log T approximate to 6.3, falling rapidly at higher temperatures. For log T < 6.3, DEMs are comparable to their peak values within an order of magnitude. The emission-weighted temperature is calculated, and its time variations are compared with those of magnetic flux. We present two possibilities for explaining the observed DEMs and temperatures variations. (1) Assuming that the observed loops are composed of a hundred thin strands with certain radius and length, we tested three time-dependent heating models and compared the resulting DEMs and temperatures with the observed quantities. This modeling used enthalpy-based thermal evolution of loops (EBTEL), a zero-dimensional (0D) hydrodynamic code. The comparisons suggest that a medium-frequency heating model with a population of different heating amplitudes can roughly reproduce the observations. (2) We also consider a loop model with steady heating and non-uniform cross-section of the loop along its length, and find that this model can also reproduce the observed DEMs, provided the loop expansion factor gamma similar to 5-10. More observational constraints are required to better understand the nature of coronal heating in the short emerging loops on the quiet Sun. C1 [Chitta, L. P.; van Ballegooijen, A. A.; DeLuca, E. E.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Chitta, L. P.; Kariyappa, R.; Hasan, S. S.] Indian Inst Astrophys, Bangalore 560034, Karnataka, India. [Hanslmeier, A.] Graz Univ, IGAM, Inst Phys, A-8010 Graz, Austria. RP Chitta, LP (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS 15, Cambridge, MA 02138 USA. RI DeLuca, Edward/L-7534-2013; OI DeLuca, Edward/0000-0001-7416-2895; Chitta, Lakshmi Pradeep/0000-0002-9270-6785 FU NASA [NNM07AB07C]; Indo-Austria exchange program [INT/AUA/BMWF/P-11/2011] FX The authors thank the referee for many comments and suggestions that helped in improving the presentation of the manuscript. L.P.C. is a 2011-2013 SAO Pre-Doctoral Fellow at the Harvard-Smithsonian Center for Astrophysics. Funding for L.P.C. and E.E.D. is provided by NASA contract NNM07AB07C. Funding from the Indo-Austria exchange program (INT/AUA/BMWF/P-11/2011) is acknowledged. L.P.C. thanks Jim Klimchuk, Steve Saar, and Mark Weber for many useful suggestions and discussions. Courtesy of NASA/SDO and the AIA and HMI science teams. This research has made use of NASA's Astrophysics Data System. NR 41 TC 4 Z9 4 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAY 1 PY 2013 VL 768 IS 1 AR 32 DI 10.1088/0004-637X/768/1/32 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 130ZT UT WOS:000317960500032 ER PT J AU Fransson, C Larsson, J Spyromilio, J Chevalier, R Groningsson, P Jerkstrand, A Leibundgut, B McCray, R Challis, P Kirshner, RP Kjaer, K Lundqvist, P Sollerman, J AF Fransson, Claes Larsson, Josefin Spyromilio, Jason Chevalier, Roger Groningsson, Per Jerkstrand, Anders Leibundgut, Bruno McCray, Richard Challis, Peter Kirshner, Robert P. Kjaer, Karina Lundqvist, Peter Sollerman, Jesper TI LATE SPECTRAL EVOLUTION OF THE EJECTA AND REVERSE SHOCK IN SN 1987A SO ASTROPHYSICAL JOURNAL LA English DT Article DE line: identification; line: profiles; supernovae: individual (1987A); X-rays: general ID HUBBLE-SPACE-TELESCOPE; VELOCITY LY-ALPHA; INNER CIRCUMSTELLAR RING; SUPERNOVA REMNANT 1987A; ACTIVE GALACTIC NUCLEI; RAY LIGHT-CURVE; LINE EMISSION; OPTICAL-EMISSION; H-ALPHA; SN-1987A AB We present observations with the Very Large Telescope and Hubble Space Telescope (HST) of the broad emission lines from the inner ejecta and reverse shock of SN 1987A from 1999 February until 2012 January (days 4381-9100 after explosion). We detect broad lines from H alpha, H beta, Mg I], Na I, [O I], [Ca II], and a feature at similar to 9220 angstrom. We identify the latter line with Mg II lambda lambda 9218, 9244, which is most likely pumped by Ly alpha fluorescence. H alpha and H beta both have a centrally peaked component extending to similar to 4500 km s(-1) and a very broad component extending to greater than or similar to 11,000 km s(-1), while the other lines have only the central component. The low-velocity component comes from unshocked ejecta, heated mainly by X-rays from the circumstellar environment, whereas the very broad component comes from faster ejecta passing through the reverse shock, created by the collision with the circumstellar ring. The flux in H alpha from the reverse shock has increased by a factor of four to six from 2000 to 2007. After that there is a tendency of flattening of the light curve, similar to what may be seen in the optical lines from the shocked ring. The core component seen in H alpha, [Ca II], and Mg II has experienced a similar increase, which is consistent with that found from HST photometry. The energy deposition of the external X-rays is calculated using explosion models for SN 1987A and we predict that the outer parts of the unshocked ejecta will continue to brighten because of this. The external X-ray illumination also explains the edge-brightened morphology of the ejecta seen in the HST images. We finally discuss evidence for dust in the ejecta from line asymmetries. C1 [Fransson, Claes; Groningsson, Per; Jerkstrand, Anders; Lundqvist, Peter; Sollerman, Jesper] Stockholm Univ, AlbaNova Univ Ctr, Oskar Klein Ctr, Dept Astron, SE-10691 Stockholm, Sweden. [Larsson, Josefin] KTH, Dept Phys, SE-10691 Stockholm, Sweden. [Larsson, Josefin] AlbaNova, Oskar Klein Ctr, SE-10691 Stockholm, Sweden. [Spyromilio, Jason; Kjaer, Karina] ESO, D-85748 Garching, Germany. [Chevalier, Roger] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA. [Jerkstrand, Anders] Queens Univ Belfast, Sch Math & Phys, Belfast BT7 1NN, Antrim, North Ireland. [McCray, Richard] Univ Colorado, JILA, Boulder, CO 80309 USA. [Challis, Peter; Kirshner, Robert P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Fransson, C (reprint author), Stockholm Univ, AlbaNova Univ Ctr, Oskar Klein Ctr, Dept Astron, SE-10691 Stockholm, Sweden. EM claes@astro.su.se RI Jerkstrand, Anders/K-9648-2015; OI Jerkstrand, Anders/0000-0001-8005-4030; Sollerman, Jesper/0000-0003-1546-6615; /0000-0003-0065-2933 FU Swedish Research Council; Swedish National Space Board; National Science Foundation [NSF PHY11-25915]; ESO observational programs [66.D-0589(A), 70.D-0379(A), 074.D-0761(A), 078.D-0521(A,B), 080.D-0727(A,B), 082.D-0273(A,B), 086.D-0713(A), 088.D-0638(A,C)]; NASA through grants from the Space Telescope Science Institute [02563, 03853, 04445, 05480, 06020, 07434, 08243, 08648, 09114, 09428, 10263, 11181, 11973, 12241]; NASA [NAS5-26555] FX We are grateful to the referee for a careful reading of the paper and several constructive suggestions. This work is supported by the Swedish Research Council and the Swedish National Space Board and also in part by the National Science Foundation under Grant NSF PHY11-25915 to the Kavli Institute for Theoretical Physics. This work is based on ESO observational programs 66.D-0589(A), 70.D-0379(A), 074.D-0761(A), 078.D-0521(A,B), 080.D-0727(A,B), 082.D-0273(A,B), 086.D-0713(A), and 088.D-0638(A,C). Support for GO program numbers 02563, 03853,04445, 05480, 06020, 07434, 08243, 08648, 09114, 09428,10263, 11181, 11973, and 12241 was provided by NASA 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. NR 59 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 J9 ASTROPHYS J JI Astrophys. J. PD MAY 1 PY 2013 VL 768 IS 1 AR 88 DI 10.1088/0004-637X/768/1/88 PG 22 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 130ZT UT WOS:000317960500088 ER PT J AU Kraus, S Ireland, MJ Sitko, ML Monnier, JD Calvet, N Espaillat, C Grady, CA Harries, TJ Honig, SF Russell, RW Swearingen, JR Werren, C Wilner, DJ AF Kraus, Stefan Ireland, Michael J. Sitko, Michael L. Monnier, John D. Calvet, Nuria Espaillat, Catherine Grady, Carol A. Harries, Tim J. Hoenig, Sebastian F. Russell, Ray W. Swearingen, Jeremy R. Werren, Chelsea Wilner, David J. TI RESOLVING THE GAP AND AU-SCALE ASYMMETRIES IN THE PRE-TRANSITIONAL DISK OF V1247 ORIONIS SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; protoplanetary disks; stars: pre-main sequence; techniques: interferometric ID PRE-MAIN-SEQUENCE; YOUNG STELLAR OBJECTS; STAR SAO 206462; ALL-SKY SURVEY; T TAURI STARS; PROTOPLANETARY DISKS; INNER DISK; INFRARED VARIABILITY; TRANSITIONAL DISKS; DATA REDUCTION AB Pre-transitional disks are protoplanetary disks with a gapped disk structure, potentially indicating the presence of young planets in these systems. In order to explore the structure of these objects and their gap-opening mechanism, we observed the pre-transitional disk V1247 Orionis using the Very Large Telescope Interferometer, the Keck Interferometer, Keck-II, Gemini South, and IRTF. This allows us to spatially resolve the AU-scale disk structure from near-to mid-infrared wavelengths (1.5-13 mu m), tracing material at different temperatures and over a wide range of stellocentric radii. Our observations reveal a narrow, optically thick inner-disk component (located at 0.18 AU from the star) that is separated from the optically thick outer disk (radii greater than or similar to 46 AU), providing unambiguous evidence for the existence of a gap in this pre-transitional disk. Surprisingly, we find that the gap region is filled with significant amounts of optically thin material with a carbon-dominated dust mineralogy. The presence of this optically thin gap material cannot be deduced solely from the spectral energy distribution, yet it is the dominant contributor at mid-infrared wavelengths. Furthermore, using Keck/NIRC2 aperture masking observations in the H, K', and L' bands, we detect asymmetries in the brightness distribution on scales of similar to 15-40 AU, i.e., within the gap region. The detected asymmetries are highly significant, yet their amplitude and direction changes with wavelength, which is not consistent with a companion interpretation but indicates an inhomogeneous distribution of the gap material. We interpret this as strong evidence for the presence of complex density structures, possibly reflecting the dynamical interaction of the disk material with sub-stellar mass bodies that are responsible for the gap clearing. C1 [Kraus, Stefan; Espaillat, Catherine; Wilner, David J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Kraus, Stefan; Monnier, John D.; Calvet, Nuria] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Kraus, Stefan; Harries, Tim J.] Univ Exeter, Sch Phys, Exeter EX4 4QL, Devon, England. [Ireland, Michael J.] Macquarie Univ, Dept Phys & Astron, Sydney, NSW 2109, Australia. [Sitko, Michael L.; Swearingen, Jeremy R.; Werren, Chelsea] Univ Cincinnati, Dept Phys, Cincinnati, OH 45221 USA. [Sitko, Michael L.] Space Sci Inst, Boulder, CO 80301 USA. [Grady, Carol A.] Eureka Sci Inc, Oakland, CA 94602 USA. [Grady, Carol A.] NASA, Goddard Space Flight Ctr, Exoplanets & Stellar Astrophys Lab, Greenbelt, MD 20771 USA. [Hoenig, Sebastian F.] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA. [Russell, Ray W.] Aerosp Corp, Los Angeles, CA 90009 USA. RP Kraus, S (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS-78, Cambridge, MA 02138 USA. OI Hoenig, Sebastian/0000-0002-6353-1111 FU Keck observatory (NASA program) [N121IV]; Keck observatory (NOAO program) [N121N2]; Gemini South (NOAO program) [GS-2011B-Q-19]; ESO telescopes at the Paranal Observatory [088.C-0868(A), 088.C-0763(A+B)]; National Aeronautics and Space Administration; California Institute of Technology (Caltech); NASA through the Sagan Fellowship Program; W. M. Keck Foundation; Aerospace Corporation's Independent Research and Development (IRD) program; NASA ADP grant [NNX09AC73G] FX Based on observations made with the Keck observatory (NASA program ID N121IV and NOAO program ID N121N2), Gemini South (NOAO program ID GS-2011B-Q-19), and with ESO telescopes at the Paranal Observatory (ESO program IDs 088.C-0868(A)and 088.C-0763(A+B)).; Visiting Astronomer, NASA Infrared Telescope Facility, operated by the University of Hawaii under contract with the National Aeronautics and Space Administration.; We thank the referee, Jose Caballero, for his detailed report, which helped to improve the presentation of this paper. This work was done in part under contract with the California Institute of Technology (Caltech), funded by NASA through the Sagan Fellowship Program (S. K. and C. E. are Sagan Fellows). Data presented herein were obtained at the W. M. Keck Observatory from telescope time allocated to the National Aeronautics and Space Administration through the agency's scientific partnership with the California Institute of Technology and the University of California. The Observatory was made possible by the generous financial support of the W. M. Keck Foundation. The authors wish to recognize and acknowledge the very significant cultural role and reverence that the summit of Mauna Kea has always had within the indigenous Hawaiian community. We are most fortunate to have the opportunity to conduct observations from this mountain. This work was supported in part by the Aerospace Corporation's Independent Research and Development (IR&D) program. This work was supported by NASA ADP grant NNX09AC73G. NR 87 TC 19 Z9 19 U1 1 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAY 1 PY 2013 VL 768 IS 1 AR 80 DI 10.1088/0004-637X/768/1/80 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 130ZT UT WOS:000317960500080 ER PT J AU Lanz, L Zezas, A Brassington, N Smith, HA Ashby, MLN da Cunha, E Fazio, GG Hayward, CC Hernquist, L Jonsson, P AF Lanz, Lauranne Zezas, Andreas Brassington, Nicola Smith, Howard A. Ashby, Matthew L. N. da Cunha, Elisabete Fazio, Giovanni G. Hayward, Christopher C. Hernquist, Lars Jonsson, Patrik TI GLOBAL STAR FORMATION RATES AND DUST EMISSION OVER THE GALAXY INTERACTION SEQUENCE SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: interactions; galaxies: photometry; galaxies: star formation; infrared: galaxies; ultraviolet: galaxies ID SWIFT ULTRAVIOLET/OPTICAL TELESCOPE; MULTIBAND IMAGING PHOTOMETER; HERSCHEL-SPIRE INSTRUMENT; GALACTIC NUCLEUS ACTIVITY; SPITZER-SPACE-TELESCOPE; INFRARED ARRAY CAMERA; INITIAL MASS FUNCTION; DIGITAL SKY SURVEY; SIMILAR-TO 2; NEARBY GALAXIES AB We measured and modeled spectral energy distributions (SEDs) in 28 bands from the ultraviolet to the far-infrared (FIR) for 31 interacting galaxies in 14 systems. The sample is drawn from the Spitzer Interacting Galaxy Survey, which probes a range of galaxy interaction parameters at multiple wavelengths with an emphasis on the infrared bands. The subset presented in this paper consists of all galaxies for which FIR Herschel SPIRE observations are publicly available. Our SEDs combine the Herschel photometry with multi-wavelength data from Spitzer, GALEX, Swift UVOT, and 2MASS. While the shapes of the SEDs are broadly similar across our sample, strongly interacting galaxies typically have more mid-infrared emission relative to their near-infrared and FIR emission than weakly or moderately interacting galaxies. We modeled the full SEDs to derive host galaxy star formation rates (SFRs), specific star formation rates (sSFRs), stellar masses, dust temperatures, dust luminosities, and dustmasses. We find increases in the dust luminosity and mass, SFR, and cold (15-25 K) dust temperature as the interaction progresses from moderately to strongly interacting and between non-interacting and strongly interacting galaxies. We also find increases in the SFR between weakly and strongly interacting galaxies. In contrast, the sSFR remains unchanged across all the interaction stages. The ultraviolet photometry is crucial for constraining the age of the stellar population and the SFR, while dust mass is primarily determined by SPIRE photometry. The SFR derived from the SED modeling agrees well with rates estimated by proportionality relations that depend on infrared emission. C1 [Lanz, Lauranne; Zezas, Andreas; Smith, Howard A.; Ashby, Matthew L. N.; Fazio, Giovanni G.; Hernquist, Lars] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Zezas, Andreas] Univ Crete, Dept Phys, Iraklion 71003, Crete, Greece. [Zezas, Andreas] Inst Theoret & Computat Phys, Iraklion 71003, Crete, Greece. [Zezas, Andreas] Fdn Res & Technol Hellas, Iraklion 71110, Crete, Greece. [Brassington, Nicola] Univ Hertfordshire, Sch Phys Astron & Math, Hatfield AL10 9AB, Herts, England. [da Cunha, Elisabete] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Hayward, Christopher C.] Heidelberger Inst Theoret Studien, D-69118 Heidelberg, Germany. [Jonsson, Patrik] Space Explorat Technol, Hawthorne, CA 90250 USA. RP Lanz, L (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM llanz@head.cfa.harvard.edu RI Hayward, Christopher/I-4756-2012; Zezas, Andreas/C-7543-2011; OI Hayward, Christopher/0000-0003-4073-3236; Zezas, Andreas/0000-0001-8952-676X; Lanz, Lauranne/0000-0002-3249-8224; da Cunha, Elisabete/0000-0001-9759-4797 FU National Aeronautics and Space Administration; NASA [NNX10AD68G, NASA JPL RSA 1369566]; EU IRG grant [224878]; [AR-12011X] FX We are grateful to Gregory Snyder, Maria Koutoulaki, and Flora Stanley for their classifications of our galaxies, Steven Willner for his classifications and helpful comments, Volker Tolls for his assistance in processing Herschel data, Don Neill and Susan Neff at the GALEX helpdesk for the reprocessing of the observation of NGC 3690/IC 694, Erik Hoversten for his assistance with regards to the UVOT corrections, Christopher Klein for his preparation of the IRAC observations, and Joseph Hora for his assistance with galaxies on the edge of SPIRE observations. This work was based on archival data obtained from the Spitzer Science Archive, the Mikulski Archive for Space Telescopes (MAST), the Swift data archive, and the Herschel Science Archive. 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. This work was supported in party NASA grant NNX10AD68G and NASA JPL RSA 1369566. A.Z. acknowledges support from AR-12011X Chandra grant and EU IRG grant 224878. NR 117 TC 32 Z9 32 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 MAY 1 PY 2013 VL 768 IS 1 AR 90 DI 10.1088/0004-637X/768/1/90 PG 33 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 130ZT UT WOS:000317960500090 ER PT J AU Larsson, J Fransson, C Kjaer, K Jerkstrand, A Kirshner, RP Leibundgut, B Lundqvist, P Mattila, S McCray, R Sollerman, J Spyromilio, J Wheeler, JC AF Larsson, Josefin Fransson, Claes Kjaer, Karina Jerkstrand, Anders Kirshner, Robert P. Leibundgut, Bruno Lundqvist, Peter Mattila, Seppo McCray, Richard Sollerman, Jesper Spyromilio, Jason Wheeler, J. Craig TI THE MORPHOLOGY OF THE EJECTA IN SUPERNOVA 1987A: A STUDY OVER TIME AND WAVELENGTH SO ASTROPHYSICAL JOURNAL LA English DT Article DE supernovae: individual (SN 1987A) ID CORE-COLLAPSE SUPERNOVAE; INNER CIRCUMSTELLAR RING; CASSIOPEIA-A SUPERNOVA; SN 1987A; LINE EMISSION; LIGHT-CURVE; CHANDRA OBSERVATIONS; HOT-SPOTS; REMNANT; EVOLUTION AB We present a study of the morphology of the ejecta in Supernova 1987A based on images and spectra from the Hubble Space Telescope (HST) as well as integral field spectroscopy from VLT/SINFONI. The HST observations were obtained between 1994 and 2011 and primarily probe the outer H-rich zones of the ejecta. The SINFONI observations were obtained in 2005 and 2011 and instead probe the [Si I]+[Fe II] emission from the inner regions. We find a strong temporal evolution of the morphology in the HST images, from a roughly elliptical shape before similar to 5000 days, to a more irregular, edge-brightened morphology with a "hole" in the middle thereafter. This transition is a natural consequence of the change in the dominant energy source powering the ejecta, from radioactive decay before similar to 5000 days to X-ray input from the circumstellar interaction thereafter. The [Si I]+[Fe II] images display a more uniform morphology, which may be due to a remaining significant contribution from radioactivity in the inner ejecta and the higher abundance of these elements in the core. Both the Ha and the [Si I]+[Fe II] line profiles show that the ejecta are distributed fairly close to the plane of the inner circumstellar ring, which is assumed to define the rotational axis of the progenitor star. The Ha emission extends to higher velocities than [Si I]+[Fe II], as expected from theoretical models. There is no clear symmetry axis for all the emission. Instead, we find that the emission is concentrated to clumps and that the emission is distributed somewhat closer to the ring in the north than in the south. This north-south asymmetry may be partially explained by dust absorption. We compare our results with explosion models and find some qualitative agreement, but note that the observations show a higher degree of large-scale asymmetry. C1 [Larsson, Josefin] KTH, Dept Phys, SE-10691 Stockholm, Sweden. [Larsson, Josefin] AlbaNova, Oskar Klein Ctr, SE-10691 Stockholm, Sweden. [Fransson, Claes; Lundqvist, Peter; Sollerman, Jesper] Stockholm Univ, AlbaNova, Dept Astron, SE-10691 Stockholm, Sweden. [Fransson, Claes; Lundqvist, Peter; Sollerman, Jesper] Stockholm Univ, AlbaNova, Oskar Klein Ctr, SE-10691 Stockholm, Sweden. [Kjaer, Karina; Leibundgut, Bruno; Spyromilio, Jason] ESO, D-85748 Garching, Germany. [Jerkstrand, Anders] Queens Univ Belfast, Astrophys Res Ctr, Sch Maths & Phys, Belfast BT7 1NN, Antrim, North Ireland. [Kirshner, Robert P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Mattila, Seppo] Univ Turku, Finnish Ctr Astron ESO FINCA, FI-21500 Piikkio, Finland. [McCray, Richard] Univ Colorado, JILA, Boulder, CO 80309 USA. [Wheeler, J. Craig] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA. RP Larsson, J (reprint author), KTH, Dept Phys, SE-10691 Stockholm, Sweden. RI Jerkstrand, Anders/K-9648-2015; OI Jerkstrand, Anders/0000-0001-8005-4030; Sollerman, Jesper/0000-0003-1546-6615; /0000-0003-0065-2933 FU Swedish National Space Board; Swedish Research Council; National Science Foundation [NSF PHY11-25915]; NASA through grants from the Space Telescope Science Institute [02563, 03853, 04445, 05480, 06020, 07434, 08243, 08648, 09114, 09428, 10263, 11181, 11973, 12241]; NASA [NAS5-26555]; European Organisation for Astronomical Research in the Southern Hemisphere, Chile (ESO Programme) [076.D0558, 086.D-0713(C)] FX We thank the anonymous referee for a careful reading of the manuscript. This work was supported by the Swedish National Space Board and the Swedish Research Council. R.P.K.'s work was supported in part by the National Science Foundation under Grant NSF PHY11-25915 to the Kavli Institute for Theoretical Physics. Support for HST GO program numbers 02563, 03853, 04445, 05480, 06020, 07434, 08243, 08648, 09114, 09428, 10263, 11181, 11973, and 12241 was provided by NASA 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. The ground-based observations were collected at the European Organisation for Astronomical Research in the Southern Hemisphere, Chile (ESO Programme 076.D0558 and 086.D-0713(C)). NR 60 TC 19 Z9 19 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 MAY 1 PY 2013 VL 768 IS 1 AR 89 DI 10.1088/0004-637X/768/1/89 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 130ZT UT WOS:000317960500089 ER PT J AU Martini, P Miller, ED Brodwin, M Stanford, SA Gonzalez, AH Bautz, M Hickox, RC Stern, D Eisenhardt, PR Galametz, A Norman, D Jannuzi, BT Dey, A Murray, S Jones, C Brown, MJI AF Martini, Paul Miller, E. D. Brodwin, M. Stanford, S. A. Gonzalez, Anthony H. Bautz, M. Hickox, R. C. Stern, D. Eisenhardt, P. R. Galametz, A. Norman, D. Jannuzi, B. T. Dey, A. Murray, S. Jones, C. Brown, M. J. I. TI THE CLUSTER AND FIELD GALAXY ACTIVE GALACTIC NUCLEUS FRACTION AT z=1-1.5: EVIDENCE FOR A REVERSAL OF THE LOCAL ANTICORRELATION BETWEEN ENVIRONMENT AND AGN FRACTION SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: active; galaxies: clusters: general; galaxies: evolution; X-rays: galaxies; X-rays: galaxies: clusters; X-rays: general ID SUPERMASSIVE BLACK-HOLES; DIGITAL-SKY-SURVEY; IRAC SHALLOW SURVEY; SIMILAR-TO 1; CHANDRA MULTIWAVELENGTH PROJECT; ULTRALUMINOUS INFRARED GALAXIES; FORMATION-DENSITY RELATION; EMISSION-LINE GALAXIES; HUBBLE-SPACE-TELESCOPE; LOW-REDSHIFT CLUSTERS AB The fraction of cluster galaxies that host luminous active galactic nuclei (AGNs) is an important probe of AGN fueling processes, the cold interstellar medium at the centers of galaxies, and how tightly black holes and galaxies co-evolve. We present a new measurement of the AGN fraction in a sample of 13 clusters of galaxies (M >= 10(14) M-circle dot) at 1 < z < 1.5 selected from the Spitzer/IRAC Shallow Cluster Survey, as well as the field fraction in the immediate vicinity of these clusters, and combine these data with measurements from the literature to quantify the relative evolution of cluster and field AGN from the present to z similar to 3. We estimate that the cluster AGN fraction at 1 < z < 1.5 is f(A) = 3.0(-1.4)(+2.4)% for AGNs with a rest-frame, hard X-ray luminosity greater than L-X,L- H >= 10(44) erg s(-1). This fraction is measured relative to all cluster galaxies more luminous than M-3.6*(z)+ 1, where M-3.6*(z) is the absolute magnitude of the break in the galaxy luminosity function at the cluster redshift in the IRAC 3.6 mu m bandpass. The cluster AGN fraction is 30 times greater than the 3 sigma upper limit on the value for AGNs of similar luminosity at z similar to 0.25, as well as more than an order of magnitude greater than the AGN fraction at z similar to 0.75. AGNs with L-X,L- H >= 10(43) erg s(-1) exhibit similarly pronounced evolution with redshift. In contrast to the local universe, where the luminous AGN fraction is higher in the field than in clusters, the X-ray and MIR-selected AGN fractions in the field and clusters are consistent at 1 < z < 1.5. This is evidence that the cluster AGN population has evolved more rapidly than the field population from z similar to 1.5 to the present. This environment-dependent AGN evolution mimics the more rapid evolution of star-forming galaxies in clusters relative to the field. C1 [Martini, Paul] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. [Martini, Paul] Ohio State Univ, Ctr Cosmol & Astroparticle Phys, Columbus, OH 43210 USA. [Miller, E. D.; Bautz, M.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Brodwin, M.] Univ Missouri, Dept Phys & Astron, Kansas City, MO 64110 USA. [Stanford, S. A.] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA. [Stanford, S. A.] Lawrence Livermore Natl Lab, Inst Geophys & Planetary Phys, Livermore, CA 94551 USA. [Gonzalez, Anthony H.] Univ Florida, Dept Astron, Gainesville, FL 32611 USA. [Hickox, R. C.] Dartmouth Coll, Dept Phys & Astron, Wilder Lab 6127, Hanover, NH 03755 USA. [Stern, D.; Eisenhardt, P. R.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Galametz, A.] INAF Osservatorio Roma, I-00040 Monte Porzio Catone, Italy. [Norman, D.; Dey, A.] Natl Opt Astron Observ, Tucson, AZ 85719 USA. [Jannuzi, B. T.] Univ Arizona, Dept Astron, Tucson, AZ 85721 USA. [Jannuzi, B. T.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Murray, S.; Jones, C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Brown, M. J. I.] Monash Univ, Sch Phys, Clayton, Vic 3800, Australia. RP Martini, P (reprint author), North Amer ALMA Sci Ctr, Charlottesville, VA 22903 USA. EM martini@astronomy.ohio-state.edu RI Brown, Michael/B-1181-2015 OI Brown, Michael/0000-0002-1207-9137 FU U.S. Department of Energy by Lawrence Livermore National Laboratory [DE-AC52-07NA27344]; National Aeronautics and Space Administration through Chandra Award [GO9-0150A]; National Aeronautics Space Administration [NAS8-03060] FX We thank Daryl Haggard for calculating the field AGN fraction based on our AGN and galaxy luminosity thresholds. We also appreciate a thoughtful and helpful review from the referee. P. M. appreciates support from the sabbatical visitor program at the North American ALMA Science Center (NAASC) at NRAO and the hospitality of both the NAASC and the University of Virginia while this work was completed. The work of P. R. M. E. and D. S. was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA. Part of this work was performed under the auspices of the U.S. Department of Energy by Lawrence Livermore National Laboratory under Contract DE-AC52-07NA27344. Support for this work was provided by the National Aeronautics and Space Administration through Chandra Award Number GO9-0150A 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 NAS8-03060. NR 117 TC 37 Z9 38 U1 0 U2 7 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAY 1 PY 2013 VL 768 IS 1 AR 1 DI 10.1088/0004-637X/768/1/1 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 130ZT UT WOS:000317960500001 ER PT J AU Rappaport, S Deck, K Levine, A Borkovits, T Carter, J El Mellah, I Sanchis-Ojeda, R Kalomeni, B AF Rappaport, S. Deck, K. Levine, A. Borkovits, T. Carter, J. El Mellah, I. Sanchis-Ojeda, R. Kalomeni, B. TI TRIPLE-STAR CANDIDATES AMONG THE KEPLER BINARIES SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries: close; binaries: eclipsing; binaries: general; celestial mechanics; stars: formation; stars: statistics ID STELLAR 3-BODY PROBLEM; HIERARCHICAL TRIPLE; ECLIPSING BINARIES; ADDITIONAL COMPONENTS; CONTACT BINARIES; LOW-MASS; SPECTROSCOPIC BINARIES; ORBITAL EVOLUTION; TIMING VARIATIONS; ERROR-CORRECTION AB We present the results of a search through the photometric database of Kepler eclipsing binaries looking for evidence of hierarchical triple-star systems. The presence of a third star orbiting the binary can be inferred from eclipse timing variations. We apply a simple algorithm in an automated determination of the eclipse times for all 2157 binaries. The "calculated" eclipse times, based on a constant period model, are subtracted from those observed. The resulting O-C (observed minus calculated times) curves are then visually inspected for periodicities in order to find triple-star candidates. After eliminating false positives due to the beat frequency between the similar to 1/2 hr Kepler cadence and the binary period, 39 candidate triple systems were identified. The periodic O-C curves for these candidates were then fit for contributions from both the classical Roemer delay and so-called physical delay, in an attempt to extract a number of the system parameters of the triple. We discuss the limitations of the information that can be inferred from these O-C curves without further supplemental input, e.g., ground-based spectroscopy. Based on the limited range of orbital periods for the triple-star systems to which this search is sensitive, we can extrapolate to estimate that at least 20% of all close binaries have tertiary companions. C1 [Rappaport, S.; Deck, K.; Sanchis-Ojeda, R.] MIT, Dept Phys, Cambridge, MA 02139 USA. [Rappaport, S.; Deck, K.; Sanchis-Ojeda, R.] Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Levine, A.] 37 575 MIT Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Borkovits, T.] Baja Astron Observ, H-6500 Baja, Hungary. [Borkovits, T.] MTA CSFK, Konkoly Observ, H-1121 Budapest, Hungary. [Borkovits, T.] ELTE Gothard Lendulet Res Grp, H-9700 Szombathely, Hungary. [Carter, J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [El Mellah, I.] ENS Cachan, F-94235 Cachan, France. [Kalomeni, B.] Univ Ege, Dept Astron & Space Sci, TR-35100 Bornova, Turkey. [Kalomeni, B.] Izmir Inst Technol, Dept Phys, TR-35430 Izmir, Turkey. RP Rappaport, S (reprint author), MIT, Dept Phys, 70 Vassar St, Cambridge, MA 02139 USA. EM sar@mit.edu; kdeck@mit.edu; aml@space.mit.edu; borko@electra.bajaobs.hu; jacarter@cfa.harvard.edu; ielmelah@ens-cachan.fr; rsanchis@mit.edu FU NASA by the Space Telescope Science Institute [HF-51267.01-A]; NASA [NAS 5-26555]; National Science Foundation FX The authors thank Josh Winn for very helpful discussions. We acknowledge Kathy Tran who participated in some of the eclipse timing analysis, focusing on the behavior of contact binaries. The authors are grateful to the Kepler Eclipsing Binary Team for generating the catalog of eclipsing binaries utilized in this work. Specifically, we thank Andrej Prsa for providing us with a list of newly rejected and "uncertain" binaries, a number of which are now considered to be pulsating stars. J.A.C. acknowledges support for this work that was provided by NASA through Hubble Fellowship Grant HF-51267.01-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. K.M.D. acknowledges support from a National Science Foundation Graduate Fellowship. NR 57 TC 56 Z9 56 U1 1 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAY 1 PY 2013 VL 768 IS 1 AR 33 DI 10.1088/0004-637X/768/1/33 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 130ZT UT WOS:000317960500033 ER PT J AU Temim, T Slane, P Castro, D Plucinsky, PP Gelfand, J Dickel, JR AF Temim, Tea Slane, Patrick Castro, Daniel Plucinsky, Paul P. Gelfand, Joseph Dickel, John R. TI HIGH-ENERGY EMISSION FROM THE COMPOSITE SUPERNOVA REMNANT MSH 15-56 SO ASTROPHYSICAL JOURNAL LA English DT Article DE gamma rays: ISM; ISM: individual objects (MSH 15-56, G326.1-1.8); ISM: supernova remnants; pulsars: general; X-rays: ISM ID LARGE-AREA TELESCOPE; PULSAR WIND NEBULA; CHANDRA OBSERVATIONS; EVOLUTION; CATALOG; G326.3-1.8; MODEL; RAY AB MSH 15-56 (G326.3-1.8) is a composite supernova remnant (SNR) that consists of an SNR shell and a displaced pulsar wind nebula (PWN) in the radio. We present XMM-Newton and Chandra X-ray observations of the remnant that reveal a compact source at the tip of the radio PWN and complex structures that provide evidence for mixing of the supernova (SN) ejecta with PWN material following a reverse shock interaction. The X-ray spectra are well fitted by a non-thermal power-law model whose photon index steepens with distance from the presumed pulsar, and a thermal component with an average temperature of 0.55 keV. The enhanced abundances of silicon and sulfur in some regions, and the similar temperature and ionization timescale, suggest that much of the X-ray emission can be attributed to SN ejecta that have either been heated by the reverse shock or swept up by the PWN. We find one region with a lower temperature of 0.3 keV that appears to be in ionization equilibrium. Assuming the Sedov model, we derive a number of SNR properties, including an age of 16,500 yr. Modeling of the gamma-ray emission detected by Fermi shows that the emission may originate from the reverse shock-crushed PWN. C1 [Temim, Tea] NASA, Goddard Space Flight Ctr, Observat Cosmol Lab, Greenbelt, MD 20771 USA. [Temim, Tea] Oak Ridge Associated Univ, Oak Ridge, TN 37831 USA. [Slane, Patrick; Plucinsky, Paul P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Castro, Daniel] MIT Kavli Ctr Astrophys & Space Res, Cambridge, MA 02139 USA. [Gelfand, Joseph] New York Univ Abu Dhabi, Abu Dhabi, U Arab Emirates. [Dickel, John R.] Univ New Mexico, Dept Phys & Astron, Albuquerque, NM 87131 USA. RP Temim, T (reprint author), NASA, Goddard Space Flight Ctr, Observat Cosmol Lab, Code 665, Greenbelt, MD 20771 USA. EM tea.temim@nasa.gov RI Gelfand, Joseph/F-1110-2015; OI Gelfand, Joseph/0000-0003-4679-1058; Temim, Tea/0000-0001-7380-3144 FU NASA; NASA [NAS8-03060, NNX11AQ09G] FX T.T. 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. P. S. and P. P. acknowledge partial support from NASA contract NAS8-03060, and P. S. acknowledges partial support from NASA grant NNX11AQ09G. NR 35 TC 4 Z9 4 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 MAY 1 PY 2013 VL 768 IS 1 AR 61 DI 10.1088/0004-637X/768/1/61 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 130ZT UT WOS:000317960500061 ER PT J AU Tilvi, V Papovich, C Tran, KVH Labbe, I Spitler, LR Straatman, CMS Persson, SE Monson, A Glazebrook, K Quadri, RF van Dokkum, P Ashby, MLN Faber, SM Fazio, GG Finkelstein, SL Ferguson, HC Grogin, NA Kacprzak, GG Kelson, DD Koekemoer, AM Murphy, D McCarthy, PJ Newman, JA Salmon, B Willner, SP AF Tilvi, V. Papovich, C. Tran, K. -V. H. Labbe, I. Spitler, L. R. Straatman, C. M. S. Persson, S. E. Monson, A. Glazebrook, K. Quadri, R. F. van Dokkum, P. Ashby, M. L. N. Faber, S. M. Fazio, G. G. Finkelstein, S. L. Ferguson, H. C. Grogin, N. A. Kacprzak, G. G. Kelson, D. D. Koekemoer, A. M. Murphy, D. McCarthy, P. J. Newman, J. A. Salmon, B. Willner, S. P. TI DISCOVERY OF LYMAN BREAK GALAXIES AT z similar to 7 FROM THE zFourGE SURVEY SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: formation; galaxies: high-redshift; galaxies: luminosity function, mass function; galaxies: star formation ID ULTRA-DEEP-FIELD; HUBBLE-SPACE-TELESCOPE; STAR-FORMING GALAXIES; LY-ALPHA EMITTERS; UV LUMINOSITY FUNCTION; STELLAR MASS DENSITY; HIGH-REDSHIFT GALAXIES; EXTRAGALACTIC LEGACY SURVEY; REST-FRAME ULTRAVIOLET; Z-DROPOUT GALAXIES AB Star-forming galaxies at redshiftsz > 6 are likely responsible for the reionization of the universe, and it is important to study the nature of these galaxies. We present three candidates for z similar to 7 Lyman break galaxies (LBGs) from a 155 arcmin(2) area in the CANDELS/COSMOS field imaged by the deep FourStar Galaxy Evolution (zFourGE) survey. The FourStar medium-band filters provide the equivalent of R similar to 10 spectroscopy, which cleanly distinguishes between z similar to 7 LBGs and brown dwarf stars. The distinction between stars and galaxies based on an object's angular size can become unreliable even when using Hubble Space Telescope imaging; there exists at least one very compact z similar to 7 candidate (FWHM similar to 0.5-1 kpc) that is indistinguishable from a point source. The medium-band filters provide narrower redshift distributions compared with broadband-derived redshifts. The UV luminosity function derived using the three z similar to 7 candidates is consistent with previous studies, suggesting an evolution at the bright end (MUV similar to -21.6 mag) from z similar to 7 to z similar to 5. Fitting the galaxies' spectral energy distributions, we predict Ly alpha equivalent widths for the two brightest LBGs, and find that the presence of a Ly alpha line affects the medium-band flux thereby changing the constraints on stellar masses and UV spectral slopes. This illustrates the limitations of deriving LBG properties using only broadband photometry. The derived specific star-formation rates for the bright LBGs are similar to 13 Gyr(-1), slightly higher than the lower-luminosity LBGs, implying that the star-formation rate increases with stellar mass for these galaxies. C1 [Tilvi, V.; Papovich, C.; Tran, K. -V. H.] Texas A&M Univ, George P & Cynthia Woods Mitchell Inst Fundamenta, College Stn, TX 77843 USA. [Tilvi, V.; Papovich, C.; Tran, K. -V. H.] Texas A&M Univ, Dept Phys & Astron, College Stn, TX USA. [Labbe, I.; Straatman, C. M. S.] Leiden Univ, Sterrewacht Leiden, NL-2300 RA Leiden, Netherlands. [Spitler, L. R.; Glazebrook, K.; Kacprzak, G. G.] Swinburne Univ Technol, Ctr Astrophys & Supercomp, Hawthorn, Vic 3122, Australia. [Persson, S. E.; Monson, A.; Quadri, R. F.; Kelson, D. D.; Murphy, D.; McCarthy, P. J.] Carnegie Observ, Pasadena, CA 91101 USA. [van Dokkum, P.] Yale Univ, Dept Astron, New Haven, CT 06520 USA. [Ashby, M. L. N.; Fazio, G. G.; Willner, S. P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Faber, S. M.] Univ Calif Santa Cruz, Dept Astron & Astrophys, UCO Lick Observ, Santa Cruz, CA 95064 USA. [Finkelstein, S. L.] Univ Texas Austin, Austin, TX 78712 USA. [Ferguson, H. C.; Grogin, N. A.; Koekemoer, A. M.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Newman, J. A.] Univ Pittsburgh, Pittsburgh, PA 15260 USA. RP Tilvi, V (reprint author), Texas A&M Univ, George P & Cynthia Woods Mitchell Inst Fundamenta, College Stn, TX 77843 USA. RI Glazebrook, Karl/N-3488-2015; OI Glazebrook, Karl/0000-0002-3254-9044; Koekemoer, Anton/0000-0002-6610-2048 FU National Science Foundation [AST-1009707]; NASA [NAS5-26555]; HST [GO-12060]; NASA through Space Telescope Science Institute [GO-12060]; Australian Research Council [DP1094370]; NASA through JPL/Caltech FX This work was supported by the National Science Foundation grant AST-1009707. This work is based on observations taken by the CANDELS Multi-Cycle Treasury Program with the NASA/ESA HST, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555. This work is supported by HST program No. GO-12060. Support for Program number GO-12060 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, Inc., under NASA contract NAS5-26555. Australian access to the Magellan Telescopes was supported through the National Collaborative Research Infrastructure Strategy of the Australian Federal Government. L. R. S. acknowledges funding from a Australian Research Council Discovery Program grant DP1094370. 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. We acknowledge generous support from the Texas A&M University and the George P. and Cynthia Woods Institute for Fundamental Physics and Astronomy. NR 115 TC 24 Z9 24 U1 0 U2 7 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAY 1 PY 2013 VL 768 IS 1 AR 56 DI 10.1088/0004-637X/768/1/56 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 130ZT UT WOS:000317960500056 ER PT J AU Weiss, LM Marcy, GW Rowe, JF Howard, AW Isaacson, H Fortney, JJ Miller, N Demory, BO Fischer, DA Adams, ER Dupree, AK Howell, SB Kolbl, R Johnson, JA Horch, EP Everett, ME Fabrycky, DC Seager, S AF Weiss, Lauren M. Marcy, Geoffrey W. Rowe, Jason F. Howard, Andrew W. Isaacson, Howard Fortney, Jonathan J. Miller, Neil Demory, Brice-Olivier Fischer, Debra A. Adams, Elisabeth R. Dupree, Andrea K. Howell, Steve B. Kolbl, Rea Johnson, John Asher Horch, Elliott P. Everett, Mark E. Fabrycky, Daniel C. Seager, Sara TI THE MASS OF KOI-94d AND A RELATION FOR PLANET RADIUS, MASS, AND INCIDENT FLUX SO ASTROPHYSICAL JOURNAL LA English DT Article DE planets and satellites: composition; stars: individual (KOI, 94, KIC 6462863, 2MASS J19491993+4153280); techniques: photometric; techniques: spectroscopic ID COROT SPACE MISSION; TRANSITING HOT JUPITER; LOW-DENSITY PLANET; SOLAR-TYPE STAR; SUN-LIKE STAR; HOBBY-EBERLY TELESCOPE; FOLLOW-UP PROGRAM; GAS-GIANT PLANET; METAL-POOR STAR; B-LIKE PLANETS AB We measure the mass of a modestly irradiated giant planet, KOI-94d. We wish to determine whether this planet, which is in a 22 day orbit and receives 2700 times as much incident flux as Jupiter, is as dense as Jupiter or rarefied like inflated hot Jupiters. KOI-94 also hosts at least three smaller transiting planets, all of which were detected by the Kepler mission. With 26 radial velocities of KOI-94 from the W.M. Keck Observatory and a simultaneous fit to the Kepler light curve, we measure the mass of the giant planet and determine that it is not inflated. Support for the planetary interpretation of the other three candidates comes from gravitational interactions through transit timing variations, the statistical robustness of multi-planet systems against false positives, and several lines of evidence that no other star resides within the photometric aperture. We report the properties of KOI-94b (M-P = 10.5 +/- 4.6 M-circle plus, R-P = 1.71 +/- 0.16 R-circle plus, P = 3.74 days), KOI-94c (M-P = 15.6(15.6)(+5.7) M-circle plus, R-P = 4.32 +/- 0.41 R-circle plus, P = 10.4 days), KOI-94d (M-P = 106 +/- 11 M-circle plus, R-P = 11.27 +/- 1.06 R-circle plus, P = 22.3 days), and KOI-94e (M-P = 35(-28)(+18) M-circle plus, R-P = 6.56 +/- 0.62 R-circle plus, P = 54.3 days). The radial velocity analyses of KOI-94b and KOI-94e offer marginal (>2 sigma) mass detections, whereas the observations of KOI-94c offer only an upper limit to its mass. Using the KOI-94 system and other planets with published values for both mass and radius (138 exoplanets total, including 35 with M-P < 150 M-circle plus), we establish two fundamental planes for exoplanets that relate their mass, incident flux, and radius from a few Earth masses up to 13 Jupiter masses: (R-P/R-circle plus) = 1.78(M-P/M-circle plus) 0.53(F/erg s(-1) cm(-2))(-0.03) for M-P < 150 M-circle plus, and R-P/R-circle plus = 2.45(M-P/M-circle plus)(-0.039)(F/erg s(-1) cm(-2))(0.094) for M-P > 150 M-circle dot. These equations can be used to predict the radius or mass of a planet. C1 [Weiss, Lauren M.; Marcy, Geoffrey W.; Isaacson, Howard; Kolbl, Rea] Univ Calif Berkeley, Dept Astron, Hearst Field Annex B 20, Berkeley, CA 94720 USA. [Rowe, Jason F.; Howell, Steve B.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Howard, Andrew W.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Fortney, Jonathan J.; Miller, Neil] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. [Demory, Brice-Olivier; Seager, Sara] MIT, Cambridge, MA 02139 USA. [Fischer, Debra A.] Yale Univ, Dept Astron, New Haven, CT 06510 USA. [Adams, Elisabeth R.; Dupree, Andrea K.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Johnson, John Asher] CALTECH, Pasadena, CA 91106 USA. [Horch, Elliott P.] So Connecticut State Univ, Dept Phys, New Haven, CT 06515 USA. [Everett, Mark E.] Natl Opt Astron Observ, Tucson, AZ 85719 USA. [Fabrycky, Daniel C.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. RP Weiss, LM (reprint author), Univ Calif Berkeley, Dept Astron, Hearst Field Annex B 20, 601 Campbell Hall, Berkeley, CA 94720 USA. EM lweiss@berkeley.edu RI Howard, Andrew/D-4148-2015; OI Howard, Andrew/0000-0001-8638-0320; Fortney, Jonathan/0000-0002-9843-4354; Weiss, Lauren/0000-0002-3725-3058; Demory, Brice-Olivier/0000-0002-9355-5165; Fabrycky, Daniel/0000-0003-3750-0183 FU NSF [DGE 1106400] FX L.M.W. is financially supported by the National Science Foundation Graduate Research Fellowship Program, Grant DGE 1106400. NR 177 TC 90 Z9 91 U1 2 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 MAY 1 PY 2013 VL 768 IS 1 AR 14 DI 10.1088/0004-637X/768/1/14 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 130ZT UT WOS:000317960500014 ER PT J AU Garzon-Lopez, CX Bohlman, SA Olff, H Jansen, PA AF Garzon-Lopez, Carol X. Bohlman, Stephanie A. Olff, Han Jansen, Patrick A. TI Mapping Tropical Forest Trees Using High-Resolution Aerial Digital Photographs SO BIOTROPICA LA English DT Article DE Barro Colorado Island; high-resolution aerial digital photography; remote sensing; spatial patterns; tropical forest ID RAIN-FOREST; SPATIAL-PATTERNS; SCALE; DISPERSAL; IMAGERY; IDENTIFICATION; BIODIVERSITY; LIMITATION; MANAGEMENT; DYNAMICS AB The spatial arrangement of tree species is a key aspect of community ecology. Because tree species in tropical forests occur at low densities, it is logistically challenging to measure distributions across large areas. In this study, we evaluated the potential use of canopy tree crown maps, derived from high-resolution aerial digital photographs, as a relatively simple method for measuring large-scale tree distributions. At Barro Colorado Island, Panama, we used high-resolution aerial digital photographs (similar to 0.129m/pixel) to identify tree species and map crown distributions of four target tree species. We determined crown mapping accuracy by comparing aerial and ground-mapped distributions and tested whether the spatial characteristics of the crown maps reflect those of the ground-mapped trees. Nearly a quarter (22%) of the common canopy species had sufficiently distinctive crowns to be good candidates for reliable mapping. The errors of commission (crowns misidentified as a target species) were relatively low, but the errors of omission (missed canopy trees of the target species) were high. Only 40 percent of canopy individuals were mapped on the air photographs. Despite failing to accurately predict exact abundances of canopy trees, crown distributions accurately reproduced the clumping patterns and spatial autocorrelation features of three of four tree species and predicted areas of high and low abundance. We discuss a range of ecological and forest management applications for which this method can be useful. C1 [Garzon-Lopez, Carol X.; Olff, Han; Jansen, Patrick A.] Univ Groningen, Ctr Life Sci, NL-9747 AG Groningen, Netherlands. [Bohlman, Stephanie A.] Univ Florida, Sch Forest Resources & Conservat, Gainesville, FL 32611 USA. [Bohlman, Stephanie A.; Jansen, Patrick A.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. [Jansen, Patrick A.] Wageningen Univ, Ctr Ecosyst Studies, NL-6700 AA Wageningen, Netherlands. RP Garzon-Lopez, CX (reprint author), Univ Groningen, Ctr Life Sci, Nijenborgh 7, NL-9747 AG Groningen, Netherlands. EM c.x.garzon@gmail.com RI Garzon-Lopez, Carol/G-6251-2014; Jansen, Patrick/G-2545-2015; Olff, Han/A-8516-2008 OI Garzon-Lopez, Carol/0000-0002-4099-2740; Jansen, Patrick/0000-0002-4660-0314; Olff, Han/0000-0003-2154-3576 FU National Science Foundation [DEB 0453665]; University of Groningen FX We thank Helene Muller-Landau for initiating the photo acquisition and the University of Minnesota for funding, We also thank the Smithsonian Tropical Research Institute for their logistical support, and the Center of Tropical Forest Science for making publicly available information regarding the 50-ha Dynamics Plot. We are very grateful to Joe Wright and Helene Muller-Landau for his vital support and sharing data of the 6-ha plots, funded by the National Science Foundation (DEB 0453665). We specially wish to thank Alejandro Ordonez for his input to the manuscript and Marcos Guerra for taking the photographs. The Ubbo Emmius scholarship program of the University of Groningen (CXG) funded this work. NR 54 TC 3 Z9 3 U1 3 U2 59 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0006-3606 J9 BIOTROPICA JI Biotropica PD MAY PY 2013 VL 45 IS 3 BP 308 EP 316 DI 10.1111/btp.12009 PG 9 WC Ecology SC Environmental Sciences & Ecology GA 135UU UT WOS:000318314900006 ER PT J AU Yorke, SR Schnitzer, SA Mascaro, J Letcher, SG Carson, WP AF Yorke, Suzanne R. Schnitzer, Stefan A. Mascaro, Joseph Letcher, Susan G. Carson, Walter P. TI Increasing Liana Abundance and Basal Area in a Tropical Forest: The Contribution of Long-distance Clonal Colonization SO BIOTROPICA LA English DT Article DE climate change; Costa Rica; La Selva Biological Station; recruitment; succession; vegetative reproduction ID BARRO-COLORADO ISLAND; TREE REGENERATION; TEMPERATE FORESTS; SPECIES RICHNESS; LOWLAND FOREST; CANOPY LIANAS; RAIN-FOREST; WET FOREST; DIVERSITY; GAPS AB Recent evidence suggests that liana abundance and biomass are increasing in Neotropical forests, representing a major structural change to tropical ecosystems. Explanations for these increases, however, remain largely untested. Over an 8-yr period (19992007), we censused lianas in nine, 24x36m permanent plots in old-growth and selectively logged forest at La Selva Biological Station, Costa Rica to test whether: (1) liana abundance and basal area are increasing in this forest; (2) the increase is being driven by increased recruitment, decreased mortality, or both; and (3) long-distance clonal colonization explains the increase in liana abundance and basal area. We defined long-distance clonal colonization as lianas that entered and rooted in the plots as vegetative propagules of stems that originated from outside or above the plot, and were present in 2007, but not in 1999 or 2002. Our hypotheses were supported in the old-growth forest: mean liana abundance and BA (1cm diameter) increased 15 and 20 percent, respectively, and clonal colonization from outside of the plots contributed 19 and 60 percent (respectively) to these increases. Lianas colonized clonally by falling vertically from the forest canopy above or growing horizontally along the forest floor and re-rootingcommon forms of colonization for many liana species. In the selectively logged forest, liana abundance and BA did not change, and thus the pattern of increasing lianas may be restricted to old-growth forests. In summary, our data support the hypothesis that lianas are increasing in old-growth forests, and that long-distance clonal colonization is a major contributor. C1 [Yorke, Suzanne R.; Schnitzer, Stefan A.; Mascaro, Joseph] Univ Wisconsin Milwaukee, Dept Biol Sci, Milwaukee, WI 53201 USA. [Schnitzer, Stefan A.; Mascaro, Joseph] Smithsonian Trop Res Inst, Ancon, Panama. [Letcher, Susan G.] SUNY Coll Purchase, Dept Environm Studies, Purchase, NY 10577 USA. [Carson, Walter P.] Univ Pittsburgh, Dept Biol Sci, Pittsburgh, PA 15260 USA. [Mascaro, Joseph] Carnegie Inst Sci, Dept Global Ecol, Stanford, CA 94305 USA. RP Schnitzer, SA (reprint author), Univ Wisconsin Milwaukee, Dept Biol Sci, POB 413, Milwaukee, WI 53201 USA. EM S1@uwm.edu OI Schnitzer, Stefan/0000-0002-2715-9455; Letcher, Susan/0000-0002-9475-7674 FU University of Wisconsin - Milwaukee Research Growth Initiative program; University of Wisconsin - Milwaukee Center for Latin American and Caribbean Studies; NSF [DEB-0613666, DEB-0845071, DEB-9527729, DEB-0212054]; Andrew Mellon Foundation FX We thank Laura Ingwell and Orlando Vargas for help with data collection, and David Clark and Deborah Clark provided helpful comments on land-use history at La Selva, as well as on an early draft of the manuscript. This study was supported by the University of Wisconsin - Milwaukee Research Growth Initiative program, the University of Wisconsin - Milwaukee Center for Latin American and Caribbean Studies, NSF DEB-0613666, NSF DEB-0845071 to SAS, DEB-9527729 and DEB-0212054 to WPC, and an Andrew Mellon Foundation Research Awards in Tropical Biology to WPC and SAS. The Organization for Tropical Studies and the staff at La Selva Biological Station provided logistic support. NR 49 TC 33 Z9 35 U1 3 U2 48 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0006-3606 J9 BIOTROPICA JI Biotropica PD MAY PY 2013 VL 45 IS 3 BP 317 EP 324 DI 10.1111/btp.12015 PG 8 WC Ecology SC Environmental Sciences & Ecology GA 135UU UT WOS:000318314900007 ER PT J AU Young, H Griffin, RH Wood, CL Nunn, CL AF Young, Hillary Griffin, Randi H. Wood, Chelsea L. Nunn, Charles L. TI Does habitat disturbance increase infectious disease risk for primates? SO ECOLOGY LETTERS LA English DT Article DE Amplification effect; dilution effect; disease prevalence; disturbance; geographic range overlap; parasites; primates; species richness ID SPECIES-DIVERSITY; PARASITE DIVERSITY; BIODIVERSITY LOSS; HOST-SPECIFICITY; PUBLICATION BIAS; ONLINE RESOURCE; BETA REGRESSION; WILD PRIMATES; PATTERNS; PREVALENCE AB Many studies have suggested that ecosystem conservation protects human and wildlife populations against infectious disease. We tested this hypothesis using data on primates and their parasites. First, we tested for relationships between species' resilience to human disturbance and their parasite richness, prevalence and immune defences, but found no associations. We then conducted a meta-analysis of the effects of disturbance on parasite prevalence, which revealed no overall effect, but a positive effect for one of four types of parasites (indirectly transmitted parasites). Finally, we conducted intraspecific analyses of malaria prevalence as a function of mammalian species richness in chimpanzees and gorillas, and an interspecific analysis of geographic overlap and parasite species richness, finding that higher levels of host richness favoured greater parasite risk. These results suggest that anthropogenic effects on disease transmission are complex, and highlight the need to define the conditions under which environmental change will increase or decrease disease transmission. C1 [Young, Hillary] Harvard Univ, Ctr Environm, Cambridge, MA 02138 USA. [Young, Hillary] Smithsonian Inst, Div Mammals, Washington, DC 20013 USA. [Griffin, Randi H.; Nunn, Charles L.] Harvard Univ, Dept Human Evolutionary Biol, Cambridge, MA 02138 USA. [Wood, Chelsea L.] Stanford Univ, Dept Biol, Stanford, CA 94305 USA. RP Young, H (reprint author), Harvard Univ, Ctr Environm, Cambridge, MA 02138 USA. EM hyoung@fas.harvard.edu NR 51 TC 31 Z9 32 U1 7 U2 164 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1461-023X EI 1461-0248 J9 ECOL LETT JI Ecol. Lett. PD MAY PY 2013 VL 16 IS 5 BP 656 EP 663 DI 10.1111/ele.12094 PG 8 WC Ecology SC Environmental Sciences & Ecology GA 132OA UT WOS:000318077200011 PM 23448139 ER PT J AU Harrison, RD Tan, S Plotkin, JB Slik, F Detto, M Brenes, T Itoh, A Davies, SJ AF Harrison, Rhett D. Tan, Sylvester Plotkin, Joshua B. Slik, Ferry Detto, Matteo Brenes, Tania Itoh, Akira Davies, Stuart J. TI Consequences of defaunation for a tropical tree community SO ECOLOGY LETTERS LA English DT Article DE Biodiversity; bushmeat; conservation; defaunation; hunting; national park; rainforest; seed dispersal; spatial pattern; tropical ID SEED DISPERSAL; EMPTY FOREST; RAIN-FOREST; NEOTROPICAL TREE; BUSHMEAT; RECRUITMENT; GROWTH; VERTEBRATES; PREDATION; REMOVAL AB Hunting affects a considerably greater area of the tropical forest biome than deforestation and logging combined. Often even large remote protected areas are depleted of a substantial proportion of their vertebrate fauna. However, understanding of the long-term ecological consequences of defaunation in tropical forests remains poor. Using tree census data from a large-scale plot monitored over a 15-year period since the approximate onset of intense hunting, we provide a comprehensive assessment of the immediate consequences of defaunation for a tropical tree community. Our data strongly suggest that over-hunting has engendered pervasive changes in tree population spatial structure and dynamics, leading to a consistent decline in local tree diversity over time. However, we do not find any support for suggestions that over-hunting reduces above-ground biomass or biomass accumulation rate in this forest. To maintain critical ecosystem processes in tropical forests increased efforts are required to protect and restore wildlife populations. C1 [Harrison, Rhett D.] Chinese Acad Sci, Key Lab Biodivers & Biogeog, Kunming Inst Bot, Kunming 650201, Yunnan, Peoples R China. [Harrison, Rhett D.] World Agroforestry Ctr, East Asia Off, Kunming 650201, Yunnan, Peoples R China. [Tan, Sylvester] Ctr Trop Forest Sci, Miri, Sarawak, Malaysia. [Plotkin, Joshua B.] Univ Penn, Dept Biol, Lynch Labs 219, Philadelphia, PA 19104 USA. [Slik, Ferry] Chinese Acad Sci, Ctr Integrat Conservat, Xishuangbanna Trop Bot Garden, Mengla 666303, Yunnan, Peoples R China. [Detto, Matteo; Brenes, Tania] Smithsonian Trop Res Inst, Smithsonian Inst Global Earth Observ, Ctr Trop Forest Sci, Balboa, Panama. [Itoh, Akira] Osaka City Univ, Osaka 5588585, Japan. [Davies, Stuart J.] Smithsonian Trop Res Inst, Ctr Trop Forest Sci, Smithsonian Inst Global Earth Observ, Washington, DC 20012 USA. RP Harrison, RD (reprint author), Chinese Acad Sci, Key Lab Biodivers & Biogeog, Kunming Inst Bot, Kunming 650201, Yunnan, Peoples R China. EM rhett_d_harrison@yahoo.co.uk RI Plotkin, Joshua/E-6947-2013 NR 49 TC 54 Z9 61 U1 11 U2 160 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1461-023X EI 1461-0248 J9 ECOL LETT JI Ecol. Lett. PD MAY PY 2013 VL 16 IS 5 BP 687 EP 694 DI 10.1111/ele.12102 PG 8 WC Ecology SC Environmental Sciences & Ecology GA 132OA UT WOS:000318077200015 PM 23489437 ER PT J AU Keller, JK Sutton-Grier, AE Bullock, AL Megonigal, JP AF Keller, Jason K. Sutton-Grier, Ariana E. Bullock, Allyson L. Megonigal, J. Patrick TI Anaerobic Metabolism in Tidal Freshwater Wetlands: I. Plant Removal Effects on Iron Reduction and Methanogenesis SO ESTUARIES AND COASTS LA English DT Article DE Anaerobic microbial metabolism; Iron reduction; Jug Bay Wetlands Sanctuary, Maryland, USA; Methane; Plant removal; Tidal freshwater wetland ID FE(III) OXIDE REDUCTION; METHANE PRODUCTION; FERRIC IRON; SEDIMENTS; MARSHES; RHIZOSPHERE; EMISSIONS; OXIDATION; MACROPHYTES; KINETICS AB For energetic reasons, iron reduction suppresses methanogenesis in tidal freshwater wetlands; however, when iron reduction is limited by iron oxide availability, methanogenesis dominates anaerobic carbon mineralization. Plants can mediate this microbial competition by releasing oxygen into the rhizosphere and supplying oxidized iron for iron reducers. We utilized a plant removal experiment in two wetland sites to test the hypothesis that, in the absence of plants, rates of iron reduction would be diminished, allowing methanogenesis to dominate anaerobic metabolism. In both sites, methanogenesis was the primary anaerobic mineralization pathway, with iron reduction dominating only early and late in the growing season in the site with a less organic soil. These patterns were not influenced by the presence of plants, demonstrating that plants were not a key control of microbial metabolism. Instead, we suggest that site conditions, including soil chemistry, and temperature are important controls of the pathways of anaerobic metabolism. C1 [Keller, Jason K.] Chapman Univ, Sch Earth & Environm Sci, Orange, CA 92782 USA. [Keller, Jason K.; Sutton-Grier, Ariana E.; Bullock, Allyson L.; Megonigal, J. Patrick] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. RP Keller, JK (reprint author), Smithsonian Environm Res Ctr, POB 28, Edgewater, MD 21037 USA. EM jkeller@chapman.edu OI Sutton-Grier, Ariana/0000-0002-1242-7728 FU NSF [DEB-0516400]; Smithsonian Post-Doctoral Fellowships FX Chris Swarth at the Jug Bay Wetlands Sanctuary allowed unfettered access to our research sites for this project. We thank Jim Duls, Nick Mudd, Lucinda Williams, Pamela Weisenhorn, Sara McQueeney, Kyle Chambers, and Eric Pfoutz for assistance with field and laboratory work on this project. Comments from two anonymous reviewers greatly improved this manuscript. This research was supported by NSF DEB-0516400 to JPM and Smithsonian Post-Doctoral Fellowships to JKK and AES-G. NR 36 TC 5 Z9 6 U1 3 U2 55 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 1559-2723 J9 ESTUAR COAST JI Estuaries Coasts PD MAY PY 2013 VL 36 IS 3 BP 457 EP 470 DI 10.1007/s12237-012-9527-6 PG 14 WC Environmental Sciences; Marine & Freshwater Biology SC Environmental Sciences & Ecology; Marine & Freshwater Biology GA 135NP UT WOS:000318295300002 ER PT J AU Emerson, D Bellows, W Keller, JK Moyer, CL Sutton-Grier, A Megonigal, JP AF Emerson, David Bellows, Wendy Keller, Jason K. Moyer, Craig L. Sutton-Grier, Ariana Megonigal, J. Patrick TI Anaerobic Metabolism in Tidal Freshwater Wetlands: II. Effects of Plant Removal on Archaeal Microbial Communities SO ESTUARIES AND COASTS LA English DT Article DE Anaerobic microbial metabolism; Methane; Methanogen; Thaumarchaeota; Euryarchaeota; Tidal freshwater wetland ID MANIPULATED ENVIRONMENTAL VARIABILITY; 16S RIBOSOMAL-RNA; METHANE PRODUCTION; HYDROGENOTROPHIC METHANOGEN; MINEROTROPHIC FEN; NICHE SEPARATION; SEQUENCE DATA; SALT-MARSH; REDUCTION; OXIDATION AB The interaction of plant and microbial communities are known to influence the dynamics of methane emission in wetlands. Plant manipulations were conducted in an organic rich (JB-organic) and a mineral rich (JB-mineral) site in a tidal freshwater wetland to determine if plant removal impacted archaeal populations. In concert, a suite of process-based measurements also determined the effects of plant removal on rates of methanogenesis and Fe-reduction. The microbial populations were analyzed with clone libraries of the SSU ribosomal RNA (rRNA) gene from selected plots, and terminal restriction length polymorphism (tRFLP) of the SSU rRNA and the methyl-coenzyme M reductase (mcrA) gene. Overall, methanogenesis dominated anaerobic carbon mineralization at both sites during the most active growing season. A total of 114 SSU rRNA clones from four different plots revealed a diversity of Euryarchaeota including representatives of the Methanomicrobiales, Methanosarcinales and Thermoplasmatales. The clone libraries were dominated by the Thaumarchaeota, accounting for 65 % of clones, although their diversity was low. A total of 112 tRFLP profiles were generated from 56 samples from 25 subplots; the patterns for both SSU rRNA and mcrA showed little variation between sites, either with plant treatment or with the growing season. Overall these results suggest that wetland soil archaeal populations were resilient to changes in the associated surface plant communities. The work also revealed the presence of novel, mesophilic Thaumarchaeota of unknown metabolic function. C1 [Emerson, David; Bellows, Wendy] Bigelow Lab Ocean Sci, East Boothbay, ME USA. [Keller, Jason K.] Chapman Univ, Orange, CA USA. [Moyer, Craig L.] Western Washington Univ, Bellingham, WA 98225 USA. [Sutton-Grier, Ariana; Megonigal, J. Patrick] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. RP Emerson, D (reprint author), Bigelow Lab Ocean Sci, POB 380, East Boothbay, ME USA. EM demerson@bigelow.org OI Sutton-Grier, Ariana/0000-0002-1242-7728 FU NSF [0516400]; Smithsonian Post-Doctoral Fellowships FX We are indebted to Dr. Emily Fleming and Dr. Joyce McBeth for assistance and advice in developing phylogenetic trees. Chris Swarth at the Jug Bay Wetlands Sanctuary allowed unfettered access to our research sites for this project and provided important background references about the Jug Bay ecosystem. We thank Jim Duls, Nicholas Mudd, and Todd Plaia for assistance with field component of this work and laboratory work on this project. The editorial comments of Chris Swarth and Aat Barendregt, as well as two anonymous reviewers, are greatly appreciated. This research was supported by collaborative NSF grant 0516400 to JPM and DE and Smithsonian Post-Doctoral Fellowships to JKK and AESG. NR 39 TC 4 Z9 6 U1 2 U2 42 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 1559-2723 J9 ESTUAR COAST JI Estuaries Coasts PD MAY PY 2013 VL 36 IS 3 BP 471 EP 481 DI 10.1007/s12237-012-9496-9 PG 11 WC Environmental Sciences; Marine & Freshwater Biology SC Environmental Sciences & Ecology; Marine & Freshwater Biology GA 135NP UT WOS:000318295300003 ER PT J AU Bullock, AL Sutton-Grier, AE Megonigal, JP AF Bullock, Allyson L. Sutton-Grier, Ariana E. Megonigal, J. Patrick TI Anaerobic Metabolism in Tidal Freshwater Wetlands: III. Temperature Regulation of Iron Cycling SO ESTUARIES AND COASTS LA English DT Article DE Iron cycling; Iron oxidation; Iron reduction; Microbial respiration; Tidal freshwater wetland; Temperature response; Jug Bay Sanctuary ID ORGANIC-MATTER MINERALIZATION; FE(III) OXIDE REDUCTION; SALT-MARSH SEDIMENTS; FERRIC IRON; METHANE PRODUCTION; CARBON OXIDATION; OXIDIZING BACTERIA; SULFATE-REDUCTION; ROOT-ZONE; RHIZOSPHERE AB Understanding the ecological processes that regulate the production and fate of methane (CH4) in wetland soils is essential for forecasting wetland CH4 emissions. Iron reduction is an important carbon mineralization pathway that is capable of suppressing CH4 production in freshwater wetlands, but our understanding of temperature regulation of iron oxide respiration and the subsequent impacts on CH4 production is limited. We tested the hypothesis that temperature regulates iron reduction rates indirectly through differential effects on Fe(II) oxidation versus Fe(III) reduction, which ultimately determines the size of the microbially labile, poorly crystalline Fe(III) pool. Our study indicates that rates of iron reduction are more sensitive to changes in temperature than rates of iron oxidation, which creates imbalance in the relative proportion of Fe(II) and Fe(III) in the poorly crystalline soil iron pool as temperatures change. Our results suggest that warmer temperatures can cause the Fe(III) oxide pool to decline, limiting the Fe(III) supply to iron reducers and relieving competition for organic carbon with methanogens. C1 [Bullock, Allyson L.; Sutton-Grier, Ariana E.; Megonigal, J. Patrick] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. RP Megonigal, JP (reprint author), Smithsonian Environm Res Ctr, 647 Contees Wharf Rd, Edgewater, MD 21037 USA. EM megonigalp@si.edu OI Sutton-Grier, Ariana/0000-0002-1242-7728 FU NSF [DEB-0516400] FX We thank Jug Bay Wetlands Sanctuary for providing access to the study site; Cindy Gilmour, Wayne Coats, and Pat Neale for the use of the incubators and the SERC Science and Coffee Discussion Group for feedback on experimental design. Thanks to Andrew Graham for helping with figures and statistics and Jason Keller for comments and advice. This work was funded by NSF DEB-0516400 to JPM. NR 30 TC 6 Z9 6 U1 1 U2 54 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 1559-2723 J9 ESTUAR COAST JI Estuaries Coasts PD MAY PY 2013 VL 36 IS 3 BP 482 EP 490 DI 10.1007/s12237-012-9536-5 PG 9 WC Environmental Sciences; Marine & Freshwater Biology SC Environmental Sciences & Ecology; Marine & Freshwater Biology GA 135NP UT WOS:000318295300004 ER PT J AU Swarth, CW Delgado, P Whigham, DF AF Swarth, Christopher W. Delgado, Patricia Whigham, Dennis F. TI Vegetation Dynamics in a Tidal Freshwater Wetland: A Long-Term Study at Differing Scales SO ESTUARIES AND COASTS LA English DT Article DE Tidal freshwater wetlands; Plant communities; Succession; Annuals; Perennials; Patuxent River; Sea level rise ID UPPER CHESAPEAKE BAY; DELAWARE RIVER; PATUXENT RIVER; SEED-BANK; MARSH; USA; SEDIMENTATION; PATTERNS; ESTUARY; ACCUMULATION AB Tidal freshwater wetlands are complex, species-rich ecosystems located at the interface between tidal estuaries and nontidal rivers. This study conducted on the Patuxent River estuary in Maryland was designed to assess vegetation dynamics over several decades to determine if there were directional changes in the dominant communities. Aerial photographs (1970, 1989, and 2007) documented broad-scale spatial changes in major plant communities. The coverage of areas dominated by Nuphar lutea and Phragmites australis expanded; mixed vegetation and scrub-shrub habitats were essentially unchanged; and Typha and Zizania aquatica communities fluctuated in coverage. Data collected between 1988 and 2010 from permanent plots and transects were used to examine fine-scale changes. Shifts in the importance of some species through time were observed, but there were no directional changes in community species composition. The lack of directional change as measured at a fine scale is characteristic of tidal freshwater wetlands in which variations in the abundance of individual species, especially annuals, are responsible for most short-term change in species composition. Changes in the composition of plant communities are interpreted as responses to variations in vertical accretion, stability of habitat types, invasive plant species, and herbivores. In the future, vegetation changes are likely to occur as a result of the intrusion of brackish water and increased flooding associated with global climate change and sea level rise. This long-term study establishes a baseline from which potential future changes to tidal freshwater wetlands can be better understood. C1 [Swarth, Christopher W.] Jug Bay Wetlands Sanctuary, Lothian, MD 20711 USA. [Delgado, Patricia] Maryland Dept Nat Resources, Chesapeake Bay Natl Estuarine Res Reserve Marylan, Annapolis, MD 21401 USA. [Whigham, Dennis F.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. RP Swarth, CW (reprint author), Jug Bay Wetlands Sanctuary, 1361 Wrighton Rd, Lothian, MD 20711 USA. EM cswarth@jugbay.org OI Whigham, Dennis/0000-0003-1488-820X FU Anne Arundel County Department of Recreation and Parks; Friends of Jug Bay FX We thank Laura Perry, Jennifer D'Avanzo, Kathy Szlavecz, Christine Gault, Karyn Molines, Jeff Campbell, Cathy Ervin, Holly Budd, Rachel Dickey, Claudia Jones, John Schwartz, and Charlie Muise for their help with the fieldwork. Greg Kearns (Maryland National Capital Park and Planning Commission) helped interpret the aerial photographs and Becky Lang and Janice Henderson provided the digital cartography. Mary Leck and two anonymous reviewers provided helpful comments that improved the manuscript. Funding was provided by the Anne Arundel County Department of Recreation and Parks and the Friends of Jug Bay. NR 64 TC 4 Z9 5 U1 1 U2 63 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 1559-2723 J9 ESTUAR COAST JI Estuaries Coasts PD MAY PY 2013 VL 36 IS 3 BP 559 EP 574 DI 10.1007/s12237-012-9568-x PG 16 WC Environmental Sciences; Marine & Freshwater Biology SC Environmental Sciences & Ecology; Marine & Freshwater Biology GA 135NP UT WOS:000318295300010 ER PT J AU Clark, MA La Plante, PC Greenhill, LJ AF Clark, M. A. La Plante, P. C. Greenhill, L. J. TI Accelerating radio astronomy cross-correlation with graphics processing units SO INTERNATIONAL JOURNAL OF HIGH PERFORMANCE COMPUTING APPLICATIONS LA English DT Article DE radio astronomy; graphics processing units; signal processing; correlation ID PROTOTYPE AB We present a highly parallel implementation of the cross-correlation of time-series data using graphics processing units (GPUs), which is scalable to hundreds of independent inputs and suitable for the processing of signals from 'large-N' arrays of many radio antennas. The computational part of the algorithm, the X-engine, is implemented efficiently on NVIDIA's Fermi architecture, sustaining up to 79% of the peak single-precision floating-point throughput. We compare performance obtained for hardware- and software-managed caches, observing significantly better performance for the latter. The high performance reported involves use of a multi-level data tiling strategy in memory and use of a pipelined algorithm with simultaneous computation and transfer of data from host to device memory. The speed of code development, flexibility, and low cost of the GPU implementations compared with application-specific integrated circuit (ASIC) and field programmable gate array (FPGA) implementations have the potential to greatly shorten the cycle of correlator development and deployment, for cases where some power-consumption penalty can be tolerated. C1 [Clark, M. A.; Greenhill, L. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Clark, M. A.] NVIDIA Corp, Santa Clara, CA USA. [La Plante, P. C.] Loyola Univ Maryland, Baltimore, MD USA. RP Clark, MA (reprint author), NVIDIA Corp, 2701 San Tomas Expressway, Santa Clara, CA USA. EM mikec@seas.harvard.edu OI La Plante, Paul/0000-0002-4693-0102 FU National Science Foundation [PHY-0835713]; NVIDIA via Harvard CUDA Center of Excellence FX This work was supported in part by the National Science Foundation (grant number PHY-0835713).; We would like to thank NVIDIA for support via the Harvard CUDA Center of Excellence. We would like to thank D Mitchell, S Ord, and R Wayth for helpful discussions. We thank Kathryn Hollar and the Harvard SEAS REU program for enabling the research that contributed to this work. NR 23 TC 6 Z9 8 U1 0 U2 10 PU SAGE PUBLICATIONS LTD PI LONDON PA 1 OLIVERS YARD, 55 CITY ROAD, LONDON EC1Y 1SP, ENGLAND SN 1094-3420 J9 INT J HIGH PERFORM C JI Int. J. High Perform. Comput. Appl. PD MAY PY 2013 VL 27 IS 2 BP 178 EP 192 DI 10.1177/1094342012444794 PG 15 WC Computer Science, Hardware & Architecture; Computer Science, Interdisciplinary Applications; Computer Science, Theory & Methods SC Computer Science GA 136IW UT WOS:000318356600009 ER PT J AU Parenti, LR Ebach, MC AF Parenti, Lynne R. Ebach, Malte C. TI Evidence and hypothesis in biogeography SO JOURNAL OF BIOGEOGRAPHY LA English DT Editorial Material DE Biogeographical regions; co-evolution; dispersal; historical biogeography; Indo-Pacific; molecular clock; Sulawesi; vicariance; volcanoes ID FRESH-WATER; HISTORICAL BIOGEOGRAPHY; ANCESTRAL AREAS; ORIGIN CONCEPT; PHYLOGENY; DISPERSAL; EVOLUTION; ISLANDS; VICARIANCE; TELEOSTEI AB Evidence can provide support for or against a particular biogeographical hypothesis. Treating a hypothesis as if it were evidence or an empirical observation confounds many biogeographical analyses. We focus on two recent publications that address, in part, the evolution of the biota of Sulawesi, the large Indonesian island in the centre of the Indo-Australian Archipelago. Many biogeographical explanations are hampered by invoking simple notions of mechanism or process dispersal and vicariance or constraints, such as dispersal from a centre of origin, and, in so doing, dismiss more complex geological phenomena such as emergent volcanoes within island chains or composite areas as irrelevant. Moreover, they do not search for, therefore never discover, biogeographical patterns that may better explain the distribution of biota through time. C1 [Parenti, Lynne R.] Smithsonian Inst, Dept Vertebrate Zool, Natl Museum Nat Hist, Washington, DC 20013 USA. [Ebach, Malte C.] Univ New S Wales, Sch Biol Earth & Environm Sci, Sydney, NSW 2052, Australia. RP Parenti, LR (reprint author), Smithsonian Inst, Dept Vertebrate Zool, Natl Museum Nat Hist, POB 37012 MRC 159, Washington, DC 20013 USA. EM parentil@si.edu OI Ebach, Malte/0000-0002-9594-9010 NR 51 TC 10 Z9 11 U1 5 U2 46 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 MAY PY 2013 VL 40 IS 5 BP 813 EP 820 DI 10.1111/jbi.12069 PG 8 WC Ecology; Geography, Physical SC Environmental Sciences & Ecology; Physical Geography GA 131KX UT WOS:000317993000001 ER PT J AU Lisney, TJ Stecyk, K Kolominsky, J Schmidt, BK Corfield, JR Iwaniuk, AN Wylie, DR AF Lisney, Thomas J. Stecyk, Karyn Kolominsky, Jeffrey Schmidt, Brian K. Corfield, Jeremy R. Iwaniuk, Andrew N. Wylie, Douglas R. TI Ecomorphology of eye shape and retinal topography in waterfowl (Aves: Anseriformes: Anatidae) with different foraging modes SO JOURNAL OF COMPARATIVE PHYSIOLOGY A-NEUROETHOLOGY SENSORY NEURAL AND BEHAVIORAL PHYSIOLOGY LA English DT Article DE Duck; Feeding behavior; Retinal ganglion cell; Visual acuity; Visual streak ID GANGLION-CELL LAYER; OIL DROPLET DISTRIBUTION; DUCK ANAS-PLATYRHYNCHOS; SPATIAL VISUAL-ACUITY; DABBLING DUCKS; REGIONAL SPECIALIZATION; QUANTITATIVE-ANALYSIS; CANADA GEESE; PROCELLARIIFORM SEABIRDS; TYRANT FLYCATCHERS AB Despite the large body of literature on ecomorphological adaptations to foraging in waterfowl, little attention has been paid to their sensory systems, especially vision. Here, we compare eye shape and retinal topography across 12 species representing 4 different foraging modes. Eye shape was significantly different among foraging modes, with diving and pursuit-diving species having relatively smaller corneal diameters compared to non-diving species. This may be associated with differences in ambient light intensity while foraging or an ability to tightly constrict the pupil in divers in order to facilitate underwater vision. Retinal topography was similar across all species, consisting of an oblique visual streak, a central area of peak cell density, and no discernible fovea. Because the bill faces downwards when the head is held in the normal posture in waterfowl, the visual streak will be held horizontally, allowing the horizon to be sampled with higher visual acuity. Estimates of spatial resolving power were similar among species with only the Canada goose having a higher spatial resolution. Overall, we found no evidence of ecomorphological adaptations to different foraging modes in the retinal ganglion cell layer in waterfowl. Rather, retinal topography in these birds seems to reflect the 'openness' of their habitats. C1 [Lisney, Thomas J.; Stecyk, Karyn; Wylie, Douglas R.] Univ Alberta, Dept Psychol, Edmonton, AB, Canada. [Kolominsky, Jeffrey; Wylie, Douglas R.] Univ Alberta, Ctr Neurosci, Edmonton, AB, Canada. [Schmidt, Brian K.] Smithsonian Inst, Natl Museum Nat Hist, Div Birds, Washington, DC 20013 USA. [Corfield, Jeremy R.; Iwaniuk, Andrew N.] Univ Lethbridge, Dept Neurosci, Canadian Ctr Behav Neurosci, Lethbridge, AB T1K 3M4, Canada. RP Lisney, TJ (reprint author), Univ Alberta, Dept Psychol, Edmonton, AB, Canada. EM tomlisney@gmail.com FU Natural Sciences and Engineering Council of Canada (NSERC) FX All of our methods adhered to Canadian Council for Animal Care Guidelines and were approved by the University of Lethbridge Animal Welfare Committee. We wish to thank George Iwaniuk, Greg Sanbourn, Udo Hannebaum and the curatorial staff of the Division of Birds for providing specimens for this study. Gerald Romanchuk kindly allowed us to use his photograph of a redhead. Heather Lisney and Vincent and Angela Galipeau provided essential support during the preparation of the paper. Funding was provided by the Natural Sciences and Engineering Council of Canada (NSERC) Discovery Grants and Discovery Accelerator Supplements to ANI and DRW. NR 117 TC 15 Z9 16 U1 9 U2 52 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0340-7594 J9 J COMP PHYSIOL A JI J. Comp. Physiol. A -Neuroethol. Sens. Neural Behav. Physiol. PD MAY PY 2013 VL 199 IS 5 BP 385 EP 402 DI 10.1007/s00359-013-0802-1 PG 18 WC Behavioral Sciences; Neurosciences; Physiology; Zoology SC Behavioral Sciences; Neurosciences & Neurology; Physiology; Zoology GA 131JQ UT WOS:000317989600006 PM 23475299 ER PT J AU Andersen, KM Turner, BL AF Andersen, Kelly M. Turner, Benjamin L. TI Preferences or plasticity in nitrogen acquisition by understorey palms in a tropical montane forest SO JOURNAL OF ECOLOGY LA English DT Article DE ammonium; Arecaece; community assembly; ecophysiology; glycine; habitat filtering; niche partitioning; nitrate; Panama; plantsoil (below-ground) interactions ID N-15 NATURAL-ABUNDANCE; ORGANIC-NITROGEN; RAIN-FOREST; NUTRIENT LIMITATION; ISOTOPE COMPOSITION; SOIL MICROBES; ARCTIC TUNDRA; PLANTS; ARECACEAE; GROWTH AB Soil nitrogen (N) occurs in a range of chemical forms from simple inorganic compounds, such as nitrate (NO3 ) and ammonium (NH4 +), to organic compounds, such as amino acids. Plants differ in their capacity to use these various forms, which might influence the distribution of species across environmental nutrient gradients. We tested the hypothesis that the distribution of understorey palm species along a soil N gradient in a tropical montane forest in Panama is related to preferences for different chemical forms of N. We conducted a field experiment using 15N-labelled ammonium, nitrate and glycine to examine whether tropical plants show preferences for, or are flexible in, their use of chemical forms of soil N. All species used N from inorganic and organic sources and showed no preference for chemical forms of N. However, across all species, the overall N acquisition pattern was glycinenitrateammonium. Species from low-nutrient sites dominated by ammonium and organic N forms had inherently slow N uptake rates. Synthesis. Patterns in the distribution of understorey palms were related to nitrogen (N) uptake rates rather than preferences for N chemical forms. Down-regulation of N uptake rates may be an important adaptation for plant species associated with low-N soils, with plasticity in N acquisition patterns from various N sources important in alleviating competition for soil N. C1 [Andersen, Kelly M.; Turner, Benjamin L.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. RP Andersen, KM (reprint author), San Diego Zoo, Inst Conservat Res, Escondido, CA 92027 USA. EM kanderse@life.illinois.edu RI Turner, Benjamin/E-5940-2011 OI Turner, Benjamin/0000-0002-6585-0722 FU University of Illinois - Champaign/Urbana Programme in Ecology, Evolution, and Conservation Biology Summer Research Award; Govindjee and Rajni Govindjee Award; STRI Postdoctoral Fellowship FX We thank Jim Dalling, Gregory Goldsmith, Nelly Ramos, Didimo Urena, David Navarro and Leidys Rodriguez for their assistance with fieldwork and plant preparation and Dayana Agudo and Tania Romero for laboratory support. Funding was provided by the University of Illinois - Champaign/Urbana Programme in Ecology, Evolution, and Conservation Biology Summer Research Award and the Govindjee and Rajni Govindjee Award and STRI Postdoctoral Fellowship to KMA. The Smithsonian Tropical Research Institute and Enel Fortuna provided logistical support. Modified needles were provided by Jan Jansa and Fabienne Zeugin in the Plant Nutrition Group at ETH Zurich. Jim Dalling, Jordan Mayor and two anonymous reviewers provided helpful comments on previous versions of the manuscript. NR 46 TC 14 Z9 15 U1 3 U2 64 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0022-0477 J9 J ECOL JI J. Ecol. PD MAY PY 2013 VL 101 IS 3 BP 819 EP 825 DI 10.1111/1365-2745.12070 PG 7 WC Plant Sciences; Ecology SC Plant Sciences; Environmental Sciences & Ecology GA 134CH UT WOS:000318186800027 ER PT J AU Gomez-Mestre, I Warkentin, KM AF Gomez-Mestre, I. Warkentin, K. M. TI Risk-induced hatching timing shows low heritability and evolves independently of spontaneous hatching in red-eyed treefrogs SO JOURNAL OF EVOLUTIONARY BIOLOGY LA English DT Article DE Agalychnis; heritability; inducible defences; life-history evolution; limits of plasticity; quantitative genetics ID ADAPTIVE PHENOTYPIC PLASTICITY; QUANTITATIVE-GENETIC-ANALYSIS; PREDATION RISK; AGALYCHNIS-CALLIDRYAS; REACTION NORMS; TRADE-OFFS; EMBRYO BEHAVIOR; RANA-TEMPORARIA; EVOLUTION; EGGS AB Plasticity in the timing of transitions between stages of complex life cycles allows organisms to adjust their growth and development to local environmental conditions. Genetic variation in such plasticity is common, but the evolution of context-dependent transition timing may be constrained by information reliability, lag-time and developmental constraints. We studied the genetic architecture of hatching plasticity in embryos of the red-eyed treefrog (Agalychnis callidryas) in response to simulated predator attacks using a series of paternal and maternal half-sibs from a captive breeding colony of wild-collected animals. We compared the developmental timing of induced early hatching across sibships and estimated cross-environment genetic correlations between induced and spontaneous hatching traits. Additive genetic variance for induced early hatching was very low, indicating a constraint on the short-term evolution of earlier hatching timing. This constraint is likely related to the maturation of the hatching mechanism. The most plastic genotypes produced the most extreme spontaneous hatching phenotypes, indicating that developmental range, per se, is not constrained. Cross-environment genetic correlation in hatching timing was negligible, so the evolution of spontaneous hatching in this species has not depended on the evolution of risk-induced hatching and vice versa. C1 [Gomez-Mestre, I.; Warkentin, K. M.] Boston Univ, Dept Biol, Boston, MA 02215 USA. [Gomez-Mestre, I.] CSIC, Estn Biol Donana, Dept Wetland Ecol, E-41080 Seville, Spain. [Warkentin, K. M.] Smithsonian Trop Res Inst, Panama City, Panama. RP Gomez-Mestre, I (reprint author), Estn Biol Donana, Avda Amer Vespucio S-N, E-41092 Seville, Spain. EM igmestre@ebd.csic.es RI Gomez-Mestre, Ivan/F-8226-2014; CSIC, EBD Donana/C-4157-2011 OI Gomez-Mestre, Ivan/0000-0003-0094-8195; CSIC, EBD Donana/0000-0003-4318-6602 FU National Science Foundation [IBN-0234439]; National Geographic Society [7541-03]; Boston University FX We thank D. Fenolio for advice in setting up the frog colony, and J. Perry for assistance in building the rain chambers. We thank E. Collins, A. D'Amato, A. Gehrke, C. Hanlon, T. Iijima, S. Poo, J. Rogge and V. Saccoccio, for their help in frog care. We also thank two anonymous reviewers for their constructive comments. This study was funded by grants from National Science Foundation (IBN-0234439), National Geographic Society (7541-03) and Boston University. It was conducted under Boston University IACUC protocols #03-019 and 06-016. NR 69 TC 2 Z9 2 U1 0 U2 37 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1010-061X J9 J EVOLUTION BIOL JI J. Evol. Biol. PD MAY PY 2013 VL 26 IS 5 BP 1079 EP 1089 DI 10.1111/jeb.12121 PG 11 WC Ecology; Evolutionary Biology; Genetics & Heredity SC Environmental Sciences & Ecology; Evolutionary Biology; Genetics & Heredity GA 135MJ UT WOS:000318291900014 PM 23621370 ER PT J AU Castillo, RF Ubelaker, DH Acosta, JAL de la Rosa, RJE Garcia, IG AF Fernandez Castillo, Rafael Ubelaker, Douglas H. Lorente Acosta, Jose Antonio Esteban de la Rosa, Rafael Jose Garcia Garcia, Inmaculada TI Effect of Temperature on Bone Tissue: Histological Changes SO JOURNAL OF FORENSIC SCIENCES LA English DT Article DE forensic science; forensic anthropology; burned bones; cremains; thermal; histology ID ELECTRON-MICROSCOPE OBSERVATIONS; HUMAN REMAINS; IDENTIFICATION; PRESERVATION; FIRE AB The analysis of burned human remains has been of great interest among forensic anthropologists largely due to the difficulty that their recovery, classification, reconstruction, and identification present. The main purpose of this analysis is to present histological methodology for the interpretation of bones altered by thermal processes. We include analyses of the microscopic changes among bones exposed to different temperatures, with the goal of establishing categories of histological morphology in relation to fire temperature. Samples of bone (ilium) were exposed systematically to controlled temperatures. Analysis of the resulting histological changes has allowed the formation of a clear four-stage classification of the alterations observed. This classification should prove useful in assessing bone changes in relation to temperature of exposure, particularly in cases where this temperature was previously not known. C1 [Fernandez Castillo, Rafael] Univ Granada, Fac Med, Lab Anthropol, Granada 18012, Spain. [Ubelaker, Douglas H.] Natl Museum Nat Hist, Smithsonian Inst, Dept Anthropol, Washington, DC 20560 USA. [Lorente Acosta, Jose Antonio] Univ Granada, Fac Med, Dept Legal Med, Granada 18012, Spain. [Esteban de la Rosa, Rafael Jose] Acad Med Ctr Virgen de las Nieves, Granada 18014, Spain. [Garcia Garcia, Inmaculada] Univ Granada, Sch Hlth Sci, Granada 18012, Spain. RP Castillo, RF (reprint author), Univ Granada, Dept Anthropol, Fac Med, Avda Madrid S-N, E-18071 Granada, Spain. EM rafaelfernandez@ugr.es RI Castillo, Rafael/H-2178-2013; Garcia, Inmaculada/H-4450-2015; Esteban de la Rosa, Rafael Jose/A-9212-2016; OI Castillo, Rafael/0000-0002-1814-5254; Esteban de la Rosa, Rafael Jose/0000-0002-0558-0441; Garcia, Inmaculada Garcia/0000-0003-0500-7175 NR 27 TC 5 Z9 5 U1 2 U2 38 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0022-1198 EI 1556-4029 J9 J FORENSIC SCI JI J. Forensic Sci. PD MAY PY 2013 VL 58 IS 3 BP 578 EP 582 DI 10.1111/1556-4029.12093 PG 5 WC Medicine, Legal SC Legal Medicine GA 132DT UT WOS:000318048800002 ER PT J AU Liu, XL Wen, J Nie, ZL Johnson, G Liang, ZS Chang, ZY AF Liu, Xiao-Lin Wen, Jun Nie, Ze-Long Johnson, Gabriel Liang, Zong-Suo Chang, Zhao-Yang TI Polyphyly of the Padus group of Prunus (Rosaceae) and the evolution of biogeographic disjunctions between eastern Asia and eastern North America SO JOURNAL OF PLANT RESEARCH LA English DT Article DE Biogeography; Asian-North American disjunction; Padus; Phylogeny; Prunus; Rosaceae ID CHLOROPLAST DNA; EARLY EOCENE; PHYLOGENETIC INFERENCE; NUCLEOTIDE-SEQUENCES; WASHINGTON-STATE; FOSSIL WOODS; SYSTEMATICS; PRUNOCERASUS; TERTIARY; MODEL AB Prunus subgenus Padus is a group with a wide distribution in temperate eastern Asia and eastern North America with one species extending to Europe and one to Central America. Phylogenetic relationships of subgenus Padus were reconstructed using sequences of nuclear ribosomal ITS, and plastid ndhF gene, and rps16 intron and rpl16 intron. Prunus subgenus Padus is shown to be polyphyletic. Taxa of subgenus Padus and subgenus Laurocerasus are highly intermixed in both the ITS and the plastid trees. The results support two disjunctions between eastern North America and Eurasia within the Padus group. One disjunction is between Prunus virginiana of eastern North America and P. padus of Eurasia, estimated to have diverged at 2.99 (95 % HPD 0.59-6.15)-4.1 (95 % HPD 0.63-8.59) mya. The other disjunction is between P. serotina and its Asian relatives. The second disjunction may have occurred earlier than the former one, but the age estimate is difficult due to the unresolved phylogenetic position of the P. serotina complex. C1 [Liu, Xiao-Lin; Liang, Zong-Suo; Chang, Zhao-Yang] Northwest Agr & Forest Univ, Coll Life Sci, Yangling 712100, Shaanxi, Peoples R China. [Wen, Jun; Johnson, Gabriel] Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, Washington, DC 20013 USA. [Nie, Ze-Long] Chinese Acad Sci, Key Lab Plant Biodivers & Biogeog, Kunming Inst Bot, Kunming 650204, Yunnan, Peoples R China. RP Liang, ZS (reprint author), Northwest Agr & Forest Univ, Coll Life Sci, Yangling 712100, Shaanxi, Peoples R China. EM bingdch@163.com; WENJ@si.edu; liangzs@ms.iswc.ac.cn RI Nie, Ze-Long/N-8471-2015 OI Nie, Ze-Long/0000-0001-8065-3981 FU China Scholarship Council; National Science Foundation (NSF) [DEB 0515431]; Natural Science Foundation of China [30625004]; Smithsonian Endowment Program; National Natural Science Foundation of China [31129001]; Laboratory of Analytical Biology of the National Museum of Natural History, the Smithsonian Institution FX We thank John Clark, Tao Deng, Michael Dillon, Steve Ginzsbarg, Ruth Kiew, Sue Lutz, Ying Meng, Michael Nee, Elizabeth Widjaja, Tingshuang Yi, Tze Leung Yao, and Zhuo Zhou for assistance in obtaining samples and/or field assistance. The study was supported by the China Scholarship Council, the National Science Foundation (NSF Award number DEB 0515431), the Natural Science Foundation of China (Project no. 30625004 to J. Wen and T. Yi), the Smithsonian Endowment Program, the National Natural Science Foundation of China (Grant no. 31129001), and the Laboratory of Analytical Biology of the National Museum of Natural History, the Smithsonian Institution. Staff of the Arnold Arboretum of Harvard University kindly provided samples for the study. NR 72 TC 5 Z9 6 U1 3 U2 45 PU SPRINGER JAPAN KK PI TOKYO PA CHIYODA FIRST BLDG EAST, 3-8-1 NISHI-KANDA, CHIYODA-KU, TOKYO, 101-0065, JAPAN SN 0918-9440 J9 J PLANT RES JI J. Plant Res. PD MAY PY 2013 VL 126 IS 3 BP 351 EP 361 DI 10.1007/s10265-012-0535-1 PG 11 WC Plant Sciences SC Plant Sciences GA 133YY UT WOS:000318178000004 PM 23239308 ER PT J AU Agnarsson, I Gregoric, M Blackledge, TA Kuntner, M AF Agnarsson, Ingi Gregoric, Matjaz Blackledge, Todd A. Kuntner, Matjaz TI The phylogenetic placement of Psechridae within Entelegynae and the convergent origin of orb-like spider webs SO JOURNAL OF ZOOLOGICAL SYSTEMATICS AND EVOLUTIONARY RESEARCH LA English DT Article DE Fecenia; Psechrus; orb web; evolution; convergence ID WEAVING SPIDERS; MECHANICAL-PROPERTIES; BUILDING SPIDERS; CAPTURE THREADS; SINGLE ORIGIN; ARANEAE; EVOLUTION; SILK; BEHAVIOR; ECOLOGY AB Evolutionary convergence of phenotypic traits provides evidence for their functional success. The origin of the orb web was a critical event in the diversification of spiders that facilitated a spectacular radiation of approximately 12000 species and promoted the evolution of novel web types. How the orb web evolved from ancestral web types, and how many times orb-like architectures evolved in spiders, has been debated for a long time. The little known spider genus Fecenia (Psechridae) constructs a web that resembles the archetypical orb web, but morphological data suggest that Psechridae (Psechrus+Fecenia) does not belong in Orbiculariae, the true orb weavers', but to the retrolateral tibial apophysis (RTA) clade' consisting mostly of wandering spiders, but also including spiders building less regular webs. Yet, the data are sparse and no molecular phylogenetic study has estimated Fecenia's exact position in the tree of life. Adding new data to sequences pulled from GenBank, we reconstruct a phylogeny of Entelegynae and phylogenetically test the monophyly and placement of Psechridae, and in doing so, the alternative hypotheses of monophyletic origin of the orb web and the pseudo-orb versus their independent origins, a potentially spectacular case of behavioural convergence. We also discuss the implications of our results for Entelegynae systematics. Our results firmly place a monophyletic Psechridae within the RTA clade, phylogenetically distant from true orb weavers. The architectural similarities of the orb and the pseudo-orb are therefore clearly convergent, as also suggested by detailed comparisons of these two web types, as well as the spiders' web-building behaviours and ontogenetic development. The convergence of Fecenia webs with true orbs provides a remarkable opportunity to investigate how these complex sets of traits may have interacted during the evolution of the orb. C1 [Agnarsson, Ingi] Univ Vermont, Dept Biol, Burlington, VT 05405 USA. [Agnarsson, Ingi; Kuntner, Matjaz] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA. [Gregoric, Matjaz; Kuntner, Matjaz] Slovenian Acad Sci & Arts, Ctr Sci Res, Inst Biol, Ljubljana, Slovenia. [Blackledge, Todd A.] Univ Akron, Dept Biol, Akron, OH 44325 USA. [Blackledge, Todd A.] Univ Akron, Integrated Biosci Program, Akron, OH 44325 USA. [Kuntner, Matjaz] Hubei Univ, Coll Life Sci, Wuhan, Hubei, Peoples R China. RP Agnarsson, I (reprint author), Univ Vermont, Dept Biol, Burlington, VT 05405 USA. EM iagnarsson@gmail.com; matjaz.gregoric@gmail.com; blackledge@uakron.edu; kuntner@gmail.com FU Conservation International RAP programme; NSF [IOS-0745379, DEB-1050187-1050253]; Slovenian Research Agency [J1-2063] FX We thank two anonymous reviewers for valuable comments that improved the manuscript. D. Li and Singapore National Parks kindly helped with organizing field collections. S. Richards and the Conservation International RAP programme sponsored and organized fieldwork in Papua. Work was supported by NSF grants no. IOS-0745379 and DEB-1050187-1050253 and by the Slovenian Research Agency grant no. J1-2063. NR 58 TC 14 Z9 14 U1 1 U2 28 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0947-5745 J9 J ZOOL SYST EVOL RES JI J. Zool. Syst. Evol. Res. PD MAY PY 2013 VL 51 IS 2 BP 100 EP 106 DI 10.1111/jzs.12007 PG 7 WC Evolutionary Biology; Zoology SC Evolutionary Biology; Zoology GA 132CK UT WOS:000318045300002 ER PT J AU Kerekes, J Kaspari, M Stevenson, B Nilsson, RH Hartmann, M Amend, A Bruns, TD AF Kerekes, Jennifer Kaspari, Michael Stevenson, Bradley Nilsson, R. Henrik Hartmann, Martin Amend, Anthony Bruns, Thomas D. TI Nutrient enrichment increased species richness of leaf litter fungal assemblages in a tropical forest SO MOLECULAR ECOLOGY LA English DT Article DE diversity; fungi; leaf litter; LSU; macronutrients; micronutrients; rDNA ITS ID PHYLOGENETIC DIVERSITY; ECTOMYCORRHIZAL FUNGI; COMMUNITY ANALYSIS; SEQUENCING DATA; BOREAL FOREST; RAIN-FORESTS; NITROGEN; PHOSPHORUS; GROWTH; DECOMPOSITION AB Microbial communities play a major role in terrestrial ecosystem functioning, but the determinates of their diversity and functional interactions are not well known. In this study, we explored leaf litter fungal diversity in a diverse Panama lowland tropical forest in which a replicated factorial N, P, K and micronutrient fertilization experiment of 40x40 m plots had been ongoing for nine years. We extracted DNA from leaf litter samples and used fungal-specific amplification and a 454 pyrosequencing approach to sequence two loci, the nuclear ribosomal internal transcribed spacer (ITS) region and the nuclear ribosomal large subunit (LSU) D1 region. Using a 95% sequence similarity threshold for ITS1 spacer recovered a total of 2523 OTUs, and the number of unique ITS1 OTUs per 0.51.0g leaf litter sample ranged from 55 to 177. Ascomycota were the dominant phylum among the leaf litter fungi (71% of the OTUs), followed by Basidiomycota (26% of the OTUs). In contrast to our expectations based on temperate ecosystems, long-term addition of nutrients increased, rather than decreased, species richness relative to controls. Effect of individual nutrients was more subtle and seen primarily as changes in community compositions especially at lower taxonomic levels, rather than as significant changes in species richness. For example, plots receiving P tended to show a greater similarity in community composition compared to the other nutrient treatments, the +PK, +NK and +NPK plots appeared to be more dominated by the Nectriaceae than other treatments, and indicator species for particular nutrient combinations were identified. C1 [Kerekes, Jennifer; Bruns, Thomas D.] Univ Calif Berkeley, Dept Plant & Microbial Biol, Berkeley, CA 94720 USA. [Kaspari, Michael; Stevenson, Bradley] Univ Oklahoma, Dept Biol, Grad Program EEB, Norman, OK 73019 USA. [Kaspari, Michael] Smithsonian Trop Res Inst, Balboa, Panama. [Stevenson, Bradley] Univ Oklahoma, Dept Bot & Microbiol, Norman, OK 73019 USA. [Nilsson, R. Henrik] Univ Gothenburg, Dept Biol & Environm Sci, S-40530 Gothenburg, Sweden. [Hartmann, Martin] Swiss Fed Res Inst WSL, Birmensdorf, Switzerland. [Hartmann, Martin] Agroscope Reckenholz Tanikon Res Stn ART, Zurich, Switzerland. [Amend, Anthony] Univ Hawaii Manoa, Dept Bot, Honolulu, HI 96822 USA. RP Kerekes, J (reprint author), Univ Calif Berkeley, Dept Plant & Microbial Biol, Berkeley, CA 94720 USA. EM jenkerekes@gmail.com RI Stevenson, Bradley/A-2786-2011; Hartmann, Martin/M-9371-2016; OI Stevenson, Bradley/0000-0001-9432-9744; Hartmann, Martin/0000-0001-8069-5284; Kaspari, Michael/0000-0002-9717-5768; Nilsson, Henrik/0000-0002-8052-0107 FU NASA; American Philosophical Society; NSF DEB [0842038]; Swedish Research Council of Environment, Agricultural Sciences, and Spatial Planning (FORMAS) [215-2011-498] FX This work was supported by funding from NASA's Harriett G. Jenkins Pre-Doctoral Fellowship Program (JPFP), NASA's JPFP Mini Research Award and the American Philosophical Society's Lewis and Clark Fund for Exploration and Field Research to JK. We thank Nhu Nguyen and three anonymous reviewers for valuable editorial advice. MK fieldwork was supported by NSF DEB 0842038. RHN acknowledges financial support from the Swedish Research Council of Environment, Agricultural Sciences, and Spatial Planning (FORMAS, 215-2011-498). NR 73 TC 20 Z9 20 U1 3 U2 129 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0962-1083 EI 1365-294X J9 MOL ECOL JI Mol. Ecol. PD MAY PY 2013 VL 22 IS 10 BP 2827 EP 2838 DI 10.1111/mec.12259 PG 12 WC Biochemistry & Molecular Biology; Ecology; Evolutionary Biology SC Biochemistry & Molecular Biology; Environmental Sciences & Ecology; Evolutionary Biology GA 133ZS UT WOS:000318180000017 PM 23601077 ER PT J AU Becker, NI Tschapka, M Kalko, EKV Encarnacao, JA AF Becker, Nina I. Tschapka, Marco Kalko, Elisabeth K. V. Encarnacao, Jorge A. TI Balancing the Energy Budget in Free-Ranging Male Myotis daubentonii Bats SO PHYSIOLOGICAL AND BIOCHEMICAL ZOOLOGY LA English DT Article ID LONG-EARED BATS; BODY-TEMPERATURE; DAILY TORPOR; INSECTIVOROUS BATS; PLECOTUS-AURITUS; DIGESTIVE EFFICIENCY; HUNTING BEHAVIOR; SEASONAL-CHANGES; METABOLIC-RATE; ENERGETICS AB Mammals use five main, mutually nonexclusive mechanisms to balance energy budgets: torpor, metabolic compensation, change in activity patterns, change in ingested energy, and/or variability in digestive efficiency. Bats, as small and actively flying mammals, have a high mass-specific energy demand; therefore, balancing mechanisms should be pronounced in this group. We found that male Myotis daubentonii exhibited marked variation in the relative importance of these different mechanisms during their period of seasonal activity in response to extrinsic (ambient temperature, insect abundance) and intrinsic (reproduction, body condition) factors. Cold ambient temperatures in spring facilitated long and frequent daily torpor bouts, whereas in early summer, increased energy intake was the dominant factor in energy balancing. Intake was further increased in late summer, when insect abundance was highest, and daily torpor bouts were shorter and less frequent than in early summer. In autumn, males used metabolic compensation to reduce their resting metabolic rate in addition to daily torpor. Metabolic compensation might be one of the mechanisms that allow males to maintain high body temperature during the day while decreasing the need for foraging time at night, thus maximizing their opportunities to mate. C1 [Becker, Nina I.; Tschapka, Marco; Kalko, Elisabeth K. V.] Univ Ulm, Inst Expt Ecol, D-89069 Ulm, Germany. [Becker, Nina I.; Encarnacao, Jorge A.] Univ Giessen, Mammalian Ecol Grp, Dept Anim Ecol & Systemat, D-35390 Giessen, Germany. [Tschapka, Marco; Kalko, Elisabeth K. V.] Smithsonian Trop Res Inst, Balboa, Panama. RP Becker, NI (reprint author), Univ Ulm, Inst Expt Ecol, D-89069 Ulm, Germany. EM nina.becker@uni-ulm.de FU Landesgraduiertenforderung Baden-Wurttemberg FX We thank U. Kierdorf for helpful comments on the manuscript and the Mammalian Ecology Group and all students who helped in the fieldwork and contributed to data collection, especially M. Bohm, M. Krafft, M. S. Otto, A. Roswag, and R. Sauerbrei. The study was financially supported by a grant of the Landesgraduiertenforderung Baden-Wurttemberg to N.I.B. NR 65 TC 8 Z9 9 U1 0 U2 45 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 1522-2152 J9 PHYSIOL BIOCHEM ZOOL JI Physiol. Biochem. Zool. PD MAY-JUN PY 2013 VL 86 IS 3 BP 361 EP 369 DI 10.1086/670527 PG 9 WC Physiology; Zoology SC Physiology; Zoology GA 135EL UT WOS:000318270100008 PM 23629886 ER PT J AU Finn, B AF Finn, Bernard TI UNDERWATER CABLES SO PROCEEDINGS OF THE IEEE LA English DT Editorial Material C1 Smithsonian Inst, Washington, DC 20560 USA. RP Finn, B (reprint author), Smithsonian Inst, Washington, DC 20560 USA. NR 0 TC 0 Z9 0 U1 1 U2 1 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 0018-9219 J9 P IEEE JI Proc. IEEE PD MAY PY 2013 VL 101 IS 5 SI SI BP 1253 EP 1259 DI 10.1109/JPROC.2013.2252716 PG 7 WC Engineering, Electrical & Electronic SC Engineering GA 133SK UT WOS:000318159900013 ER PT J AU Thomas, DB Ksepka, DT AF Thomas, Daniel B. Ksepka, Daniel T. TI A history of shifting fortunes for African penguins SO ZOOLOGICAL JOURNAL OF THE LINNEAN SOCIETY LA English DT Article DE diversity; extinction; Langebaanweg; Sphenisciformes; Western Cape ID WESTERN CAPE PROVINCE; SOUTH-AFRICA; EARLY PLIOCENE; LATE TERTIARY; LANGEBAANWEG; SPHENISCIFORMES; AVES; RECORD; SITE; AGE AB Africa is home today to only a single breeding species of penguin, Spheniscus demersus (black-footed penguin), which is endangered with extinction. Spheniscus demersus has been the only breeding species of penguin to share African coastlines with humans over the last 400000 years. Interestingly, African penguin diversity was substantially higher before the evolution of archaic humans. The fossil record indicates that a diverse assemblage of penguin species inhabited the southern African coasts for much of the Neogene. Previous excavations have identified four distinct species in Early Pliocene coastal marine deposits. Here we extend this pattern of high diversity and report the oldest record of penguins from Africa. Seventeen penguin specimens were identified from the Saldanha Steel locality, revealing the presence of at least four distinct species in South Africa during the Miocene. The largest of these species reached the size of the extant Aptenodytes patagonicus (king penguin), whereas the smallest was approximately the size of the smallest extant penguin Eudyptula minor (little blue penguin). Recovery of Miocene penguin remains is in accordance with earlier predictions of multiple pre-Pliocene colonizations of Africa and supports a higher level of ecological diversity amongst African penguins in the past.(c) 2013 The Linnean Society of London C1 [Thomas, Daniel B.] Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Washington, DC 20013 USA. [Ksepka, Daniel T.] N Carolina State Univ, Dept Marine Earth & Atmospher Sci, Raleigh, NC 27695 USA. [Ksepka, Daniel T.] North Carolina Museum Nat Sci, Dept Paleontol, Raleigh, NC 27601 USA. RP Thomas, DB (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Washington, DC 20013 USA. EM thomasd@si.edu FU NSF [DEB: 0949899] FX We thank P. Haarhoff, K. Van Willingh, and R. Govender for arranging access to the specimens, and D. Roberts for providing the Saldanha Steel borehole log. Comments by two anonymous reviewers improved the quality of this manuscript. Research was supported by NSF award DEB: 0949899. NR 65 TC 2 Z9 2 U1 7 U2 31 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0024-4082 J9 ZOOL J LINN SOC-LOND JI Zool. J. Linn. Soc. PD MAY PY 2013 VL 168 IS 1 BP 207 EP 219 DI 10.1111/zoj.12024 PG 13 WC Zoology SC Zoology GA 134RE UT WOS:000318231100007 ER PT J AU Hinde, K Foster, AB Landis, LM Rendina, D Oftedal, OT Power, ML AF Hinde, Katie Foster, Alison B. Landis, Lauren M. Rendina, Danielle Oftedal, Olav T. Power, Michael L. TI Brief Communication: Daughter Dearest: Sex-Biased Calcium in Mother's Milk Among Rhesus Macaques SO AMERICAN JOURNAL OF PHYSICAL ANTHROPOLOGY LA English DT Article DE maternal investment; infant skeletal development; lactation; life history; nutrition ID BONE-MINERAL CONTENT; LIFE-HISTORY; SIZE DIMORPHISM; HIGH PHOSPHORUS; MACACA-MULATTA; NATURAL-SELECTION; GAMBIAN MOTHERS; TRACE-ELEMENTS; CAYO-SANTIAGO; LACTATION AB Mother's milk provides building blocks necessary for infant development and growth postnatally. Minerals in milk are particularly important for infant skeletal development and may reflect maternal characteristics that are associated with the capacity to synthesize milk and sex-specific developmental priorities of the infant. Using a large sample of mother-infant dyads assigned to the outdoor breeding colony at the California National Primate Research Center (N=104), we investigated the relationship of milk calcium (Ca) and phosphorus (P) concentrations and the ratio of Ca/P to maternal and infant characteristics and to other milk variables. Ca and P are largely associated with casein micelles, and as expected, both Ca and P were positively correlated with protein concentrations in milk. Neither Ca nor P concentrations were associated with maternal parity. Mothers rearing daughters tended to produce higher mean Ca concentration in milk, and consequently a higher Ca/P ratio, than did mothers rearing sons, even though protein concentration was not elevated. These results suggest that the Ca/P ratio in rhesus milk may have been under separate selective pressure from protein content to facilitate the accelerated rate of skeletal calcification that has been observed in female Macaca mulatta infants. Am J Phys Anthropol 151:144-150, 2013. (C) 2013 Wiley Periodicals, Inc. C1 [Hinde, Katie] Harvard Univ, Dept Human Evolutionary Biol, Cambridge, MA 02138 USA. [Hinde, Katie; Foster, Alison B.; Landis, Lauren M.] Univ Calif Davis, Calif Natl Primate Res Ctr, Brain Mind & Behav Unit, Davis, CA USA. [Hinde, Katie; Power, Michael L.] Smithsonian Natl Zool Pk, Nutr Lab, Washington, DC USA. [Rendina, Danielle] Univ Chicago, Div Social Sci, Chicago, IL 60637 USA. [Oftedal, Olav T.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. [Power, Michael L.] Amer Coll Obstetricians & Gynecologists, Washington, DC USA. RP Hinde, K (reprint author), Harvard Univ, Dept Human Evolutionary Biol, 11 Divin Ave, Cambridge, MA 02138 USA. EM khinde@fas.harvard.edu OI Hinde, Katie/0000-0002-0528-866X FU NSF [BCS-0921978, BCS-0525025]; NIH [R24RRRR019970, P51RRRR000169 (CNPRC)] FX Grant sponsor: NSF; Grant number: BCS-0921978 and BCS-0525025 (to KH); Grant sponsor: NIH; Grant number: R24RRRR019970 (J.P. Capitanio); P51RRRR000169 (CNPRC). NR 68 TC 10 Z9 10 U1 0 U2 22 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0002-9483 J9 AM J PHYS ANTHROPOL JI Am. J. Phys. Anthropol. PD MAY PY 2013 VL 151 IS 1 BP 144 EP 150 DI 10.1002/ajpa.22229 PG 7 WC Anthropology; Evolutionary Biology SC Anthropology; Evolutionary Biology GA 132AN UT WOS:000318040200014 PM 23446791 ER PT J AU Li, D Kauffmann, J Zhang, Q Chen, W AF Li, D. Kauffmann, J. Zhang, Q. Chen, W. TI MASSIVE QUIESCENT CORES IN ORION: DYNAMICAL STATE REVEALED BY HIGH-RESOLUTION AMMONIA MAPS SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE instrumentation: interferometers; ISM: clouds; ISM: individual objects (Orion); stars: formation Online-only material: color figures ID MOLECULAR CLOUDS; DENSE CORES; DARK CLOUDS; PROTOSTELLAR CORES; INITIAL CONDITIONS; KINEMATICS; OUTFLOWS; CLUSTERS; SHAPES; STARS AB We present combined Very Large Array and Green Bank Telescope images of NH3 inversion transitions (1, 1) and (2, 2) toward OMC2 and OMC3. We focus on the relatively quiescent Orion cores, which are away from the Trapezium cluster and have no sign of massive protostars or evolved star formation. The 5 '' angular resolution and 0.6kms(-1) velocity resolution enable us to study the thermal and dynamic state of these cores at similar to 0.02 pc scales, comparable to or smaller than those of the current dust continuum surveys. We measure temperatures for a total of 30 cores, with average masses of 11 M-circle dot, radii of 0.039 pc, virial mass ratio (R-vir) over bar = 3.9, and critical mass ratio (R-C) over bar = 1.5. Twelve sources contain Spitzer protostars. The thus defined starless and protostellar subsamples have similar temperature, line width, but different masses, with an average of 7.3 M-circle dot for the former and 16 M-circle dot for the latter. Compared to other Gould Belt dense cores, more Orion cores have a high gravitational-to-kinetic energy ratio and more cores have a larger than unity critical mass ratio. Orion dense cores have velocity dispersions similar to those of cores in low-mass star-forming regions but larger masses for given size. Some cores appear to have truly supercritical gravitational-to-kinetic energy ratios, even when considering significant observational uncertainties: thermal and non-thermal gas motions alone cannot prevent collapse. C1 [Li, D.] Chinese Acad Sci, Natl Astron Observ, Beijing, Peoples R China. [Li, D.] Space Sci Inst, Boulder, CO USA. [Li, D.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. [Kauffmann, J.] CALTECH, Dept Astron, Pasadena, CA 91125 USA. [Zhang, Q.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Chen, W.] Peking Univ, Beijing 100871, Peoples R China. RP Li, D (reprint author), Chinese Acad Sci, Natl Astron Observ, Chaoyang Dist Datun Rd A20, Beijing, Peoples R China. EM ithaca.li@gmail.com OI Zhang, Qizhou/0000-0003-2384-6589 NR 37 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 MAY 1 PY 2013 VL 768 IS 1 AR L5 DI 10.1088/2041-8205/768/1/L5 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 130KD UT WOS:000317912900005 ER PT J AU Schreeg, LA Mack, MC Turner, BL AF Schreeg, Laura A. Mack, Michelle C. Turner, Benjamin L. TI Leaf litter inputs decrease phosphate sorption in a strongly weathered tropical soil over two time scales SO BIOGEOCHEMISTRY LA English DT Article DE Phosphorus; Tropical forest; Nutrient cycling; Dissolved organic carbon; Soil organic matter ID DISSOLVED ORGANIC-CARBON; DECIDUOUS FOREST FLOOR; PHOSPHORUS ADSORPTION; VARIABLE-CHARGE; IONIC-STRENGTH; COMPETITIVE ADSORPTION; MICROBIAL BIOMASS; HUMIC SUBSTANCES; MATTER; KAOLINITE AB In strongly weathered soils, leaf litter not only returns phosphorus (P) to the soil environment, it may also modify soil properties and soil solution chemistry, with the potential to decrease phosphate sorption and increase plant available P. Using a radioactive phosphate tracer (P-32) and 1 h laboratory incubations we investigated the effect of litter inputs on phosphate sorption over two time scales: (1) long-term field litter manipulations (litter addition, control and litter removal) and (2) pulses of litter leachate (i.e. water extracts of leaf litter) from five species. Leachate pulse effects were compared to a simulated throughfall, which served as a control solution. Soil receiving long-term doubling of leaf litter maintained five-fold more phosphate in solution than the litter removal soil. In addition to the quantity of phosphate sorbed, the field litter addition treatment decreased the strength of phosphate sorption, as evaluated through extraction of sorbed P-32 using a weakly acidic ammonium fluoride solution (Bray 1). In litter removal soil, leachate pulses significantly reduced phosphate sorption in comparison to the throughfall control for all five species evaluated. However, the ability of leachate pulses to reduce phosphate sorption decreased when soil had received field litter inputs. Across soils the effect of leachate pulses on phosphate sorption increased with net sorption of dissolved organic C, with the exception of leachate from one species that had a higher index of aromatic C concentration. These results demonstrate that litter inputs, as both long-term inputs and short-term leachate pulses, can decrease the quantity and strength of phosphate sorption, which may increase the biological availability of this key nutrient. C1 [Schreeg, Laura A.; Mack, Michelle C.] Univ Florida, Dept Biol, Gainesville, FL USA. [Schreeg, Laura A.] Univ Florida, Sch Nat Resources & Environm, Gainesville, FL USA. [Schreeg, Laura A.; Turner, Benjamin L.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. RP Schreeg, LA (reprint author), Brown Univ, Dept Ecol & Evolutionary Biol, 80 Waterman St,Box G-W, Providence, RI 02912 USA. EM Laura_Schreeg@brown.edu RI Turner, Benjamin/E-5940-2011 OI Turner, Benjamin/0000-0002-6585-0722 FU ANAM; Panamanian Ministry of Health; University of Florida; STRI; NSF [0909734] FX We thank Mirna Fernandez and Noelle Beckman for help on the canopy crane, Tania Romero for help in the laboratory, and Emma Sayer and Ed Tanner for support in the field and access to plots. Ben Bolker, Andrew Hein, Ted Schuur, Nick Comerford, Jan Jansa and Fabienne Zeugin provided helpful conversations, advice and/or logistical support. We also than ANAM and the Panamanian Ministry of Health for support. LAS was funded by an Alumni Fellowship from the University of Florida and a STRI short-term fellowship. The research was supported by a NSF Doctoral Dissertation Improvement Grant (#0909734; awarded to MCM, BLT and LAS). NR 95 TC 13 Z9 13 U1 1 U2 71 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0168-2563 J9 BIOGEOCHEMISTRY JI Biogeochemistry PD MAY PY 2013 VL 113 IS 1-3 BP 507 EP 524 DI 10.1007/s10533-012-9781-5 PG 18 WC Environmental Sciences; Geosciences, Multidisciplinary SC Environmental Sciences & Ecology; Geology GA 129ST UT WOS:000317863300031 ER PT J AU Tierney, SM Fischer, CN Rehan, SM Kapheim, KM Wcislo, WT AF Tierney, S. M. Fischer, C. N. Rehan, S. M. Kapheim, K. M. Wcislo, W. T. TI Frequency of social nesting in the sweat bee Megalopta genalis (Halictidae) does not vary across a rainfall gradient, despite disparity in brood production and body size SO INSECTES SOCIAUX LA English DT Article DE Social evolution; Seasonality; Rainfall gradient; Eusocial behaviour; Augochlorini ID PRIMITIVELY EUSOCIAL BEE; RUBICUNDUS HYMENOPTERA; LIGATUS HYMENOPTERA; TROPICAL FOREST; ECUADORIA HYMENOPTERA; SOLITARY BEHAVIOR; DRY SEASON; EVOLUTION; PATTERNS; BIOLOGY AB Local environmental conditions can facilitate or preclude the development of eusocial colonies in insects that facultatively express behavioural-caste polyphenism. To explore how environmental variability relates to the expression of social behaviour, we collected 120 nests of the facultatively social sweat bee, Megalopta genalis (Halictidae: Augochlorini), along a nearly twofold rainfall gradient in central Panama. Brood rearing activity of bees in seasonal neotropical forests should track flowering phenologies, which are typically set by rainfall and phylogenetic patterns. Nests were collected at roughly similar times of year from three sites comprising wet, moist and dry lowland tropical forests. There were significant differences in ovarian development, brood production and body size across sites for some comparisons, but no effect on the proportion of social colonies collected at each site. Results show that phenotypes of M. genalis relevant to social behaviour (ovarian development, brood production, body size) may be responsive to variation in local environment over distances of < 20 km. C1 [Tierney, S. M.; Fischer, C. N.; Rehan, S. M.; Kapheim, K. M.; Wcislo, W. T.] Smithsonian Trop Res Inst, Panama City 084303092, Panama. [Tierney, S. M.] Flinders Univ S Australia, Sch Biol Sci, Adelaide, SA 5001, Australia. [Fischer, C. N.] Yale Univ, Dept Mol Cellular & Dev Biol, New Haven, CT 06511 USA. [Rehan, S. M.] Univ Penn, Dept Biol Sci, Philadelphia, PA 19104 USA. [Kapheim, K. M.] Univ Illinois, Dept Entomol, Urbana, IL 61801 USA. [Kapheim, K. M.] Univ Illinois, Inst Genom Biol, Urbana, IL 61801 USA. RP Tierney, SM (reprint author), Smithsonian Trop Res Inst, Panama City 084303092, Panama. EM simon.tierney@flinders.edu.au; wcislow@si.edu RI Tierney, Simon/H-2410-2015; OI Tierney, Simon/0000-0002-8812-6753; Fischer, Caleb/0000-0003-4223-8511 FU STRI Earl S. Tupper Postdoctoral Fellowship; SI Restricted Endowment Grant; STRI-Butler University Internship; STRI Short Term Fellowship FX We thank P. Galgani and Smithsonian Tropical Research Institute (STRI) support staff for logistical help, O. Acevedo, D. Roubik, staff of the Sierra Llorona Lodge and the administration of the Parque Natural Metropolitano facilitated access to field sites. We gratefully acknowledge R. Condit for the use of STRI's long-term database and S. Dennis for advice on R. The manuscript was further improved by suggestions from M. Schwarz, B. Turner, M. J. West-Eberhard and two anonymous reviewers. Research was supported by STRI Earl S. Tupper Postdoctoral Fellowship to SMT; a SI Restricted Endowment Grant to WTW, SMT and KMK; a STRI-Butler University Internship to CNF; a STRI Short Term Fellowship to SMR. We are grateful to the Autoridad National del Medioambiente of the Republic of Panama for research permit no. SEX/A-34-09. NR 55 TC 4 Z9 4 U1 1 U2 29 PU SPRINGER BASEL AG PI BASEL PA PICASSOPLATZ 4, BASEL, 4052, SWITZERLAND SN 0020-1812 J9 INSECT SOC JI Insect. Soc. PD MAY PY 2013 VL 60 IS 2 BP 163 EP 172 DI 10.1007/s00040-012-0280-4 PG 10 WC Entomology SC Entomology GA 127IM UT WOS:000317691900005 ER PT J AU Hong, T AF Hong, Terry TI The Goddess Chronicle. SO LIBRARY JOURNAL LA English DT Book Review C1 [Hong, Terry] Smithsonian BookDragon, Washington, DC USA. RP Hong, T (reprint author), Smithsonian BookDragon, Washington, DC USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU REED BUSINESS INFORMATION PI NEW YORK PA 360 PARK AVENUE SOUTH, NEW YORK, NY 10010 USA SN 0363-0277 J9 LIBR J JI Libr. J. PD MAY 1 PY 2013 VL 138 IS 8 BP 74 EP 74 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA 132IE UT WOS:000318060300034 ER PT J AU Chang, SW Protopapas, P Kim, DW Byun, YI AF Chang, S. -W. Protopapas, P. Kim, D. -W. Byun, Y. -I. TI STATISTICAL PROPERTIES OF GALACTIC delta SCUTI STARS: REVISITED SO ASTRONOMICAL JOURNAL LA English DT Article DE catalogs; stars: variables: delta Scuti; ultraviolet: stars; X-rays: stars ID SX-PHOENICIS STARS; ALL-SKY SURVEY; SERENDIPITOUS SOURCE CATALOG; EXTREME-ULTRAVIOLET SOURCES; ECLIPSING BINARY-SYSTEM; EUV-SELECTED SAMPLE; DA WHITE-DWARFS; RR LYRAE STARS; A-TYPE STARS; VARIABLE-STARS AB We present statistical characteristics of 1578 delta Scuti stars including nearby field stars and cluster member stars within the Milky Way. We obtained 46% of these stars (718 stars) from work by Rodriguez and collected the remaining 54% of stars (860 stars) from other literature. We updated the entries with the latest information of sky coordinates, color, rotational velocity, spectral type, period, amplitude, and binarity. The majority of our sample is well characterized in terms of typical period range (0.02-0.25 days), pulsation amplitudes (<0.5 mag), and spectral types (A-F type). Given this list of d Scuti stars, we examined relations between their physical properties (i.e., periods, amplitudes, spectral types, and rotational velocities) for field stars and cluster members, and confirmed that the correlations of properties are not significantly different from those reported in Rodriguez's work. All the delta Scuti stars are cross-matched with several X-ray and UV catalogs, resulting in 27 X-ray and 41 UV-only counterparts. These counterparts are interesting targets for further study because of their uniqueness in showing delta Scuti-type variability and X-ray/UV emission at the same time. The compiled catalog can be accessed through the Web interface http://stardb.yonsei.ac.kr/DeltaScuti. C1 [Chang, S. -W.; Kim, D. -W.; Byun, Y. -I.] Yonsei Univ, Dept Astron, Seoul 120749, South Korea. [Protopapas, P.; Kim, D. -W.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Protopapas, P.] Harvard Univ, Inst Appl Computat Sci, Sch Engn & Appl Sci, Cambridge, MA 02138 USA. RP Chang, SW (reprint author), Yonsei Univ, Dept Astron, Seoul 120749, South Korea. EM seowony@galaxy.yonsei.ac.kr; kim@mpia-hd.mpg.de FU National Research Foundation of Korea (NRF); Ministry of Education, Science, and Technology [2012R1A1A2006924] FX This research was supported by the Basic Science Research Program through the National Research Foundation of Korea (NRF) funded by the Ministry of Education, Science, and Technology (2012R1A1A2006924). The analysis in this paper has been done using the Odyssey cluster supported by the FAS Research Computing Group at Harvard. This research has made use of the SIMBAD database, operated at CDS, Strasbourg, France. This software uses source code created at the Centre de Donnees Astronomiques de Strasbourg (CDS), France. NR 121 TC 11 Z9 11 U1 0 U2 8 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 MAY PY 2013 VL 145 IS 5 AR 132 DI 10.1088/0004-6256/145/5/132 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 122PD UT WOS:000317329100016 ER PT J AU Pillitteri, I Evans, NR Wolk, SJ Syal, MB AF Pillitteri, Ignazio Evans, Nancy Remage Wolk, Scott J. Syal, Megan Bruck TI XMM-NEWTON OBSERVATION OF THE alpha PERSEI CLUSTER SO ASTRONOMICAL JOURNAL LA English DT Article DE open clusters and associations: individual (alpha Persei); stars: activity; X-rays: stars ID YOUNG OPEN CLUSTER; COUNTING DETECTOR IMAGES; X-RAY SPECTROSCOPY; LOW-MASS MEMBERS; WAVELET TRANSFORMS; STARS; ROSAT; PLEIADES; IDENTIFICATION; EVOLUTION AB We report on the analysis of an archival observation of part of the alpha Persei cluster obtained with XMM-Newton. We detected 102 X-ray sources in the band 0.3-8.0 keV, of which 39 of them are associated with the cluster as evidenced by appropriate magnitudes and colors from Two Micron All Sky Survey photometry. We extend the X-ray luminosity distribution (XLD) for M dwarfs, to add to the XLD found for hotter dwarfs from spatially extensive surveys of the whole cluster by ROSAT. Some of the hotter stars are identified as a background, possible slightly older group of stars at a distance of approximately 500 pc. C1 [Pillitteri, Ignazio; Evans, Nancy Remage; Wolk, Scott J.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. [Syal, Megan Bruck] Brown Univ, Dept Geol Sci, Providence, RI 02912 USA. RP Evans, NR (reprint author), Smithsonian Astrophys Observ, MS 4,60 Garden St, Cambridge, MA 02138 USA. EM ipillitteri@cfa.harvard.edu; nevans@cfa.harvard.edu RI Pillitteri, Ignazio/L-1549-2016 OI Pillitteri, Ignazio/0000-0003-4948-6550 FU XMM-Newton guest investigator program [NNX09AP46G]; Chandra X-ray Center NASA [NAS8-03060] FX I.P. is grateful to Dr. E. Franciosini for providing an unpublished catalog of members of alpha Persei. We thank an anonymous referee for comments that improved the presentation of the paper. The XMM-Newton guest investigator program supported IP through grant NNX09AP46G. Support for this work was also provided from the Chandra X-ray Center NASA Contract NAS8-03060. Vizier and SIMBAD were used in the preparation of this study. NR 26 TC 3 Z9 3 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 J9 ASTRON J JI Astron. J. PD MAY PY 2013 VL 145 IS 5 AR 143 DI 10.1088/0004-6256/145/5/143 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 122PD UT WOS:000317329100027 ER PT J AU Dent, DH DeWalt, SJ Denslow, JS AF Dent, Daisy H. DeWalt, Saara J. Denslow, Julie S. TI Secondary forests of central Panama increase in similarity to old-growth forest over time in shade tolerance but not species composition SO JOURNAL OF VEGETATION SCIENCE LA English DT Article DE Barro Colorado Island; Forest succession; Seedling bank; Tropical forest ID TROPICAL FOREST; NEOTROPICAL FOREST; SEED DISPERSAL; RAIN-FORESTS; COSTA-RICA; TREE; SUCCESSION; CHRONOSEQUENCE; RECRUITMENT; ABUNDANCE AB Question Does species and functional composition of secondary tropical forests more closely follow a deterministic or a stochastic model of succession? Location The Barro Colorado Nature Monument (BCNM), central Panama. The BCNM comprises Barro Colorado Island (BCI) and five adjacent mainland peninsulas and is a mosaic of tropical old-growth (OG) and secondary forests (SF). Methods We studied the species and functional composition of seedling, sapling and adult tree communities in a chronosequence of SF stands ranging in age from 20 to 100yrs since abandonment, as well as two OG stands for comparison. Functional composition was defined as the representation of species with different degrees of shade tolerance. We also examined patterns of species diversity and dominance to better understand processes driving compositional changes. Results Species diversity recovered rapidly, and, by 20yrs, species richness for all size classes was equivalent if not higher in SF compared to OG. Species diversity tended to be lower and species dominance higher for seedlings than saplings or adults. Seedling, sapling and adult tree species composition did not clearly increase in similarity to OG with forest age. Instead, differences in species composition among stands reflected variation in dominance by particular species. Light-demanding species became less common and shade-tolerant species more common over stand age, with the functional composition of older secondary forests converging on that of OG. The seedling and sapling communities across the chronosequence were composed of a shade-tolerant subset of those species found in the stands as adults. Conclusion Our results suggest that recruitment into the seedling community of SF is determined by both predictable (e.g. selection for shade-tolerant species) and unpredictable factors (e.g. species-specific reproduction events and dispersal limitation). Recruitment into the sapling and tree communities reflects stronger, and potentially compounded, selection for shade-tolerant species. Therefore, changes in the species composition of regenerating forests in this area appear to be unpredictable, even though the functional composition follows a more deterministic and predictable trajectory with convergence on OG over time. C1 [Dent, Daisy H.] Smithsonian Trop Res Inst, Balboa, Panama. [Dent, Daisy H.] Univ Stirling, Stirling FK9 4LA, Scotland. [DeWalt, Saara J.] Clemson Univ, Dept Biol Sci, Clemson, SC 29634 USA. [Denslow, Julie S.] US Forest Serv, Inst Pacific Isl Forestry, USDA, Hilo, HI 96720 USA. RP Dent, DH (reprint author), Smithsonian Trop Res Inst, Apartado Postal 0843-03092, Balboa, Panama. EM daisy.h.dent@gmail.com; saarad@clemson.edu; jdenslow@fs.fed.us RI Dent, Daisy/L-3549-2016 OI Dent, Daisy/0000-0002-1219-7344 FU NSF [DEB 928031]; SENACYT [COL10-052] FX We would like to thank the Smithsonian Tropical Research Institute for providing logistical support, the late Eduardo Sierra, who assisted with plant identification and verification, and Robin Chazdon, Miquel De Caceres and an anonymous reviewer for comments that improved the manuscript. Research was supported by NSF grant DEB 928031 and SENACYT grant COL10-052. NR 68 TC 22 Z9 25 U1 8 U2 82 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1100-9233 J9 J VEG SCI JI J. Veg. Sci. PD MAY PY 2013 VL 24 IS 3 BP 530 EP 542 DI 10.1111/j.1654-1103.2012.01482.x PG 13 WC Plant Sciences; Ecology; Forestry SC Plant Sciences; Environmental Sciences & Ecology; Forestry GA 118IF UT WOS:000317018300013 ER PT J AU Telleria, MC Sancho, G Funk, VA Ventosa, I Roque, N AF Telleria, Maria C. Sancho, Gisela Funk, Vicky A. Ventosa, Iralys Roque, Nadia TI Pollen morphology and its taxonomic significance in the tribe Gochnatieae (Compositae, Gochnatioideae) SO PLANT SYSTEMATICS AND EVOLUTION LA English DT Article DE Gochnatieae; Gochnatioideae; Compositae; Pollen; LM; SEM; TEM ID MUTISIOIDEAE ASTERACEAE; MUTISIEAE; GENERA; RICHTERAGO; GENUS AB In the context of recent molecular phylogenies of the basal grades of Compositae, we investigated the utility of pollen morphology within the tribe Gochnatieae. The pollen of 64 species of Anastraphia, Cnicothamnus, Cyclolepis, Gochnatia, Pentaphorus, and Richterago was studied using light microscopy and scanning electron microscopy. In addition, three extra-Gochnatieae genera (Ianthopappus, Leucomeris, and Nouelia) were examined as they were traditionally morphologically related to members of the tribe Gochnatieae. Three of the species of Gochnatieae were examined using transmission electron microscopy. Two pollen types, and two new subtypes, have been recognized on the basis of the pollen shape, size, and exine sculpture. The pollen features of Gochnatia sect. Moquiniastrum and G. cordata are similar and distinctive within the genus and support the recently re-circumscribed section Hedraiophyllum. Within the species with echinate pollen surface, the distinctive spine length of Anastraphia supports its recent resurrection as a genus. The identity of Pentaphorus could not be supported by pollen features as was for other morphological characteristics. The pollen features shared across Cyclolepis, Ianthopappus, Leucomeris, Nouelia and Gochnatia sect. Moquiniastrum, as well as those shared by Richterago and Anastraphia could be a result of parallel evolution. C1 [Telleria, Maria C.] Museo La Plata, Lab Sistemat & Biol Evolut, La Plata, Buenos Aires, Argentina. [Sancho, Gisela] Museo La Plata, Div Vasc Plants, La Plata, Buenos Aires, Argentina. [Funk, Vicky A.] US Natl Herbarium, Smithsonian Inst, Dept Bot, Washington, DC 20013 USA. [Ventosa, Iralys] CITMA, Inst Ecol & Sistemat, Vicedirecc Plantas Vasc & Herbario Nacl, Habana 10800, Japan. [Roque, Nadia] Univ Fed Bahia, Inst Biol, Herbario Alexandre Leal Costa, BR-40170110 Salvador, BA, Brazil. RP Telleria, MC (reprint author), Museo La Plata, Lab Sistemat & Biol Evolut, Paseo Bosque S-N,B1900FWA, La Plata, Buenos Aires, Argentina. EM mariatelleria@fcnym.unlp.edu.ar FU Consejo Nacional de Investigaciones Cientificas y Tecnicas (CONICET), Argentina [PIP 02340]; Agencia Nacional de Promocion Cientifica y Tecnologica (PICT) [01977] FX We are grateful to curators of the herbaria who lent us the specimens studied here. We are also grateful to SEM services of the Facultad de Ciencias Naturales y Museo de La Plata and Palynological Laboratory of the Swedish Museum of Natural History of Stockholm. Support was provided by Consejo Nacional de Investigaciones Cientificas y Tecnicas (CONICET), Argentina (PIP 02340) and Agencia Nacional de Promocion Cientifica y Tecnologica (PICT No. 01977). NR 30 TC 8 Z9 8 U1 1 U2 24 PU SPRINGER WIEN PI WIEN PA SACHSENPLATZ 4-6, PO BOX 89, A-1201 WIEN, AUSTRIA SN 0378-2697 J9 PLANT SYST EVOL JI Plant Syst. Evol. PD MAY PY 2013 VL 299 IS 5 BP 935 EP 948 DI 10.1007/s00606-013-0774-1 PG 14 WC Plant Sciences; Evolutionary Biology SC Plant Sciences; Evolutionary Biology GA 128CC UT WOS:000317744700011 ER PT J AU Sofaer, HR Sillett, TS Peluc, SI Morrison, SA Ghalambor, CK AF Sofaer, Helen R. Sillett, T. Scott Peluc, Susana I. Morrison, Scott A. Ghalambor, Cameron K. TI Differential effects of food availability and nest predation risk on avian reproductive strategies SO BEHAVIORAL ECOLOGY LA English DT Article DE breeding phenology; clutch size; life-history strategies; parental care; phenotypic plasticity ID CLUTCH SIZE; PHENOTYPIC PLASTICITY; SPATIAL HETEROGENEITY; POPULATION-STRUCTURE; VISITATION RATES; BREEDING BIRDS; SITE SELECTION; DARWINS FINCH; SIBERIAN JAY; EVOLUTION AB Spatial and temporal variation in resource abundance and predation risk can favor the evolution of phenotypic plasticity as a means of tracking changing environments. However, because food abundance and predation risk often covary in nature, few studies have separated their effects or tested whether different phenotypic traits respond to the same sources of environmental variation. We investigated patterns of parental investment and behavior over a 7-year period in 2 island populations of orange-crowned warblers (Oreothlypis celata) that showed little genetic divergence but experienced dramatic temporal variation in rainfall and spatial variation in nest predation risk. The amount of rainfall in each year was correlated with food abundance, and birds on both islands initiated breeding earlier and laid larger clutches in wetter years. In contrast, the rate at which parents visited their nests was not affected by rainfall but was negatively correlated with nest predation risk both within and between islands. Our results suggest that although the effects of food availability and nest predation have been viewed as mutually exclusive drivers of entire suites of life-history and behavioral traits, these traits can differ in their sensitivity to resource abundance or mortality risk, and traits that are often correlated can be decoupled under appropriate environmental conditions. C1 [Sofaer, Helen R.; Ghalambor, Cameron K.] Colorado State Univ, Grad Degree Program Ecol, Ft Collins, CO 80523 USA. [Sofaer, Helen R.; Ghalambor, Cameron K.] Colorado State Univ, Dept Biol, Ft Collins, CO 80523 USA. [Sillett, T. Scott] Natl Zool Pk, Migratory Bird Ctr, Smithsonian Conservat Biol Inst, Washington, DC 20013 USA. [Peluc, Susana I.] Univ Nacl Cordoba, Fac Ciencias Exactas Fis & Nat, Ctr Zool Aplicada, CONICET, RA-5000 Cordoba, Argentina. [Morrison, Scott A.] Nature Conservancy, San Francisco, CA 94105 USA. RP Sofaer, HR (reprint author), Colorado State Univ, Grad Degree Program Ecol, 1878 Campus Delivery, Ft Collins, CO 80523 USA. EM helen@lamar.colostate.edu FU Nature Conservancy; Smithsonian Institution; American Ornithologists' Union Graduate Research Award; Frank M. Chapman Memorial Grant from the American Museum of Natural History; UCR/NRS Mildred E. Mathias Graduate Student Research Grant; Colorado State University; National Science Foundation Grant-Integrative Graduate Education and Research Traineeship Program Grant DGE [0221595]; National Science Foundation [846175]; Smithsonian Institution Predoctoral Fellowship FX This work was supported by The Nature Conservancy, the Smithsonian Institution, an American Ornithologists' Union Graduate Research Award (H.R.S.), a Frank M. Chapman Memorial Grant from the American Museum of Natural History (H.R.S.), and a UCR/NRS Mildred E. Mathias Graduate Student Research Grant (S.I.P.). H.R.S. was supported by Colorado State University, National Science Foundation Grant-Integrative Graduate Education and Research Traineeship Program Grant DGE-#0221595 (administered by the PRIMES program at Colorado State University), National Science Foundation Grant #846175 to C.K.G., and by a Smithsonian Institution Predoctoral Fellowship. NR 84 TC 14 Z9 14 U1 5 U2 95 PU OXFORD UNIV PRESS INC PI CARY PA JOURNALS DEPT, 2001 EVANS RD, CARY, NC 27513 USA SN 1045-2249 EI 1465-7279 J9 BEHAV ECOL JI Behav. Ecol. PD MAY-JUN PY 2013 VL 24 IS 3 BP 698 EP 707 DI 10.1093/beheco/ars212 PG 10 WC Behavioral Sciences; Biology; Ecology; Zoology SC Behavioral Sciences; Life Sciences & Biomedicine - Other Topics; Environmental Sciences & Ecology; Zoology GA 122LR UT WOS:000317320100020 ER PT J AU Cardoni, DA Greenberg, R Maldonado, JE Isacch, JP AF Cardoni, Daniel A. Greenberg, Russell Maldonado, Jesus E. Isacch, Juan P. TI Morphological adaptation to coastal marshes in spite of limited genetic structure in the Neotropical passerine Spartonoica maluroides (Aves: Furnariidae) SO BIOLOGICAL JOURNAL OF THE LINNEAN SOCIETY LA English DT Article DE bay-capped wren-spinetail; convergent evolution; genetic; melanism; morphology; phenotypic plasticity; saltmarsh ID FEATHER-DEGRADING BACILLI; PLAIN SWAMP SPARROW; SALT-MARSH; MITOCHONDRIAL-DNA; POPULATION-GROWTH; TIDAL MARSHES; PHENOTYPIC PLASTICITY; DARWINS FINCHES; BILL SIZE; CONVERGENT EVOLUTION AB Tidal marshes present profound adaptive challenges to terrestrial vertebrates. For example, North American sparrows have relatively longer and thinner bills and darker dorsal plumage in coastal saltmarshes than in interior marshes. Bay-capped wren-spinetail (Furnariidae; Spartonoica maluroides) show a strong association with South American saltmarshes. We hypothesized that bay-capped wren-spinetail have similar morphological adaptations to North American sparrows to the saltmarsh environment, which would be indicative of the generality of selection on these traits in the coastal saltmarsh ecosystem. We captured individuals of S.maluroides from coastal saltmarshes and interior marshes. Populations were compared based on morphology and molecular markers. We found significant phenotypic differences in bill shape and plumage coloration (melanism) between S.maluroides populations from coastal and inland marshes. The low levels of genetic variation, weak geographical structure and shallow divergences, based on mitochondrial DNA and microsatellite data, suggest that coastal populations had a recent demographic expansion. Our results are consistent with the pattern of morphological divergence found between North American Emberizids. The possibility of convergent evolutionary adaptations between saltmarsh North American Emberizids and South American Furnariids suggests that there are strong selective pressures associated with saltmarsh environments on the beak, leading to adaptations for food acquisition, and on plumage coloration for better camouflage for predator avoidance (melanism).(c) 2013 The Linnean Society of London, Biological Journal of the Linnean Society, 2013, 109, 7891. C1 [Cardoni, Daniel A.; Isacch, Juan P.] Univ Nacl Mar del Plata, Consejo Nacl Invest Cient & Tecn, Fac Ciencias Exactas & Nat, IIMyC, RA-7600 Mar Del Plata, Argentina. [Greenberg, Russell] Smithsonian Natl Zool Pk, Migratory Bird Ctr, Washington, DC USA. [Maldonado, Jesus E.] Smithsonian Conservat Biol Inst, Ctr Conservat & Evolutionary Genet, Washington, DC 20008 USA. [Maldonado, Jesus E.] Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Washington, DC 20013 USA. RP Cardoni, DA (reprint author), Univ Nacl Mar del Plata, Consejo Nacl Invest Cient & Tecn, Fac Ciencias Exactas & Nat, IIMyC, Funes 3250, RA-7600 Mar Del Plata, Argentina. EM acardoni@mdp.edu.ar FU Smithsonian Institution; Smithsonian; CONICET; Universidad Nacional de Mar del Plata; Agencia Nacional de Promocion Cientifica y Tecnologica (Argentina); Kathleen S. Anderson Award FX We thank R. Fleischer, D. Hawley, S. Sonsthagen, B. Ryder, D. Redding, and N. Rotzel for assistance and support in the genetics laboratory at the CCEG. We thank P. Micheluti (Mar Chiquita Cordoba), M. Roda (Salado basin), and J. P. Carricart (Punta Lara) for assistance at captured sites. We thank S. Bachman for help in the field, and C. Azcueta for providing transportation. We thank P. Iriarte and M. Mora for molecular analysis help. Financial support was provided by the Smithsonian Institution restricted endowment funds, Smithsonian graduate student fellowship and a Short Term Visitor grant, CONICET, Universidad Nacional de Mar del Plata, Agencia Nacional de Promocion Cientifica y Tecnologica (Argentina), Kathleen S. Anderson Award Sigma Xi Grant-in-Aid of Research. NR 91 TC 5 Z9 5 U1 3 U2 32 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0024-4066 EI 1095-8312 J9 BIOL J LINN SOC JI Biol. J. Linnean Soc. PD MAY PY 2013 VL 109 IS 1 BP 78 EP 91 DI 10.1111/bij.12019 PG 14 WC Evolutionary Biology SC Evolutionary Biology GA 122YO UT WOS:000317354800007 ER PT J AU Malcolm, KD McShea, WJ Van Deelen, TR Bacon, HJ Liu, F Putman, S Zhu, X Brown, JL AF Malcolm, K. D. McShea, W. J. Van Deelen, T. R. Bacon, H. J. Liu, F. Putman, S. Zhu, X. Brown, J. L. TI Analyses of fecal and hair glucocorticoids to evaluate short- and long-term stress and recovery of Asiatic black bears (Ursus thibetanus) removed from bile farms in China SO GENERAL AND COMPARATIVE ENDOCRINOLOGY LA English DT Article DE Fecal glucocorticoids; Hair cortisol; Asiatic black bear; Ursus thibetanus; Bile farming; Stress ID PANDAS AILUROPODA-MELANOLEUCA; CORTISOL-LEVELS; GRIZZLY BEARS; HORMONES; CARNIVORES; DOMINANCE; WILDLIFE; BEHAVIOR; HISTORY; MAMMALS AB Demand for traditional Chinese medicines has given rise to the practice of maintaining Asiatic black bears (Ursus thibetanus) in captivity to harvest bile. We evaluated hypothalamic-pituitary-adrenal (HPA) activity in Asiatic black bears on a bile farm in China by measuring cortisol in hair. We also monitored hair and fecal glucocorticoid metabolites as bears acclimated to improved husbandry at the Animals Asia Foundation China Bear Rescue Center (CBRC) after removal from other bile farms. Fecal samples were collected twice weekly for similar to 1 year, and hair was obtained from bears upon arrival at the CBRC and again >= 163 days later. Paired hair samples showed declines in cortisol concentrations of 12-88% in 38 of 45 (84%, p < 0.001) bears after arrival and acclimation at the rehabilitation facility. Concentrations of cortisol in hair from bears on the bile farm were similar to initial concentrations upon arrival at the CBRC but were higher than those collected after bears had been at the CBRC for >= 163 days. Fecal glucocorticoid concentrations varied across months and were highest in April and declined through December, possibly reflecting seasonal patterns, responses to the arrival and socialization of new bears at the CBRC, and/or annual metabolic change. Data from segmental analysis of hair supports the first of these explanations. Our findings indicate that bears produced elevated concentrations of glucocorticoids on bile farms, and that activity of the HPA axis declined following relocation. Thus, hair cortisol analyses are particularly well suited to long-term, retrospective assessments of glucocorticoids in ursids. By contrast, fecal measures were not clearly associated with rehabilitation, but rather reflected more subtle endocrine changes, possibly related to seasonality. (C) 2013 Elsevier Inc. All rights reserved. C1 [Malcolm, K. D.; Van Deelen, T. R.] Univ Wisconsin, Dept Forest & Wildlife Ecol, Madison, WI 53706 USA. [Malcolm, K. D.; McShea, W. J.; Putman, S.; Brown, J. L.] Smithsonian Inst, Smithsonian Conservat Biol Inst, Natl Zool Pk, Front Royal, VA USA. [Bacon, H. J.] Anim Asia Fdn, Sichuan Lonqiao Black Bear Rescue Ctr, Chengdu, Sichuan Provinc, Peoples R China. [Liu, F.] Chinese Acad Forestry, Inst Forestry Ecol Environm & Protect, Beijing, Peoples R China. [Zhu, X.] Peking Univ, Sch Life Sci, Beijing 100871, Peoples R China. RP Malcolm, KD (reprint author), Univ Wisconsin, Dept Forest & Wildlife Ecol, 1630 Linden Dr, Madison, WI 53706 USA. EM karl.d.malcolm@gmail.com FU Morris Animal Foundation; Animals Asia Foundation; Integrative Graduate Education and Research Traineeship (IGERT) program at the University of Wisconsin-Madison FX We are grateful for the dedicated assistance of the animal care and veterinary staff at the Animals Asia Foundation China Bear Rescue Centre. Caroline Nelson was particularly integral to orchestrating sample collection and storage for the duration of the study. We thank the staff at the Endocrinology Laboratory of the Chengdu Research Base of Giant Panda Breeding for allowing us access to their facilities in support of this work, and to the managers of the bear farm in Dujiangyan, China for granting us permission to collect hair samples from their bears. We also thank Wang Dajun and Gong Jien for providing logistical support throughout the study. Randall Malcolm, Carol Rindahl, Du Beibei, Li Jiao, Qi Ruijuan, and Wu Lan each made meaningful and extensive contributions in the laboratory. We thank Josh Posner, Teri Allendorf, and the Integrative Graduate Education and Research Traineeship (IGERT) program at the University of Wisconsin-Madison for their support. This research was made possible by the financial contributions from the Morris Animal Foundation and the Animals Asia Foundation. NR 49 TC 11 Z9 11 U1 8 U2 91 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0016-6480 J9 GEN COMP ENDOCR JI Gen. Comp. Endocrinol. PD MAY 1 PY 2013 VL 185 BP 97 EP 106 DI 10.1016/j.ygcen.2013.01.014 PG 10 WC Endocrinology & Metabolism SC Endocrinology & Metabolism GA 120EQ UT WOS:000317154000011 PM 23416358 ER PT J AU Langley, JA Mozdzer, TJ Shepard, KA Hagerty, SB Megonigal, JP AF Langley, J. Adam Mozdzer, Thomas J. Shepard, Katherine A. Hagerty, Shannon B. Megonigal, J. Patrick TI Tidal marsh plant responses to elevated CO2, nitrogen fertilization, and sea level rise SO GLOBAL CHANGE BIOLOGY LA English DT Article DE marsh organ; mesocosms; plant productivity; Schoenoplectus americanus; soil elevation; Spartina patens ID LOUISIANA SALT-MARSH; SPARTINA-ALTERNIFLORA; SULFIDE CONCENTRATION; COASTAL WETLANDS; ATMOSPHERIC CO2; BRACKISH MARSH; GROWTH; ROOT; BIOMASS; BAY AB Elevated CO2 and nitrogen (N) addition directly affect plant productivity and the mechanisms that allow tidal marshes to maintain a constant elevation relative to sea level, but it remains unknown how these global change drivers modify marsh plant response to sea level rise. Here we manipulated factorial combinations of CO2 concentration (two levels), N availability (two levels) and relative sea level (six levels) using in situ mesocosms containing a tidal marsh community composed of a sedge, Schoenoplectus americanus, and a grass, Spartina patens. Our objective is to determine, if elevated CO2 and N alter the growth and persistence of these plants in coastal ecosystems facing rising sea levels. After two growing seasons, we found that N addition enhanced plant growth particularly at sea levels where plants were most stressed by flooding (114% stimulation in the+10cm treatment), and N effects were generally larger in combination with elevated CO2 (288% stimulation). N fertilization shifted the optimal productivity of S. patens to a higher sea level, but did not confer S. patens an enhanced ability to tolerate sea level rise. S. americanus responded strongly to N only in the higher sea level treatments that excluded S. patens. Interestingly, addition of N, which has been suggested to accelerate marsh loss, may afford some marsh plants, such as the widespread sedge, S. americanus, the enhanced ability to tolerate inundation. However, if chronic N pollution reduces the availability of propagules of S. americanus or other flood-tolerant species on the landscape scale, this shift in species dominance could render tidal marshes more susceptible to marsh collapse. C1 [Langley, J. Adam] Villanova Univ, Dept Biol, Villanova, PA 19003 USA. [Mozdzer, Thomas J.] Bryn Mawr Coll, Dept Biol, Bryn Mawr, PA 19010 USA. [Shepard, Katherine A.] Cary Inst Ecosyst Studies, Millbrook, NY 12545 USA. [Hagerty, Shannon B.] Univ Arizona, Dept Biol, Flagstaff, AZ 86011 USA. [Mozdzer, Thomas J.; Megonigal, J. Patrick] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. RP Langley, JA (reprint author), Villanova Univ, Dept Biol, Villanova, PA 19003 USA. EM adam.langley@villanova.edu RI Mozdzer, Thomas/A-3599-2014 OI Mozdzer, Thomas/0000-0002-1053-0967 FU USGS Global Change Research Program [06ERAG0011]; National Science Foundation's Long-term Research Environmental Biology program [DEB-0950080] FX We thank J. Duls, G. Peresta, A. Peresta, and N. Mudd for the construction and maintenance of the field site at the Smithsonian Global Climate Change Research Wetland, M. Russell for statistical advice, and two anonymous reviewers for helpful comments. The field study was supported by the USGS Global Change Research Program (cooperative agreement 06ERAG0011), the US Department of Energy (DE-FG02-97ER62458), US Department of Energy's Office of Science (BER) through the Coastal Center of the National Institute of Climate Change Research at Tulane University, the National Science Foundation's Long-term Research Environmental Biology program (DEB-0950080) and Research Experience for Undergraduates (REU) program, and the Smithsonian Institution. Use of trade, product, or firm names does not imply endorsement by the US Government. NR 43 TC 27 Z9 27 U1 19 U2 213 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1354-1013 J9 GLOBAL CHANGE BIOL JI Glob. Change Biol. PD MAY PY 2013 VL 19 IS 5 BP 1495 EP 1503 DI 10.1111/gcb.12147 PG 9 WC Biodiversity Conservation; Ecology; Environmental Sciences SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 121ZN UT WOS:000317284700014 ER PT J AU Fishelson, L Baldwin, CC Hastings, PA AF Fishelson, Lev Baldwin, Carole C. Hastings, Philip A. TI Gonad morphology, gametogenesis, and reproductive modes in fishes of the tribe starksiini(Teleostei, Blenniiformes) SO JOURNAL OF MORPHOLOGY LA English DT Article DE Starksiini blennies; reproductive organs; internal fertilization; ovuliparity; zygoparity; embryoparity; comparative biology ID ATHERINOMORPH FISHES; GERMINAL EPITHELIUM; TESTIS STRUCTURE; TELEOSTEI; PERCIFORMES; EVOLUTION; CLINIDAE; SPERMATOGENESIS; VIVIPARITY; SPERMATOCYTOGENESIS AB A comparative study of the reproductive organs in 17 of the 30 species of the tribe Starksiini (Labrisomidae, Blenniiformes) and related labrisomids reveals the major traits of gamete form and production and likely reproductive modes. The testes are of the lobular type and have a testicular gland and sperm ducts. Isodiametric sperm (aquasperm) with a globular head or anisodiametric sperm (introsperm) with an elongate head, or both, were observed in the studied species. Both types have either one or two flagella in the sperm tail. Ovaries of the Starksiini are bilobed and exhibit synchronous or asynchronous egg production. Although viviparity or ovoviviparity reportedly characterizes the group, our study revealed evidence of both internal and external fertilization and three modes of reproduction. External fertilization or ovuliparity is suggested for the Starksia atlantica and S. lepicoelia species complexes by the presence in males of a short genital papilla that is not reinforced through adhesion with the first anal-fin spine and by the absence of sperm within the ovaries. Internal fertilization and zygoparity is indicated for most species by the presence of an intromittent papilla in males that is adhered to the first anal-fin spine, nests of sperm within the ovaries, absence of embryos within the ovarian lamellae and usually thick egg envelopes bearing dense covers of adhesive filaments. Internal fertilization and embryoparity is indicated for starksia fulva and Xenomedea rhodopyga by an intromittent papilla that is adhered to the first anal-fin spine of males, anisodiametric sperm in males, delicate egg envelopes without adhesive filaments and developing embryos within follicular envelopes or within the follicle in females. Although many of these features are seen in the internally fertilizing clinid blennies, starksiins differ in retaining the testicular gland typical of labrisomids and in lacking sperm packaging typical of other internally fertilizing teleosts. J. Morphol., 2013. (c) 2013 Wiley Periodicals, Inc. C1 [Fishelson, Lev] Tel Aviv Univ, Dept Zool, IL-69978 Tel Aviv, Israel. [Baldwin, Carole C.] Smithsonian Inst, Div Fishes, Natl Museum Nat Hist, Washington, DC 20560 USA. [Hastings, Philip A.] Univ Calif San Diego, Scripps Inst Oceanog, Div Marine Biol Res, La Jolla, CA 92093 USA. RP Hastings, PA (reprint author), Univ Calif San Diego, Scripps Inst Oceanog, Div Marine Biol Res, 9500 Gilman Dr, La Jolla, CA 92093 USA. EM phastings@ucsd.edu NR 55 TC 1 Z9 2 U1 2 U2 26 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0362-2525 EI 1097-4687 J9 J MORPHOL JI J. Morphol. PD MAY PY 2013 VL 274 IS 5 BP 496 EP 511 DI 10.1002/jmor.20110 PG 16 WC Anatomy & Morphology SC Anatomy & Morphology GA 122AH UT WOS:000317286700002 PM 23293058 ER PT J AU Peiro, DF Baeza, JA Mantelatto, FL AF Peiro, Douglas F. Antonio Baeza, J. Mantelatto, Fernando L. TI Host-use pattern and sexual dimorphism reveals the mating system of the symbiotic pea crab Austinixa aidae (Crustacea: Brachyura: Pinnotheridae) SO JOURNAL OF THE MARINE BIOLOGICAL ASSOCIATION OF THE UNITED KINGDOM LA English DT Article DE Axiidea; Callianassidae; mating system; pea crab; Pinnotheres; sexual dimorphism; symbiosis ID SHRIMP CALLICHIRUS-MAJOR; URCHIN TETRAPYGUS-NIGER; SOCIAL MONOGAMY; LIFE-HISTORY; LIOPETROLISTHES-MITRA; SOUTHWESTERN ATLANTIC; POPULATION-DYNAMICS; INACHUS-PHALANGIUM; RELATIVE GROWTH; SNAPPING SHRIMP AB Austinixa aidae inhabits burrows of the ghost shrimp Callichirus major at Pereque-acu beach, Ubatuba, Brazil. We described the host-use pattern and sexual dimorphism of A. aidae to test for monogamy given the generality of this mating system in the subfamily Pinnothereliinae (family Pinnotheridae) to which A. aidae belongs. Against expectations, A. aidae lives as solitary individuals within burrows more frequently than expected by chance alone. Additional observations suggested that A. aidae exhibits a polygynandrous mating system with males moving among burrows in search of receptive females. First, only 21% of the burrows harboured heterosexual pairs of crabs and the body size of paired crabs was poorly correlated. This suggests pair instability and frequent shifts among burrows by male and/or female crabs, as reported before for other symbiotic crustaceans in which the body size of paired crabs is poorly correlated. Second, males paired with females that were sexually receptive (without embryos) or that have been receptive recently (carrying early embryos) were found more frequently than expected by chance alone. The above agrees with that reported for species in which sexual pairing does not last long. Third, sexual dimorphism in terms of claw size and coloration was evident. Claws were larger in males than in females, a condition that argues in favour of male-male competition in A. aidae. In addition, the body coloration of males was more similar to the sand grains of the beach than that of females. This sex-specific coloration suggests that males are 'better adapted' than females to roam on the surface of the beach in search of burrows because their coloration should diminish the risk of detection by predators. Experiments are needed to reveal the details of the polygynandrous mating system herein inferred for A. aidae and to understand those conditions favouring particular reproductive strategies in symbiotic decapod crustaceans. C1 [Peiro, Douglas F.; Mantelatto, Fernando L.] Univ Sao Paulo, Lab Bioecol & Crustacean Systemat LBSC, Fac Philosophy Sci & Letters Ribeirao Preto FFCLR, Dept Biol,Postgrad Program Comparat Biol, BR-14040901 Ribeirao Preto, SP, Brazil. [Antonio Baeza, J.] Smithsonian Marine Stn Ft Pierce, Ft Pierce, FL USA. [Antonio Baeza, J.] Old Dominion Univ, Dept Biol Sci, Norfolk, VA 23435 USA. [Antonio Baeza, J.] Univ Catolica Norte, Fac Ciencias Mar, Dept Biol Marina, Larrondo 1281, Coquimbo, Chile. RP Mantelatto, FL (reprint author), Univ Sao Paulo, Lab Bioecol & Crustacean Systemat LBSC, Fac Philosophy Sci & Letters Ribeirao Preto FFCLR, Dept Biol,Grad Program Comparat Biol, Ave Bandeirantes 3900, BR-14040901 Ribeirao Preto, SP, Brazil. EM flmantel@usp.br RI Mantelatto, Fernando/H-2695-2012; Peiro, Douglas/E-1203-2011; OI Mantelatto, Fernando/0000-0002-8497-187X; Peiro, Douglas/0000-0003-4928-1432; Baeza, Juan Antonio/0000-0002-2573-6773 FU CAPES-Brazil (Coordenacao de Aperfeicoamento de Pessoal de Nivel Superior); CNPq-Brazil (Conselho Nacional de Desenvolvimento Cientifico e Tecnologico) [302748/2010-5]; CNPq [471794/2006-6, 473050/2007-2]; FAPESP [2010/50188-8] FX This study formed part of a Master's degree thesis by D.F.P., and was supported by a fellowship from CAPES-Brazil (Coordenacao de Aperfeicoamento de Pessoal de Nivel Superior). F.L.M. and D.F.P. are grateful to CNPq-Brazil (Conselho Nacional de Desenvolvimento Cientifico e Tecnologico) for an ongoing research grant (302748/2010-5) and PhD fellowships, respectively. Part of this study was supported under funding from the CNPq (471794/2006-6, 473050/2007-2) and FAPESP (2010/50188-8) to F. L. M. J.A.B. is most grateful to Maria Lucia Negreiros-Fransozo, Paula Araujo, Adilson Fransozo, Alexandre Oliveira de Almeida, Ricardo Cunha Lima and the Sociedade Brasileira de Carcinologia that made possible his visit to Brazil during 2010 and this collaboration. Special thanks to all members of the Laboratory of Bioecology and Crustacean Systematics of FFCLRP/USP for their help during field and laboratory work, and to Jennifer Rasch for English revision. The support of the Postgraduate Program in Comparative Biology of FFCLRP/USP and of the Centro de Biologia Marinha (CEBIMar/USP) during the collections is also acknowledged. All experiments conducted in this study complied with current applicable state and federal laws of Brazil. This is contribution number 862 of the Smithsonian Marine Station at Fort Pierce. NR 58 TC 7 Z9 7 U1 1 U2 14 PU CAMBRIDGE UNIV PRESS PI NEW YORK PA 32 AVENUE OF THE AMERICAS, NEW YORK, NY 10013-2473 USA SN 0025-3154 J9 J MAR BIOL ASSOC UK JI J. Mar. Biol. Assoc. U.K. PD MAY PY 2013 VL 93 IS 3 BP 715 EP 723 DI 10.1017/S0025315412000720 PG 9 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA 121JA UT WOS:000317238100016 ER PT J AU Hesselberg, T AF Hesselberg, Thomas TI Web-Building Flexibility Differs in Two Spatially Constrained Orb Spiders SO JOURNAL OF INSECT BEHAVIOR LA English DT Article DE Web-building behavior; behavioral flexibility; orb web geometry; area optimization; Araneidae ID OPTIMAL AREA USE; ARANEUS-DIADEMATUS; WEAVING SPIDERS; REGENERATED LEGS; TOOL-USE; BEHAVIOR; SIZE; ARANEIDAE; GEOMETRY; CONSTRUCTION AB Shelter and trap-building animals that compete for limited space and/or face costly relocations benefit from being flexible in their construction behavior. Orb spiders are good examples of this and their easily quantifiable two-dimensional webs allow us to analyze the behavioral adaptations and costs in terms of higher error levels or less precision resulting from building webs in sub-optimal conditions. Here I study behavioral flexibility in spatially constrained spiders by analyzing a wide range of web parameters including measures that indicate errors during web-building. I compare the geometry of laboratory webs of two orb spiders, Cyclosa caroli and Eustala illicita, built in differently shaped experimental frames and report two major findings. i) The two species differ in their ability to build webs in constrained spaces. ii) E. illicita adjusted a range of parameters including shape, area utilization and mesh height in response to spatial constraints, but kept other parameters constant, most notably the length of anchor threads and the shape of the auxiliary spiral. I furthermore found that constrained spiders did not make significantly more errors during web-building than when they had amble space available. C1 [Hesselberg, Thomas] Smithsonian Trop Res Inst, Balboa 084303092, Ancon, Panama. RP Hesselberg, T (reprint author), Univ Oxford, Dept Zool, S Parks Rd, Oxford OX1 3PS, England. EM thomas.hesselberg@zoo.ox.ac.uk FU Smithsonian Postdoctoral Fellowship FX Thanks to Diomedes Quientero, Roberto Miranda and Nikolaj Scharff for helping to identify the spider species and to William Eberhard and two anonymous reviewers for their helpful comments to a previous version of the manuscript. The author gratefully acknowledges the permission granted by the Parque Natural Metropolitano and the Autoridad Nacional del Ambiente (ANAM permits no. SE/A-81-08 and SE/A-104-08) to carry out this study. The study was funded by a Smithsonian Postdoctoral Fellowship. NR 52 TC 8 Z9 8 U1 1 U2 30 PU SPRINGER/PLENUM PUBLISHERS PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0892-7553 J9 J INSECT BEHAV JI J. Insect Behav. PD MAY PY 2013 VL 26 IS 3 BP 283 EP 303 DI 10.1007/s10905-012-9335-7 PG 21 WC Entomology SC Entomology GA 117RZ UT WOS:000316972100002 ER PT J AU Smith, P Scott, N Cacciali, P Atkinson, K AF Smith, Paul Scott, Norman Cacciali, Pier Atkinson, Karina TI Rhachidelus brazili (Squamata: Serpentes): first records from Paraguay and clarification of the correct spelling of the generic name SO SALAMANDRA LA English DT Editorial Material C1 [Smith, Paul] Fauna Paraguay, Encarnacion, Paraguay. [Smith, Paul; Cacciali, Pier; Atkinson, Karina] Reserva Nat Laguna Blanca, Santa Rosa Del Aguaray, San Pedro, Paraguay. [Scott, Norman] Smithsonian Inst, Creston, CA 93432 USA. RP Smith, P (reprint author), Fauna Paraguay, Encarnacion, Paraguay. EM faunaparaguay@gmail.com RI sebastianovitsch, stepan/G-8507-2013 NR 27 TC 1 Z9 1 U1 0 U2 0 PU DEUTSCHE GESELLSCHAFT HERPETOLOGIE TERRARIENKUNDE E V PI RHEINBACH PA C/O WOLFGANG BISCHOFF, MUSEUM A KOENIG, POSTFACH 1421, ADENAUERALLEE 160, RHEINBACH, BONN D-53113, GERMANY SN 0036-3375 J9 SALAMANDRA JI Salamandra PD APR 30 PY 2013 VL 49 IS 1 BP 56 EP 58 PG 3 WC Marine & Freshwater Biology; Zoology SC Marine & Freshwater Biology; Zoology GA 136CV UT WOS:000318338600008 ER PT J AU Yao, NY Gorshkov, AV Laumann, CR Lauchli, AM Ye, J Lukin, MD AF Yao, N. Y. Gorshkov, A. V. Laumann, C. R. Laeuchli, A. M. Ye, J. Lukin, M. D. TI Realizing Fractional Chern Insulators in Dipolar Spin Systems SO PHYSICAL REVIEW LETTERS LA English DT Article ID POLAR-MOLECULES; QUANTUM AB Strongly correlated quantum systems can exhibit exotic behavior controlled by topology. We predict that the nu = 1/2 fractional Chern insulator arises naturally in a two-dimensional array of driven, dipolar-interacting spins. As a specific implementation, we analyze how to prepare and detect synthetic gauge potentials for the rotational excitations of ultracold polar molecules trapped in a deep optical lattice. With the motion of the molecules pinned, under certain conditions, these rotational excitations form a fractional Chern insulating state. We present a detailed experimental blueprint for its realization and demonstrate that the implementation is consistent with near-term capabilities. Prospects for the realization of such phases in solid-state dipolar systems are discussed as are their possible applications. C1 [Yao, N. Y.; Laumann, C. R.; Lukin, M. D.] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. [Gorshkov, A. V.] CALTECH, Inst Quantum Informat & Matter, Pasadena, CA 91125 USA. [Laumann, C. R.] Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom & Mol Phys, Cambridge, MA 02138 USA. [Laeuchli, A. M.] Univ Innsbruck, Inst Theoret Phys, A-6020 Innsbruck, Austria. [Ye, J.] NIST, JILA, Boulder, CO 80309 USA. [Ye, J.] Univ Colorado, Dept Phys, Boulder, CO 80309 USA. RP Yao, NY (reprint author), Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. RI Ye, Jun/C-3312-2011; Gorshkov, Alexey/A-9848-2008; Lauchli, Andreas/B-1930-2008; Yao, Norman/A-3929-2009 OI Gorshkov, Alexey/0000-0003-0509-3421; Lauchli, Andreas/0000-0002-2272-2691; Yao, Norman/0000-0003-0194-7266 FU NSF; DOE [FG02-97ER25308]; CUA; DARPA; AFOSR MURI; NIST; Lawrence Golub Fellowship; Lee A. DuBridge Foundation; IQIM; Gordon and Betty Moore Foundation FX We gratefully acknowledge the insights of P. Zoller, E. Demler, and S. Bennett. We thank M. Hafezi, A. Chandran, N. Lindner, S. Stellmer, F. Schreck, W. Campbell, A. M. Rey, J. Preskill, K. Hazzard, S. Manmana, E. M. Stoudenmire, S. Todadri, and J. Alicea for helpful discussions. This work was supported, in part, by the NSF, DOE (FG02-97ER25308), CUA, DARPA, AFOSR MURI, NIST, Lawrence Golub Fellowship, Lee A. DuBridge Foundation, IQIM and the Gordon and Betty Moore Foundation. NR 48 TC 80 Z9 81 U1 0 U2 18 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 APR 29 PY 2013 VL 110 IS 18 AR 185302 DI 10.1103/PhysRevLett.110.185302 PG 5 WC Physics, Multidisciplinary SC Physics GA 145KK UT WOS:000319014400004 PM 23683213 ER PT J AU Kula, RR AF Kula, Robert R. TI A new species and new distribution records for Braconidae from Mountain Lake Biological Station in southwestern Virginia and a redescription of Pentapleura foveolata Viereck SO ZOOTAXA LA English DT Article DE Alysia; biodiversity; Coelinius; Eastern Deciduous Forest; parasitoid; taxonomy ID SENSU-LATO HYMENOPTERA; NEW-WORLD; EPIPHYTIC BRYOPHYTES; NORTH-AMERICA; ALYSIINAE; REVISION; HALIDAY; KEY AB One new species of Alysiinae, Coelinius wrayi Kula, is described. Pentapleura foveolata Viereck, also in Alysiinae and previously known only from a male collected at the type locality in Connecticut, is redescribed based on six females and two males collected at Mountain Lake Biological Station (MLBS) in Virginia. Morphological variation for Alysia (Alysia) salebrosa Wharton is discussed given variation observed in specimens from MLBS. Sixty-two species of Braconidae collected at MLBS in August of 2009 are listed along with 12 species reported previously from MLBS. Host use for the 62 species is discussed; 31 are in Alysiinae or Opiinae, subfamilies that exclusively contain parasitoids of cyclorrhaphous flies. Fifteen species are reported from Virginia for the first time. Problematic couplets in a key to species of Spathius Nees for North America (Marsh & Strazanac 2009) are discussed using specimens from MLBS. C1 ARS, Systemat Entomol Lab, Beltsville Agr Res Ctr, USDA,Natl Museum Nat Hist,Smithsonian Inst, Washington, DC 20013 USA. RP Kula, RR (reprint author), ARS, Systemat Entomol Lab, Beltsville Agr Res Ctr, USDA,Natl Museum Nat Hist,Smithsonian Inst, POB 37012,MRC 168, Washington, DC 20013 USA. EM Robert.Kula@ars.usda.gov NR 58 TC 0 Z9 0 U1 0 U2 9 PU MAGNOLIA PRESS PI AUCKLAND PA PO BOX 41383, AUCKLAND, ST LUKES 1030, NEW ZEALAND SN 1175-5326 J9 ZOOTAXA JI Zootaxa PD APR 29 PY 2013 VL 3641 IS 5 BP 501 EP 523 PG 23 WC Zoology SC Zoology GA 132JA UT WOS:000318062500001 PM 26287103 ER PT J AU Ferraro, JV Plummer, TW Pobiner, BL Oliver, JS Bishop, LC Braun, DR Ditchfield, PW Seaman, JW Binetti, KM Seaman, JW Hertel, F Potts, R AF Ferraro, Joseph V. Plummer, Thomas W. Pobiner, Briana L. Oliver, James S. Bishop, Laura C. Braun, David R. Ditchfield, Peter W. Seaman, John W., III Binetti, Katie M. Seaman, John W., Jr. Hertel, Fritz Potts, Richard TI Earliest Archaeological Evidence of Persistent Hominin Carnivory SO PLOS ONE LA English DT Article ID SKELETAL ELEMENT ABUNDANCES; FATTY-ACID-COMPOSITION; OLDUVAI-GORGE; HUMAN-EVOLUTION; FLK ZINJANTHROPUS; CARCASS TRANSPORT; EARLY PLEISTOCENE; KANJERA SOUTH; TOOTH-MARK; ARCHAEOFAUNAL ASSEMBLAGES AB The emergence of lithic technology by similar to 2.6 million years ago (Ma) is often interpreted as a correlate of increasingly recurrent hominin acquisition and consumption of animal remains. Associated faunal evidence, however, is poorly preserved prior to similar to 1.8 Ma, limiting our understanding of early archaeological (Oldowan) hominin carnivory. Here, we detail three large well-preserved zooarchaeological assemblages from Kanjera South, Kenya. The assemblages date to similar to 2.0 Ma, pre-dating all previously published archaeofaunas of appreciable size. At Kanjera, there is clear evidence that Oldowan hominins acquired and processed numerous, relatively complete, small ungulate carcasses. Moreover, they had at least occasional access to the fleshed remains of larger, wildebeest-sized animals. The overall record of hominin activities is consistent through the stratified sequence - spanning hundreds to thousands of years - and provides the earliest archaeological evidence of sustained hominin involvement with fleshed animal remains (i.e., persistent carnivory), a foraging adaptation central to many models of hominin evolution. C1 [Ferraro, Joseph V.; Binetti, Katie M.] Baylor Univ, Dept Anthropol, Waco, TX 76798 USA. [Ferraro, Joseph V.; Binetti, Katie M.] Baylor Univ, Inst Archaeol, Waco, TX 76798 USA. [Plummer, Thomas W.] Queens Coll, Dept Anthropol, Flushing, NY USA. [Plummer, Thomas W.] NYCEP, Flushing, NY USA. [Pobiner, Briana L.; Potts, Richard] Smithsonian Inst, Natl Museum Nat Hist, Human Origins Program, Washington, DC 20560 USA. [Oliver, James S.] Illinois State Museum, Dept Anthropol, Springfield, IL USA. [Oliver, James S.; Bishop, Laura C.] Liverpool John Moores Univ, Sch Nat Sci & Psychol, Res Ctr Evolutionary Anthropol & Palaeoecol, Liverpool L3 5UX, Merseyside, England. [Braun, David R.] George Washington Univ, Dept Anthropol, Washington, DC USA. [Ditchfield, Peter W.] Univ Oxford, Res Lab Archaeol & Hist Art, Oxford, England. [Seaman, John W., III; Seaman, John W., Jr.] Baylor Univ, Dept Stat Sci, Waco, TX 76798 USA. [Hertel, Fritz] Calif State Univ Northridge, Dept Biol, Northridge, CA 91330 USA. [Potts, Richard] Natl Museums Kenya, Dept Earth Sci, Palaeontol Sect, Nairobi, Kenya. RP Ferraro, JV (reprint author), Baylor Univ, Dept Anthropol, Waco, TX 76798 USA. EM joseph_ferraro@baylor.edu OI Bishop, Laura/0000-0002-4216-8667 FU National Science Foundation; Leakey Foundation; Wenner-Gren Foundation; National Geographic Society; Leverhulme Trust; University of California; Baylor University; City University of New York FX This research was supported by funding from the National Science Foundation, Leakey Foundation, Wenner-Gren Foundation, National Geographic Society, The Leverhulme Trust, University of California, Baylor University, and the City University of New York. Additional logistical support was provided by the Smithsonian Institution's Human Origins Program and the Peter Buck Fund for Human Origins Research, the British Institute in Eastern Africa, and the National Museums of Kenya. The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 94 TC 29 Z9 29 U1 10 U2 50 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 APR 25 PY 2013 VL 8 IS 4 AR e62174 DI 10.1371/journal.pone.0062174 PG 10 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 136DM UT WOS:000318341400041 PM 23637995 ER PT J AU Le Sage, D Arai, K Glenn, DR DeVience, SJ Pham, LM Rahn-Lee, L Lukin, MD Yacoby, A Komeili, A Walsworth, RL AF Le Sage, D. Arai, K. Glenn, D. R. DeVience, S. J. Pham, L. M. Rahn-Lee, L. Lukin, M. D. Yacoby, A. Komeili, A. Walsworth, R. L. TI Optical magnetic imaging of living cells SO NATURE LA English DT Article ID MAGNETOTACTIC BACTERIA; AMBIENT CONDITIONS; DIAMOND; SPIN; RESONANCE; ELECTRON; SENSOR AB Magnetic imaging is a powerful tool for probing biological and physical systems. However, existing techniques either have poor spatial resolution compared to optical microscopy and are hence not generally applicable to imaging of sub-cellular structure (for example, magnetic resonance imaging(1)), or entail operating conditions that preclude application to living biological samples while providing submicrometre resolution (for example, scanning superconducting quantum interference device microscopy(2), electron holography(3) and magnetic resonance force microscopy(4)). Here we demonstrate magnetic imaging of living cells (magnetotactic bacteria) under ambient laboratory conditions and with sub-cellular spatial resolution (400 nanometres), using an optically detected magnetic field imaging array consisting of a nanometre-scale layer of nitrogen-vacancy colour centres implanted at the surface of a diamond chip. With the bacteria placed on the diamond surface, we optically probe the nitrogen-vacancy quantum spin states and rapidly reconstruct images of the vector components of the magnetic field created by chains of magnetic nanoparticles (magnetosomes) produced in the bacteria. We also spatially correlate these magnetic field maps with optical images acquired in the same apparatus. Wide-field microscopy allows parallel optical and magnetic imaging of multiple cells in a population with submicrometre resolution and a field of view in excess of 100 micrometres. Scanning electron microscope images of the bacteria confirm that the correlated optical and magnetic images can be used to locate and characterize the magnetosomes in each bacterium. Our results provide a new capability for imaging bio-magnetic structures in living cells under ambient conditions with high spatial resolution, and will enable the mapping of a wide range of magnetic signals within cells and cellular networks(5,6). C1 [Le Sage, D.; Glenn, D. R.; Walsworth, R. L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Le Sage, D.; Glenn, D. R.; Lukin, M. D.; Yacoby, A.; Walsworth, R. L.] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. [Arai, K.] MIT, Dept Phys, Cambridge, MA 02139 USA. [Glenn, D. R.; Walsworth, R. L.] Harvard Univ, Ctr Brain Sci, Cambridge, MA 02138 USA. [DeVience, S. J.] Harvard Univ, Dept Chem & Chem Biol, Cambridge, MA 02138 USA. [Pham, L. M.] Harvard Univ, Sch Engn & Appl Sci, Cambridge, MA 02138 USA. [Rahn-Lee, L.; Komeili, A.] Univ Calif Berkeley, Dept Plant & Microbial Biol, Berkeley, CA 94720 USA. RP Walsworth, RL (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM rwalsworth@cfa.harvard.edu RI DeVience, Stephen/D-7274-2012; OI DeVience, Stephen/0000-0003-3142-7296; Le Sage, David/0000-0003-1678-9491 FU David and Lucille Packard Foundation Fellowship in Science and Engineering; National Institutes of Health [R01GM084122]; NSF; DARPA QuASAR programme FX We thank L. Qian for discussions about related experiments using a scanning SQUID microscope in the laboratory of K. A. Moler, J. W. Lichtman and R. Schalek for access to the SEM, S. G. Turney for access to the water-immersion objective and advice regarding cell immobilization, and P. R. Hemmer and H. Park for technical discussions. A. K. was supported by a David and Lucille Packard Foundation Fellowship in Science and Engineering and by the National Institutes of Health (R01GM084122). This work was supported by the NSF and the DARPA QuASAR programme. NR 32 TC 122 Z9 123 U1 40 U2 355 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 0028-0836 J9 NATURE JI Nature PD APR 25 PY 2013 VL 496 IS 7446 BP 486 EP U105 DI 10.1038/nature12072 PG 6 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 131HU UT WOS:000317984400037 PM 23619694 ER PT J AU Connolly, CB Au, YS Chae, E Tscherbul, TV Buchachenko, AA Lu, HI Ketterle, W Doyle, JM AF Connolly, Colin Bryant Au, Yat Shan Chae, Eunmi Tscherbul, Timur V. Buchachenko, Alexei A. Lu, Hsin-I Ketterle, Wolfgang Doyle, John M. TI Spin-Orbit Suppression of Cold Inelastic Collisions of Aluminum and Helium SO PHYSICAL REVIEW LETTERS LA English DT Article ID EARTH ATOMS AB We present a quantitative study of suppression of cold inelastic collisions by the spin-orbit interaction. We prepare cold ensembles of >10(11) Al(P-2(1/2)) atoms via cryogenic buffer-gas cooling and use a single-beam optical pumping method to measure their magnetic (mJ-changing) and fine-structure (J-changing) collisions with He-3 atoms at millikelvin temperatures over a range of magnetic fields from 0.5 to 6 T. The experimentally determined rates are in good agreement with the functional form predicted by quantum scattering calculations using ab initio potentials. This comparison provides direct experimental evidence for a proposed model of suppressed inelasticity in collisions of atoms in P-2(1/2) states [T. V. Tscherbul et al., Phys. Rev. A 80, 040701(R) (2009)], which may allow for sympathetic cooling of other P-2(1/2) atoms (e. g., In, Tl and metastable halogens). DOI: 10.1103/PhysRevLett.110.173202 C1 [Connolly, Colin Bryant; Au, Yat Shan; Chae, Eunmi; Doyle, John M.] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. [Ketterle, Wolfgang] MIT, Dept Phys, Cambridge, MA 02139 USA. [Connolly, Colin Bryant; Au, Yat Shan; Chae, Eunmi; Tscherbul, Timur V.; Lu, Hsin-I; Ketterle, Wolfgang; Doyle, John M.] Harvard MIT Ctr Ultracold Atoms, Cambridge, MA 02138 USA. [Tscherbul, Timur V.] Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom Mol & Opt Phys, Cambridge, MA 02138 USA. [Tscherbul, Timur V.] Univ Toronto, Dept Chem, Chem Phys Theory Grp, Toronto, ON M5S 3H6, Canada. [Buchachenko, Alexei A.] Moscow MV Lomonosov State Univ, Dept Chem, Moscow 119991, Russia. [Buchachenko, Alexei A.] Russian Acad Sci, Inst Problems Chem Phys, Chernogolovka 142432, Moscow District, Russia. [Lu, Hsin-I] Harvard Univ, Sch Engn & Appl Sci, Cambridge, MA 02138 USA. RP Connolly, CB (reprint author), Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. RI Buchachenko, Alexei/C-8452-2012; Tscherbul, Timur/K-3286-2014 OI Buchachenko, Alexei/0000-0003-0701-5531; Tscherbul, Timur/0000-0001-5689-040X FU NSF [PHY-1067990]; Harvard/MIT Center for Ultracold Atoms; RFBR [11-03-00081] FX This work was supported by the NSF under Grant No. PHY-1067990 and through the Harvard/MIT Center for Ultracold Atoms, and by RFBR under Project No. 11-03-00081. NR 29 TC 3 Z9 3 U1 1 U2 20 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 APR 23 PY 2013 VL 110 IS 17 AR 173202 DI 10.1103/PhysRevLett.110.173202 PG 5 WC Physics, Multidisciplinary SC Physics GA 130KT UT WOS:000317915200013 PM 23679723 ER PT J AU Chornock, R Berger, E Rest, A Milisavljevic, D Lunnan, R Foley, RJ Soderberg, AM Smartt, SJ Burgasser, AJ Challis, P Chomiuk, L Czekala, I Drout, M Fong, W Huber, ME Kirshner, RP Leibler, C McLeod, B Marion, GH Narayan, G Riess, AG Roth, KC Sanders, NE Scolnic, D Smith, K Stubbs, CW Tonry, JL Valenti, S Burgett, WS Chambers, KC Hodapp, KW Kaiser, N Kudritzki, RP Magnier, EA Price, PA AF Chornock, R. Berger, E. Rest, A. Milisavljevic, D. Lunnan, R. Foley, R. J. Soderberg, A. M. Smartt, S. J. Burgasser, A. J. Challis, P. Chomiuk, L. Czekala, I. Drout, M. Fong, W. Huber, M. E. Kirshner, R. P. Leibler, C. McLeod, B. Marion, G. H. Narayan, G. Riess, A. G. Roth, K. C. Sanders, N. E. Scolnic, D. Smith, K. Stubbs, C. W. Tonry, J. L. Valenti, S. Burgett, W. S. Chambers, K. C. Hodapp, K. W. Kaiser, N. Kudritzki, R. -P. Magnier, E. A. Price, P. A. TI PS1-10afx AT z=1.388: PAN-STARRS1 DISCOVERY OF A NEW TYPE OF SUPERLUMINOUS SUPERNOVA SO ASTROPHYSICAL JOURNAL LA English DT Article DE supernovae: individual (PS1-10afx); surveys ID HUBBLE-SPACE-TELESCOPE; GAMMA-RAY BURST; CORE-COLLAPSE SUPERNOVAE; DIGITAL SKY SURVEY; IA SUPERNOVAE; LIGHT CURVES; LUMINOUS SUPERNOVAE; SHOCK BREAKOUT; STAR-FORMATION; IC SUPERNOVAE AB We present the Pan-STARRS1 discovery of PS1-10afx, a unique hydrogen-deficient superluminous supernova (SLSN) at redshift z = 1.388. The light curve peaked at z(P1) = 21.7 mag, making PS1-10afx comparable to the most luminous known SNe, with M-u = -22.3 mag. Our extensive optical and near-infrared observations indicate that the bolometric light curve of PS1-10afx rose on the unusually fast timescale of similar to 12 days to the extraordinary peak luminosity of 4.1 x 10(44) erg s(-1) (M-bol = -22.8 mag) and subsequently faded rapidly. Equally important, the spectral energy distribution is unusually red for an SLSN, with a color temperature of similar to 6800 K near maximum light, in contrast to previous hydrogen-poor SLSNe, which are bright in the ultraviolet (UV). The spectra more closely resemble those of a normal SN Ic than any known SLSN, with a photospheric velocity of similar to 11,000 km s(-1) and evidence for line blanketing in the rest-frame UV. Despite the fast rise, these parameters imply a very large emitting radius (greater than or similar to 5 x 10(15) cm). We demonstrate that no existing theoretical model can satisfactorily explain this combination of properties: (1) a nickel-powered light curve cannot match the combination of high peak luminosity with the fast timescale; (2) models powered by the spindown energy of a rapidly rotating magnetar predict significantly hotter and faster ejecta; and (3) models invoking shock breakout through a dense circumstellar medium cannot explain the observed spectra or color evolution. The host galaxy is well detected in pre-explosion imaging with a luminosity near L*, a star formation rate of similar to 15 M-circle dot yr(-1), and is fairly massive (similar to 2 x 10(10) M-circle dot), with a stellar population age of similar to 10(8) yr, also in contrast to the young dwarf hosts of known hydrogen-poor SLSNe. PS1-10afx is distinct from known examples of SLSNe in its spectra, colors, light-curve shape, and host galaxy properties, suggesting that it resulted from a different channel than other hydrogen-poor SLSNe. C1 [Chornock, R.; Berger, E.; Milisavljevic, D.; Lunnan, R.; Foley, R. J.; Soderberg, A. M.; Challis, P.; Czekala, I.; Drout, M.; Fong, W.; Kirshner, R. P.; McLeod, B.; Marion, G. H.; Narayan, G.; Sanders, N. E.; Stubbs, C. W.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Rest, A.; Riess, A. G.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Smartt, S. J.; Smith, K.] Queens Univ Belfast, Sch Math & Phys, Astrophys Res Ctr, Belfast BT7 1NN, Antrim, North Ireland. [Burgasser, A. J.] Univ Calif San Diego, Ctr Astrophys & Space Sci, La Jolla, CA 92093 USA. [Chomiuk, L.] Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA. [Huber, M. E.; Tonry, J. L.; Burgett, W. S.; Chambers, K. C.; Hodapp, K. W.; Kaiser, N.; Kudritzki, R. -P.; Magnier, E. A.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Leibler, C.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95060 USA. [Riess, A. G.; Scolnic, D.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Roth, K. C.] Gemini Observ, Hilo, HI 96720 USA. [Stubbs, C. W.] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. [Valenti, S.] Las Cumbres Observ Global Telescope Network Inc, Goleta, CA 93117 USA. [Valenti, S.] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA. [Price, P. A.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. RP Chornock, R (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM rchornock@cfa.harvard.edu RI Stubbs, Christopher/C-2829-2012; OI Stubbs, Christopher/0000-0003-0347-1724; Lunnan, Ragnhild/0000-0001-9454-4639; Narayan, Gautham/0000-0001-6022-0484; Czekala, Ian/0000-0002-1483-8811; Chambers, Kenneth /0000-0001-6965-7789 FU European Research Council under the European Union [291222]; National Aeronautics and Space Administration issued through the Planetary Science Division of the NASA Science Mission Directorate [NNX08AR22G]; Gemini Observatory [GN-2010B-Q-5, GS-2010B-Q-4, GN-2010B-DD-2]; NASA [NAS5-26555]; [GO-5623]; [GO-9114] FX This paper includes data gathered with the 6.5 m Magellan Telescopes located at Las Campanas Observatory, Chile. We thank the staffs at PS1, Gemini, Magellan, and the VLT for their assistance with performing these observations. We are grateful for the grants of DD time at Gemini and the VLT. We acknowledge J. Strader for obtaining some FourStar observations, as well as the MMIRS observers who helped obtained some of the data here during the fall 2010 queue observations: M. Kriek, I. Labbe, J. Roll, D. Sand, and S. Wuyts. S.J.S. acknowledges funding from the European Research Council under the European Union's Seventh Framework Programme (FP7/2007-2013)/ERC Grant agreement No. 291222. The Pan-STARRS1 Surveys (PS1) have been made possible through contributions of the Institute for Astronomy, the University of Hawaii, the Pan-STARRS Project Office, the Max-Planck Society and its participating institutes, the Max Planck Institute for Astronomy, Heidelberg and the Max Planck Institute for Extraterrestrial Physics, Garching, The Johns Hopkins University, Durham University, the University of Edinburgh, Queen's University Belfast, the Harvard-Smithsonian Center for Astrophysics, the Las Cumbres Observatory Global Telescope Network Incorporated, the National Central University of Taiwan, the Space Telescope Science Institute, and the National Aeronautics and Space Administration under grant No. NNX08AR22G issued through the Planetary Science Division of the NASA Science Mission Directorate. Some observations were obtained under Program IDs GN-2010B-Q-5 (PI: Berger), GS-2010B-Q-4 (PI: Berger), and GN-2010B-DD-2 (PI: Chornock) at the Gemini Observatory, which is operated by the Association of Universities for Research in Astronomy, Inc., under a cooperative agreement with the NSF on behalf of the Gemini partnership: the National Science Foundation (United States), the Science and Technology Facilities Council (United Kingdom), the National Research Council (Canada), CONICYT (Chile), the Australian Research Council (Australia), Ministerio da Ciencia, Tecnologia e Inovacao (Brazil) and Ministerio de Ciencia, Tecnologia e Innovacion Productiva (Argentina). Some observations were collected at the European Organisation for Astronomical Research in the Southern Hemisphere, Chile under DDT programme 286.D-5005 (PI: Smartt). The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. Some of the archival data presented in this paper were taken under programs GO-5623 and GO-9114 (PI: Kirshner) and were obtained from the Mikulski Archive for Space Telescopes (MAST). STScI is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555. Some of the computations in this paper were run on the Odyssey cluster supported by the FAS Science Division Research Computing Group at Harvard University. NR 123 TC 30 Z9 30 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 APR 20 PY 2013 VL 767 IS 2 AR 162 DI 10.1088/0004-637X/767/2/162 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 122VR UT WOS:000317346800065 ER PT J AU Cool, RJ Moustakas, J Blanton, MR Burles, SM Coil, AL Eisenstein, DJ Wong, KC Zhu, GT Aird, J Bernstein, RA Bolton, AS Hogg, DW Mendez, AJ AF Cool, Richard J. Moustakas, John Blanton, Michael R. Burles, Scott M. Coil, Alison L. Eisenstein, Daniel J. Wong, Kenneth C. Zhu, Guangtun Aird, James Bernstein, Rebecca A. Bolton, Adam S. Hogg, David W. Mendez, Alexander J. TI THE PRISM MULTI-OBJECT SURVEY (PRIMUS). II. DATA REDUCTION AND REDSHIFT FITTING SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: distances and redshifts; galaxies: evolution; galaxies: high-redshift; large-scale structure of universe; surveys ID DIGITAL SKY SURVEY; VLT DEEP SURVEY; STAR-FORMATION; SPECTRA; PRIMUS; SPECTROSCOPY; GALAXIES; AGN AB The PRIsm MUlti-object Survey (PRIMUS) is a spectroscopic galaxy redshift survey to z similar to 1 completed with a low-dispersion prism and slitmasks allowing for simultaneous observations of similar to 2500 objects over 0.18 deg2. The final PRIMUS catalog includes similar to 130,000 robust redshifts over 9.1 deg(2). In this paper, we summarize the PRIMUS observational strategy and present the data reduction details used to measure redshifts, redshift precision, and survey completeness. The survey motivation, observational techniques, fields, target selection, slitmask design, and observations are presented in Coil et al. Comparisons to existing higher-resolution spectroscopic measurements show a typical precision of sigma(z)/(1 + z) = 0.005. PRIMUS, both in area and number of redshifts, is the largest faint galaxy redshift survey completed to date and is allowing for precise measurements of the relationship between active galactic nuclei and their hosts, the effects of environment on galaxy evolution, and the build up of galactic systems over the latter half of cosmic history. C1 [Cool, Richard J.] MMT Observ, Tucson, AZ 85721 USA. [Moustakas, John] Siena Coll, Dept Phys, Loudonville, NY 12211 USA. [Blanton, Michael R.; Hogg, David W.] 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.; Aird, James; Mendez, Alexander J.] Univ Calif San Diego, Ctr Astrophys & Space Sci, Dept Phys, San Diego, CA 92093 USA. [Eisenstein, Daniel J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Wong, Kenneth C.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Zhu, Guangtun] Johns Hopkins Univ, Dept Phys & Astron, Ctr Astrophys Sci, Baltimore, MD 21218 USA. [Bernstein, Rebecca A.] Univ Calif Santa Cruz, UCA Lick Observ, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. [Bolton, Adam S.] Univ Utah, Dept Phys & Astron, Salt Lake City, UT 84112 USA. RP Cool, RJ (reprint author), MMT Observ, Tucson, AZ 85721 USA. RI Zhu, Guangtun/C-8552-2012; OI Zhu, Guangtun/0000-0002-7574-8078; Hogg, David/0000-0003-2866-9403 FU NSF [AST-0607701, 0908246, 0908442, 0908354]; NASA [08-ADP08-0019, NAS 5-26555]; NASA through Hubble Fellowship [HF-01217] FX This paper includes data gathered with the 6.5 m 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. Some of the data used for this project is from the CFHTLS public data release, which includes 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. This work is based in part on data products produced at TERAPIX and the Canadian Astronomy Data Centre as part of the Canada-France-Hawaii Telescope Legacy Survey, a collaborative project of NRC and CNRS. Funding for PRIMUS has been provided by NSF grants AST-0607701, 0908246, 0908442, 0908354, and NASA grant 08-ADP08-0019. R. J. C. was supported 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. NR 21 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 APR 20 PY 2013 VL 767 IS 2 AR 118 DI 10.1088/0004-637X/767/2/118 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 122VR UT WOS:000317346800021 ER PT J AU Cranmer, SR van Ballegooijen, AA Woolsey, LN AF Cranmer, Steven R. van Ballegooijen, Adriaan A. Woolsey, Lauren N. TI CONNECTING THE SUN'S HIGH-RESOLUTION MAGNETIC CARPET TO THE TURBULENT HELIOSPHERE SO ASTROPHYSICAL JOURNAL LA English DT Article DE interplanetary medium; magnetohydrodynamics (MHD); solar wind; Sun: corona; Sun: magnetic topology; turbulence ID FAST SOLAR-WIND; SOLIS VECTOR-SPECTROMAGNETOGRAPH; ADVANCED-COMPOSITION-EXPLORER; PRESSURE-BALANCED STRUCTURES; ELECTRON HEAT-CONDUCTION; G-BAND BRIGHT; QUIET-SUN; CORONAL HOLES; ALFVEN WAVES; 1 AU AB The solar wind is connected to the Sun's atmosphere by flux tubes that are rooted in an ever-changing pattern of positive and negative magnetic polarities on the surface. Observations indicate that the magnetic field is filamentary and intermittent across a wide range of spatial scales. However, we do not know to what extent the complex flux-tube topology seen near the Sun survives as the wind expands into interplanetary space. In order to study the possible long-distance connections between the corona and the heliosphere, we developed new models of turbulence-driven solar wind acceleration along empirically constrained field lines. We used a potential field model of the quiet Sun to trace field lines into the ecliptic plane with unprecedented spatial resolution at their footpoints. For each flux tube, a one-dimensional model was created with an existing wave/turbulence code that solves equations of mass, momentum, and energy conservation from the photosphere to 4 AU. To take account of stream-stream interactions between flux tubes, we used those models as inner boundary conditions for a time-steady magnetohydrodynamic description of radial and longitudinal structure in the ecliptic. Corotating stream interactions smear out much of the smallest-scale variability, making it difficult to see how individual flux tubes on granular or supergranular scales can survive out to 1 AU. However, our models help clarify the level of "background" variability with which waves and turbulent eddies should be expected to interact. Also, the modeled fluctuations in magnetic field magnitude were seen to match measured power spectra quite well. C1 [Cranmer, Steven R.; van Ballegooijen, Adriaan A.; Woolsey, Lauren N.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Cranmer, SR (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. OI van Ballegooijen, Adriaan/0000-0002-5622-3540 FU National Aeronautics and Space Administration (NASA) [NNX09AB27G, NNX10AC11G] FX The authors gratefully acknowledge Bill Matthaeus, Spiro Antiochos, Zoran Mikic, Aaron Roberts, and the anonymous referee for valuable discussions. This work was supported by the National Aeronautics and Space Administration (NASA) under grants NNX09AB27G and NNX10AC11G to the Smithsonian Astrophysical Observatory. The SOLIS data used in this paper are produced cooperatively by NSF/NSO and NASA/LWS. The OMNI solar wind data were obtained from the GSFC/SPDF OMNIWeb interface, and we thank Dave McComas and Ruth Skoug (ACE/SWEPAM) and Chuck Smith and Norm Ness (ACE/MAG) for providing the majority of the OMNI measurements that were used in this paper. NR 137 TC 10 Z9 10 U1 0 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 APR 20 PY 2013 VL 767 IS 2 AR 125 DI 10.1088/0004-637X/767/2/125 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 122VR UT WOS:000317346800028 ER PT J AU Giannini, T Lorenzetti, D De Luca, M Strafella, F Elia, D Maiolo, B Marengo, M Maruccia, Y Massi, F Nisini, B Olmi, L Salama, A Smith, HA AF Giannini, T. Lorenzetti, D. De Luca, M. Strafella, F. Elia, D. Maiolo, B. Marengo, M. Maruccia, Y. Massi, F. Nisini, B. Olmi, L. Salama, A. Smith, H. A. TI SPITZER-IRAC SURVEY OF MOLECULAR JETS IN VELA-D SO ASTROPHYSICAL JOURNAL LA English DT Article DE infrared: stars; ISM: clouds; ISM: individual objects (Vela Molecular Ridge); ISM: jets and outflows; stars: formation; surveys ID YOUNG STELLAR OBJECTS; INFRARED ARRAY CAMERA; CLASS-I SOURCES; 2-DIMENSIONAL RADIATIVE-TRANSFER; SPECTRAL ENERGY-DISTRIBUTIONS; EXTENDED GREEN OBJECTS; RIDGE-CLOUD-D; STAR-FORMATION; PROTOSTELLAR JETS; HYDROGEN EMISSION AB We present a survey of H-2 jets from young protostars in the Vela-D molecular cloud (VMR-D), based on Spitzer-IRAC data between 3.6 mu m and 8.0 mu m. Our search has led to the identification of 15 jets (two new discoveries) and about 70 well-aligned knots within 1.2 deg(2). We compare the Infrared Array Camera (IRAC) maps with observations of the H-2 1-0 S(1) line at 2.12 mu m, with a Spitzer-MIPS map at 24 mu m and 70 mu m, and with a map of the dust continuum emission at 1.2 mm. From such a comparison, we find a tight association between molecular jets and dust peaks. The jet candidate exciting sources have been searched for in the published catalog of the young stellar objects of VMR-D. In particular, we searched for all the sources of Class II or (preferentially) earlier which are located close to the jet center and aligned with it. Furthermore, the association between jet and exciting source was validated by estimating the differential extinction between the jet opposite lobes. We are able to find a best-candidate exciting source in all but two jets, for which two alternative candidates are given. Four exciting sources are not (or very barely) observed at wavelengths shorter than 24 mu m, suggesting that they are very young protostars. Three of them are also associated with the most compact jets (projected length less than or similar to 0.1 pc). The exciting source spectral energy distributions (SEDs) have been constructed and modeled by means of all the available photometric data between 1.2 mu m and 1.2 mm. From SEDs fits, we derive the main source parameters, which indicate that most of them are low-mass protostars. A significant correlation is found between the projected jet length and the [24]-[70] color, which is consistent with an evolutionary scenario according to which shorter jets are associated with younger sources. A rough correlation is found between IRAC line cooling and exciting source bolometric luminosity, in agreement with the previous literature. The emerging trend suggests that mass loss and mass accretion are tightly related phenomena and that both decrease with time. C1 [Giannini, T.; Lorenzetti, D.; Nisini, B.; Salama, A.] INAF Osservatorio Astron Roma, I-00040 Monte Porzio Catone, Italy. [De Luca, M.] UPMC UCP, Ecole Normale Super, Observ Paris, LERMA LRA,UMR CNRS 8112, F-75231 Paris 05, France. [Strafella, F.; Maiolo, B.; Maruccia, Y.] Univ Salento, Dipartimento Matemat & Fis, I-73100 Lecce, Italy. [Elia, D.] INAF Ist Astrofis & Planetol Spaziali, I-00133 Rome, Italy. [Marengo, M.] Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA. [Massi, F.] INAF Osservatorio Astrofis Arcetri, I-50125 Florence, Italy. [Olmi, L.] Univ Puerto Rico, Dept Phys, UPR Stn, San Juan, PR 00936 USA. [Smith, H. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Giannini, T (reprint author), INAF Osservatorio Astron Roma, Via Frascati 33, I-00040 Monte Porzio Catone, Italy. OI Lorenzetti, Dario/0000-0001-6415-4162; Giannini, Teresa/0000-0002-0224-096X; Massi, Fabrizio/0000-0001-6407-8032; Olmi, Luca/0000-0002-1162-7947; Elia, Davide/0000-0002-9120-5890; , Brunella Nisini/0000-0002-9190-0113 NR 66 TC 6 Z9 6 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 APR 20 PY 2013 VL 767 IS 2 AR 147 DI 10.1088/0004-637X/767/2/147 PG 22 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 122VR UT WOS:000317346800050 ER PT J AU Guo, H Zehavi, I Zheng, Z Weinberg, DH Berlind, AA Blanton, M Chen, YM Eisenstein, DJ Ho, S Kazin, E Manera, M Maraston, C McBride, CK Nuza, SE Padmanabhan, N Parejko, JK Percival, WJ Ross, AJ Ross, NP Samushia, L Sanchez, AG Schlegel, DJ Schneider, DP Skibba, RA Swanson, MEC Tinker, JL Tojeiro, R Wake, DA White, M Bahcall, NA Bizyaev, D Brewington, H Bundy, K da Costa, LNA Ebelke, G Malanushenko, E Malanushenko, V Oravetz, D Rossi, G Simmons, A Snedden, S Streblyanska, A Thomas, D AF Guo, Hong Zehavi, Idit Zheng, Zheng Weinberg, David H. Berlind, Andreas A. Blanton, Michael Chen, Yanmei Eisenstein, Daniel J. Ho, Shirley Kazin, Eyal Manera, Marc Maraston, Claudia McBride, Cameron K. Nuza, Sebastian E. Padmanabhan, Nikhil Parejko, John K. Percival, Will J. Ross, Ashley J. Ross, Nicholas P. Samushia, Lado Sanchez, Ariel G. Schlegel, David J. Schneider, Donald P. Skibba, Ramin A. Swanson, Molly E. C. Tinker, Jeremy L. Tojeiro, Rita Wake, David A. White, Martin Bahcall, Neta A. Bizyaev, Dmitry Brewington, Howard Bundy, Kevin da Costa, Luiz N. A. Ebelke, Garrett Malanushenko, Elena Malanushenko, Viktor Oravetz, Daniel Rossi, Graziano Simmons, Audrey Snedden, Stephanie Streblyanska, Alina Thomas, Daniel TI THE CLUSTERING OF GALAXIES IN THE SDSS-III BARYON OSCILLATION SPECTROSCOPIC SURVEY: LUMINOSITY AND COLOR DEPENDENCE AND REDSHIFT EVOLUTION SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology: observations; cosmology: theory; galaxies: distances and redshifts; galaxies: halos galaxies: statistics; large-scale structure of universe ID DIGITAL SKY SURVEY; HALO OCCUPATION DISTRIBUTION; DARK-MATTER HALOES; 2-POINT CORRELATION-FUNCTION; MEDIUM-BAND SURVEY; VLT DEEP SURVEY; RED GALAXIES; SPECTRAL TYPE; 2DF-SDSS LRG; ACOUSTIC-OSCILLATIONS AB We measure the luminosity and color dependence and the redshift evolution of galaxy clustering in the Sloan Digital Sky Survey-III Baryon Oscillation Spectroscopic Survey Ninth Data Release. We focus on the projected two-point correlation function (2PCF) of subsets of its CMASS sample, which includes about 260,000 galaxies over similar to 3300 deg(2) in the redshift range 0.43 < z < 0.7. To minimize the selection effect on galaxy clustering, we construct well-defined luminosity and color subsamples by carefully accounting for the CMASS galaxy selection cuts. The 2PCF of the whole CMASS sample, if approximated by a power-law, has a correlation length of r(0) = 7.93 +/- 0.06 h(-1) Mpc and an index of gamma = 1.85 +/- 0.01. Clear dependences on galaxy luminosity and color are found for the projected 2PCF in all redshift bins, with more luminous and redder galaxies generally exhibiting stronger clustering and steeper 2PCF. The color dependence is also clearly seen for galaxies within the red sequence, consistent with the behavior of SDSS-II main sample galaxies at lower redshifts. At a given luminosity (k + e corrected), no significant evolution of the projected 2PCFs with redshift is detected for red sequence galaxies. We also construct galaxy samples of fixed number density at different redshifts, using redshiftdependent magnitude thresholds. The clustering of these galaxies in the CMASS redshift range is found to be consistent with that predicted by passive evolution. Our measurements of the luminosity and color dependence and redshift evolution of galaxy clustering will allow for detailed modeling of the relation between galaxies and dark matter halos and new constraints on galaxy formation and evolution. C1 [Guo, Hong; Zehavi, Idit] Case Western Reserve Univ, Dept Astron, Cleveland, OH 44106 USA. [Guo, Hong; Zheng, Zheng] Univ Utah, Dept Phys & Astron, Salt Lake City, UT 84112 USA. [Weinberg, David H.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. [Weinberg, David H.] Ohio State Univ, CCAPP, Columbus, OH 43210 USA. [Berlind, Andreas A.] Vanderbilt Univ, Dept Phys & Astron, Nashville, TN 37235 USA. [Blanton, Michael; Tinker, Jeremy L.] NYU, Ctr Cosmol & Particle Phys, New York, NY 10003 USA. [Chen, Yanmei] Nanjing Univ, Dept Astron, Nanjing 210093, Jiangsu, Peoples R China. [Eisenstein, Daniel J.; McBride, Cameron K.; Swanson, Molly E. C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Ho, Shirley; Ross, Nicholas P.; Schlegel, David J.; White, Martin] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA. [Ho, Shirley] Carnegie Mellon Univ, Dept Phys, Pittsburgh, PA 15213 USA. [Kazin, Eyal] Swinburne Univ Technol, Ctr Astrophys & Supercomp, Hawthorn, Vic 3122, Australia. [Manera, Marc; Maraston, Claudia; Percival, Will J.; Ross, Ashley J.; Samushia, Lado; Tojeiro, Rita; Thomas, Daniel] Univ Portsmouth, Inst Cosmol & Gravitat, Portsmouth PO1 3FX, Hants, England. [Maraston, Claudia; Thomas, Daniel] SEPnet, South East Phys Network, Highfield, England. [Nuza, Sebastian E.] Leibniz Inst Astrophys Potsdam AIP, D-14482 Potsdam, Germany. [Padmanabhan, Nikhil; Parejko, John K.] Yale Univ, Dept Phys, New Haven, CT 06520 USA. [Samushia, Lado] Ilia State Univ, Natl Abastumani Astrophys Observ, GE-1060 Tbilisi, Rep of Georgia. [Sanchez, Ariel G.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Schneider, Donald P.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Schneider, Donald P.] Penn State Univ, Inst Gravitat & Cosmos, University Pk, PA 16802 USA. [Skibba, Ramin A.] Univ Calif San Diego, Ctr Astrophys & Space Sci, San Diego, CA 92093 USA. [Wake, David A.] Yale Univ, Dept Astron, New Haven, CT 06520 USA. [Wake, David A.] Univ Wisconsin, Dept Astron, Madison, WI 53706 USA. [White, Martin] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. [White, Martin] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Bahcall, Neta A.] Princeton Univ Observ, Princeton, NJ 08544 USA. [Bizyaev, Dmitry; Brewington, Howard; Ebelke, Garrett; Malanushenko, Elena; Malanushenko, Viktor; Oravetz, Daniel; Simmons, Audrey; Snedden, Stephanie] Apache Point Observ, Sunspot, NM 88349 USA. [Bundy, Kevin] Univ Tokyo, Kavli Inst Phys & Math Universe, Kashiwa, Chiba 2778582, Japan. [da Costa, Luiz N. A.] Observ Nacl, BR-20921400 Rio De Janeiro, RJ, Brazil. [da Costa, Luiz N. A.] Lab Interinst E Astron LineA, BR-20921400 Rio De Janeiro, RJ, Brazil. [Rossi, Graziano] CEA, Ctr Saclay, Irfu SPP, F-91191 Gif Sur Yvette, France. [Rossi, Graziano] Univ Paris 07, Paris Ctr Cosmol Phys PCCP, F-75205 Paris, France. [Rossi, Graziano] Univ Paris 07, Lab APC, F-75205 Paris, France. [Streblyanska, Alina] Inst Astrofis Canarias, E-38200 Tenerife, Spain. [Streblyanska, Alina] Univ La Laguna, Dept Astrofis, E-38206 Tenerife, Spain. RP Guo, H (reprint author), Case Western Reserve Univ, Dept Astron, Cleveland, OH 44106 USA. RI Guo, Hong/A-8084-2010; da Costa, Luiz Alberto/I-1326-2013; Guo, Hong/J-5797-2015; White, Martin/I-3880-2015 OI da Costa, Luiz Alberto/0000-0002-7731-277X; Guo, Hong/0000-0003-4936-8247; White, Martin/0000-0001-9912-5070 FU NSF [AST-0907947, AST-1055081, AST-0901965]; Alfred P. Sloan Foundation; National Science Foundation; U. S. Department of Energy Office of Science FX We thank Joanne Cohn, Peder Norberg, Rom ' an Scoccimarro, and Benjamin Weiner for helpful discussions. We thank the anonymous referee for useful comments. H. G., I. Z., and Z. Z. were supported by NSF grant AST-0907947. R. A. S. was supported by NSF grant AST-1055081 and MECS was supported by NSF grant AST-0901965.; Funding for SDSS-III has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, and the U. S. Department of Energy Office of Science. The SDSS-III Web site is http://www. sdss3. org/.; SDSS-III is managed by the Astrophysical Research Consortium for the Participating Institutions of the SDSS-III Collaboration including the University of Arizona, the Brazilian Participation Group, Brookhaven National Laboratory, University of Cambridge, Carnegie Mellon University, University of Florida, the French Participation Group, the German Participation Group, Harvard University, the Instituto de Astrofisica de Canarias, the Michigan State/Notre Dame/JINA Participation Group, Johns Hopkins University, Lawrence Berkeley National Laboratory, Max Planck Institute for Astrophysics, Max Planck Institute for Extraterrestrial Physics, New Mexico State University, New York University, Ohio State University, Pennsylvania State University, University of Portsmouth, Princeton University, the Spanish Participation Group, University of Tokyo, University of Utah, Vanderbilt University, University of Virginia, University of Washington, and Yale University. NR 113 TC 32 Z9 32 U1 1 U2 9 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD APR 20 PY 2013 VL 767 IS 2 AR 122 DI 10.1088/0004-637X/767/2/122 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 122VR UT WOS:000317346800025 ER PT J AU Hezaveh, YD Marrone, DP Fassnacht, CD Spilker, JS Vieira, JD Aguirre, JE Aird, KA Aravena, M Ashby, MLN Bayliss, M Benson, BA Bleem, LE Bothwell, M Brodwin, M Carlstrom, JE Chang, CL Chapman, SC Crawford, TM Crites, AT De Breuck, C de Haan, T Dobbs, MA Fomalont, EB George, EM Gladders, MD Gonzalez, AH Greve, TR Halverson, NW High, FW Holder, GP Holzapfel, WL Hoover, S Hrubes, JD Husband, K Hunter, TR Keisler, R Lee, AT Leitch, EM Lueker, M Luong-Van, D Malkan, M McIntyre, V McMahon, JJ Mehl, J Menten, KM Meyer, SS Mocanu, LM Murphy, EJ Natoli, T Padin, S Plagge, T Reichardt, CL Rest, A Ruel, J Ruhl, JE Sharon, K Schaffer, KK Shaw, L Shirokoff, E Stalder, B Staniszewski, Z Stark, AA Story, K Vanderlinde, K Weiss, A Welikala, N Williamson, R AF Hezaveh, Y. D. Marrone, D. P. Fassnacht, C. D. Spilker, J. S. Vieira, J. D. Aguirre, J. E. Aird, K. A. Aravena, M. Ashby, M. L. N. Bayliss, M. Benson, B. A. Bleem, L. E. Bothwell, M. Brodwin, M. Carlstrom, J. E. Chang, C. L. Chapman, S. C. Crawford, T. M. Crites, A. T. De Breuck, C. de Haan, T. Dobbs, M. A. Fomalont, E. B. George, E. M. Gladders, M. D. Gonzalez, A. H. Greve, T. R. Halverson, N. W. High, F. W. Holder, G. P. Holzapfel, W. L. Hoover, S. Hrubes, J. D. Husband, K. Hunter, T. R. Keisler, R. Lee, A. T. Leitch, E. M. Lueker, M. Luong-Van, D. Malkan, M. McIntyre, V. McMahon, J. J. Mehl, J. Menten, K. M. Meyer, S. S. Mocanu, L. M. Murphy, E. J. Natoli, T. Padin, S. Plagge, T. Reichardt, C. L. Rest, A. Ruel, J. Ruhl, J. E. Sharon, K. Schaffer, K. K. Shaw, L. Shirokoff, E. Stalder, B. Staniszewski, Z. Stark, A. A. Story, K. Vanderlinde, K. Weiss, A. Welikala, N. Williamson, R. TI ALMA OBSERVATIONS OF SPT-DISCOVERED, STRONGLY LENSED, DUSTY, STAR-FORMING GALAXIES SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: high-redshift; galaxies: starburst; gravitational lensing: strong; techniques: interferometric ID SOUTH-POLE TELESCOPE; SUBMILLIMETER GALAXIES; NUMBER COUNTS; HIGH-REDSHIFT; INTERSTELLAR-MEDIUM; INFRARED GALAXIES; GAS FRACTIONS; MOLECULAR GAS; FIELD; EVOLUTION AB We present Atacama Large Millimeter/submillimeter Array (ALMA) 860 mu m imaging of four high-redshift (z = 2.8-5.7) dusty sources that were detected using the South Pole Telescope (SPT) at 1.4 mm and are not seen in existing radio to far-infrared catalogs. At 1 ''.5 resolution, the ALMA data reveal multiple images of each submillimeter source, separated by 1 ''-3 '', consistent with strong lensing by intervening galaxies visible in near-IR imaging of these sources. We describe a gravitational lens modeling procedure that operates on the measured visibilities and incorporates self-calibration-like antenna phase corrections as part of the model optimization, which we use to interpret the source structure. Lens models indicate that SPT0346-52, located at z = 5.7, is one of the most luminous and intensely star-forming sources in the universe with a lensing corrected FIR luminosity of 3.7 x 10(13) L circle dot and star formation surface density of 4200M circle dot yr(-1) kpc(-2). We find magnification factors of 5 to 22, with lens Einstein radii of 1 ''.1-2 ''.0 and Einstein enclosed masses of 1.6-7.2 x 10(11)M circle dot. These observations confirm the lensing origin of these objects, allow us to measure their intrinsic sizes and luminosities, and demonstrate the important role that ALMA will play in the interpretation of lensed submillimeter sources. C1 [Hezaveh, Y. D.; de Haan, T.; Dobbs, M. A.; Holder, G. P.; Shaw, L.; Vanderlinde, K.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada. [Marrone, D. P.; Spilker, J. S.; Bothwell, M.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Fassnacht, C. D.] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA. [Vieira, J. D.; Lueker, M.; Padin, S.; Shirokoff, E.; Staniszewski, Z.] CALTECH, Pasadena, CA 91125 USA. [Aguirre, J. E.] Univ Penn, Philadelphia, PA 19104 USA. [Aird, K. A.; Hrubes, J. D.; Luong-Van, D.] Univ Chicago, Chicago, IL 60637 USA. [Aravena, M.; De Breuck, C.] European So Observ, D-85748 Garching, Germany. [Ashby, M. L. N.; Bayliss, M.; Stalder, B.; Stark, A. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Bayliss, M.; Ruel, J.] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. [Benson, B. A.; Bleem, L. E.; Carlstrom, J. E.; Chang, C. L.; Crawford, T. M.; Crites, A. T.; Gladders, M. D.; High, F. W.; Hoover, S.; Keisler, R.; Leitch, E. M.; McMahon, J. J.; Mehl, J.; Meyer, S. S.; Mocanu, L. M.; Natoli, T.; Padin, S.; Plagge, T.; Sharon, K.; Schaffer, K. K.; Story, K.; Williamson, R.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Benson, B. A.; Carlstrom, J. E.; Chang, C. L.; Hoover, S.; McMahon, J. J.; Meyer, S. S.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA. [Bleem, L. E.; Carlstrom, J. E.; Keisler, R.; Meyer, S. S.; Natoli, T.; Story, K.] Univ Chicago, Dept Phys, Chicago, IL 60637 USA. [Brodwin, M.] Univ Missouri, Dept Phys & Astron, Kansas City, MO 64110 USA. [Carlstrom, J. E.; Crawford, T. M.; Crites, A. T.; Gladders, M. D.; High, F. W.; Leitch, E. M.; Mehl, J.; Meyer, S. S.; Mocanu, L. M.; Padin, S.; Plagge, T.; Sharon, K.; Williamson, R.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. [Carlstrom, J. E.; Chang, C. L.] Argonne Natl Lab, Argonne, IL 60439 USA. [Chapman, S. C.] Dalhousie Univ, Dept Phys & Atmospher Sci, Halifax, NS B3H 3J5, Canada. [Chapman, S. C.; Husband, K.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Fomalont, E. B.; Hunter, T. R.] Natl Radio Astron Observ, Charlottesville, VA 22903 USA. [George, E. M.; Holzapfel, W. L.; Lee, A. T.; Reichardt, C. L.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. [Gonzalez, A. H.] Univ Florida, Dept Astron, Gainesville, FL 32611 USA. [Greve, T. R.] UCL, Dept Phys & Astron, London WC1E 6BT, England. [Halverson, N. W.] Univ Colorado, Dept Astrophys & Planetary Sci, Boulder, CO 80309 USA. [Halverson, N. W.] Univ Colorado, Dept Phys, Boulder, CO 80309 USA. [Lee, A. T.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Div Phys, Berkeley, CA 94720 USA. [Malkan, M.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. [McIntyre, V.] CSIRO, Australia Telescope Natl Facil, Epping, NSW 1710, Australia. [McMahon, J. J.] Univ Michigan, Dept Phys, Ann Arbor, MI 48109 USA. [Menten, K. M.; Weiss, A.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Murphy, E. J.] Observ Carnegie Inst Sci, Pasadena, CA 91101 USA. [Rest, A.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Ruhl, J. E.; Staniszewski, Z.] Case Western Reserve Univ, Dept Phys, Ctr Educ & Res Cosmol & Astrophys, Cleveland, OH 44106 USA. [Sharon, K.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Schaffer, K. K.] Sch Art Inst Chicago, Liberal Arts Dept, Chicago, IL 60603 USA. [Shaw, L.] Yale Univ, Dept Phys, New Haven, CT 06520 USA. [Welikala, N.] Univ Paris 11, Inst Astrophys Spatiale, F-91405 Orsay, France. [Welikala, N.] CNRS, F-91405 Orsay, France. RP Hezaveh, YD (reprint author), McGill Univ, Dept Phys, 3600 Rue Univ, Montreal, PQ H3A 2T8, Canada. RI Aravena, Manuel/O-2361-2014; Williamson, Ross/H-1734-2015; Holzapfel, William/I-4836-2015; OI Williamson, Ross/0000-0002-6945-2975; Marrone, Daniel/0000-0002-2367-1080; Aird, Kenneth/0000-0003-1441-9518; Reichardt, Christian/0000-0003-2226-9169; De Breuck, Carlos/0000-0002-6637-3315; Hunter, Todd/0000-0001-6492-0090; Stark, Antony/0000-0002-2718-9996 FU National Science Foundation [ANT-0638937]; Kavli Foundation; Gordon and Betty Moore Foundation; NASA from the Space Telescope Science Institute [HST-GO-12659]; NSERC; CRC program; CIfAR; FQRNT through International Training Program and Doctoral Research scholarships; Science and Technologies Facilities Council; [PHY-1125897] FX The SPT is supported by the National Science Foundation through grant ANT-0638937, with partial support through PHY-1125897, the Kavli Foundation, and the Gordon and Betty Moore Foundation. This paper makes use of the following ALMA data: ADS/JAO. ALMA #2011.0.00957. S and #2011.0.00958. S. ALMA is a partnership of ESO (representing its member states), NSF (USA) and NINS (Japan), together with NRC (Canada) and NSC and ASIAA (Taiwan), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by ESO, AUI/NRAO and NAOJ. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. Partial support for this work was provided by NASA through grant HST-GO-12659 from the Space Telescope Science Institute and an award for Herschel analysis issued by JPL/Caltech for OT2_jvieira_5. Work at McGill is supported by NSERC, the CRC program, and CIfAR. Y.D.H. acknowledges the support of FQRNT through International Training Program and Doctoral Research scholarships. T.R.G. acknowledges support from the Science and Technologies Facilities Council. NR 62 TC 52 Z9 52 U1 1 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 APR 20 PY 2013 VL 767 IS 2 AR 132 DI 10.1088/0004-637X/767/2/132 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 122VR UT WOS:000317346800035 ER PT J AU Huber, D Chaplin, WJ Christensen-Dalsgaard, J Gilliland, RL Kjeldsen, H Buchhave, LA Fischer, DA Lissauer, JJ Rowe, JF Sanchis-Ojeda, R Basu, S Handberg, R Hekker, S Howard, AW Isaacson, H Karoff, C Latham, DW Lund, MN Lundkvist, M Marcy, GW Miglio, A Aguirre, VS Stello, D Arentoft, T Barclay, T Bedding, TR Burke, CJ Christiansen, JL Elsworth, YP Haas, MR Kawaler, SD Metcalfe, TS Mullally, F Thompson, SE AF Huber, Daniel Chaplin, William J. Christensen-Dalsgaard, Jorgen Gilliland, Ronald L. Kjeldsen, Hans Buchhave, Lars A. Fischer, Debra A. Lissauer, Jack J. Rowe, Jason F. Sanchis-Ojeda, Roberto Basu, Sarbani Handberg, Rasmus Hekker, Saskia Howard, Andrew W. Isaacson, Howard Karoff, Christoffer Latham, David W. Lund, Mikkel N. Lundkvist, Mia Marcy, Geoffrey W. Miglio, Andrea Aguirre, Victor Silva Stello, Dennis Arentoft, Torben Barclay, Thomas Bedding, Timothy R. Burke, Christopher J. Christiansen, Jessie L. Elsworth, Yvonne P. Haas, Michael R. Kawaler, Steven D. Metcalfe, Travis S. Mullally, Fergal Thompson, Susan E. TI FUNDAMENTAL PROPERTIES OF KEPLER PLANET-CANDIDATE HOST STARS USING ASTEROSEISMOLOGY SO ASTROPHYSICAL JOURNAL LA English DT Article DE planetary systems; stars: late-type; stars: oscillations; techniques: photometric; techniques: spectroscopic ID SOLAR-LIKE OSCILLATIONS; TRANSIT TIMING OBSERVATIONS; 1ST 4 MONTHS; STELLAR EVOLUTION DATABASE; FINE GUIDANCE SENSOR; MAIN-SEQUENCE STARS; RED-GIANT STARS; SUN-LIKE STAR; EXTRASOLAR PLANETS; INPUT CATALOG AB We have used asteroseismology to determine fundamental properties for 66 Kepler planet-candidate host stars, with typical uncertainties of 3% and 7% in radius and mass, respectively. The results include new asteroseismic solutions for four host stars with confirmed planets (Kepler-4, Kepler-14, Kepler-23 and Kepler-25) and increase the total number of Kepler host stars with asteroseismic solutions to 77. A comparison with stellar properties in the planet-candidate catalog by Batalha et al. shows that radii for subgiants and giants obtained from spectroscopic follow-up are systematically too low by up to a factor of 1.5, while the properties for unevolved stars are in good agreement. We furthermore apply asteroseismology to confirm that a large majority of cool main-sequence hosts are indeed dwarfs and not misclassified giants. Using the revised stellar properties, we recalculate the radii for 107 planet candidates in our sample, and comment on candidates for which the radii change from a previously giant-planet/brown-dwarf/stellar regime to a sub-Jupiter size or vice versa. A comparison of stellar densities from asteroseismology with densities derived from transit models in Batalha et al. assuming circular orbits shows significant disagreement for more than half of the sample due to systematics in the modeled impact parameters or due to planet candidates that may be in eccentric orbits. Finally, we investigate tentative correlations between host-star masses and planet-candidate radii, orbital periods, and multiplicity, but caution that these results may be influenced by the small sample size and detection biases. C1 [Huber, Daniel; Lissauer, Jack J.; Rowe, Jason F.; Barclay, Thomas; Burke, Christopher J.; Christiansen, Jessie L.; Haas, Michael R.; Mullally, Fergal; Thompson, Susan E.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Chaplin, William J.; Miglio, Andrea; Elsworth, Yvonne P.] Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England. [Chaplin, William J.; Christensen-Dalsgaard, Jorgen; Kjeldsen, Hans; Handberg, Rasmus; Karoff, Christoffer; Lund, Mikkel N.; Lundkvist, Mia; Aguirre, Victor Silva; Stello, Dennis; Arentoft, Torben; Bedding, Timothy R.] Aarhus Univ, Dept Phys & Astron, Stellar Astrophys Ctr, DK-8000 Aarhus C, Denmark. [Gilliland, Ronald L.] Penn State Univ, Ctr Exoplanets & Habitable Worlds, University Pk, PA 16802 USA. [Buchhave, Lars A.] Univ Copenhagen, Niels Bohr Inst, DK-2100 Copenhagen, Denmark. [Buchhave, Lars A.] Univ Copenhagen, Nat Hist Museum Denmark, Ctr Star & Planet Format, DK-1350 Copenhagen, Denmark. [Fischer, Debra A.; Basu, Sarbani] Yale Univ, Dept Astron, New Haven, CT 06511 USA. [Sanchis-Ojeda, Roberto] MIT, Dept Phys, Cambridge, MA 02139 USA. [Hekker, Saskia] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 XH Amsterdam, Netherlands. [Howard, Andrew W.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Isaacson, Howard; Marcy, Geoffrey W.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Latham, David W.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Stello, Dennis; Bedding, Timothy R.] Univ Sydney, Sch Phys, Sydney Inst Astron SIfA, Sydney, NSW 2006, Australia. [Kawaler, Steven D.] Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA. [Metcalfe, Travis S.] Space Sci Inst, Boulder, CO 80301 USA. RP Huber, D (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. EM daniel.huber@nasa.gov RI Howard, Andrew/D-4148-2015; OI Lund, Mikkel Norup/0000-0001-9214-5642; Lundkvist, Mia Sloth/0000-0002-8661-2571; Fischer, Debra/0000-0003-2221-0861; Handberg, Rasmus/0000-0001-8725-4502; Kawaler, Steven/0000-0002-6536-6367; Howard, Andrew/0000-0001-8638-0320; Bedding, Timothy/0000-0001-5943-1460; Buchhave, Lars A./0000-0003-1605-5666; Metcalfe, Travis/0000-0003-4034-0416; Karoff, Christoffer/0000-0003-2009-7965; Bedding, Tim/0000-0001-5222-4661; Basu, Sarbani/0000-0002-6163-3472 FU NASA's Science Mission Directorate; NSF [AST-1105930]; Netherlands Organisation for Scientific Research (NWO); NASA [NNX13AE91G]; Danish National Research Foundation [DNRF106]; ASTERISK project (ASTERoseismic Investigations with SONG and Kepler); European Research Council [267864] FX We thank Willie Torres, Josh Winn, and our anonymous referee for helpful comments and discussions. We furthermore gratefully acknowledge the entire Kepler team and everyone involved in the Kepler mission for making this paper possible. Funding for the Kepler mission is provided by NASA's Science Mission Directorate. D.H. is supported by an appointment to the NASA Postdoctoral Program at Ames Research Center, administered by Oak Ridge Associated Universities through a contract with NASA. S.B. acknowledges NSF grant AST-1105930. S.H. acknowledges financial support from the Netherlands Organisation for Scientific Research (NWO). T.S.M. acknowledges NASA grant NNX13AE91G. Funding for the Stellar Astrophysics Centre is provided by The Danish National Research Foundation (Grant DNRF106). The research is supported by the ASTERISK project (ASTERoseismic Investigations with SONG and Kepler) funded by the European Research Council (Grant agreement No.: 267864). NR 153 TC 108 Z9 108 U1 1 U2 6 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD APR 20 PY 2013 VL 767 IS 2 AR 127 DI 10.1088/0004-637X/767/2/127 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 122VR UT WOS:000317346800030 ER PT J AU Ingleby, L Calvet, N Herczeg, G Blaty, A Walter, F Ardila, D Alexander, R Edwards, S Espaillat, C Gregory, SG Hillenbrand, L Brown, A AF Ingleby, Laura Calvet, Nuria Herczeg, Gregory Blaty, Alex Walter, Frederick Ardila, David Alexander, Richard Edwards, Suzan Espaillat, Catherine Gregory, Scott G. Hillenbrand, Lynne Brown, Alexander TI ACCRETION RATES FOR T TAURI STARS USING NEARLY SIMULTANEOUS ULTRAVIOLET AND OPTICAL SPECTRA SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; stars: chromospheres; stars: pre-main sequence; ultraviolet: stars ID MAIN-SEQUENCE STARS; LOW MASS STARS; INFRARED PHOTOMETRIC VARIABILITY; ETA CHAMAELEONTIS CLUSTER; AURIGA MOLECULAR CLOUD; X-SHOOTER SPECTROSCOPY; MAGNETOSPHERIC ACCRETION; CHAMELEON-I; BROWN DWARFS; CHROMOSPHERIC EMISSION AB We analyze the accretion properties of 21 low-mass T Tauri stars using a data set of contemporaneous near-UV (NUV) through optical observations obtained with the Hubble Space Telescope Imaging Spectrograph and the ground-based Small and Medium Aperture Research Telescope System, a unique data set because of the nearly simultaneous broad wavelength coverage. Our data set includes accreting T Tauri stars in Taurus, Chamaeleon I, eta Chamaeleon, and the TW Hydra Association. For each source we calculate the accretion rate ((M) over dot) by fitting the NUV and optical excesses above the photosphere, produced in the accretion shock, introducing multiple accretion components characterized by a range in energy flux (or density) for the first time. This treatment is motivated by models of the magnetospheric geometry and accretion footprints, which predict that high-density, low filling factor accretion spots coexist with low-density, high filling factor spots. By fitting the UV and optical spectra with multiple accretion components, we can explain excesses which have been observed in the near-IR. Comparing our estimates of (M) over dot to previous estimates, we find some discrepancies; however, they may be accounted for when considering assumptions for the amount of extinction and variability in optical spectra. Therefore, we confirm many previous estimates of the accretion rate. Finally, we measure emission line luminosities from the same spectra used for the (M) over dot estimates, to produce correlations between accretion indicators (H beta, Ca II K, CII], and Mg II) and accretion properties obtained simultaneously. C1 [Ingleby, Laura; Calvet, Nuria; Blaty, Alex] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Herczeg, Gregory] Peking Univ, Kavli Inst Astron & Astrophys, Beijing 100871, Peoples R China. [Walter, Frederick] SUNY Stony Brook, Stony Brook, NY 11794 USA. [Ardila, David] CALTECH, NASA Herschel Sci Ctr, Pasadena, CA 91125 USA. [Alexander, Richard] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. [Edwards, Suzan] Smith Coll, Dept Astron, Northampton, MA 01063 USA. [Espaillat, Catherine] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Gregory, Scott G.; Hillenbrand, Lynne] CALTECH, Dept Astrophys, Pasadena, CA 91125 USA. [Gregory, Scott G.] Univ St Andrews, Sch Phys & Astron, St Andrews KY16 9SS, Fife, Scotland. [Brown, Alexander] Univ Colorado, Ctr Astrophys & Space Astron, Boulder, CO 80309 USA. RP Ingleby, L (reprint author), Univ Michigan, Dept Astron, 830 Dennison Bldg,500 Church St, Ann Arbor, MI 48109 USA. EM lingleby@umich.edu; ncalvet@umich.edu; ablaty@umich.edu OI Gregory, Scott/0000-0003-3674-5568; Herczeg, Gregory/0000-0002-7154-6065 FU NASA [11616, NAS 5-26555]; University of Colorado; Sagan Exoplanet Fellowship from NASA; Science and Technology Facilities Council (STFC) through an Advanced Fellowship [ST/G00711X/1]; STFC via a Ernest Rutherford Fellowship [ST/J003255/1] FX We thank Melissa McClure for valuable discussions regarding extinction estimates and veiling in the NIR and providing results prior to publication. We also thank Ted Bergin, Lee Hartmann, Jon Miller, and Fred Adams for providing comments on an early version of this paper as part of L. Ingleby's thesis. This work was supported by NASA grants for Guest Observer program 11616 to the University of Michigan, Caltech, and the University of Colorado. Based on observations made with the NASA/ESA Hubble Space Telescope, obtained from the Space Telescope Science Institute data archive. STScI is operated by the Association of Universities for Research in Astronomy, Inc. under NASA Contract NAS 5-26555. C. E. was supported by a Sagan Exoplanet Fellowship from NASA and administered by the NASA Exoplanet Science Institute. R. D. A. acknowledges support from the Science and Technology Facilities Council (STFC) through an Advanced Fellowship (ST/G00711X/1). S. G. G. acknowledges support from STFC via a Ernest Rutherford Fellowship (ST/J003255/1). NR 101 TC 57 Z9 57 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 APR 20 PY 2013 VL 767 IS 2 AR 112 DI 10.1088/0004-637X/767/2/112 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 122VR UT WOS:000317346800015 ER PT J AU Kuo, CY Braatz, JA Reid, MJ Lo, KY Condon, JJ Impellizzeri, CMV Henkel, C AF Kuo, C. Y. Braatz, J. A. Reid, M. J. Lo, K. Y. Condon, J. J. Impellizzeri, C. M. V. Henkel, C. TI THE MEGAMASER COSMOLOGY PROJECT. V. AN ANGULAR-DIAMETER DISTANCE TO NGC 6264 AT 140 Mpc SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; galaxies: active; galaxies: ISM; galaxies: nuclei; galaxies: Seyfert; masers ID ACTIVE GALAXY NGC-4258; GEOMETRIC DISTANCE; ACCELERATING UNIVERSE; DARK ENERGY; UGC 3789; SUPERNOVAE; CONSTANT; II. AB We present the direct measurement of the Hubble constant, yielding the direct measurement of the angular-diameter distance to NGC 6264 using the H2O megamaser technique. Our measurement is based on sensitive observations of the circumnuclear megamaser disk from four observations with the Very Long Baseline Array, the Green Bank Telescope (GBT), and the Effelsberg telescope. We also monitored the maser spectral profile for 2.3 years using the GBT to measure accelerations of maser lines by tracking their line-of-sight velocities as they change with time. The measured accelerations suggest that the systemic maser spots have a significantly wider radial distribution than in the archetypal megamaser in NGC 4258. We model the maser emission as arising from a circumnuclear disk with orbits dominated by the central black hole. The best fit of the data gives a Hubble constant of H-0 = 68 +/- 9 km s(-1) Mpc(-1), which corresponds to an angular-diameter distance of 144 +/- 19 Mpc. In addition, the fit also gives a mass of the central black hole of (3.09 +/- 0.42) x 10(7) M-circle dot. The result demonstrates the feasibility of measuring distances to galaxies located well into the Hubble flow by using circumnuclear megamaser disks. C1 [Kuo, C. Y.] Acad Sinica, Inst Astron & Astrophys, Taipei 10617, Taiwan. [Braatz, J. A.; Lo, K. Y.; Condon, J. J.; Impellizzeri, C. M. V.] Natl Radio Astron Observ, Charlottesville, VA 22903 USA. [Reid, M. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Henkel, C.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Henkel, C.] King Abdulaziz Univ, Fac Sci, Dept Astron, Jeddah, Saudi Arabia. RP Kuo, CY (reprint author), Acad Sinica, Inst Astron & Astrophys, POB 23-141, Taipei 10617, Taiwan. RI Faculty of, Sciences, KAU/E-7305-2017 NR 18 TC 18 Z9 18 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 APR 20 PY 2013 VL 767 IS 2 AR 155 DI 10.1088/0004-637X/767/2/155 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 122VR UT WOS:000317346800058 ER PT J AU Newman, SF Genzel, R Schreiber, NMF Griffin, KS Mancini, C Lilly, SJ Renzini, A Bouche, N Burkert, A Buschkamp, P Carollo, CM Cresci, G Davies, R Eisenhauer, F Genel, S Hicks, EKS Kurk, J Lutz, D Naab, T Peng, YJ Sternberg, A Tacconi, LJ Wuyts, S Zamorani, G Vergani, D AF Newman, Sarah F. Genzel, Reinhard Schreiber, Natascha M. Foerster Griffin, Kristen Shapiro Mancini, Chiara Lilly, Simon J. Renzini, Alvio Bouche, Nicolas Burkert, Andreas Buschkamp, Peter Carollo, C. Marcella Cresci, Giovanni Davies, Ric Eisenhauer, Frank Genel, Shy Hicks, Erin K. S. Kurk, Jaron Lutz, Dieter Naab, Thorsten Peng, Yingjie Sternberg, Amiel Tacconi, Linda J. Wuyts, Stijn Zamorani, Gianni Vergani, Daniela TI THE SINS/zC-SINF SURVEY OF z similar to 2 GALAXY KINEMATICS: THE NATURE OF DISPERSION-DOMINATED GALAXIES SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: evolution; galaxies: high-redshift; infrared: galaxies ID STAR-FORMING GALAXIES; INTEGRAL FIELD SPECTROSCOPY; MASS-METALLICITY RELATION; LYMAN-BREAK GALAXIES; TULLY-FISHER RELATION; ULTRA DEEP FIELD; HIGH-REDSHIFT; DISK GALAXIES; COSMOLOGICAL SIMULATIONS; STELLAR POPULATIONS AB We analyze the spectra, spatial distributions, and kinematics of Ha, [N II], and [ S II] emission in a sample of 38, z similar to 2.2 UV/optically selected star-forming galaxies (SFGs) from the SINS and zC-SINF surveys, 34 of which were observed in the adaptive optics mode of SINFONI and 30 of those contain data presented for the first time here. This is supplemented by kinematic data from 43 z similar to 1-2.5 galaxies from the literature. None of these 81 galaxies is an obvious major merger. We find that the kinematic classification of high-z SFGs as "dispersion dominated" or "rotation dominated" correlates most strongly with their intrinsic sizes. Smaller galaxies are more likely "dispersion-dominated" for two main reasons: (1) the rotation velocity scales linearly with galaxy size but intrinsic velocity dispersion does not depend on size or may even increase in smaller galaxies, and as such, their ratio is systematically lower for smaller galaxies, and (2) beam smearing strongly decreases large-scale velocity gradients and increases observed dispersion much more for galaxies with sizes at or below the resolution. Dispersion-dominated SFGs may thus have intrinsic properties similar to "rotation-dominated" SFGs, but are primarily more compact, lower mass, less metal enriched, and may have higher gas fractions, plausibly because they represent an earlier evolutionary state. C1 [Newman, Sarah F.; Genzel, Reinhard] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Genzel, Reinhard; Schreiber, Natascha M. Foerster; Buschkamp, Peter; Davies, Ric; Eisenhauer, Frank; Kurk, Jaron; Lutz, Dieter; Tacconi, Linda J.; Wuyts, Stijn] Max Planck Inst Extraterr Phys MPE, D-85748 Garching, Germany. [Genzel, Reinhard] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. [Griffin, Kristen Shapiro] Northrop Grumman Aerosp Syst, Space Sci Res Grp, Redondo Beach, CA 90278 USA. [Mancini, Chiara; Renzini, Alvio] Osserv Astron Padova, I-35122 Padua, Italy. [Lilly, Simon J.; Carollo, C. Marcella; Peng, Yingjie] ETH, Dept Phys, Inst Astron, CH-8093 Zurich, Switzerland. [Bouche, Nicolas] Univ Toulouse, UPS OMP, IRAP, Toulouse, France. [Bouche, Nicolas] CNRS, IRAP, F-31400 Toulouse, France. [Burkert, Andreas] Ludwig Maximilians Univ USM, Univ Sternwarte, D-81679 Munich, Germany. [Cresci, Giovanni] Osserv Astrofis Arcetri, Ist Nazl Astrofis, I-50125 Florence, Italy. [Genel, Shy] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Hicks, Erin K. S.] Univ Washington, Dept Astron, Seattle, WA 98195 USA. [Naab, Thorsten] Max Planck Inst Astrophys, D-85748 Garching, Germany. [Sternberg, Amiel] Tel Aviv Univ, Sch Phys & Astron, IL-69978 Tel Aviv, Israel. [Zamorani, Gianni] INAF Osservatorio Astron Bologna, I-40127 Bologna, Italy. [Vergani, Daniela] INAF Ist Astrofis Spaziale & Fis Cosm Bologna, I-40129 Bologna, Italy. RP Newman, SF (reprint author), Univ Calif Berkeley, Dept Astron, Campbell Hall, Berkeley, CA 94720 USA. EM sfnewman@berkeley.edu OI Vergani, Daniela/0000-0003-0898-2216; Cresci, Giovanni/0000-0002-5281-1417 FU NSF grfp grant; ASI grant "COFIS-Analisi Dati"; INAF grant "PRIN" FX We thank the referee for a detailed and thoughtful review which led to substantial improvements in the paper. We thank the ESO staff, especially those at Paranal Observatory, for their ongoing support during the many past and continuing observing runs over which the SINS project is being carried out. We also acknowledge the SINFONI and PARSEC teams, whose devoted work on the instrument and laser paved the way for the success of the SINS observations. S.F.N. is supported by an NSF grfp grant. C. M., A. R. and G.Z. acknowledge partial support by the ASI grant "COFIS-Analisi Dati" and by the INAF grant "PRIN-2008" and "PRIN-2010." NR 149 TC 51 Z9 51 U1 0 U2 7 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD APR 20 PY 2013 VL 767 IS 2 AR 104 DI 10.1088/0004-637X/767/2/104 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 122VR UT WOS:000317346800007 ER PT J AU Reid, MJ Braatz, JA Condon, JJ Lo, KY Kuo, CY Impellizzeri, CMV Henkel, C AF Reid, M. J. Braatz, J. A. Condon, J. J. Lo, K. Y. Kuo, C. Y. Impellizzeri, C. M. V. Henkel, C. TI THE MEGAMASER COSMOLOGY PROJECT. IV. A DIRECT MEASUREMENT OF THE HUBBLE CONSTANT FROM UGC 3789 SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmological parameters; dark energy; distance scale; galaxies: individual (UGC 3789); galaxies: nuclei; masers ID ACTIVE GALAXY NGC-4258; LUMINOUS RED GALAXIES; GEOMETRIC DISTANCE; SPACE-TELESCOPE; SFI++; SCALE; DISK; II. AB In Papers I and II from the Megamaser Cosmology Project, we reported initial observations of H2O masers in an accretion disk of a supermassive black hole at the center of the galaxy UGC 3789, which gave an angular-diameter distance to the galaxy and an estimate of H-0 with 16% uncertainty. We have since conducted more very long baseline interferometric observations of the spatial-velocity structure of these H2O masers, as well as continued monitoring of its spectrum to better measure maser accelerations. These more extensive observations, combined with improved modeling of the masers in the accretion disk of the central supermassive black hole, confirm our previous results, but with significantly improved accuracy. We find H-0 = 68.9 +/- 7.1 km s(-1) Mpc(-1); this estimate of H-0 is independent of other methods and is accurate to +/- 10%, including sources of systematic error. This places UGC 3789 at an angular-diameter distance of 49.6 +/- 5.1 Mpc, with a central supermassive black hole of (1.16 +/- 0.12) x 10(7) M-circle dot. C1 [Reid, M. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Braatz, J. A.; Condon, J. J.; Lo, K. Y.; Kuo, C. Y.; Impellizzeri, C. M. V.] Natl Radio Astron Observ, Charlottesville, VA 22903 USA. [Henkel, C.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Henkel, C.] King Abdulaziz Univ, Fac Sci, Dept Astron, Jeddah, Saudi Arabia. RP Reid, MJ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Faculty of, Sciences, KAU/E-7305-2017 NR 19 TC 29 Z9 29 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 APR 20 PY 2013 VL 767 IS 2 AR 154 DI 10.1088/0004-637X/767/2/154 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 122VR UT WOS:000317346800057 ER PT J AU Werner, N Oonk, JBR Canning, REA Allen, SW Simionescu, A Kos, J van Weeren, RJ Edge, AC Fabian, AC von der Linden, A Nulsen, PEJ Reynolds, CS Ruszkowski, M AF Werner, N. Oonk, J. B. R. Canning, R. E. A. Allen, S. W. Simionescu, A. Kos, J. van Weeren, R. J. Edge, A. C. Fabian, A. C. von der Linden, A. Nulsen, P. E. J. Reynolds, C. S. Ruszkowski, M. TI THE NATURE OF FILAMENTARY COLD GAS IN THE CORE OF THE VIRGO CLUSTER SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: clusters: intracluster medium; galaxies: individual (M87); infrared: ISM ID COOLING FLOW CLUSTERS; SPACE-TELESCOPE OBSERVATIONS; MOLECULAR-HYDROGEN EMISSION; FAR-INFRARED SPECTROSCOPY; ACTIVE GALACTIC NUCLEUS; TURBULENT MIXING LAYERS; H-ALPHA FILAMENTS; X-RAY-EMISSION; C-II LINE; CENTRAL GALAXIES AB We present a multi-wavelength study of the emission-line nebulae located similar to 38 '' (3 kpc in projection) southeast of the nucleus of M87, the central dominant galaxy of the Virgo Cluster. We report the detection of far-infrared (FIR) [C II] line emission at 158 mu m from the nebulae using observations made with the Herschel Photodetector Array Camera and Spectrometer (PACS). The infrared line emission is extended and co-spatial with optical H alpha+ [N II], far-ultraviolet C IV lines, and soft X-ray emission. The filamentary nebulae evidently contain multi-phase material spanning a temperature range of at least five orders of magnitude, from similar to 100 K to similar to 10(7) K. This material has most likely been uplifted by the active galactic nucleus from the center of M87. The thermal pressure of the 10(4) K phase appears to be significantly lower than that of the surrounding hot intracluster medium (ICM), indicating the presence of additional turbulent and magnetic pressure in the filaments. If the turbulence in the filaments is subsonic then the magnetic field strength required to balance the pressure of the surrounding ICM is B similar to 30-70 mu G. The spectral properties of the soft X-ray emission from the filaments indicate that it is due to thermal plasma with kT similar to 0.5-1 keV, which is cooling by mixing with the cold gas and/or radiatively. Charge exchange can be ruled out as a significant source of soft X-rays. Both cooling and mixing scenarios predict gas with a range of temperatures. This is at first glance inconsistent with the apparent lack of X-ray emitting gas with kT < 0.5 keV. However, we show that the missing very soft X-ray emission could be absorbed by the cold gas in the filaments with an integrated hydrogen column density of N-H similar to 1.6 x 10(21) cm(-2), providing a natural explanation for the apparent temperature floor to the X-ray emission at kT similar to 0.5 keV. The FIR through ultraviolet line emission is most likely primarily powered by the ICM particles penetrating the cold gas following a shearing induced mixing process. An additional source of energy may, in principle, be provided by X-ray photoionization from cooling X-ray emitting plasma. The relatively small line ratio of [O I]/[C II] < 7.2 indicates a large optical depth in the FIR lines. The large optical depth in the FIR lines and the intrinsic absorption inferred from the X-ray and optical data imply significant reservoirs of cold atomic and molecular gas distributed in filaments with small volume filling fraction, but large area covering factor. C1 [Werner, N.; Canning, R. E. A.; Allen, S. W.; Simionescu, A.; von der Linden, A.] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94305 USA. [Oonk, J. B. R.; Kos, J.] Netherlands Inst Radio Astron, ASTRON, NL-7990 AA Dwingeloo, Netherlands. [Allen, S. W.] SLAC Natl Accelerator Lab, Menlo Pk, CA 94025 USA. [Kos, J.] Univ Ljubljana, Fac Math & Phys, Ljubljana 1000, Slovenia. [van Weeren, R. J.; Nulsen, P. E. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Edge, A. C.] Univ Durham, Dept Phys, Inst Computat Cosmol, Durham DH1 3LE, England. [Fabian, A. C.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [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. [Ruszkowski, M.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Ruszkowski, M.] Michigan Ctr Theoret Phys, Ann Arbor, MI 48109 USA. RP Werner, N (reprint author), Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, 452 Lomita Mall, Stanford, CA 94305 USA. EM norbertw@stanford.edu OI Edge, Alastair/0000-0002-3398-6916; Nulsen, Paul/0000-0003-0297-4493; van Weeren, Reinout/0000-0002-0587-1660 FU NASA issued by JPL/Caltech [1428053]; NASA [PF9-00070, PF2-130104, NAS8-03060]; Chandra X-ray Center; U.S. Department of Energy [DE-AC02-76SF00515]; NSF [AST 1008454] FX This work is based in part on observations made with Herschel, a European Space Agency Cornerstone Mission with significant participation by NASA. Support for this work was provided by NASA through award number 1428053 issued by JPL/Caltech. Support for this work was provided by NASA through Einstein Postdoctoral grant numbers PF9-00070 (A.S.) and PF2-130104 (R.v.W.) awarded by the Chandra X-ray Center, which is operated by the Smithsonian Astrophysical Observatory for NASA under contract NAS8-03060. S.W.A. acknowledges support from the U.S. Department of Energy under contract number DE-AC02-76SF00515. M.R. acknowledges NSF grant AST 1008454. NR 100 TC 26 Z9 27 U1 0 U2 8 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD APR 20 PY 2013 VL 767 IS 2 AR 153 DI 10.1088/0004-637X/767/2/153 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 122VR UT WOS:000317346800056 ER PT J AU Zauderer, BA Berger, E Margutti, R Pooley, GG Sari, R Soderberg, AM Brunthaler, A Bietenholz, MF AF Zauderer, B. A. Berger, E. Margutti, R. Pooley, G. G. Sari, R. Soderberg, A. M. Brunthaler, A. Bietenholz, M. F. TI RADIO MONITORING OF THE TIDAL DISRUPTION EVENT SWIFT J164449.3+573451. II. THE RELATIVISTIC JET SHUTS OFF AND A TRANSITION TO FORWARD SHOCK X-RAY/RADIO EMISSION SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; radiation mechanisms: non-thermal; techniques: interferometric ID MASSIVE BLACK-HOLES; STARS; GALAXIES; OUTBURST; FLARES AB We present continued multi-frequency radio observations of the relativistic tidal disruption event Swift J164449.3+573451 (Sw 1644+57) extending to t approximate to 600 days. The data were obtained with the JVLA and AMI Large Array as part of our on-going study of the jet energetics and the density structure of the parsec-scale environment around the disrupting supermassive black hole. We combine these data with public Swift/XRT and Chandra X-ray observations over the same time-frame to show that the jet has undergone a dramatic transition starting at approximate to 500 days, with a sharp decline in the X-ray flux by about a factor of 170 on a timescale of delta t/t less than or similar to 0.2 (and by a factor of 15 in delta t/t approximate to 0.05). The rapid decline rules out a forward shock origin (direct or reprocessing) for the X-ray emission at less than or similar to 500 days, and instead points to internal dissipation in the inner jet. On the other hand, our radio data uniquely demonstrate that the low X-ray flux measured by Chandra at approximate to 610 days is consistent with emission from the forward shock. Furthermore, the Chandra data are inconsistent with thermal emission from the accretion disk itself since the expected temperature of similar to 30-60 eV and inner radius of similar to 2-10 R-s cannot accommodate the observed flux level or the detected emission at greater than or similar to 1 keV. We associate the rapid decline with a turn off of the relativistic jet when the mass accretion rate dropped below similar to(M) over dot(Edd) approximate to 0.006 M-circle dot yr(-1) (for a 3 x 10(6) M-circle dot black hole and order unity efficiency) indicating that the peak accretion rate was about 330 (M) over dot(Edd), and the total accreted mass by t approximate to 500 days is about 0.15 M-circle dot. From the radio data we further find significant flattening in the integrated energy of the forward shock at t greater than or similar to 250 days with E-j,E-iso approximate to 2 x 10(54) erg (E-j approximate to 10(52) erg for a jet opening angle, theta(j) = 0.1) following a rise by about a factor of 15 at approximate to 30-250 days. Projecting forward, we predict that the emission in the radio and X-ray bands will evolve in tandem with similar decline rates. C1 [Zauderer, B. A.; Berger, E.; Margutti, R.; Soderberg, A. M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Pooley, G. G.] Univ Cambridge, Cavendish Lab, Mullard Radio Observ, Cambridge CB3 0HE, England. [Sari, R.] Hebrew Univ Jerusalem, Racah Inst Phys, IL-91904 Jerusalem, Israel. [Brunthaler, A.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Bietenholz, M. F.] York Univ, Dept Phys & Astron, Toronto, ON M3J 2R7, Canada. [Bietenholz, M. F.] Hartebeesthoek Radio Astron Observ, ZA-1740 Krugersdorp, South Africa. RP Zauderer, BA (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. FU National Science Foundation [AST-1107973]; David and Lucile Packard Foundation Fellowship for Science and Engineering; European Union [275596]; University of Cambridge; STFC FX We thank Ramesh Narayan, Ryan Chornock, and Martin Elvis for detailed and helpful discussions. E.B. acknowledges support from the National Science Foundation through Grant AST-1107973. A.M.S. acknowledges support from the David and Lucile Packard Foundation Fellowship for Science and Engineering. A.B. was supported by a Marie Curie Outgoing International Fellowship (FP7) of the European Union (project number 275596). The AMI arrays are supported by the University of Cambridge and the STFC. This work made use of data supplied by the UK Swift Science Data Centre at the University of Leicester. NR 21 TC 42 Z9 42 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 APR 20 PY 2013 VL 767 IS 2 AR 152 DI 10.1088/0004-637X/767/2/152 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 122VR UT WOS:000317346800055 ER PT J AU Dawson, RI Murray-Clay, RA AF Dawson, Rebekah I. Murray-Clay, Ruth A. TI GIANT PLANETS ORBITING METAL-RICH STARS SHOW SIGNATURES OF PLANET-PLANET INTERACTIONS SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE planets and satellites: dynamical evolution and stability ID HOT JUPITERS; HOST STARS; KEPLER; MASS; EXOPLANETS; FREQUENCY; ALIGNMENT; SEARCH; SYSTEM; KECK AB Gas giants orbiting interior to the ice line are thought to have been displaced from their formation locations by processes that remain debated. Here we uncover several new metallicity trends, which together may indicate that two competing mechanisms deliver close-in giant planets: gentle disk migration, operating in environments with a range of metallicities, and violent planet-planet gravitational interactions, primarily triggered in metal-rich systems in which multiple giant planets can form. First, we show with 99.1% confidence that giant planets with semimajor axes between 0.1 and 1 AU orbiting metal-poor stars ([Fe/H] < 0) are confined to lower eccentricities than those orbiting metal-rich stars. Second, we show with 93.3% confidence that eccentric proto-hot Jupiters undergoing tidal circularization primarily orbit metal-rich stars. Finally, we show that only metal-rich stars host a pile-up of hot Jupiters, helping account for the lack of such a pile-up in the overall Kepler sample. Migration caused by stellar perturbers (e.g., stellar Kozai) is unlikely to account for the trends. These trends further motivate follow-up theoretical work addressing which hot Jupiter migration theories can also produce the observed population of eccentric giant planets between 0.1 and 1 AU. C1 [Dawson, Rebekah I.; Murray-Clay, Ruth A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Dawson, RI (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS-10, Cambridge, MA 02138 USA. EM rdawson@cfa.harvard.edu FU NSF-GRFP [DGE-1144152]; NASA Exoplanet Exploration Program; NASA Science Mission directorate; NASA [NAS5-26555]; NASA Office of Space Science [NNX09AF08G] FX The NSF-GRFP (DGE-1144152) supports R.I.D. We thank the referee for the helpful, timely report. We express our gratitude to John Johnson for many illuminating discussions about the three-day pile-up, the period distribution of giant planets, observational approaches to distinguishing the origins of hot Jupiters, valuable insights on previous collaborations connected to this investigation, and extensive comments. We thank B. Scott Gaudi and Andrew Gould for helpful comments and corrections, including altering us about XO-3-b. We thank Daniel Fabrycky for many helpful comments, Courtney Dressing for occurrence rate insights, and Subo Dong, Zachory Berta, David Charbonneau, Sean Andrews, Matthew Holman, Jason Wright, and Kevin Schlaufman for useful discussions.; We used the Exoplanet Orbit Database and Exoplanet Data Explorer at exoplanets.org, and the NASA Exoplanet Archive, operated by Caltech, under contract with the NASA Exoplanet Exploration Program. We include data collected by the Kepler mission, funded by the NASA Science Mission directorate, and are grateful to the Kepler Team for long and extensive efforts in producing this rich data set. Some data were obtained from MAST. The Association of Universities for Research in Astronomy, Inc. operates STScI under NASA contract NAS5-26555. The NASA Office of Space Science supports MAST for non-HST data via grants (including NNX09AF08G) and contracts. NR 52 TC 70 Z9 71 U1 0 U2 5 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 APR 20 PY 2013 VL 767 IS 2 AR L24 DI 10.1088/2041-8205/767/2/L24 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 123SN UT WOS:000317411100004 ER PT J AU Munoz-Jaramillo, A Dasi-Espuig, M Balmaceda, LA DeLuca, EE AF Munoz-Jaramillo, Andres Dasi-Espuig, Maria Balmaceda, Laura A. DeLuca, Edward E. TI SOLAR CYCLE PROPAGATION, MEMORY, AND PREDICTION: INSIGHTS FROM A CENTURY OF MAGNETIC PROXIES SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE Sun: activity; Sun: dynamo; Sun: surface magnetism ID POLAR FACULAE; DYNAMO MODELS; TILT ANGLES; TRANSPORT; FIELD; SUN; SOLAR-CYCLE-24; CONVECTION; EVOLUTION; STRENGTH AB The solar cycle and its associated magnetic activity are the main drivers behind changes in the interplanetary environment and Earth's upper atmosphere (commonly referred to as space weather). These changes have a direct impact on the lifetime of space-based assets and can create hazards to astronauts in space. In recent years there has been an effort to develop accurate solar cycle predictions (with aims at predicting the long-term evolution of space weather), leading to nearly a hundred widely spread predictions for the amplitude of solar cycle 24. A major contributor to the disagreement is the lack of direct long-term databases covering different components of the solar magnetic field (toroidal versus poloidal). Here, we use sunspot area and polar faculae measurements spanning a full century (as our toroidal and poloidal field proxies) to study solar cycle propagation, memory, and prediction. Our results substantiate predictions based on the polar magnetic fields, whereas we find sunspot area to be uncorrelated with cycle amplitude unless multiplied by area-weighted average tilt. This suggests that the joint assimilation of tilt and sunspot area is a better choice (with aims to cycle prediction) than sunspot area alone, and adds to the evidence in favor of active region emergence and decay as the main mechanism of poloidal field generation (i.e., the Babcock-Leighton mechanism). Finally, by looking at the correlation between our poloidal and toroidal proxies across multiple cycles, we find solar cycle memory to be limited to only one cycle. C1 [Munoz-Jaramillo, Andres; DeLuca, Edward E.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Munoz-Jaramillo, Andres] Univ Corp Atmospheric Res, Boulder, CO 80307 USA. [Munoz-Jaramillo, Andres] Univ Utah, Dept Phys & Astron, Salt Lake City, UT 84112 USA. [Dasi-Espuig, Maria] Max Planck Inst Sonnensyst Forsch, D-37191 Katlenburg Lindau, Germany. [Balmaceda, Laura A.] Inst Astron Terr & Space Sci ICATE CONICET, San Juan, Argentina. RP Munoz-Jaramillo, A (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM amunoz@cfa.harvard.edu; dasi@mps.mpg.de; lbalmaceda@icate-conicet.gob.ar; edeluca@cfa.harvard.edu RI DeLuca, Edward/L-7534-2013; OI DeLuca, Edward/0000-0001-7416-2895; Munoz-Jaramillo, Andres/0000-0002-4716-0840; Balmaceda, Laura/0000-0003-1162-5498 FU NASA; Lockheed Martin [SP02H1701R] FX We thank Piet Martens and an anonymous referee for useful discussions and suggestions. This research is supported by the NASA Living With a Star Jack Eddy Postdoctoral Fellowship Program, administered by the UCAR Visiting Scientist Programs. Andres Munoz-Jaramillo is very grateful to David Kieda for his support and sponsorship at the University of Utah. E. DeLuca was supported by contract SP02H1701R from Lockheed Martin to SAO. NR 41 TC 29 Z9 29 U1 0 U2 1 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 APR 20 PY 2013 VL 767 IS 2 AR L25 DI 10.1088/2041-8205/767/2/L25 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 123SN UT WOS:000317411100005 ER PT J AU Williams, PKG Berger, E Zauderer, BA AF Williams, Peter K. G. Berger, Edo Zauderer, B. Ashley TI QUASI-QUIESCENT RADIO EMISSION FROM THE FIRST RADIO-EMITTING T DWARF SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE brown dwarfs; radio continuum: stars; stars: individual (2MASS J10475385+2124234) ID LOW-MASS STARS; ELECTRON-CYCLOTRON MASER; BROWN DWARFS; MAGNETIC-FIELDS; LARGE-SCALE; ACTIVE STARS; COOL STARS; SKY SURVEY; GENERATION; DISCOVERY AB Radio detections of ultracool dwarfs provide insight into their magnetic fields and the dynamos that maintain them, especially at the very bottom of the main sequence, where other activity indicators dramatically weaken. Until recently, radio emission was only detected in the M and L dwarf regimes, but this has changed with the Arecibo detection of rapid polarized flares from the T6.5 dwarf 2MASS J10475385+2124234. Here, we report the detection of quasi-quiescent radio emission from this source at 5.8 GHz using the Karl G. Jansky Very Large Array. The spectral luminosity is L-nu = (2.2 +/- 0.7) x 10(12) erg s(-1) Hz(-1), a factor of similar to 100 times fainter than the Arecibo flares. Our detection is the lowest luminosity yet achieved for an ultracool dwarf. Although the emission is fully consistent with being steady, unpolarized, and broad band, we find tantalizing hints for variability. We exclude the presence of short-duration flares as seen by Arecibo, although this is not unexpected given estimates of the duty cycle. Follow-up observations of this object will offer the potential to constrain its rotation period, electron density, and the strength and configuration of the magnetic field. Equally important, follow-up observations will address the question of whether the electron cyclotron maser instability, which is thought to produce the flares seen by Arecibo, also operates in the very different parameter regime of the emission we detect, or whether instead this ultracool dwarf exhibits both maser and gyrosynchrotron radiation, potentially originating from substantially different locations. C1 [Williams, Peter K. G.; Berger, Edo; Zauderer, B. Ashley] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Williams, PKG (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM pwilliams@cfa.harvard.edu OI Williams, Peter/0000-0003-3734-3587 FU National Science Foundation [AST-1008361] FX We thank Matthew Route and Aleksander Wolszczan for insight into the Arecibo results and useful discussion on the manuscript, and the anonymous referee for comments that improved the Letter. We thank the NRAO for granting the Director's Discretionary Time used to make the observations presented in this Letter. We acknowledge support for this work from the National Science Foundation through Grant AST-1008361. The VLA is operated 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. This research has made use of NASA's Astrophysics Data System and the SIMBAD database, operated at CDS, Strasbourg, France. NR 34 TC 18 Z9 18 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 APR 20 PY 2013 VL 767 IS 2 AR L30 DI 10.1088/2041-8205/767/2/L30 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 123SN UT WOS:000317411100010 ER PT J AU Riechers, DA Bradford, CM Clements, DL Dowell, CD Perez-Fournon, I Ivison, RJ Bridge, C Conley, A Fu, H Vieira, JD Wardlow, J Calanog, J Cooray, A Hurley, P Neri, R Kamenetzky, J Aguirre, JE Altieri, B Arumugam, V Benford, DJ Bethermin, M Bock, J Burgarella, D Cabrera-Lavers, A Chapman, SC Cox, P Dunlop, JS Earle, L Farrah, D Ferrero, P Franceschini, A Gavazzi, R Glenn, J Solares, EAG Gurwell, MA Halpern, M Hatziminaoglou, E Hyde, A Ibar, E Kovacs, A Krips, M Lupu, RE Maloney, PR Martinez-Navajas, P Matsuhara, H Murphy, EJ Naylor, BJ Nguyen, HT Oliver, SJ Omont, A Page, MJ Petitpas, G Rangwala, N Roseboom, IG Scott, D Smith, AJ Staguhn, JG Streblyanska, A Thomson, AP Valtchanov, I Viero, M Wang, L Zemcov, M Zmuidzinas, J AF Riechers, Dominik A. Bradford, C. M. Clements, D. L. Dowell, C. D. Perez-Fournon, I. Ivison, R. J. Bridge, C. Conley, A. Fu, Hai Vieira, J. D. Wardlow, J. Calanog, J. Cooray, A. Hurley, P. Neri, R. Kamenetzky, J. Aguirre, J. E. Altieri, B. Arumugam, V. Benford, D. J. Bethermin, M. Bock, J. Burgarella, D. Cabrera-Lavers, A. Chapman, S. C. Cox, P. Dunlop, J. S. Earle, L. Farrah, D. Ferrero, P. Franceschini, A. Gavazzi, R. Glenn, J. Solares, E. A. Gonzalez Gurwell, M. A. Halpern, M. Hatziminaoglou, E. Hyde, A. Ibar, E. Kovacs, A. Krips, M. Lupu, R. E. Maloney, P. R. Martinez-Navajas, P. Matsuhara, H. Murphy, E. J. Naylor, B. J. Nguyen, H. T. Oliver, S. J. Omont, A. Page, M. J. Petitpas, G. Rangwala, N. Roseboom, I. G. Scott, D. Smith, A. J. Staguhn, J. G. Streblyanska, A. Thomson, A. P. Valtchanov, I. Viero, M. Wang, L. Zemcov, M. Zmuidzinas, J. TI A dust-obscured massive maximum-starburst galaxy at a redshift of 6.34 SO NATURE LA English DT Article ID STAR-FORMING GALAXIES; SIMILAR-TO 6; MOLECULAR GAS; SUBMILLIMETER GALAXIES; EARLY UNIVERSE; HOST GALAXY; QUASARS; DISKS; FIELD AB Massive present-day early-type (elliptical and lenticular) galaxies probably gained the bulk of their stellar mass and heavy elements through intense, dust-enshrouded starbursts-that is, increased rates of star formation-in the most massive dark-matter haloes at early epochs. However, it remains unknown how soon after the Big Bang massive starburst progenitors exist. The measured redshift (z) distribution of dusty, massive starbursts has long been suspected to be biased low in z owing to selection effects(1), as confirmed by recent findings of systems with redshifts as high as similar to 5 (refs 2-4). Here we report the identification of a massive starburst galaxy at z = 6.34 through a submillimetre colour-selection technique. We unambiguously determined the redshift from a suite of molecular and atomic fine-structure cooling lines. These measurements reveal a hundred billion solar masses of highly excited, chemically evolved interstellar medium in this galaxy, which constitutes at least 40 per cent of the baryonic mass. A 'maximum starburst' converts the gas into stars at a rate more than 2,000 times that of the Milky Way, a rate among the highest observed at any epoch. Despite the overall downturn in cosmic star formation towards the highest redshifts(5), it seems that environments mature enough to form the most massive, intense starbursts existed at least as early as 880 million years after the Big Bang. C1 [Riechers, Dominik A.; Bradford, C. M.; Dowell, C. D.; Bridge, C.; Vieira, J. D.; Cooray, A.; Bock, J.; Kovacs, A.; Murphy, E. J.; Nguyen, H. T.; Viero, M.; Zemcov, M.; Zmuidzinas, J.] CALTECH, Pasadena, CA 91125 USA. [Riechers, Dominik A.] Cornell Univ, Ithaca, NY 14853 USA. [Bradford, C. M.; Dowell, C. D.; Bock, J.; Naylor, B. J.; Nguyen, H. T.; Zemcov, M.; Zmuidzinas, J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Clements, D. L.; Hyde, A.] Univ London Imperial Coll Sci Technol & Med, Blackett Lab, Astrophys Grp, London SW7 2AZ, England. [Perez-Fournon, I.; Cabrera-Lavers, A.; Ferrero, P.; Martinez-Navajas, P.; Streblyanska, A.] Inst Astrofis Canarias, E-38200 Tenerife, Spain. [Perez-Fournon, I.; Cabrera-Lavers, A.; Ferrero, P.; Martinez-Navajas, P.; Streblyanska, A.] Univ La Laguna, Dept Astrofis, E-38205 Tenerife, Spain. [Ivison, R. J.; Ibar, E.] Royal Observ, UK Astron Technol Ctr, Edinburgh EH9 3HJ, Midlothian, Scotland. [Ivison, R. J.; Arumugam, V.; Dunlop, J. S.; Roseboom, I. G.; Thomson, A. P.] Univ Edinburgh, Royal Observ, Inst Astron, Edinburgh EH9 3HJ, Midlothian, Scotland. [Conley, A.; Earle, L.; Glenn, J.; Maloney, P. R.] Univ Colorado, Ctr Astrophys & Space Astron UCB 389, Boulder, CO 80309 USA. [Fu, Hai; Wardlow, J.; Calanog, J.; Cooray, A.] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA. [Hurley, P.; Oliver, S. J.; Roseboom, I. G.; Smith, A. J.; Wang, L.] Univ Sussex, Dept Phys & Astron, Ctr Astron, Brighton BN1 9QH, E Sussex, England. [Neri, R.; Cox, P.; Krips, M.] Inst Radio Astron Millimetr, F-38406 St Martin Dheres, France. [Kamenetzky, J.; Glenn, J.; Rangwala, N.] Univ Colorado, Dept Astrophys & Planetary Sci, CASA UCB 389, Boulder, CO 80309 USA. [Aguirre, J. E.; Lupu, R. E.] Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA. [Altieri, B.; Valtchanov, I.] European Space Astron Ctr, Herschel Sci Ctr, Madrid 28691, Spain. [Benford, D. J.; Staguhn, J. G.] NASA, Observat Cosmol Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Bethermin, M.] Univ Paris Diderot, CEA Saclay, Lab AIM Paris Saclay, CEA,DSM,Irfu,CNRS, F-91191 Gif Sur Yvette, France. [Bethermin, M.] Univ Paris 11, IAS, F-91405 Orsay, France. [Bethermin, M.] CNRS, UMR 8617, F-91405 Orsay, France. [Burgarella, D.] Aix Marseille Univ, CNRS, Lab Astrophys Marseille, UMR7326, F-13388 Marseille, France. [Cabrera-Lavers, A.] Grantecan SA, Ctr Astrofis La Palma, E-38712 Brena Baja, La Palma, Spain. [Chapman, S. C.; Solares, E. A. Gonzalez] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Farrah, D.] Virginia Tech, Dept Phys, Blacksburg, VA 24061 USA. [Franceschini, A.] Univ Padua, Dipartimento Fis & Astron, I-35122 Padua, Italy. [Gavazzi, R.; Omont, A.] Univ Paris 06, CNRS, Inst Astrophys Paris, UMR 7095, F-75014 Paris, France. [Gurwell, M. A.; Petitpas, G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Halpern, M.; Scott, D.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada. [Hatziminaoglou, E.] ESO, D-85748 Garching, Germany. [Kovacs, A.] Univ Minnesota, Inst Astrophys, Minneapolis, MN 55455 USA. [Matsuhara, H.] Japan Aerosp & Explorat Agcy, Inst Space & Astronaut Sci, Sagamihara, Kanagawa 2298510, Japan. [Murphy, E. J.] CALTECH, Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA. [Page, M. J.] Univ Coll London, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England. [Staguhn, J. G.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. RP Riechers, DA (reprint author), CALTECH, 1200 East Calif Blvd,MC 249-17, Pasadena, CA 91125 USA. EM dr@astro.cornell.edu RI sebastianovitsch, stepan/G-8507-2013; Lupu, Roxana/P-9060-2014; Wardlow, Julie/C-9903-2015; Kovacs, Attila/C-1171-2010; Ivison, R./G-4450-2011; Benford, Dominic/D-4760-2012; OI Lupu, Roxana/0000-0003-3444-5908; Wardlow, Julie/0000-0003-2376-8971; Kovacs, Attila/0000-0001-8991-9088; Ivison, R./0000-0001-5118-1313; Benford, Dominic/0000-0002-9884-4206; Scott, Douglas/0000-0002-6878-9840; Bethermin, Matthieu/0000-0002-3915-2015; Altieri, Bruno/0000-0003-3936-0284 NR 30 TC 160 Z9 160 U1 1 U2 30 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 0028-0836 J9 NATURE JI Nature PD APR 18 PY 2013 VL 496 IS 7445 BP 329 EP 333 DI 10.1038/nature12050 PG 5 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 126FV UT WOS:000317599200030 PM 23598341 ER PT J AU Bowman, JD Cairns, I Kaplan, DL Murphy, T Oberoi, D Staveley-Smith, L Arcus, W Barnes, DG Bernardi, G Briggs, FH Brown, S Bunton, JD Burgasser, AJ Cappallo, RJ Chatterjee, S Corey, BE Coster, A Deshpande, A deSouza, L Emrich, D Erickson, P Goeke, RF Gaensler, BM Greenhill, LJ Harvey-Smith, L Hazelton, BJ Herne, D Hewitt, JN Johnston-Hollitt, M Kasper, JC Kincaid, BB Koenig, R Kratzenberg, E Lonsdale, CJ Lynch, MJ Matthews, LD McWhirter, SR Mitchell, DA Morales, MF Morgan, EH Ord, SM Pathikulangara, J Prabu, T Remillard, RA Robishaw, T Rogers, AEE Roshi, AA Salah, JE Sault, RJ Shankar, NU Srivani, KS Stevens, JB Subrahmanyan, R Tingay, SJ Wayth, RB Waterson, M Webster, RL Whitney, AR Williams, AJ Williams, CL Wyithe, JSB AF Bowman, Judd D. Cairns, Iver Kaplan, David L. Murphy, Tara Oberoi, Divya Staveley-Smith, Lister Arcus, Wayne Barnes, David G. Bernardi, Gianni Briggs, Frank H. Brown, Shea Bunton, John D. Burgasser, Adam J. Cappallo, Roger J. Chatterjee, Shami Corey, Brian E. Coster, Anthea Deshpande, Avinash deSouza, Ludi Emrich, David Erickson, Philip Goeke, Robert F. Gaensler, B. M. Greenhill, Lincoln J. Harvey-Smith, Lisa Hazelton, Bryna J. Herne, David Hewitt, Jacqueline N. Johnston-Hollitt, Melanie Kasper, Justin C. Kincaid, Barton B. Koenig, Ronald Kratzenberg, Eric Lonsdale, Colin J. Lynch, Mervyn J. Matthews, Lynn D. McWhirter, S. Russell Mitchell, Daniel A. Morales, Miguel F. Morgan, Edward H. Ord, Stephen M. Pathikulangara, Joseph Prabu, Thiagaraj Remillard, Ronald A. Robishaw, Timothy Rogers, Alan E. E. Roshi, Anish A. Salah, Joseph E. Sault, Robert J. Shankar, N. Udaya Srivani, K. S. Stevens, Jamie B. Subrahmanyan, Ravi Tingay, Steven J. Wayth, Randall B. Waterson, Mark Webster, Rachel L. Whitney, Alan R. Williams, Andrew J. Williams, Christopher L. Wyithe, J. Stuart B. TI Science with the Murchison Widefield Array SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF AUSTRALIA LA English DT Article DE dark ages, reionisation, first stars; instrumentation: interferometers; radio continuum: general; radio lines: general; Sun: general ID GAMMA-RAY BURSTS; CORONAL MASS EJECTIONS; INTERPLANETARY SCINTILLATION OBSERVATIONS; ROTATING RADIO TRANSIENTS; TERRESTRIAL KILOMETRIC RADIATION; 21 CENTIMETER FLUCTUATIONS; MAGNETIZED NEUTRON-STARS; UPPER-ATMOSPHERE RADAR; LARGE-SCALE STRUCTURE; GALACTIC HII-REGIONS AB Significant new opportunities for astrophysics and cosmology have been identified at low radio frequencies. The Murchison Widefield Array is the first telescope in the southern hemisphere designed specifically to explore the low-frequency astronomical sky between 80 and 300 MHz with arcminute angular resolution and high survey efficiency. The telescope will enable new advances along four key science themes, including searching for redshifted 21-cm emission from the EoR in the early Universe; Galactic and extragalactic all-sky southern hemisphere surveys; time-domain astrophysics; and solar, heliospheric, and ionospheric science and space weather. The Murchison Widefield Array is located in Western Australia at the site of the planned Square Kilometre Array (SKA) low-band telescope and is the only low-frequency SKA precursor facility. In this paper, we review the performance properties of the Murchison Widefield Array and describe its primary scientific objectives. C1 [Bowman, Judd D.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85069 USA. [Cairns, Iver; Murphy, Tara; deSouza, Ludi; Gaensler, B. M.; Robishaw, Timothy] Univ Sydney, Sydney Inst Astron, Sydney, NSW 2006, Australia. [Kaplan, David L.] Univ Wisconsin, Dept Phys, Milwaukee, WI USA. [Murphy, Tara; Staveley-Smith, Lister; Briggs, Frank H.; Gaensler, B. M.; Mitchell, Daniel A.; Subrahmanyan, Ravi; Tingay, Steven J.; Wayth, Randall B.; Webster, Rachel L.; Wyithe, J. Stuart B.] ARC Ctr Excellence All Sky Astrophys CAASTRO, Redfern, NSW, Australia. [Oberoi, Divya] Natl Ctr Radio Astrophys, Pune, Maharashtra, India. [Staveley-Smith, Lister; Williams, Andrew J.] Univ Western Australia, ICRAR, Perth, WA 6009, Australia. [Arcus, Wayne; Emrich, David; Herne, David; Lynch, Mervyn J.; Ord, Stephen M.; Tingay, Steven J.; Wayth, Randall B.; Waterson, Mark] Curtin Univ, ICRAR, Perth, WA 6845, Australia. [Barnes, David G.] Monash Univ, Monash E Res Ctr, Melbourne, Vic 3004, Australia. [Bernardi, Gianni; Greenhill, Lincoln J.; Kasper, Justin C.; Mitchell, Daniel A.; Wayth, Randall B.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Briggs, Frank H.; deSouza, Ludi; Waterson, Mark] Australian Natl Univ, Res Sch Astron & Astrophys, Canberra, ACT, Australia. [Brown, Shea; Stevens, Jamie B.] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA. [Burgasser, Adam J.] Univ Calif San Diego, Dept Phys, La Jolla, CA 92093 USA. [Cappallo, Roger J.; Corey, Brian E.; Coster, Anthea; Erickson, Philip; Kincaid, Barton B.; Kratzenberg, Eric; Lonsdale, Colin J.; Matthews, Lynn D.; McWhirter, S. Russell; Rogers, Alan E. E.; Salah, Joseph E.; Whitney, Alan R.] MIT, Haystack Observ, Westford, MA 01886 USA. [Chatterjee, Shami] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. [Deshpande, Avinash; Prabu, Thiagaraj; Shankar, N. Udaya; Srivani, K. S.; Subrahmanyan, Ravi] Raman Res Inst, Bangalore 560080, Karnataka, India. [Goeke, Robert F.; Hewitt, Jacqueline N.; Morgan, Edward H.; Remillard, Ronald A.; Williams, Christopher L.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Hazelton, Bryna J.; Morales, Miguel F.] Univ Washington, Dept Phys, Seattle, WA 98195 USA. [Johnston-Hollitt, Melanie] Victoria Univ Wellington, Sch Chem & Phys Sci, Wellington, New Zealand. [Mitchell, Daniel A.; Sault, Robert J.; Webster, Rachel L.; Wyithe, J. Stuart B.] Univ Melbourne, Sch Phys, Melbourne, Vic, Australia. [Robishaw, Timothy] Domin Radio Astrophys Observ, Penticton, BC, Canada. [Roshi, Anish A.] Natl Radio Astron Observ, Charlottesville, WV USA. RP Bowman, JD (reprint author), Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85069 USA. EM judd.bowman@asu.edu RI Robishaw, Timothy/B-2654-2014; Staveley-Smith, Lister/A-1683-2011; Bunton, John/A-4944-2008; Kasper, Justin/D-1152-2010; Wayth, Randall/B-2444-2013; Williams, Andrew/K-2931-2013; Emrich, David/B-7002-2013; Deshpande, Avinash/D-4868-2012; Udayashankar , N/D-4901-2012; M, Manjunath/N-4000-2014; Subrahmanyan, Ravi/D-4889-2012; OI Murphy, Tara/0000-0002-2686-438X; Robishaw, Timothy/0000-0002-4217-5138; Staveley-Smith, Lister/0000-0002-8057-0294; Cairns, Iver/0000-0001-6978-9765; Gaensler, Bryan/0000-0002-3382-9558; Kasper, Justin/0000-0002-7077-930X; Wayth, Randall/0000-0002-6995-4131; Williams, Andrew/0000-0001-9080-0105; Emrich, David/0000-0002-4058-1837; M, Manjunath/0000-0001-8710-0730; Wyithe, Stuart/0000-0001-7956-9758 FU U.S. National Science Foundation [AST-0457585, PHY-0835713, CAREER-0847753, AST-0908884]; Australian Research Council (LIEF) [LE0775621, LE0882938]; U.S. Air Force Office of Scientific Research [FA9550-0510247]; Centre for All-sky Astrophysics (an Australian Research Council Centre of Excellence) [CE110001020]; Smithsonian Astrophysical Observatory; MIT School of Science; Raman Research Institute; Australian National University; Victoria University of Wellington via New Zealand Ministry of Economic Development [MED-E1799]; National Collaborative Research Infrastructure Strategy, Education Investment Fund; Australia India Strategic Research Fund; Astronomy Australia Limited FX This scientific work makes use of the Murchison Radio-astronomy Observatory. We acknowledge the Wajarri Yamatji people as the traditional owners of the Observatory site. Support for the MWA comes from the U.S. National Science Foundation (grants AST-0457585, PHY-0835713, CAREER-0847753, and AST-0908884), the Australian Research Council (LIEF grants LE0775621 and LE0882938), the U.S. Air Force Office of Scientific Research (grant FA9550-0510247), and the Centre for All-sky Astrophysics (an Australian Research Council Centre of Excellence funded by grant CE110001020). Support is also provided by the Smithsonian Astrophysical Observatory, the MIT School of Science, the Raman Research Institute, the Australian National University, and the Victoria University of Wellington (via grant MED-E1799 from the New Zealand Ministry of Economic Development and an IBM Shared University Research Grant). The Australian Federal government provides additional support via the National Collaborative Research Infrastructure Strategy, Education Investment Fund, and the Australia India Strategic Research Fund, and Astronomy Australia Limited, under contract to Curtin University. We acknowledge the iVEC Petabyte Data Store, the Initiative in Innovative Computing and the CUDA Center for Excellence sponsored by NVIDIA at Harvard University, and the International Centre for Radio Astronomy Research (ICRAR), a Joint Venture of Curtin University and The University of Western Australia, funded by the Western Australian State government. NR 315 TC 21 Z9 21 U1 0 U2 18 PU CAMBRIDGE UNIV PRESS PI NEW YORK PA 32 AVENUE OF THE AMERICAS, NEW YORK, NY 10013-2473 USA SN 1323-3580 EI 1448-6083 J9 PUBL ASTRON SOC AUST JI Publ. Astron. Soc. Aust. PD APR 16 PY 2013 VL 30 AR UNSP e031 DI 10.1017/pas.2013.009 PG 28 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 168JT UT WOS:000320702400002 ER PT J AU Perez, L Curtis, J Brenner, M Hodell, D Escobar, J Lozano, S Schwalb, A AF Perez, Liseth Curtis, Jason Brenner, Mark Hodell, David Escobar, Jaime Lozano, Socorro Schwalb, Antje TI Stable isotope values (delta O-18 & delta C-13) of multiple ostracode species in a large Neotropical lake as indicators of past changes in hydrology SO QUATERNARY SCIENCE REVIEWS LA English DT Article DE Stable isotopes; Autecology; Ostracoda; Neotropics; Late Pleistocene-early Holocene; Environmental change; Lake hydrodynamics; Lake level change ID LAGO PETEN ITZA; LOWLAND CENTRAL-AMERICA; CLIMATE-CHANGE; ENVIRONMENTAL HISTORY; CARBON ISOTOPES; TROPICAL LAKE; GUATEMALA; OXYGEN; RECORD; WATER AB Modern lake hydrodynamics, ostracode species autecology, stable isotopes (delta O-18 and delta C-13) of multiple ostracode species, ostracode taphonomy and sediment geochemistry were studied to improve interpretation of the late Pleistocene-early Holocene (similar to 24-10 ka) stable isotope record of ostracodes in sediment core PI-6 from Lago Peten Itza, northern Guatemala. Oxygen and carbon stable isotopes in modern and fossil species assemblages of Lago Peten Itza were used as indicators of changes in the balance between evaporation and precipitation, past lake level and carbon source. Ostracode taphonomy was used to detect past periods of strong currents, high-energy environments, and possible partial or full mixing of the lake. The modern lake water isotopic composition displays clear seasonal differences that are independent of lake level fluctuations. Modern benthic species displayed lower delta O-18 and delta C-13 values than nektobenthic species, with differences of 3.0 parts per thousand and 5.3 parts per thousand, respectively. Valves of nektobenthic species display higher values of delta C-13 because these ostracodes live in shallower environments among abundant algae and aquatic plants, where productivity is high. The benthic species Limnocythere opesta Brehm, 1939 displayed the smallest average offset from delta O-18 water (+0.3 parts per thousand) and the largest offset from delta C-13(DIC) values (-4.1 parts per thousand) among studied ostracode species. Nektobenthic species Heterocypris punctata Keyser, 1975 displayed the smallest difference relative to the delta C-13(DIC) values (-0.1 parts per thousand). Late Pleistocene-early Holocene climate conditions and water levels in Lago Peten Itza can be summarized as follows: 1) high lake levels and cold conditions (Last Glacial Maximum [LGM], similar to 24-19 ka), 2) fluctuating lake levels and cold conditions (Heinrich Stadial 1 [HS1], similar to 19-15 ka), 3) high lake levels and warm and wetter conditions (Bolling-Allerod [BA], similar to 15-13 ka), 4) low lake levels and dry conditions (Younger Dryas [YD], similar to 13-11.5 ka) and 5) high lake levels and warm and wetter conditions (early Holocene, similar to 11.5-10.0 ka). Average lake level fluctuation in Lago Peten Itza during the late Pleistocene-early Holocene was as much as similar to 25 m. Ostracode analyses suggest that the LGM was characterized by relatively low delta O-18 (+4.7 to +6.0 parts per thousand), and delta C-13 values (-7.1 to -6.4 parts per thousand) in ostracode valves, high inferred water depths and high percentages of broken adult and juvenile valves (>66%), suggesting a high-energy environment, strong currents, partial to full mixing, downslope transport, colder water temperatures and wetter conditions. An increase in the relative abundance of the benthic species L. opesta and higher numbers of broken valves suggest heavy precipitation events during the LGM (similar to 23.7, 21.7, 20.8 and 20.1 ka). HS1 was predominantly dry, but we identified times when lake levels were slightly higher, at the onset of the deglacial and a brief period (similar to 17-16 ka) between HS1b and HS1a. All studied climate proxies indicate wetter and warmer conditions and lake system stability during the BA. Lake levels dropped during the YD and gradually increased during the Preboreal and early Holocene. We demonstrate that modern and fossil ostracode isotopic signatures, species assemblages and taphonomy can be used together with physical and geochemical variables in Lago Peten Itza sediments to make high-resolution inferences about late Pleistocene-early Holocene environmental changes in the lowland Neotropics. (C) 2012 Elsevier Ltd. All rights reserved. C1 [Perez, Liseth; Lozano, Socorro] Univ Nacl Autonoma Mexico, Inst Geol, Mexico City 04510, DF, Mexico. [Curtis, Jason; Brenner, Mark] Univ Florida, Dept Geol Sci, Gainesville, FL 32611 USA. [Curtis, Jason; Brenner, Mark] Univ Florida, Land Use & Environm Change Inst, Gainesville, FL 32611 USA. [Hodell, David] Univ Cambridge, Dept Earth Sci, Godwin Lab Palaeoclimate Res, Cambridge CB2 3EQ, England. [Escobar, Jaime] Univ Norte, Dept Ingn Civil & Ambiental, Barranquilla, Colombia. [Escobar, Jaime] Smithsonian Trop Res Inst, Ctr Trop Paleoecol & Archaeol, Panama City, Panama. [Perez, Liseth; Schwalb, Antje] Tech Univ Carolo Wilhelmina Braunschweig, Inst Geosyst & Bioindikat, D-38106 Braunschweig, Germany. RP Perez, L (reprint author), Univ Nacl Autonoma Mexico, Inst Geol, Mexico City 04510, DF, Mexico. EM lcpereza@geologia.unam.mx FU Deutsche Forschungsgemeinschaft (DFG) [Schw 671-3]; Technische Universitat Braunschweig (TU-BS, Germany); National Science Foundation (NSF, USA); International Continental Scientific Drilling Program (ICDP); Swiss Federal Institute of Technology; Swiss National Science Foundation FX We thank all who assisted us during field trips to Logo Peten Itza and other regional waterbodies. We are grateful to the following people and agencies: Roberto Moreno, Margarita Palmieri, Margaret Dix, Eleonor de Tott (Universidad del Valle de Guatemala), Consejo Nacional de Areas Protegidas (CONAP), Asociacion para el Manejo y Desarrollo Sostenible de la cuenca del Lago Peten Itza (AMPI), Michael Hillesheim, Burkhard Scharf, Julia Lorenschat, Rita Bugja, Susanne Kruger, Wolfgang Riss and Evgenia Vinogradova and the team of the Peten Itza scientific sampling party as well as the staff of the National Lacustrine Core Facility (LacCore, Minnesota, USA) for core curation and members of the Drilling, Observation and Sampling of the Earth's Continental Crust (DOSECC) for their support during drilling operations in Logo Peten Itza in 2006. The Deutsche Forschungsgemeinschaft (DFG, grant Schw 671-3), Technische Universitat Braunschweig (TU-BS, Germany), National Science Foundation (NSF, USA), International Continental Scientific Drilling Program (ICDP), Swiss Federal Institute of Technology and Swiss National Science Foundation provided financial support for core recovery and analysis. NR 49 TC 9 Z9 10 U1 0 U2 32 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0277-3791 J9 QUATERNARY SCI REV JI Quat. Sci. Rev. PD APR 15 PY 2013 VL 66 SI SI BP 96 EP 111 DI 10.1016/j.quascirev.2012.10.044 PG 16 WC Geography, Physical; Geosciences, Multidisciplinary SC Physical Geography; Geology GA 124FF UT WOS:000317448500010 ER PT J AU Hong, T AF Hong, Terry TI Five Star Billionaire SO LIBRARY JOURNAL LA English DT Book Review C1 [Hong, Terry] Smithsonian BookDragon, Washington, DC USA. RP Hong, T (reprint author), Smithsonian BookDragon, Washington, DC USA. NR 1 TC 0 Z9 0 U1 0 U2 1 PU REED BUSINESS INFORMATION PI NEW YORK PA 360 PARK AVENUE SOUTH, NEW YORK, NY 10010 USA SN 0363-0277 J9 LIBR J JI Libr. J. PD APR 15 PY 2013 VL 138 IS 7 BP 71 EP 71 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA 124IW UT WOS:000317458000067 ER PT J AU McLaughlin, BM AF McLaughlin, B. M. TI An R-matrix with pseudo-state approach to the single photon double ionization and excitation of the He-like Li+ ion SO JOURNAL OF PHYSICS B-ATOMIC MOLECULAR AND OPTICAL PHYSICS LA English DT Article ID ELECTRON-IMPACT EXCITATION; HELIUM ISOELECTRONIC SEQUENCE; X-RAY OBSERVATIONS; DOUBLE-PHOTOIONIZATION; XMM-NEWTON; ATOM SCATTERING; CROSS-SECTIONS; CHANDRA; DIAGNOSTICS; ENERGIES AB The success of the R-matrix with pseudo-state (RMPS) method to model single photoionization processes, benchmarked against dedicated synchrotron light source measurements, is exploited and extended to investigate, single photon double ionization cross-sections for the He-like, Li+ ion. We investigate these processes from both the ground state and the excited 1s2s S-1,S-3 metastable levels of this He-like system. Comparisons of the results from the RMPS method are made with other state-of-the-art theoretical approaches such as time-dependent close-coupling (TDCC), B-splines and the convergent close-coupling (CCC). Excellent agreement with various other theoretical approaches are achieved but differences occur which are highlighted and discussed. For the ground state the peak of the cross-section is similar to 2 kilo-barns (Kb), that for the 1s2s S-1 state is similar to 6 and similar to 1 Kb for the corresponding 1s2s S-3 state. All the cross-sections for single photon double ionization are extremely small, being in the region of 2-10 Kb, or less, rendering their experimental determination extremely challenging. C1 [McLaughlin, B. M.] Queens Univ Belfast, Sch Math & Phys, CTAMOP, Belfast BT7 1NN, Antrim, North Ireland. [McLaughlin, B. M.] Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom & Mol Phys, Cambridge, MA 02138 USA. RP McLaughlin, BM (reprint author), Queens Univ Belfast, Sch Math & Phys, CTAMOP, David Bates Bldg,7 Coll Pk, Belfast BT7 1NN, Antrim, North Ireland. EM b.mclaughlin@qub.ac.uk FU National Science Foundation; Queen's University Belfast; National Science Foundation [OCI-1053575] FX BMMcL acknowledges support by the National Science Foundation through a grant to the Institute for Theoretical Atomic and Molecular Physics (ITAMP) at the Harvard-Smithsonian Center for Astrophysics under the visitor's program where this work was completed. ITAMP is supported by a grant from the National Science Foundation. Thanks are due to Queen's University Belfast for the award of a Visiting Research Fellowship and to Dr Jim McCann for useful discussions. We thank Dr Ulrich Kleiman for the provision of the TDCC data and Professor Igor Bray for the CCC data. Helpful discussions with Professor Alex Dalgarno FRS, Dr John C Raymond and Professor Philip Stancil, on the astrophysical applications are gratefully acknowledged. Professors Mitch S Pindzola and Connor P Ballance are gratefully acknowledged for many helpful and stimulating conversions on R-matrix collision theory and parallel computing throughout the course of this work. The computational work was carried out at the National Energy Research Scientific Computing Center in Oakland, CA, USA and on the Kraken XT5 facility at the National Institute for Computational Science (NICS) in Knoxville, TN, USA. The Kraken XT5 facility is a resource of the Extreme Science and Engineering Discovery Environment (XSEDE), which is supported by National Science Foundation grant no. OCI-1053575. NR 61 TC 5 Z9 5 U1 0 U2 12 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0953-4075 EI 1361-6455 J9 J PHYS B-AT MOL OPT JI J. Phys. B-At. Mol. Opt. Phys. PD APR 14 PY 2013 VL 46 IS 7 AR 075204 DI 10.1088/0953-4075/46/7/075204 PG 7 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA 111YB UT WOS:000316556800011 ER PT J AU Belthangady, C Bar-Gill, N Pham, LM Arai, K Le Sage, D Cappellaro, P Walsworth, RL AF Belthangady, C. Bar-Gill, N. Pham, L. M. Arai, K. Le Sage, D. Cappellaro, P. Walsworth, R. L. TI Dressed-State Resonant Coupling between Bright and Dark Spins in Diamond SO PHYSICAL REVIEW LETTERS LA English DT Article ID ROOM-TEMPERATURE; BATH; MAGNETOMETRY; DYNAMICS AB Under ambient conditions, spin impurities in solid-state systems are found in thermally mixed states and are optically "dark"; i.e., the spin states cannot be optically controlled. Nitrogen-vacancy (NV) centers in diamond are an exception in that the electronic spin states are "bright"; i.e., they can be polarized by optical pumping, coherently manipulated with spin-resonance techniques, and read out optically, all at room temperature. Here we demonstrate a scheme to resonantly couple bright NV electronic spins to dark substitutional-nitrogen (P1) electronic spins by dressing their spin states with oscillating magnetic fields. This resonant coupling mechanism can be used to transfer spin polarization from NV spins to nearby dark spins and could be used to cool a mesoscopic bath of dark spins to near-zero temperature, thus providing a resource for quantum information and sensing, and aiding studies of quantum effects in many-body spin systems. DOI: 10.1103/PhysRevLett.110.157601 C1 [Belthangady, C.; Bar-Gill, N.; Le Sage, D.; Walsworth, R. L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Belthangady, C.; Bar-Gill, N.; Le Sage, D.; Walsworth, R. L.] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. [Pham, L. M.] Harvard Univ, Sch Engn & Appl Sci, Cambridge, MA 02138 USA. [Arai, K.] MIT, Dept Phys, Cambridge, MA 02139 USA. [Cappellaro, P.] MIT, Nucl Sci & Engn Dept, Cambridge, MA 02139 USA. RP Belthangady, C (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM rwalsworth@cfa.harvard.edu RI Cappellaro, Paola/B-1413-2010; OI Cappellaro, Paola/0000-0003-3207-594X; Le Sage, David/0000-0003-1678-9491 FU NIST; NSF; DARPA (QuEST program); DARPA (QuASAR program) FX This work was supported by NIST, NSF and DARPA (QuEST and QuASAR programs). We gratefully acknowledge the provision of diamond samples by Apollo, and helpful technical discussions with Stephen DeVience, Michael Grinolds, Patrick Maletinsky, Ashok Ajoy, Alexandre Cooper, Mikhail Lukin, Amir Yacoby, and Fedor Jelezko. NR 30 TC 23 Z9 23 U1 0 U2 43 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 APR 12 PY 2013 VL 110 IS 15 AR 157601 DI 10.1103/PhysRevLett.110.157601 PG 5 WC Physics, Multidisciplinary SC Physics GA 126DQ UT WOS:000317592500013 PM 25167312 ER PT J AU Uzdin, R AF Uzdin, Raam TI Resources needed for non-unitary quantum operations SO JOURNAL OF PHYSICS A-MATHEMATICAL AND THEORETICAL LA English DT Article AB Non-unitary operations generated by an effective non-Hermitian Hamiltonian can be used to create quantum state manipulations which are impossible in Hermitian quantum mechanics. These operations include state preparation (or cooling) and non-orthogonal state discrimination. In this work we put a lower bound on the resources needed for the construction of some given non-unitary evolution. Passive systems are studied in detail and a general feature of such systems is derived. After interpreting our results using the singular value decomposition, several examples are studied analytically. In particular, we put a lower bound on the resources needed for non-Hermitian state preparation and non-orthogonal state discrimination. C1 [Uzdin, Raam] Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom Mol & Opt Phys ITAMP, Cambridge, MA 02138 USA. RP Uzdin, R (reprint author), Hebrew Univ Jerusalem, Racah Inst Phys, IL-91904 Jerusalem, Israel. EM raam@mail.huji.ac.il NR 9 TC 3 Z9 3 U1 1 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 1751-8113 J9 J PHYS A-MATH THEOR JI J. Phys. A-Math. Theor. PD APR 12 PY 2013 VL 46 IS 14 AR 145302 DI 10.1088/1751-8113/46/14/145302 PG 12 WC Physics, Multidisciplinary; Physics, Mathematical SC Physics GA 114GN UT WOS:000316729200014 ER PT J AU Dikow, RB Smith, WL AF Dikow, Rebecca B. Smith, William Leo TI Genome-level homology and phylogeny of Vibrionaceae (Gammaproteobacteria: Vibrionales) with three new complete genome sequences SO BMC MICROBIOLOGY LA English DT Article ID CHROMOSOMES AB Background: Phylogenetic hypotheses based on complete genome data are presented for the Gammaproteobacteria family Vibrionaceae. Two taxon samplings are presented: one including all those taxa for which the genome sequences are complete in terms of arrangement (chromosomal location of fragments; 19 taxa) and one for which the genome sequences contain multiple contigs (44 taxa). Analyses are presented under the Maximum Parsimony and Maximum Likelihood optimality criteria for total evidence datasets, the two chromosomes separately, and individual analyses of locally collinear blocks. Three of the genomes included in the 44 taxon dataset, those of Vibrio gazogenes, Salinivibrio costicola, and Aliivibrio logei have been newly sequenced and their genome sequences are documented here. Results: Phylogenetic results for the 19-taxon datasets show similar levels of collinear subset of dataset incongruence as a previous study of 22 taxa from the sister family Shewanellaceae, while also echoing the strong phylogenetic performance of random subsets of data also shown in this study. Phylogenetic results for both the 19-taxon and 44-taxon datasets corroborate previous hypotheses about the placement of Photobacterium and Aliivibrio within Vibrionaceae and also highlight problems with how Photobacterium is delimited and indicate that it likely should be dissolved into Vibrio to produce a phylogenetic taxonomy. The 19-taxon and 44-taxon trees based on the large chromosome are congruent for the majority of taxa that are present in both datasets. Analyses of the 44-taxon sampling based on the second, small chromosome are quite different from those based on the large chromosome, which is not surprising given the dramatically divergent nature of the small chromosome and the difficulty in postulating primary homologies. Conclusions: The phylogenetic analyses presented here represent the most comprehensive genome-level phylogenetic analyses in terms of taxa and data. Based on the availability of genome data for many bacterial species on GenBank, many other bacterial groups would also be amenable to similar genome-scale phylogenetic analyses even when present in multiple contigs. The result that collinear subsets of data are incongruent with the concatenated dataset and with each other while random data subsets show very little incongruence echoes the result of previous work on Shewanellaceae. The 44-taxon phylogenetic analysis presented here thus represents the future of phylogenomic analyses in scope and complexity. C1 [Dikow, Rebecca B.] Univ Chicago, Comm Evolutionary Biol, Chicago, IL 60637 USA. [Dikow, Rebecca B.; Smith, William Leo] Field Museum Nat Hist, Div Fishes, Chicago, IL 60605 USA. RP Dikow, RB (reprint author), Smithsonian Inst, Natl Zool Pk, Ctr Conservat & Evolutionary Genet, POB 37012,MRC 108, Washington, DC 20013 USA. EM dikowR@si.edu FU Lerner-Gray Fund for Marine Research (American Museum of Natural History); University of Chicago Committee on Evolutionary Biology Hinds Fund; Pritzker Lab for Molecular Systematics lab grant; Field Museum Women's Board; Emerging Pathogens Project; Davee Foundation; Dr. Ralph and Marian Falk Medical Research Trust FX The authors thank Dionysios Antonopoulos, Michael Coates, Torsten Dikow, Shannon Hackett, Olivier Rieppel, and Ward Wheeler for discussion and reading earlier drafts. Research was supported by the Lerner-Gray Fund for Marine Research (American Museum of Natural History), the University of Chicago Committee on Evolutionary Biology Hinds Fund and Pritzker Lab for Molecular Systematics lab grant. RBD also received stipend support from The Field Museum Women's Board and the Emerging Pathogens Project (funded by The Davee Foundation and The Dr. Ralph and Marian Falk Medical Research Trust). The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 25 TC 5 Z9 5 U1 0 U2 7 PU BIOMED CENTRAL LTD PI LONDON PA 236 GRAYS INN RD, FLOOR 6, LONDON WC1X 8HL, ENGLAND SN 1471-2180 J9 BMC MICROBIOL JI BMC Microbiol. PD APR 11 PY 2013 VL 13 AR 80 DI 10.1186/1471-2180-13-80 PG 13 WC Microbiology SC Microbiology GA 150NC UT WOS:000319396600001 PM 23578061 ER PT J AU Albrecht, S Setiawan, J Torres, G Fabrycky, DC Winn, JN AF Albrecht, Simon Setiawan, Johny Torres, Guillermo Fabrycky, Daniel C. Winn, Joshua N. TI THE BANANA PROJECT. IV. TWO ALIGNED STELLAR ROTATION AXES IN THE YOUNG ECCENTRIC BINARY SYSTEM EP CRUCIS: PRIMORDIAL ORIENTATION AND TIDAL ALIGNMENT SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries: eclipsing; stars: early-type; stars: formation; stars: individual (EP Crucis, DI Herculis); stars: kinematics and dynamics; stars: rotation; techniques: spectroscopic ID SPIN-ORBIT ALIGNMENT; ECLIPSING BINARIES; PLANETARY SYSTEM; MISALIGNED SPIN; APSIDAL MOTION; Y-2 ISOCHRONES; DI HERCULIS; STARS; EVOLUTION; MODELS AB With observations of the EP Cru system, we continue our series of measurements of spin-orbit angles in eclipsing binary star systems, the BANANA project (Binaries Are Not Always Neatly Aligned). We find a close alignment between the sky projections of the rotational and orbital angular momentum vectors for both stars (beta(p) = - 1.degrees 8 +/- 1.degrees 6 and \beta(s)\ < 17 degrees). We also derive precise absolute dimensions and stellar ages for this system. The EP Cru and DI Her systems provide an interesting comparison: they have similar stellar types and orbital properties, but DI Her is younger and has major spin-orbit misalignments, raising the question of whether EP Cru also had a large misalignment at an earlier phase of evolution. We show that tidal dissipation is an unlikely explanation for the good alignment observed today, because realignment happens on the same timescale as spin-orbit synchronization, and the stars in EP Cru are far from synchronization (they are spinning nine times too quickly). Therefore it seems that some binaries form with aligned axes, while other superficially similar binaries are formed with misaligned axes. C1 [Albrecht, Simon; Winn, Joshua N.] MIT, Dept Phys, Cambridge, MA 02139 USA. [Albrecht, Simon; Winn, Joshua N.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Setiawan, Johny] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Setiawan, Johny] Embassy Republ Indonesia, D-10557 Berlin, Germany. [Torres, Guillermo] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Fabrycky, Daniel C.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. RP Albrecht, S (reprint author), MIT, Dept Phys, Cambridge, MA 02139 USA. OI Fabrycky, Daniel/0000-0003-3750-0183 FU La Silla Paranal Observatory [084.C-1008]; Netherlands Organisation for Scientific Research (NWO); NASA [NNX09AB33G]; NSF [1108595]; NASA through Hubble Fellowship [HF-51272.01-A]; STScI; AURA [NAS 5-26555] FX Based on observations made with ESOs 2.2 m Telescopes at the La Silla Paranal Observatory under program ID 084.C-1008 (12.5%) and under MPIA guaranteed time (87.5%).; The authors are grateful to Peter Eggleton for insightful discussions on binary evolution and for making his TOPPLE code available to us. We thank John Southworth for providing us with the spectra used in the study by Clausen et al. (2007). S. A. acknowledges support during part of this project by a Rubicon fellowship from the Netherlands Organisation for Scientific Research (NWO). Work by S. A. and J.N.W. was supported by NASA Origins award NNX09AB33G and NSF grant No. 1108595. D. C. F. acknowledges NASA support through Hubble Fellowship grant HF-51272.01-A, awarded by STScI, operated by AURA under contract NAS 5-26555. This research has made use of the following web resources: http://simbad.u-strasbg.fr, http://adswww.harvard.edu, http://arxiv.org. NR 34 TC 9 Z9 9 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD APR 10 PY 2013 VL 767 IS 1 AR 32 DI 10.1088/0004-637X/767/1/32 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 117IT UT WOS:000316947500032 ER PT J AU Bai, XN Stone, JM AF Bai, Xue-Ning Stone, James M. TI LOCAL STUDY OF ACCRETION DISKS WITH A STRONG VERTICAL MAGNETIC FIELD: MAGNETOROTATIONAL INSTABILITY AND DISK OUTFLOW SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; instabilities; magnetohydrodynamics (MHD); methods: numerical; turbulence ID ANGULAR-MOMENTUM TRANSPORT; 3-DIMENSIONAL MAGNETOHYDRODYNAMIC SIMULATIONS; MRI-DRIVEN TURBULENCE; SPINNING BLACK-HOLE; ZERO NET FLUX; MHD SIMULATIONS; SHEARING BOX; GAS-PRESSURE; NUMERICAL SIMULATIONS; DOMINATED ACCRETION AB We perform three-dimensional, vertically-stratified, local shearing-box ideal MHD simulations of the magnetorotational instability (MRI) that include a net vertical magnetic flux, which is characterized by midplane plasma beta(0) (ratio of gas to magnetic pressure). We have considered beta(0) = 10(2), 10(3), and 10(4), and in the first two cases the most unstable linear MRI modes are well resolved in the simulations. We find that the behavior of the MRI turbulence strongly depends on beta(0): the radial transport of angular momentum increases with net vertical flux, achieving alpha similar to 0.08 for beta = 10(4) and alpha greater than or similar to 1.0 for beta(0) = 100, where alpha is the height-integrated and mass-weighted Shakura-Sunyaev parameter. A critical value lies at beta(0) similar to 10(3): for beta(0) greater than or similar to 10(3), the disk consists of a gas pressure dominated midplane and a magnetically dominated corona. The turbulent strength increases with net flux, and angular momentum transport is dominated by turbulent fluctuations. The magnetic dynamo that leads to cyclic flips of large-scale fields still exists, but becomes more sporadic as net flux increases. For beta(0) less than or similar to 10(3), the entire disk becomes magnetically dominated. The turbulent strength saturates, and the magnetic dynamo is fully quenched. Stronger large-scale fields are generated with increasing net flux, which dominates angular momentum transport. A strong outflow is launched from the disk by the magnetocentrifugal mechanism, and the mass flux increases linearly with net vertical flux and shows sign of saturation at beta(0) less than or similar to 10(2). However, the outflow is unlikely to be directly connected to a global wind: for beta(0) greater than or similar to 10(3), the large-scale field has no permanent bending direction due to dynamo activities, while for beta(0) less than or similar to 10(3), the outflows from the top and bottom sides of the disk bend towards opposite directions, inconsistent with a physical disk wind geometry. Global simulations are needed to address the fate of the outflow. C1 [Bai, Xue-Ning; Stone, James M.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. RP Bai, XN (reprint author), Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, 60 Garden St,MS-51, Cambridge, MA 02138 USA. EM xbai@cfa.harvard.edu FU NASA through Hubble Fellowship grant from the Space Telescope Science Institute [HST-HF-51301.01-A]; NASA [NAS5-26555]; National Science Foundation [AST-0908269] FX We thank Sebastian Fromang and Geoffroy Lesur for sharing with us their submitted manuscripts, and the referee, Geoffroy Lesur for helpful comments that improved the clarity of this paper. We also acknowledge Adam Burrows, Sebastian Fromang, Shu-ichiro Inutsuka, Anders Johansen, Geoffroy Lesur, Ramesh Narayan, Gordon Ogilvie, Dimitrios Psaltis, Aleksander Sadowski, Takeru Suzuki, Taku Takeuchi, Alexander Tchekhovskoy, and Feng Yuan for useful discussions. X.N.B. acknowledges support for program number HST-HF-51301.01-A provided by NASA through a Hubble Fellowship 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. J.M.S. acknowledges support from the National Science Foundation through grant AST-0908269. This work used computational facilities provided by PICSciE at Princeton University. NR 96 TC 65 Z9 65 U1 0 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 APR 10 PY 2013 VL 767 IS 1 AR 30 DI 10.1088/0004-637X/767/1/30 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 117IT UT WOS:000316947500030 ER PT J AU Bailey, V Hinz, PM Currie, T Su, KYL Esposito, S Hill, JM Hoffmann, WF Jones, T Kim, J Leisenring, J Meyer, M Murray-Clay, R Nelson, MJ Pinna, E Puglisi, A Rieke, G Rodigas, T Skemer, A Skrutskie, MF Vaitheeswaran, V Wilson, JC AF Bailey, Vanessa Hinz, Philip M. Currie, Thayne Su, Kate Y. L. Esposito, Simone Hill, John M. Hoffmann, William F. Jones, Terry Kim, Jihun Leisenring, Jarron Meyer, Michael Murray-Clay, Ruth Nelson, Matthew J. Pinna, Enrico Puglisi, Alfio Rieke, George Rodigas, Timothy Skemer, Andrew Skrutskie, Michael F. Vaitheeswaran, Vidhya Wilson, John C. TI A THERMAL INFRARED IMAGING STUDY OF VERY LOW MASS, WIDE-SEPARATION BROWN DWARF COMPANIONS TO UPPER SCORPIUS STARS: CONSTRAINING CIRCUMSTELLAR ENVIRONMENTS SO ASTROPHYSICAL JOURNAL LA English DT Article DE brown dwarfs; circumstellar matter; instrumentation: adaptive optics; open clusters and associations: individual (Upper Scorpius); stars: individual (GSC 06214-00210, 1RXS 160929.1-210524, and HIP 78530) ID YOUNG SUBSTELLAR COMPANION; ORBITING HR 8799; SOLAR-TYPE STARS; EDGE-ON DISK; OB ASSOCIATION; PLANET FORMATION; MU-M; GALILEAN SATELLITES; EVOLUTIONARY MODELS; ADAPTIVE OPTICS AB We present a 3-5 mu m LBT/MMT adaptive optics imaging study of three Upper Scorpius stars with brown dwarf (BD) companions with very low masses/mass ratios (M-BD < 25 M-Jup; M-BD/M-star approximate to 1%-2%) and wide separations (300-700 AU): GSC 06214, 1RXS 1609, and HIP 78530. We combine these new thermal IR data with existing 1-4 mu m and 24 mu m photometry to constrain the properties of the BDs and identify evidence for circumprimary/circumsecondary disks in these unusual systems. We confirm that GSC 06214B is surrounded by a disk, further showing that this disk produces a broadband IR excess due to small dust near the dust sublimation radius. An unresolved 24 mu m excess in the system may be explained by the contribution from this disk. 1RXS 1609B exhibits no 3-4 mu m excess, nor does its primary; however, the system as a whole has a modest 24 mu m excess, which may come from warm dust around the primary and/or BD. Neither object in the HIP 78530 system exhibits near- to mid-IR excesses. We additionally find that the 1-4 mu m colors of HIP 78530B match a spectral type of M3 +/- 2, inconsistent with the M8 spectral type assigned based on its near-IR spectrum, indicating that it may be a low-mass star rather than a BD. We present new upper limits on additional low-mass companions in the system (< 5 M-Jup beyond 175 AU). Finally, we examine the utility of circumsecondary disks as probes of the formation histories of wide BD companions, finding that the presence of a disk may disfavor BD formation near the primary with subsequent outward scattering. C1 [Bailey, Vanessa; Hinz, Philip M.; Su, Kate Y. L.; Hoffmann, William F.; Rieke, George; Rodigas, Timothy; Skemer, Andrew; Vaitheeswaran, Vidhya] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Currie, Thayne] Univ Toronto, Dept Astron & Astrophys, Toronto, ON M5S 3H4, Canada. [Esposito, Simone; Pinna, Enrico; Puglisi, Alfio] Osserv Astrofis Arcetri, I-50125 Florence, Italy. [Hill, John M.] Univ Arizona, Large Binocular Telescope Observ, Tucson, AZ 85721 USA. [Jones, Terry] Univ Minnesota, Sch Phys & Astron, Minneapolis, MN 55455 USA. [Kim, Jihun] Univ Arizona, Coll Opt Sci, Tucson, AZ 85721 USA. [Leisenring, Jarron; Meyer, Michael] ETH, Inst Angew Phys, CH-8093 Zurich, Switzerland. [Murray-Clay, Ruth; Skrutskie, Michael F.] Harvard Univ, Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Nelson, Matthew J.; Wilson, John C.] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA. RP Bailey, V (reprint author), Univ Arizona, Steward Observ, 933 N Cherry Ave, Tucson, AZ 85721 USA. EM vbailey@as.arizona.edu OI Esposito, Simone/0000-0002-3114-677X; Pinna, Enrico/0000-0002-6243-5697; Skemer, Andrew/0000-0001-6098-3924; Rodigas, Timothy/0000-0002-7535-2997; Su, Kate/0000-0002-3532-5580; Bailey, Vanessa/0000-0002-5407-2806 FU National Aeronautics and Space Administration; National Science Foundation; NASA [NSF 0705296]; National Science Foundation Graduate Research Fellowship [NSF DGE-1143953] FX We gratefully acknowledge the hard work and dedication of all members of the LBTI team including: Tom McMahon, Paul Arbo, Teresa Bippert-Plymate, Oli Durney, Manny Montoya, Mitch Nash, and Elliot Solheid. We thank the anonymous referee for helpful comments; Daniel Apai, Laird Close, Michael Cushing, and Kevin Luhman for their insightful discussions; Brendan Bowler for sharing his GSC 06214A SPEX data; and the LBT and MMT staff for their support of these observations. 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. We utilized data products from the Wide-field Infrared Survey Explorer, which is a joint project of the University of California, Los Angeles, and the Jet Propulsion Laboratory/California Institute of Technology, funded by the National Aeronautics and Space Administration. We also utilized 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. LBTI is funded by a NASA grant in support of the Exoplanet Exploration Program (NSF 0705296). V. B. is supported by the National Science Foundation Graduate Research Fellowship (NSF DGE-1143953). NR 85 TC 20 Z9 20 U1 1 U2 14 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD APR 10 PY 2013 VL 767 IS 1 AR 31 DI 10.1088/0004-637X/767/1/31 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 117IT UT WOS:000316947500031 ER PT J AU Dressing, CD Charbonneau, D AF Dressing, Courtney D. Charbonneau, David TI THE OCCURRENCE RATE OF SMALL PLANETS AROUND SMALL STARS SO ASTROPHYSICAL JOURNAL LA English DT Article DE catalogs; methods: data analysis; planetary systems; stars: low-mass; surveys; techniques: photometric ID LOW-MASS STARS; TRANSIT TIMING OBSERVATIONS; KEPLER INPUT CATALOG; CANDIDATE HOST STARS; ORBITING M-DWARFS; NEARBY M DWARFS; SUN-LIKE STAR; EFFECTIVE TEMPERATURES; HABITABLE-ZONE; STELLAR EVOLUTION AB We use the optical and near-infrared photometry from the Kepler Input Catalog to provide improved estimates of the stellar characteristics of the smallest stars in the Kepler target list. We find 3897 dwarfs with temperatures below 4000 K, including 64 planet candidate host stars orbited by 95 transiting planet candidates. We refit the transit events in the Kepler light curves for these planet candidates and combine the revised planet/ star radius ratios with our improved stellar radii to revise the radii of the planet candidates orbiting the cool target stars. We then compare the number of observed planet candidates to the number of stars around which such planets could have been detected in order to estimate the planet occurrence rate around cool stars. We find that the occurrence rate of 0.5-4R circle plus. planets with orbital periods shorter than 50 days is 0.90(-0.03)(+0.04) planets per star. The occurrence rate of Earth- size (0.5- 1.4R circle plus) planets is constant across the temperature range of our sample at 0.51(- 0.05)(+0.06) Earth-size planets per star, but the occurrence of 1.4-4R(circle plus) planets decreases significantly at cooler temperatures. Our sample includes two Earth- size planet candidates in the habitable zone, allowing us to estimate that the mean number of Earth- size planets in the habitable zone is 0.15(-0.06) (+0.13) planets per cool star. Our 95% confidence lower limit on the occurrence rate of Earth- size planets in the habitable zones of cool stars is 0.04 planets per star. With 95% confidence, the nearest transiting Earth- size planet in the habitable zone of a cool star is within 21 pc. Moreover, the nearest non- transiting planet in the habitable zone is within 5 pc with 95% confidence. C1 [Dressing, Courtney D.; Charbonneau, David] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Dressing, CD (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM cdressing@cfa.harvard.edu OI Dressing, Courtney/0000-0001-8189-0233; Charbonneau, David/0000-0002-9003-484X FU National Science Foundation [NNX12AC77G]; NASA Science Mission directorate; National Aeronautics and Space Administration; National Science Foundation; NASA [NAS5-26555]; NASA Office of Space Science [NNX09AF08G] FX C.D. is supported by a National Science Foundation Graduate Research Fellowship. We acknowledge support from the Kepler Participating Scientist Program via grant NNX12AC77G. We thank the referee, Philip Muirhead, for providing comments that improved the paper. We acknowledge helpful conversations with S. Ballard, Z. Berta, J. Carter, R. Dawson, J.-M. Desert, A. Dupree, F. Fressin, A. Howard, J. Irwin, D. Latham, A. Mann, R. Murray-Clay, and G. Torres. We thank R. Kopparapu for correspondence that led to a correction. This paper includes data collected by the Kepler mission. Funding for the Kepler mission is provided by the NASA Science Mission directorate. We thank the Kepler team for acquiring, reducing, and sharing their data. 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. All of the data presented in this paper were obtained from the Mikulski Archive for Space Telescopes (MAST). STScI is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555. Support for MAST for non-HST data is provided by the NASA Office of Space Science via grant NNX09AF08G and by other grants and contracts. NR 86 TC 250 Z9 250 U1 4 U2 31 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD APR 10 PY 2013 VL 767 IS 1 AR 95 DI 10.1088/0004-637X/767/1/95 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 117IT UT WOS:000316947500095 ER PT J AU Foley, RJ Challis, PJ Chornock, R Ganeshalingam, M Li, W Marion, GH Morrell, NI Pignata, G Stritzinger, MD Silverman, JM Wang, X Anderson, JP Filippenko, AV Freedman, WL Hamuy, M Jha, SW Kirshner, RP McCully, C Persson, SE Phillips, MM Reichart, DE Soderberg, AM AF Foley, Ryan J. Challis, P. J. Chornock, R. Ganeshalingam, M. Li, W. Marion, G. H. Morrell, N. I. Pignata, G. Stritzinger, M. D. Silverman, J. M. Wang, X. Anderson, J. P. Filippenko, A. V. Freedman, W. L. Hamuy, M. Jha, S. W. Kirshner, R. P. McCully, C. Persson, S. E. Phillips, M. M. Reichart, D. E. Soderberg, A. M. TI TYPE Iax SUPERNOVAE: A NEW CLASS OF STELLAR EXPLOSION SO ASTROPHYSICAL JOURNAL LA English DT Article DE supernovae: general; supernovae: individual (SN 1991bj, SN 1999ax, SN 2002bp, SN 2002cx, SN 2003gq, SN 2004cs, SN 2004gw, SN 2005P, SN 2005cc, SN 2005hk, SN 2006hn, SN 2007J, SN 2007ie, SN 2007qd, SN 2008A, SN 2008ae, SN 2008ge, SN 2008ha, SN 2009J, SN 2009ku, SN 2010ae, SN 2010el, SN 2011ay, SN 2011ce, SN 2012Z) ID CHANDRASEKHAR MASS MODELS; HELIUM SHELL DETONATIONS; PHOTOMETRY DATA RELEASE; ACCRETING WHITE-DWARFS; LIGHT CURVES; SN 2005HK; THERMONUCLEAR SUPERNOVAE; IMAGE SUBTRACTION; TIME DISTRIBUTION; OPTICAL-SPECTRA AB We describe observed properties of the Type Iax class of supernovae (SNe Iax), consisting of SNe observationally similar to its prototypical member, SN 2002cx. The class currently has 25 members, and we present optical photometry and/ or optical spectroscopy for most of them. SNe Iax are spectroscopically similar to SNe Ia, but have lower maximum-light velocities (2000 less than or similar to broken vertical bar v broken vertical bar less than or similar to 8000 km s(-1)), typically lower peak magnitudes (-14.2 >= M-V,M-peak greater than or similar to -18.9 mag), and most have hot photospheres. Relative to SNe Ia, SNe Iax have low luminosities for their light-curve shape. There is a correlation between luminosity and light-curve shape, similar to that of SNe Ia, but offset from that of SNe Ia and with larger scatter. Despite a host-galaxy morphology distribution that is highly skewed to late-type galaxies without any SNe Iax discovered in elliptical galaxies, there are several indications that the progenitor stars are white dwarfs (WDs): evidence of C/ O burning in their maximum-light spectra, low (typically similar to 0.5 M-circle dot) ejecta masses, strong Fe lines in their late-time spectra, a lack of X-ray detections, and deep limits on massive stars and star formation at the SN sites. However, two SNe Iax show strong He lines in their spectra. The progenitor system and explosion model that best fits all of the data is a binary system of a C/ O WD that accretes matter from a He star and has a deflagration. At least some of the time, this explosion will not disrupt the WD. The small number of SNe in this class prohibit a detailed analysis of the homogeneity and heterogeneity of the entire class. We estimate that in a given volume there are 31(-13)(+17) SNe Iax for every 100 SNe Ia, and for every 1M(circle dot) of iron generated by SNe Ia at z = 0, SNe Iax generate similar to 0.036M(circle dot). Being the largest class of peculiar SNe, thousands of SNe Iax will be discovered by LSST. Future detailed observations of SNe Iax should further our understanding of both their progenitor systems and explosions as well as those of SNe Ia. C1 [Foley, Ryan J.; Challis, P. J.; Chornock, R.; Marion, G. H.; Kirshner, R. P.; Soderberg, A. M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Ganeshalingam, M.; Li, W.; Silverman, J. M.; Filippenko, A. V.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Morrell, N. I.; Phillips, M. M.] Las Campanas Observ, Carnegie Observ, La Serena, Chile. [Pignata, G.] Univ Andres Bello, Dept Ciencias Fis, Santiago, Chile. [Stritzinger, M. D.] Aarhus Univ, Dept Phys & Astron, DK-8000 Aarhus C, Denmark. [Silverman, J. M.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA. [Wang, X.] Tsinghua Univ, Dept Phys, Beijing 100084, Peoples R China. [Wang, X.] Tsinghua Univ, Tsinghua Ctr Astrophys THCA, Beijing 100084, Peoples R China. [Anderson, J. P.; Hamuy, M.] Univ Chile, Dept Astron, Santiago, Chile. [Freedman, W. L.; Persson, S. E.] Observ Carnegie Inst Washington, Pasadena, CA 91101 USA. [Jha, S. W.; McCully, C.] Rutgers State Univ, Dept Phys & Astron, Piscataway, NJ 08854 USA. [Reichart, D. E.] Univ N Carolina, Dept Phys & Astron, Chapel Hill, NC USA. RP Foley, RJ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM rfoley@cfa.harvard.edu RI Wang, Xiaofeng/J-5390-2015; Hamuy, Mario/G-7541-2016; OI stritzinger, maximilian/0000-0002-5571-1833 FU Clay Fellowship; NSF [AST-1211196, AST-0908886, AST-1211916, AST-0306969, AST-0607438, AST-1008343]; Gary & Cynthia Bengier, the Richard & Rhoda Goldman Fund; Christopher R. Redlich Fund; TABASGO Foundation; Danish Agency for Science and Technology and Innovation; Millennium Center for Supernova Science [P10-064-F]; CONICYT; Programa Iniciativa Cientifica Milenio de MIDEPLAN; CONICYT through FONDECYT [3110142, 11090421]; NSF CAREER [AST-0847157] FX R.J.F. is supported by a Clay Fellowship. Supernova research at Harvard is supported by NSF grant AST-1211196. A. V. F.' s supernova group at U. C. Berkeley is supported by Gary & Cynthia Bengier, the Richard & Rhoda Goldman Fund, the Christopher R. Redlich Fund, the TABASGO Foundation, and NSF grants AST-0908886 and AST-1211916. KAIT and its ongoing operation were made possible by donations from Sun Microsystems, Inc., the Hewlett-Packard Company, AutoScope Corporation, Lick Observatory, the NSF, the University of California, the Sylvia & Jim Katzman Foundation, and the TABASGO Foundation. CSP material is based upon work supported by the NSF under grants AST-0306969, AST-0607438, and AST-1008343. M. S. acknowledges generous support provided by the Danish Agency for Science and Technology and Innovation through a SapereAude Level 2 grant. J. A., M. H., and G. P. acknowledge support provided by the Millennium Center for Supernova Science through grant P10-064-F (funded by "Programa Bicentenario de Ciencia y Tecnologia de CONICYT" and "Programa Iniciativa Cientifica Milenio de MIDEPLAN"), with input from "Fondo de Innovacion para la Competitividad, del Ministerio de Economia, Fomento y Turismo de Chile." J. A. and G. P. also acknowledge support by CONICYT through FONDECYT grants 3110142 and 11090421, respectively. Support for this research at Rutgers University was provided in part by NSF CAREER award AST-0847157 to S. W. J. We thank all of the amateur astronomers who have searched for supernovae. The discovery of many SNe Iax is the result of their tireless effort. We especially thank C. Moore, discoverer of SN 2008ha. We gratefully acknowledge L. Bildsten, A. GalYam, M. Hicken, D. Leonard, R. Margutti, T. Matheson, K. Moore, J. Nordin, L. O " stman, H. Perets, T. Piro, E. RamirezRuiz, D. Sahu, K. Shen, V. Stanishev, and S. Valenti for providing data, insights, and/or help for this study. R. Assef, A. Barth, V. Bennert, P. Berlind, P. Blanchard, G. Canalizo, B. Cenko, K. Clubb, D. Cohen, A. Diamond-Stanic, G. Folatelli, S. Hoenig, J. Irwin, M. Lazarova, N. Lee, A. Miller, A. Morgan, P. Nugent, D. Poznanski, J. Rex, A. Sonnenfeld, T. Steele, B. Tucker, and J. Walsh helped obtain some data presented in this paper; we thank them for their time. We are indebted to the staffs at the La Silla, Las Campanas, Lick, Keck, and Fred L. Whipple Observatories for their dedicated services. 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 (NASA); the observatory was made possible by the generous financial support of the W. M. Keck Foundation. This research has made use of the NASA/IPAC Extragalactic Database (NED), which is operated by the Jet Propulsion Laboratory, California Institute ofTechnology, under contract with NASA. The analysis pipeline used to reduce the DEIMOS data was developed at UC Berkeley with support from NSF grant AST-0071048. NTT data was obtained under ESO Programme was 080. A-0516. Part of the analysis occurred when R. J. F. visited the Aspen Center for Physics during the Summer 2012 workshops, " NonGaussianity as aWindow to the Primordial Universe" and " The Evolution ofMassive Stars and Progenitors of GRBs," as well as during his time at the Center as an independent researcher. This material is based upon work supported in part by the National Science Foundation under grant No.; 1066293 and the hospitality of the Aspen Center for Physics. Some analysis was performed at the Woody Creek Community Center in Woody Creek, CO. Facilities: Du Pont(Tek5), ESO: 3.6m(EFOSC), FLWO: 1.5m (FAST), Keck: I(LRIS), KAIT, Shane(Kast), Magellan: Baade (IMACS), Magellan: Clay(LDSS3), NTT(EMMI), CTIO: PROMPT, Swope(SITe3) NR 170 TC 100 Z9 101 U1 3 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 APR 10 PY 2013 VL 767 IS 1 AR 57 DI 10.1088/0004-637X/767/1/57 PG 28 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 117IT UT WOS:000316947500057 ER PT J AU Follette, KB Tamura, M Hashimoto, J Whitney, B Grady, C Close, L Andrews, SM Kwon, J Wisniewski, J Brandt, TD Mayama, S Kandori, R Dong, RB Abe, L Brandner, W Carson, J Currie, T Egner, SE Feldt, M Goto, M Guyon, O Hayano, Y Hayashi, M Hayashi, S Henning, T Hodapp, K Ishii, M Iye, M Janson, M Knapp, GR Kudo, T Kusakabe, N Kuzuhara, M McElwain, MW Matsuo, T Miyama, S Morino, JI Moro-Martin, A Nishimura, T Pyo, TS Serabyn, E Suto, H Suzuki, R Takami, M Takato, N Terada, H Thalmann, C Tomono, D Turner, EL Watanabe, M Yamada, T Takami, H Usuda, T AF Follette, Katherine B. Tamura, Motohide Hashimoto, Jun Whitney, Barbara Grady, Carol Close, Laird Andrews, Sean M. Kwon, Jungmi Wisniewski, John Brandt, Timothy D. Mayama, Satoshi Kandori, Ryo Dong, Ruobing Abe, Lyu Brandner, Wolfgang Carson, Joseph Currie, Thayne Egner, Sebastian E. Feldt, Markus Goto, Miwa Guyon, Olivier Hayano, Yutaka Hayashi, Masahiko Hayashi, Saeko Henning, Thomas Hodapp, Klaus Ishii, Miki Iye, Masanori Janson, Markus Knapp, Gillian R. Kudo, Tomoyuki Kusakabe, Nobuhiko Kuzuhara, Masayuki McElwain, Michael W. Matsuo, Taro Miyama, Shoken Morino, Jun-Ichi Moro-Martin, Amaya Nishimura, Tetsuo Pyo, Tae-Soo Serabyn, Eugene Suto, Hiroshi Suzuki, Ryuji Takami, Michihiro Takato, Naruhisa Terada, Hiroshi Thalmann, Christian Tomono, Daigo Turner, Edwin L. Watanabe, Makoto Yamada, Toru Takami, Hideki Usuda, Tomonori TI MAPPING H-BAND SCATTERED LIGHT EMISSION IN THE MYSTERIOUS SR21 TRANSITIONAL DISK SO ASTROPHYSICAL JOURNAL LA English DT Article DE planetary systems; protoplanetary disks; stars: individual (SR21); stars: pre-main sequence; techniques: polarimetric ID MAIN-SEQUENCE STARS; 2-DIMENSIONAL RADIATIVE-TRANSFER; YOUNG STELLAR OBJECTS; PROTOPLANETARY DISKS; CIRCUMSTELLAR DUST; PROTOSTELLAR ENVELOPES; SIZE DISTRIBUTION; MOLECULAR CLOUD; FORMING REGION; GIANT PLANETS AB We present the first near infrared (NIR) spatially resolved images of the circumstellar transitional disk around SR21. These images were obtained with the Subaru HiCIAO camera, adaptive optics, and the polarized differential imaging technique. We resolve the disk in scattered light at H-band for stellocentric 0 ''.1 <= r <= 0 ''.6 (12 less than or similar to r less than or similar to 75 AU). We compare our results with previously published spatially resolved 880 mu m continuum Submillimeter Array images that show an inner r less than or similar to 36 AU cavity in SR21. Radiative transfer models reveal that the large disk depletion factor invoked to explain SR21's sub-mm cavity cannot be "universal" for all grain sizes. Even significantly more moderate depletions (delta = 0.1, 0.01 relative to an undepleted disk) than those that reproduce the sub-mm cavity (delta similar to 10(-6)) are inconsistent with our H-band images when they are assumed to carry over to small grains, suggesting that surface grains scattering in the NIR either survive or are generated by whatever mechanism is clearing the disk midplane. In fact, the radial polarized intensity profile of our H-band observations is smooth and steeply inwardly-increasing (r(-3)), with no evidence of a break at the 36 AU sub-mm cavity wall. We hypothesize that this profile is dominated by an optically thin disk envelope or atmosphere component. We also discuss the compatibility of our data with the previously postulated existence of a sub-stellar companion to SR21 at r similar to 10-20 AU, and find that we can neither exclude nor verify this scenario. This study demonstrates the power of multiwavelength imaging of transitional disks to inform modeling efforts, including the debate over precisely what physical mechanism is responsible for clearing these disks of their large midplane grains. C1 [Follette, Katherine B.; Close, Laird] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Tamura, Motohide; Hashimoto, Jun; Kwon, Jungmi; Kandori, Ryo; Iye, Masanori; Kusakabe, Nobuhiko; Kuzuhara, Masayuki; Morino, Jun-Ichi; Suto, Hiroshi] Natl Astron Observ Japan, Mitaka, Tokyo 1818588, Japan. [Tamura, Motohide; Kwon, Jungmi] Grad Univ Adv Studies Sokendai, Dept Astron Sci, Tokyo 1818588, Japan. [Whitney, Barbara] Univ Wisconsin, Dept Astron, Madison, WI 53706 USA. [Grady, Carol] Eureka Sci, Oakland, CA 96002 USA. [Andrews, Sean M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Wisniewski, John] Univ Oklahoma, HL Dodge Dept Phys & Astron, Norman, OK 73019 USA. [Brandt, Timothy D.; Dong, Ruobing; Janson, Markus; Knapp, Gillian R.; Turner, Edwin L.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. [Mayama, Satoshi] Grad Univ Adv Studies Sokendai, Ctr Promot Integrated Sci, Hayama, Kanagawa 2400193, Japan. [Abe, Lyu] Univ Nice Sophia Antipolis, CNRS, Observ Cote Azur, Lab Lagrange,UMR7293, F-06300 Nice, France. [Brandner, Wolfgang; Feldt, Markus; Henning, Thomas] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Carson, Joseph] Coll Charleston, Dept Phys & Astron, Charleston, SC 29424 USA. [Currie, Thayne] Univ Toronto, Dept Astron & Astrophys, Toronto, ON M5S 3H4, Canada. [Egner, Sebastian E.; Guyon, Olivier; Hayano, Yutaka; Hayashi, Saeko; Ishii, Miki; Kudo, Tomoyuki; Nishimura, Tetsuo; Pyo, Tae-Soo; Takato, Naruhisa; Terada, Hiroshi; Tomono, Daigo; Takami, Hideki; Usuda, Tomonori] Subaru Telescope, Hilo, HI 96720 USA. [Goto, Miwa] Univ Munich, Univ Sternwarte Munchen, D-81679 Munich, Germany. [Hayashi, Masahiko] Univ Tokyo, Dept Astron, Bunkyo Ku, Tokyo 1130033, Japan. [Hodapp, Klaus] Univ Hawaii, Inst Astron, Hilo, HI 96720 USA. [McElwain, Michael W.] NASA, Goddard Space Flight Ctr, ExoPlanets & Stellar Astrophys Lab, Greenbelt, MD 20771 USA. [Matsuo, Taro] Kyoto Univ, Dept Astron, Sakyo Ku, Kitashirakawa Oiwake, Kyoto 6068502, Japan. [Miyama, Shoken] Hiroshima Univ, Off President, Higashihiroshima 7398511, Japan. [Moro-Martin, Amaya] Inst Nacl Tecn Aeroespacial, CAB INTA CSIC, Dept Astrofis, E-28850 Madrid, Spain. [Serabyn, Eugene] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Suzuki, Ryuji] TMT Observ Corp, Pasadena, CA 91105 USA. [Takami, Michihiro] Acad Sinica, Inst Astron & Astrophys, Taipei 106, Taiwan. [Thalmann, Christian] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 XH Amsterdam, Netherlands. [Turner, Edwin L.] Univ Tokyo, Kavli Inst Phys & Math Universe, Kashiwa, Chiba 2778568, Japan. [Watanabe, Makoto] Hokkaido Univ, Dept Cosmosci, Sapporo, Hokkaido 0600810, Japan. [Yamada, Toru] Tohoku Univ, Astron Inst, Aoba Ku, Sendai, Miyagi 9808578, Japan. RP Follette, KB (reprint author), Univ Arizona, Steward Observ, 933 N Cherry Ave, Tucson, AZ 85721 USA. EM kfollette@as.arizona.edu RI MIYAMA, Shoken/A-3598-2015; Watanabe, Makoto/E-3667-2016 OI Watanabe, Makoto/0000-0002-3656-4081 FU National Science Foundation; MEXT; [NSF-AST 1009314]; [NSF-AST 1009203] FX We gratefully acknowledge funding from the National Science Foundation East Asian and Pacific Summer Institute Fellowship (Follette), NSF-AST 1009314 (Wisniewski) and NSF-AST 1009203 (Carson). We are grateful to Collette Salyk, Glenn Schneider, Dean Hines, Don McCarthy, Vanessa Bailey, and Johanna Teske for their insightful comments. The authors wish to recognize and acknowledge the very significant cultural role and reverence that the summit of Mauna Kea has always had within the indigenous Hawaiian community. We are most fortunate to have the opportunity to conduct observations from this mountain. Part of this work was carried out at JPL. This work is partly supported by a Grant-in-Aid for Science Research in a Priority Area from MEXT. NR 77 TC 42 Z9 42 U1 0 U2 8 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD APR 10 PY 2013 VL 767 IS 1 AR 10 DI 10.1088/0004-637X/767/1/10 PG 26 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 117IT UT WOS:000316947500010 ER PT J AU Ko, J Hwang, HS Lee, JC Sohn, YJ AF Ko, Jongwan Hwang, Ho Seong Lee, Jong Chul Sohn, Young-Jong TI THE MID-INFRARED AND NEAR-ULTRAVIOLET EXCESS EMISSIONS OF QUIESCENT GALAXIES ON THE RED SEQUENCE SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: evolution; galaxies: stellar content; infrared: galaxies; surveys; ultraviolet: galaxies ID DIGITAL SKY SURVEY; COLOR-MAGNITUDE RELATION; SPECTRAL ENERGY-DISTRIBUTIONS; LUMINOUS INFRARED GALAXIES; ASYMPTOTIC GIANT BRANCH; ACTIVE GALACTIC NUCLEI; ON-ORBIT PERFORMANCE; STAR-FORMATION; EVOLUTION-EXPLORER; CLUSTER GALAXIES AB We study the mid-infrared (IR) and near-ultraviolet (UV) excess emissions of spectroscopically selected quiescent galaxies on the optical red sequence. We use the Wide-field Infrared Survey Explorer mid-IR and Galaxy Evolution Explorer near-UV data for a spectroscopic sample of galaxies in the Sloan Digital Sky Survey Data Release 7 to study the possible connection between quiescent red-sequence galaxies with and without mid-IR/near-UV excess. Among 648 12 mu m detected quiescent red-sequence galaxies without Ha emission, 26% and 55% show near-UV and mid-IR excess emissions, respectively. When we consider only bright (M-r < -21.5) galaxies with an early-type morphology, the fraction of galaxies with recent star formation is still 39%. The quiescent red-sequence galaxies with mid-IR and near-UV excess emissions are optically fainter and have slightly smaller D(n)4000 than those without mid-IR and near-UV excess emissions. We also find that mid-IR weighted mean stellar ages of quiescent red-sequence galaxies with mid-IR excess are larger than those with near-UV excess, and smaller than those without mid-IR and near-UV excess. The environmental dependence of the fraction of quiescent red-sequence galaxies with mid-IR and near-UV excess seems strong even though the trends of quiescent red-sequence galaxies with near-UV excess differ from those with mid-IR excess. These results indicate that the recent star formation traced by near-UV (less than or similar to 1 Gyr) and mid-IR (less than or similar to 2 Gyr) excess is not negligible among nearby, quiescent, red, early-type galaxies. We suggest a possible evolutionary scenario of quiescent red-sequence galaxies from quiescent red-sequence galaxies with near-UV excess to those with mid-IR excess to those without near-UV and mid-IR excess. C1 [Ko, Jongwan; Lee, Jong Chul] Korea Astron & Space Sci Inst, Taejon 305348, South Korea. [Hwang, Ho Seong] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. [Sohn, Young-Jong] Yonsei Univ, Dept Astron, Seoul 120749, South Korea. RP Ko, J (reprint author), Korea Astron & Space Sci Inst, Taejon 305348, South Korea. EM jwko@kasi.re.kr NR 64 TC 13 Z9 13 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 APR 10 PY 2013 VL 767 IS 1 AR 90 DI 10.1088/0004-637X/767/1/90 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 117IT UT WOS:000316947500090 ER PT J AU Lee, SH Slane, PO Ellison, DC Nagataki, S Patnaude, DJ AF Lee, Shiu-Hang Slane, Patrick O. Ellison, Donald C. Nagataki, Shigehiro Patnaude, Daniel J. TI A CR-HYDRO-NEI MODEL OF MULTI-WAVELENGTH EMISSION FROM THE VELA JR. SUPERNOVA REMNANT (SNR RX J0852.0-4622) SO ASTROPHYSICAL JOURNAL LA English DT Article DE acceleration of particles; cosmic rays; ISM: supernova remnants; shock waves ID DIFFUSIVE SHOCK ACCELERATION; EFFICIENT PARTICLE-ACCELERATION; MAGNETIC-FIELD AMPLIFICATION; COSMIC-RAY ACCELERATION; LARGE-AREA TELESCOPE; TEV GAMMA-RAY; GALACTIC SUPERNOVA; NONEQUILIBRIUM IONIZATION; NORTHWESTERN RIM; LINE EMISSION AB Based largely on energy budget considerations and the observed cosmic-ray (CR) ionic composition, supernova remnant (SNR) blast waves are the most likely sources of CR ions with energies at least up to the "knee" near 10(15) eV. Shocks in young shell-type TeV-bright SNRs are surely producing TeV particles, but the emission could be dominated by ions producing pi(0)-decay emission or electrons producing inverse Compton gamma rays. Unambiguously identifying the GeV-TeV emission process in a particular SNR will not only help pin down the origin of CRs, it will also add significantly to our understanding of the diffusive shock acceleration (DSA) mechanism and improve our understanding of supernovae and the impact SNRs have on the circumstellar medium. In this study, we investigate the Vela Jr. SNR, an example of TeV-bright non-thermal SNRs. We perform hydrodynamic simulations coupled with nonlinear DSA and non-equilibrium ionization near the forward shock to confront currently available multi-wavelength data. We find, with an analysis similar to that used earlier for SNR RX J1713.7-3946, that self-consistently modeling the thermal X-ray line emission with the non-thermal continuum in our one-dimensional model strongly constrains the fitting parameters, and this leads convincingly to a leptonic origin for the GeV-TeV emission for Vela Jr. This conclusion is further supported by applying additional constraints from observation, including the radial brightness profiles of the SNR shell in TeV gamma rays, and the spatial variation of the X-ray synchrotron spectral index. We will discuss implications of our models on future observations by the next-generation telescopes. C1 [Lee, Shiu-Hang; Nagataki, Shigehiro] Kyoto Univ, Yukawa Inst Theoret Phys, Sakyo Ku, Kyoto 6068502, Japan. [Slane, Patrick O.; Patnaude, Daniel J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Ellison, Donald C.] N Carolina State Univ, Dept Phys, Raleigh, NC 27695 USA. RP Lee, SH (reprint author), Kyoto Univ, Yukawa Inst Theoret Phys, Sakyo Ku, Oiwake Cho Kitashirakawa, Kyoto 6068502, Japan. EM lee@yukawa.kyoto-u.ac.jp; slane@cfa.harvard.edu; don_ellison@ncsu.edu; nagataki@yukawa.kyoto-u.ac.jp; dpatnaude@cfa.harvard.edu FU NASA [ATP02-0042-0006, NNH04Zss001N-LTSA, 06-ATP06-21, NNX11AE03G, NAS8-03060]; Ministry of Education, Culture, Sports, Science and Technology [23105709]; Japan Society for the Promotion of Science [19104006, 23340069]; Global COE Program, The Next Generation of Physics, Spun from Universality and Emergence, from MEXT of Japan FX The authors acknowledge important discussions with Takaaki Tanaka and Hidetoshi Sano concerning this work. They also thank the anonymous referee for providing valuable suggestions on improving the quality of this manuscript. D. C. E. acknowledges support from NASA grants ATP02-0042-0006, NNH04Zss001N-LTSA, 06-ATP06-21, and NNX11AE03G. P. S. acknowledges support from NASA Contract NAS8-03060. S.N. acknowledges support from Ministry of Education, Culture, Sports, Science and Technology (No. 23105709), Japan Society for the Promotion of Science (No. 19104006 and No. 23340069), and the Global COE Program, The Next Generation of Physics, Spun from Universality and Emergence, from MEXT of Japan. NR 38 TC 12 Z9 12 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD APR 10 PY 2013 VL 767 IS 1 AR 20 DI 10.1088/0004-637X/767/1/20 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 117IT UT WOS:000316947500020 ER PT J AU Milisavljevic, D Margutti, R Soderberg, AM Pignata, G Chomiuk, L Fesen, RA Bufano, F Sanders, NE Parrent, JT Parker, S Mazzali, P Pian, E Pickering, T Buckley, DAH Crawford, SM Gulbis, AAS Hettlage, C Hooper, E Nordsieck, KH O'Donoghue, D Husser, TO Potter, S Kniazev, A Kotze, P Romero-Colmenero, E Vaisanen, P Wolf, M Bietenholz, MF Bartel, N Fransson, C Walker, ES Brunthaler, A Chakraborti, S Levesque, EM MacFadyen, A Drescher, C Bock, G Marples, P Anderson, JP Benetti, S Reichart, D Ivarsen, K AF Milisavljevic, Dan Margutti, Raffaella Soderberg, Alicia M. Pignata, Giuliano Chomiuk, Laura Fesen, Robert A. Bufano, Filomena Sanders, Nathan E. Parrent, Jerod T. Parker, Stuart Mazzali, Paolo Pian, Elena Pickering, Timothy Buckley, David A. H. Crawford, Steven M. Gulbis, Amanda A. S. Hettlage, Christian Hooper, Eric Nordsieck, Kenneth H. O'Donoghue, Darragh Husser, Tim-Oliver Potter, Stephen Kniazev, Alexei Kotze, Paul Romero-Colmenero, Encarni Vaisanen, Petri Wolf, Marsha Bietenholz, Michael F. Bartel, Norbert Fransson, Claes Walker, Emma S. Brunthaler, Andreas Chakraborti, Sayan Levesque, Emily M. MacFadyen, Andrew Drescher, Colin Bock, Greg Marples, Peter Anderson, Joseph P. Benetti, Stefano Reichart, Daniel Ivarsen, Kevin TI MULTI-WAVELENGTH OBSERVATIONS OF SUPERNOVA 2011ei: TIME-DEPENDENT CLASSIFICATION OF TYPE IIb AND Ib SUPERNOVAE AND IMPLICATIONS FOR THEIR PROGENITORS SO ASTROPHYSICAL JOURNAL LA English DT Article DE supernovae: general; supernovae: individual (SN 2011ei) ID CORE-COLLAPSE SUPERNOVAE; WOLF-RAYET STARS; SOUTHERN SPECTROPHOTOMETRIC STANDARDS; SWIFT ULTRAVIOLET/OPTICAL TELESCOPE; THEORETICAL LIGHT CURVES; HYPERNOVA SN 1998BW; X-RAY; STRIPPED-ENVELOPE; RADIO-EMISSION; SHOCK BREAKOUT AB We present X-ray, UV/optical, and radio observations of the stripped-envelope, core-collapse supernova (SN) 2011ei, one of the least luminous SNe IIb or Ib observed to date. Our observations begin with a discovery within similar to 1 day of explosion and span several months afterward. Early optical spectra exhibit broad, Type II-like hydrogen Balmer profiles that subside rapidly and are replaced by Type Ib-like He-rich features on a timescale of one week. High-cadence monitoring of this transition suggests absorption attributable to a high-velocity (greater than or similar to 12,000 km s(-1)) H-rich shell, which is likely present in many Type Ib events. Radio observations imply a shock velocity of v approximate to 0.13 c and a progenitor star average mass-loss rate of (M) over dot approximate to 1.4 x 10(-5) M-circle dot yr(-1) (assuming wind velocity v(w) = 10(3) km s(-1)). This is consistent with independent constraints from deep X-ray observations with Swift-XRT and Chandra. Overall, the multi-wavelength properties of SN 2011ei are consistent with the explosion of a lower-mass (3-4 M-circle dot), compact (R-* less than or similar to 1 x 10(11) cm), He-core star. The star retained a thin hydrogen envelope at the time of explosion, and was embedded in an inhomogeneous circumstellar wind suggestive of modest episodic mass loss. We conclude that SN 2011ei's rapid spectral metamorphosis is indicative of time-dependent classifications that bias estimates of the relative explosion rates for Type IIb and Ib objects, and that important information about a progenitor star's evolutionary state and mass loss immediately prior to SN explosion can be inferred from timely multi-wavelength observations. C1 [Milisavljevic, Dan; Margutti, Raffaella; Soderberg, Alicia M.; Chomiuk, Laura; Sanders, Nathan E.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Pignata, Giuliano; Bufano, Filomena] Univ Andres Bello, Dept Ciencias Fis, Santiago, Chile. [Chomiuk, Laura] Natl Radio Astron Observ, Socorro, NM 87801 USA. [Fesen, Robert A.; Parrent, Jerod T.] Dartmouth Coll, Dept Phys & Astron, Hanover, NH 03755 USA. [Parrent, Jerod T.] Las Cumbres Observ Global Telescope Network, Goleta, CA 93117 USA. [Parker, Stuart] Parkdale Observ, Canterbury 7495, New Zealand. [Mazzali, Paolo] Max Planck Inst Astrophys, D-85748 Garching, Germany. [Mazzali, Paolo; Benetti, Stefano] INAF Osservatorio Astron Padova, I-35122 Padua, Italy. [Mazzali, Paolo] Univ Calif Santa Barbara, Kavli Inst Theoret Phys, Santa Barbara, CA 93106 USA. [Pian, Elena] Trieste Astron Observ, INAF, I-34143 Trieste, Italy. [Pian, Elena; Walker, Emma S.] Scuola Normale Super Pisa, I-56126 Pisa, Italy. [Pickering, Timothy; Buckley, David A. H.; Crawford, Steven M.; Gulbis, Amanda A. S.; Hettlage, Christian; Potter, Stephen; Kniazev, Alexei; Kotze, Paul; Romero-Colmenero, Encarni; Vaisanen, Petri] S African Astron Observ, ZA-7935 Cape Town, South Africa. [Pickering, Timothy; Buckley, David A. H.; Crawford, Steven M.; Gulbis, Amanda A. S.; Hettlage, Christian; Kniazev, Alexei; Kotze, Paul; Romero-Colmenero, Encarni; Vaisanen, Petri] Southern African Large Telescope, ZA-7935 Cape Town, South Africa. [Hooper, Eric; Nordsieck, Kenneth H.; Wolf, Marsha] Univ Wisconsin, Dept Astron, Madison, WI 53706 USA. [Husser, Tim-Oliver] Univ Gottingen, Inst Astrophys, D-37077 Gottingen, Germany. [Bietenholz, Michael F.; Bartel, Norbert] York Univ, Dept Phys & Astron, Toronto, ON M3J 1P3, Canada. [Bietenholz, Michael F.] Hartebeesthoek Radio Observ, ZA-1740 Krugersdorp, South Africa. [Fransson, Claes] Stockholm Univ, Oskar Klein Ctr, Dept Astron, SE-10691 Stockholm, Sweden. [Brunthaler, Andreas] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Chakraborti, Sayan] Tata Inst Fundamental Res, Dept Astron & Astrophys, Bombay 400005, Maharashtra, India. [Levesque, Emily M.] Univ Colorado, Dept Astrophys & Planetary Sci, CASA, Boulder, CO 80309 USA. [MacFadyen, Andrew] NYU, Dept Phys, New York, NY 10003 USA. [Bock, Greg] Windaroo Lakes Observ, Windaroo, Qld, Australia. [Marples, Peter] Loganholme Observ, Loganholme, Qld, Australia. [Anderson, Joseph P.] Univ Chile, Dept Astron, Santiago, Chile. [Reichart, Daniel; Ivarsen, Kevin] Univ N Carolina, Dept Phys & Astron, Chapel Hill, NC 27599 USA. RP Milisavljevic, D (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM dmilisav@cfa.harvard.edu OI Benetti, Stefano/0000-0002-3256-0016; MacFadyen, Andrew/0000-0002-0106-9013; Pian, Elena/0000-0001-8646-4858 FU National Aeronautics and Space Administration through Chandra Award [12500613]; Chandra X-ray Observatory Center; National Aeronautics Space Administration [NAS8-03060]; proyecto regular UNAB [DI-28-11/R]; National Research Foundation (NRF) of South Africa; Marie Curie Outgoing International Fellowship (FP7) of the European Union [275596]; Millennium Center for Supernova Science [P10-064-F]; Programa Bicentenario de Ciencia y Tecnologia de CONICYT; Programa Iniciativa Cientifica Milenio de MIDEPLAN; FONDECYT [3120227]; CONICYT through FONDECYT [3110142] FX We thank an anonymous referee for suggestions that improved the manuscript. R. Chornock provided helpful comments. Some of the observations reported in this paper were obtained with the Southern African Large Telescope (SALT), as well as the 6.5 mMagellan Telescopes located at Las Campanas Observatory, Chile. Additional observations were obtained at the Southern Astrophysical Research (SOAR) telescope, which is a joint project of the Ministerio da Ciencia, Tecnologia, e Inovacao (MCTI) da Republica Federativa do Brasil, the U. S. National Optical Astronomy Observatory (NOAO), the University of North Carolina at Chapel Hill (UNC), and Michigan State University (MSU). Support for this work was provided by the National Aeronautics and Space Administration through Chandra Award Number 12500613 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-NAS8-03060. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. L. C. is a Jansky Fellow of the National Radio Astronomy Observatory. G. P. acknowledges support from "proyecto regular UNAB" DI-28-11/R. All SAAO and SALT co-authors acknowledge the support from the National Research Foundation (NRF) of South Africa. A. B. was supported by a Marie Curie Outgoing International Fellowship (FP7) of the European Union (project number 275596). G. P., F. B., and J. A. acknowledge support provided by the Millennium Center for Supernova Science through grant P10-064-F (funded by " Programa Bicentenario de Ciencia y Tecnologia de CONICYT" and " Programa Iniciativa Cientifica Milenio de MIDEPLAN"). F. B. acknowledges support from FONDECYT through Postdoctoral grant 3120227. J. A. acknowledges support by CONICYT through FONDECYT grant 3110142, and by the Millennium Center for Supernova Science (P10-064-F), with input from the " Fondo de Innvacin para La Competitividad, de Ministerio de Economa, Fomento Y Turismo de Chile." Partially based on observations (program ID 184. D-1140) collected at the European Organisation for Astronomical Research in the Southern Hemisphere, Chile. S. B. is partially supported by the PRIN-INAF 2009 with the project " Supernovae Variety and Nucleosynthesis Yields." ESO VLT observations were taken within theGOprogram 089. D-0032 (PI: P. Mazzali) with UT1/FORS2. P. M. and E. P. acknowledge financial support from INAF PRIN 2011 and ASI-INAF grants I/088/06/0 and I/009/10/0. D. M, E. P., and P. M. thank the Institute of Nuclear Theory at University of Washington where part of this work was accomplished. This paper made extensive use of the SUSPECT database (http://www. nhn. ou. edu/~ suspect/). IRAF is distributed by the National Optical Astronomy Observatory, which is operated by the Association of Universities for Research in Astronomy (AURA) under cooperative agreement with theNational Science Foundation. PYRAF is a product of the Space Telescope Science Institute, which is operated by AURA for NASA. Dust maps were accessed via the NASA/IPAC Infrared Science archive at http://irsa. ipac. caltech. edu/applications/DUST/. NR 162 TC 30 Z9 30 U1 0 U2 15 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD APR 10 PY 2013 VL 767 IS 1 AR 71 DI 10.1088/0004-637X/767/1/71 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 117IT UT WOS:000316947500071 ER PT J AU Moustakas, J Coil, AL Aird, J Blanton, MR Cool, RJ Eisenstein, DJ Mendez, AJ Wong, KC Zhu, GT Arnouts, S AF Moustakas, John Coil, Alison L. Aird, James Blanton, Michael R. Cool, Richard J. Eisenstein, Daniel J. Mendez, Alexander J. Wong, Kenneth C. Zhu, Guangtun Arnouts, Stephane TI PRIMUS: CONSTRAINTS ON STAR FORMATION QUENCHING AND GALAXY MERGING, AND THE EVOLUTION OF THE STELLAR MASS FUNCTION FROM z=0-1 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: evolution; galaxies: high-redshift; large-scale structure of universe; surveys ID DIGITAL SKY SURVEY; COLOR-MAGNITUDE DIAGRAM; ASYMPTOTIC GIANT BRANCH; ACTIVE GALACTIC NUCLEI; SIMILAR-TO 2; OPTICAL LUMINOSITY FUNCTION; EXTRAGALACTIC SURVEY ESIS; SUPERMASSIVE BLACK-HOLES; FRANCE-HAWAII-TELESCOPE; SPITZER-SPACE-TELESCOPE AB We measure the evolution of the stellar mass function (SMF) from z = 0-1 using multi-wavelength imaging and spectroscopic redshifts from the PRismMUlti-object Survey (PRIMUS) and the Sloan Digital Sky Survey (SDSS). From PRIMUS we construct an i < 23 flux-limited sample of similar to 40,000 galaxies at z = 0.2-1.0 over five fields totaling approximate to 5.5 deg(2), and from the SDSS we select similar to 170,000 galaxies at z = 0.01-0.2 that we analyze consistently with respect to PRIMUS to minimize systematic errors in our evolutionary measurements. We find that the SMF of all galaxies evolves relatively little since z = 1, although we do find evidence for mass assembly downsizing; we measure a approximate to 30% increase in the number density of similar to 10(10) M-circle dot galaxies since z approximate to 0.6, and a less than or similar to 10% change in the number density of all greater than or similar to 10(11) M-circle dot galaxies since z approximate to 1. Dividing the sample into star-forming and quiescent using an evolving cut in specific star formation rate, we find that the number density of similar to 10(10) M-circle dot star-forming galaxies stays relatively constant since z approximate to 0.6, whereas the space density of greater than or similar to 10(11) M-circle dot star-forming galaxies decreases by similar to 50% between z approximate to 1 and z approximate to 0. Meanwhile, the number density of similar to 10(10) M-circle dot quiescent galaxies increases steeply toward low redshift, by a factor of similar to 2-3 since z approximate to 0.6, while the number of massive quiescent galaxies remains approximately constant since z approximate to 1. These results suggest that the rate at which star-forming galaxies are quenched increases with decreasing stellar mass, but that the bulk of the stellar mass buildup within the quiescent population occurs around similar to 10(10.8) M-circle dot. In addition, we conclude that mergers do not appear to be a dominant channel for the stellar mass buildup of galaxies at z < 1, even among massive (greater than or similar to 10(11) M-circle dot) quiescent galaxies. C1 [Moustakas, John] Siena Coll, Dept Phys & Astron, Loudonville, NY 12211 USA. [Coil, Alison L.; Mendez, Alexander J.] Univ Calif San Diego, Dept Phys, Ctr Astrophys & Space Sci, La Jolla, CA 92093 USA. [Aird, James] Univ Durham, Dept Phys, Durham DH1 3LE, England. [Blanton, Michael R.] NYU, Dept Phys, Ctr Cosmol & Particle Phys, New York, NY 10003 USA. [Cool, Richard J.] Univ Arizona, MMT Observ, Tucson, AZ 85721 USA. [Eisenstein, Daniel J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Wong, Kenneth C.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Zhu, Guangtun] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Arnouts, Stephane] Canada France Hawaii Telescope Corp, Kamuela, HI 96743 USA. [Arnouts, Stephane] Aix Marseille Univ, CNRS, LAM, UMR 7326, F-13388 Marseille, France. RP Moustakas, J (reprint author), Siena Coll, Dept Phys & Astron, 515 Loudon Rd, Loudonville, NY 12211 USA. EM jmoustakas@siena.edu RI Zhu, Guangtun/C-8552-2012; OI Zhu, Guangtun/0000-0002-7574-8078 FU NSF [AST-0607701, 0908246, 0908442, 0908354]; NASA [08-ADP08-0019, 08-ADP08-0072]; Alfred P. Sloan Foundation; NSF CAREER award [AST-1055081]; National Science Foundation; U.S. Department of Energy; National Aeronautics and Space Administration; Japanese Monbukagakusho; Max Planck Society; Higher Education Funding Council for England; American Museum of Natural History, Astrophysical Institute Potsdam, University of Basel; University of Cambridge; Case Western Reserve University; University of Chicago; Drexel University; Fermilab; Institute for Advanced Study; Japan Participation Group; Johns Hopkins University; Joint Institute for Nuclear Astrophysics; Kavli Institute for Particle Astrophysics and Cosmology; Korean Scientist Group; Chinese Academy of Sciences (LAMOST); Los Alamos National Laboratory; Max-Planck-Institute for Astronomy (MPIA); Max-Planck-Institute for Astrophysics (MPA); New Mexico State University; Ohio State University; University of Pittsburgh; University of Portsmouth; Princeton University; United States Naval Observatory; University of Washington FX Funding for PRIMUS has been provided by NSF grants AST-0607701, 0908246, 0908442, 0908354, and NASA grant 08-ADP08-0019. A. L. C. acknowledges support from the Alfred P. Sloan Foundation and NSF CAREER award AST-1055081, and M. R. B. acknowledges financial support through NASA grant 08-ADP08-0072.; 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; data products from the Wide-field Infrared Survey Explorer, which is a joint project of the University of California, Los Angeles, and the Jet Propulsion Laboratory/California Institute of Technology, funded by the National Aeronautics and Space Administration; 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; 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; and data products produced at TERAPIX and the Canadian Astronomy Data Centre as part of the Canada-France-Hawaii Telescope Legacy Survey, a collaborative project of NRC and CNRS. The Galaxy Evolution Explorer (GALEX) is a NASA Small Explorer, whose mission was developed in cooperation with the Centre National d'Etudes Spatiales of France and the Korean Ministry of Science and Technology. 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. The Participating Institutions are the American Museum of Natural History, Astrophysical Institute Potsdam, University of Basel, University of Cambridge, Case Western Reserve University, University of Chicago, Drexel University, Fermilab, the Institute for Advanced Study, the Japan Participation Group, Johns Hopkins University, the Joint Institute for Nuclear Astrophysics, the Kavli Institute for Particle Astrophysics and Cosmology, the Korean Scientist Group, the Chinese Academy of Sciences (LAMOST), Los Alamos National Laboratory, the Max-Planck-Institute for Astronomy (MPIA), the Max-Planck-Institute for Astrophysics (MPA), New Mexico State University, Ohio State University, University of Pittsburgh, University of Portsmouth, Princeton University, the United States Naval Observatory, and the University of Washington. NR 246 TC 182 Z9 182 U1 0 U2 9 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD APR 10 PY 2013 VL 767 IS 1 AR 50 DI 10.1088/0004-637X/767/1/50 PG 34 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 117IT UT WOS:000316947500050 ER PT J AU Rines, K Geller, MJ Diaferio, A Kurtz, MJ AF Rines, Kenneth Geller, Margaret J. Diaferio, Antonaldo Kurtz, Michael J. TI MEASURING THE ULTIMATE HALO MASS OF GALAXY CLUSTERS: REDSHIFTS AND MASS PROFILES FROM THE HECTOSPEC CLUSTER SURVEY (HeCS) SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology: observations; galaxies: clusters: general; galaxies: kinematics and dynamics ID DIGITAL SKY SURVEY; REGION NEARBY SURVEY; LARGE-SCALE STRUCTURE; X-RAY LUMINOSITY; INFALL REGION; RICH CLUSTERS; RADIO-HALO; LAMBDA-CDM; ENVIRONMENTAL DEPENDENCE; MULTIWAVELENGTH ANALYSIS AB The infall regions of galaxy clusters represent the largest gravitationally bound structures in a Lambda CDM universe. Measuring cluster mass profiles into the infall regions provides an estimate of the ultimate mass of these halos. We use the caustic technique to measure cluster mass profiles from galaxy redshifts obtained with the Hectospec Cluster Survey (HeCS), an extensive spectroscopic survey of galaxy clusters with MMT/Hectospec. We survey 58 clusters selected by X-ray flux at 0.1 < z < 0.3. The survey includes 22,680 unique MMT/Hectospec redshifts for individual galaxies; 10,145 of these galaxies are cluster members. For each cluster, we acquired high signal-to-noise spectra for similar to 200 cluster members and a comparable number of foreground/background galaxies. The cluster members trace out infall patterns around the clusters. The members define a very narrow red sequence. We demonstrate that the determination of velocity dispersion is insensitive to the inclusion of bluer members (a small fraction of the cluster population). We apply the caustic technique to define membership and estimate the mass profiles to large radii. The ultimate halo mass of clusters (the mass that remains bound in the far future of a Lambda CDM universe) is on average (1.99 +/- 0.11) M-200, a new observational cosmological test in essential agreement with simulations. Summed profiles binned in M-200 and in L-X demonstrate that the predicted Navarro-Frenk-White form of the density profile is a remarkably good representation of the data in agreement with weak lensing results extending to large radius. The concentration of these summed profiles is also consistent with theoretical predictions. C1 [Rines, Kenneth] Western Washington Univ, Dept Phys & Astron, Bellingham, WA 98225 USA. [Rines, Kenneth; Geller, Margaret J.; Kurtz, Michael J.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. [Diaferio, Antonaldo] Univ Turin, Dipartimento Fis, Turin, Italy. [Diaferio, Antonaldo] Ist Nazl Fis Nucl, Sez Torino, I-10125 Turin, Italy. RP Rines, K (reprint author), Western Washington Univ, Dept Phys & Astron, Bellingham, WA 98225 USA. EM kenneth.rines@wwu.edu; diaferio@ph.unito.it OI Kurtz, Michael/0000-0002-6949-0090 FU Cottrell College Science Award from the Research Corporation; INFN grant [PD51]; PRIN-MIUR; Smithsonian Institution; 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; Korean Scientist Group; Los Alamos National Laboratory; Max-Planck-Institute for Astronomy (MPIA); Max-Planck-Institute for Astrophysics (MPA); New Mexico State University; University of Pittsburgh; University of Portsmouth; Princeton University; United States Naval Observatory; University of Washington FX K.R. was funded by a Cottrell College Science Award from the Research Corporation. A. D. acknowledges partial support from the INFN grant PD51 and the PRIN-MIUR-2008 grant "Matter-antimatter asymmetry, dark matter and dark energy in the LHC Era." Research support for M. J. G. and M. J. K. is provided by the Smithsonian Institution. We thank YuYing Zhang, Keiichi Umetsu, Rien van de Weygaert, and the anonymous referee for helpful comments and suggestions.; 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, the Korean Scientist Group, 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, University of Portsmouth, Princeton University, the United States Naval Observatory, and the University of Washington. NR 111 TC 65 Z9 65 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 APR 10 PY 2013 VL 767 IS 1 AR 15 DI 10.1088/0004-637X/767/1/15 PG 21 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 117IT UT WOS:000316947500015 ER PT J AU Rogers, J Lopez-Morales, M Apai, D Adams, E AF Rogers, Justin Lopez-Morales, Mercedes Apai, Daniel Adams, Elisabeth TI BENCHMARK TESTS FOR MARKOV CHAIN MONTE CARLO FITTING OF EXOPLANET ECLIPSE OBSERVATIONS SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries: eclipsing; methods: analytical; methods: statistical; planetary systems; stars: individual (CoRoT-1); techniques: photometric ID INFRARED THERMAL EMISSION; GROUND-BASED DETECTION; LIGHT CURVES; SECONDARY ECLIPSE; EXTRASOLAR PLANET; HD 189733B; BAND DETECTION; HOT JUPITERS; WASP-12B; SPECTRUM AB Ground-based observations of exoplanet eclipses provide important clues to the planets' atmospheric physics, yet systematics in light curve analyses are not fully understood. It is unknown if measurements suggesting near-infrared flux densities brighter than models predict are real, or artifacts of the analysis processes. We created a large suite of model light curves, using both synthetic and real noise, and tested the common process of light curve modeling and parameter optimization with a Markov Chain Monte Carlo algorithm. With synthetic white noise models, we find that input eclipse signals are generally recovered within 10% accuracy for eclipse depths greater than the noise amplitude, and to smaller depths for higher sampling rates and longer baselines. Red noise models see greater discrepancies between input and measured eclipse signals, often biased in one direction. Finally, we find that in real data, systematic biases result even with a complex model to account for trends, and significant false eclipse signals may appear in a non-Gaussian distribution. To quantify the bias and validate an eclipse measurement, we compare both the planet-hosting star and several of its neighbors to a separately chosen control sample of field stars. Re-examining the Rogers et al. K s-band measurement of CoRoT-1b finds an eclipse 3190(-440)(+370) ppm deep centered at phi(me) = 0.50418(-0.00203)(+0.00197). Finally, we provide and recommend the use of selected data sets we generated as a benchmark test for eclipse modeling and analysis routines, and propose criteria to verify eclipse detections. C1 [Rogers, Justin] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Rogers, Justin; Lopez-Morales, Mercedes] Carnegie Inst Sci, Dept Terr Magnetism, Washington, DC 20015 USA. [Lopez-Morales, Mercedes; Adams, Elisabeth] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Apai, Daniel] Univ Arizona, Dept Astron, Tucson, AZ USA. [Apai, Daniel] Univ Arizona, Dept Planetary Sci, Tucson, AZ 85721 USA. RP Rogers, J (reprint author), Johns Hopkins Univ, Dept Phys & Astron, 366 Bloomberg Ctr,3400 N Charles St, Baltimore, MD 21218 USA. EM rogers@pha.jhu.edu FU National Science Foundation [AST-0908278]; Space Telescope Science Institute [D0101.90131] FX This research has been supported by the National Science Foundation through grant AST-0908278. Critical support was provided by the Space Telescope Science Institute Director's Discretionary Research Fund D0101.90131. We thank the scientific editor and the anonymous referee for insightful comments and suggestions, and Veselin Kostov for helpful discussion. NR 43 TC 7 Z9 7 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 APR 10 PY 2013 VL 767 IS 1 AR 64 DI 10.1088/0004-637X/767/1/64 PG 22 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 117IT UT WOS:000316947500064 ER PT J AU Sarma, AP Brogan, CL Bourke, TL Eftimova, M Troland, TH AF Sarma, A. P. Brogan, C. L. Bourke, T. L. Eftimova, M. Troland, T. H. TI VERY LARGE ARRAY OH ZEEMAN OBSERVATIONS OF THE STAR-FORMING REGION S88B SO ASTROPHYSICAL JOURNAL LA English DT Article DE H II regions; ISM: clouds; ISM: individual objects (S88B); ISM: kinematics and dynamics; ISM: magnetic fields; ISM: molecules ID H-II REGIONS; MAGNETIC-FIELD STRENGTHS; MOLECULAR CLOUDS; HIGH-RESOLUTION; AMBIPOLAR-DIFFUSION; DUST CLOUDS; HII-REGIONS; OUTFLOWS; EXCITATION; ENERGETICS AB We present observations of the Zeeman effect in OH thermal absorption main lines at 1665 and 1667 MHz taken with the Very Large Array toward the star-forming region S88B. The OH absorption profiles toward this source are complicated, and contain several blended components toward a number of positions. Almost all of the OH absorbing gas is located in the eastern parts of S88B, toward the compact continuum source S88B-2 and the eastern parts of the extended continuum source S88B-1. The ratio of 1665/1667 MHz OH line intensities indicates the gas is likely highly clumped, in agreement with other molecular emission line observations in the literature. S88-B appears to present a similar geometry to the well-known star-forming region M17, in that there is an edge-on eastward progression from ionized to molecular gas. The detected magnetic fields appear to mirror this eastward transition; we detected line-of-sight magnetic fields ranging from 90 to 400 mu G, with the lowest values of the field to the southwest of the S88B-1 continuum peak, and the highest values to its northeast. We used the detected fields to assess the importance of the magnetic field in S88B by a number of methods; we calculated the ratio of thermal to magnetic pressures, we calculated the critical field necessary to completely support the cloud against self-gravity and compared it to the observed field, and we calculated the ratio of mass to magnetic flux in terms of the critical value of this parameter. All these methods indicated that the magnetic field in S88B is dynamically significant, and should provide an important source of support against gravity. Moreover, the magnetic energy density is in approximate equipartition with the turbulent energy density, again pointing to the importance of the magnetic field in this region. C1 [Sarma, A. P.; Eftimova, M.] De Paul Univ, Dept Phys, Chicago, IL 60614 USA. [Brogan, C. L.] Natl Radio Astron Observ, Charlottesville, VA 22903 USA. [Bourke, T. L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Troland, T. H.] Univ Kentucky, Dept Phys & Astron, Lexington, KY 40506 USA. RP Sarma, AP (reprint author), De Paul Univ, Dept Phys, 2219 N Kenmore Ave,Byrne Hall 211, Chicago, IL 60614 USA. EM asarma@depaul.edu FU Cottrell College Science Award (CCSA) grant from Research Corporation; NSF [AST 03-07642] FX This work has been partially supported by a Cottrell College Science Award (CCSA) grant from Research Corporation to A. P. S., and by start-up funds to A. P. S. at DePaul University. T. H. T. acknowledges NSF grant AST 03-07642. We thank Kaisa Young (nee Mueller) and H. Saito for sending us digital versions of their data for comparison. We have used extensively the NASA Astrophysics Data System (ADS) astronomy abstract service, the astro-ph web server, and the SIMBAD database. NR 45 TC 2 Z9 2 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD APR 10 PY 2013 VL 767 IS 1 AR 24 DI 10.1088/0004-637X/767/1/24 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 117IT UT WOS:000316947500024 ER PT J AU Weiss, A De Breuck, C Marrone, DP Vieira, JD Aguirre, JE Aird, KA Aravena, M Ashby, MLN Bayliss, M Benson, BA Bethermin, M Biggs, AD Bleem, LE Bock, JJ Bothwell, M Bradford, CM Brodwin, M Carlstrom, JE Chang, CL Chapman, SC Crawford, TM Crites, AT de Haan, T Dobbs, MA Downes, TP Fassnacht, CD George, EM Gladders, MD Gonzalez, AH Greve, TR Halverson, NW Hezaveh, YD High, FW Holder, GP Holzapfel, WL Hoover, S Hrubes, JD Husband, K Keisler, R Lee, AT Leitch, EM Lueker, M Luong-Van, D Malkan, M McIntyre, V McMahon, JJ Mehl, J Menten, KM Meyer, SS Murphy, EJ Padin, S Plagge, T Reichardt, CL Rest, A Rosenman, M Ruel, J Ruhl, JE Schaffer, KK Shirokoff, E Spilker, JS Stalder, B Staniszewski, Z Stark, AA Story, K Vanderlinde, K Welikala, N Williamson, R AF Weiss, A. De Breuck, C. Marrone, D. P. Vieira, J. D. Aguirre, J. E. Aird, K. A. Aravena, M. Ashby, M. L. N. Bayliss, M. Benson, B. A. Bethermin, M. Biggs, A. D. Bleem, L. E. Bock, J. J. Bothwell, M. Bradford, C. M. Brodwin, M. Carlstrom, J. E. Chang, C. L. Chapman, S. C. Crawford, T. M. Crites, A. T. de Haan, T. Dobbs, M. A. Downes, T. P. Fassnacht, C. D. George, E. M. Gladders, M. D. Gonzalez, A. H. Greve, T. R. Halverson, N. W. Hezaveh, Y. D. High, F. W. Holder, G. P. Holzapfel, W. L. Hoover, S. Hrubes, J. D. Husband, K. Keisler, R. Lee, A. T. Leitch, E. M. Lueker, M. Luong-Van, D. Malkan, M. McIntyre, V. McMahon, J. J. Mehl, J. Menten, K. M. Meyer, S. S. Murphy, E. J. Padin, S. Plagge, T. Reichardt, C. L. Rest, A. Rosenman, M. Ruel, J. Ruhl, J. E. Schaffer, K. K. Shirokoff, E. Spilker, J. S. Stalder, B. Staniszewski, Z. Stark, A. A. Story, K. Vanderlinde, K. Welikala, N. Williamson, R. TI ALMA REDSHIFTS OF MILLIMETER-SELECTED GALAXIES FROM THE SPT SURVEY: THE REDSHIFT DISTRIBUTION OF DUSTY STAR-FORMING GALAXIES SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology: observations; early universe; galaxies: evolution; galaxies: high-redshift; ISM: molecules ID HUBBLE-DEEP-FIELD; SOUTH-POLE TELESCOPE; SCUBA SUPER-MAP; DEGREE EXTRAGALACTIC SURVEY; SUBMILLIMETER GALAXIES; MOLECULAR GAS; FORMATION HISTORY; NUMBER COUNTS; HERSCHEL ATLAS; LABOCA SURVEY AB Using the Atacama Large Millimeter/submillimeter Array, we have conducted a blind redshift survey in the 3 mm atmospheric transmission window for 26 strongly lensed dusty star- forming galaxies (DSFGs) selected with the South Pole Telescope. The sources were selected to have S-1.4mm > 20 mJy and a dust- like spectrum and, to remove low- z sources, not have bright radio (S-843MHz < 6 mJy) or far- infrared counterparts (S100 mu m < 1 Jy, S-60 mu m < 200 mJy). We robustly detect 44 line features in our survey, which we identify as redshifted emission lines of (CO)-C-12, (CO)-C-13, CI, H2O, and H2O+. We find one or more spectral features in 23 sources yielding a similar to 90% detection rate for this survey; in 12 of these sources we detect multiple lines, while in 11 sources we detect only a single line. For the sources with only one detected line, we break the redshift degeneracy with additional spectroscopic observations if available, or infer the most likely line identification based on photometric data. This yields secure redshifts for similar to 70% of the sample. The three sources with no lines detected are tentatively placed in the redshift desert between 1.7< z< 2.0. The resulting mean redshift of our sample is z = 3.5. This finding is in contrast to the redshift distribution of radio- identified DSFGs, which have a significantly lower mean redshift of z = 2.3 and for which only 10%- 15% of the population is expected to be at z> 3. We discuss the effect of gravitational lensing on the redshift distribution and compare our measured redshift distribution to that of models in the literature. C1 [Weiss, A.; Menten, K. M.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [De Breuck, C.; Aravena, M.; Biggs, A. D.] European So Observ, D-85748 Garching, Germany. [Marrone, D. P.; Bothwell, M.; Spilker, J. S.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Vieira, J. D.; Bock, J. J.; Downes, T. P.; Lueker, M.; Padin, S.; Shirokoff, E.; Staniszewski, Z.] CALTECH, Pasadena, CA 91125 USA. [Aguirre, J. E.; Rosenman, M.] Univ Penn, Philadelphia, PA 19104 USA. [Aird, K. A.; Hrubes, J. D.; Luong-Van, D.] Univ Chicago, Chicago, IL 60637 USA. [Ashby, M. L. N.; Bayliss, M.; Stalder, B.; Stark, A. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Bayliss, M.; Ruel, J.] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. [Benson, B. A.; Bleem, L. E.; Carlstrom, J. E.; Chang, C. L.; Crawford, T. M.; Crites, A. T.; Gladders, M. D.; High, F. W.; Hoover, S.; Keisler, R.; Leitch, E. M.; McMahon, J. J.; Mehl, J.; Meyer, S. S.; Padin, S.; Plagge, T.; Schaffer, K. K.; Story, K.; Williamson, R.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Benson, B. A.; Carlstrom, J. E.; Chang, C. L.; Hoover, S.; McMahon, J. J.; Meyer, S. S.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA. [Bethermin, M.] Univ Paris Diderot, CEA Saclay, CNRS, CEA,DSM,Irfu,Lab AIM Paris Saclay, F-91191 Gif Sur Yvette, France. [Bleem, L. E.; Carlstrom, J. E.; Keisler, R.; Meyer, S. S.; Story, K.] Univ Chicago, Dept Phys, Chicago, IL 60637 USA. [Bock, J. J.; Bradford, C. M.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Brodwin, M.] Univ Missouri, Dept Phys & Astron, Kansas City, MO 64110 USA. [Carlstrom, J. E.; Crawford, T. M.; Crites, A. T.; Gladders, M. D.; High, F. W.; Leitch, E. M.; Mehl, J.; Meyer, S. S.; Padin, S.; Plagge, T.; Williamson, R.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. [Carlstrom, J. E.; Chang, C. L.] Argonne Natl Lab, Argonne, IL 60439 USA. [Chapman, S. C.] Dalhousie Univ, Dept Phys & Atmospher Sci, Halifax, NS B3H 3J5, Canada. [Chapman, S. C.; Husband, K.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [de Haan, T.; Dobbs, M. A.; Hezaveh, Y. D.; Holder, G. P.; Vanderlinde, K.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada. [Fassnacht, C. D.] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA. [George, E. M.; Holzapfel, W. L.; Lee, A. T.; Reichardt, C. L.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. [Gonzalez, A. H.] Univ Florida, Dept Astron, Gainesville, FL 32611 USA. [Greve, T. R.] UCL, Dept Phys & Astron, London WC1E 6BT, England. [Halverson, N. W.] Univ Colorado, Dept Astrophys & Planetary Sci, Boulder, CO 80309 USA. [Halverson, N. W.] Univ Colorado, Dept Phys, Boulder, CO 80309 USA. [Lee, A. T.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Div Phys, Berkeley, CA 94720 USA. [Malkan, M.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. [McIntyre, V.] CSIRO, Australia Telescope Natl Facil, Epping, NSW 1710, Australia. [McMahon, J. J.] Univ Michigan, Dept Phys, Ann Arbor, MI 48109 USA. [Murphy, E. J.] Observ Carnegie Inst Sci, Pasadena, CA 91101 USA. [Rest, A.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Ruhl, J. E.; Staniszewski, Z.] Case Western Reserve Univ, Dept Phys, Ctr Educ & Res Cosmol & Astrophys, Cleveland, OH 44106 USA. [Schaffer, K. K.] Sch Art Inst Chicago, Liberal Arts Dept, Chicago, IL 60603 USA. [Welikala, N.] Univ Paris 11, Inst Astrophys Spatiale, F-91405 Orsay, France. [Welikala, N.] CNRS, F-91405 Orsay, France. RP Weiss, A (reprint author), Max Planck Inst Radioastron, Hugel 69, D-53121 Bonn, Germany. RI Aravena, Manuel/O-2361-2014; Williamson, Ross/H-1734-2015; Holzapfel, William/I-4836-2015; OI Williamson, Ross/0000-0002-6945-2975; Marrone, Daniel/0000-0002-2367-1080; Aird, Kenneth/0000-0003-1441-9518; Reichardt, Christian/0000-0003-2226-9169; De Breuck, Carlos/0000-0002-6637-3315; Bethermin, Matthieu/0000-0002-3915-2015; Stark, Antony/0000-0002-2718-9996 NR 85 TC 87 Z9 87 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 APR 10 PY 2013 VL 767 IS 1 AR 88 DI 10.1088/0004-637X/767/1/88 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 117IT UT WOS:000316947500088 ER PT J AU Perez, AEG Cunha, K Shetrone, M Majewski, SR Johnson, JA Smith, VV Schiavon, RP Holtzman, J Nidever, D Zasowski, G Prieto, CA Beers, TC Bizyaev, D Ebelke, G Eisenstein, DJ Frinchaboy, PM Girardi, L Hearty, FR Malanushenko, E Malanushenko, V Meszaros, S O'Connell, RW Oravetz, D Pan, KK Robin, AC Schneider, DP Schultheis, M Skrutskie, MF Simmonsand, A Wilson, JC AF Garcia Perez, Ana E. Cunha, Katia Shetrone, Matthew Majewski, Steven R. Johnson, Jennifer A. Smith, Verne V. Schiavon, Ricardo P. Holtzman, Jon Nidever, David Zasowski, Gail Allende Prieto, Carlos Beers, Timothy C. Bizyaev, Dmitry Ebelke, Garrett Eisenstein, Daniel J. Frinchaboy, Peter M. Girardi, Leo Hearty, Fred R. Malanushenko, Elena Malanushenko, Viktor Meszaros, Szabolcs O'Connell, Robert W. Oravetz, Daniel Pan, Kaike Robin, Annie C. Schneider, Donald P. Schultheis, Mathias Skrutskie, Michael F. Simmonsand, Audrey Wilson, John C. TI VERY METAL-POOR STARS IN THE OUTER GALACTIC BULGE FOUND BY THE APOGEE SURVEY SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE stars: abundances; stars: atmospheres; Galaxy: center; Galaxy: structure ID MILKY-WAY BULGE; FLAMES-GIRAFFE SPECTRA; CHEMICAL EVOLUTION; BAADES WINDOW; ABUNDANCE ANALYSIS; OXYGEN ABUNDANCES; THICK DISK; K GIANTS; METALLICITY DISTRIBUTION; INFRARED-SPECTROSCOPY AB Despite its importance for understanding the nature of early stellar generations and for constraining Galactic bulge formation models, at present little is known about the metal-poor stellar content of the central Milky Way. This is a consequence of the great distances involved and intervening dust obscuration, which challenge optical studies. However, the Apache Point Observatory Galactic Evolution Experiment (APOGEE), a wide-area, multifiber, high-resolution spectroscopic survey within Sloan Digital Sky Survey III, is exploring the chemistry of all Galactic stellar populations at infrared wavelengths, with particular emphasis on the disk and the bulge. An automated spectral analysis of data on 2403 giant stars in 12 fields in the bulge obtained during APOGEE commissioning yielded five stars with low metallicity ([Fe/H] <= -1.7), including two that are very metal-poor [Fe/H] similar to -2.1 by bulge standards. Luminosity-based distance estimates place the 5 stars within the outer bulge, where 1246 of the other analyzed stars may reside. A manual reanalysis of the spectra verifies the low metallicities, and finds these stars to be enhanced in the alpha-elements O, Mg, and Si without significant alpha-pattern differences with other local halo or metal-weak thick-disk stars of similar metallicity, or even with other more metal-rich bulge stars. While neither the kinematics nor chemistry of these stars can yet definitively determine which, if any, are truly bulge members, rather than denizens of other populations co-located with the bulge, the newly identified stars reveal that the chemistry of metal-poor stars in the central Galaxy resembles that of metal-weak thick-disk stars at similar metallicity. C1 [Garcia Perez, Ana E.; Majewski, Steven R.; Hearty, Fred R.; O'Connell, Robert W.; Skrutskie, Michael F.; Wilson, John C.] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA. [Cunha, Katia] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Cunha, Katia] Observ Nacl, Rio De Janeiro, Brazil. [Shetrone, Matthew] Univ Texas Austin, McDonald Observ, Ft Davis, TX 79734 USA. [Johnson, Jennifer A.; Zasowski, Gail] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. [Smith, Verne V.; Beers, Timothy C.] Natl Opt Astron Observ, Tucson, AZ 85719 USA. [Schiavon, Ricardo P.] Gemini Observ, Hilo, HI 96720 USA. [Holtzman, Jon] New Mexico State Univ, Dept Astron, Las Cruces, NM 88003 USA. [Nidever, David] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Allende Prieto, Carlos] Univ La Laguna, Dept Astrofis, E-38206 Tenerife, Spain. [Allende Prieto, Carlos; Meszaros, Szabolcs] Inst Astrofis Canarias, E-38205 Tenerife, Spain. [Beers, Timothy C.] Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA. [Beers, Timothy C.] Michigan State Univ, JINA, E Lansing, MI 48824 USA. [Bizyaev, Dmitry; Ebelke, Garrett; Malanushenko, Elena; Malanushenko, Viktor; Oravetz, Daniel; Pan, Kaike; Simmonsand, Audrey] Apache Point Observ, Sunspot, NM 88349 USA. [Eisenstein, Daniel J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Frinchaboy, Peter M.] Texas Christian Univ, Dept Phys & Astron, Ft Worth, TX 76129 USA. [Girardi, Leo] Lab Interinst & Astron LIneA, BR-20921400 Rio De Janeiro, RJ, Brazil. [Girardi, Leo] Osserv Astron Padova, INAF, I-35122 Padua, Italy. [Robin, Annie C.; Schultheis, Mathias] Univ Franche Comte, OSU THETA, Inst Utinam, CNRS UMR6213, F-25000 Besancon, France. [Schneider, Donald P.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. RP Perez, AEG (reprint author), Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA. RI Meszaros, Szabolcs/N-2287-2014 OI Meszaros, Szabolcs/0000-0001-8237-5209 FU NSF [AST11-09718, AST-907873]; Alfred P. Sloan Foundation; National Science Foundation; U.S. Department of Energy Office of Science FX We acknowledge funding from NSF grants AST11-09718 and AST-907873. Funding for SDSS-III has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, and the U.S. Department of Energy Office of Science. The SDSS-III Web site is http://www.sdss3.org/.SDSS-III is managed by the Astrophysical Research Consortium for the Participating Institutions of the SDSS-III Collaboration including the University of Arizona, the Brazilian Participation Group, Brookhaven National Laboratory, University of Cambridge, Carnegie Mellon University, University of Florida, the French Participation Group, the German Participation Group, Harvard University, the Instituto de Astrofisica de Canarias, the Michigan State/Notre Dame/JINA Participation Group, Johns Hopkins University, Lawrence Berkeley National Laboratory, Max Planck Institute for Astrophysics, Max Planck Institute for Extraterrestrial Physics, New Mexico State University, New York University, Ohio State University, Pennsylvania State University, University of Portsmouth, Princeton University, the Spanish Participation Group, University of Tokyo, University of Utah, Vanderbilt University, University of Virginia, University of Washington, and Yale University. NR 49 TC 22 Z9 22 U1 0 U2 5 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 APR 10 PY 2013 VL 767 IS 1 AR L9 DI 10.1088/2041-8205/767/1/L9 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 118CB UT WOS:000316998900009 ER PT J AU Neufeld, DA Tolls, V Agundez, M Gonzalez-Alfonso, E Decin, L Daniel, F Cernicharo, J Melnick, GJ Schmidt, M Szczerba, R AF Neufeld, David A. Tolls, Volker Agundez, Marcelino Gonzalez-Alfonso, Eduardo Decin, Leen Daniel, Fabien Cernicharo, Jose Melnick, Gary J. Schmidt, Miroslaw Szczerba, Ryszard TI HERSCHEL/HIFI SEARCH FOR (H2O)-O-17 AND (H2O)-O-18 IN IRC+10216: CONSTRAINTS ON MODELS FOR THE ORIGIN OF WATER VAPOR SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE circumstellar matter; stars: abundances; stars: AGB and post-AGB ID GIANT BRANCH STARS; CIRCUMSTELLAR ENVELOPES; MOLECULAR-SPECTROSCOPY; COLOGNE DATABASE; LINE SURVEY; CARBON; SUBMILLIMETER; CHEMISTRY; HIFI; CDMS AB We report the results of a sensitive search for the minor isotopologues of water, (H2O)-O-17 and (H2O)-O-18, toward the carbon-rich asymptotic giant branch star IRC+10216 (a.k.a. CW Leonis) using the HIFI instrument on the Herschel Space Observatory. This search was motivated by the fact that any detection of isotopic enhancement in the (H2O)-O-17 and (H2O)-O-18 abundances would have strongly implicated CO photodissociation as the source of the atomic oxygen needed to produce water in a carbon-rich circumstellar envelope. Our observations place an upper limit of 1/470 on the (H2O)-O-17 and (H2O)-O-16 abundance ratio. Given the isotopic O-17/O-16 ratio of 1/840 inferred previously for the photosphere of IRC+10216, this result places an upper limit of a factor 1.8 on the extent of any isotope-selective enhancement of (H2O)-O-17 in the circumstellar material, and provides an important constraint on any model that invokes CO photodissociation as the source of O for H2O production. In the context of the clumpy photodissociation model proposed previously for the origin of water in IRC+10216, our limit implies that (CO)-C-12-O-16 ( not (CO)-C-13-O-16 or SiO) must be the dominant source of O-16 for H2O production, and that the effects of self-shielding can only have reduced the (CO)-C-12-O-16 photodissociation rate by at most a factor similar to 2. C1 [Neufeld, David A.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Tolls, Volker; Melnick, Gary J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Agundez, Marcelino] Univ Bordeaux, LAB, UMR 5804, F-33270 Floirac, France. [Agundez, Marcelino] CNRS, LAB, UMR 5804, F-33270 Floirac, France. [Gonzalez-Alfonso, Eduardo] Univ Alcala de Henares, Dept Fis & Matemat, E-28871 Madrid, Spain. [Decin, Leen] Katholieke Univ Leuven, Inst Sterrenkunde, B-3001 Louvain, Belgium. [Decin, Leen] Univ Amsterdam, Sterrenkundig Inst Anton Pannekoek, NL-1098 Amsterdam, Netherlands. [Daniel, Fabien; Cernicharo, Jose] CSIC INTA, Ctr Astrobiol, Dept Astrofis, E-28850 Madrid, Spain. [Schmidt, Miroslaw; Szczerba, Ryszard] Polish Acad Sci, Nicolaus Copernicus Astron Ctr, PL-87100 Torun, Poland. RP Neufeld, DA (reprint author), Johns Hopkins Univ, Dept Phys & Astron, 3400 North Charles St, Baltimore, MD 21218 USA. RI Agundez, Marcelino/I-5369-2012 OI Agundez, Marcelino/0000-0003-3248-3564 FU National Aeronautics and Space Administration; Spanish Ministerio de Ciencia e Innovacion [AYA2010-21697-C05-01]; Polish NCN grant [203 581040] FX This research was performed, in part, through a JPL contract funded by the National Aeronautics and Space Administration. E.G.-A. is a Research Associate at the Harvard-Smithsonian Center for Astrophysics, and thanks the Spanish Ministerio de Ciencia e Innovacion for support under project AYA2010-21697-C05-01. R.S. and M.S. acknowledge support from Polish NCN grant No. 203 581040. NR 26 TC 4 Z9 4 U1 1 U2 8 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 APR 10 PY 2013 VL 767 IS 1 AR L3 DI 10.1088/2041-8205/767/1/L3 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 118CB UT WOS:000316998900003 ER PT J AU Park, S Badenes, C Mori, K Kaida, R Bravo, E Schenck, A Eriksen, KA Hughes, JP Slane, PO Burrows, DN Lee, JJ AF Park, Sangwook Badenes, Carles Mori, Koji Kaida, Ryohei Bravo, Eduardo Schenck, Andrew Eriksen, Kristoffer A. Hughes, John P. Slane, Patrick O. Burrows, David N. Lee, Jae-Joon TI A SUPER-SOLAR METALLICITY FOR THE PROGENITOR OF KEPLER'S SUPERNOVA SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE ISM: individual objects (Kepler's supernova remnants); ISM: supernova remnants; X-rays: ISM ID CHANDRASEKHAR-MASS MODELS; X-RAY-SPECTRUM; IA SUPERNOVAE; REMNANT; CONSTRAINTS; EMISSION AB We have performed deep X-ray observations of the remnant of Kepler's supernova (SN 1604) as a Key Project of the Suzaku Observatory. Our main goal is to detect secondary Fe-peak elements in the supernova (SN) ejecta to gain insights into the Type Ia SN explosion mechanism and the nature of the progenitor. Here, we report our initial results. We made a conclusive detection of X-ray emission lines from highly ionized Mn, Cr, and Ni as well as Fe. The observed Mn-to-Cr line flux ratio is similar to 0.60, similar to 30% larger than that measured in Tycho's remnant. We estimate an Mn-to-Cr mass ratio of similar to 0.77, which is strongly suggestive of a large neutron excess in the progenitor star before the onset of the thermonuclear runaway. The observed Ni-to-Fe line flux ratio (similar to 0.03) corresponds to a mass ratio of similar to 0.06, which is generally consistent with the products of the explosive Si-burning regime in Type Ia explosion models, and rules out contamination from the products of neutron-rich nuclear statistical equilibrium in the shocked ejecta. Together with the previously suggested luminous nature of the explosion, these mass ratios provide strong evidence for a super-solar metallicity in the SN progenitor (similar to 3 Z(circle dot)). Kepler's SN was likely the thermonuclear explosion of a white dwarf formed in the recent past that must have exploded through a relatively prompt channel. C1 [Park, Sangwook; Schenck, Andrew] Univ Texas Arlington, Dept Phys, Arlington, TX 76019 USA. [Badenes, Carles] Univ Pittsburgh, Dept Phys & Astron, Pittsburgh, PA 15260 USA. [Badenes, Carles] Univ Pittsburgh, Pittsburgh Particle Phys Astrophys & Cosmol Ctr P, Pittsburgh, PA 15260 USA. [Mori, Koji; Kaida, Ryohei] Miyazaki Univ, Dept Appl Phys, Miyazaki 8892192, Japan. [Bravo, Eduardo] Univ Politecn Cataluna, Dept Fis & Engn Nucl, E-08173 Sant Cugat Del Valles, Spain. [Eriksen, Kristoffer A.] Los Alamos Natl Lab, XDT 6, Los Alamos, NM 87545 USA. [Hughes, John P.] Rutgers State Univ, Dept Phys & Astron, Piscataway, NJ 08854 USA. [Slane, Patrick O.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Burrows, David N.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Lee, Jae-Joon] Korea Astron & Space Sci Inst, Taejon 305348, South Korea. RP Park, S (reprint author), Univ Texas Arlington, Dept Phys, Box 19059, Arlington, TX 76019 USA. EM s.park@uta.edu; badenes@pitt.edu RI XRAY, SUZAKU/A-1808-2009; OI Bravo, Eduardo/0000-0003-0894-6450 FU NASA [NNX09AV42G, NNX10AR47G, NAS8-03060]; MEXT [24740167] FX The authors thank H. Kai and T. Yoshidome for their help with the XIS instrumental background investigation. This work has been supported in part by the NASA grants NNX09AV42G and NNX10AR47G. The work of K.M. has been partially supported by the Grant-in-Aid for Young Scientists (B) of the MEXT (No. 24740167). P.O.S. acknowledges partial support from NASA contract NAS8-03060. NR 31 TC 9 Z9 9 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 APR 10 PY 2013 VL 767 IS 1 AR L10 DI 10.1088/2041-8205/767/1/L10 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 118CB UT WOS:000316998900010 ER PT J AU Leray, M Agudelo, N Mills, SC Meyer, CP AF Leray, Matthieu Agudelo, Natalia Mills, Suzanne C. Meyer, Christopher P. TI Effectiveness of Annealing Blocking Primers versus Restriction Enzymes for Characterization of Generalist Diets: Unexpected Prey Revealed in the Gut Contents of Two Coral Reef Fish Species SO PLOS ONE LA English DT Article ID POLYMERASE-CHAIN-REACTION; DNA BARCODES; INVERTEBRATE PREDATORS; SECONDARY PREDATION; MOLECULAR APPROACH; ANTARCTIC KRILL; PCR; SEQUENCES; AMPLIFICATION; IDENTIFICATION AB Characterization of predator-prey interactions is challenging as researchers have to rely on indirect methods that can be costly, biased and too imprecise to elucidate the complexity of food webs. DNA amplification and sequencing techniques of gut and fecal contents are promising approaches, but their success largely depends on the ability to amplify the taxonomic array of prey consumed and then match prey amplicons with reference sequences. When little a priori information on diet is available or a generalist predator is targeted, versatile primer sets (also referred to as universal or general primers) as opposed to group- or species-specific primer sets are the most powerful to unveil the full range of prey consumed. However, versatile primers are likely to preferentially amplify the predominant, less degraded predator DNA if no manipulation is performed to exclude this confounding DNA template. In this study we compare two approaches that eliminate the confounding predator template: restriction digestion and the use of annealing blocking primers. First, we use a preliminary DNA barcode library provided by the Moorea BIOCODE project to 1) evaluate the cutting frequency of commercially available restriction enzymes and 2) design predator specific annealing blocking primers. We then compare the performance of the two predator removal strategies for the detection of prey templates using two versatile primer sets from the gut contents of two generalist coral reef fish species sampled in Moorea. Our study demonstrates that blocking primers should be preferentially used over restriction digestion for predator DNA removal as they recover greater prey diversity. We also emphasize that a combination of versatile primers may be required to best represent the breadth of a generalist's diet. C1 [Leray, Matthieu; Mills, Suzanne C.] Univ Perpignan, CBETM, USR CRIOBE CNRS EPHE 3278, Lab Excellence Corail, F-66025 Perpignan, France. [Leray, Matthieu; Agudelo, Natalia; Meyer, Christopher P.] Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, Washington, DC 20560 USA. RP Leray, M (reprint author), Univ Perpignan, CBETM, USR CRIOBE CNRS EPHE 3278, Lab Excellence Corail, F-66025 Perpignan, France. EM leray.upmc@gmail.com RI Mills, Suzanne/K-5538-2012 FU Gordon and Betty Moore Foundation; Smithsonian Institution Fellowship Program; France American Cultural Exchange program (FACE - puf) FX This work was funded by the Gordon and Betty Moore Foundation, Smithsonian Institution Fellowship Program and France American Cultural Exchange program (FACE - puf). The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 69 TC 7 Z9 7 U1 6 U2 64 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 APR 8 PY 2013 VL 8 IS 4 AR e58076 DI 10.1371/journal.pone.0058076 PG 11 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 130FG UT WOS:000317898000002 PM 23579925 ER PT J AU Bhongale, SG Mathey, L Zhao, EH Yelin, SF Lemeshko, M AF Bhongale, S. G. Mathey, L. Zhao, Erhai Yelin, S. F. Lemeshko, Mikhail TI Quantum Phases of Quadrupolar Fermi Gases in Optical Lattices SO PHYSICAL REVIEW LETTERS LA English DT Article ID MANY-BODY PHYSICS; RYDBERG ATOMS; MOLECULES AB We introduce a new platform for quantum simulation of many-body systems based on nonspherical atoms or molecules with zero dipole moments but possessing a significant value of electric quadrupole moments. We consider a quadrupolar Fermi gas trapped in a 2D square optical lattice, and show that the peculiar symmetry and broad tunability of the quadrupole-quadrupole interaction results in a rich phase diagram encompassing unconventional BCS and charge density wave phases, and opens up a perspective to create a topological superfluid. Quadrupolar species, such as metastable alkaline-earth atoms and homonuclear molecules, are stable against chemical reactions and collapse and are readily available in experiment at high densities. DOI: 10.1103/PhysRevLett.110.155301 C1 [Bhongale, S. G.; Zhao, Erhai] George Mason Univ, Sch Phys Astron & Computat Sci, Fairfax, VA 22030 USA. [Mathey, L.] Univ Hamburg, Zentrum Opt Quantentechnol, D-22761 Hamburg, Germany. [Mathey, L.] Univ Hamburg, Inst Laserphys, D-22761 Hamburg, Germany. [Yelin, S. F.] Univ Connecticut, Dept Phys, Storrs, CT 06269 USA. [Yelin, S. F.; Lemeshko, Mikhail] Harvard Smithsonian Ctr Astrophys, ITAMP, Cambridge, MA 02138 USA. [Yelin, S. F.; Lemeshko, Mikhail] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. RP Bhongale, SG (reprint author), George Mason Univ, Sch Phys Astron & Computat Sci, Fairfax, VA 22030 USA. EM mlemeshko@cfa.harvard.edu RI Mathey, Ludwig/A-9644-2009; Zhao, Erhai/B-3463-2010 OI Zhao, Erhai/0000-0001-8954-1601 FU NSF [PHY-1205504]; NIST [60NANB12D244]; Landesexzellenzinitiative Hamburg; Science and Research Foundation Hamburg; Joachim Herz Stiftung; Deutsche Forschungsgemeinschaft [SFB 925]; NSF; National Science Foundation; Air Force Office of Scientific Research FX We are grateful to Charles Clark, Robin Cote, Hendrik Weimer, and Shan-Wen Tsai for discussions. S.G.B. and E.Z. are supported by NSF (Grant No. PHY-1205504) and NIST (Grant No. 60NANB12D244). L.M. acknowledges support from the Landesexzellenzinitiative Hamburg, which is financed by the Science and Research Foundation Hamburg and supported by the Joachim Herz Stiftung, and from the Deutsche Forschungsgemeinschaft under Grant No. SFB 925. M.L. acknowledges support from NSF through a grant for the Institute for Theoretical Atomic, Molecular, and Optical Physics at Harvard University and Smithsonian Astrophysical Observatory. S.F.Y. acknowledges financial support from the National Science Foundation and Air Force Office of Scientific Research. NR 45 TC 17 Z9 17 U1 0 U2 9 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 APR 8 PY 2013 VL 110 IS 15 AR 155301 DI 10.1103/PhysRevLett.110.155301 PG 5 WC Physics, Multidisciplinary SC Physics GA 120SD UT WOS:000317191400012 PM 25167282 ER PT J AU Mason, RP Schartup, AT Hollweg, TA Blacom, PH Gilmour, CC AF Mason, Robert P. Schartup, Amina T. Hollweg, Terill A. Blacom, Prentiss H. Gilmour, Cynthia C. TI Examining the role of sulfur in the biogeochemical cycling of mercury and methylmercury in coastal sediments through measurements and models SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY LA English DT Meeting Abstract CT 245th National Spring Meeting of the American-Chemical-Society (ACS) CY APR 07-11, 2013 CL New Orleans, LA SP Amer Chem Soc C1 [Mason, Robert P.; Schartup, Amina T.; Blacom, Prentiss H.] Univ Connecticut, Dept Marine Sci, Groton, CT 06340 USA. [Schartup, Amina T.] Harvard Univ, Sch Publ Hlth, Boston, MA 02115 USA. [Hollweg, Terill A.] Stratus Consulting Inc, Boulder, CO 80302 USA. [Gilmour, Cynthia C.] Smithsonian, Environm Res Ctr, Edgewater, MD 21037 USA. EM robert.mason@uconn.edu NR 0 TC 0 Z9 0 U1 0 U2 6 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0065-7727 J9 ABSTR PAP AM CHEM S JI Abstr. Pap. Am. Chem. Soc. PD APR 7 PY 2013 VL 245 MA 175-GEOC PG 1 WC Chemistry, Multidisciplinary SC Chemistry GA 216SF UT WOS:000324303600422 ER PT J AU Davenport, S Yin, Q Mark, D Harelimana, I Schulte, B Brown, J Goodwin, T AF Davenport, Stephanie Yin, Qin Mark, Daniel Harelimana, Innocent Schulte, Bruce Brown, Janine Goodwin, Thomas TI Urinary chemical signals of musth in immature male African elephants SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY LA English DT Meeting Abstract CT 245th National Meeting of the American-Chemical-Society (ACS) CY APR 07-11, 2013 CL New Orleans, LA SP Amer Chem Soc C1 [Davenport, Stephanie; Yin, Qin; Mark, Daniel; Harelimana, Innocent; Goodwin, Thomas] Hendrix Coll, Dept Chem, Conway, AR 72032 USA. [Schulte, Bruce] Western Kentucky Univ, Dept Biol, Bowling Green, KY 42101 USA. [Brown, Janine] Natl Zool Pk, Smithsonian Conservat Biol Inst, Front Royal, VA 22630 USA. EM goodwin@hendrix.edu NR 0 TC 0 Z9 0 U1 2 U2 9 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0065-7727 J9 ABSTR PAP AM CHEM S JI Abstr. Pap. Am. Chem. Soc. PD APR 7 PY 2013 VL 245 MA 1158-CHED PG 1 WC Chemistry, Multidisciplinary SC Chemistry GA 210RD UT WOS:000323851302933 ER PT J AU Zhang, JY Mitroy, J Yan, ZC Babb, JF Sadeghpour, HR Schwingenschlogl, U AF Zhang, J. -Y. Mitroy, J. Yan, Z. -C. Babb, J. F. Sadeghpour, H. R. Schwingenschloegl, U. TI Long-range interactions of excited He atoms with the alkaline earth atoms Mg, Ca, and Sr SO JOURNAL OF CHEMICAL PHYSICS LA English DT Article ID METASTABLE HELIUM-ATOMS; PENNING-IONIZATION; CROSS-SECTIONS; SOLID-SURFACES; RYDBERG ATOMS; DISPERSION; MOLECULES; STATES; IONS; NE AB Dispersion coefficients for the long-range interactions of the first four excited states of He, i.e., He(2 S-1,S- 3) and He(2 P-1,P- 3), with the low-lying states of the alkaline earth atoms Mg, Ca, and Sr are calculated by summing over the reduced matrix elements of multipole transition operators. (C) 2013 American Institute of Physics. [http://dx.doi.org/10.1063/1.4794048] C1 [Zhang, J. -Y.; Schwingenschloegl, U.] King Abdullah Univ Sci & Technol, Div Phys Sci & Engn, Thuwal 239556900, Saudi Arabia. [Mitroy, J.] Charles Darwin Univ, Sch Engn, Darwin, NT 0909, Australia. [Yan, Z. -C.] Chinese Acad Sci, Wuhan Inst Phys & Math, State Key Lab Magnet Resonance & Atom & Mol Phys, Wuhan 430071, Peoples R China. [Yan, Z. -C.] Chinese Acad Sci, Ctr Cold Atom Phys, Wuhan 430071, Peoples R China. [Yan, Z. -C.] Univ New Brunswick, Dept Phys, Fredericton, NB E3B 5A3, Canada. [Babb, J. F.; Sadeghpour, H. R.] Harvard Smithsonian Ctr Astrophys, ITAMP, Cambridge, MA 02138 USA. RP Zhang, JY (reprint author), King Abdullah Univ Sci & Technol, Div Phys Sci & Engn, Thuwal 239556900, Saudi Arabia. EM Junyi.Zhang@kaust.edu.sa; Udo.Schwingenschlogl@kaust.edu.sa RI Mitroy, James/N-2162-2013; Yan, Zong-Chao/F-6668-2014 OI Mitroy, James/0000-0002-2477-1251; FU NSERC of Canada; Canadian computing facilities of SHARCnet; ACEnet; Chinese Academy of Sciences CAS/SAFEA International Partnership Program for Creative Research Teams; National Science Foundation through; Smithsonian Astrophysical Observatory FX Z.-C. Yan was supported by the NSERC of Canada, by the Canadian computing facilities of SHARCnet and ACEnet, and in part by the Chinese Academy of Sciences CAS/SAFEA International Partnership Program for Creative Research Teams. J. F. Babb and H. R. Sadeghpour were supported by the National Science Foundation through a grant for the Institute of Theoretical Atomic, Molecular, and Optical Physics at Harvard University and Smithsonian Astrophysical Observatory. NR 40 TC 1 Z9 1 U1 0 U2 12 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 APR 7 PY 2013 VL 138 IS 13 AR 134317 DI 10.1063/1.4794048 PG 6 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA 128SG UT WOS:000317788500036 PM 23574237 ER PT J AU Thompson, RC Allam, AH Lombardi, GP Wann, LS Sutherland, ML Sutherland, JD Soliman, MA Frohlich, B Mininberg, DT Monge, JM Vallodolid, CM Cox, SL Abd el-Maksoud, G Badr, I Miyamoto, MI el-Din, AEN Narula, J Finch, CE Thomas, GS AF Thompson, Randall C. Allam, Adel H. Lombardi, Guido P. Wann, L. Samuel Sutherland, M. Linda Sutherland, James D. Soliman, Muhammad Al-Tohamy Frohlich, Bruno Mininberg, David T. Monge, Janet M. Vallodolid, Clide M. Cox, Samantha L. Abd el-maksoud, Gomaa Badr, Ibrahim Miyamoto, Michael I. el-Din, Abd el-Halim Nur Narula, Jagat Finch, Caleb E. Thomas, Gregory S. TI Atherosclerosis across 4000 years of human history: the Horus study of four ancient populations SO LANCET LA English DT Article ID EGYPTIAN MUMMIES; LESIONS AB Background Atherosclerosis is thought to be a disease of modern human beings and related to contemporary lifestyles. However, its prevalence before the modern era is unknown. We aimed to evaluate preindustrial populations for atherosclerosis. Methods We obtained whole body CT scans of 137 mummies from four different geographical regions or populations spanning more than 4000 years. Individuals from ancient Egypt, ancient Peru, the Ancestral Puebloans of southwest America, and the Unangan of the Aleutian Islands were imaged. Atherosclerosis was regarded as definite if a calcified plaque was seen in the wall of an artery and probable if calcifications were seen along the expected course of an artery. Findings Probable or definite atherosclerosis was noted in 47 (34%) of 137 mummies and in all four geographical populations: 29 (38%) of 76 ancient Egyptians, 13 (25%) of 51 ancient Peruvians, two (40%) of five Ancestral Puebloans, and three (60%) of five Unangan hunter gatherers (p=NS). Atherosclerosis was present in the aorta in 28 (20%) mummies, iliac or femoral arteries in 25 (18%), popliteal or tibial arteries in 25 (18%), carotid arteries in 17 (12%), and coronary arteries in six (4%). Of the five vascular beds examined, atherosclerosis was present in one to two beds in 34 (25%) mummies, in three to four beds in 11 (8%), and in all five vascular beds in two (1%). Age at time of death was positively correlated with atherosclerosis (mean age at death was 43 [SD 10] years for mummies with atherosclerosis vs 32 [15] years for those without; p<0.0001) and with the number of arterial beds involved (mean age was 32 [SD 15] years for mummies with no atherosclerosis, 42 [10] years for those with atherosclerosis in one or two beds, and 44 [8] years for those with atherosclerosis in three to five beds; p<0.0001). Interpretation Atherosclerosis was common in four preindustrial populations including preagricultural hunter-gatherers. Although commonly assumed to be a modern disease, the presence of atherosclerosis in premodern human beings raises the possibility of a more basic predisposition to the disease. C1 [Thompson, Randall C.] St Lukes Mid Amer Heart Inst, Kansas City, MO 64111 USA. [Thompson, Randall C.] Univ Missouri, Sch Med, Kansas City, MO 64108 USA. [Allam, Adel H.] Azhar Med Sch, Cairo, Egypt. [Lombardi, Guido P.] Catedra Pedro Weiss, Lab Paleopatol, Lima, Peru. [Lombardi, Guido P.] Univ Peruana Cayetano Heredia, Lima, Peru. [Wann, L. Samuel] Columbia St Marys Healthcare, Milwaukee, WI USA. [Sutherland, M. Linda] Newport Diagnost Ctr, Newport Beach, CA USA. [Sutherland, James D.] South Coast Radiol Med Grp, Laguna Hills, CA USA. [Soliman, Muhammad Al-Tohamy] Natl Res Ctr, Giza, Egypt. [Frohlich, Bruno] Natl Museum Nat Hist, Smithsonian Inst, Washington, DC 20560 USA. [Mininberg, David T.] Metropolitan Museum Art, New York, NY 10028 USA. [Mininberg, David T.] Weill Cornell Med Coll, New York, NY USA. [Monge, Janet M.; Cox, Samantha L.] Univ Penn, Museum Archaeol & Anthropol, Philadelphia, PA 19104 USA. [Vallodolid, Clide M.] Museo Sitio Puruchuco Arturo Jimenez Borja, Lima, Peru. [Cox, Samantha L.] Univ Cambridge, Cambridge, England. [Abd el-maksoud, Gomaa; el-Din, Abd el-Halim Nur] Cairo Univ, Cairo, Egypt. [Badr, Ibrahim] Inst Restorat, Alexandria, Egypt. [Miyamoto, Michael I.] Mission Internal Med Grp, Mission Viejo, CA USA. [el-Din, Abd el-Halim Nur] Univ Sci & Technol, 6th October City, Egypt. [Narula, Jagat] Mt Sinai, New York, NY USA. [Finch, Caleb E.] Univ So Calif, Los Angeles, CA USA. [Thomas, Gregory S.] Long Beach Mem Med Ctr, Long Beach, CA USA. [Thomas, Gregory S.] Univ Calif Irvine, Irvine, CA USA. RP Thompson, RC (reprint author), St Lukes Mid Amer Heart Inst, Kansas City, MO 64111 USA. EM rthompson@saint-lukes.org RI Al-Tohamy, Muhammad/B-4273-2016 OI Al-Tohamy, Muhammad/0000-0001-9368-2570 FU National Endowment for the Humanities [HJ-50069-12]; Paleocardiology Foundation; Siemens; National Bank of Egypt; St Luke's Hospital Foundation of Kansas City; National Endowment for the Humanities FX National Endowment for the Humanities, Paleocardiology Foundation, The National Bank of Egypt, Siemens, and St Luke's Hospital Foundation of Kansas City.; Funding for the study was supplied by the National Endowment for the Humanities (#HJ-50069-12), the Paleocardiology Foundation, Siemens, the National Bank of Egypt, and the St Luke's Hospital Foundation of Kansas City. The study also would not have been possible without the generosity of numerous museum and medical personnel who aided in the CT scanning or provided essential CT images or anthropological data. We thank the Metropolitan Museum of Art for generously providing us with full access to the data that they had gathered for their 1997 study.10 We also thank Kevin F Kennedy of the Saint Luke's Mid America Heart Institute for statistical analysis, John N Makaryus and Amgad N Makaryus of the North Shore LIJ Health System for providing the CT data for mummies 71-76, Jon Kardatzke of the Museum of World Treasures, Wichita, KS, for access to the CT data for mummies 68 and 69, Sallam Lotfy Mohamed of Alfascan, Cairo, Egypt, for his expert postprocessing CT assistance, Hany Abd el-Rahman Amer of the National Research Center, Giza, Egypt, for his skilled assistance in the imaging of mummies 1-44, Yrma Soledad Quispe Zapana of the Instituto Nacional de Ciencias Neurologicas, Lima, Peru for making possible the CT scanning of mummies 79-113 and 123-127 and Janet Oshiro, for her anthropological research in Peru. NR 30 TC 80 Z9 85 U1 2 U2 37 PU ELSEVIER SCIENCE INC PI NEW YORK PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA SN 0140-6736 EI 1474-547X J9 LANCET JI Lancet PD APR 6 PY 2013 VL 381 IS 9873 BP 1211 EP 1222 DI 10.1016/S0140-6736(13)60598-X PG 12 WC Medicine, General & Internal SC General & Internal Medicine GA 122WU UT WOS:000317350100031 PM 23489753 ER PT J AU Nikolic, S van de Ven, G Heng, K Kupko, D Husemann, B Raymond, JC Hughes, JP Falcon-Barroso, J AF Nikolic, Sladjana van de Ven, Glenn Heng, Kevin Kupko, Daniel Husemann, Bernd Raymond, John C. Hughes, John P. Falcon-Barroso, Jesus TI An Integral View of Fast Shocks Around Supernova 1006 SO SCIENCE LA English DT Article ID BALMER-DOMINATED SHOCKS; COLLISIONLESS SHOCKS; AZIMUTHAL VARIATIONS; OPTICAL-EMISSION; HIGH-ENERGY; SN-1006; REMNANTS; ACCELERATION; WAVE; GAS AB Supernova remnants are among the most spectacular examples of astrophysical pistons in our cosmic neighborhood. The gas expelled by the supernova explosion is launched with velocities similar to 1000 kilometers per second into the ambient, tenuous interstellar medium, producing shocks that excite hydrogen lines. We have used an optical integral-field spectrograph to obtain high-resolution spatial-spectral maps that allow us to study in detail the shocks in the northwestern rim of supernova 1006. The two-component Ha line is detected at 133 sky locations. Variations in the broad line widths and the broad-to-narrow line intensity ratios across tens of atomic mean free paths suggest the presence of suprathermal protons, the potential seed particles for generating high-energy cosmic rays. C1 [Nikolic, Sladjana; van de Ven, Glenn] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Heng, Kevin] Univ Bern, Ctr Space & Habitabil, CH-3012 Bern, Switzerland. [Kupko, Daniel; Husemann, Bernd] Leibniz Inst Astrophys Potsdam AIP, D-14482 Potsdam, Germany. [Raymond, John C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Hughes, John P.] Rutgers State Univ, Dept Phys & Astron, Piscataway, NJ 08854 USA. [Falcon-Barroso, Jesus] Inst Astrofis Canarias, E-38205 San Cristobal la Laguna, Tenerife, Spain. RP Nikolic, S (reprint author), Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany. EM nikolic@mpia.de OI Knezevic, Sladjana/0000-0003-1416-8069 FU International Max Planck Research School for Astronomy and Cosmic Physics at the University of Heidelberg; European Southern Observatory Telescopes at the La Silla Paranal Observatory [085.D-0983] FX This work was supported by the International Max Planck Research School for Astronomy and Cosmic Physics at the University of Heidelberg. The paper is based on observations made with European Southern Observatory Telescopes at the La Silla Paranal Observatory under program ID 085.D-0983. NR 28 TC 20 Z9 20 U1 0 U2 4 PU AMER ASSOC ADVANCEMENT SCIENCE PI WASHINGTON PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA SN 0036-8075 J9 SCIENCE JI Science PD APR 5 PY 2013 VL 340 IS 6128 BP 45 EP 48 DI 10.1126/science.1228297 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 118XS UT WOS:000317061100039 PM 23413189 ER PT J AU Donovan, SK Pawson, DJ AF Donovan, Stephen K. Pawson, Doris J. TI An Intersection in Time and Space: Significance of Modern Invertebrate Borings in Upper Cretaceous Echinoids SO ICHNOS-AN INTERNATIONAL JOURNAL FOR PLANT AND ANIMAL TRACES LA English DT Article DE Ichnology; Reworked fossils; Hardouinia; Entobia; Gastrochaenolites; Caulostrepsis ID NOMENCLATURE AB Reworked fossils may contribute unique data to ichnology, stratigraphy, and paleoecology. Reworked Upper Cretaceous echinoids are found on Ocean Isle Beach, North Carolina, United States. Tests of Hardouinia sp. cf. H. mortonis were intensely bored by clionaid sponges (Entobia) and bivalves (Gastrochaenolites), with rare polychaete annelids (Caulostrepsis). Evidence for a high-energy environment in the Late Cretaceous is provided by the sandstone infill and a geopetal infill. Hardouinia were bored on all surfaces, largely lack surface detail and have been corraded, exposing the internal structure of some borings, indicating that these specimens were tumbled in a modern, high energy marine environment. Borers showed substrate preferences: Entobia is largely limited to the test, but do penetrate the sandstone infill in some specimens; Caulostrepsis mainly infested the crystalline calcite of the echinoid test; and Gastrochaenolites penetrated both tests and lithified sandstone infill. This Entobia-Gastrochaenolites assemblage in these echinoids differs from the Entobia-Caulostrepsis assemblage recognized from the approximately coeval, but spatially distant, tests of Upper Cretaceous Echinocorys ex gr. scutata found reworked on the North Sea coast of Norfolk, England. Unlike the Entobia-Gastrochaenolites association of North Carolina, the boring association in Norfolk is between Entobia and Caulostrepsis, which are found in both tests and chalk infill. Thus, the lithology of the infill is an important factor in determining these differences. C1 [Donovan, Stephen K.] Naturalis Biodivers Ctr, Dept Geol, NL-2300 RA Leiden, Netherlands. [Pawson, Doris J.] Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, Washington, DC 20560 USA. RP Donovan, SK (reprint author), Naturalis Biodivers Ctr, Dept Geol, Postbus 9517, NL-2300 RA Leiden, Netherlands. EM Steve.Donovan@naturalis.nl RI Donovan, Stephen/O-1285-2015 FU Department of Invertebrate Zoology; National Museum of Natural History, Washington, DC FX This research was undertaken during the term of a Smithsonian Institution Short-Term Visitor Grant to S. K. D., held in the Department of Invertebrate Zoology, National Museum of Natural History, Washington, DC, which he gratefully acknowledges. Constructive review comments by Dr. Ana Santos (Universidad de Huelva, Spain), a second, but anonymous, reviewer, and associate editor Dr. Rob MacNaughton (Geological Survey of Canada, Calgary) are all gratefully acknowledged. NR 37 TC 5 Z9 6 U1 0 U2 2 PU TAYLOR & FRANCIS INC PI PHILADELPHIA PA 325 CHESTNUT ST, SUITE 800, PHILADELPHIA, PA 19106 USA SN 1042-0940 J9 ICHNOS JI Ichnos PD APR 3 PY 2013 VL 20 IS 2 BP 81 EP 87 DI 10.1080/10420940.2013.787072 PG 7 WC Paleontology SC Paleontology GA 150HX UT WOS:000319381900004 ER PT J AU Rodriguez, A Hernandez, JC Clemente, S Coppard, SE AF Rodriguez, Adriana Carlos Hernandez, Jose Clemente, Sabrina Edward Coppard, Simon TI A new species of Diadema (Echinodermata: Echinoidea: Diadematidae) from the eastern Atlantic Ocean and a neotype designation of Diadema antillarum (Philippi, 1845) SO ZOOTAXA LA English DT Article DE Diadematidae; Diadema antillarum; Diadema africanum sp nov eastern Atlantic Ocean; test; spines; pedicellariae; taxonomy ID SEA-URCHIN DIADEMA; GENERA DIADEMA; TAXONOMIC SIGNIFICANCE; MASS MORTALITY; PANAMA; ECHINOTHRIX; MORPHOLOGY; ISTHMUS; GROWTH; DNA AB Diadema africanum sp. nov. Rodriguez et al. 2013 occurs in the eastern Atlantic Ocean at depths of 1-80 meters off Madeira Islands, Salvage Islands, Canary Islands, Cape Verde Islands, Sao Tome Islands and at the continental coast off Senegal and Ghana. This species was previously considered an eastern Atlantic population of D. antillarum. Genetic distances between the holotype of D. africanum and the neotype of D. antillarum herein designated, measured 3.34% in Cytochrome oxidase I, 3.80% in ATPase-8 and 2.31% in ATPase-6. Such divergence is similar to that already highlighted between other accepted species of Diadema. Morphometric analysis of test, spine and pedicellarial characters also separated D. africanum from D. antillarum and reveals that this new species is morphologically similar to D. antillarum ascensionis from the mid Atlantic. The tridentate pedicellariae, which have been shown to have diagnostic characters which discriminate among species of Diadema, occur as both broad and narrow valved forms in D. antillarum from the western Atlantic. In D. africanum the tridentate pedicellariae occur only as a single form which is characterized by moderately broad and curved valves, with an expanded distal gripping region. This form of tridentate pedicellaria is very similar to that of D. antillarum ascensionis from the central Atlantic, with only slight variations in valve serration and valve curvature differentiating the two forms. C1 [Rodriguez, Adriana; Carlos Hernandez, Jose; Clemente, Sabrina] Univ La Laguna, Fac Biol, Dept Biol Anim, Biodiversidad Ecol Marina & Conservac BIOECOMAC, San Cristobal la Laguna 38206, Spain. [Edward Coppard, Simon] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. RP Rodriguez, A (reprint author), Univ La Laguna, Fac Biol, Dept Biol Anim, Biodiversidad Ecol Marina & Conservac BIOECOMAC, Ave Astrofis Francisco Sanchez Sn, San Cristobal la Laguna 38206, Spain. EM adrianar@ull.es RI Clemente, Sabrina/B-3855-2014; Clemente, Sabrina/C-6909-2013; Hernandez, Jose Carlos/F-9971-2010 OI Clemente, Sabrina/0000-0003-1930-2052; Hernandez, Jose Carlos/0000-0002-1539-1783 NR 47 TC 15 Z9 17 U1 0 U2 14 PU MAGNOLIA PRESS PI AUCKLAND PA PO BOX 41383, AUCKLAND, ST LUKES 1030, NEW ZEALAND SN 1175-5326 EI 1175-5334 J9 ZOOTAXA JI Zootaxa PD APR 3 PY 2013 VL 3636 IS 1 BP 144 EP 170 PG 27 WC Zoology SC Zoology GA 117FU UT WOS:000316939700006 ER PT J AU Datovo, A Vari, RP AF Datovo, Alessio Vari, Richard P. TI The Jaw Adductor Muscle Complex in Teleostean Fishes: Evolution, Homologies and Revised Nomenclature (Osteichthyes: Actinopterygii) SO PLOS ONE LA English DT Article ID TREWAVAS 1933 PISCES; PHYLOGENETIC-RELATIONSHIPS; FEEDING MECHANISM; CICHLID FISHES; FUNCTIONAL-MORPHOLOGY; CRANIAL MORPHOLOGY; MODULATORY MULTIPLICITY; ANATOMICAL DESCRIPTION; HEAD-MUSCLES; PERCIFORMES AB The infraclass Teleostei is a highly diversified group of bony fishes that encompasses 96% of all species of living fishes and almost half of extant vertebrates. Evolution of various morphological complexes in teleosts, particularly those involving soft anatomy, remains poorly understood. Notable among these problematic complexes is the adductor mandibulae, the muscle that provides the primary force for jaw adduction and mouth closure and whose architecture varies from a simple arrangement of two segments to an intricate complex of up to ten discrete subdivisions. The present study analyzed multiple morphological attributes of the adductor mandibulae in representatives of 53 of the 55 extant teleostean orders, as well as significant information from the literature in order to elucidate the homologies of the main subdivisions of this muscle. The traditional alphanumeric terminology applied to the four main divisions of the adductor mandibulae - A(1), A(2), A(3), and A omega - patently fails to reflect homologous components of that muscle across the expanse of the Teleostei. Some features traditionally used as landmarks for identification of some divisions of the adductor mandibulae proved highly variable across the Teleostei; notably the insertion on the maxilla and the position of muscle components relative to the path of the ramus mandibularis trigeminus nerve. The evolutionary model of gain and loss of sections of the adductor mandibulae most commonly adopted under the alphanumeric system additionally proved ontogenetically incongruent and less parsimonious than a model of subdivision and coalescence of facial muscle sections. Results of the analysis demonstrate the impossibility of adapting the alphanumeric terminology so as to reflect homologous entities across the spectrum of teleosts. A new nomenclatural scheme is proposed in order to achieve congruence between homology and nomenclature of the adductor mandibulae components across the entire Teleostei. C1 [Datovo, Alessio] Univ Sao Paulo, Museu Zool, Lab Ictiol, Sao Paulo, Brazil. [Datovo, Alessio] Univ Sao Paulo, Lab Ictiol Ribeirao Preto, Dept Biol, Fac Filosofia Ciencias & Letras Ribeirao Preto, Sao Paulo, Brazil. [Datovo, Alessio] Smithsonian Inst, Dept Vertebrate Zool, Natl Museum Nat Hist, Washington, DC 20560 USA. [Vari, Richard P.] Smithsonian Inst, Div Fishes, Dept Vertebrate Zool, Natl Museum Nat Hist, Washington, DC 20560 USA. RP Datovo, A (reprint author), Univ Sao Paulo, Museu Zool, Lab Ictiol, Sao Paulo, Brazil. EM adatovo@gmail.com RI Datovo, Alessio/K-7133-2016; Museu de Zoologia da USP, MZ-USP/Q-2192-2016 FU Fundacao de Amparo a Pesquisa do Estado de Sao Paulo (FAPESP) [2006/56445-7, 2010/18984-9]; Herbert R. and Evelyn Axelrod Chair in Systematic Ichthyology, Division of Fishes of the National Museum of Natural History, Smithsonian Institution; Office of the Associate Director for Science, National Museum of Natural History, Smithsonian Institution; FAPESP [2004/09219-6, 2009/54931-0] FX This study was supported by the Fundacao de Amparo a Pesquisa do Estado de Sao Paulo (FAPESP #2006/56445-7 and #2010/18984-9); the Herbert R. and Evelyn Axelrod Chair in Systematic Ichthyology, Division of Fishes of the National Museum of Natural History, Smithsonian Institution; and The Office of the Associate Director for Science, National Museum of Natural History, Smithsonian Institution. Equipment used in this study was provided by infrastructural projects from FAPESP (#2004/09219-6 and #2009/54931-0). The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 182 TC 19 Z9 20 U1 4 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 APR 2 PY 2013 VL 8 IS 4 AR e60846 DI 10.1371/journal.pone.0060846 PG 23 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 127RY UT WOS:000317717300152 PM 23565279 ER PT J AU Parmentier, I Duminil, J Kuzmina, M Philippe, M Thomas, DW Kenfack, D Chuyong, GB Cruaud, C Hardy, OJ AF Parmentier, Ingrid Duminil, Jerome Kuzmina, Maria Philippe, Morgane Thomas, Duncan W. Kenfack, David Chuyong, George B. Cruaud, Corinne Hardy, Olivier J. TI How Effective Are DNA Barcodes in the Identification of African Rainforest Trees? SO PLOS ONE LA English DT Article ID LAND PLANTS; TAXONOMISTS; PHYLOGENY; DIVERSITY; SEQUENCES; REGIONS; RATES AB Background: DNA barcoding of rain forest trees could potentially help biologists identify species and discover new ones. However, DNA barcodes cannot always distinguish between closely related species, and the size and completeness of barcode databases are key parameters for their successful application. We test the ability of rbcL, matK and trnH-psbA plastid DNA markers to identify rain forest trees at two sites in Atlantic central Africa under the assumption that a database is exhaustive in terms of species content, but not necessarily in terms of haplotype diversity within species. Methodology/Principal Findings: We assess the accuracy of identification to species or genus using a genetic distance matrix between samples either based on a global multiple sequence alignment (GD) or on a basic local alignment search tool (BLAST). Where a local database is available (within a 50 ha plot), barcoding was generally reliable for genus identification (95-100% success), but less for species identification (71-88%). Using a single marker, best results for species identification were obtained with trnH-psbA. There was a significant decrease of barcoding success in species-rich clades. When the local database was used to identify the genus of trees from another region and did include all genera from the query individuals but not all species, genus identification success decreased to 84-90%. The GD method performed best but a global multiple sequence alignment is not applicable on trnH-psbA. Conclusions/Significance: Barcoding is a useful tool to assign unidentified African rain forest trees to a genus, but identification to a species is less reliable, especially in species-rich clades, even using an exhaustive local database. Combining two markers improves the accuracy of species identification but it would only marginally improve genus identification. Finally, we highlight some limitations of the BLAST algorithm as currently implemented and suggest possible improvements for barcoding applications. C1 [Parmentier, Ingrid; Duminil, Jerome; Philippe, Morgane; Hardy, Olivier J.] Univ Libre Brussels, Fac Sci, Brussels, Belgium. [Duminil, Jerome] Biovers Int, Subreg Off Cent Africa, Yaounde, Cameroon. [Kuzmina, Maria] Univ Guelph, Biodivers Inst Ontario, Canadian Ctr DNA Barcoding, Guelph, ON N1G 2W1, Canada. [Thomas, Duncan W.] Oregon State Univ, Dept Bot & Plant Pathol, Corvallis, OR 97331 USA. [Kenfack, David] Smithsonian Inst, Dept Bot, Washington, DC 20560 USA. [Chuyong, George B.] Univ Buea, Dept Plant & Anim Sci, Buea, Cameroon. [Cruaud, Corinne] Commissariat Energie Atom & Energies Alternat CEA, Inst Genom Genoscope, Evry, France. RP Hardy, OJ (reprint author), Univ Libre Brussels, Fac Sci, Brussels, Belgium. EM ohardy@ulb.ac.be OI Hardy, Olivier/0000-0003-2052-1527 FU Centre National de Sequencage (Genoscope, France); Government of Canada through Genome Canada; Ontario Genomics Institute [2008-OGI-ICI-03]; Belgian Fund for Scientific Research (Fonds de la Recherche Scientifique-FNRS) [MIS 4.519.10]; FRS-FNRS FX DNA extraction and sequencing were financed by the Centre National de Sequencage (Genoscope, France, http://www.genoscope.cns.fr/spip/), the Government of Canada through Genome Canada and the Ontario Genomics Institute (2008-OGI-ICI-03), and by the Belgian Fund for Scientific Research (Fonds de la Recherche Scientifique-FNRS, http://www1.frs-fnrs.be/) through grant MIS 4.519.10. IP and JD (postdoctoral researchers), and OJH (research associate) are financed by the FRS-FNRS. The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 44 TC 21 Z9 23 U1 1 U2 63 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 APR 2 PY 2013 VL 8 IS 4 AR e54921 DI 10.1371/journal.pone.0054921 PG 10 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 127RY UT WOS:000317717300001 PM 23565134 ER PT J AU Townsend, AK Sillett, TS Lany, NK Kaiser, SA Rodenhouse, NL Webster, MS Holmes, RT AF Townsend, Andrea K. Sillett, T. Scott Lany, Nina K. Kaiser, Sara A. Rodenhouse, Nicholas L. Webster, Michael S. Holmes, Richard T. TI Warm Springs, Early Lay Dates, and Double Brooding in a North American Migratory Songbird, the Black-Throated Blue Warbler SO PLOS ONE LA English DT Article ID SPARROW MELOSPIZA-MELODIA; CLIMATE-CHANGE AFFECTS; NON-BREEDING SEASON; DENDROICA-CAERULESCENS; POPULATION-DYNAMICS; NEOTROPICAL MIGRANT; LONG-TERM; AVIAN POPULATION; BIRD POPULATION; GREAT TITS AB Numerous studies have correlated the advancement of lay date in birds with warming climate trends, yet the fitness effects associated with this phenological response have been examined in only a small number of species. Most of these species-primarily insectivorous cavity nesters in Europe-exhibit fitness declines associated with increasing asynchrony with prey. Here, we use 25 years of demographic data, collected from 1986 to 2010, to examine the effects of spring temperature on breeding initiation date, double brooding, and annual fecundity in a Nearctic - Neotropical migratory songbird, the black-throated blue warbler (Setophaga caerulescens). Data were collected from birds breeding at the Hubbard Brook Experimental Forest, New Hampshire, USA, where long-term trends toward warmer springs have been recorded. We found that black-throated blue warblers initiated breeding earlier in warmer springs, that early breeders were more likely to attempt a second brood than those starting later in the season, and that double brooding and lay date were linked to higher annual fecundity. Accordingly, we found selection favored earlier breeding in most years. However, in contrast to studies of several other long-distance migratory species in Europe, this selection pressure was not stronger in warmer springs, indicating that these warblers were able to adjust mean lay date appropriately to substantial inter-annual variation in spring temperature. Our results suggest that this North American migratory songbird might not experience the same fecundity declines as songbirds that are unable to adjust their timing of breeding in pace with spring temperatures. C1 [Townsend, Andrea K.; Kaiser, Sara A.; Webster, Michael S.] Cornell Univ, Cornell Lab Ornithol, Ithaca, NY USA. [Townsend, Andrea K.; Kaiser, Sara A.; Webster, Michael S.] Cornell Univ, Dept Neurobiol & Behav, Ithaca, NY 14853 USA. [Townsend, Andrea K.; Sillett, T. Scott] Smithsonian Inst, Natl Zool Pk, Smithsonian Conservat Biol Inst, Migratory Bird Ctr, Washington, DC 20008 USA. [Lany, Nina K.; Holmes, Richard T.] Dartmouth Coll, Dept Biol Sci, Hanover, NH 03755 USA. [Rodenhouse, Nicholas L.] Wellesley Coll, Dept Biol Sci, Wellesley, MA 02181 USA. RP Townsend, AK (reprint author), Univ Calif Davis, Dept Wildlife Fish & Conservat Biol, Davis, CA 95616 USA. EM aktownsend@ucdavis.edu OI Kaiser, Sara/0000-0002-6464-3238 FU United States National Science Foundation; Dartmouth College; Wellesley College; Smithsonian Institution; Cornell University; United States National Science Foundation [DEB 01-08488] FX This research was supported by grants from the United States National Science Foundation and by Dartmouth College, Wellesley College, the Smithsonian Institution, and Cornell University. The authors thank the many students and field assistants who have worked with them over the past 25 years. This manuscript is a contribution of the Hubbard Brook Ecosystem Study. Hubbard Brook is part of the Long-Term Ecological Research network, which is supported by the United States National Science Foundation (DEB 01-08488). The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 61 TC 18 Z9 18 U1 4 U2 81 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 APR 2 PY 2013 VL 8 IS 4 AR e59467 DI 10.1371/journal.pone.0059467 PG 9 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 127RY UT WOS:000317717300022 PM 23565154 ER PT J AU Lassman, TC AF Lassman, Thomas C. TI Reforming Weapon Systems Acquisition in the Department of Defense: The Case of the US Army's Advanced Attack Helicopter SO JOURNAL OF POLICY HISTORY LA English DT Article C1 Smithsonian Inst, Natl Air & Space Museum, Div Space Hist, Washington, DC 20560 USA. RP Lassman, TC (reprint author), Smithsonian Inst, Natl Air & Space Museum, Div Space Hist, Washington, DC 20560 USA. EM lassmant@si.edu NR 145 TC 1 Z9 1 U1 0 U2 1 PU CAMBRIDGE UNIV PRESS PI NEW YORK PA 32 AVENUE OF THE AMERICAS, NEW YORK, NY 10013-2473 USA SN 0898-0306 EI 1528-4190 J9 J POLICY HIST JI J. Policy Hist. PD APR PY 2013 VL 25 IS 2 BP 173 EP 206 DI 10.1017/S089803061300002X PG 34 WC History; Political Science SC History; Government & Law GA AA8XW UT WOS:000331379300002 ER PT J AU Rog, S Ryan, MJ Mueller, U Lampert, KP AF Rog, Stefanie Ryan, Michael J. Mueller, Ulrich Lampert, Kathrin P. TI EVIDENCE FOR MORPHOLOGICAL AND GENETIC DIVERSIFICATION OF TUNGARA FROG POPULATIONS ON ISLANDS SO HERPETOLOGICAL CONSERVATION AND BIOLOGY LA English DT Article DE amphibians; dispersal; mating call; microsatellite markers; morphology; Physalaemus (Engystomops) pustulosus; population genetics, speciation ID PHYSALAEMUS-PUSTULOSUS; SEXUAL SELECTION; BODY-SIZE; MICROSATELLITE LOCI; RODENT POPULATIONS; DARWINS FINCHES; EVOLUTION; SPECIATION; BOTTLENECKS; GIGANTISM AB Despite the ongoing debate about the mechanisms involved in speciation processes, evolutionary biologists agree that isolation is a key factor in promoting the evolution of different species. Islands provide natural models for the study of isolated populations. Populations on islands are usually small and may also be subject to intense directional selection or genetic drift. In this study we investigated island populations of the Tungara Frog, Physalaemus (Engystomops) pustulosus, and documented their level of morphological, genetic, and behavioral divergence. We also compared our results to a mainland population. We found that larger islands and/or islands characterized by more human traffic with the mainland were more likely to harbor populations of Tungara Frogs than smaller islands. All island populations differed significantly from the mainland population and from each other at the genetic and, to a slightly lesser degree, morphological levels. Male mating calls had also diverged but did not show a clear pattern. We conclude that isolated populations of Tungara Frogs diverge very rapidly. They might therefore provide useful models for the investigation of evolution in small populations and potentially of speciation processes. C1 [Rog, Stefanie; Ryan, Michael J.; Mueller, Ulrich] Univ Texas Austin, Sect Integrat Biol, Austin, TX 78712 USA. [Ryan, Michael J.] Smithsonian Trop Res Inst, Balboa, Panama. [Lampert, Kathrin P.] Univ Wurzburg, Dept Physiol Chem 1, Bioctr, D-97074 Wurzburg, Germany. RP Lampert, KP (reprint author), Ruhr Univ Bochum, Dept Evolutionary Ecol & Biodivers Anim, Univ Str 150, D-44780 Bochum, Germany. EM kathrin.lampert@ruhr-uni-bochum.de FU A. Stanley Rand fellowship; NSF [IOB 0544096, DEB-0639879, IOS-0920138]; University of Wurzburg FX We would like to thank Andrew J. Crawford for comments that greatly improved the manuscript. Also, we thank Autoridad Nacional del Ambiente of the Republic of Panama and STRI for research and export permits. Smithsonian Tropical Research Institute provided invaluable logistical support. This work was supported by an A. Stanley Rand fellowship to SR, by NSF grant IOB 0544096 to MJR, and NSF awards DEB-0639879 and IOS-0920138 to UGM and by the University of Wurzburg. The research presented complies with the current laws of the countries in which it was performed. NR 66 TC 0 Z9 1 U1 3 U2 14 PU HERPETOLOGICAL CONSERVATION & BIOLOGY PI CORVALLIS PA C/O R BRUCE BURY, USGS FOREST & RANGELAND, CORVALLIS, OR 00000 USA SN 2151-0733 EI 1931-7603 J9 HERPETOL CONSERV BIO JI Herpetol. Conserv. Biol. PD APR PY 2013 VL 8 IS 1 BP 228 EP 239 PG 12 WC Zoology SC Zoology GA 256ZJ UT WOS:000327352400021 ER PT J AU Yahara, T Javadi, F Onoda, Y de Queiroz, LP Faith, DP Prado, DE Akasaka, M Kadoya, T Ishihama, F Davies, S Slik, JWF Yi, TS Ma, KP Bin, C Darnaedi, D Pennington, RT Tuda, M Shimada, M Ito, M Egan, AN Buerki, S Raes, N Kajita, T Vatanparast, M Mimura, M Tachida, H Iwasa, Y Smith, GF Victor, JE Nkonki, T AF Yahara, Tetsukazu Javadi, Firouzeh Onoda, Yusuke de Queiroz, Luciano Paganucci Faith, Daniel P. Prado, Darien E. Akasaka, Munemitsu Kadoya, Taku Ishihama, Fumiko Davies, Stuart Slik, J. W. Ferry Yi, Tingshuang Ma, Keping Bin, Chen Darnaedi, Dedy Pennington, R. Toby Tuda, Midori Shimada, Masakazu Ito, Motomi Egan, Ashley N. Buerki, Sven Raes, Niels Kajita, Tadashi Vatanparast, Mohammad Mimura, Makiko Tachida, Hidenori Iwasa, Yoh Smith, Gideon F. Victor, Janine E. Nkonki, Tandiwe TI Global legume diversity assessment: Concepts, key indicators, and strategies SO TAXON LA English DT Review DE distribution model; extinction risk; Fabaceae; functional diversity; genetic diversity; phylogenetic diversity; species loss ID SPECIES DISTRIBUTION MODELS; VASCULAR PLANT DIVERSITY; FUNCTIONAL DIVERSITY; PHYLOGENETIC DIVERSITY; GENETIC DIVERSITY; BIODIVERSITY LOSS; GLYCINE-SOJA; EVOLUTIONARY DIVERSIFICATION; LEGUMINOSAE-PAPILIONOIDEAE; CALLOSOBRUCHUS COLEOPTERA AB While many plant species are considered threatened under anthropogenic pressure, it remains uncertain how rapidly we are losing plant species diversity. To fill this gap, we propose a Global Legume Diversity Assessment (GLDA) as the first step of a global plant diversity assessment. Here we describe the concept of GLDA and its feasibility by reviewing relevant approaches and data availability. We conclude that Fabaceae is a good proxy for overall angiosperm diversity in many habitats and that much relevant data for GLDA are available. As indicators of states, we propose comparison of species richness with phylogenetic and functional diversity to obtain an integrated picture of diversity. As indicators of trends, species loss rate and extinction risks should be assessed. Specimen records and plot data provide key resources for assessing legume diversity at a global scale, and distribution modeling based on these records provide key methods for assessing states and trends of legume diversity. GLDA has started in Asia, and we call for a truly global legume diversity assessment by wider geographic collaborations among various scientists. C1 [Yahara, Tetsukazu] Kyushu Univ, Ctr Asian Conservat Ecol, Fukuoka 8128581, Japan. [Yahara, Tetsukazu; Javadi, Firouzeh; Mimura, Makiko; Tachida, Hidenori; Iwasa, Yoh] Kyushu Univ, Dept Biol, Fukuoka 8128581, Japan. [Onoda, Yusuke] Kyoto Univ, Grad Sch Agr, Kyoto 6068502, Japan. [de Queiroz, Luciano Paganucci] Feira de Santana State Univ, Dept Biol Sci, BR-44036900 Feira De Santana, Brazil. [Faith, Daniel P.] Australian Museum, Sydney, NSW 2010, Australia. [Prado, Darien E.] UNR, Fac Ciencias Agr, Catedra Bot, Zavalla, Argentina. [Akasaka, Munemitsu] Univ Tokyo, Sch Agr & Life Sci, Lab Wildlife Biol, Tokyo 1138656, Japan. [Kadoya, Taku; Ishihama, Fumiko] Natl Inst Environm Studies, Div Environm Biol, Tsukuba, Ibaraki 3058506, Japan. [Davies, Stuart] Smithsonian Inst, CTFS SIGEO, Washington, DC 20013 USA. [Slik, J. W. Ferry] Chinese Acad Sci, Xishuangbanna Trop Bot Garden, Plant Geog Lab, Mengla 666303, Yunnan, Peoples R China. [Yi, Tingshuang] Chinese Acad Sci, Kunming Inst Bot, Kunming 650204, Yunnan, Peoples R China. [Ma, Keping] Chinese Acad Sci, Inst Bot, Beijing 100093, Peoples R China. [Bin, Chen] Chinese Acad Sci, Inst Bot, Reference & Informat Serv Ctr, Beijing 100093, Peoples R China. [Darnaedi, Dedy] Indonesian Inst Sci, Biol Res Ctr, Bogor 16122, Indonesia. [Pennington, R. Toby] Royal Bot Garden Edinburgh, Edinburgh EH3 5LR, Midlothian, Scotland. [Tuda, Midori] Kyushu Univ, Inst Biol Control, Fac Agr, Fukuoka 8128581, Japan. [Shimada, Masakazu; Ito, Motomi] Univ Tokyo, Dept Syst Sci Biol, Meguro Ku, Tokyo 1538902, Japan. [Egan, Ashley N.] E Carolina Univ, Dept Biol, Greenville, NC 27858 USA. [Egan, Ashley N.] E Carolina Univ, North Carolina Ctr Biodivers, Greenville, NC 27858 USA. [Buerki, Sven] Royal Bot Gardens, Jodrell Lab, Richmond TW9 3DS, Surrey, England. [Raes, Niels] Naturalis Biodivers Ctr, NL-2300 RA Leiden, Netherlands. [Raes, Niels] Leiden Univ, Sect NHN, NL-2300 RA Leiden, Netherlands. [Kajita, Tadashi; Vatanparast, Mohammad] Chiba Univ, Grad Sch Sci, Dept Biol, Chiba 2638522, Japan. [Smith, Gideon F.; Victor, Janine E.; Nkonki, Tandiwe] South African Natl Biodivers Inst, Biosystemat Res & Biodivers Collect Div, ZA-0001 Pretoria, South Africa. [Smith, Gideon F.] Univ Pretoria, Dept Plant Sci, HGWJ Schweickerdt Herbarium, ZA-0002 Pretoria, South Africa. [Smith, Gideon F.] Univ Coimbra, Dept Ciencias Vida, Ctr Funct Ecol, P-3001455 Coimbra, Portugal. RP Yahara, T (reprint author), Kyushu Univ, Ctr Asian Conservat Ecol, 6-10-1 Hakozaki, Fukuoka 8128581, Japan. EM tet.yahara@gmail.com RI Raes, Niels/A-9645-2011; Kadoya, Taku/L-7536-2013; de Queiroz, Luciano Paganucci/I-1378-2012; AKASAKA, Munemitsu/G-1172-2013; Onoda, Yusuke/L-7179-2015; Buerki, Sven/F-6008-2012; U-ID, Kyushu/C-5291-2016; Iwasa, Yoh/G-5368-2010 OI Raes, Niels/0000-0002-4329-4892; Kadoya, Taku/0000-0002-7816-5484; de Queiroz, Luciano Paganucci/0000-0001-7436-0939; Onoda, Yusuke/0000-0001-6245-2342; Iwasa, Yoh/0000-0003-0691-1852 FU Ministry of the Environment, Japan; JSPS FX This paper is an outcome of the workshop on the global legume diversity assessment held from 19 to 22 August 2011 in Kyushu University, Japan, supported by the Environment Research and Technology Development Fund (S9) of the Ministry of the Environment, Japan and the JSPS fund for Global Center of Excellence Program "Asian Conservation Ecology". We also thank members of GEO BON Working Group 1 and the Science Committee members of the bioGENESIS core project of DVERSITAS who gave us stimulating and constructive comments on ideas of global legume diversity assessments. NR 216 TC 13 Z9 13 U1 1 U2 36 PU INT ASSOC PLANT TAXONOMY-IAPT PI BRATISLAVA PA C/O INST BOTANY, SLOVAK ACAD SCIENCES DUBRAVSKA CESTA 9, SK-845 23 BRATISLAVA, SLOVAKIA SN 0040-0262 J9 TAXON JI Taxon PD APR PY 2013 VL 62 IS 2 BP 249 EP 266 PG 18 WC Plant Sciences; Evolutionary Biology SC Plant Sciences; Evolutionary Biology GA 196CM UT WOS:000322751000002 ER PT J AU Delprete, PG Feuillet, C AF Delprete, Piero G. Feuillet, Christian TI MARIE-FRANCOISE PREVOST "FANCHON" (1941-2013) SO TAXON LA English DT Biographical-Item C1 [Delprete, Piero G.] UMR AMAP, IRD, F-97323 Cayenne, French Guiana, France. [Feuillet, Christian] Smithsonian Inst, Dept Systemat Biol Bot, MRC 166, Washington, DC 20560 USA. RP Delprete, PG (reprint author), UMR AMAP, IRD, BP 165, F-97323 Cayenne, French Guiana, France. EM piero.delprete@ird.fr NR 1 TC 0 Z9 0 U1 0 U2 1 PU INT ASSOC PLANT TAXONOMY-IAPT PI BRATISLAVA PA C/O INST BOTANY, SLOVAK ACAD SCIENCES DUBRAVSKA CESTA 9, SK-845 23 BRATISLAVA, SLOVAKIA SN 0040-0262 J9 TAXON JI Taxon PD APR PY 2013 VL 62 IS 2 BP 419 EP 419 PG 1 WC Plant Sciences; Evolutionary Biology SC Plant Sciences; Evolutionary Biology GA 196CM UT WOS:000322751000027 ER PT J AU Li, R Wen, J AF Li, Rong Wen, Jun TI Phylogeny and Biogeography of Dendropanax (Araliaceae), an Amphi-Pacific Disjunct Genus Between Tropical/Subtropical Asia and the Neotropics SO SYSTEMATIC BOTANY LA English DT Article DE AmphiPacific tropical disjunction; Araliaceae; biogeography; Dendropanax; phylogeny ID CHLOROPLAST DNA PHYLOGENY; NUCLEAR RIBOSOMAL DNA; NORTHERN-HEMISPHERE; SEQUENCE DATA; GEOGRAPHIC RANGE; RPS16 INTRON; DATA SETS; EVOLUTION; TERTIARY; APIACEAE AB Dendropanax (Araliaceae) is a genus of about 80 species disjunctly distributed in tropical to subtropical Asia and the Neotropics, showing an amphi-Pacific tropical disjunction. The phylogeny of the genus was constructed by sampling 95 accessions representing 33 species of Dendropanax and 43 closely related taxa using sequences of the nuclear ribosomal internal transcribed spacer (ITS) region and six plastid regions (the ndhF gene, the trnL-trnF region, the rps16 intron, the atpB-rbcL intergenic spacer, the rpl16 intron, and the psbA-trnH intergenic spacer). Phylogenetic analyses of the combined plastid and ITS data suggested that the monophyly of Dendropanax was not supported because the Asian D. lancifolius - D. hainanensis clade did not group with the main Dendropanax clade. Nevertheless, the maximally parsimonious trees (MPTs) from the analysis constraining Dendropanax as a monophyletic group were only one step longer than the unconstrained MPTs. The New and Old World Dendropanax species except D. lancifolius and D. hainanensis each formed a robustly supported clade, and the two clades were sister to each other. Based on the biogeographic analyses and fossil-calibrated Bayesian dating, Dendropanax was hypothesized to have originated in the Old World and migrated into the New World via the North Atlantic land bridges in the early Tertiary. The amphi-Pacific intercontinental disjunction of Dendropanax was dated to be 41.83 mya with a 95% high posterior density [HPD] interval of 28.46-56.15 mya. C1 [Li, Rong] Chinese Acad Sci, Kunming Inst Bot, Key Lab Biodivers & Biogeog, Kunming 650204, Yunnan, Peoples R China. [Wen, Jun] Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, MRC 166, Washington, DC 20013 USA. RP Wen, J (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, MRC 166, Washington, DC 20013 USA. EM wenj@si.edu FU National Science Foundation [DEB-0196051, DEB-0108536]; Natural Science Foundation of China [30828001]; John D. and Catherine T. MacArthur Foundation; Laboratory of Analytical Biology at the National Museum of Natural History of the Smithsonian Institution FX The study was supported by grants from the National Science Foundation (DEB-0196051, and DEB-0108536), the Natural Science Foundation of China (30828001 to J. Wen and T. Yi), the John D. and Catherine T. MacArthur Foundation, and the Laboratory of Analytical Biology at the National Museum of Natural History of the Smithsonian Institution. Laboratory assistance was provided by Jeff Hunt, Lei Xie, Xinwei Xu, and Yunjuan Zuo. We thank Michael Nee, Ki-Oug Yoo, Akiko Soejima, J. F. Maxwell, Paul Fine, Hang Li, Yunfei Deng, H. Kato, Yumin Shui, John L. Clark, Peter Fritsch, and Yuguo Wang for assistance with collecting samples, and Associate Editor Lynn Bohs and two reviewers for their most helpful comments and suggestions, which greatly improved the paper. NR 142 TC 15 Z9 15 U1 0 U2 20 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 APR-JUN PY 2013 VL 38 IS 2 BP 536 EP 551 DI 10.1600/036364413X666606 PG 16 WC Plant Sciences; Evolutionary Biology SC Plant Sciences; Evolutionary Biology GA 157JW UT WOS:000319893400024 ER PT J AU Hallworth, MT Studds, CE Sillett, TS Marra, PP AF Hallworth, Michael T. Studds, Colin E. Sillett, T. Scott Marra, Peter P. TI Do archival light-level geolocators and stable hydrogen isotopes provide comparable estimates of breeding-ground origin? SO AUK LA English DT Article DE Bayesian; deuterium; discrimination; migratory bird; Ovenbird; Seiurus aurocapilla; solar geolocator; stable isotopes ID MIGRATORY CONNECTIVITY; NEOTROPICAL MIGRANT; SONGBIRD MIGRATION; GENETIC-MARKERS; BIRDS; MOLT; FEATHERS; AREAS; PHILOPATRY; DISPERSAL AB Migratory connectivity for small migratory passerines has been quantified primarily with stable hydrogen isotopes in feathers (delta H-2(F)) because, until recently, we lacked the technology to track small organisms over long distances. Direct tracking of small passerines throughout the annual cycle is now possible with archival light-level geolocators. Our objective was to evaluate whether delta H-2(F) and geolocators produce similar breeding-origin assignments for the same individual birds sampled during the non-breeding season. We estimated breeding origin with geolocators and delta H-2(F) and validated those estimates using a population of Ovenbirds (Seiurus aurocapilla) from a known breeding location at Hubbard Brook Experimental Forest, New Hampshire. We also deployed geolocators on Ovenbirds in Jamaica and Florida during March 2010-2011. We performed stable hydrogen isotope analysis on feathers of birds whose geolocators we recovered (Jamaica: n = 9; Florida: n = 3). Probabilistic assignments of delta H-2(F) that accounted for regional variation in feather-isotope discrimination predicted breeding origins that agreed with kernel density estimates of origin derived from geolocators. By contrast, assignments of delta H-2(F) using the common assumption of a consistent feather-isotope discrimination across space predicted breeding origins that overlapped minimally with those from geolocators. Finally, Bayesian analyses that incorporated prior information of Ovenbird abundance across the breeding range yielded more accurate assignments for both site-independent and site-specific discrimination factors. Our findings suggest that creating more detailed feather isoscapes by increasing the number of validation locations and sampling underrepresented portions of species distributions could increase the accuracy of geographic assignments using delta H-2(F). C1 [Hallworth, Michael T.; Studds, Colin E.; Sillett, T. Scott; Marra, Peter P.] Natl Zool Pk, Smithsonian Conservat Biol Inst, Migratory Bird Ctr, Washington, DC 20013 USA. [Hallworth, Michael T.] George Mason Univ, Coll Sci, Fairfax, VA 22030 USA. [Studds, Colin E.] Univ Queensland, ARC Ctr Excellence Environm Decis, NERP Environm Decis Hub, Ctr Biodivers & Conservat Sci, Brisbane, Qld 4072, Australia. RP Hallworth, MT (reprint author), Natl Zool Pk, Smithsonian Conservat Biol Inst, Migratory Bird Ctr, MRC 5503, Washington, DC 20013 USA. EM mhallwor@masonlive.gmu.edu RI Studds, Colin/C-3701-2012 FU James Bond Fund at the Smithsonian Institution; U.S. National Science Foundation; Cosmos Club FX Supplemental materials are available at dx.doi.org/10.1525/auk.2013.13037. We thank N. Cooper, J. Gautreaux, D. Narango, R. Reitsma, L. Rowse, R. Terrill, M. Thomas, and C. Tonra for assistance with field work; K. Hobson and S. Van Wilgenburg for providing valuable comments on the manuscript; and E. McKinnon and K. Fraser for organizing and inviting us to present at the Beyond Connectivity: Using Geolocators to Explore Bird Migration Strategies symposium at the North American Ornithological Conference in Vancouver, British Columbia, in 2012. We also thank A. Jahn and two anonymous reviewers for their comments on the manuscript. This research was supported by the James Bond Fund at the Smithsonian Institution (M.T.H. and P.P.M.), the U.S. National Science Foundation (P.P.M. and T.S.S.), and the Cosmos Club (M.T.H.). Ovenbird Breeding Bird Survey data were obtained from Patuxent Wildlife Research Center's Relative Abundance Shapefiles for Geographic Analyses webpage (www.mbr-pwrc.usgs.gov/bbs/shape_ra10.html). NR 49 TC 11 Z9 11 U1 2 U2 53 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 APR PY 2013 VL 130 IS 2 BP 273 EP 282 DI 10.1525/auk.2013.13037 PG 10 WC Ornithology SC Zoology GA 157KV UT WOS:000319895900008 ER PT J AU Schachner, ER Lyson, TR Farmer, CG AF Schachner, Emm R. Lyson, Tyler R. Farmer, C. G. TI Evolution of the respiratory system in Testudines: anatomy and phylogeny SO FASEB JOURNAL LA English DT Meeting Abstract CT Joint Annual Meeting of the ASPET/BPS at Experimental Biology (EB) CY APR 20-24, 2013 CL Boston, MA SP ASPET, British Pharmacol Soc (BPS) C1 [Schachner, Emm R.] Univ Utah, Dept Biol, Salt Lake City, UT 84112 USA. [Lyson, Tyler R.] Smithsonian Inst, Dept Vertebrate Zool, Natl Museum Nat Hist, Washington, DC 20560 USA. [Farmer, C. G.] Univ Utah, Dept Biol, Salt Lake City, UT 84112 USA. NR 0 TC 0 Z9 0 U1 0 U2 2 PU FEDERATION AMER SOC EXP BIOL PI BETHESDA PA 9650 ROCKVILLE PIKE, BETHESDA, MD 20814-3998 USA SN 0892-6638 J9 FASEB J JI Faseb J. PD APR PY 2013 VL 27 MA 79.1 PG 1 WC Biochemistry & Molecular Biology; Biology; Cell Biology SC Biochemistry & Molecular Biology; Life Sciences & Biomedicine - Other Topics; Cell Biology GA 156YK UT WOS:000319860502260 ER PT J AU Frable, BW Baldwin, CC Luther, BM Weigt, LA AF Frable, Benjamin W. Baldwin, Carole C. Luther, Brendan M. Weigt, Lee A. TI A new species of western Atlantic lizardfish (Teleostei: Synodontidae: Synodus) and resurrection of Synodus bondi Fowler, 1939, as a valid species from the Caribbean with redescriptions of S. bondi, S. foetens (Linnaeus, 1766), and S. intermedius (Agassiz, 1829) SO FISHERY BULLETIN LA English DT Article ID GULF-OF-MEXICO; FISH COLLECTION; DNA BARCODES; GOBIIDAE; MORPHOLOGY; SPECIATION; GENETICS AB Western Atlantic synodontid species were studied as part of an ongoing effort to reanalyze Caribbean shorefish diversity. A neighbor-joining tree constructed from cytochrome c oxidase I (COI) data revealed 2 highly divergent genetic lineages within both Synodus intermedius (Agassiz, 1829) (Sand Diver) and S. foetens (Linnaeus, 1766) (Inshore Lizardfish). A new species, Synodus macrostigmus, is described for one of the S. intermedius lineages. Synodus macrostigmus and S. intermedius differ in number of lateral-line scales, caudal pigmentation, size of the scapular blotch, and shape of the anterior-nostril flap. Synodus macrostigmus and S. intermedius have overlapping geographic and depth distributions, but S. macrostigmus generally inhabits deeper water (>28 m) than does S. intermedius and is known only from coastal waters of the southeastern United States and the Gulf of Mexico, in contrast to those areas and the Caribbean for S. intermedius. Synodus bondi Fowler, 1939, is resurrected from the synonymy of S. foetens for one of the S. foetens genetic lineages. The 2 species differ in length and shape of the snout, number of anal-fin rays, and shape of the anterior-nostril flap. Synodus bondi and S. foetens co-occur in the central Caribbean, but S. bondi otherwise has a more southerly distribution than does S. foetens. Redescriptions are provided for S. intermedius, S. foetens, and S. bondi. Neotypes are designated for S. intermedius and S. foetens. A revised key to Synodus species in the western Atlantic is presented. C1 [Frable, Benjamin W.; Baldwin, Carole C.; Luther, Brendan M.; Weigt, Lee A.] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20013 USA. [Frable, Benjamin W.] Oregon State Univ, Dept Fisheries & Wildlife, Corvallis, OR 97331 USA. RP Frable, BW (reprint author), Smithsonian Inst, Natl Museum Nat Hist, POB 37012, Washington, DC 20013 USA. EM frableb@si.edu FU Hunterdon Oceanographic Research Fund; Smithsonian Marine Station at Fort Pierce [905] FX We would like to thank the many people who facilitated this study: A. Driskell, A. Ormos, D. Smith, R. Myers, A. Bentley, P. Webster, E. Wiley, R. Robins, M. Sabaj Perez, J. Lundberg, B. Nagareda, R. Causse, C. Ferrara, D. Johnson, C. Boucher, D. R. Robertson, J. Van Tassell, C. Castillo, S. Raredon, B. Collette, and Z. Baldwin. Research in Florida was conducted pursuant to Special Activities License no. 07SR-1024B to the second author. This article is contribution number 935 of the Caribbean Coral Reef Ecosystems Program, Smithsonian Institution, supported in part by the Hunterdon Oceanographic Research Fund and Smithsonian Marine Station at Fort Pierce contribution number 905. NR 59 TC 5 Z9 6 U1 0 U2 11 PU NATL MARINE FISHERIES SERVICE SCIENTIFIC PUBL OFFICE PI SEATTLE PA 7600 SAND POINT WAY NE BIN C15700, SEATTLE, WA 98115 USA SN 0090-0656 EI 1937-4518 J9 FISH B-NOAA JI Fish. Bull. PD APR PY 2013 VL 111 IS 2 BP 122 EP 146 DI 10.7755/FB.111.2.2 PG 25 WC Fisheries SC Fisheries GA 149HQ UT WOS:000319310000002 ER PT J AU Dauser, T Garcia, J Wilms, J Bock, M Brenneman, LW Falanga, M Fukumura, K Reynolds, CS AF Dauser, T. Garcia, J. Wilms, J. Boeck, M. Brenneman, L. W. Falanga, M. Fukumura, K. Reynolds, C. S. TI Irradiation of an accretion disc by a jet: general properties and implications for spin measurements of black holes SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE accretion, accretion discs; black hole physics; lines: profiles; galaxies: active; galaxies: nuclei ID X-RAY REFLECTION; ADVECTION-DOMINATED ACCRETION; K-ALPHA LINE; XMM-NEWTON; IRON LINE; CYGNUS X-1; GX 339-4; ACTIVE GALAXY; 1H 0707-495; HARD STATE AB X-ray irradiation of the accretion disc leads to strong reflection features, which are then broadened and distorted by relativistic effects. We present a detailed, general relativistic approach to model this irradiation for different geometries of the primary X-ray source. These geometries include the standard point source on the rotational axis as well as more jet-like sources, which are radially elongated and accelerating. Incorporating this code in the RELLINE model for relativistic line emission, the line shape for any configuration can be predicted. We study how different irradiation geometries affect the determination of the spin of the black hole. Broad emission lines are produced only for compact irradiating sources situated close to the black hole. This is the only case where the black hole spin can be unambiguously determined. In all other cases the line shape is narrower, which could either be explained by a low spin or an elongated source. We conclude that in those cases and independent of the quality of the data no unique solution for the spin exists and therefore only a lower limit of the spin value can be given. C1 [Dauser, T.; Wilms, J.; Boeck, M.] Dr Karl Remeis Observ, D-96049 Bamberg, Germany. [Dauser, T.; Wilms, J.; Boeck, M.] Erlangen Ctr Astroparticle Phys, D-96049 Bamberg, Germany. [Garcia, J.; Reynolds, C. S.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Garcia, J.; Reynolds, C. S.] Univ Maryland, Maryland Astron Ctr Theory & Computat, College Pk, MD 20742 USA. [Boeck, M.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Brenneman, L. W.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Falanga, M.] Int Space Sci Inst, CH-3012 Bern, Switzerland. [Fukumura, K.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA. RP Dauser, T (reprint author), Dr Karl Remeis Observ, Sternwartstr 7, D-96049 Bamberg, Germany. EM thomas.dauser@sternwarte.uni-erlangen.de RI Wilms, Joern/C-8116-2013 OI Wilms, Joern/0000-0003-2065-5410 FU European Commission [ITN 215212]; Elitenetzwerk Bayern; Deutsches Zentrum fur Luft- und Raumfahrt [50 OR 1113] FX We acknowledge support from the European Commission under contract ITN 215212 'Black Hole Universe' by a fellowship from the Elitenetzwerk Bayern, and by the Deutsches Zentrum fur Luft- und Raumfahrt under contract number 50 OR 1113. We thank John E. Davis for the development of the SLXFIG module used to prepare the figures in this paper, Katja Pottschmidt and John Tomsick for useful discussions, and the referee, Andy Fabian, for his constructive comments which helped in improving this paper. NR 105 TC 68 Z9 68 U1 0 U2 2 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD APR PY 2013 VL 430 IS 3 BP 1694 EP 1708 DI 10.1093/mnras/sts710 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 148QG UT WOS:000319260500014 ER PT J AU Vogelsberger, M Zavala, J AF Vogelsberger, Mark Zavala, Jesus TI Direct detection of self-interacting dark matter SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE methods: numerical; dark matter ID PHASE-SPACE STRUCTURE; HALOES; SUBHALOES; SUBSTRUCTURE; SIMULATIONS; EVOLUTION; CAUSTICS; CORES AB Self-interacting dark matter offers an interesting alternative to collisionless dark matter because of its ability to preserve the large-scale success of the cold dark matter model, while seemingly solving its challenges on small scales. We present here the first study of the expected dark matter detection signal in a fully cosmological context taking into account different self-scattering models for dark matter. We demonstrate that models with constant and velocity-dependent cross-sections, which are consistent with observational constraints, lead to distinct signatures in the velocity distribution, because non-thermalized features found in the cold dark matter distribution are thermalized through particle scattering. Depending on the model, self-interaction can lead to a 10 per cent reduction of the recoil rates at high energies, corresponding to a minimum speed that can cause recoil larger than 300 km s(-1), compared to the cold dark matter case. At lower energies these differences are smaller than 5 per cent for all models. The amplitude of the annual modulation signal can increase by up to 25 per cent, and the day of maximum amplitude can shift by about two weeks with respect to the cold dark matter expectation. Furthermore, the exact day of phase reversal of the modulation signal can also differ by about a week between the different models. In general, models with velocity-dependent cross-sections peaking at the typical velocities of dwarf galaxies lead only to minor changes in the detection signals, whereas allowed constant cross-section models lead to significant changes. We conclude that different self-interacting dark matter scenarios might be distinguished from each other through the details of direct detection signals. Furthermore, detailed constraints on the intrinsic properties of dark matter based on null detections should take into account the possibility of self-scattering and the resulting effects on the detector signal. C1 [Vogelsberger, Mark] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Zavala, Jesus] Univ Waterloo, Dept Phys & Astron, Waterloo, ON N2L 3G1, Canada. [Zavala, Jesus] Perimeter Inst Theoret Phys, Waterloo, ON N2L 2Y5, Canada. RP Vogelsberger, M (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM mvogelsberger@cfa.harvard.edu RI Zavala Franco, Jesus/M-5152-2014 OI Zavala Franco, Jesus/0000-0003-4442-908X FU University of Waterloo; Perimeter Institute for Theoretical Physics; Government of Canada through Industry Canada; Province of Ontario through the Ministry of Research Innovation; CITA National Fellowship; NASA through Hubble Fellowship [HST-HF-51317.01] FX We thank Volker Springel for giving us access to GADGET-3, Philippe Di Stefano and Naoki Yoshida for initial discussions that inspired this work, Adrian Jenkins for generating the initial conditions of Aq-F-4, Adrienne Erickcek, Lars Hernquist, Michael Kuhlen, Avi Loeb, Josef Pradler, Kris Sigurdson, Paul Torrey and Simon White for useful suggestions. JZ is supported by the University of Waterloo and the Perimeter Institute for Theoretical Physics. Research at Perimeter Institute is supported by the Government of Canada through Industry Canada and by the Province of Ontario through the Ministry of Research & Innovation. JZ acknowledges financial support by a CITA National Fellowship. MV acknowledges support from NASA through Hubble Fellowship grant HST-HF-51317.01. NR 50 TC 28 Z9 28 U1 0 U2 3 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 APR PY 2013 VL 430 IS 3 BP 1722 EP 1735 DI 10.1093/mnras/sts712 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 148QG UT WOS:000319260500016 ER PT J AU Hopkins, PF Cox, TJ Hernquist, L Narayanan, D Hayward, CC Murray, N AF Hopkins, Philip F. Cox, Thomas J. Hernquist, Lars Narayanan, Desika Hayward, Christopher C. Murray, Norman TI Star formation in galaxy mergers with realistic models of stellar feedback and the interstellar medium SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies: active; galaxies: evolution; galaxies: formation; galaxies: star formation; cosmology: theory ID ULTRALUMINOUS INFRARED GALAXIES; SUPERMASSIVE BLACK-HOLES; MOVING-MESH COSMOLOGY; REDSHIFT SUBMILLIMETER GALAXIES; GAS-RICH MERGERS; PARTICLE HYDRODYNAMICS SIMULATIONS; SPITZER MIDINFRARED SPECTROSCOPY; CO-H2 CONVERSION FACTOR; DUST-OBSCURED GALAXIES; TULLY-FISHER RELATION AB We use hydrodynamic simulations with detailed, explicit models for stellar feedback to study galaxy mergers. These high-resolution (similar to 1 pc) simulations follow the formation and destruction of individual giant molecular clouds (GMC) and star clusters. We find that the final starburst is dominated by in situ star formation, fuelled by gas which flows inwards due to global torques. The resulting high gas density results in rapid star formation. The gas is self-gravitating, and forms massive (less than or similar to 10(10) M-circle dot) GMC and subsequently super star clusters (with masses up to 10(8) M-circle dot). However, in contrast to some recent simulations, the bulk of new stars which eventually form the central bulge are not born in super-clusters which then sink to the centre of the galaxy. This is because feedback efficiently disperses GMC after they turn several per cent of their mass into stars. In other words, most of the mass that reaches the nucleus does so in the form of gas. The Kennicutt-Schmidt law emerges naturally as a consequence of feedback balancing gravitational collapse, independent of the small-scale star formation microphysics. The same mechanisms that drive this relation in isolated galaxies, in particular radiation pressure from infrared photons, extend, with no fine-tuning, over seven decades in star formation rate (SFR) to regulate star formation in the most extreme starburst systems with densities greater than or similar to 10(4) M-circle dot pc(-2). This feedback also drives super-winds with large mass-loss rates; however, a significant fraction of the wind material falls back on to the discs at later times, leading to higher post-starburst SFRs in the presence of stellar feedback. This suggests that strong active galactic nucleus feedback may be required to explain the sharp cut-offs in SFR that are observed in post-merger galaxies. We compare the results to those from simulations with no explicit resolution of GMC or feedback ['effective equation-of-state' (EOS) models]. We find that global galaxy properties are similar between EOS and resolved-feedback models. The relic structure and mass profile, and the total mass of stars formed in the nuclear starburst are quite similar, as is the morphological structure during and after mergers (tails, bridges, etc.). Disc survival in sufficiently gas rich mergers is similar in the two cases, and the new models follow the same scalings as derived for the efficiency of disc re-formation after a merger as derived from previous work with the simplified EOS models. While the global galaxy properties are similar between EOS and feedback models, subgalaxy-scale properties and the SFRs can be quite different: the more detailed models exhibit significantly higher star formation in tails and bridges (especially in shocks), and allow us to resolve the formation of super star clusters. In the new models, the star formation is more strongly time-variable and drops more sharply between close passages. The instantaneous burst enhancement can be higher or lower, depending on the details of the orbit and initial structural properties of the galaxies; first-passage bursts are more sensitive to these details than those at the final coalescence. C1 [Hopkins, Philip F.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Cox, Thomas J.] Carnegie Observ, Pasadena, CA 91101 USA. [Hernquist, Lars] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Narayanan, Desika] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Hayward, Christopher C.] Heidelberger Inst Theoret Studien, D-69118 Heidelberg, Germany. [Murray, Norman] Univ Toronto, Canadian Inst Theoret Astrophys, Toronto, ON M5S 3H8, Canada. [Murray, Norman] Univ Alberta, Canada Res Chair Astron & Astrophys, Edmonton, AB T6G 2M7, Canada. RP Hopkins, PF (reprint author), Univ Calif Berkeley, Dept Astron, 601 Campbell Hall, Berkeley, CA 94720 USA. EM phopkins@astro.berkeley.edu RI Hayward, Christopher/I-4756-2012 OI Hayward, Christopher/0000-0003-4073-3236 FU NASA through Chandra X-ray Observatory Center [PF1-120083]; NASA [NAS8-03060] FX We thank Eliot Quataert for helpful discussions and contributions motivating this work, and our referee, Matthias Steinmetz, for several useful suggestions. Support for PFH was provided by NASA through Einstein Postdoctoral Fellowship Award Number PF1-120083 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. NR 180 TC 75 Z9 75 U1 0 U2 0 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 APR PY 2013 VL 430 IS 3 BP 1901 EP 1927 DI 10.1093/mnras/stt017 PG 27 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 148QG UT WOS:000319260500030 ER PT J AU Raddi, R Drew, JE Fabregat, J Steeghs, D Wright, NJ Sale, SE Farnhill, HJ Barlow, MJ Greimel, R Sabin, L Corradi, RML Drake, JJ AF Raddi, R. Drew, J. E. Fabregat, J. Steeghs, D. Wright, N. J. Sale, S. E. Farnhill, H. J. Barlow, M. J. Greimel, R. Sabin, L. Corradi, R. M. L. Drake, J. J. TI First results of an H alpha based search of classical Be stars in the Perseus Arm and beyond SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE stars: early-type; stars: emission-line, Be; dust, extinction; ISM: structure; Galaxy: structure ID NORTHERN GALACTIC PLANE; T-TAURI STARS; MILKY-WAY; INTERSTELLAR EXTINCTION; SPIRAL STRUCTURE; W4 CHIMNEY/SUPERBUBBLE; ABSOLUTE MAGNITUDES; MOLECULAR CLOUD; OPEN CLUSTERS; IPHAS AB We investigate a region of the Galactic plane, between 120 degrees <= l <= 140 degrees and -1 degrees <= b <= +4 degrees, and uncover a population of moderately reddened (E(B - V) similar to 1) classical Be stars within and beyond the Perseus and Outer Arms. 370 candidate emission-line stars (13 less than or similar to r less than or similar to 16) selected from the Isaac Newton Telescope Photometric H alpha Survey of the Northern Galactic plane have been followed up spectroscopically. A subset of these, 67 stars with properties consistent with those of classical Be stars, have been observed at sufficient spectral resolution (Delta lambda approximate to 2-4 angstrom) at blue wavelengths to narrow down their spectral types. We determine these to a precision estimated to be +/-1 subtype and then we measure reddenings via spectral energy distribution fitting with reference to appropriate model atmospheres. Corrections for contribution to colour excess from circumstellar discs are made using an established scaling to H alpha emission equivalent width. Spectroscopic parallaxes are obtained after luminosity class has been constrained via estimates of distances to neighbouring A/F stars with similar reddenings. Overwhelmingly, the stars in the sample are confirmed as luminous classical Be stars at heliocentric distances ranging from 2 kpc up to similar to 2 kpc. However, the errors are presently too large to enable the cumulative distribution function with respect to distance to distinguish between models placing the stars exclusively in spiral arms, or in a smooth exponentially declining distribution. C1 [Raddi, R.; Drew, J. E.; Farnhill, H. J.] Univ Hertfordshire, Ctr Astrophys Res, STRI, Hatfield AL10 9AB, Herts, England. [Fabregat, J.] Univ Valencia, Astron Observ, E-46100 Burjassot, Spain. [Steeghs, D.] Univ Warwick, Dept Phys, Coventry CV4 9BU, W Midlands, England. [Wright, N. J.; Drake, J. J.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. [Sale, S. E.] Univ Valparaiso, Dept Fis & Astron, Fac Ciencias, Valparaiso, Chile. [Sale, S. E.] Pontificia Univ Catolica Chile, Dept Astron & Astrofis, Santiago 22, Chile. [Sale, S. E.] Rudolf Peierls Ctr Theoret Phys, Oxford OX1 3NP, England. [Barlow, M. J.] UCL, Dept Phys & Astron, London WC1E 6BT, England. [Greimel, R.] Graz Univ, Inst Phys, Inst Geophys Astrophys & Meteorol, A-8010 Graz, Austria. [Sabin, L.] Univ Guadalajara, Inst Aston & Meteorol, Dept Fis, CUCEI, Guadalajara 44130, Jal, Mexico. [Corradi, R. M. L.] Inst Astrofis Canarias, E-38200 Tenerife, Spain. [Corradi, R. M. L.] Univ La Laguna, Dept Astrofis, E-38206 Tenerife, Spain. RP Raddi, R (reprint author), Univ Hertfordshire, Ctr Astrophys Res, STRI, Coll Lane Campus, Hatfield AL10 9AB, Herts, England. EM r.raddi1@herts.ac.uk RI Steeghs, Danny/C-5468-2009; Barlow, Michael/A-5638-2009; Fabregat, Juan/F-9066-2016; OI Steeghs, Danny/0000-0003-0771-4746; Barlow, Michael/0000-0002-3875-1171; Fabregat, Juan/0000-0002-5986-9347; Sale, Stuart/0000-0003-2155-0995; Raddi, Roberto/0000-0002-9090-9191 FU University of Hertfordshire; Spanish Plan Nacional de I+D+i; FEDER [AYA2010-18352]; Generalitat Valenciana [PROMETEO/2009/064]; Ministry for the Economy, Development, and Tourism's Programa Iniciativa Cientifica Milenio [P07-021-F] FX This paper makes use of data obtained as part of IPHAS carried out at the Isaac Newton Telescope (INT). The INT is operated at the island of La Palma by the Isaac Newton Group in the Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias. All IPHAS data are processed by the Cambridge Astronomical Survey Unit, at the Institute of Astronomy in Cambridge. We also acknowledge the use of data obtained at the INT and the Nordic Optical Telescope as part of a CCI International Time Programme. The low-resolution spectra were obtained at the FLWO 1.5 m with FAST, which is operated by Harvard-Smithsonian Center for Astrophysics. In particular, we would like to thank Perry Berlind and Mike Calkins for their role in obtaining most of the FLWO 1.5 m/FAST data. RR acknowledges the University of Hertfordshire for the studentship support. The work of JF is supported by the Spanish Plan Nacional de I+D+i and FEDER under contract AYA2010-18352, and partially supported by the Generalitat Valenciana project of excellence PROMETEO/2009/064. DS acknowledges an STFC Advanced Fellowship. Support for SES is provided by the Ministry for the Economy, Development, and Tourism's Programa Iniciativa Cientifica Milenio through grant P07-021-F, awarded to The Milky Way Millennium Nucleus. NR 66 TC 6 Z9 6 U1 0 U2 8 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 APR PY 2013 VL 430 IS 3 BP 2169 EP 2187 DI 10.1093/mnras/stt038 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 148QG UT WOS:000319260500052 ER PT J AU Liu, GL Zakamska, NL Greene, JE Nesvadba, NPH Liu, X AF Liu, Guilin Zakamska, Nadia L. Greene, Jenny E. Nesvadba, Nicole P. H. Liu, Xin TI Observations of feedback from radio-quiet quasars - I. Extents and morphologies of ionized gas nebulae SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE quasars: emission lines ID DIGITAL SKY SURVEY; ACTIVE GALACTIC NUCLEI; HUBBLE-SPACE-TELESCOPE; EMISSION-LINE NEBULAE; BLACK-HOLE MASS; INTEGRAL-FIELD SPECTROSCOPY; TYPE-2 QUASARS; II QUASARS; HOST GALAXIES; SEYFERT-GALAXIES AB Black hole feedback - the strong interaction between the energy output of supermassive black holes and their surrounding environments - is routinely invoked to explain the absence of overly luminous galaxies, the black hole versus bulge correlations and the similarity of black hole accretion and star formation histories. Yet direct probes of this process in action are scarce and limited to small samples of active nuclei. In this paper, we present Gemini Integral Field Unit observations of the distribution of ionized gas around luminous, obscured, radio-quiet quasars at z similar to 0.5. We detect extended ionized gas nebulae via [O III] lambda 5007 angstrom emission in every case, with a mean diameter of 28 kpc. These nebulae are nearly perfectly round, with H beta surface brightness declining proportional to R-3.5 +/- (1.0). The regular morphologies of nebulae around radio-quiet quasars are in striking contrast with lumpy or elongated [O III] nebulae seen around radio galaxies at low and high redshifts. We present the uniformly measured size-luminosity relationship of [O III] nebulae around Seyfert 2 galaxies and type 2 quasars spanning six orders of magnitude in luminosity and confirm the flat slope of the correlation (R-[O III] proportional to L-[O III](0.25+/-0.02)). We propose a model of clumpy nebulae in which clouds that produce line emission transition from being ionization-bounded at small distances from the quasar to being matter-bounded in the outer parts of the nebula. The model - which has a declining pressure profile - qualitatively explains line ratio profiles and surface brightness profiles seen in our sample. It is striking that we see such smooth and round large-scale gas nebulosities in this sample, which are inconsistent with illuminated merger debris and which we suggest may be the signature of accretion energy from the nucleus reaching gas at large scales. C1 [Liu, Guilin; Zakamska, Nadia L.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Greene, Jenny E.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. [Nesvadba, Nicole P. H.] Univ Paris 11, CNRS, Inst Astrophys Spatiale, F-91405 Orsay, France. [Liu, Xin] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Liu, GL (reprint author), Johns Hopkins Univ, Dept Phys & Astron, 3400 North Charles St, Baltimore, MD 21218 USA. EM liu@pha.jhu.edu FU Alfred P. Sloan Fellowship; Theodore Dunham, Jr. Grant of the Fund for Astrophysical Research; NASA through Einstein Postdoctoral Fellowship [PF0-110076]; NASA [NAS8-03060] FX We thank M. Swinbank and M. Westmoquette for help with data reduction. We acknowledge useful discussions with R. Cen, E. Choi, V. Gaibler, J. Krolik, M. C. Miller, N. Murray, G. S. Novak, J. P. Ostriker, J. Silk, A. Socrates, S. Tremaine, S. Veilleux and the anonymous referee. NLZ is grateful to the Institute for Advanced Study in Princeton, NJ (where part of this work was performed) for hospitality. NLZ is supported in part by the Alfred P. Sloan Fellowship. GL and NLZ acknowledge support from the Theodore Dunham, Jr. Grant of the Fund for Astrophysical Research. Support for the work of XL was provided by NASA through Einstein Postdoctoral Fellowship grant number PF0-110076 awarded by the Chandra X-ray Center, which is operated by the Smithsonian Astrophysical Observatory for NASA under contract NAS8-03060. NR 115 TC 53 Z9 53 U1 0 U2 4 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 APR PY 2013 VL 430 IS 3 BP 2327 EP 2345 DI 10.1093/mnras/stt051 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 148QG UT WOS:000319260500062 ER PT J AU Bar-Gill, N Pham, LM Jarmola, A Budker, D Walsworth, RL AF Bar-Gill, N. Pham, L. M. Jarmola, A. Budker, D. Walsworth, R. L. TI Solid-state electronic spin coherence time approaching one second SO NATURE COMMUNICATIONS LA English DT Article ID DIAMOND; DYNAMICS; RESOLUTION; BATH; NMR AB Solid-state spin systems such as nitrogen-vacancy colour centres in diamond are promising for applications of quantum information, sensing and metrology. However, a key challenge for such solid-state systems is to realize a spin coherence time that is much longer than the time for quantum spin manipulation protocols. Here we demonstrate an improvement of more than two orders of magnitude in the spin coherence time (T-2) of nitrogen-vacancy centres compared with previous measurements: T-2 approximate to 0.6 s at 77 K. We employed dynamical decoupling pulse sequences to suppress nitrogen-vacancy spin decoherence, and found that T-2 is limited to approximately half of the longitudinal spin relaxation time over a wide range of temperatures, which we attribute to phonon-induced decoherence. Our results apply to ensembles of nitrogen-vacancy spins, and thus could advance quantum sensing, enable squeezing and many-body entanglement, and open a path to simulating driven, interaction-dominated quantum many-body Hamiltonians. C1 [Bar-Gill, N.; Walsworth, R. L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Bar-Gill, N.; Walsworth, R. L.] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. [Pham, L. M.] Harvard Univ, Sch Engn & Appl Sci, Cambridge, MA 02138 USA. [Jarmola, A.; Budker, D.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. [Budker, D.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Div Nucl Sci, Berkeley, CA 94720 USA. RP Bar-Gill, N (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM nbar-gill@cfa.harvard.edu; rwalsworth@cfa.harvard.edu RI Budker, Dmitry/F-7580-2016 OI Budker, Dmitry/0000-0002-7356-4814 FU DARPA QuASAR program; QuEST program; MURI-QuISM program; NSF; IMOD; NATO Science for Peace Programme FX This research has been supported by the DARPA QuASAR, QuEST and MURI-QuISM programs, NSF, IMOD, and the NATO Science for Peace Programme. We gratefully acknowledge the provision of diamond samples by Element Six, and helpful technical discussions with Ran Fischer, Daniel Twitchen, Matthew Markham, Alastair Stacey, Keigo Arai, Chinmay Belthangady, David Glenn and David Le Sage. NR 35 TC 127 Z9 128 U1 3 U2 86 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 APR PY 2013 VL 4 AR 1743 DI 10.1038/ncomms2771 PG 6 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 143MR UT WOS:000318872100100 PM 23612284 ER PT J AU Ortega, HE Graupner, PR Asai, Y TenDyke, K Qiu, DY Shen, YYC Rios, N Arnold, AE Coley, PD Kursar, TA Gerwick, WH Cubilla-Rios, L AF Ortega, Humberto E. Graupner, Paul R. Asai, Yumi TenDyke, Karen Qiu, Dayong Shen, Young Yongchun Rios, Nivia Arnold, A. Elizabeth Coley, Phyllis D. Kursar, Thomas A. Gerwick, William H. Cubilla-Rios, Luis TI Mycoleptodiscins A and B, Cytotoxic Alkaloids from the Endophytic Fungus Mycoleptodiscus sp F0194 SO JOURNAL OF NATURAL PRODUCTS LA English DT Article ID RED PYRROLOQUINOLINE ALKALOIDS; METABOLITES AB Two novel reddish-orange alkaloids, mycoleptodiscin A (1) and mycoleptodiscin B (2), were isolated from liquid cultures of the endophytic fungus Mycoleptodiscus sp. that had been isolated from Desmotes incomparabilis in Panama. Elucidation of their structures was accomplished using 1D and 2D NMR spectroscopy in combination with IR spectroscopic and MS data. These compounds are indole-terpenes with a new skeleton uncommon in nature. Mycoleptodiscin B (2) was active in inhibiting the growth of cancer cell lines with IC50 values in the range 0.60-0.78 mu M. C1 [Ortega, Humberto E.; Cubilla-Rios, Luis] Univ Panama, Fac Nat Exact Sci & Technol, Lab Trop Bioorgan Chem, Panama City, Panama. [Graupner, Paul R.] Dow AgroSci, Nat Prod Discovery, Indianapolis, IN 46268 USA. [Asai, Yumi] Eisai & Co Ltd, Tsukuba, Ibaraki 3002635, Japan. [TenDyke, Karen; Qiu, Dayong; Shen, Young Yongchun] Eisai Inc, Andover, MA 01810 USA. [Rios, Nivia] Univ Panama, Dept Microbiol, Panama City, Panama. [Arnold, A. Elizabeth] Univ Arizona, Sch Plant Sci, Tucson, AZ USA. [Coley, Phyllis D.; Kursar, Thomas A.] Univ Utah, Dept Biol, Salt Lake City, UT 84112 USA. [Coley, Phyllis D.; Kursar, Thomas A.; Cubilla-Rios, Luis] Smithsonian Trop Res Inst, Panama City, Panama. [Gerwick, William H.] Univ Calif San Diego, Scripps Inst Oceanog, La Jolla, CA 92093 USA. RP Cubilla-Rios, L (reprint author), Univ Panama, Fac Nat Exact Sci & Technol, Lab Trop Bioorgan Chem, Panama City, Panama. EM lucr@ancon.up.ac.pa FU U.S. NIH (ICBG-Panama) [2 U01TW006634-06]; College of Agriculture and Life Sciences at the University of Arizona FX This work was supported by a U.S. NIH grant for the International Cooperative Biodiversity Groups Program (ICBG-Panama; 2 U01TW006634-06) and the College of Agriculture and Life Sciences at the University of Arizona. We express our thanks to Dr. C. Spadafora for conducting the MCF-7 bioassay, M. Gunatilaka for assisting in classifying the isolate, Dr. E. Suh of Eisai Inc. for his encouragement and support, and the personnel of Panama's Autoridad Nacional del Ambiente for facilitating this research. NR 17 TC 16 Z9 17 U1 7 U2 41 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0163-3864 J9 J NAT PROD JI J. Nat. Prod. PD APR PY 2013 VL 76 IS 4 BP 741 EP 744 DI 10.1021/np300792t PG 4 WC Plant Sciences; Chemistry, Medicinal; Pharmacology & Pharmacy SC Plant Sciences; Pharmacology & Pharmacy GA 135CX UT WOS:000318264700038 PM 23560689 ER PT J AU Shockley, FW Greenwalt, D AF Shockley, Floyd W. Greenwalt, Dale TI PTENIDIUM KISHENEHNICUM (COLEOPTERA: PTILIIDAE), A NEW FOSSIL DESCRIBED FROM THE KISHENEHN OIL SHALES, WITH A CHECKLIST OF PREVIOUSLY KNOWN FOSSIL PTILIIDS SO PROCEEDINGS OF THE ENTOMOLOGICAL SOCIETY OF WASHINGTON LA English DT Article DE compression fossil; feather-winged beetles; fossil beetles; taxonomy; paleoentomology ID FEATHERWING BEETLES; INSECTS AB Ptenidium kishenehnicum Shockley and Greenwalt, a new species of feather-winged beetle (Coleoptera: Ptiliidae), is described from 46 million year old Kishenehn oil shales in Montana, USA. This compression fossil is the first beetle species to be described from this formation. A checklist of known fossils and their ages is provided. C1 [Shockley, Floyd W.] Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol, Washington, DC 20013 USA. [Greenwalt, Dale] Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20013 USA. RP Shockley, FW (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol, POB 37012,MRC 165, Washington, DC 20013 USA. EM ShockleyF@si.edu; GreenwaltD@si.edu NR 35 TC 5 Z9 5 U1 0 U2 5 PU ENTOMOL SOC WASHINGTON PI WASHINGTON PA SMITHSONIAN INSTITUTION DEPT ENTOMOLOGY, WASHINGTON, DC 20560 USA SN 0013-8797 J9 P ENTOMOL SOC WASH JI Proc. Entomol. Soc. Wash. PD APR PY 2013 VL 115 IS 2 BP 173 EP 181 DI 10.4289/0013-8797.115.2.173 PG 9 WC Entomology SC Entomology GA 141VF UT WOS:000318753900007 ER PT J AU Looper, MD Mazur, JE Blake, JB Spence, HE Schwadron, NA Golightly, MJ Case, AW Kasper, JC Townsend, LW AF Looper, M. D. Mazur, J. E. Blake, J. B. Spence, H. E. Schwadron, N. A. Golightly, M. J. Case, A. W. Kasper, J. C. Townsend, L. W. TI The radiation environment near the lunar surface: CRaTER observations and Geant4 simulations SO SPACE WEATHER-THE INTERNATIONAL JOURNAL OF RESEARCH AND APPLICATIONS LA English DT Article AB At the start of the Lunar Reconnaissance Orbiter mission in 2009, its Cosmic Ray Telescope for the Effects of Radiation instrument measured the radiation environment near the Moon during the recent deep solar minimum, when galactic cosmic rays (GCRs) were at the highest level observed during the space age. We present observations that show the combined effects of GCR primaries, secondary particles (albedo) created by the interaction of GCRs with the lunar surface, and the interactions of these particles in the shielding material overlying the silicon solid-state detectors of the Cosmic Ray Telescope for the Effects of Radiation. We use Geant4 to model the energy and angular distribution of the albedo particles, and to model the response of the sensor to the various particle species reaching the 50 kilometer altitude of the Lunar Reconnaissance Orbiter. Using simulations to gain insight into the observations, we are able to present preliminary energy-deposit spectra for evaluation of the radiation environment's effects on other sensitive materials, whether biological or electronic, that would be exposed to a similar near-lunar environment. C1 [Looper, M. D.; Blake, J. B.] Aerosp Corp, El Segundo, CA 90245 USA. [Mazur, J. E.] Aerosp Corp, Chantilly, VA USA. [Spence, H. E.; Schwadron, N. A.; Golightly, M. J.] Univ New Hampshire, Inst Study Earth Oceans & Space, Durham, NH 03824 USA. [Case, A. W.; Kasper, J. C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Townsend, L. W.] Univ Tennessee, Dept Nucl Engn, Knoxville, TN 37996 USA. RP Looper, MD (reprint author), Aerosp Corp, El Segundo, CA 90245 USA. EM mark.d.looper@aero.org RI Kasper, Justin/D-1152-2010; OI Kasper, Justin/0000-0002-7077-930X; Spence, Harlan/0000-0002-2526-2205 FU NASA [GC189307NGA] FX We acknowledge the efforts of the CRaTER instrument team in developing and fielding the instrument hardware, as well as the LRO project team at NASA GSFC for the success of the LRO mission. This work was supported by NASA under contract GC189307NGA. NR 11 TC 7 Z9 7 U1 1 U2 7 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 1542-7390 J9 SPACE WEATHER JI Space Weather PD APR PY 2013 VL 11 IS 4 BP 142 EP 152 DI 10.1002/swe.20034 PG 11 WC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology & Atmospheric Sciences SC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology & Atmospheric Sciences GA 140EH UT WOS:000318636700005 ER PT J AU Moser, WE Richardson, DJ Hammond, CI Lazo-Wasem, EA AF Moser, William E. Richardson, Dennis J. Hammond, Charlotte I. Lazo-Wasem, Eric A. TI Redescription of Placobdella papillifera Verrill, 1872 (Hirudinida: Glossiphoniidae) SO BULLETIN OF THE PEABODY MUSEUM OF NATURAL HISTORY LA English DT Article DE Placobdella papillifera; Helobdella papillata; Clepsine; Glossiphoniidae; Hirudinida; Hirudinea; leeches; Verrill; Connecticut; New England ID MITOCHONDRIAL GENE-SEQUENCES; MORPHOLOGICAL DATA; PHYLOGENY; RECORDS AB The identification and taxonomy of Placobdella papillifera (Verrill, 1872) Moore, 1952 have been blurred by its varieties and have been compounded by the apparent lack of type material. Leeches collected from May 2008 through August 2012 from West River, New Haven, New Haven County, Connecticut, the type locality of Clepsine papillifera Verrill, 1872, were consistant with P. papillifera (Verrill, 1872) Moore 1952 as described by Verrill (1872). The acquisition of these specimens from the type locality facilitated redescription of P. papillifera. A neotype is designated to stabilize the concept of P. papillifera. Placobdella papillifera appears to exhibit relatively low host specificity, having been documented on Chrysemys picta, Chelydra serpentina, Sternotherus odoratus and Homo sapiens in this study. Molecular comparison of CO-I sequence data from P. papillifera revealed differences of 15% from Placobdella ornata, 16% from P. rugosa, 18% from P. all, 17% from P. multilineata and 14% from P. parasitica. C1 [Moser, William E.] Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, Museum Support Ctr MRC 534, Suitland, MD 20746 USA. [Richardson, Dennis J.; Hammond, Charlotte I.] Quinnipiac Coll, Sch Biol Sci, Hamden, CT 06518 USA. [Lazo-Wasem, Eric A.] Yale Univ, Peabody Museum Nat Hist, Div Invertebrate Zool, New Haven, CT 06520 USA. RP Moser, WE (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, Museum Support Ctr MRC 534, 4210 Silver Hill Rd, Suitland, MD 20746 USA. EM moserw@si.edu; Dennis.Richardson@quinnipiac.edu; Charlotte.Hammond@quinnipiac.edu; eric.lazo-wasem@yale.edu FU Department of Biological Sciences; Schools of Arts and Sciences and Health Sciences at Quinnipiac University, Hamden, Connecticut FX Kristen E. Richardson and Krystal A. Lazos (Quinnipiac University) assisted in field collection. Lourdes M. Rojas (Division of Invertebrate Zoology, Peabody Museum of Natural History, Yale University) provided valuable assistance in specimen management. Harry Coyle (New Haven Parks and Recreation) provided valuable logistic insight. The State of Connecticut Department of Energy and Environmental Protection granted permission to collect leeches. Allen Collins (National Systematics Laboratory, National Marine Fisheries Service, Washington, DC) provided valuable assistance and insight with molecular data analyses. Funding for this project was provided in part by the Department of Biological Sciences and the Schools of Arts and Sciences and Health Sciences at Quinnipiac University, Hamden, Connecticut. NR 24 TC 0 Z9 1 U1 2 U2 7 PU PEABODY MUSEUM NATURAL HISTORY-YALE UNIV PI NEW HAVEN PA 170 WHITNEY AVE, PO BOX 208118, NEW HAVEN, CT 06520-8118 USA SN 0079-032X J9 B PEABODY MUS NAT HI JI Bull. Peabody Mus. Natl. Hist. PD APR PY 2013 VL 54 IS 1 BP 125 EP 131 PG 7 WC Biodiversity Conservation; Ecology SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 137RV UT WOS:000318456000005 ER PT J AU Vinn, O Luque, J AF Vinn, Olev Luque, Javier TI First record of a pectinariid-like (Polychaeta, Annelida) agglutinated worm tube from the Late Cretaceous of Colombia SO CRETACEOUS RESEARCH LA English DT Article DE Polychaeta; Pectinariidae; Tubeworms; Santonian; South America ID CALIFORNIA; FAUNAS AB The earliest agglutinated pectinariid-like tube with a modern appearance is described from the Late Cretaceous (Santonian, similar to 84 My) of Colombia. The rare agglutinated fossil tube is composed of sorted skeletal material, quartz sand, and unidentified carbonaceous fragments. It's solitary and non-encrusting life mode, the straight conical shape, and the agglutinated tube wall composed of sand-sized grains, supports affinity with the tube-building Family Pectinariidae. This finding suggests that Pectinariidae might have first appeared in the Neotropics at least by the late Mesozoic. (c) 2012 Elsevier Ltd. All rights reserved. C1 [Vinn, Olev] Univ Tartu, Dept Geol, EE-50411 Tartu, Estonia. [Luque, Javier] Smithsonian Trop Res Inst, Panama City 084303092, Panama. RP Vinn, O (reprint author), Univ Tartu, Dept Geol, Ravila 14A, EE-50411 Tartu, Estonia. EM olev.vinn@ut.ee; javierluquec@gmail.com OI Vinn, Olev/0000-0002-2889-2544 FU STRI; Paleontological Society; Estonian Science Foundation [ETF9064]; Estonian Ministry of Education and Science [SF0180051s08] FX J.L. thanks Carlos Jaramillo (STRI) for providing funds and facilities to allow the collection of the specimen and development of the present research. Harry A. ten Hove, Sancia van der Meij, Michal Zaton, Igor A. Jirkov, Mario H. Londono Mesa, Sergio Salazar, Alexander Tzelin and Stephen Gardiner are thanked for their valuable comments and advice. Cesar Silva (STRI) and Jakeline Vanegas assisted in the field. Fernando Etayo-Serna (Colombian Geological Survey) supplied intellectual support. Kecia Kerr (McGill) assisted with editing of the manuscript. Hans Hillewaert photographed the extant pectinariid polychaete. Jose Arenas (Colombian Geological Survey) provided export permits. O.V. is grateful to The Paleontological Society for receipt of a J.J. Sepkoski Grant, to the Estonian Science Foundation for grant ETF9064 and to a target-financed project from the Estonian Ministry of Education and Science (SF0180051s08) for financial support. We are grateful to Mark A. Wilson (The College of Wooster) and anonymous reviewer for the constructive reviews. We also are grateful to journal editor Peter Harries for several improvements in the manuscript. NR 18 TC 6 Z9 6 U1 1 U2 6 PU ACADEMIC PRESS LTD- ELSEVIER SCIENCE LTD PI LONDON PA 24-28 OVAL RD, LONDON NW1 7DX, ENGLAND SN 0195-6671 J9 CRETACEOUS RES JI Cretac. Res. PD APR PY 2013 VL 41 BP 107 EP 110 DI 10.1016/j.cretres.2012.11.004 PG 4 WC Geology; Paleontology SC Geology; Paleontology GA 112HG UT WOS:000316582700010 ER PT J AU Trinidad, MA Curiel, S Estalella, R Canto, J Raga, A Torrelles, JM Patel, NA Gomez, JF Anglada, G Carrasco-Gonzalez, C Rodriguez, LF AF Trinidad, M. A. Curiel, S. Estalella, R. Canto, J. Raga, A. Torrelles, J. M. Patel, N. A. Gomez, J. F. Anglada, G. Carrasco-Gonzalez, C. Rodriguez, L. F. TI Formation and evolution of the water maser outflow event in AFGL 2591 VLA 3-N SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE masers; stars: formation; ISM: individual objects: AFGL 2591; ISM: jets and outflows ID YOUNG STELLAR OBJECTS; MASSIVE PROTOSTAR CEPHEUS; LARGE PROPER MOTIONS; STAR-FORMING REGION; HIGH-VELOCITY; PROTOPLANETARY DISKS; MOLECULAR OUTFLOWS; RADIO-CONTINUUM; BIPOLAR OUTFLOW; MAGNETIC-FIELD AB In this paper we analyse multi-epoch very long baseline interferometry water maser observations carried out with the Very Long Baseline Array towards the high-mass star-forming region AFGL 2591. We detected maser emission associated with the radio continuum sources VLA 2 and VLA 3. In addition, a water maser cluster, VLA 3-N, was detected similar to 0.5 arcsec north of VLA 3. We concentrate the discussion of this paper on the spatio-kinematical distribution of the water masers towards VLA 3-N. The water maser emission towards the region VLA 3-N shows two bow-shock-like structures, northern and southern, separated from each other by similar to 100 mas (similar to 330 au). The spatial distribution and kinematics of the water masers in this cluster have persisted over a time span of 7 yr. The northern bow shock has a somewhat irregular morphology, while the southern one has a remarkably smooth morphology. We measured the proper motions of 33 water maser features, which have an average proper motion velocity of similar to 1.3mas yr(-1) (similar to 20 km s(-1)). The morphology and the proper motions of this cluster of water masers show systematic expanding motions that could imply one or two different centres of star formation activity. We made a detailed model for the southern structure, proposing two different kinematic models to explain the three-dimensional spatio-kinematical distribution of the water masers: (1) a static central source driving the two bow-shock structures and (2) two independent driving sources, one of them exciting the northern bow-shock structure, and the other one, a young runaway star moving in the local molecular medium exciting and moulding the remarkably smoother southern bow-shock structure. Future observations will be necessary to discriminate between the two scenarios, in particular by identifying the still unseen driving source(s). C1 [Trinidad, M. A.] Univ Guanajuato, Dept Astron, Guanajuato 36000, Mexico. [Curiel, S.; Canto, J.] Univ Nacl Autonoma Mexico, Inst Astron, Mexico City 04510, DF, Mexico. [Estalella, R.] Univ Barcelona, Dept Astron & Meteorol, E-08028 Barcelona, Spain. [Estalella, R.] Univ Barcelona, Inst Ciencies Cosmos, IEEC, E-08028 Barcelona, Spain. [Raga, A.] Univ Nacl Autonoma Mexico, Inst Ciencias Nucl, Mexico City 04510, DF, Mexico. [Torrelles, J. M.] Univ Barcelona, IEEC, CSIC, Inst Ciencias Espacio, E-08028 Barcelona, Spain. [Patel, N. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Gomez, J. F.; Anglada, G.] CSIC, Inst Astrofis Andalucia, E-18080 Granada, Spain. [Carrasco-Gonzalez, C.] Max Planck Inst Radioastron MPIfR, D-53121 Bonn, Germany. [Rodriguez, L. F.] UNAM, Ctr Radioastron & Astrofis, Morelia 58089, Michoacan, Mexico. RP Trinidad, MA (reprint author), Univ Guanajuato, Dept Astron, Apdo Postal 144, Guanajuato 36000, Mexico. EM trinidad@astro.ugto.mx; torrelles@ieec.cat RI Gomez, Jose Francisco/D-8392-2016; OI Gomez, Jose Francisco/0000-0002-7065-542X; Torrelles, Jose Maria/0000-0002-6896-6085 FU MICINN (Spain) [AYA2011-30228-C03]; FEDER funds; CONACyT [61547, 60581, 168251, 82543]; DGAPA; UNAM; CONACyT (Mexico); AGAUR (Catalonia) [2009SGR1172] FX We would like to thank our referee for the very careful and useful report on our manuscript. GA, CC-G, RE, JFG and JMT acknowledge support from MICINN (Spain) AYA2011-30228-C03 grant (co-funded with FEDER funds). JC and ACR acknowledge support from CONACyT grant 61547. SC acknowledges support from CONACyT grants 60581 and 168251. LFR acknowledges the support of DGAPA, UNAM and CONACyT (Mexico). MAT acknowledges support from CONACyT grant 82543. RE and JMT acknowledge support from AGAUR (Catalonia) 2009SGR1172 grant. The ICC (UB) is a CSIC-Associated Unit through the ICE (CSIC). NR 55 TC 7 Z9 7 U1 0 U2 3 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 APR PY 2013 VL 430 IS 2 BP 1309 EP 1323 DI 10.1093/mnras/sts707 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 135FY UT WOS:000318275000044 ER PT J AU Carretti, E Brown, S Staveley-Smith, L Malarecki, M Bernardi, G Gaensler, BM Haverkorn, M Kesteven, MJ Poppi, S AF Carretti, E. Brown, S. Staveley-Smith, L. Malarecki, M. Bernardi, G. Gaensler, B. M. Haverkorn, M. Kesteven, M. J. Poppi, S. TI Detection of a radio bridge in Abell 3667 SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE acceleration of particles; polarization; radiation mechanisms: non-thermal; shock waves; galaxies: clusters: general; galaxies: clusters: individual: A3667 ID LARGE-SCALE STRUCTURE; X-RAY-EMISSION; CLUSTER MERGERS; SHOCK-WAVES; NONTHERMAL EMISSION; GALAXY CLUSTERS; COSMIC-RAYS; HALOS; PREDICTIONS; FREQUENCY AB We have detected a radio bridge of unpolarized synchrotron emission connecting the NW relic of the galaxy cluster Abell 3667 to its central regions. We used data at 2.3 GHz from the S-band Polarization All Sky Survey and at 3.3 GHz from a follow-up observation, both conducted with the Parkes radio telescope. This emission is further aligned with a diffuse X-ray tail, and represents the most compelling evidence for an association between intracluster medium turbulence and diffuse synchrotron emission. This is the first clear detection of a bridge associated both with an outlying cluster relic and X-ray diffuse emission. All the indicators point towards the synchrotron bridge being related to the post-shock turbulent wake trailing the shock front generated by a major merger in a massive cluster. Although predicted by simulations, this is the first time such emission is detected with high significance and clearly associated with the path of a confirmed shock. Although the origin of the relativistic electrons is still unknown, the turbulent re-acceleration model provides a natural explanation for the large-scale emission. The equipartition magnetic field intensity of the bridge is B-eq = 2.2 +/- 0.3 mu G. We further detect diffuse emission coincident with the central regions of the cluster for the first time. C1 [Carretti, E.] CSIRO Astron & Space Sci, Parkes, NSW 2870, Australia. [Brown, S.; Kesteven, M. J.] CSIRO Astron & Space Sci, Epping, NSW 1710, Australia. [Brown, S.] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA. [Staveley-Smith, L.; Malarecki, M.] Univ Western Australia, Int Ctr Radio Astron Res, Crawley, WA 6009, Australia. [Staveley-Smith, L.] CAASTRO ARC Ctr Excellence All Sky Astrophys, Redfern, NSW 2016, Australia. [Bernardi, G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Gaensler, B. M.] Univ Sydney, Sydney Inst Astron, Sch Phys A29, Sydney, NSW 2006, Australia. [Haverkorn, M.] Radboud Univ Nijmegen, Dept Astrophys IMAPP, NL-6500 GL Nijmegen, Netherlands. [Haverkorn, M.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [Poppi, S.] INAF D Osservatorio Astron Cagliari, I-09012 Capoterra, CA, Italy. RP Carretti, E (reprint author), CSIRO Astron & Space Sci, POB 276, Parkes, NSW 2870, Australia. EM Ettore.Carretti@csiro.au RI Gaensler, Bryan/F-8655-2010; Staveley-Smith, Lister/A-1683-2011; OI Staveley-Smith, Lister/0000-0002-8057-0294; Carretti, Ettore/0000-0002-3973-8403; Poppi, Sergio/0000-0002-4698-2607; Gaensler, Bryan/0000-0002-3382-9558 FU Australian Laureate Fellowship from the Australian Research Council [FL100100114]; Netherlands Organisation for Scientific Research (NWO); Commonwealth of Australia; National Aeronautics and Space Administration; [639.042.915] FX This work has been carried out in the framework of the S-PASS collaboration. We would like to thank Alexis Finoguenov for the electronic image of the XMM X-ray emission of A3667 and an anonymous referee for useful comments that helped improve the paper. BMG acknowledges the support of an Australian Laureate Fellowship from the Australian Research Council through grant FL100100114. MH acknowledges the support of the research programme 639.042.915, which is partly financed by the Netherlands Organisation for Scientific Research (NWO). The Parkes radio telescope is part of the Australia Telescope National Facility which is funded by the Commonwealth of Australia for operation as a National Facility managed by CSIRO. The ATCA is part of the Australia Telescope National Facility 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 Extra-galactic Database (NED) which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. NR 36 TC 8 Z9 8 U1 0 U2 1 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 APR PY 2013 VL 430 IS 2 BP 1414 EP 1422 DI 10.1093/mnras/stt002 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 135FY UT WOS:000318275000056 ER PT J AU Bjerkeli, P Liseau, R Nisini, B Tafalla, M Bergman, P Melnick, G Rydbeck, G AF Bjerkeli, P. Liseau, R. Nisini, B. Tafalla, M. Bergman, P. Melnick, G. Rydbeck, G. TI Physical properties of outflows Comparing CO- and H2O-based parameters in Class 0 sources SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE ISM: molecules; ISM: jets and outflows; stars: formation; stars: winds, outflows ID DRIVEN MOLECULAR OUTFLOWS; STAR-FORMING REGIONS; PROTOSTELLAR OUTFLOWS; BIPOLAR OUTFLOW; WATER EMISSION; HERSCHEL-PACS; H-2 EMISSION; SHOCK-WAVES; L1157; HIFI AB Context. The observed physical properties of outflows from low-mass sources put constraints on possible ejection mechanisms. Historically, these quantities have been derived from CO using ground-based observations. It is, therefore, important to investigate whether parameters such as momentum rate (thrust) and mechanical luminosity (power) are the same when different molecular tracers are used. Aims. Our objective is to determine the outflow momentum, dynamical time-scale, thrust, energy, and power using CO and H2O as tracers of outflow activity. Methods. Within the framework of the Water In Star-forming regions with Herschel (WISH) key program, three molecular outflows from Class 0 sources have been mapped using the Heterodyne Instrument for the Far Infrared (HIFI) instrument aboard Herschel. We used these observations together with previously published H-2 data to infer the physical properties of the outflows. We compared the physical properties derived here with previous estimates based on CO observations. Results. Inspection of the spatial distribution of H2O and H-2 confirms that these molecules are co-spatial. The most prominent emission peaks in H-2 coincide with strong H2O emission peaks and the estimated widths of the flows when using the two tracers are comparable. Conclusions. For the momentum rate and the mechanical luminosity, inferred values are not dependent on which tracer is used, i.e. the values agree to within a factor of 4 and 3, respectively. C1 [Bjerkeli, P.; Liseau, R.; Rydbeck, G.] Chalmers, Dept Earth & Space Sci, Onsala Space Observ, S-43992 Onsala, Sweden. [Nisini, B.] INAF Osservatorio Astron Roma, I-00040 Monte Porzio Catone, Italy. [Tafalla, M.] Observ Astron Nacl IGN, Madrid 28014, Spain. [Bergman, P.] Chalmers, Onsala Space Observ, S-43992 Onsala, Sweden. [Melnick, G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Bjerkeli, P (reprint author), Chalmers, Dept Earth & Space Sci, Onsala Space Observ, S-43992 Onsala, Sweden. EM per.bjerkeli@chalmers.se OI Bjerkeli, Per/0000-0002-7993-4118 FU Swedish National Space Board (SNSB) FX P. Bjerkeli wishes to thank Eva Wirstrom for the interesting discussions. We also appreciate the valuable comments made by the anonymous referee. The authors appreciate the support from the Swedish National Space Board (SNSB). 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 Astronomico Nacional (IGN), Centro de Astrobiologia (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. NR 39 TC 3 Z9 3 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 APR PY 2013 VL 552 AR L8 DI 10.1051/0004-6361/201321194 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 130JW UT WOS:000317912000152 ER PT J AU Busca, NG Delubac, T Rich, J Bailey, S Font-Ribera, A Kirkby, D Le Goff, JM Pieri, MM Slosar, A Aubourg, E Bautista, JE Bizyaev, D Blomqvist, M Bolton, AS Bovy, J Brewington, H Borde, A Brinkmann, J Carithers, B Croft, RAC Dawson, KS Ebelke, G Eisenstein, DJ Hamilton, JC Ho, S Hogg, DW Honscheid, K Lee, KG Lundgren, B Malanushenko, E Malanushenko, V Margala, D Maraston, C Mehta, K Miralda-Escude, J Myers, AD Nichol, RC Noterdaeme, P Olmstead, MD Oravetz, D Palanque-Delabrouille, N Pan, K Paris, I Percival, WJ Petitjean, P Roe, NA Rollinde, E Ross, NP Rossi, G Schlegel, DJ Schneider, DP Shelden, A Sheldon, ES Simmons, A Snedden, S Tinker, JL Viel, M Weaver, BA Weinberg, DH White, M Yeche, C York, DG AF Busca, N. G. Delubac, T. Rich, J. Bailey, S. Font-Ribera, A. Kirkby, D. Le Goff, J-M. Pieri, M. M. Slosar, A. Aubourg, E. Bautista, J. E. Bizyaev, D. Blomqvist, M. Bolton, A. S. Bovy, J. Brewington, H. Borde, A. Brinkmann, J. Carithers, B. Croft, R. A. C. Dawson, K. S. Ebelke, G. Eisenstein, D. J. Hamilton, J-C. Ho, S. Hogg, D. W. Honscheid, K. Lee, K-G. Lundgren, B. Malanushenko, E. Malanushenko, V. Margala, D. Maraston, C. Mehta, K. Miralda-Escude, J. Myers, A. D. Nichol, R. C. Noterdaeme, P. Olmstead, M. D. Oravetz, D. Palanque-Delabrouille, N. Pan, K. Paris, I. Percival, W. J. Petitjean, P. Roe, N. A. Rollinde, E. Ross, N. P. Rossi, G. Schlegel, D. J. Schneider, D. P. Shelden, A. Sheldon, E. S. Simmons, A. Snedden, S. Tinker, J. L. Viel, M. Weaver, B. A. Weinberg, D. H. White, M. Yeche, C. York, D. G. TI Baryon acoustic oscillations in the Ly alpha forest of BOSS quasars SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE cosmology: observations; dark energy; large-scale structure of Universe; cosmological parameters ID DIGITAL SKY SURVEY; HUBBLE-SPACE-TELESCOPE; DATA RELEASE 9; LUMINOUS RED GALAXIES; SMALL-SCALE STRUCTURE; LINE-OF-SIGHT; SDSS-III; SPECTROSCOPIC SURVEY; POWER-SPECTRUM; DARK ENERGY AB We report a detection of the baryon acoustic oscillation (BAO) feature in the three-dimensional correlation function of the transmitted flux fraction in the Ly alpha forest of high-redshift quasars. The study uses 48 640 quasars in the redshift range 2.1 <= z <= 3.5 from the Baryon Oscillation Spectroscopic Survey (BOSS) of the third generation of the Sloan Digital Sky Survey (SDSS-III). At a mean redshift z = 2.3, we measure the monopole and quadrupole components of the correlation function for separations in the range 20 h(-1) Mpc < r < 200 h(-1) Mpc. A peak in the correlation function is seen at a separation equal to (1.01 +/- 0.03) times the distance expected for the BAO peak within a concordance Lambda CDM cosmology. This first detection of the BAO peak at high redshift, when the universe was strongly matter dominated, results in constraints on the angular diameter distance D-A and the expansion rate H at z = 2.3 that, combined with priors on H-0 and the baryon density, require the existence of dark energy. Combined with constraints derived from cosmic microwave background observations, this result implies H(z = 2.3) = (224 +/- 8) km s(-1) Mpc(-1), indicating that the time derivative of the cosmological scale parameter (a) over dot = H(z = 2.3)/(1 + z) is significantly greater than that measured with BAO at z similar to 0.5. This demonstrates that the expansion was decelerating in the range 0.7 < z < 2.3, as expected from the matter domination during this epoch. Combined with measurements of H-0, one sees the pattern of deceleration followed by acceleration characteristic of a dark-energy dominated universe. C1 [Busca, N. G.; Aubourg, E.; Bautista, J. E.; Hamilton, J-C.] Univ Paris 07, CNRS, IN2P3, APC,CEA,Observ Paris, Paris, France. [Delubac, T.; Rich, J.; Le Goff, J-M.; Borde, A.; Palanque-Delabrouille, N.; Rossi, G.; Yeche, C.] CEA, Ctr Saclay, IRFU, F-91191 Gif Sur Yvette, France. [Bailey, S.; Font-Ribera, A.; Carithers, B.; Roe, N. A.; Ross, N. P.; Schlegel, D. J.; White, M.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA. [Kirkby, D.; Blomqvist, M.; Margala, D.] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA. [Pieri, M. M.; Maraston, C.; Nichol, R. C.; Percival, W. J.] Univ Portsmouth, Inst Cosmol & Gravitat, Portsmouth PO1 3FX, Hants, England. [Slosar, A.; Sheldon, E. S.; Snedden, S.] Brookhaven Natl Lab, Upton, NY 11973 USA. [Bizyaev, D.; Brewington, H.; Brinkmann, J.; Ebelke, G.; Malanushenko, E.; Malanushenko, V.; Oravetz, D.; Pan, K.; Shelden, A.; Simmons, A.] Apache Point Observ, Sunspot, NM 88349 USA. [Bolton, A. S.; Dawson, K. S.; Olmstead, M. D.] Univ Utah, Dept Phys & Astron, Salt Lake City, UT 84112 USA. [Bovy, J.] Inst Adv Study, Princeton, NJ 08540 USA. [Croft, R. A. C.; Ho, S.] Carnegie Mellon Univ, Bruce & Astrid McWilliams Ctr Cosmol, Pittsburgh, PA 15213 USA. [Eisenstein, D. J.] Harvard Univ, Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Hogg, D. W.; Tinker, J. L.; Weaver, B. A.] NYU, Ctr Cosmol & Particle Phys, New York, NY 10003 USA. [Honscheid, K.] Ohio State Univ, Dept Phys, Columbus, OH 43210 USA. [Honscheid, K.] Ohio State Univ, Ctr Cosmol & Astroparticle Phys, Columbus, OH 43210 USA. [Lee, K-G.] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Lundgren, B.] Univ Wisconsin, Dept Astron, Madison, WI 53706 USA. [Mehta, K.] Univ Arizona, Steward Observ, Tucson, AZ 85121 USA. [Miralda-Escude, J.] Inst Catalana Recerca & Estudis Avancats, Barcelona, Spain. [Miralda-Escude, J.] Univ Barcelona, IEEC, Inst Ciencies Cosmos, E-08028 Barcelona, Spain. [Myers, A. D.] Univ Wyoming, Dept Phys & Astron, Laramie, WY 82071 USA. [Noterdaeme, P.; Paris, I.; Petitjean, P.; Rollinde, E.] Univ Paris 06, F-75014 Paris, France. [Noterdaeme, P.; Paris, I.; Petitjean, P.; Rollinde, E.] CNRS, Inst Astrophys Paris, F-75014 Paris, France. [Schneider, D. P.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Schneider, D. P.] Penn State Univ, Inst Gravitat & Cosmos, University Pk, PA 16802 USA. [Viel, M.] Osserv Astron Trieste, INAF, I-34131 Trieste, Italy. [Viel, M.] Natl Inst Nucl Phys, I-34127 Trieste, Italy. [Weinberg, D. H.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. [York, D. G.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60615 USA. [York, D. G.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60615 USA. [Font-Ribera, A.] Univ Zurich, Inst Theoret Phys, CH-8057 Zurich, Switzerland. [Paris, I.] Univ Chile, Dept Astron, Santiago, Chile. RP Busca, NG (reprint author), Univ Paris 07, CNRS, IN2P3, APC,CEA,Observ Paris, 10 Rue A Domon & L Duquet, Paris, France. EM ngbusca@apc.univ-paris7.fr RI Ho, Shirley/P-3682-2014; White, Martin/I-3880-2015; Croft, Rupert/N-8707-2014; OI Ho, Shirley/0000-0002-1068-160X; White, Martin/0000-0001-9912-5070; Croft, Rupert/0000-0003-0697-2583; Miralda-Escude, Jordi/0000-0002-2316-8370; Viel, Matteo/0000-0002-2642-5707 FU Alfred P. Sloan Foundation; National Science Foundation; US Department of Energy Office of Science; Agence Nationale de la Recherche [ANR-08-BLAN-0222]; European Union Seventh Framework Programme (FP7) [PIIF-GA-2011-301665]; University of Arizona; Brazilian Participation Group; Brookhaven National Laboratory; University of Cambridge; Carnegie Mellon University; University of Florida; French Participation Group; German Participation Group; Harvard University; Instituto de Astrofisica de Canarias; Michigan State/Notre Dame/JINA Participation Group; Johns Hopkins University; Lawrence Berkeley National Laboratory; Max Planck Institute for Astrophysics; Max Planck Institute for Extraterrestrial Physics; New Mexico State University; New York University; Ohio State University; Pennsylvania State University; University of Portsmouth; Princeton University; Spanish Participation Group; University of Tokyo; University of Utah; Vanderbilt University; University of Virginia; University of Washington; Yale University FX We thank Carlos Allende Prieto, Ashley Ross and Uros Seljak for stimulating discussions and Adam Riess for providing the data points of Riess et al. (2007) in Fig. 21. Funding for SDSS-III has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, and the US Department of Energy Office of Science. The SDSS-III web site is http://www.sdss3.org/. The French Participation Group of SDSS-III was supported by the Agence Nationale de la Recherche under contract ANR-08-BLAN-0222. The research leading to these results has received funding from the European Union Seventh Framework Programme (FP7/2007-2013) under grant agreement No. PIIF-GA-2011-301665. SDSS-III is managed by the Astrophysical Research Consortium for the Participating Institutions of the SDSS-III Collaboration including the University of Arizona, the Brazilian Participation Group, Brookhaven National Laboratory, University of Cambridge, Carnegie Mellon University, University of Florida, the French Participation Group, the German Participation Group, Harvard University, the Instituto de Astrofisica de Canarias, the Michigan State/Notre Dame/JINA Participation Group, Johns Hopkins University, Lawrence Berkeley National Laboratory, Max Planck Institute for Astrophysics, Max Planck Institute for Extraterrestrial Physics, New Mexico State University, New York University, Ohio State University, Pennsylvania State University, University of Portsmouth, Princeton University, the Spanish Participation Group, University of Tokyo, University of Utah, Vanderbilt University, University of Virginia, University of Washington, and Yale University. NR 100 TC 157 Z9 158 U1 2 U2 14 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD APR PY 2013 VL 552 AR A96 DI 10.1051/0004-6361/201220724 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 130JW UT WOS:000317912000096 ER PT J AU Deller, AT Forbrich, J Loinard, L AF Deller, A. T. Forbrich, J. Loinard, L. TI A very long baseline interferometry detection of the class I protostar IRS5 in Corona Australis SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE stars: protostars; radio continuum: stars; astrometry; techniques: high angular resolution ID YOUNG STELLAR OBJECTS; POLARIZED RADIO-EMISSION; STAR-FORMING REGION; T-TAURI SYSTEM; X-RAY; VLBA DETERMINATION; DISTANCE; CLOUD; CLUSTER; SOUTH AB Aims. Very long baseline interferometry yields physical constraints on the compact radio emission of young stellar objects. At the same time, such measurements can be used for precise astrometric measurements of parallaxes and proper motions. Here, we aimed to make the first detections of very compact radio emission from class I protostars in the Corona Australis star-forming region. Methods. We have used the Long Baseline Array (LBA) to observe the protostars IRS 5 and IRS 7 in the Corona Australis star-forming region in three separate epochs. Results. We report the first firm radio detection of a class I protostar using very long baseline interferometry. We have detected the previously known non-thermal source IRS 5b, part of a binary system. IRS 5a and IRS 5N were undetected, as were all sources in the IRS 7 region. Conclusions. These results underline the unusual nature of IRS 5b as a genuine protostar with confirmed non-thermal radio emission. Also, these observations highlight the potential of the LBA as a tool to provide precision astrometric measurements of individual young stellar objects in southern star-forming regions that are not accessible to the Very Long Baseline Array in the northern hemisphere. C1 [Deller, A. T.] Netherlands Inst Radio Astron ASTRON, NL-7990 AA Dwingeloo, Netherlands. [Forbrich, J.] Univ Vienna, Dept Astrophys, A-1180 Vienna, Austria. [Forbrich, J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Loinard, L.] Univ Nacl Autonoma Mexico, Ctr Radiostron & Astrofis, Morelia 58089, Michoacan, Mexico. [Loinard, L.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. RP Deller, AT (reprint author), Netherlands Inst Radio Astron ASTRON, NL-7990 AA Dwingeloo, Netherlands. EM deller@astron.nl OI Deller, Adam/0000-0001-9434-3837 FU Commonwealth of Australia; NWO Veni Fellowship; Austrian Science Fund; DGAPA; UNAM; CONACyT (Mexico); Alexander von Humboldt Stiftung FX The Long Baseline Array is part of the Australia Telescope National Facility which is funded by the Commonwealth of Australia for operation as a National Facility managed by CSIRO. A.T.D. was supported by an NWO Veni Fellowship. This publication is supported by the Austrian Science Fund (FWF). L.L. acknowledges the financial support of DGAPA, UNAM, CONACyT (Mexico), and the Alexander von Humboldt Stiftung. NR 40 TC 7 Z9 7 U1 0 U2 0 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD APR PY 2013 VL 552 AR A51 DI 10.1051/0004-6361/201321085 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 130JW UT WOS:000317912000051 ER PT J AU Gallenne, A Monnier, JD Merand, A Kervella, P Kraus, S Schaefer, GH Gieren, W Pietrzynski, G Szabados, L Che, X Baron, F Pedretti, E McAlister, H ten Brummelaar, T Sturmann, J Sturmann, L Turner, N Farrington, C Vargas, N AF Gallenne, A. Monnier, J. D. Merand, A. Kervella, P. Kraus, S. Schaefer, G. H. Gieren, W. Pietrzynski, G. Szabados, L. Che, X. Baron, F. Pedretti, E. McAlister, H. ten Brummelaar, T. Sturmann, J. Sturmann, L. Turner, N. Farrington, C. Vargas, N. TI Multiplicity of Galactic Cepheids from long-baseline interferometry I. CHARA/MIRC detection of the companion of V1334 Cygni SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE techniques: interferometric; instrumentation: high angular resolution; stars: variables: Cepheids; binaries: close ID SURFACE BRIGHTNESS RELATIONS; PERIOD-LUMINOSITY RELATION; VIRTUAL OBSERVATORY TOOL; CLASSICAL CEPHEIDS; DISTANCE SCALE; SPECKLE INTERFEROMETRY; SEARCHING CALIBRATORS; MASS DISCREPANCY; VARIABLE-STAR; PULSATION AB Context. More than 60% of Cepheids are in binary or multiple systems. Studying such systems could lead to a better understanding of the age and evolution of Cepheids. These are also useful tools to estimate the mass of Cepheids, and constrain theoretical models of their pulsation and evolution. Aims. We aim at determining the masses of Cepheids in binary systems, as well as their geometric distances and the flux contribution of the companions. The combination of interferometry with spectroscopy will off er a unique and independent estimate of the Cepheid masses. Methods. Using long-baseline interferometry at visible and infrared wavelengths, it is possible to spatially resolve binary systems containing a Cepheid down to milliarcsecond separations. Based on the resulting visual orbit and radial velocities, we can then derive the fundamental parameters of these systems, particularly the masses of the components and the geometric distance. We therefore performed interferometric observations of the first-overtone mode Cepheid V1334 Cyg with the CHARA/MIRC combiner. Results. We report the first detection of a Cepheid companion using long-baseline interferometry. We detect the signature of a companion orbiting V1334 Cyg at two epochs. We measure a flux ratio between the companion and the Cepheid f = 3.10 +/- 0.08%, giving an apparent magnitude m(H) = 8.47 +/- 0.15 mag. The combination of interferometric and spectroscopic data have enabled the unique determination of the orbital elements. P = 1938..6 +/- 1.2 days, T-p = 2 443 616.1 +/- 7.3, a = 8.54 +/- 0.51 mas, i = 124.7 +/- 1.8 degrees, e = 0.190 +/- 0.013, omega = 228.7 +/- 1.6 degrees, and Omega = 206.3 +/- 9.4 degrees. We derive a minimal distance d similar to 691 pc, a minimum mass for both stars of 3.6 M-circle dot, with a spectral type earlier than B5.5V for the companion star. Our measured flux ratio suggests that radial velocity detection of the companion using spectroscopy is within reach, and would provide an orbital parallax and model-free masses. C1 [Gallenne, A.; Gieren, W.; Pietrzynski, G.] Univ Concepcion, Dept Astron, Concepcion, Chile. [Monnier, J. D.; Che, X.; Baron, F.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Merand, A.] European So Observ, Santiago 19, Chile. [Kervella, P.] Univ Paris Diderot, UPMC, CNRS UMR 8109, LESIA,Observ Paris, F-92195 Meudon, France. [Kraus, S.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Schaefer, G. H.; McAlister, H.; ten Brummelaar, T.; Sturmann, J.; Sturmann, L.; Turner, N.; Farrington, C.; Vargas, N.] Georgia State Univ, CHARA Array, Mt Wilson, CA 91023 USA. [Szabados, L.] Hungarian Acad Sci, Konkoly Observ, Res Ctr Astron & Earth Sci, H-1121 Budapest, Hungary. [Pedretti, E.] Univ St Andrews, Sch Phys & Astron, St Andrews KY16 9SS, Fife, Scotland. [Pietrzynski, G.] Univ Warsaw Observ, PL-00478 Warsaw, Poland. RP Gallenne, A (reprint author), Univ Concepcion, Dept Astron, Casilla 160, Concepcion, Chile. EM agallenne@astro-udec.cl FU National Science Foundation [AST-0908253]; Georgia State University; W. M. Keck Foundation; Packard Foundation; NASA Exoplanet Science Institute; NSF [AST-0707927, AST-0807577]; BASAL Centro de Astrofisica y Tecnologias Afines (CATA) [PFB-06/2007]; Polish National Science Centre grant MAESTRO; Polish Ministry of Science grant Ideas Plus; ONERA; Observatoire de Paris; CNRS; University Denis Diderot Paris 7; FONDECYT [3130361]; ESTEC [4000106398/12/NL/KML] FX The authors would like to thank the CHARA Array and Mount Wilson Observatory staff for their support. Research conducted at the CHARA Array is funded by the National Science Foundation through NSF grant AST-0908253, by Georgia State University, the W. M. Keck Foundation, the Packard Foundation, and the NASA Exoplanet Science Institute. J.D.M. acknowledges funding from the NSF grants AST-0707927 and AST-0807577. W. G. and G. P. gratefully acknowledge financial support for this work from the BASAL Centro de Astrofisica y Tecnologias Afines (CATA) PFB-06/2007. Support from the Polish National Science Centre grant MAESTRO and the Polish Ministry of Science grant Ideas Plus (awarded to G. P.) is also acknowledge. This research received the support of PHASE, the high angular resolution partnership between ONERA, Observatoire de Paris, CNRS, and University Denis Diderot Paris 7. A. G. acknowledges support from FONDECYT grant 3130361. LSz has been supported by the ESTEC Contract No. 4000106398/12/NL/KML. This work made use of the SIMBAD and VIZIER astrophysical database from CDS, Strasbourg, France and the bibliographic informations from the NASA Astrophysics Data System. This research has made use of the Jean-Marie Mariotti Center LITpro service, co-developed by CRAL, LAOG and FIZEAU, and SearchCal service, co-developed by FIZEAU and LAOG/IPAG, and of CDS Astronomical Databases SIMBAD and VIZIER. NR 54 TC 12 Z9 12 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 APR PY 2013 VL 552 AR A21 DI 10.1051/0004-6361/201321091 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 130JW UT WOS:000317912000021 ER PT J AU Gunther, HM Schneider, PC Li, ZY AF Guenther, H. M. Schneider, P. C. Li, Z. -Y. TI The evolution of the jet from Herbig Ae star HD 163296 from 1999 to 2011 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE circumstellar matter; stars: formation; stars: pre-main sequence; X-rays: stars; stars: individual: HD 163296 ID T-TAURI STARS; X-RAY JET; HUBBLE-SPACE-TELESCOPE; DG-TAURI; EMISSION-LINES; YOUNG STARS; MASS-LOSS; MAGNETIC-FIELDS; ACCRETION DISKS; ATOMIC DATABASE AB Young A and B stars, the so-called Herbig Ae/Be stars (HAeBe), are surrounded by active accretion disks and drive outflows. We study the jet HH 409, which is launched from the HAeBe star HD 163296, using new and archival observations from Chandra and HST/STIS. In X-rays we can show that the central source is not significantly extended. The approaching jet, but not the counterjet, is detected in Ly alpha. In addition, there is red-shifted Ly alpha emission extended in the same direction as the jet, which is also absent in the counterjet. We can rule out an accretion or disk-wind origin for this feature. In the optical we find the knots B and B2 in the counterjet. Knot B has been observed previously, so we can derive its proper motion of (0.37 +/- 0.01)'' yr(-1). Its electron density is 3000 cm(-3), thus the cooling time scale is only a few months, so the knot needs to be reheated continuously. The shock speed derived from models of H alpha and forbidden emission lines decreased from 50 km s(-1) in 1999 to 30 km s(-1) in 2011 because the shock front loses energy as it travels along the jet. Knot B2 is observed at a similar position in 2011 to where knot B was in 1999, but shows a lower ionization fraction and higher mass loss rate, proving that there are variations in the jet launching conditions. C1 [Guenther, H. M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Schneider, P. C.] Univ Hamburg, Hamburger Sternwarte, D-21029 Hamburg, Germany. [Li, Z. -Y.] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA. RP Gunther, HM (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM hguenther@cfa.harvard.edu OI Gunther, Hans Moritz/0000-0003-4243-2840 FU National Aeronautics and Space Administration (NASA) [GO2-13015X, TM0-11002X]; NASA [NAS8-03060, NAS5-26555]; Space Telescope Science Institute [GO-12186.01-A]; DLR [50 OR 1112] FX Support for this work was provided by the National Aeronautics and Space Administration (NASA) through Chandra Awards Number GO2-13015X and TM0-11002X 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. Further support comes from grant GO-12186.01-A from the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555. P. C. S. acknowledges support from the DLR under 50 OR 1112. Some of the data presented in this paper were obtained from the Mikulski Archive for Space Telescopes (MAST). NR 55 TC 6 Z9 6 U1 0 U2 0 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD APR PY 2013 VL 552 AR A142 DI 10.1051/0004-6361/201220772 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 130JW UT WOS:000317912000141 ER PT J AU Hassall, TE Stappers, BW Weltevrede, P Hessels, JWT Alexov, A Coenen, T Karastergiou, A Kramer, M Keane, EF Kondratiev, VI van Leeuwen, J Noutsos, A Pilia, M Serylak, M Sobey, C Zagkouris, K Fender, R Bell, ME Broderick, J Eisloffel, J Falcke, H Griessmeier, JM Kuniyoshi, M Miller-Jones, JCA Wise, MW Wucknitz, O Zarka, P Asgekar, A Batejat, F Bentum, MJ Bernardi, G Best, P Bonafede, A Breitling, F Bruggen, M Butcher, HR Ciardi, B de Gasperin, F de Reijer, JP Duscha, S Fallows, RA Ferrari, C Frieswijk, W Garrett, MA Gunst, AW Heald, G Hoeft, M Juette, E Maat, P McKean, JP Norden, MJ Pandey-Pommier, M Pizzo, R Polatidis, AG Reich, W Rottgering, H Sluman, J Tang, Y Tasse, C Vermeulen, R van Weeren, RJ Wijnholds, SJ Yatawatta, S AF Hassall, T. E. Stappers, B. W. Weltevrede, P. Hessels, J. W. T. Alexov, A. Coenen, T. Karastergiou, A. Kramer, M. Keane, E. F. Kondratiev, V. I. van Leeuwen, J. Noutsos, A. Pilia, M. Serylak, M. Sobey, C. Zagkouris, K. Fender, R. Bell, M. E. Broderick, J. Eisloeffel, J. Falcke, H. Griessmeier, J. -M. Kuniyoshi, M. Miller-Jones, J. C. A. Wise, M. W. Wucknitz, O. Zarka, P. Asgekar, A. Batejat, F. Bentum, M. J. Bernardi, G. Best, P. Bonafede, A. Breitling, F. Brueggen, M. Butcher, H. R. Ciardi, B. de Gasperin, F. de Reijer, J. -P. Duscha, S. Fallows, R. A. Ferrari, C. Frieswijk, W. Garrett, M. A. Gunst, A. W. Heald, G. Hoeft, M. Juette, E. Maat, P. McKean, J. P. Norden, M. J. Pandey-Pommier, M. Pizzo, R. Polatidis, A. G. Reich, W. Rottgering, H. Sluman, J. Tang, Y. Tasse, C. Vermeulen, R. van Weeren, R. J. Wijnholds, S. J. Yatawatta, S. TI Differential frequency-dependent delay from the pulsar magnetosphere SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE pulsars: general; pulsars: individual: PSR B0809+74; telescopes ID RADIO PULSARS; DRIFTING SUBPULSES; PSR B0809+74; EMISSION; MODEL; POLARIZATION; TELESCOPE; STABILITY; RADIATION; PROFILES AB Some radio pulsars show clear "drifting subpulses", in which subpulses are seen to drift in pulse longitude in a systematic pattern. Here we examine how the drifting subpulses of PSR B0809+74 evolve with time and observing frequency. We show that the subpulse period (P-3) is constant on timescales of days, months and years, and between 14-5100 MHz. Despite this, the shapes of the driftbands change radically with frequency. Previous studies have concluded that, while the subpulses appear to move through the pulse window approximately linearly at low frequencies (<500 MHz), a discrete step of similar to 180 degrees in subpulse phase is observed at higher frequencies (>820 MHz) near to the peak of the average pulse profile. We use LOFAR, GMRT, GBT, WSRT and Effelsberg 100-m data to explore the frequency-dependence of this phase step. We show that the size of the subpulse phase step increases gradually, and is observable even at low frequencies. We attribute the subpulse phase step to the presence of two separate driftbands, whose relative arrival times vary with frequency - one driftband arriving 30 pulses earlier at 20 MHz than it does at 1380 MHz, whilst the other arrives simultaneously at all frequencies. The drifting pattern which is observed here cannot be explained by either the rotating carousel model or the surface oscillation model, and could provide new insight into the physical processes happening within the pulsar magnetosphere. C1 [Hassall, T. E.; Fender, R.; Bell, M. E.; Broderick, J.] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England. [Stappers, B. W.; Weltevrede, P.; Kramer, M.] Univ Manchester, Sch Phys & Astron, Jodrell Bank Ctr Astrophys, Manchester M13 9PL, Lancs, England. [Hessels, J. W. T.; Kondratiev, V. I.; van Leeuwen, J.; Pilia, M.; Falcke, H.; Wise, M. W.; Asgekar, A.; Bentum, M. J.; Butcher, H. R.; de Reijer, J. -P.; Duscha, S.; Fallows, R. A.; Frieswijk, W.; Garrett, M. A.; Gunst, A. W.; Heald, G.; Maat, P.; McKean, J. P.; Norden, M. J.; Pizzo, R.; Polatidis, A. G.; Sluman, J.; Tang, Y.; van Weeren, R. J.; Wijnholds, S. J.; Yatawatta, S.] Netherlands Inst Radio Astron ASTRON, NL-7990 AA Dwingeloo, Netherlands. [Hessels, J. W. T.; Alexov, A.; Coenen, T.; van Leeuwen, J.; Miller-Jones, J. C. A.; Wise, M. W.] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1090 GE Amsterdam, Netherlands. [Alexov, A.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Karastergiou, A.; Zagkouris, K.] Univ Oxford, Oxford OX1 3RH, England. [Kramer, M.; Keane, E. F.; Noutsos, A.; Sobey, C.; Kuniyoshi, M.; Wucknitz, O.; Reich, W.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Serylak, M.; Griessmeier, J. -M.] CNRS INSU, Observ Paris, Stn Radioastron Nancay, F-18330 Nancay, France. [Serylak, M.; Griessmeier, J. -M.] CNRS, UMR 7328, LPC2E, Lab Phys & Chim Environm & Espace, F-45071 Orleans 02, France. [Bell, M. E.] Univ Sydney, Sydney Inst Astron, ARC Ctr Excellence All Sky Astrophys CAASTRO, Sydney, NSW 2016, Australia. [Eisloeffel, J.; Hoeft, M.] Thuringer Landessternwarte, D-07778 Tautenburg, Germany. [Falcke, H.] Radboud Univ Nijmegen, IMAPP, Dept Astrophys, NL-6500 GL Nijmegen, Netherlands. [Miller-Jones, J. C. A.] Curtin Univ Technol, Int Ctr Radio Astron Res, Perth, WA 6845, Australia. [Wucknitz, O.] Univ Bonn, Argelander Inst Astron, D-53121 Bonn, Germany. [Zarka, P.; Tasse, C.] Observ Paris, CNRS, UMR 8109, LESIA, F-92195 Meudon, France. [Batejat, F.] Chalmers, Dept Earth & Space Sci, Onsala Space Observ, S-43992 Onsala, Sweden. [Bernardi, G.] Univ Groningen, Kapteyn Astron Inst, NL-9700 AV Groningen, Netherlands. [Best, P.] Univ Edinburgh, Royal Observ Edinburgh, Inst Astron, Edinburgh EH9 3HJ, Midlothian, Scotland. [Bonafede, A.; Brueggen, M.; de Gasperin, F.] Univ Hamburg, D-21029 Hamburg, Germany. [Bonafede, A.] Jacobs Univ Bremen, D-28759 Bremen, Germany. [Breitling, F.] Leibniz Inst Astrophys Potsdam AIP, D-14482 Potsdam, Germany. [Butcher, H. R.] Australian Natl Univ, Res Sch Astron & Astrophys, Weston, ACT 2611, Australia. [Ciardi, B.; de Gasperin, F.] Max Planck Inst Astrophys, D-85741 Garching, Germany. [Ferrari, C.] Univ Nice Sophia Antipolis, Observ Cote Azur, Lab Lagrange, CNRS,UMR7293, F-06300 Nice, France. [Garrett, M. A.; Pandey-Pommier, M.; Rottgering, H.; van Weeren, R. J.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [Juette, E.] Ruhr Univ Bochum, Astron Inst, D-44780 Bochum, Germany. [Pandey-Pommier, M.] Observ Lyon, Ctr Rech Astrophys Lyon, F-69561 St Genis Laval, France. [van Weeren, R. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Hassall, TE (reprint author), Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England. EM tomehassall@gmail.com RI Miller-Jones, James/B-2411-2013; Ciardi, Benedetta/N-7625-2015; Kondratiev, Vladislav/N-1105-2015; Falcke, Heino/H-5262-2012; Yatawatta, Sarod/E-6037-2013; OI Miller-Jones, James/0000-0003-3124-2814; Kondratiev, Vladislav/0000-0001-8864-7471; Falcke, Heino/0000-0002-2526-6724; Yatawatta, Sarod/0000-0001-5619-4017; de Gasperin, Francesco/0000-0003-4439-2627; van Weeren, Reinout/0000-0002-0587-1660 FU European Research Council [267697]; STFC; Netherlands Research School for Astronomy [NOVA3- NW3-2.3.1]; European Commission [FP7- PEOPLE-2007-4-3-IRG, 224838]; Leverhulme Trust; DFG (German Research Foundation), Magnetisation of Interstellar and Intergalactic Media [FOR 1254]; Agence Nationale de la Recherche [ANR-09-JCJC-0001-01]; Netherlands Foundation for Scientific Research NWO FX The authors would like to thank Axel Jessner, Rachel Rosen, Paul Demorest, Vishal Gajjar and Balchandra Joshi for sharing data with us, and Geoff Wright for his insight and helpful discussions. T. E. H. is funded by European Research Council Advanced Grant 267697 "4 Pi Sky: Extreme Astrophysics with Revolutionary Radio Telescopes". B. W. S. and P. W. are supported through an STFC rolling grant. J.W.T.H. is a Veni Fellow of the Netherlands Foundation for Scientific Research. J.v.L. and T. C. are supported by the Netherlands Research School for Astronomy (Grant NOVA3- NW3-2.3.1) and by the European Commission (Grant FP7- PEOPLE-2007-4-3-IRG #224838). A. K. is grateful to the Leverhulme Trust for financial support. C. S. is supported by the DFG (German Research Foundation) within the framework of the Research Unit FOR 1254, Magnetisation of Interstellar and Intergalactic Media: The Prospects of Low-Frequency Radio Observations. C. F. acknowledges financial support by the Agence Nationale de la Recherche through grant ANR-09-JCJC-0001-01. LOFAR, the Low Frequency Array designed and constructed by ASTRON, has facilities in several countries, that are owned by various parties (each with their own funding sources), and that are collectively operated by the International LOFAR Telescope (ILT) foundation under a joint scientific policy. This publication made use of observations taken with the 100-m telescope of the MPIfR (Max-Planck-Institut fur Radioastronomie) at Effelsberg. The Westerbork Synthesis Radio Telescope is operated by the ASTRON (Netherlands Foundation for Research in Astronomy) with support from the Netherlands Foundation for Scientific Research NWO. 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 NASA's Astrophysics Data System Bibliographic Services. NR 43 TC 6 Z9 6 U1 1 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 EI 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD APR PY 2013 VL 552 AR A61 DI 10.1051/0004-6361/201220764 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 130JW UT WOS:000317912000061 ER PT J AU Rani, B Krichbaum, TP Fuhrmann, L Bottcher, M Lott, B Aller, HD Aller, MF Angelakis, E Bach, U Bastieri, D Falcone, AD Fukazawa, Y Gabanyi, KE Gupta, AC Gurwell, M Itoh, R Kawabata, KS Krips, M Lahteenmaki, AA Liu, X Marchili, N Max-Moerbeck, W Nestoras, I Nieppola, E Quintana-Lacaci, G Readhead, ACS Richards, JL Sasada, M Sievers, A Sokolovsky, K Stroh, M Tammi, J Tornikoski, M Uemura, M Ungerechts, H Urano, T Zensus, JA AF Rani, B. Krichbaum, T. P. Fuhrmann, L. Boettcher, M. Lott, B. Aller, H. D. Aller, M. F. Angelakis, E. Bach, U. Bastieri, D. Falcone, A. D. Fukazawa, Y. Gabanyi, K. E. Gupta, A. C. Gurwell, M. Itoh, R. Kawabata, K. S. Krips, M. Lahteenmaki, A. A. Liu, X. Marchili, N. Max-Moerbeck, W. Nestoras, I. Nieppola, E. Quintana-Lacaci, G. Readhead, A. C. S. Richards, J. L. Sasada, M. Sievers, A. Sokolovsky, K. Stroh, M. Tammi, J. Tornikoski, M. Uemura, M. Ungerechts, H. Urano, T. Zensus, J. A. TI Radio to gamma-ray variability study of blazar S5 0716+714 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE galaxies: active; BL Lacertae objects: individual: S5 0716+714; gamma rays: galaxies; X-rays: galaxies; radio continuum: galaxies ID BL LACERTAE OBJECTS; INVERSE-COMPTON CATASTROPHE; ACTIVE GALACTIC NUCLEI; ENERGY PEAKED BLAZARS; LARGE-AREA TELESCOPE; X-RAY; INTRADAY VARIABILITY; LIGHT CURVES; ELECTROMAGNETIC-SPECTRUM; EXTRAGALACTIC SOURCES AB We present the results of a series of radio, optical, X-ray, and gamma-ray observations of the BL Lac object S50716+714 carried out between April 2007 and January 2011. The multifrequency observations were obtained using several ground-and space-based facilities. The intense optical monitoring of the source reveals faster repetitive variations superimposed on a long-term variability trend on a time scale of similar to 350 days. Episodes of fast variability recur on time scales of similar to 60-70 days. The intense and simultaneous activity at optical and gamma-ray frequencies favors the synchrotron self-Compton mechanism for the production of the high-energy emission. Two major low-peaking radio flares were observed during this high optical/gamma-ray activity period. The radio flares are characterized by a rising and a decaying stage and agrees with the formation of a shock and its evolution. We found that the evolution of the radio flares requires a geometrical variation in addition to intrinsic variations of the source. Different estimates yield robust and self-consistent lower limits of delta >= 20 and equipartition magnetic field B-eq >= 0.36 G. Causality arguments constrain the size of emission region theta <= 0.004 mas. We found a significant correlation between flux variations at radio frequencies with those at optical and gamma-rays. The optical/GeV flux variations lead the radio variability by similar to 65 days. The longer time delays between low-peaking radio outbursts and optical flares imply that optical flares are the precursors of radio ones. An orphan X-ray flare challenges the simple, one-zone emission models, rendering them too simple. Here we also describe the spectral energy distribution modeling of the source from simultaneous data taken through different activity periods. C1 [Rani, B.; Krichbaum, T. P.; Fuhrmann, L.; Angelakis, E.; Bach, U.; Marchili, N.; Nestoras, I.; Sokolovsky, K.; Zensus, J. A.] MPIfR, D-53121 Bonn, Germany. [Boettcher, M.] Ohio Univ, Dept Phys & Astron, Inst Astrophys, Athens, OH 45701 USA. [Boettcher, M.] North West Univ, Ctr Space Res, ZA-2531 Potchefstroom, South Africa. [Lott, B.] Univ Bordeaux 1, CNRS IN2p3, Ctr Etud Nucl Bordeaux Gradignan, F-33175 Gradignan, France. [Aller, H. D.; Aller, M. F.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Bastieri, D.] Ist Nazl Fis Nucl, Sez Padova, I-35131 Padua, Italy. [Bastieri, D.; Marchili, N.] Univ Padua, Dipartimento Fis & Astron, I-35131 Padua, Italy. [Falcone, A. D.; Stroh, M.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Fukazawa, Y.; Itoh, R.; Urano, T.] Hiroshima Univ, Dept Phys Sci, Hiroshima 7398526, Japan. [Gabanyi, K. E.] FOMI Satellite Geodet Observ, H-1592 Budapest, Hungary. [Gabanyi, K. E.] Hungarian Acad Sci, Konkoly Observ, Res Ctr Astron & Earth Sci, H-1121 Budapest, Hungary. [Gupta, A. C.] Aryabhatta Res Inst Observat Sci ARIES, Manora Peak 263129, Nainital, India. [Gurwell, M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Kawabata, K. S.; Sasada, M.; Uemura, M.] Hiroshima Univ, Hiroshima Astrophys Sci Ctr, Hiroshima 7398526, Japan. [Krips, M.] IRAM, F-38406 St Martin Dheres, France. [Lahteenmaki, A. A.; Nieppola, E.; Tammi, J.; Tornikoski, M.] Aalto Univ, Metsahovi Radio Observ, Kylmala, Finland. [Liu, X.] Chinese Acad Sci, Xinjiang Astron Observ, Urumqi 830011, Peoples R China. [Max-Moerbeck, W.; Readhead, A. C. S.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA. [Quintana-Lacaci, G.; Sievers, A.; Ungerechts, H.] Inst Radioastron Milimetr IRAM, Granada 18012, Spain. [Quintana-Lacaci, G.] INTA CSIC, CAB, Madrid 28850, Spain. [Richards, J. L.] Purdue Univ, Dept Phys, W Lafayette, IN 47907 USA. [Sasada, M.] Kyoto Univ, Dept Astron, Sakyo Ku, Kyoto 6068502, Japan. [Sokolovsky, K.] PN Lebedev Phys Inst, Ctr Astro Space, Moscow 117997, Russia. RP Rani, B (reprint author), MPIfR, Hugel 69, D-53121 Bonn, Germany. EM brani@mpifr-bonn.mpg.de RI Sokolovsky, Kirill/D-2246-2015; Lahteenmaki, Anne/L-5987-2013; OI Sokolovsky, Kirill/0000-0001-5991-6863; Sasada, Mahito/0000-0001-5946-9960; Bastieri, Denis/0000-0002-6954-8862; Angelakis, Emmanouil/0000-0001-7327-5441; Quintana-Lacaci, Guillermo/0000-0002-5417-1943 FU Fermi/LAT Collaboration; National Aeronautics and Space Administration; Department of Energy in the United States; Commissariat a l'Energie Atomique; Centre National de la Recherche Scientifique/Institut National de Physique Nucleaire et de Physique des Particules in France; Agenzia Spaziale Italiana; Istituto Nazionale di Fisica Nucleare in Italy; Ministry of Education, Culture, Sports, Science and Technology (MEXT); High Energy Accelerator Research Organization (KEK); Japan Aerospace Exploration Agency (JAXA) in Japan; K.A. Wallenberg Foundation; Swedish Research Council; Swedish National Space Board in Sweden; INSU/CNRS (France); MPG (Germany); IGN (Spain); Smithsonian Institution; Academia Sinica; International Max Planck Research School (IMPRS) for Astronomy and Astrophysics at the University of Bonn; International Max Planck Research School (IMPRS) for Astronomy and Astrophysics at the University of Cologne; ASI [I/005/11/0]; NASA [NNX10AU14G]; National Natural Science Foundation of China [11273050]; NSF; NASA; University of Michigan; "Consejeria de Economia, Innovacion y Ciencia" of the Regional Government of Andalucia [P09-FQM-4784]; "Ministerio de Economia y Competitividad" of Spain [AYA2010-14844]; Academy of Finland [212656, 210338, 121148] FX The Fermi/LAT Collaboration acknowledges the generous support of a number of agencies and institutes that have supported the Fermi/LAT Collaboration. These include the National Aeronautics and Space Administration and the Department of Energy in the United States, the Commissariat a l'Energie Atomique and the Centre National de la Recherche Scientifique/Institut National de Physique Nucleaire et de Physique des Particules in France, the Agenzia Spaziale Italiana and the Istituto Nazionale di Fisica Nucleare in Italy, the Ministry of Education, Culture, Sports, Science and Technology (MEXT), High Energy Accelerator Research Organization (KEK) and Japan Aerospace Exploration Agency (JAXA) in Japan, and the K.A. Wallenberg Foundation, the Swedish Research Council and the Swedish National Space Board in Sweden. This research is partly based on observations with the 100-m telescope of the MPIfR (Max-Planck-Institut fur Radioastronomie) at Effelsberg. This work has made use of observations with the IRAM 30-m telescope. IRAM is supported by INSU/CNRS (France), MPG (Germany) and IGN (Spain). 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. The observations made use of the Noto telescope operated by INAF - Istituto di Radioastronomia. B. R. gratefully acknowledges the travel support the COSPAR Capacity-Building Workshop fellowship program. I.N. was supported for this research through a stipend from the International Max Planck Research School (IMPRS) for Astronomy and Astrophysics at the Universities of Bonn and Cologne. N.M. is funded by an ASI fellowship under contract number I/005/11/0. We also acknowledge the Swift Team and the Swift/XRT monitoring program efforts, as well as analysis supported by NASA Fermi GI grants NNX10AU14G. L. X. is supported by the National Natural Science Foundation of China (No. 11273050). Work at UMRAO has been supported by a series of grants from the NSF and from NASA. Support for operation of the observatory was provided by the University of Michigan. I. A. acknowledges funding by the "Consejeria de Economia, Innovacion y Ciencia" of the Regional Government of Andalucia through grant P09-FQM-4784, an by the "Ministerio de Economia y Competitividad" of Spain through grant AYA2010-14844. The Metsahovi team acknowledges the support from the Academy of Finland to our observing projects (numbers 212656, 210338, 121148, and others). We thank Ivan Agudo for his contribution at the 30 m telescope and for discussion. We would like to thank Marcello Giroletti, the internal referee from Fermi/LAT team for his useful suggestions and comments. We thank the referee for several helpful suggestions. We would also like to thank Jeff Hodgson for the help in finalizing the text. NR 87 TC 24 Z9 25 U1 1 U2 15 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 EI 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD APR PY 2013 VL 552 AR A11 DI 10.1051/0004-6361/201321058 PG 24 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 130JW UT WOS:000317912000011 ER PT J AU Sasaki, M Plucinsky, PP Gaetz, TJ Bocchino, F AF Sasaki, M. Plucinsky, P. P. Gaetz, T. J. Bocchino, F. TI Chandra observation of the Galactic supernova remnant CTB 109 (G109.1-1.0) SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE shock waves; ISM: supernova remnants; X-rays: ISM; X-rays: individuals: SNR CTB 109 ID LARGE-MAGELLANIC-CLOUD; X-RAY PULSAR; CTB-109 G109.1-1.0; EJECTA; DISTANCE AB Context. We study the X-ray emission of the Galactic supernova remnant (SNR) CTB 109 (G109.1-1.0), which is well-known for its enigmatic half-shell morphology both in radio and in X-rays and is associated with the anomalous X-ray pulsar (AXP) 1E 2259+586. Aims. We want to understand the origin of the X-ray bright feature inside the SNR called the Lobe and the details of the interaction of the SNR shock wave with the ambient interstellar medium (ISM). Methods. The Lobe and the northeastern part of the SNR were observed with Chandra ACIS-I. We analysed the spectrum of the X-ray emission by dividing the entire observed emission into small regions. The X-ray emission is best reproduced with one-component or two-component non-equilibrium ionisation models depending on the position. In the two-component model, one emission component represents the shocked ISM and the other the shocked ejecta. Results. We detect enhanced element abundances, in particular for Si and Fe, in and around the Lobe. There is one particular region next to the Lobe with a high Si abundance of 3.3 (2.6-4.0) times the solar value. This is the first, unequivocal detection of ejecta in CTB 109. Conclusions. The new Chandra data confirm that the Lobe was created by the interaction of the SNR shock and the supernova ejecta with a dense and inhomogeneous medium in the environment of SNR CTB 109. The newly calculated age of the SNR is t approximate to 1.4 x 10(4) yr. C1 [Sasaki, M.] Univ Tubingen, Inst Astron & Astrophys, D-72076 Tubingen, Germany. [Plucinsky, P. P.; Gaetz, T. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Bocchino, F.] INAF Osservatorio Astron Palermo, I-90134 Palermo, Italy. RP Sasaki, M (reprint author), Univ Tubingen, Inst Astron & Astrophys, Sand 1, D-72076 Tubingen, Germany. EM sasaki@astro.uni-tuebingen.de RI Sasaki, Manami/P-3045-2016; OI Sasaki, Manami/0000-0001-5302-1866; Bocchino, Fabrizio/0000-0002-2321-5616 FU Deutsche Forschungsgemeinschaft through the Emmy Noether Research Grant [2131/1]; NASA [NAS8-03060] FX M.S. acknowledges support by the Deutsche Forschungsgemeinschaft through the Emmy Noether Research Grant SA 2131/1. P.P.P. and T.J.G. acknowledge support from NASA contract NAS8-03060. NR 29 TC 6 Z9 6 U1 0 U2 1 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD APR PY 2013 VL 552 AR A45 DI 10.1051/0004-6361/201220836 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 130JW UT WOS:000317912000045 ER PT J AU Sotomayor-Beltran, C Sobey, C Hessels, JWT de Bruyn, G Noutsos, A Alexov, A Anderson, J Asgekar, A Avruch, IM Beck, R Bell, ME Bell, MR Bentum, MJ Bernardi, G Best, P Birzan, L Bonafede, A Breitling, F Broderick, J Brouw, WN Bruggen, M Ciardi, B de Gasperin, F Dettmar, RJ van Duin, A Duscha, S Eisloffel, J Falcke, H Fallows, RA Fender, R Ferrari, C Frieswijk, W Garrett, MA Griessmeier, J Grit, T Gunst, AW Hassall, TE Heald, G Hoeft, M Horneffer, A Iacobelli, M Juette, E Karastergiou, A Keane, E Kohler, J Kramer, M Kondratiev, VI Koopmans, LVE Kuniyoshi, M Kuper, G van Leeuwen, J Maat, P Macario, G Markoff, S McKean, JP Mulcahy, DD Munk, H Orru, E Paas, H Pandey-Pommier, M Pilia, M Pizzo, R Polatidis, AG Reich, W Rottgering, H Serylak, M Sluman, J Stappers, BW Tagger, M Tang, Y Tasse, C ter Veen, S Vermeulen, R van Weeren, RJ Wijers, RAMJ Wijnholds, SJ Wise, MW Wucknitz, O Yatawatta, S Zarka, P AF Sotomayor-Beltran, C. Sobey, C. Hessels, J. W. T. de Bruyn, G. Noutsos, A. Alexov, A. Anderson, J. Asgekar, A. Avruch, I. M. Beck, R. Bell, M. E. Bell, M. R. Bentum, M. J. Bernardi, G. Best, P. Birzan, L. Bonafede, A. Breitling, F. Broderick, J. Brouw, W. N. Brueggen, M. Ciardi, B. de Gasperin, F. Dettmar, R. -J. van Duin, A. Duscha, S. Eisloffel, J. Falcke, H. Fallows, R. A. Fender, R. Ferrari, C. Frieswijk, W. Garrett, M. A. Griessmeier, J. Grit, T. Gunst, A. W. Hassall, T. E. Heald, G. Hoeft, M. Horneffer, A. Iacobelli, M. Juette, E. Karastergiou, A. Keane, E. Kohler, J. Kramer, M. Kondratiev, V. I. Koopmans, L. V. E. Kuniyoshi, M. Kuper, G. van Leeuwen, J. Maat, P. Macario, G. Markoff, S. McKean, J. P. Mulcahy, D. D. Munk, H. Orru, E. Paas, H. Pandey-Pommier, M. Pilia, M. Pizzo, R. Polatidis, A. G. Reich, W. Rottgering, H. Serylak, M. Sluman, J. Stappers, B. W. Tagger, M. Tang, Y. Tasse, C. ter Veen, S. Vermeulen, R. van Weeren, R. J. Wijers, R. A. M. J. Wijnholds, S. J. Wise, M. W. Wucknitz, O. Yatawatta, S. Zarka, P. TI Calibrating high-precision Faraday rotation measurements for LOFAR and the next generation of low-frequency radio telescopes SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE polarization; techniques: polarimetric ID GALACTIC MAGNETIC-FIELD; PULSAR ROTATION; ARRAY; MHZ; DEPOLARIZATION; DISPERSION; GALAXY; VLA AB Faraday rotation measurements using the current and next generation of low-frequency radio telescopes will provide a powerful probe of astronomical magnetic fields. However, achieving the full potential of these measurements requires accurate removal of the time-variable ionospheric Faraday rotation contribution. We present ionFR, a code that calculates the amount of ionospheric Faraday rotation for a specific epoch, geographic location, and line-of-sight. ionFR uses a number of publicly available, GPS-derived total electron content maps and the most recent release of the International Geomagnetic Reference Field. We describe applications of this code for the calibration of radio polarimetric observations, and demonstrate the high accuracy of its modeled ionospheric Faraday rotations using LOFAR pulsar observations. These show that we can accurately determine some of the highest-precision pulsar rotation measures ever achieved. Precision rotation measures can be used to monitor rotation measure variations - either intrinsic or due to the changing line-of-sight through the interstellar medium. This calibration is particularly important for nearby sources, where the ionosphere can contribute a significant fraction of the observed rotation measure. We also discuss planned improvements to ionFR, as well as the importance of ionospheric Faraday rotation calibration for the emerging generation of low-frequency radio telescopes, such as the SKA and its pathfinders. C1 [Sotomayor-Beltran, C.; Dettmar, R. -J.; Juette, E.] Ruhr Univ Bochum, Astron Inst, D-44780 Bochum, Germany. [Sobey, C.; Noutsos, A.; Anderson, J.; Beck, R.; Horneffer, A.; Keane, E.; Kohler, J.; Kramer, M.; Kuniyoshi, M.; Mulcahy, D. D.; Reich, W.; Wucknitz, O.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Hessels, J. W. T.; de Bruyn, G.; Asgekar, A.; Avruch, I. M.; Bentum, M. J.; Brouw, W. N.; van Duin, A.; Duscha, S.; Falcke, H.; Fallows, R. A.; Frieswijk, W.; Garrett, M. A.; Griessmeier, J.; Grit, T.; Gunst, A. W.; Heald, G.; Kondratiev, V. I.; Kuper, G.; van Leeuwen, J.; Maat, P.; McKean, J. P.; Munk, H.; Orru, E.; Pilia, M.; Pizzo, R.; Polatidis, A. G.; Sluman, J.; Tang, Y.; Vermeulen, R.; van Weeren, R. J.; Wijnholds, S. J.; Wise, M. W.; Yatawatta, S.] ASTRON, NL-7990 AA Dwingeloo, Netherlands. [Hessels, J. W. T.; Alexov, A.; van Leeuwen, J.; Markoff, S.; Wijers, R. A. M. J.; Wise, M. W.] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 XH Amsterdam, Netherlands. [de Bruyn, G.; Avruch, I. M.; Bernardi, G.; Brouw, W. N.; Koopmans, L. V. E.] Kapteyn Astron Inst, NL-9700 AV Groningen, Netherlands. [Alexov, A.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Avruch, I. M.] SRON Netherlands Insitute Space Res, NL-3584 CA Utrecht, Netherlands. [Bell, M. E.] Univ Sydney, Sydney Inst Astron, ARC Ctr Excellence All Sky Astrophys CAASTRO, Sydney, NSW 2006, Australia. [Bell, M. E.; Broderick, J.; Fender, R.; Hassall, T. E.] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England. [Bell, M. R.; Ciardi, B.; de Gasperin, F.] Max Planck Inst Astrophys, D-85741 Garching, Germany. [Best, P.] Univ Edinburgh, Inst Astron, Royal Observ Edinburgh, Edinburgh EH9 3HJ, Midlothian, Scotland. [Birzan, L.; Garrett, M. A.; Iacobelli, M.; Pandey-Pommier, M.; Rottgering, H.; van Weeren, R. J.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [Bonafede, A.; Brueggen, M.; de Gasperin, F.] Univ Hamburg, D-21029 Hamburg, Germany. [Bonafede, A.] Jacobs Univ Bremen, D-28759 Bremen, Germany. [Breitling, F.] Leibniz Inst Astrophys Potsdam AIP, D-14482 Potsdam, Germany. [Eisloffel, J.; Hoeft, M.] Thuringer Landessternwarte, D-07778 Tautenburg, Germany. [Falcke, H.; Orru, E.; ter Veen, S.] Radboud Univ Nijmegen, Dept Astrophys, IMAPP, NL-6500 GL Nijmegen, Netherlands. [Ferrari, C.; Macario, G.] Univ Nice Sophia Antipolis, Observ Cote Azur, Lab Lagrange, CNRS,UMR 7293, F-06300 Nice, France. [Griessmeier, J.; Serylak, M.; Tagger, M.] CNRS, UMR 7328, Lab Phys & Chim Environm & Espace LPC2E, F-45071 Orleans 02, France. [Hassall, T. E.; Kramer, M.; Stappers, B. W.] Univ Manchester, Sch Phys & Astron, Jodrell Bank Ctr Astrophys, Manchester M13 9PL, Lancs, England. [Karastergiou, A.] Univ Oxford, Oxford OX1 3RH, England. [Kondratiev, V. I.] PN Lebedev Phys Inst, Ctr Astro Space, Moscow 117997, Russia. [Paas, H.] Univ Groningen, CIT, NL-9700 AB Groningen, Netherlands. [Pandey-Pommier, M.] Observ Lyon, Ctr Rech Astrophys Lyon, F-69561 St Genis Laval, France. [Serylak, M.] CNRS INSU, Observ Paris, Stn Radioastron Nancay, F-18330 Nancay, France. [Tasse, C.; Zarka, P.] Observ Paris, CNRS, UMR 8109, LESIA, F-92195 Meudon, France. [van Weeren, R. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Wucknitz, O.] Univ Bonn, Argelander Inst Astron, D-53121 Bonn, Germany. RP Sotomayor-Beltran, C (reprint author), Ruhr Univ Bochum, Astron Inst, Univ Str 150, D-44780 Bochum, Germany. EM sotomayor@astro.rub.de RI Tagger, Michel/O-6615-2014; Ciardi, Benedetta/N-7625-2015; Kondratiev, Vladislav/N-1105-2015; Falcke, Heino/H-5262-2012; Yatawatta, Sarod/E-6037-2013; OI Tagger, Michel/0000-0003-2962-3220; Kondratiev, Vladislav/0000-0001-8864-7471; Falcke, Heino/0000-0002-2526-6724; Yatawatta, Sarod/0000-0001-5619-4017; Wijers, Ralph/0000-0002-3101-1808; de Gasperin, Francesco/0000-0003-4439-2627; van Weeren, Reinout/0000-0002-0587-1660 FU Deutsche Forschungsgemeinschaft (DFG) [FOR 1254]; Veni Fellowship of the Netherlands Foundation for Scientific Research (NWO); DFG [WU 588/1-1]; European Commission (European Reintegration) [PERG02-GA-2007-224897]; Agence Nationale de la Recherche [ANR-09-JCJC-0001-01] FX The authors want to express their gratitude to Dr. Dominic Schnitzeler and Dr. David Champion for their valuable comments and suggestions to improve the quality of the paper. C.S.B. and C.S. would like to thank the Deutsche Forschungsgemeinschaft (DFG) which funded this work within the research unit FOR 1254 "Magnetisation of Interstellar and Intergalactic Media: The Prospects of Low-Frequency Radio Observations". J.W.T.H. was funded for this work by a Veni Fellowship of the Netherlands Foundation for Scientific Research (NWO). O.W. is supported by the DFG (Emmy-Noether Grant WU 588/1-1) and by the European Commission (European Reintegration Grant PERG02-GA-2007-224897 WIDEMAP). C.F. and G.M. acknowledge financial support by the Agence Nationale de la Recherche through grant ANR-09-JCJC-0001-01. The Low Frequency Array (LOFAR) was designed and constructed by ASTRON, the Netherlands Institute for Radio Astronomy, and has facilities in several countries, that are owned by various parties (each with their own funding sources), and that are collectively operated by the International LOFAR Telescope (ILT) foundation under a joint scientific policy. The WSRT is operated by ASTRON/NWO. NR 49 TC 24 Z9 24 U1 0 U2 5 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 EI 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD APR PY 2013 VL 552 AR A58 DI 10.1051/0004-6361/201220728 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 130JW UT WOS:000317912000058 ER PT J AU Zwintz, K Fossati, L Guenther, DB Ryabchikova, T Baglin, A Themessl, N Barnes, TG Matthews, JM Auvergne, M Bohlender, D Chaintreuil, S Kuschnig, R Moffat, AFJ Rowe, JF Rucinski, SM Sasselov, D Weiss, WW AF Zwintz, K. Fossati, L. Guenther, D. B. Ryabchikova, T. Baglin, A. Themessl, N. Barnes, T. G. Matthews, J. M. Auvergne, M. Bohlender, D. Chaintreuil, S. Kuschnig, R. Moffat, A. F. J. Rowe, J. F. Rucinski, S. M. Sasselov, D. Weiss, W. W. TI Regular frequency patterns in the young delta Scuti star HD 261711 observed by the CoRoT and MOST satellites SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE stars: variables: delta Scuti; stars: oscillations; stars: individual: HD261711; techniques: photometric; techniques: spectroscopic ID PRE-MAIN-SEQUENCE; CLUSTER NGC 2264; LINE-DATA-BASE; DIFFERENTIAL ROTATION; MODEL ATMOSPHERES; STELLAR EVOLUTION; PRAESEPE CLUSTER; F-STARS; PHOTOMETRY; SPACE AB Context. The internal structure of pre-main-sequence (PMS) stars is poorly constrained at present. This could change significantly through high-quality asteroseismological observations of a sample of such stars. Aims. We concentrate on an asteroseismological study of HD261711, a rather hot delta Scuti-type pulsating member of the young open cluster NGC 2264 located at the blue border of the instability region. HD261711 was discovered to be a PMS delta Scuti star using the time series photometry obtained by the MOST satellite in 2006. Methods. High-precision, time-series photometry of HD261711 was obtained by the MOST and CoRoT satellites in four separate new observing runs that are put into context with the star's fundamental atmospheric parameters obtained from spectroscopy. Frequency Analysis was performed using Period04. The spectral analysis was performed using equivalent widths and spectral synthesis. Results. With the new MOST data set from 2011/12 and the two CoRoT light curves from 2008 and 2011/12, the delta Scuti variability was confirmed and regular groups of frequencies were discovered. The two pulsation frequencies identified in the data from the first MOST observing run in 2006 are confirmed and 23 new delta Scuti-type frequencies were discovered using the CoRoT data. Weighted average frequencies for each group were determined and are related to l = 0 and l = 1 p-modes. Evidence for amplitude modulation of the frequencies in two groups is seen. The effective temperature (T-eff) was derived to be 8600 +/- 200K, log g is 4.1 +/- 0.2, and the projected rotational velocity (upsilon sin i) is 53 +/- 1 km s(-1). Using our T-eff value and the radius of 1.8 +/- 0.5 R-circle dot derived from spectral energy distribution (SED) fitting, we get a luminosity log L/L-circle dot of 1.20 +/- 0.14 which agrees well to the seismologically determined values of 1.65 R-circle dot and, hence, a log L/L-circle dot of 1.13. The radial velocity of 14 +/- 2 km s(-1) we derived for HD261711, confirms the star's membership to NGC 2264. Conclusions. Our asteroseismic models suggest that HD261711 is a delta Scuti-type star close to the zero-age main sequence (ZAMS) with a mass of 1.8 to 1.9 M-circle dot. With an age of about 10 million years derived from asteroseismology, the star is either a young ZAMS star or a late PMS star just before the onset of hydrogen-core burning. The observed splittings about the l = 0 and 1 parent modes may be an artifact of the Fourier derived spectrum of frequencies with varying amplitudes. C1 [Zwintz, K.] Katholieke Univ Leuven, Inst Sterrenkunde, B-3001 Louvain, Belgium. [Zwintz, K.; Themessl, N.; Kuschnig, R.; Weiss, W. W.] Univ Vienna, Inst Astron, A-1180 Vienna, Austria. [Fossati, L.] Univ Bonn, Argelander Inst Astron, D-53121 Bonn, Germany. [Guenther, D. B.] St Marys Univ, Dept Phys & Astron, Halifax, NS B3H 3C3, Canada. [Ryabchikova, T.] Russian Acad Sci, Inst Astron, Moscow 119017, Russia. [Baglin, A.; Auvergne, M.; Chaintreuil, S.] Observ Paris, LESIA, F-92195 Meudon, France. [Barnes, T. G.] Univ Texas Austin, McDonald Observ, Austin, TX 79734 USA. [Matthews, J. M.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada. [Bohlender, D.] Natl Res Council Canada, Herzberg Inst Astrophys, Victoria, BC V9E 2E7, Canada. [Moffat, A. F. J.] Univ Montreal, Dept Phys, Montreal, PQ H3C 3J7, Canada. [Rowe, J. F.] NASA Ames Res Pk, Moffett Field, CA 94035 USA. [Rucinski, S. M.] Univ Toronto, Dept Astron & Astrophys, Toronto, ON M5S 3H4, Canada. [Sasselov, D.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Zwintz, K (reprint author), Katholieke Univ Leuven, Inst Sterrenkunde, Celestijnenlaan 200D, B-3001 Louvain, Belgium. EM konstanze.zwintz@ster.kuleuven.be OI Zwintz, Konstanze/0000-0001-9229-8315 FU Research Foundation - Flanders (FWO); Austrian Fonds zur Forderung der wissenschaftlichen Forschung [P 21830-N16, P22691-N16]; Russian Academy of Sciences "Non-stationary phenomena in the Universe"; Natural Sciences and Engineering Research Council (NSERC) of Canada; Austrian Research Promotion Agency-ALR FX K.Z. receives a Pegasus Marie Curie Fellowship of the Research Foundation - Flanders (FWO). This investigation has been supported by the Austrian Fonds zur Forderung der wissenschaftlichen Forschung through project P 21830-N16 (PI: M. Breger). T.R. acknowledges partial financial support from Basic Research Program of the Russian Academy of Sciences "Non-stationary phenomena in the Universe". D.B.G., J.M., A.F.J.M. and S.M.R. acknowledge the funding support of the Natural Sciences and Engineering Research Council (NSERC) of Canada. R.K. and W.W.W. are supported by the Austrian Fonds zur Forderung der wissenschaftlichen Forschung (P22691-N16) and by the Austrian Research Promotion Agency-ALR. Spectroscopic data were obtained with the 2.7-m telescope at Mc Donald Observatory, Texas, US and at the Dominion Astrophysical Observatory, Herzberg Institute of Astrophysics, National Research Council of Canada. NR 71 TC 5 Z9 5 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 APR PY 2013 VL 552 AR A68 DI 10.1051/0004-6361/201220934 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 130JW UT WOS:000317912000068 ER PT J AU Touchon, JC McCoy, MW Vonesh, JR Warkentin, KM AF Touchon, Justin C. McCoy, Michael W. Vonesh, James R. Warkentin, Karen M. TI Effects of plastic hatching timing carry over through metamorphosis in red-eyed treefrogs SO ECOLOGY LA English DT Article DE Agalychnis callidryas; Anura; carry-over effects; Gamboa, Panama; latent effects; life-history switch point; Neotropical treefrog; Pantala flavescens; phenotypic plasticity ID COMPLEX LIFE-HISTORIES; TRADE-OFFS; TREE FROG; AGALYCHNIS-CALLIDRYAS; XENOPUS-LAEVIS; HYPEROLIUS-SPINIGULARIS; DIFFERENTIAL PREDATION; PHENOTYPIC PLASTICITY; ADAPTIVE PLASTICITY; FIELD EXPERIMENTS AB Environmentally cued plasticity in hatching timing is widespread in animals. As with later life-history switch points, plasticity in hatching timing may have carryover effects that affect subsequent interactions with predators and competitors. Moreover, the strength of such effects of hatching plasticity may be context dependent. We used red-eyed treefrogs, Agalychnis callidryas, to test for lasting effects of hatching timing (four or six days post-oviposition) under factorial combinations of resource levels (high or low) and predation risk (none, caged, or lethal Pantala flavescens dragonfly naiads). Tadpoles were raised in 400-L mesocosms in Gamboa, Panama, from hatching until all animals had metamorphosed or died, allowing assessment of effects across a nearly six-month period of metamorphosis. Hatching early reduced survival to metamorphosis, increased larval growth, and had context-dependent effects on metamorph phenotypes. Early during the period of metamorph emergence, early-hatched animals were larger than late-hatched ones, but this effect attenuated over time. Early-hatched animals also left the water with relatively longer tails. Lethal predators dramatically reduced survival to metamorphosis, with most mortality occurring early in the larval period. Predator effects on the timing of metamorphosis and metamorph size and tail length depended upon resources. For example, lethal predators reduced larval periods, and this effect was stronger with low resources. Predators affected metamorph size early in the period of metamorphosis, whereas resource levels were a stronger determinant of phenotype for animals that metamorphosed later. Effects of hatching timing were detectable on top of strong effects of larval predators and resources, across two subsequent life stages, and some were as strong as or stronger than effects of resources. Plasticity in hatching timing is ecologically important and currently underappreciated. Effects on metamorph numbers and phenotypes may impact subsequent interactions with predators, competitors, and mates, with potentially cascading effects on recruitment and fitness. C1 [Touchon, Justin C.; McCoy, Michael W.; Warkentin, Karen M.] Boston Univ, Dept Biol, Boston, MA 02215 USA. [Touchon, Justin C.; Warkentin, Karen M.] Smithsonian Trop Res Inst, Balboa, Panama. [McCoy, Michael W.] E Carolina Univ, Dept Biol, Greenville, NC 27858 USA. [Vonesh, James R.] Virginia Commonwealth Univ, Dept Biol, Richmond, VA 23284 USA. RP Touchon, JC (reprint author), Smithsonian Trop Res Inst, Apartado Postal 0843-03092, Balboa, Panama. EM TouchonJC@si.edu RI Vonesh, James/I-1573-2013 OI Vonesh, James/0000-0003-2481-9988 FU Autoridad Nacional del Ambiente de Panama for permits [SC/A-32-09, SC/A-73-09]; Boston University IACUC [08-011]; National Science Foundation [DEB-0717220, DEB-0716923] FX We thank the Smithsonian Tropical Research Institute (STRI) for logistical support and the Autoridad Nacional del Ambiente de Panama for permits (SC/A-32-09 and SC/A-73-09). This research was conducted under Boston University IACUC protocol number 08-011. We thank C. Asquith, S. Gonzalez, A. Lebron, H. Macleod, C. Silva, I. Smith, and R. Tarvin for assistance with the experiment, and two anonymous reviewers for helpful comments on the paper. This research was funded by the National Science Foundation (DEB-0717220 to J. R. Vonesh and DEB-0716923 to K. M. Warkentin), Boston University, Virginia Commonwealth University, and STRI. NR 74 TC 20 Z9 20 U1 5 U2 58 PU ECOLOGICAL SOC AMER PI WASHINGTON PA 1990 M STREET NW, STE 700, WASHINGTON, DC 20036 USA SN 0012-9658 EI 1939-9170 J9 ECOLOGY JI Ecology PD APR PY 2013 VL 94 IS 4 BP 850 EP 860 PG 11 WC Ecology SC Environmental Sciences & Ecology GA 131BF UT WOS:000317964900010 ER PT J AU Sapijanskas, J Potvin, C Loreau, M AF Sapijanskas, Jurgis Potvin, Catherine Loreau, Michel TI Beyond shading: Litter production by neighbors contributes to overyielding in tropical trees SO ECOLOGY LA English DT Article DE belowground interactions; biodiversity and ecosystem functioning; facilitation; forest stand dynamics; interspecific interactions; light competition; litter; mixed-species forests; neighborhood; over-yielding; Sardinilla Project; Panama; tree plantation ID BIODIVERSITY EXPERIMENT; ECOSYSTEM FUNCTION; MIXED PLANTATIONS; CARBON STORAGE; USE EFFICIENCY; RAIN-FOREST; DIVERSITY; COMPETITION; GROWTH; MODEL AB The influence of biodiversity on ecosystem functioning is now well established. However, our ability to predict the ecological consequences of biodiversity changes remains limited by our poor understanding of the mechanisms underlying biodiversity effects. We disentangled the contributions of light competition and residual neighborhood interactions in a 10-year-old biodiversity experiment with tropical trees that display overyielding, i.e., higher community-level yields in mixtures compared with monocultures. We developed models of individual tree growth that partition the effects of neighboring trees into shading and residual effects assumed to reflect primarily belowground interactions. These models reject the hypothesis that reduced light competition in mixtures is the only mechanism driving overyielding. After factoring out the effects of shading, litter production by neighbors was a far better predictor of tree growth than traditional crowding indices; it contributed to overyielding by producing pairwise interactions that ranged from competitive to facilitative, but which, on average, concentrated competition within species. Consistent with litter-mediated biodiversity effects, the magnitude of overyielding increased over time. Our results provide evidence for diversity effects extending beyond that of light and reveal the neglected role of litter-mediated interactions among trees. C1 [Sapijanskas, Jurgis; Potvin, Catherine; Loreau, Michel] McGill Univ, Dept Biol, Montreal, PQ H3A 1B1, Canada. [Sapijanskas, Jurgis] AgroParisTech ENGREF, Ecole Natl Genie Rural Eaux & Forets, Direct Sci, F-75015 Paris, France. [Potvin, Catherine] Smithsonian Trop Res Inst, Balboa, Panama. [Loreau, Michel] CNRS, Ctr Biodivers Theory & Modelling, Expt Ecol Stn, F-09200 Moulis, France. RP Sapijanskas, J (reprint author), AgroParisTech ENGREF, 19 Ave Maine, F-75015 Paris, France. EM jurgis.sapijanskas@polytechnique.org FU French Ministry of Agriculture; Natural Sciences and Engineering Research Council of Canada; Canada Research Chair Programme; TULIP Laboratory of Excellence [ANR-10-LABX-41]; Smithsonian Tropical Research Institute FX We are grateful to Jose Monteza for invaluable help in maintaining the experimental plantation and data collection. Fabienne Zeugin kindly provided her data on leaf nutrient content. We thank Benoit Courbaud, Forest Isbell, Paul Leadley, Justin Marleau, Chadwick Oliver, Alain Paquette, and an anonymous reviewer for helpful comments that substantially strengthened the manuscript. Jurgis Sapijanskas was funded by the French Ministry of Agriculture. Catherine Potvin and Michel Loreau were funded by Discovery grants from the Natural Sciences and Engineering Research Council of Canada. Michel Loreau also acknowledges support by the Canada Research Chair Programme and the TULIP Laboratory of Excellence (ANR-10-LABX-41). The Sardinilla experiment is supported by the Smithsonian Tropical Research Institute. NR 54 TC 8 Z9 8 U1 4 U2 56 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 APR PY 2013 VL 94 IS 4 BP 941 EP 952 PG 12 WC Ecology SC Environmental Sciences & Ecology GA 131BF UT WOS:000317964900018 ER PT J AU Kita, NT Welten, KC Valley, JW Spicuzza, MJ Nakashima, D Tenner, TJ Ushikubo, T MacPherson, GJ Welzenbach, L Heck, PR Davis, AM Meier, MMM Wieler, R Caffee, MW Laubenstein, M Nishiizumi, K AF Kita, Noriko T. Welten, Kees C. Valley, John W. Spicuzza, Michael J. Nakashima, Daisuke Tenner, Travis J. Ushikubo, Takayuki MacPherson, Glenn J. Welzenbach, Linda Heck, Philipp R. Davis, Andrew M. Meier, Matthias M. M. Wieler, Rainer Caffee, Marc W. Laubenstein, Matthias Nishiizumi, Kunihiko TI Fall, classification, and exposure history of the Mifflin L5 chondrite SO METEORITICS & PLANETARY SCIENCE LA English DT Article ID COSMOGENIC NUCLIDES; OXYGEN-ISOTOPE; METEORITE SHOWER; STONY METEORITES; PRODUCTION-RATES; PARENT BODIES; AMS STANDARDS; BRECCIAS; RECORDS; ORIGIN AB The Mifflin meteorite fell on the night of April 14, 2010, in southwestern Wisconsin. A bright fireball was observed throughout a wide area of the midwestern United States. The petrography, mineral compositions, and oxygen isotope ratios indicate that the meteorite is a L5 chondrite fragmental breccia with light/dark structure. The meteorite shows a low shock stage of S2, although some shock-melted veins are present. The U,Th-He age is 0.7Ga, and the K-Ar age is 1.8Ga, indicating that Mifflin might have been heated at the time of the 470Ma L-chondrite parent body breakup and that U, Th-He, and K-Ar ages were partially reset. The cosmogenic radionuclide data indicate that Mifflin was exposed to cosmic rays while its radius was 3065cm. Assuming this exposure geometry, a cosmic-ray exposure age of 25 +/- 3Ma is calculated from cosmogenic noble gas concentrations. The low 22Ne/21Ne ratio may, however, indicate a two-stage exposure with a longer first-stage exposure at high shielding. Mifflin is unusual in having a low radiogenic gas content combined with a low shock stage and no evidence of late stage annealing; this inconsistency remains unexplained. C1 [Kita, Noriko T.; Valley, John W.; Spicuzza, Michael J.; Nakashima, Daisuke; Tenner, Travis J.; Ushikubo, Takayuki] Univ Wisconsin, Dept Geosci, Madison, WI 53706 USA. [Welten, Kees C.; Nishiizumi, Kunihiko] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [MacPherson, Glenn J.; Welzenbach, Linda] Smithsonian Inst, Natl Museum Nat Hist, Dept Mineral Sci, Washington, DC 20560 USA. [Heck, Philipp R.] Field Museum Nat Hist, Dept Geol, Robert A Pritzker Ctr Meteorit & Polar Studies, Chicago, IL 60605 USA. [Heck, Philipp R.; Davis, Andrew M.] Univ Chicago, Chicago Ctr Cosmochem, Chicago, IL 60637 USA. [Davis, Andrew M.] Univ Chicago, Dept Geophys Sci, Chicago, IL 60637 USA. [Davis, Andrew M.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA. [Meier, Matthias M. M.; Wieler, Rainer] ETH, Dept Earth Sci, CH-8092 Zurich, Switzerland. [Meier, Matthias M. M.] Lund Univ, Dept Geol, SE-22362 Lund, Sweden. [Caffee, Marc W.] Purdue Univ, Dept Phys, W Lafayette, IN 47907 USA. [Laubenstein, Matthias] Ist Nazl Fis Nucl, Lab Nazl Gran Sasso, I-67100 Assergi, AQ, Italy. RP Kita, NT (reprint author), Univ Wisconsin, Dept Geosci, Madison, WI 53706 USA. EM noriko@geology.wisc.edu RI Wieler, Rainer/A-1355-2010; Laubenstein, Matthias/C-4851-2013; Caffee, Marc/K-7025-2015; Kita, Noriko/H-8035-2016; Valley, John/B-3466-2011 OI Wieler, Rainer/0000-0001-5666-7494; Laubenstein, Matthias/0000-0001-5390-4343; Caffee, Marc/0000-0002-6846-8967; Kita, Noriko/0000-0002-0204-0765; Davis, Andrew/0000-0001-7955-6236; Meier, Matthias/0000-0002-7179-4173; Valley, John/0000-0003-3530-2722 FU NASA [NNX10AH77G, NNX08AY83G, NNX11AC69G, NNX09AG39G]; Swiss National Science Foundation FX Richard Jinkins and his family, and Terry Boudreaux are thanked for donating meteorites for analysis. Other private owners of Mifflin meteorite samples allowed initial inspection and photography. Atul Kumar provided a strewn field map and detailed information of individual masses. Richard Slaughter and others in the Geology Museum and Department of Geoscience, UW-Madison, helped search for and identify the meteorites. Brian Hess, John Fournelle, and Hiromi Konishi are thanked for preparation of Mifflin meteorite sections, and assistance to the electron microprobe analysis, and X-ray diffraction analysis, respectively. We acknowledge Henry Revercomb and Fred Best, Space Science and Engineering Center, UW-Madison, for the permission to use the photo of the fireball (Fig. 1). Mary Diman is thanked for drafting the strewn field map (Fig. 2). We acknowledge careful reviews by Addi Bischoff, Jutta Zipfel, Greg Herzog, and Associate Editor Alex Ruzicka, which improved the quality of the manuscript, and discussion with Alan Rubin. This work is supported by NASA grants NNX10AH77G (NK), NNX08AY83G (JWV), NNX11AC69G (KN), and NNX09AG39G (AMD), and the Swiss National Science Foundation. NR 43 TC 3 Z9 3 U1 1 U2 13 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1086-9379 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD APR PY 2013 VL 48 IS 4 BP 641 EP 655 DI 10.1111/maps.12077 PG 15 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 131WU UT WOS:000318029400004 ER PT J AU Lee, JC Kriss, GA Chakravorty, S Rahoui, F Young, AJ Brandt, WN Hines, DC Ogle, PM Reynolds, CS AF Lee, Julia C. Kriss, Gerard A. Chakravorty, Susmita Rahoui, Farid Young, Andrew J. Brandt, William N. Hines, Dean C. Ogle, Patrick M. Reynolds, Christopher S. TI The ionized absorber and nuclear environment of IRAS 13349+2438: multi-wavelength insights from coordinated Chandra HETGS, HST STIS, HET and Spitzer IRS SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies: active; quasars: absorption lines; quasars: emission lines; quasars: individual: IRAS 13349+2438; ultraviolet: galaxies; X-rays: galaxies ID ACTIVE GALACTIC NUCLEI; HOBBY-EBERLY TELESCOPE; DIGITAL SKY SURVEY; SPECTRAL ENERGY-DISTRIBUTIONS; LOW-RESOLUTION SPECTROGRAPH; QUASI-STELLAR OBJECTS; STAR-FORMING GALAXIES; ACCRETION DISK MODELS; X-RAY SPECTROSCOPY; BROAD-LINE REGION AB We present results from a multi-wavelength infrared (IR)-to-X-ray campaign of the infrared bright (but highly optical-ultraviolet extincted) quasi-stellar object (QSO) IRAS 13349+2438 obtained with the Chandra High Energy Transmission Grating Spectrometer (HETGS), the Hubble Space Telescope (HST) Space Telescope Imaging Spectrograph (STIS), the Hobby-Eberly Telescope (HET) 8 m and the Spitzer Infrared Spectrometer (IRS). Based on HET optical spectra of [O III], we refine the redshift of IRAS 13349 to be z = 0.108 53. The weakness of the [O III] in combination with strong Fe II in the HET spectra reveals extreme Eigenvector-1 characteristics in IRAS 13349, but the 2468 km s(-1) width of the H beta line argues against a narrow-line Seyfert 1 classification; on average, IR, optical and optical-ultraviolet (UV) spectra show IRAS 13349 to be a typical QSO. Independent estimates based on the H beta line width and fits to the IRAS 13349 spectral energy distribution (SED) both give a black hole mass of M-BH = 10(9) M-circle dot. The heavily reddened STIS UV spectra reveal for the first time blueshifted absorption from Ly alpha, N V and C IV, with components at systemic velocities of -950 km s(-1) and -75 km s(-1). The higher velocity UV lines are coincident with the lower ionization (xi similar to 1.6) WA-1 warm absorber lines seen in the X-rays with the HETGS. In addition, a xi similar to 3.4 WA-2 is also required by the data, while a xi similar to 3 WA-3 is predicted by theory and seen at less significance; all detected X-ray absorption lines are blueshifted by similar to 700-900 km s(-1). Theoretical models comparing different ionizing SEDs reveal that including the UV (i.e. the accretion disc) as part of the ionizing continuum has strong implications for the conclusions one would draw about the thermodynamic stability of the warm absorber. Specific to IRAS 13349, we find that an X-ray-UV ionizing SED favours a continuous distribution of ionization states in a smooth flow (this paper) versus discrete clouds in pressure equilibrium (previous work by other authors). Direct detections of dust are seen in both the IR and X-rays. We see weak polycyclic aromatic hydrocarbon (PAH) emission at 7.7 mu m and 11.3 mu m which may also be blended with forsterite, and 10 mu m and 18 mu m silicate emission, as well as an Fe L edge at 700 eV indicative of iron-based dust with a dust-to-gas ratio >90 per cent. We develop a geometrical model in which we view the nuclear regions of the QSO along a line of sight that passes through the upper atmosphere of an obscuring torus. This sight line is largely transparent in X-rays since the gas is ionized, but it is completely obscured by dust that blocks a direct view of the UV/optical emission region. In the context of our model, 20 per cent of the intrinsic UV/optical continuum is scattered into our sight line by the far wall of an obscuring torus. An additional 2.4 per cent of the direct light, which likely dominates the UV emission, is Thomson-scattered into our line of sight by another off-plane component of highly ionized gas. C1 [Lee, Julia C.; Chakravorty, Susmita; Rahoui, Farid] Harvard Univ, Dept Astron, Cambridge, MA 02138 USA. [Lee, Julia C.; Chakravorty, Susmita; Rahoui, Farid] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Kriss, Gerard A.; Hines, Dean C.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Kriss, Gerard A.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Young, Andrew J.] Univ Bristol, HH Wills Phys Lab, Bristol BS8 1TL, Avon, England. [Brandt, William N.] Penn State Univ, Dept Astron & Astrophys, Davey Lab 525, University Pk, PA 16802 USA. [Brandt, William N.] Penn State Univ, Inst Gravitat & Cosmos, University Pk, PA 16802 USA. [Ogle, Patrick M.] CALTECH, IPAC, Pasadena, CA 91125 USA. [Reynolds, Christopher S.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. RP Lee, JC (reprint author), Harvard Univ, Dept Astron, 60 Garden St, Cambridge, MA 02138 USA. EM jclee@head.cfa.harvard.edu RI Brandt, William/N-2844-2015; Lee, Julia/G-2381-2015 OI Brandt, William/0000-0002-0167-2453; Lee, Julia/0000-0002-7336-3588 FU Chandra Guest Observer grant [GO4-5110C]; NASA through Space Telescope Science Institute [10 088]; NASA [NAS5-26555]; NASA ADP [NNX11AJ59G] FX We are grateful to Dave Huenemoerder, John Houck, Tim Kallman and Aneta Siemiginowska for helpful dialogue and/or computing-related assistance and the referee for a thorough reading of the paper. We acknowledge the generous support of Chandra Guest Observer grant GO4-5110C for support of this work. Funding was also provided by NASA through grants for HST programme number 10 088 from the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Incorporated, under NASA contract NAS5-26555. WNB acknowledges the support from NASA ADP grant NNX11AJ59G. The HET is a joint project of the University of Texas at Austin, the Pennsylvania State University, Stanford University, Ludwig-Maximillians-Universitat Munchen and Georg-August-Universitat Gottingen. The HET is named in the honour of its principal benefactors, William P. Hobby and Robert E. Eberly. This research has made use of NASA's Astrophysics Data System Bibliographic Services. NR 135 TC 15 Z9 15 U1 0 U2 5 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 APR PY 2013 VL 430 IS 4 BP 2650 EP 2679 DI 10.1093/mnras/stt050 PG 30 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 136CZ UT WOS:000318339700010 ER PT J AU Hartoog, OE Wiersema, K Vreeswijk, PM Kaper, L Tanvir, NR Savaglio, S Berger, E Chornock, R Covino, S D'Elia, V Flores, H Fynbo, JPU Goldoni, P Gomboc, A Melandri, A Pozanenko, A Schaye, J Postigo, AD Wijers, RAMJ AF Hartoog, Olga E. Wiersema, Klaas Vreeswijk, Paul M. Kaper, Lex Tanvir, Nial R. Savaglio, Sandra Berger, Edo Chornock, Ryan Covino, Stefano D'Elia, Valerio Flores, Hector Fynbo, Johan P. U. Goldoni, Paolo Gomboc, Andreja Melandri, Andrea Pozanenko, Alexei Schaye, Joop de Ugarte Postigo, Antonio Wijers, Ralph A. M. J. TI The host-galaxy response to the afterglow of GRB 100901A SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE gamma-ray burst: individual: GRB 100901A; galaxies: abundances; galaxies: distances and redshifts; galaxies: ISM ID GAMMA-RAY BURST; LY-ALPHA SYSTEMS; HIGH-RESOLUTION SPECTROSCOPY; CHEMICAL ENRICHMENT HISTORY; RESONANCE-ABSORPTION LINES; STAR-FORMING REGIONS; ATOMIC DATA; METAL ABUNDANCES; TRANSITION-PROBABILITIES; WAVELENGTHS LONGWARD AB For gamma-ray burst 100901A, we have obtained Gemini-North and Very Large Telescope optical afterglow spectra at four epochs: 1 h, 1 d, 3 d and 1 week after the burst, thanks to the afterglow remaining unusually bright at late times. Apart from a wealth of metal resonance lines, we also detect lines arising from fine-structure levels of the ground state of Fe II, and from metastable levels of Fe II and Ni II at the host redshift (z = 1.4084). These lines are found to vary significantly in time. The combination of the data and modelling results shows that we detect the fall of the Ni II F-4(9/2) metastable level population, which to date has not been observed. Assuming that the population of the excited states is due to the ultraviolet radiation of the afterglow, we estimate an absorber distance of a few hundred pc. This appears to be a typical value when compared to similar studies. We detect two intervening absorbers (z = 1.3147, 1.3179). Despite the wide temporal range of the data, we do not see significant variation in the absorption lines of these two intervening systems. C1 [Hartoog, Olga E.; Kaper, Lex; Wijers, Ralph A. M. J.] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1090 GE Amsterdam, Netherlands. [Hartoog, Olga E.; Schaye, Joop] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [Wiersema, Klaas; Tanvir, Nial R.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. [Vreeswijk, Paul M.] Univ Iceland, Inst Sci, Ctr Astrophys & Cosmol, IS-107 Reykjavik, Iceland. [Savaglio, Sandra; Chornock, Ryan] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Berger, Edo] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Covino, Stefano; Melandri, Andrea] INAF Osservatorio Astron Brera, I-23807 Merate, LC, Italy. [D'Elia, Valerio] INAF Osservatorio Astron Roma, I-00040 Monte Porzio Catone, Italy. [D'Elia, Valerio] ASI Sci Data Ctr, I-00044 Frascati, Italy. [Flores, Hector] Univ Paris Diderot, Observ Paris, Lab GEPI, CNRS,UMR8111, F-92195 Meudon, France. [Fynbo, Johan P. U.] Univ Copenhagen, Niels Bohr Inst, Dark Cosmol Ctr, DK-2100 Copenhagen, Denmark. [Goldoni, Paolo] Univ Paris Diderot, CEA Irfu, Observ Paris, APC,CNRS,IN2P3, F-75205 Paris 13, France. [Gomboc, Andreja] Univ Ljubljana, Fac Math & Phys, SI-1000 Ljubljana, Slovenia. [Gomboc, Andreja] Ctr Excellence SPACE SI, SI-1000 Ljubljana, Slovenia. [Melandri, Andrea] Liverpool John Moores Univ, Astrophys Res Inst, Birkenhead CH41 1LD, Merseyside, England. [Pozanenko, Alexei] Space Res Inst IKI, Moscow 117997, Russia. [de Ugarte Postigo, Antonio] Inst Astrofis Andalucia IAA CSIC, E-18008 Granada, Spain. RP Hartoog, OE (reprint author), Univ Amsterdam, Astron Inst Anton Pannekoek, POB 94249, NL-1090 GE Amsterdam, Netherlands. EM O.E.Hartoog@uva.nl RI Fynbo, Johan/L-8496-2014; OI Fynbo, Johan/0000-0002-8149-8298; Wijers, Ralph/0000-0002-3101-1808; D'Elia, Valerio/0000-0002-7320-5862; de Ugarte Postigo, Antonio/0000-0001-7717-5085; Covino, Stefano/0000-0001-9078-5507; Schaye, Joop/0000-0002-0668-5560; Savaglio, Sandra/0000-0003-2354-3238 FU Gemini Observatory at Mauna Kea [GN-2010B-Q-7]; European Southern Observatory (ESO) Telescopes at the Paranal Observatory [085.A-0009(B)]; Dutch Research School for Astronomy (NOVA); ERC-StG grant [EGGS-278202]; DNRF; Slovenian Research Agency; Centre of Excellence for Space Sciences and Technologies SPACE-SI; European Union; European Regional Development Fund; Republic of Slovenia, Ministry of Higher Education, Science and Technology; RFBR [12-02-01336-a, 11-01-92202-Mong-a]; ERC [247295] FX Based on observations obtained at the Gemini Observatory at Mauna Kea under programme GN-2010B-Q-7, and observations obtained with European Southern Observatory (ESO) Telescopes at the Paranal Observatory under programme 085.A-0009(B).; OEH acknowledges the Dutch Research School for Astronomy (NOVA) for a PhD grant. JPUF acknowledges support from the ERC-StG grant EGGS-278202. The Dark Cosmology Centre is funded by the DNRF.; AG acknowledges funding from the Slovenian Research Agency and from the Centre of Excellence for Space Sciences and Technologies SPACE-SI, an operation partly financed by the European Union, European Regional Development Fund and Republic of Slovenia, Ministry of Higher Education, Science and Technology.; AP is grateful for support of the RFBR grants 12-02-01336-a and 11-01-92202-Mong-a.; RAMJ acknowledges support from the ERC via Advanced Investigator Grant no. 247295. NR 88 TC 9 Z9 9 U1 1 U2 3 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 APR PY 2013 VL 430 IS 4 BP 2739 EP 2754 DI 10.1093/mnras/stt078 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 136CZ UT WOS:000318339700016 ER PT J AU Bret, A Stockem, A Fiuza, F Ruyer, C Gremillet, L Narayan, R Silva, LO AF Bret, A. Stockem, A. Fiuza, F. Ruyer, C. Gremillet, L. Narayan, R. Silva, L. O. TI Collisionless shock formation, spontaneous electromagnetic fluctuations, and streaming instabilities SO PHYSICS OF PLASMAS LA English DT Article ID MAGNETIC-FIELD GENERATION; PARTICLE-ACCELERATION; STATISTICAL MECHANICS; RELATIVISTIC STREAMS; WEIBEL INSTABILITY; NONLINEAR-THEORY; COSMIC-RAYS; PLASMA; BEAM; ELECTRONS AB Collisionless shocks are ubiquitous in astrophysics and in the lab. Recent numerical simulations and experiments have shown how they can arise from the encounter of two collisionless plasma shells. When the shells interpenetrate, the overlapping region turns unstable, triggering the shock formation. As a first step towards a microscopic understanding of the process, we analyze here in detail the initial instability phase. On the one hand, 2D relativistic Particle-In-Cell simulations are performed where two symmetric initially cold pair plasmas collide. On the other hand, the instabilities at work are analyzed, as well as the field at saturation and the seed field which gets amplified. For mildly relativistic motions and onward, Weibel modes govern the linear phase. We derive an expression for the duration of the linear phase in good agreement with the simulations. This saturation time constitutes indeed a lower-bound for the shock formation time. (C) 2013 American Institute of Physics. [http://dx.doi.org/10.1063/1.4798541] C1 [Bret, A.] Univ Castilla La Mancha, ETSI Ind, E-13071 Ciudad Real, Spain. [Bret, A.] Inst Invest Energet & Aplicac Ind, Ciudad Real 13071, Spain. [Stockem, A.; Fiuza, F.; Silva, L. O.] Inst Super Tecn, Lab Associado, Inst Plasmas & Fusao Nucl, GoLP, Lisbon, Portugal. [Ruyer, C.; Gremillet, L.] CEA, DAM, DIF, F-91297 Arpajon, France. [Bret, A.; Narayan, R.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Bret, A (reprint author), Univ Castilla La Mancha, ETSI Ind, E-13071 Ciudad Real, Spain. RI Silva, Luis/C-3169-2009; Bret, Antoine/C-9112-2009; OI Silva, Luis/0000-0003-2906-924X; Bret, Antoine/0000-0003-2030-0046; Fiuza, Frederico/0000-0002-8502-5535; Stockem, Anne Gabriele/0000-0003-4614-8118; Narayan, Ramesh/0000-0002-1919-2730 FU Spanish Ministerio de Educacion y Ciencia [ENE2009-09276]; European Research Council (ERC) [267841]; FCT (Portugal) [PTDC/FIS/111720/2009, SFRH/BD/38952/2007] FX This work was supported by Projects ENE2009-09276 of the Spanish Ministerio de Educacion y Ciencia, the European Research Council (ERC-2010-AdG Grant 267841) and FCT (Portugal) Grant Nos. PTDC/FIS/111720/2009 and SFRH/BD/38952/2007. Thanks are due to Lorenzo Sironi for useful discussions. A. B. wishes to thank the Harvard-Smithsonian Center for Astrophysics for hosting him. NR 51 TC 45 Z9 45 U1 5 U2 31 PU AMER INST PHYSICS PI MELVILLE PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1, MELVILLE, NY 11747-4501 USA SN 1070-664X J9 PHYS PLASMAS JI Phys. Plasmas PD APR PY 2013 VL 20 IS 4 AR 042102 DI 10.1063/1.4798541 PG 9 WC Physics, Fluids & Plasmas SC Physics GA 134UY UT WOS:000318241900004 ER PT J AU Denneau, L Jedicke, R Grav, T Granvik, M Kubica, J Milani, A Veres, P Wainscoat, R Chang, D Pierfederici, F Kaiser, N Chambers, KC Heasley, JN Magnier, EA Price, PA Myers, J Kleyna, J Hsieh, H Farnocchia, D Waters, C Sweeney, WH Green, D Bolin, B Burgett, WS Morgan, JS Tonry, JL Hodapp, KW Chastel, S Chesley, S Fitzsimmons, A Holman, M Spahr, T Tholen, D Williams, GV Abe, S Armstrong, JD Bressi, TH Holmes, R Lister, T McMillan, RS Micheli, M Ryan, EV Ryan, WH Scotti, JV AF Denneau, Larry Jedicke, Robert Grav, Tommy Granvik, Mikael Kubica, Jeremy Milani, Andrea Veres, Peter Wainscoat, Richard Chang, Daniel Pierfederici, Francesco Kaiser, N. Chambers, K. C. Heasley, J. N. Magnier, Eugene A. Price, P. A. Myers, Jonathan Kleyna, Jan Hsieh, Henry Farnocchia, Davide Waters, Chris Sweeney, W. H. Green, Denver Bolin, Bryce Burgett, W. S. Morgan, J. S. Tonry, John L. Hodapp, K. W. Chastel, Serge Chesley, Steve Fitzsimmons, Alan Holman, Matthew Spahr, Tim Tholen, David Williams, Gareth V. Abe, Shinsuke Armstrong, J. D. Bressi, Terry H. Holmes, Robert Lister, Tim McMillan, Robert S. Micheli, Marco Ryan, Eileen V. Ryan, William H. Scotti, James V. TI The Pan-STARRS Moving Object Processing System SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC LA English DT Article ID EARTH-APPROACHING ASTEROIDS; SYNOPTIC SURVEY TELESCOPE; ORBIT DETERMINATION; SIZE DISTRIBUTION; POPULATION; SPACEWATCH; IDENTIFICATION; CALIBRATION; PROGRAM; ARRAY AB We describe the Pan-STARRS Moving Object Processing System (MOPS), a modern software package that produces automatic asteroid discoveries and identifications from catalogs of transient detections from next-generation astronomical survey telescopes. MOPS achieves >99.5% efficiency in producing orbits from a synthetic but realistic population of asteroids whose measurements were simulated for a Pan-STARRS4-class telescope. Additionally, using a nonphysical grid population, we demonstrate that MOPS can detect populations of currently unknown objects such as interstellar asteroids. MOPS has been adapted successfully to the prototype Pan-STARRS1 telescope despite differences in expected false detection rates, fill-factor loss, and relatively sparse observing cadence compared to a hypothetical Pan-STARRS4 telescope and survey. MOPS remains highly efficient at detecting objects but drops to 80% efficiency at producing orbits. This loss is primarily due to configurable MOPS processing limits that are not yet tuned for the Pan-STARRS1 mission. The core MOPS software package is the product of more than 15 person-years of software development and incorporates countless additional years of effort in third-party software to perform lower-level functions such as spatial searching or orbit determination. We describe the high-level design of MOPS and essential subcomponents, the suitability of MOPS for other survey programs, and suggest a road map for future MOPS development. C1 [Denneau, Larry; Jedicke, Robert; Veres, Peter; Wainscoat, Richard; Chang, Daniel; Kaiser, N.; Chambers, K. C.; Heasley, J. N.; Magnier, Eugene A.; Kleyna, Jan; Hsieh, Henry; Waters, Chris; Sweeney, W. H.; Green, Denver; Bolin, Bryce; Burgett, W. S.; Morgan, J. S.; Tonry, John L.; Hodapp, K. W.; Chastel, Serge; Tholen, David; Armstrong, J. D.; Micheli, Marco] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Grav, Tommy] Johns Hopkins Univ, Baltimore, MD USA. [Granvik, Mikael] Univ Helsinki, Dept Phys, FIN-00014 Helsinki, Finland. [Milani, Andrea; Farnocchia, Davide] Univ Pisa, Pisa, Italy. [Pierfederici, Francesco] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Price, P. A.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. [Myers, Jonathan] Univ Arizona, Tucson, AZ USA. [Farnocchia, Davide; Chesley, Steve] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Fitzsimmons, Alan] Queens Univ Belfast, Astrophys Res Ctr, Sch Math & Phys, Belfast BT7 1NN, Antrim, North Ireland. [Holman, Matthew] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Spahr, Tim; Williams, Gareth V.] Smithsonian Astrophys Observ, Cambridge, MA USA. [Abe, Shinsuke] Natl Cent Univ, Inst Astron, Taipei, Taiwan. [Bressi, Terry H.; McMillan, Robert S.; Scotti, James V.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA. [Holmes, Robert] Astron Res Inst, Charleston, IL 61920 USA. [Lister, Tim] Las Cumbres Observ Global Telescope Network Inc, Santa Barbara, CA 93117 USA. [Ryan, Eileen V.; Ryan, William H.] New Mexico Inst Min & Technol, Magdalena Ridge Observ, Socorro, NM 87801 USA. RP Denneau, L (reprint author), Univ Hawaii, Inst Astron, 2680 Woodlawn Dr, Honolulu, HI 96822 USA. EM denneau@ifa.hawaii.edu OI Chambers, Kenneth /0000-0001-6965-7789; Granvik, Mikael/0000-0002-5624-1888; Micheli, Marco/0000-0001-7895-8209 FU National Aeronautics and Space Administration issued through the Planetary Science Division of the NASA Science Mission Directorate [NNX08AR22G]; United States Air Force Research Laboratory (AFRL, Albuquerque, NM) [F29601-02-1-0268]; Large Synoptic Survey Telescope (LSST) Corporation FX The Pan-STARRS1 Survey has been made possible through contributions of the Institute for Astronomy, the University of Hawai'i, the Pan-STARRS Project Office, the Max-Planck Society and its participating institutes, the Max Planck Institute for Astronomy, Heidelberg and the Max Planck Institute for Extraterrestrial Physics, Garching, The Johns Hopkins University, Durham University, the University of Edinburgh, Queen's University Belfast, the Harvard-Smithsonian Center for Astrophysics, and the Las Cumbres Observatory Global Telescope Network, Incorporated, the National Central University of Taiwan, and the National Aeronautics and Space Administration under Grant No. NNX08AR22G issued through the Planetary Science Division of the NASA Science Mission Directorate.; The design and construction of the Panoramic Survey Telescope and Rapid Response System by the University of Hawaii Institute for Astronomy was funded by the United States Air Force Research Laboratory (AFRL, Albuquerque, NM) through grant number F29601-02-1-0268.; We acknowledge the financial and technical contributions to this work made by the Large Synoptic Survey Telescope (LSST) Corporation team, in particular Tim Axelrod, Lynne Jones and Jeff Kantor. In addition, we acknowledge the support by Pan-STARRS and LSST management to enable and facilitate this productive collaborative effort between the two projects. NR 59 TC 30 Z9 30 U1 0 U2 5 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 APR PY 2013 VL 125 IS 926 BP 357 EP 395 DI 10.1086/670337 PG 39 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 131BM UT WOS:000317965800004 ER PT J AU Fleeger, CR Heaney, PJ Post, JE AF Fleeger, Claire R. Heaney, Peter J. Post, Jeffrey E. TI A time-resolved X-ray diffraction study of Cs exchange into hexagonal H-birnessite SO AMERICAN MINERALOGIST LA English DT Article DE Hexagonal birnessite; cesium; cation exchange; time-resolved X-ray diffraction ID SYNTHETIC NA-BIRNESSITE; MANGANESE OXIDE; POWDER DIFFRACTION; RIETVELD REFINEMENT; ION-EXCHANGE; HANFORD SITE; STRUCTURAL-CHARACTERIZATION; COMPETITIVE SORPTION; MN-OXIDES; ADSORPTION AB To measure the uptake of radioactive Cs in soils that are rich in Mn oxides, we applied time-resolved synchrotron X-ray diffraction (TR-XRD), inductively coupled plasma-mass spectrometry (ICP-MS), and analytical scanning electron microscopy (SEM) to determine the kinetics and mechanisms of aqueous Cs substitution in the phyllomanganate hexagonal H-birnessite at pH values ranging from 3 to 10. We observed that the rate of Cs cation exchange into hexagonal H-birnessite exhibited only a weak dependence on pH, but the total amount of Cs loading in the interlayer region increased dramatically above pH 6.5. The increase in Cs content at higher pH may be attributed to the increasingly negative charge on the Mn-O octahedral sheets and perhaps to a structural change toward triclinic symmetry with high pH. Dissolution at low pH may have inhibited Cs sequestration. Our work supports delamination-reassembly as a mechanism of cation exchange. C1 [Fleeger, Claire R.; Heaney, Peter J.] Penn State Univ, Dept Geosci, University Pk, PA 16802 USA. [Post, Jeffrey E.] Smithsonian Inst, Dept Mineral Sci, Washington, DC 20560 USA. RP Fleeger, CR (reprint author), PPG Ind Inc, 440 Coll Pk Dr, Monroeville, PA 15146 USA. EM cfleeger@ppg.com FU NSF-DOE Center for Environmental Kinetics Analysis (CEKA) Grant [CHE-0431328]; NSF [EAR07-45374, EAR11-47728]; U.S. Department of Energy, Office of Science, Office of Basic Energy Sciences [DE-AC02-06CH11357] FX Special thanks to Peter Eng and Nancy Lazarz at APS. Funding for this research was provided by the NSF-DOE Center for Environmental Kinetics Analysis (CEKA) Grant No. CHE-0431328 and NSF Grant No. EAR07-45374 and EAR11-47728. Use of the Advanced Photon Source was supported by the U.S. Department of Energy, Office of Science, Office of Basic Energy Sciences, under contract no. DE-AC02-06CH11357. NR 54 TC 6 Z9 6 U1 1 U2 31 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 APR PY 2013 VL 98 IS 4 BP 671 EP 679 DI 10.2138/am.2013.4287 PG 9 WC Geochemistry & Geophysics; Mineralogy SC Geochemistry & Geophysics; Mineralogy GA 123FG UT WOS:000317373200017 ER PT J AU Slotten, HR AF Slotten, Hugh Richard TI The International Telecommunications Union, Space Radio Communications, and U.S. Cold War Diplomacy, 1957-1963 SO DIPLOMATIC HISTORY LA English DT Article ID TECHNOLOGY; SCIENCE; SECURITY; WEAPON; STATE AB This article examines the role of the International Telecommunications Union (ITU), a specialized agency of the United Nations, in the international effort to manage the radio spectrum. The management of the radio spectrum has been one of the most important activities of the ITU. International agreements for the use of the radio spectrum have been necessary because radio waves do not simply stop at national borders. Governments have viewed the spectrum as an international common resource.Specifically, this article focuses on the development of radio spectrum policy for one of the most significant new radio "services" of the twentieth century: radio transmissions involving outer space. Crucial ITU administrative radio conferences in 1959 and 1963 organized especially by the United States laid the foundation for the Cold War space race. A focus on the efforts by the United States to manage the meetings is particularly important for gaining a deeper understanding of Cold War diplomacy and international relations during this crucial period. In the context of total cold war, diplomacy was closely linked to a broad range of national security concerns, not only military preparedness but also the symbolic and material struggle over hearts and minds. A central concern of the early efforts to arrive at international agreements for space frequencies was satellite communications. The United States was particularly concerned about convincing the international community to set aside large blocks of frequencies for a planned global satellite communications system that would serve multiple national security objectives. The global satellite system would, in turn, play an important role in convincing other countries to agree to set aside frequencies for all forms of space communication. C1 Smithsonian Inst Natl Air & Space Museum, Washington, DC USA. RP Slotten, HR (reprint author), Smithsonian Inst Natl Air & Space Museum, Washington, DC USA. NR 138 TC 4 Z9 4 U1 0 U2 12 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0145-2096 J9 DIPLOMATIC HIST JI Dipl. Hist. PD APR PY 2013 VL 37 IS 2 BP 313 EP 371 DI 10.1093/dh/dht014 PG 59 WC History SC History GA 113VM UT WOS:000316697400006 ER PT J AU Garcia-Pena, GE Sol, D Iwaniuk, AN Szekely, T AF Garcia-Pena, G. E. Sol, D. Iwaniuk, A. N. Szekely, T. TI Sexual selection on brain size in shorebirds (Charadriiformes) SO JOURNAL OF EVOLUTIONARY BIOLOGY LA English DT Review DE birds; body size evolution; Charadriidae; life histories; parental care; trade-off ID PARENTAL CARE; BREEDING SYSTEMS; SPERM COMPETITION; LIFE-HISTORY; SOCIAL BRAIN; R PACKAGE; EGG SIZE; EVOLUTION; BIRDS; CONFLICT AB Natural selection is considered a major force shaping brain size evolution in vertebrates, whereas the influence of sexual selection remains controversial. On one hand, sexual selection could promote brain enlargement by enhancing cognitive skills needed to compete for mates. On the other hand, sexual selection could favour brain size reduction due to trade-offs between investing in brain tissue and in sexually selected traits. These opposed predictions are mirrored in contradictory relationships between sexual selection proxies and brain size relative to body size. Here, we report a phylogenetic comparative analysis that highlights potential flaws in interpreting relative brain size-mating system associations as effects of sexual selection on brain size in shorebirds (Charadriiformes), a taxonomic group with an outstanding diversity in breeding systems. Considering many ecological effects, relative brain size was not significantly correlated with testis size. In polyandrous species, however, relative brain sizes of males and females were smaller than in monogamous species, and females had smaller brain size than males. Although these findings are consistent with sexual selection reducing brain size, they could also be due to females deserting parental care, which is a common feature of polyandrous species. Furthermore, our analyses suggested that body size evolved faster than brain size, and thus the evolution of body size may be confounding the effect of the mating system on relative brain size. The brain size-mating system association in shorebirds is thus not only due to sexual selection on brain size but rather, to body size evolution and other multiple simultaneous effects. C1 [Garcia-Pena, G. E.; Sol, D.] CREAF, Cerdanyola Del Valles, Spain. [Sol, D.] CSIC, Cerdanyola Del Valles, Spain. [Iwaniuk, A. N.] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA. [Iwaniuk, A. N.] Univ Lethbridge, Dept Neurosci, Canadian Ctr Behav Neurosci, Lethbridge, AB T1K 3M4, Canada. [Szekely, T.] Univ Bath, Dept Biol & Biochem, Bath BA2 7AY, Avon, England. RP Garcia-Pena, GE (reprint author), UAB, CREAF, Barcelona 08193, Spain. EM gegp01@gmail.com OI Sol, Daniel/0000-0001-6346-6949 FU Consejo Nacional de Ciencia y Tecnologia [CONACyT-121695-161552]; Proyecto de Investigacion [CGL2010-1838]; Consolider Project from the Ministerio de Educacion y Ciencia (Spain); ANI from the Smithsonian Office of Grants and Fellowships; NERC [NE/C004167/1] FX GEGP was supported by Consejo Nacional de Ciencia y Tecnologia (CONACyT-121695-161552). DS was supported by a Proyecto de Investigacion (CGL2010-1838) grant and a Consolider Project from the Ministerio de Educacion y Ciencia (Spain), ANI by a fellowship from the Smithsonian Office of Grants and Fellowships, and TS by NERC (NE/C004167/1). We thank the curators and technical staff of the Royal Alberta Museum (Edmonton, AB, Canada), Field Museum of Natural History (Chicago, IL, USA), National Museum of Natural History (Washington, DC, USA) and Melbourne Museum (Melbourne, Australia) for access to their collections. We thank Prof. Louis Lefebvre, Prof. Tadeusz Kawecki and an anonymous reviewer for their insightful comment on a previous version of the manuscript. NR 101 TC 8 Z9 8 U1 4 U2 58 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1010-061X J9 J EVOLUTION BIOL JI J. Evol. Biol. PD APR PY 2013 VL 26 IS 4 BP 878 EP 888 DI 10.1111/jeb.12104 PG 11 WC Ecology; Evolutionary Biology; Genetics & Heredity SC Environmental Sciences & Ecology; Evolutionary Biology; Genetics & Heredity GA 123ZR UT WOS:000317432700018 PM 23489329 ER PT J AU Labandeira, CC AF Labandeira, Conrad C. TI Deep-time patterns of tissue consumption by terrestrial arthropod herbivores SO NATURWISSENSCHAFTEN LA English DT Article DE Angiosperm diversification; Ecological lags; Fossil record; Functional feeding-groups; Land-plant tissues; Trophic partitioning ID EARLY EVOLUTION; LAND PLANTS; INSECT FOLIVORY; ASSOCIATIONS; TRACHEOPHYTES; POLLINATION; ANATOMY; ORIGIN AB A survey of the fossil record of land-plant tissues and their damage by arthropods reveals several results that shed light on trophic trends in host-plant resource use by arthropods. All 14 major plant tissues were present by the end of the Devonian, representing the earliest 20 % of the terrestrial biota. During this interval, two types of time lags separate the point between when tissues first originated from their earliest consumption by herbivorous arthropods. For epidermis, parenchyma, collenchyma and xylem, live tissue consumption was rapid, occurring on average 10 m.y. after the earliest tissue records. By contrast, structural tissues (periderm, sclerenchyma), tissues with actively dividing cells (apical, lateral, intercalary meristems), and reproductive tissues (spores, megagametophytes, integuments) experienced approximately a 9-fold (92 m.y.) delay in arthropod herbivory, extending well into the Carboniferous Period. Phloem similarly presents a delay of 85 m.y., but this incongruously long lag-time may be attributed to the lack of preservation of this tissue in early vascular plants. Nevertheless, the presence of phloem can be indicated from planar spaces adjacent well-preserved xylem, or inferred from a known anatomy of the same plant taxon in better preserved material, especially permineralisations. The trophic partitioning of epidermis, parenchyma, phloem and xylem increases considerably to the present, probably a consequence of dietary specialization or consumption of whole leaves by several herbivore functional feeding groups. Structural tissues, meristematic tissues and reproductive tissues minimally have been consumed throughout the fossil record, consistent with their long lags to herbivory during the earlier Paleozoic. Neither angiosperm dominance in floras nor global environmental perturbations had any discernible effect on herbivore trophic partitioning of plant tissues. C1 [Labandeira, Conrad C.] Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20013 USA. [Labandeira, Conrad C.] Rhodes Univ, Dept Geol, ZA-6140 Grahamstown, South Africa. [Labandeira, Conrad C.] Univ Maryland, Dept Entomol, College Pk, MD 20742 USA. [Labandeira, Conrad C.] Univ Maryland, BEES Program, College Pk, MD 20742 USA. RP Labandeira, CC (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, POB 37012, Washington, DC 20013 USA. EM labandec@si.edu NR 45 TC 15 Z9 15 U1 2 U2 41 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0028-1042 EI 1432-1904 J9 NATURWISSENSCHAFTEN JI Naturwissenschaften PD APR PY 2013 VL 100 IS 4 BP 355 EP 364 DI 10.1007/s00114-013-1035-4 PG 10 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 122WI UT WOS:000317348600007 PM 23525577 ER PT J AU Nagel, E D'Alessio, P Calvet, N Espaillat, C Trinidad, MA AF Nagel, Erick D'Alessio, Paola Calvet, Nuria Espaillat, Catherine Angel Trinidad, Miguel TI THE EFFECT OF SUBLIMATION TEMPERATURE DEPENDENCIES ON DISK WALLS AROUND T TAURI STARS SO REVISTA MEXICANA DE ASTRONOMIA Y ASTROFISICA LA English DT Article DE infrared: general; protoplanetary disks; stars: pre-main sequence ID HERBIG AE/BE STARS; YOUNG STELLAR OBJECTS; ACCRETION DISKS; PROTOPLANETARY DISKS; PLANET FORMATION; INNER DISKS; COKU TAU/4; GRAINS; DUST; AU AB The dust cannot survive closer to the star from the point where a grain reaches a temperature equal to the sublimation temperature. The boundary between a dust-free and a dusty region defines the sublimation wall. In the literature two models for the structure of the wall are used: a wall with a fixed sublimation temperature and a wall with a density-dependent sublimation temperature. In the former case, the wall is vertical and in the latter, the wall is curved. We find important differences between these models' SEDs in the wavelength range from 3 to 8 mu m, the emission of the former being larger than that of the latter model. We quantify the differences in IRAC colors when these models are used to explain the observations. In the IRAC color-color diagram ([3.6]-[4.5] vs. [5.8]-[8.0]), the models are located in specific regions, either depending on the inclination, the mass accretion rate, or the model used. C1 [Nagel, Erick; Angel Trinidad, Miguel] Univ Guanajuato, Dept Astron, Guanajuato 36240, Mexico. [D'Alessio, Paola] Univ Nacl Autonoma Mexico, Ctr Radioastron & Astrofis, Morelia 58090, Michoacan, Mexico. [Calvet, Nuria] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Espaillat, Catherine] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Nagel, E (reprint author), Univ Guanajuato, Dept Astron, Guanajuato 36240, Mexico. EM erick@astro.ugto.mx; p.dalessio@crya.unam.mx; ncal-vet@umich.edu; cespail-lat@cfa.harvard.edu; trinidad@astro.ugto.mx NR 41 TC 5 Z9 5 U1 0 U2 2 PU UNIV NACIONAL AUTONOMA MEXICO, INST DE ASTRONOMIA PI MEXICO CITY PA APDO POSTAL 70-264, MEXICO CITY 04510, MEXICO SN 0185-1101 J9 REV MEX ASTRON ASTR JI Rev. Mex. Astron. Astrofis. PD APR PY 2013 VL 49 IS 1 BP 43 EP 52 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 124AZ UT WOS:000317437500005 ER PT J AU Magnier, EA Schlafly, E Finkbeiner, D Juric, M Tonry, JL Burgett, WS Chambers, KC Flewelling, HA Kaiser, N Kudritzki, RP Morgan, JS Price, PA Sweeney, WE Stubbs, CW AF Magnier, E. A. Schlafly, E. Finkbeiner, D. Juric, M. Tonry, J. L. Burgett, W. S. Chambers, K. C. Flewelling, H. A. Kaiser, N. Kudritzki, R. -P. Morgan, J. S. Price, P. A. Sweeney, W. E. Stubbs, C. W. TI THE PAN-STARRS 1 PHOTOMETRIC REFERENCE LADDER, RELEASE 12.01 SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE catalogs; instrumentation: photometers; standards; surveys (PS1); techniques: photometric ID DIGITAL SKY SURVEY; CALIBRATION; PAN-STARRS1 AB As of 2012 January 21, the Pan-STARRS 1 3 pi Survey has observed the 3/4 of the sky visible from Hawaii with a minimum of 2 and mean of 7.6 observations in five filters, g(P1), r(P1), i(P1), z(P1), y(P1). Now at the end of the second year of the mission, we are in a position to make an initial public release of a portion of this unprecedented data set. This article describes the PS1 Photometric Ladder, Release 12.01. This is the first of a series of data releases to be generated as the survey coverage increases and the data analysis improves. The Photometric Ladder has rungs every hour in right ascension and at four intervals in declination. We will release updates with increased area coverage (more rungs) from the latest data set until the PS1 survey and the final re-reduction are completed. The currently released catalog presents photometry of similar to 1000 objects per square degree in the rungs of the ladder. Saturation occurs at g(P1), r(P1), i(P1) similar to 13.5; z(P1) similar to 13.0; and y(P1) similar to 12.0. Photometry is provided for stars down to g(P1), r(P1), i(P1) similar to 19.1 in the AB system. This data release depends on the rigid "Ubercal" photometric calibration using only the photometric nights, with systematic uncertainties of (8.0, 7.0, 9.0, 10.7, 12.4) mmag in (g(P1), r(P1), i(P1), z(P1), y(P1)). Areas covered only with lower quality nights are also included, and have been tied to the Ubercal solution via relative photometry; photometric accuracy of the non-photometric regions is lower and should be used with caution. C1 [Magnier, E. A.; Tonry, J. L.; Burgett, W. S.; Chambers, K. C.; Flewelling, H. A.; Kaiser, N.; Kudritzki, R. -P.; Morgan, J. S.; Sweeney, W. E.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Schlafly, E.; Finkbeiner, D.; Juric, M.; Stubbs, C. W.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Schlafly, E.] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Price, P. A.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. RP Magnier, EA (reprint author), Univ Hawaii, Inst Astron, 2680 Woodlawn Dr, Honolulu, HI 96822 USA. RI Stubbs, Christopher/C-2829-2012; OI Stubbs, Christopher/0000-0003-0347-1724; Schlafly, Edward Ford/0000-0002-3569-7421; Chambers, Kenneth /0000-0001-6965-7789 FU National Aeronautics and Space Administration through the Planetary Science Division of the NASA Science Mission Directorate [NNX08AR22G]; National Science Foundation [AST-1009749, AST-1238877] FX The Pan-STARRS 1 Survey has been made possible through contributions of the Institute for Astronomy; the University of Hawaii; the Pan-STARRS Project Office; the Max-Planck Society and its participating institutes, the Max Planck Institute for Astronomy, Heidelberg and the Max Planck Institute for Extraterrestrial Physics, Garching; The Johns Hopkins University; Durham University; the University of Edinburgh; Queen's University Belfast; the Harvard-Smithsonian Center for Astrophysics; and the Las Cumbres Observatory Global Telescope Network, Incorporated; the National Central University of Taiwan; and the National Aeronautics and Space Administration under Grant No. NNX08AR22G issued through the Planetary Science Division of the NASA Science Mission Directorate. Partial support for this work was provided by National Science Foundation grant AST-1009749 and AST-1238877. NR 19 TC 72 Z9 72 U1 0 U2 4 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 APR PY 2013 VL 205 IS 2 AR 20 DI 10.1088/0067-0049/205/2/20 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 118PL UT WOS:000317037600010 ER PT J AU Tang, YZ Zeiner, CA Santelli, CM Hansel, CM AF Tang, Yuanzhi Zeiner, Carolyn A. Santelli, Cara M. Hansel, Colleen M. TI Fungal oxidative dissolution of the Mn(II)-bearing mineral rhodochrosite and the role of metabolites in manganese oxide formation SO ENVIRONMENTAL MICROBIOLOGY LA English DT Article ID BIOGENIC MN OXIDES; SP STRAIN SG-1; MN(II) OXIDATION; PHANEROCHAETE-CHRYSOSPORIUM; HUMIC SUBSTANCES; NADPH OXIDASES; IRON; METALLOGENIUM; BACTERIA; SUPEROXIDE AB Microbially mediated oxidation of Mn(II) to Mn(III/IV) oxides influences the cycling of metals and remineralization of carbon. Despite the prevalence of Mn(II)-bearing minerals in nature, little is known regarding the ability of microbes to oxidize mineral-hosted Mn(II). Here, we explored oxidation of the Mn(II)-bearing mineral rhodochrosite (MnCO3) and characteristics of ensuing Mn oxides by six Mn(II)-oxidizing Ascomycete fungi. All fungal species substantially enhanced rhodochrosite dissolution and surface modification. Mineral-hosted Mn(II) was oxidized resulting in formation of Mn(III/IV) oxides that were all similar to -MnO2 but varied in morphology and distribution in relation to cellular structures and the MnCO3 surface. For four fungi, Mn(II) oxidation occurred along hyphae, likely mediated by cell wall-associated proteins. For two species, Mn(II) oxidation occurred via reaction with fungal-derived superoxide produced at hyphal tips. This pathway ultimately resulted in structurally unique Mn oxide clusters formed at substantial distances from any cellular structure. Taken together, findings for these two fungi strongly point to a role for fungal-derived organic molecules in Mn(III) complexation and Mn oxide templation. Overall, this study illustrates the importance of fungi in rhodochrosite dissolution, extends the relevance of biogenic superoxide-based Mn(II) oxidation and highlights the potential role of mycogenic exudates in directing mineral precipitation. C1 [Tang, Yuanzhi; Zeiner, Carolyn A.; Hansel, Colleen M.] Harvard Univ, Sch Engn & Appl Sci, Cambridge, MA 02138 USA. [Santelli, Cara M.] Smithsonian Inst, Natl Museum Nat Hist, Dept Mineral Sci, Washington, DC 20560 USA. RP Hansel, CM (reprint author), Woods Hole Oceanog Inst, Marine Chem & Geochem Dept, Woods Hole, MA 02543 USA. EM chansel@whoi.edu RI Tang, Yuanzhi/G-5419-2013; OI Santelli, Cara/0000-0001-8617-0008 FU Department of Energy, Office of Biological and Environmental Research; National Institutes of Health, National Center for Research Resources, Biomedical Technology Program; US Department of Energy, Office of Science, Office of Basic Energy Sciences [DE-AC02-98CH10886]; National Science Foundation under NSF Award [ECS-0335765]; National Science Foundation [EAR-0846715] FX The authors thank Adiari I. V~zquez-Rodr~guez for help with thin section preparation, Christopher Lentini and Emily Estes for help with EXAFS data collection, Sam Webb (SSRL) for support on beamline 2-3, and Alice Dohnalkova (EMSL) for assistance in TEM collection. The authors also thank Associate Editor Victoria Orphan and the anonymous reviewers for their helpful suggestions. Portions of this research were conducted at the Stanford Synchrotron Radiation Lightsource (SSRL), the National Synchrotron Light Source (NSLS), the Center for Nanoscale Systems (CNS) at Harvard University and the Environmental Molecular Sciences Lab (EMSL). SSRL is a national user facility operated by Stanford University on behalf of the US Department of Energy, Office of Basic Energy Sciences. The SSRL Structural Molecular Biology Program is supported by the Department of Energy, Office of Biological and Environmental Research and by the National Institutes of Health, National Center for Research Resources, Biomedical Technology Program. NSLS is supported by the US Department of Energy, Office of Science, Office of Basic Energy Sciences, under Contract No. DE-AC02-98CH10886. CNS is a member of the National Nanotechnology Infrastructure Network (NNIN), which is supported by the National Science Foundation under NSF Award No. ECS-0335765. CNS is part of the Faculty of Arts and Sciences at Harvard University. EMSL is a national scientific user facility sponsored by the Department of Energy's Office of Biological and Environmental Research located at Pacific Northwest National Laboratory. This project was funded by the National Science Foundation, Grant Number EAR-0846715, awarded to C. M. H. NR 78 TC 13 Z9 17 U1 6 U2 80 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1462-2912 J9 ENVIRON MICROBIOL JI Environ. Microbiol. PD APR PY 2013 VL 15 IS 4 BP 1063 EP 1077 DI 10.1111/1462-2920.12029 PG 15 WC Microbiology SC Microbiology GA 122AM UT WOS:000317287200007 PM 23157705 ER PT J AU Dennenmoser, S Christy, JH AF Dennenmoser, Stefan Christy, John H. TI THE DESIGN OF A BEAUTIFUL WEAPON: COMPENSATION FOR OPPOSING SEXUAL SELECTION ON A TRAIT WITH TWO FUNCTIONS SO EVOLUTION LA English DT Article DE Biomechanics; claw; fiddler crab; secondary sexual trait compensation; sexual selection ID FIDDLER-CRABS UCA; MALE COMPETITION; TAIL STREAMERS; WAVING DISPLAY; FEMALE CHOICE; CLOSING FORCE; BARN SWALLOW; MATE CHOICE; CLAW SIZE; BODY-SIZE AB Male fiddler crabs, genus Uca, have one greatly enlarged claw with which they court females and threaten and fight other males. Longer claws are more effective signals but are thought to be less effective weapons because the relative closing force at the tip of the claw decreases with claw length. We studied claw morphology and fighting in Uca terpsichores and Uca beebei and found a mechanism that may resolve opposing selection for signaling and fighting ability. When males fought they delivered gripping forces not at the tips but at the tubercles on the inner margins of their claws' fingers. As claws grow, these tubercles remain relatively close to the apex of the gape. Consequently, the mechanical advantage that governs the forces that can be delivered at these tubercles decreases only slightly with increasing claw length allowing the claw to be an effective signal and a powerful weapon. Animal weapons are exceptionally diverse in form and detail of armature and the causes of this diversity are poorly understood. We suggest that the designs of weapons may often reflect compensatory patterns of growth and placement of armature that enhances the weapon's overall utility for multiple uses in competition for mates. C1 [Dennenmoser, Stefan] Univ Calgary, Dept Biol Sci, Calgary, AB T2N 1N4, Canada. [Christy, John H.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. RP Dennenmoser, S (reprint author), Univ Calgary, Dept Biol Sci, 2500 Univ Dr 1 NW, Calgary, AB T2N 1N4, Canada. EM christyj@si.edu FU Smithsonian Tropical Research Institute FX We thank the Smithsonian Tropical Research Institute for financial and logistical support, Taewon Kim for field assistance, and Brook Swanson for comments on an earlier version of this paper. We also thank the Unidad Administrativa de Bienes Revertidos of the Ministerio de Economia y Finanzas, the Servicio Nacional Aeronaval, and the Autoridad del Canal de Panama, Republic of Panama, for permission to access to the old Rodman Naval Base and its adjacent tidal flats on the west bank of the Panama Canal. NR 60 TC 18 Z9 18 U1 6 U2 64 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0014-3820 EI 1558-5646 J9 EVOLUTION JI Evolution PD APR PY 2013 VL 67 IS 4 BP 1181 EP 1188 DI 10.1111/evo.12018 PG 8 WC Ecology; Evolutionary Biology; Genetics & Heredity SC Environmental Sciences & Ecology; Evolutionary Biology; Genetics & Heredity GA 119XT UT WOS:000317133800021 PM 23550765 ER PT J AU Angelier, F Vleck, CM Holberton, RL Marra, PP AF Angelier, Frederic Vleck, Carol M. Holberton, Rebecca L. Marra, Peter P. TI Telomere length, non-breeding habitat and return rate in male American redstarts SO FUNCTIONAL ECOLOGY LA English DT Article DE American redstart; habitat; Setophaga ruticilla; survival; telomere dynamics ID DISTANCE MIGRATORY BIRD; LONG-LIVED BIRDS; NONBREEDING SEASON; LIFE-SPAN; SETOPHAGA-RUTICILLA; OXIDATIVE STRESS; QUANTITATIVE PCR; DYNAMICS; CANCER; WILD AB Telomeres are long repetitive noncoding sequences of DNA located at the ends of chromosomes. Recently, the study of telomere dynamics has been increasingly used to investigate ecological questions. However, little is currently known about the relationships that link environmental conditions, telomere dynamics and fitness in wild vertebrates. Using a small migratory bird (American redstart, Setophaga ruticilla), we investigated how telomere dynamics can be affected by non-breeding habitat quality and to what extent telomere length can predict the return rate of males. We show that telomeres shorten in most individuals over a 1-year period and, importantly, that telomeres of individuals wintering in a low-quality habitat shorten more than those of individuals wintering in a high-quality habitat. In addition, we found that longer telomeres are associated with a higher return rate than shorter telomeres, although the relationship between return rate and telomere length did not depend on habitat quality. Our study suggests that telomere dynamics are affected by environmental conditions and are related to indices of fitness in a migratory bird species. C1 [Angelier, Frederic; Marra, Peter P.] Smithsonian Inst, Natl Zool Pk, Migratory Bird Ctr, Smithsonian Conservat Biol Inst, Washington, DC 20008 USA. [Angelier, Frederic] CNRS, Ctr Etud Biol Chize, F-79360 Villiers En Bois, France. [Angelier, Frederic; Vleck, Carol M.] Iowa State Univ, Dept Ecol Evolut & Organismal Biol, Ames, IA 50011 USA. [Holberton, Rebecca L.] Univ Maine, Dept Biol Sci, Orono, ME 04469 USA. RP Angelier, F (reprint author), Smithsonian Inst, Natl Zool Pk, Migratory Bird Ctr, Smithsonian Conservat Biol Inst, 3001 Connecticut Ave, Washington, DC 20008 USA. EM angelier@cebc.cnrs.fr FU NSF [0717338, 0649679]; European Community [237034] FX This study was supported by NSF grants to P. P. Marra (0717338 and 0649679) and R. L. Holberton (0717338). F. Angelier was supported by the 7th research programme of the European Community FP7/2007-2013 (Marie-Curie Fellowship, no 237034). We are very grateful to J. Serb from Iowa State University for her help in the optimization of the primers and to N. Valenzuela for her help with the use of the qPCR equipment. We thank E. Corliss, J. L. Dowling, J. H. Junda, S. R. Sult, M. A. Thomas and C. M. Tonra for their assistance in the field and M. Shultz for his help in the laboratory. We thank N. Metcalfe, D. Vleck, M. Shultz and C. Foote for their comments on a previous version of the manuscript. We thank the Petroleum Corporation of Jamaica for permission to conduct this research at the Font Hill Nature Preserve and Yvette Strong and Andrea Donaldson of the Jamaica National Environmental Planning Agency for their cooperation. NR 52 TC 22 Z9 22 U1 6 U2 61 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0269-8463 EI 1365-2435 J9 FUNCT ECOL JI Funct. Ecol. PD APR PY 2013 VL 27 IS 2 BP 342 EP 350 DI 10.1111/1365-2435.12041 PG 9 WC Ecology SC Environmental Sciences & Ecology GA 122GJ UT WOS:000317306000007 ER PT J AU Brenes-Arguedas, T Roddy, AB Kursar, TA AF Brenes-Arguedas, Tania Roddy, Adam B. Kursar, Thomas A. TI Plant traits in relation to the performance and distribution of woody species in wet and dry tropical forest types in Panama SO FUNCTIONAL ECOLOGY LA English DT Article DE biomass allocation; defence; drought tolerance; photosynthesis; plasticity; rainfall gradient; shade tolerance; trade-offs; tropical forest ID CARBON-ISOTOPE DISCRIMINATION; FUNCTIONAL TRAITS; SHADE TOLERANCE; TREE SEEDLINGS; PHOTOSYNTHETIC CAPACITY; HABITAT SPECIALIZATION; DESICCATION TOLERANCE; DROUGHT PERFORMANCE; LIGHT REQUIREMENTS; CLIMATIC GRADIENT AB Understanding the factors that limit species distributions along environmental gradients is a central question of ecology. Here, we evaluate the hypothesis that the traits that result in performance trade-offs between habitats contribute to the turnover of woody species along a rainfall gradient in the Isthmus of Panama. We studied 24 plant species with contrasting distributions along this rainfall gradient. We measured 18 morphological and physiological traits, and three performance variables in seedlings planted in common garden experiments in two contrasting sites across the Isthmus. We found evidence for a trade-off suggesting that better survival during the dry season corresponded to a lower growth rate in the forest understorey. This trade-off correlated well with the distribution of the species along the rainfall gradient and was explained mostly by variation in photosynthetic capacity. While not all species fit into this trade-off, most dry-distribution species, which we had previously reported to have higher drought survival, were associated with higher stem hydraulic conductance and higher capacity for CO2 assimilation. Our interpretation is that this combination of traits may be associated mostly with desiccation avoidance (deep roots) or desiccation delay (deciduousness) rather than desiccation tolerance. Despite their higher photosynthetic capacity, these species had lower growth in the low-light understorey, probably because of higher maintenance costs (dark respiration rates). Wet-distribution species, on the other hand, had lower photosynthetic capacity and higher leaf area ratio. This strategy is typical of shade-tolerant species and may explain their higher growth rates in the low-light understorey. In conclusion, our results suggest that habitat associations along the rainfall gradient in the Isthmus of Panama may result in part from a trade-off between traits that are favourable to species that avoid or delay desiccation but that otherwise limit shade tolerance. This trade-off may limit the capacity of some dry-distribution species to colonize wet forests. C1 [Brenes-Arguedas, Tania; Kursar, Thomas A.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. [Roddy, Adam B.] Univ Calif Berkeley, Dept Integrat Biol, Berkeley, CA 94720 USA. [Kursar, Thomas A.] Univ Utah, Dept Biol, Salt Lake City, UT 84112 USA. RP Kursar, TA (reprint author), Smithsonian Trop Res Inst, POB 0843-03092, Balboa, Ancon, Panama. EM kursar@biology.utah.edu RI Roddy, Adam/M-4523-2013 OI Roddy, Adam/0000-0002-4423-8729 FU National Science Foundation [DEB-0444590] FX Funding was provided by the National Science Foundation grant DEB-0444590 to TAK and PD Coley. We thank Cecilia Blundo, Marcos Rios, Gonzalo Rivas, Natalia Anaya and Lissette Jimenez who conducted the field and laboratory work; Salomon Aguilar and Rolando Perez helped with species identification. The Smithsonian Tropical Research Institute's Center for Tropical Forest Science, the Missouri Botanical Gardens and In-Bio made species information, herbarium and distribution maps available. The Peregrine Fund kindly allowed us to access Gunn Hill. The Smithsonian Tropical Research Institute provided logistical support and research facilities. We acknowledge constructive comments from three anonymous reviewers. All work was done in compliance with the laws of Panama and the Autoridad Nacional del Ambiente. NR 59 TC 10 Z9 10 U1 7 U2 127 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0269-8463 J9 FUNCT ECOL JI Funct. Ecol. PD APR PY 2013 VL 27 IS 2 BP 392 EP 402 DI 10.1111/1365-2435.12036 PG 11 WC Ecology SC Environmental Sciences & Ecology GA 122GJ UT WOS:000317306000012 ER PT J AU Wang, HQ Richardson, MI Toigo, AD Newman, CE AF Wang, Huiqun Richardson, Mark I. Toigo, Anthony D. Newman, Claire E. TI Zonal wavenumber three traveling waves in the northern hemisphere of Mars simulated with a general circulation model SO ICARUS LA English DT Article DE Atmospheres, Dynamics; Mars; Mars, Atmosphere ID MARTIAN DUST CYCLE; WATER ICE CLOUDS; GLOBAL SURVEYOR; SPECTRAL-ANALYSIS; ORBITER CAMERA; ATMOSPHERE; STORMS; DYNAMICS; SURFACE; EDDIES AB Observations suggest a strong correlation between curvilinear shaped traveling dust storms (observed in wide angle camera images) and eastward traveling zonal wave number m = 3 waves (observed in thermal data) in the northern mid and high latitudes during the fall and winter. Using the MarsWRF General Circulation Model, we have investigated the seasonality, structure and dynamics of the simulated m = 3 traveling waves and tested the hypothesis that traveling dust storms may enhance m = 3 traveling waves under certain conditions. Our standard simulation using a prescribed "MGS dust scenario" can capture the observed major wave modes and strong near surface temperature variations before and after the northern winter solstice. The same seasonal pattern is also shown by the simulated near surface meridional wind, but not by the normalized surface pressure. The simulated eastward traveling 1.4 < T < 10 sol m = 3 waves are confined near the surface in terms of the temperature perturbation, EP flux and eddy available potential energy, and they extend higher in terms of the eddy winds and eddy kinetic energy. The signature of the simulated m = 3 traveling waves is stronger in the near surface meridional wind than in the near surface temperature field. Compared with the standard simulation, our test simulations show that the prescribed m = 3 traveling dust blobs can enhance the simulated m = 3 traveling waves during the pre- and post-solstice periods when traveling dust storms are frequently observed in images, and that they have negligible effect during the northern winter solstice period when traveling dust storms are absent. The enhancement is even greater in our simulation when dust is concentrated closer to the surface. Our simulations also suggest that dust within the 45-75 degrees N band is most effective at enhancing the simulated m = 3 traveling waves. There are multiple factors influencing the strength of the simulated m = 3 traveling waves. Among those, our study suggests that weaker near surface static stability, larger near surface baroclinic parameter, and wave-form dust forcing for latitudinally extended dust storms are favorable. Further study is needed to fully understand the importance of these factors and others. (C) 2013 Elsevier Inc. All rights reserved. C1 [Wang, Huiqun] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Richardson, Mark I.; Newman, Claire E.] Ashima Res, Pasadena, CA 91101 USA. [Toigo, Anthony D.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. RP Wang, HQ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM hwang@cfa.harvard.edu FU NASA Planetary Atmosphere program FX This paper is supported by the NASA Planetary Atmosphere program. The computations in this paper were run on the Odyssey cluster supported by the FAS Science Division Research Computing Group at Harvard University. Reviews by John Wilson and an anonymous reviewer have helped to improve this paper. NR 52 TC 8 Z9 8 U1 0 U2 10 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 APR PY 2013 VL 223 IS 2 BP 654 EP 676 DI 10.1016/j.icarus.2013.01.004 PG 23 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 116ZZ UT WOS:000316923200003 ER PT J AU Fernandez-Marin, H Bruner, G Gomez, EB Nash, DR Boomsma, JJ Wcislo, WT AF Fernandez-Marin, Hermogenes Bruner, Gaspar Gomez, Ernesto B. Nash, David R. Boomsma, Jacobus J. Wcislo, William T. TI Dynamic Disease Management in Trachymyrmex Fungus-Growing Ants (Attini: Formicidae) SO AMERICAN NATURALIST LA English DT Article DE metapleural glands; fungal symbiont; hygiene; grooming; weeding; Actinomycetales; Attini; Escovopsis ID LEAF-CUTTING ANT; METAPLEURAL GLAND SECRETION; MICROBE SYMBIOSIS; GENETIC DIVERSITY; ACROMYRMEX-OCTOSPINOSUS; MUTUALISTIC BACTERIUM; FILAMENTOUS BACTERIA; NEST ESTABLISHMENT; SOCIAL IMMUNITY; TRADE-OFF AB Multipartner mutualisms have potentially complex dynamics, with compensatory responses when one partner is lost or relegated to a minor role. Fungus-growing ants (Attini) are mutualistic associates of basidiomycete fungi and antibiotic-producing actinomycete bacteria; the former are attacked by specialized fungi (Escovopsis) and diverse generalist microbes. Ants deploy biochemical defenses from bacteria and metapleural glands (MGs) and express different behaviors to control contaminants. We studied four Trachymyrmex species that differed in relative abundance of actinomycetes to understand interactions among antimicrobial tactics that are contingent on the nature of infection. MG grooming rate and actinomycete abundance were negatively correlated. The two species with high MG grooming rates or abundant actinomycetes made relatively little use of behavioral defenses. Conversely, the two species with relatively modest biochemical defenses relied heavily on behavior. Trade-offs suggest that related species can evolutionarily diverge to rely on different defense mechanisms against the same threat. Neither bacterial symbionts nor MG secretions thus appear to be essential for mounting defenses against the specialized pathogen Escovopsis, but reduced investment in one of these defense modes tends to increase investment in the other. C1 [Fernandez-Marin, Hermogenes; Bruner, Gaspar; Gomez, Ernesto B.; Wcislo, William T.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. [Fernandez-Marin, Hermogenes; Nash, David R.; Boomsma, Jacobus J.] Univ Copenhagen, Dept Biol, Ctr Social Evolut, DK-2100 Copenhagen, Denmark. RP Fernandez-Marin, H (reprint author), Inst Invest Cient & Serv Alta Tecnol, Edificio 219, Panama City, Panama. EM fernandezh@si.edu; wcislow@si.edu RI Nash, David/B-2916-2009; Nash, David/H-4433-2012; Boomsma, Jacobus/M-2785-2014 OI Nash, David/0000-0002-0462-6794; Nash, David/0000-0002-0462-6794; Boomsma, Jacobus/0000-0002-3598-1609 FU Secretaria Nacional de Ciencia, Tecnologia y Innovacion (SENACYT; Becas, Republica de Panama); Secretaria Nacional de Ciencia, Tecnologia y Innovacion (SENACYT; International Collaboration Program) [COL09-038]; Smithsonian Tropical Research Institute (STRI); Centre for Social Evolution, Department of Biology, University of Copenhagen; Adelante Internship program at STRI; Danish National Research Foundation [DNRF57] FX We thank S. Dreier, two anonymous reviewers, and J. Tewksbury for comments and suggestions to improve earlier drafts. This work was supported by postdoctoral fellowships from the Secretaria Nacional de Ciencia, Tecnologia y Innovacion (SENACYT; Becas 2005-2010, Republica de Panama; and the International Collaboration Program, COL09-038) and the Smithsonian Tropical Research Institute (STRI) and funding from the Centre for Social Evolution, Department of Biology, University of Copenhagen to H.F.-M. Additional support was provided by general research funds from STRI to W.T.W. E.B.G. and G.B. were sponsored by the Adelante Internship program at STRI via W.T.W. J.J.B. and D.R.N. were supported by a grant from the Danish National Research Foundation (DNRF57). We thank the Autoridad Nacional del Ambiente for research and collecting permits and STRI staff for logistic support. NR 73 TC 13 Z9 13 U1 5 U2 73 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0003-0147 J9 AM NAT JI Am. Nat. PD APR PY 2013 VL 181 IS 4 BP 571 EP 582 DI 10.1086/669664 PG 12 WC Ecology; Evolutionary Biology SC Environmental Sciences & Ecology; Evolutionary Biology GA 115FE UT WOS:000316797200014 PM 23535621 ER PT J AU Detto, M Muller-Landau, HC AF Detto, Matteo Muller-Landau, Helene C. TI Fitting Ecological Process Models to Spatial Patterns Using Scalewise Variances and Moment Equations SO AMERICAN NATURALIST LA English DT Article DE moment equations; spatial logistic model; spectral analysis; negative density dependence; spatial patterns; wavelet variance ID WAVELET ANALYSIS; POPULATION-DYNAMICS; STATISTICAL-INFERENCE; HABITAT ASSOCIATIONS; DENSITY-DEPENDENCE; PLANT-COMMUNITIES; SPECTRAL-ANALYSIS; TROPICAL FORESTS; POINT-PROCESSES; TIME-SERIES AB Ecological spatial patterns are structured by a multiplicity of processes acting over a wide range of scales. We propose a new method, based on the scalewise variance-that is, the variance as a function of spatial scale, calculated here with wavelet kernel functions-to disentangle the signature of processes that act at different and similar scales on observed spatial patterns. We derive exact and approximate analytical solutions for the expected scalewise variance under different individual-based, spatially explicit models for sessile organisms (e.g., plants), using moment equations. We further determine the probability distribution of independently observed scalewise variances for a given expectation, including complete spatial randomness. Thus, we provide a new analytical test of the null model of spatial randomness to understand at which scales, if any, the variance departs significantly from randomness. We also derive the likelihood function that is needed to estimate parameters of spatial models and their uncertainties from observed patterns. The methods are demonstrated through numerical examples and case studies of four tropical tree species on Barro Colorado Island, Panama. The methods developed here constitute powerful new tools for investigating effects of ecological processes on spatial point patterns and for statistical inference of process models from spatial patterns. C1 [Detto, Matteo; Muller-Landau, Helene C.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. RP Detto, M (reprint author), Smithsonian Trop Res Inst, Apartado Postal 0843-03092, Balboa, Ancon, Panama. EM dettom@si.edu FU Smithsonian Institution Global Earth Observatories; National Science Foundation [DEB-0640386, DEB-0425651, DEB-0346488, DEB-0129874, DEB-00753102, DEB-9909347, DEB-9615226, DEB-9405933, DEB-9221033, DEB-9100058, DEB-8906869, DEB-8605042, DEB-8206992, DEB-7922197]; Center for Tropical Forest Science; Smithsonian Tropical Research Institute; John D. and Catherine T. MacArthur Foundation; Mellon Foundation; Small World Institute Fund FX We gratefully acknowledge the financial support of the Smithsonian Institution Global Earth Observatories, and we thank R. Condit and S. Hubbell for providing the Barro Colorado Island tree data and J. Calabrese and R. Chrislom for useful comments. The Barro Colorado Island forest dynamics research project was made possible by National Science Foundation grants to S. P. Hubbell (DEB-0640386, DEB-0425651, DEB-0346488, DEB-0129874, DEB-00753102, DEB-9909347, DEB-9615226, DEB-9615226, DEB-9405933, DEB-9221033, DEB-9100058, DEB-8906869, DEB-8605042, DEB-8206992, and DEB-7922197), support from the Center for Tropical Forest Science, the Smithsonian Tropical Research Institute, the John D. and Catherine T. MacArthur Foundation, the Mellon Foundation, and the Small World Institute Fund. NR 52 TC 15 Z9 15 U1 0 U2 48 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0003-0147 J9 AM NAT JI Am. Nat. PD APR PY 2013 VL 181 IS 4 BP E68 EP E82 DI 10.1086/669678 PG 15 WC Ecology; Evolutionary Biology SC Environmental Sciences & Ecology; Evolutionary Biology GA 115FE UT WOS:000316797200001 PM 23535623 ER PT J AU Andrade-Santos, F Nulsen, PEJ Kraft, RP Forman, WR Jones, C Churazov, E Vikhlinin, A AF Andrade-Santos, Felipe Nulsen, Paul E. J. Kraft, Ralph P. Forman, William R. Jones, Christine Churazov, Eugene Vikhlinin, Alexey TI DARK MATTER SUBHALOS AND THE X-RAY MORPHOLOGY OF THE COMA CLUSTER SO ASTROPHYSICAL JOURNAL LA English DT Article DE dark matter; galaxies: clusters: individual (A1656); galaxies: clusters: intracluster medium; large-scale structure of universe; X-rays: galaxies: clusters ID XMM-NEWTON OBSERVATION; THERMAL CONDUCTION; SKY SURVEY; GALAXIES; MASS; SUBSTRUCTURE; SIMULATIONS; EVOLUTION; CHANDRA; HALOES AB Structure formation models predict that clusters of galaxies contain numerous massive subhalos. The gravity of a subhalo in a cluster compresses the surrounding intracluster gas and enhances its X-ray emission. We present a simple model, which treats subhalos as slow moving and gasless, for computing this effect. Recent weak lensing measurements by Okabe et al. have determined masses of similar to 10(13) M-circle dot for three mass concentrations projected within 300 kpc of the center of the Coma Cluster, two of which are centered on the giant elliptical galaxies NGC 4889 and NGC 4874. Adopting a smooth spheroidal beta-model for the gas distribution in the unperturbed cluster, we model the effect of these subhalos on the X-ray morphology of the Coma Cluster, comparing our results to Chandra and XMM-Newton X-ray data. The agreement between the models and the X-ray morphology of the central Coma Cluster is striking. With subhalo parameters from the lensing measurements, the distances of the three subhalos from the Coma Cluster midplane along our line of sight are all tightly constrained. Using the model to fit the subhalo masses for NGC 4889 and NGC 4874 gives 9.1 x 10(12) M-circle dot and 7.6 x 10(12) M-circle dot, respectively, in good agreement with the lensing masses. These results lend strong support to the argument that NGC 4889 and NGC 4874 are each associated with a subhalo that resides near the center of the Coma Cluster. In addition to constraining the masses and 3-d location of subhalos, the X-ray data show promise as a means of probing the structure of central subhalos. C1 [Andrade-Santos, Felipe; Nulsen, Paul E. J.; Kraft, Ralph P.; Forman, William R.; Jones, Christine; Vikhlinin, Alexey] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Andrade-Santos, Felipe] Univ Sao Paulo, Dept Astron IAG, Sao Paulo, Brazil. [Churazov, Eugene] Max Planck Inst Astrophys, D-85741 Garching, Germany. RP Andrade-Santos, F (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Churazov, Eugene/A-7783-2013; OI Nulsen, Paul/0000-0003-0297-4493; Forman, William/0000-0002-9478-1682 FU Chandra [AR7-8013X]; NASA [NAS8-03060, NNX11AF76G]; FAPESP [2008/05970-0] FX We thank R. Johnson for useful discussions. The work was supported in part by Chandra Grant AR7-8013X, NASA grant NAS8-03060, FAPESP grant 2008/05970-0, and NASA grant NNX11AF76G. NR 31 TC 11 Z9 11 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD APR 1 PY 2013 VL 766 IS 2 AR 107 DI 10.1088/0004-637X/766/2/107 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 108UE UT WOS:000316320900041 ER PT J AU Burke, MJ Raychaudhury, S Kraft, RP Maccarone, TJ Brassington, NJ Hardcastle, MJ Kainulainen, J Woodley, KA Goodger, JL Sivakoff, GR Forman, WR Jones, C Murray, SS Birkinshaw, M Croston, JH Evans, DA Gilfanov, M Jordan, A Sarazin, CL Voss, R Worrall, DM Zhang, ZL AF Burke, Mark J. Raychaudhury, Somak Kraft, Ralph P. Maccarone, Thomas J. Brassington, Nicola J. Hardcastle, Martin J. Kainulainen, Jouni Woodley, Kristin A. Goodger, Joanna L. Sivakoff, Gregory R. Forman, William R. Jones, Christine Murray, Stephen S. Birkinshaw, Mark Croston, Judith H. Evans, Daniel A. Gilfanov, Marat Jordan, Andres Sarazin, Craig L. Voss, Rasmus Worrall, Diana M. Zhang, Zhongli TI SPECTRAL PROPERTIES OF X-RAY BINARIES IN CENTAURUS A SO ASTROPHYSICAL JOURNAL LA English DT Article DE black hole physics; galaxies: elliptical and lenticular, cD; galaxies: individual (Centaurus A, NGC 5128); X-rays: binaries; X-rays: galaxies ID DISC INSTABILITY MODEL; BLACK-HOLE ACCRETION; EARLY-TYPE GALAXIES; GLOBULAR-CLUSTER; LUMINOSITY FUNCTION; PARTICLE-ACCELERATION; NEUTRON-STAR; NGC 5128; OBSERVATIONAL APPEARANCE; MASS-DISTRIBUTION AB We present a spectral investigation of X-ray binaries (XBs) in NGC 5128 (Cen A), using six 100 ks Chandra observations taken over two months in 2007. We divide our sample into thermally and non-thermally dominated states based on the behavior of the fitted absorption column N-H, and present the spectral parameters of sources with L-x greater than or similar to 2 x 10(37) erg s(-1). The majority of sources are consistent with being neutron star low-mass X-ray binaries (NS LMXBs) and we identify three transient black hole (BH) LMXB candidates coincident with the dust lane, which is the remnant of a small late-type galaxy. Our results also provide tentative support for the apparent "gap" in the mass distribution of compact objects between similar to 2-5M(circle dot). We propose that BH LMXBs are preferentially found in the dust lane, and suggest this is because of the younger stellar population. The majority (similar to 70%-80%) of potential Roche lobe filling donors in the Cen A halo are greater than or similar to 12 Gyr old, while BH LMXBs require donors greater than or similar to 1 M-circle dot to produce the observed peak luminosities. This requirement for more massive donors may also explain recent results that claim a steepening of the X-ray luminosity function with age at L-x >= 5 x 10(38) erg s(-1) for the XB population of early-type galaxies; for older stellar populations, there are fewer stars greater than or similar to 1 M-circle dot, which are required to form the more luminous sources. C1 [Burke, Mark J.; Raychaudhury, Somak] Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England. [Burke, Mark J.; Kraft, Ralph P.; Forman, William R.; Jones, Christine; Murray, Stephen S.; Birkinshaw, Mark; Evans, Daniel A.; Jordan, Andres; Worrall, Diana M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Raychaudhury, Somak] Presidency Univ, Dept Phys, Kolkata 700073, India. [Maccarone, Thomas J.; Croston, Judith H.] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England. [Brassington, Nicola J.; Hardcastle, Martin J.; Goodger, Joanna L.] Univ Hertfordshire, Sch Phys Astron & Math, Hatfield AL10 9AB, Herts, England. [Kainulainen, Jouni] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Woodley, Kristin A.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada. [Woodley, Kristin A.] UC Santa Cruz, Univ Calif Observ, Santa Cruz, CA 95064 USA. [Sivakoff, Gregory R.] Univ Alberta, Dept Phys, Edmonton, AB T6G 2E1, Canada. [Birkinshaw, Mark; Worrall, Diana M.] Univ Bristol, HH Wills Phys Lab, Bristol BS8 1TL, Avon, England. [Gilfanov, Marat; Zhang, Zhongli] Max Planck Inst Astrophys, D-85741 Garching, Germany. [Gilfanov, Marat] Russian Acad Sci, Inst Space Res, Moscow 117997, Russia. [Jordan, Andres] Pontificia Univ Catolica Chile, Dept Astron & Astrofis, Santiago 22, Chile. [Sarazin, Craig L.] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA. [Voss, Rasmus] Univ Nijmegen, Dept Astrophys IMAPP, NL-6500 GL Nijmegen, Netherlands. [Murray, Stephen S.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. RP Burke, MJ (reprint author), Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England. EM mburke@star.sr.bham.ac.uk RI Sivakoff, Gregory/G-9602-2011; OI Sivakoff, Gregory/0000-0001-6682-916X; Goodger, Joanna/0000-0002-5738-4768; Jordan, Andres/0000-0002-5389-3944; Forman, William/0000-0002-9478-1682; Hardcastle, Martin/0000-0003-4223-1117 FU NASA [NAS8-03060]; University of Birmingham; NWO Vidi grant [016.093.305]; NSERC Discovery FX This work was supported by NASA grant NAS8-03060. M.J.B. thanks SAO and the University of Birmingham for financial support. R.V. is supported by NWO Vidi grant 016.093.305. G.R.S. acknowledges the support of an NSERC Discovery Grant. We also thank Rudy Wijnands, Vinay Kashyap, Jeff McClintock, Andrea Prestwich, Rob Barnard, Kim Dong-Woo, and Alastair Sanderson for useful discussions. Finally, we thank the anonymous referee for their careful consideration of our work. NR 78 TC 4 Z9 4 U1 0 U2 6 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD APR 1 PY 2013 VL 766 IS 2 AR 88 DI 10.1088/0004-637X/766/2/88 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 108UE UT WOS:000316320900022 ER PT J AU Chaplin, WJ Sanchis-Ojeda, R Campante, TL Handberg, R Stello, D Winn, JN Basu, S Christensen-Dalsgaard, J Davies, GR Metcalfe, TS Buchhave, LA Fischer, DA Bedding, TR Cochran, WD Elsworth, Y Gilliland, RL Hekker, S Huber, D Isaacson, H Karoff, C Kawaler, SD Kjeldsen, H Latham, DW Lund, MN Lundkvist, M Marcy, GW Miglio, A Barclay, T Lissauer, JJ AF Chaplin, W. J. Sanchis-Ojeda, R. Campante, T. L. Handberg, R. Stello, D. Winn, J. N. Basu, S. Christensen-Dalsgaard, J. Davies, G. R. Metcalfe, T. S. Buchhave, L. A. Fischer, D. A. Bedding, T. R. Cochran, W. D. Elsworth, Y. Gilliland, R. L. Hekker, S. Huber, D. Isaacson, H. Karoff, C. Kawaler, S. D. Kjeldsen, H. Latham, D. W. Lund, M. N. Lundkvist, M. Marcy, G. W. Miglio, A. Barclay, T. Lissauer, J. J. TI ASTEROSEISMIC DETERMINATION OF OBLIQUITIES OF THE EXOPLANET SYSTEMS KEPLER-50 AND KEPLER-65 SO ASTROPHYSICAL JOURNAL LA English DT Article DE asteroseismology; planets and satellites: formation; planets and satellites: general; stars: rotation ID SPIN-ORBIT MISALIGNMENT; SOLAR-TYPE STARS; TRANSIT TIMING OBSERVATIONS; RAPIDLY ROTATING STARS; OF-STATE TABLES; SUN-LIKE STAR; PLANET CANDIDATES; LIGHT CURVES; PHOTOMETRIC VARIABILITY; INITIAL CHARACTERISTICS AB Results on the obliquity of exoplanet host stars-the angle between the stellar spin axis and the planetary orbital axis-provide important diagnostic information for theories describing planetary formation. Here we present the first application of asteroseismology to the problem of stellar obliquity determination in systems with transiting planets and Sun-like host stars. We consider two systems observed by the NASA Kepler mission which have multiple transiting small (super-Earth sized) planets: the previously reported Kepler-50 and a new system, Kepler-65, whose planets we validate in this paper. Both stars show rich spectra of solar-like oscillations. From the asteroseismic analysis we find that each host has its rotation axis nearly perpendicular to the line of sight with the sines of the angles constrained at the 1 sigma level to lie above 0.97 and 0.91, respectively. We use statistical arguments to show that coplanar orbits are favored in both systems, and that the orientations of the planetary orbits and the stellar rotation axis are correlated. C1 [Chaplin, W. J.; Campante, T. L.; Davies, G. R.; Elsworth, Y.; Hekker, S.; Miglio, A.] Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England. [Sanchis-Ojeda, R.; Winn, J. N.] MIT, Dept Phys, Cambridge, MA 02139 USA. [Handberg, R.; Christensen-Dalsgaard, J.; Karoff, C.; Kjeldsen, H.; Lund, M. N.; Lundkvist, M.] Aarhus Univ, Dept Phys & Astron, SAC, DK-8000 Aarhus C, Denmark. [Stello, D.; Bedding, T. R.] Univ Sydney, Sch Phys, Sydney Inst Astron, Sydney, NSW 2006, Australia. [Basu, S.; Fischer, D. A.] Yale Univ, New Haven, CT 06520 USA. [Metcalfe, T. S.] White Dwarf Res Corp, Boulder, CO 80301 USA. [Buchhave, L. A.] Univ Copenhagen, Niels Bohr Inst, DK-2100 Copenhagen, Denmark. [Buchhave, L. A.] Univ Copenhagen, Nat Hist Museum Denmark, Ctr Star & Planet Format, DK-1530 Copenhagen, Denmark. [Cochran, W. D.] Univ Texas Austin, McDonald Observ, Austin, TX 78712 USA. [Gilliland, R. L.] Penn State Univ, Ctr Exoplanets & Habitable Worlds, University Pk, PA 16802 USA. [Hekker, S.] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 XH Amsterdam, Netherlands. [Huber, D.; Barclay, T.; Lissauer, J. J.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Isaacson, H.; Marcy, G. W.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Kawaler, S. D.] Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA. [Latham, D. W.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Barclay, T.] Environm Res Inst, Bay Area, Sonoma, CA 95476 USA. RP Chaplin, WJ (reprint author), Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England. OI Kawaler, Steven/0000-0002-6536-6367; Bedding, Timothy/0000-0001-5943-1460; Davies, Guy/0000-0002-4290-7351; Buchhave, Lars A./0000-0003-1605-5666; Metcalfe, Travis/0000-0003-4034-0416; Karoff, Christoffer/0000-0003-2009-7965; Bedding, Tim/0000-0001-5222-4661; Basu, Sarbani/0000-0002-6163-3472; Lund, Mikkel Norup/0000-0001-9214-5642; Lundkvist, Mia Sloth/0000-0002-8661-2571; Fischer, Debra/0000-0003-2221-0861; Handberg, Rasmus/0000-0001-8725-4502 FU NASA's Science Mission Directorate; UK Science and Technology Facilities Council (STFC); NASA Kepler Participating Scientist program [NNX12AC76G]; NSF [AST 1105930]; Danish National Research Foundation; ASTERISK project (ASTERoseismic Investigations with SONG and Kepler); European Research Council [267864]; Netherlands Organisation for Scientific Research (NWO); International Space Science Institute (ISSI) FX Funding for this Discovery mission is provided by NASA's Science Mission Directorate. The authors wish to thank the entire Kepler team, without whom these results would not be possible. W.J.C., T.L.C., G.R. D., Y.E., and A. M. acknowledge the support of the UK Science and Technology Facilities Council (STFC). J.N.W. was supported by the NASA Kepler Participating Scientist program through grant NNX12AC76G. S.B. acknowledges NSF grant AST 1105930. Funding for the Stellar Astrophysics Centre (SAC) is provided by The Danish National Research Foundation. The research is supported by the ASTERISK project (ASTERoseismic Investigations with SONG and Kepler) funded by the European Research Council (grant agreement no.:267864). S.H. acknowledges financial support from the Netherlands Organisation for Scientific Research (NWO). Computational time on Kraken at the National Institute of Computational Sciences was provided through NSF TeraGrid allocation TG-AST090107. We acknowledge the Pale Blue Dot Project, hosted by White Dwarf Research Corporation (whitedwarf.org/palebluedot), and we are also grateful for support from the International Space Science Institute (ISSI). NR 124 TC 68 Z9 68 U1 1 U2 7 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD APR 1 PY 2013 VL 766 IS 2 AR 101 DI 10.1088/0004-637X/766/2/101 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 108UE UT WOS:000316320900035 ER PT J AU Fressin, F Torres, G Charbonneau, D Bryson, ST Christiansen, J Dressing, CD Jenkins, JM Walkowicz, LM Batalha, NM AF Fressin, Francois Torres, Guillermo Charbonneau, David Bryson, Stephen T. Christiansen, Jessie Dressing, Courtney D. Jenkins, Jon M. Walkowicz, Lucianne M. Batalha, Natalie M. TI THE FALSE POSITIVE RATE OF KEPLER AND THE OCCURRENCE OF PLANETS SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries: eclipsing; methods: data analysis; methods: statistical; planetary systems ID TRANSIT TIMING VARIATIONS; SOLAR-TYPE STARS; SUN-LIKE STARS; ECLIPSING BINARIES; BLEND SCENARIOS; MULTIPLE SYSTEM; HABITABLE-ZONE; INPUT CATALOG; DATA RELEASE; CANDIDATES AB The Kepler mission is uniquely suited to study the frequencies of extrasolar planets. This goal requires knowledge of the incidence of false positives such as eclipsing binaries in the background of the targets, or physically bound to them, which can mimic the photometric signal of a transiting planet. We perform numerical simulations of the Kepler targets and of physical companions or stars in the background to predict the occurrence of astrophysical false positives detectable by the mission. Using real noise level estimates, we compute the number and characteristics of detectable eclipsing pairs involving main-sequence stars and non-main-sequence stars or planets, and we quantify the fraction of those that would pass the Kepler candidate vetting procedure. By comparing their distribution with that of the Kepler Objects of Interest (KOIs) detected during the first six quarters of operation of the spacecraft, we infer the false positive rate of Kepler and study its dependence on spectral type, candidate planet size, and orbital period. We find that the global false positive rate of Kepler is 9.4%, peaking for giant planets (6-22 R-circle plus) at 17.7%, reaching a low of 6.7% for small Neptunes (2-4 R-circle plus), and increasing again for Earth-size planets (0.8-1.25 R-circle plus) to 12.3%. Most importantly, we also quantify and characterize the distribution and rate of occurrence of planets down to Earth size with no prior assumptions on their frequency, by subtracting from the population of actual Kepler candidates our simulated population of astrophysical false positives. We find that 16.5% +/- 3.6% of main-sequence FGK stars have at least one planet between 0.8 and 1.25 R-circle plus with orbital periods up to 85 days. This result is a significant step toward the determination of eta-earth, the occurrence of Earth-like planets in the habitable zone of their parent stars. There is no significant dependence of the rates of planet occurrence between 0.8 and 4 Earth radii with spectral type. In the process, we also derive a prescription for the signal recovery rate of Kepler that enables a good match to both the KOI size and orbital period distribution, as well as their signal-to-noise distribution. C1 [Fressin, Francois; Torres, Guillermo; Charbonneau, David; Dressing, Courtney D.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Bryson, Stephen T.; Christiansen, Jessie; Jenkins, Jon M.; Batalha, Natalie M.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Walkowicz, Lucianne M.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. RP Fressin, F (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM ffressin@cfa.harvard.edu OI Charbonneau, David/0000-0002-9003-484X FU NASA [NNX12AC75G] FX We thank the anonymous referee for helpful suggestions on the original manuscript. G.T. acknowledges partial support for this work from NASA Grant NNX12AC75G (Kepler Participating Scientist Program). NR 46 TC 329 Z9 331 U1 10 U2 51 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD APR 1 PY 2013 VL 766 IS 2 AR 81 DI 10.1088/0004-637X/766/2/81 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 108UE UT WOS:000316320900015 ER PT J AU Hillier, A van Ballegooijen, A AF Hillier, Andrew van Ballegooijen, Adriaan TI ON THE SUPPORT OF SOLAR PROMINENCE MATERIAL BY THE DIPS OF A CORONAL FLUX TUBE SO ASTROPHYSICAL JOURNAL LA English DT Article DE methods: numerical; Sun: filaments, prominences ID RAYLEIGH-TAYLOR INSTABILITY; QUIESCENT PROMINENCE; MAGNETIC-FIELDS; HYDROMAGNETIC INTERIOR; NUMERICAL SIMULATIONS; MODEL; DYNAMICS; STABILITY; FILAMENTS; RECONNECTION AB The dense prominence material is believed to be supported against gravity through the magnetic tension of dipped coronal magnetic field. For quiescent prominences, which exhibit many gravity-driven flows, hydrodynamic forces are likely to play an important role in the determination of both the large-and small-scale magnetic field distributions. In this study, we present the first steps toward creating a three-dimensional magneto-hydrostatic prominence model where the prominence is formed in the dips of a coronal flux tube. Here 2.5D equilibria are created by adding mass to an initially force-free magnetic field, then performing a secondary magnetohydrodynamic relaxation. Two inverse polarity magnetic field configurations are studied in detail, a simple o-point configuration with a ratio of the horizontal field (B-x) to the axial field (By) of 1:2 and a more complex model that also has an x-point with a ratio of 1:11. The models show that support against gravity is either by total pressure or tension, with only tension support resembling observed quiescent prominences. The o-point of the coronal flux tube was pulled down by the prominence material, leading to compression of the magnetic field at the base of the prominence. Therefore, tension support comes from the small curvature of the compressed magnetic field at the bottom and the larger curvature of the stretched magnetic field at the top of the prominence. It was found that this method does not guarantee convergence to a prominence-like equilibrium in the case where an x-point exists below the prominence flux tube. The results imply that a plasma beta of similar to 0.1 is necessary to support prominences through magnetic tension. C1 [Hillier, Andrew] Kyoto Univ, Kwasan Observ, Kyoto, Japan. [Hillier, Andrew] Kyoto Univ, Hida Observ, Kyoto, Japan. [van Ballegooijen, Adriaan] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Hillier, A (reprint author), Kyoto Univ, Kwasan Observ, Kyoto, Japan. OI van Ballegooijen, Adriaan/0000-0002-5622-3540 FU Ministry of Education, Culture, Sports, Science and Technology (MEXT) of Japan; Hinode/XRT project under NASA [NNM07AB07C] FX The authors thank the staff and students of Kwasan and Hida observatories for their support and comments. The authors thank the referee for comments and suggestions that helped to improve the presentation of this work. This work was supported in part by the Grant-in-Aid for the Global COE program "The Next Generation of Physics, Spun from Universality and Emergence" from the Ministry of Education, Culture, Sports, Science and Technology (MEXT) of Japan. This work was supported by the Hinode/XRT project under NASA grant NNM07AB07C. 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). The MHD relaxations presented in this paper were carried out on the SIMSV cluster at Kwasan observatory. NR 51 TC 17 Z9 17 U1 0 U2 6 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD APR 1 PY 2013 VL 766 IS 2 AR 126 DI 10.1088/0004-637X/766/2/126 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 108UE UT WOS:000316320900060 ER PT J AU Hsiao, EY Marion, GH Phillips, MM Burns, CR Winge, C Morrell, N Contreras, C Freedman, WL Kromer, M Gall, EEE Gerardy, CL Hoflich, P Im, M Jeon, Y Kirshner, RP Nugent, PE Persson, SE Pignata, G Roth, M Stanishev, V Stritzinger, M Suntzeff, NB AF Hsiao, E. Y. Marion, G. H. Phillips, M. M. Burns, C. R. Winge, C. Morrell, N. Contreras, C. Freedman, W. L. Kromer, M. Gall, E. E. E. Gerardy, C. L. Hoeflich, P. Im, M. Jeon, Y. Kirshner, R. P. Nugent, P. E. Persson, S. E. Pignata, G. Roth, M. Stanishev, V. Stritzinger, M. Suntzeff, N. B. TI THE EARLIEST NEAR-INFRARED TIME-SERIES SPECTROSCOPY OF A TYPE Ia SUPERNOVA SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology: observations; infrared: general; supernovae: general; supernovae: individual (SN 2011fe) ID SN 2011FE; LIGHT-CURVE; OPTICAL-SPECTRA; K-CORRECTIONS; THERMONUCLEAR SUPERNOVAE; DETONATION TRANSITION; ABSOLUTE MAGNITUDES; PEAK-LUMINOSITY; HOST GALAXIES; MAXIMUM-LIGHT AB We present ten medium-resolution, high signal-to-noise ratio near-infrared (NIR) spectra of SN 2011fe from SpeX on the NASA Infrared Telescope Facility (IRTF) and Gemini Near-Infrared Spectrograph (GNIRS) on Gemini North, obtained as part of the Carnegie Supernova Project. This data set constitutes the earliest time-series NIR spectroscopy of a Type Ia supernova (SN Ia), with the first spectrum obtained at 2.58 days past the explosion and covering -14.6 to +17.3 days relative to B-band maximum. CI lambda 1.0693 mu m is detected in SN 2011fe with increasing strength up to maximum light. The delay in the onset of the NIR CI line demonstrates its potential to be an effective tracer of unprocessed material. For the first time in a SN Ia, the early rapid decline of the MgII lambda 1.0927 mu m velocity was observed, and the subsequent velocity is remarkably constant. The MgII velocity during this constant phase locates the inner edge of carbon burning and probes the conditions under which the transition from deflagration to detonation occurs. We show that the MgII velocity does not correlate with the optical light-curve decline rate Delta m(15)(B). The prominent break at similar to 1.5 mu m is the main source of concern for NIR k-correction calculations. We demonstrate here that the feature has a uniform time evolution among SNe Ia, with the flux ratio across the break strongly correlated with Delta m(15)(B). The predictability of the strength and the onset of this feature suggests that the associated k-correction uncertainties can be minimized with improved spectral templates. C1 [Hsiao, E. Y.; Phillips, M. M.; Morrell, N.; Contreras, C.; Roth, M.] Las Campanas Observ, Carnegie Observ, Colina El Pino, Chile. [Marion, G. H.; Kirshner, R. P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Burns, C. R.; Freedman, W. L.; Persson, S. E.] Carnegie Observ, Pasadena, CA 91101 USA. [Winge, C.] AURA Inc, Gemini South Observ, La Serena, Chile. [Kromer, M.; Gall, E. E. E.] Max Planck Inst Astrophys, D-85741 Garching, Germany. [Gall, E. E. E.] Queens Univ Belfast, Sch Maths & Phys, Astrophys Res Ctr, Belfast BT7 1NN, Antrim, North Ireland. [Gerardy, C. L.; Hoeflich, P.] Florida State Univ, Dept Phys, Tallahassee, FL 32306 USA. [Im, M.; Jeon, Y.] Seoul Natl Univ, Dept Phys & Astron, Astron Program, CEOU, Seoul, South Korea. [Nugent, P. E.] Lawrence Berkeley Natl Lab, Computat Cosmol Ctr, Computat Res Div, Berkeley, CA 94611 USA. [Nugent, P. E.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Pignata, G.] Univ Andres Bello, Dept Ciencias Fis, Santiago, Chile. [Stanishev, V.] Inst Super Tecn, CENTRA Ctr Multidisciplinar Astrofis, P-1049001 Lisbon, Portugal. [Stritzinger, M.] Aarhus Univ, Dept Phys & Astron, DK-8000 Aarhus C, Denmark. [Suntzeff, N. B.] Texas A&M Univ, Mitchell Inst Fundamental Phys & Astron, Dept Phys & Astron, College Stn, TX 77843 USA. RP Hsiao, EY (reprint author), Las Campanas Observ, Carnegie Observ, Casilla 601, Colina El Pino, Chile. EM hsiao@lco.cl RI Stanishev, Vallery/M-8930-2013; OI Stanishev, Vallery/0000-0002-7626-1181; Im, Myungshin/0000-0002-8537-6714; stritzinger, maximilian/0000-0002-5571-1833 FU National Science Foundation [AST-1008343]; Danish Agency for Science and Technology; Innovation through a Sapere Aude Level 2 grant; Creative Initiative program of the National Research Foundation of Korea (NRFK) [2010-0000712]; Millennium Center for Supernova Science [P10-064-F]; Programa Bicentenario de Ciencia y Tecnologia de CONICYT; Programa Iniciativa Cientifica Milenio de MIDEPLAN; Office of Science of the U.S. Department of Energy [DE-AC02-05CH11231]; [GN-2011B-Q-68] FX This paper is based on data obtained with the GeminiObservatory, under the long-term program GN-2011B-Q-68, the NASA Infrared Telescope Facility (IRTF), the United Kingdom Infrared Telescope (UKIRT), and the 6.5 m Magellan Telescopes. The Gemini Observatory is operated by the Association of Universities for Research in Astronomy, Inc., under a cooperative agreement with the NSF on behalf of the Gemini partnership: the National Science Foundation (United States), the National Research Council (Canada), CONICYT (Chile), the Australian Research Council (Australia), Ministerio da Ciencia, Tecnologia e Inovacao (Brazil) and Ministerio de Ciencia, Tecnologia e Innovacion Productiva (Argentina). UKIRT is operated by the Joint Astronomy Centre on behalf of the Science and Technology Facilities Council of the UK. We would like to thank Nancy Levenson for approving our GNIRS observations to be performed outside of the proposed observing period. Most observations were obtained at facilities on MaunaKea. The authors would like to recognize the very significant cultural role and reverence that the summit of Mauna Kea has within the indigenous community of Hawaii. We are grateful for our opportunity to conduct observations from this mountain.; This material is based upon work supported by the National Science Foundation under Grant No. AST-1008343. M.S. acknowledges the generous support provided by the Danish Agency for Science and Technology and Innovation through a Sapere Aude Level 2 grant. M.I. and Y.J. acknowledge the support from the Creative Initiative program, No. 2010-0000712, of the National Research Foundation of Korea (NRFK). G.P. acknowledges support from the Millennium Center for Supernova Science through grant P10-064-F funded by "Programa Bicentenario de Ciencia y Tecnologia de CONICYT" and "Programa Iniciativa Cientifica Milenio de MIDEPLAN."; This research used resources from the National Energy Research Scientific Computing Center (NERSC), which is supported by the Office of Science of the U.S. Department of Energy under Contract No. DE-AC02-05CH11231. We have also 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 101 TC 30 Z9 30 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 APR 1 PY 2013 VL 766 IS 2 AR 72 DI 10.1088/0004-637X/766/2/72 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 108UE UT WOS:000316320900006 ER PT J AU Kirk, H Myers, PC Bourke, TL Gutermuth, RA Hedden, A Wilson, GW AF Kirk, Helen Myers, Philip C. Bourke, Tyler L. Gutermuth, Robert A. Hedden, Abigail Wilson, Grant W. TI FILAMENTARY ACCRETION FLOWS IN THE EMBEDDED SERPENS SOUTH PROTOCLUSTER SO ASTROPHYSICAL JOURNAL LA English DT Article DE stars: formation; ISM: clouds; ISM: kinematics and dynamics; ISM: molecules ID STAR-FORMING CORES; MOLECULAR CLOUDS; DENSE CORES; DARK CLOUDS; HYPERFINE-STRUCTURE; STELLAR CLUSTERS; PERSEUS; HCN; MM; SPECTROSCOPY AB One puzzle in understanding how stars form in clusters is the source of mass-is all of the mass in place before the first stars are born, or is there an extended period when the cluster accretes material which can continuously fuel the star formation process? We use a multi-line spectral survey of the southern filament associated with the Serpens South embedded cluster-forming region in order to determine if mass is accreting from the filament onto the cluster, and whether the accretion rate is significant. Our analysis suggests that material is flowing along the filament's long axis at a rate of similar to 30 M-circle dot Myr(-1) (inferred from the N2H+ velocity gradient along the filament), and radially contracting onto the filament at similar to 130 M-circle dot Myr(-1) (inferred from HNC self-absorption). These accretion rates are sufficient to supply mass to the central cluster at a similar rate to the current star formation rate in the cluster. Filamentary accretion flows may therefore be very important in the ongoing evolution of this cluster. C1 [Kirk, Helen; Myers, Philip C.; Bourke, Tyler L.] Harvard Smithsonian Ctr Astrophys, Radio & Geoastron Div, Cambridge, MA 02138 USA. [Gutermuth, Robert A.; Wilson, Grant W.] Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA. [Hedden, Abigail] USA, Res Labs, Adelphi, MD 20783 USA. RP Kirk, H (reprint author), McMaster Univ, Origins Inst, Hamilton, ON L8S 4L8, Canada. EM kirkh@mcmaster.ca FU Smithsonian Scholarly Studies Program grant; National Science Foundation [0708158] FX We thank the referee for suggestions which helped to clarify aspects of this paper. We thank Steve Longmore for assistance with the Mopra observing setup and data reduction. We thank Phil Edwards at ATNF for allocating additional time to complete our Mopra observations, and all the ATNF Narrabri staff for their support. We thank Rachel Friesen for sending her ammonia temperature results prior to publication, and for several interesting discussions on Serpens South. We thank Elaine Winston and Scott Wolk for sharing the results of their Chandra survey of Serpens South prior to publication. H.K. thanks Paola Caselli for a valuable discussion on astrochemistry, Chris de Vries for answering queries on his infall fitter on numerous occasions, and Fabian Heitsch for a critical read-through of an earlier draft of this paper, as well as sending a copy of his filamentary accretion paper pre-publication. H.K. acknowledges funding from a Smithsonian Scholarly Studies Program grant. This research was supported in part by the National Science Foundation under grant number 0708158 (T.L.B.). NR 62 TC 64 Z9 64 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD APR 1 PY 2013 VL 766 IS 2 AR 115 DI 10.1088/0004-637X/766/2/115 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 108UE UT WOS:000316320900049 ER PT J AU Lewis, NK Knutson, HA Showman, AP Cowan, NB Laughlin, G Burrows, A Deming, D Crepp, JR Mighell, KJ Agol, E Bakos, GA Charbonneau, D Desert, JM Fischer, DA Fortney, JJ Hartman, JD Hinkley, S Howard, AW Johnson, JA Kao, M Langton, J Marcy, GW AF Lewis, Nikole K. Knutson, Heather A. Showman, Adam P. Cowan, Nicolas B. Laughlin, Gregory Burrows, Adam Deming, Drake Crepp, Justin R. Mighell, Kenneth J. Agol, Eric Bakos, Gaspar A. Charbonneau, David Desert, Jean-Michel Fischer, Debra A. Fortney, Jonathan J. Hartman, Joel D. Hinkley, Sasha Howard, Andrew W. Johnson, John Asher Kao, Melodie Langton, Jonathan Marcy, Geoffrey W. TI ORBITAL PHASE VARIATIONS OF THE ECCENTRIC GIANT PLANET HAT-P-2b SO ASTROPHYSICAL JOURNAL LA English DT Article DE atmospheric effects; methods: numerical; planets and satellites: general; planets and satellites: individual (HAT-P-2b); techniques: photometric ID TRANSIT LIGHT-CURVE; SPITZER-SPACE-TELESCOPE; INFRARED ARRAY CAMERA; IN EXTRASOLAR PLANETS; HD 189733B; ATMOSPHERIC CIRCULATION; TIDAL EVOLUTION; WARM SPITZER; EMISSION-SPECTRUM; HOT JUPITERS AB We present the first secondary eclipse and phase curve observations for the highly eccentric hot Jupiter HAT-P-2b in the 3.6, 4.5, 5.8, and 8.0 mu m bands of the Spitzer Space Telescope. The 3.6 and 4.5 mu m data sets span an entire orbital period of HAT-P-2b (P = 5.6334729 d), making them the longest continuous phase curve observations obtained to date and the first full-orbit observations of a planet with an eccentricity exceeding 0.2. We present an improved non-parametric method for removing the intrapixel sensitivity variations in Spitzer data at 3.6 and 4.5 mu m that robustly maps position-dependent flux variations. We find that the peak in planetary flux occurs at 4.39 +/- 0.28, 5.84 +/- 0.39, and 4.68 +/- 0.37 hr after periapse passage with corresponding maxima in the planet/star flux ratio of 0.1138% +/- 0.0089%, 0.1162% +/- 0.0080%, and 0.1888% +/- 0.0072% in the 3.6, 4.5, and 8.0 mu m bands, respectively. Our measured secondary eclipse depths of 0.0996% +/- 0.0072%, 0.1031% +/- 0.0061%, 0.071% (+0.029%)(-0.013%), and 0.1392% +/- 0.0095% in the 3.6, 4.5, 5.8, and 8.0 mu m bands, respectively, indicate that the planet cools significantly from its peak temperature before we measure the dayside flux during secondary eclipse. We compare our measured secondary eclipse depths to the predictions from a one-dimensional radiative transfer model, which suggests the possible presence of a transient day side inversion in HAT-P-2b's atmosphere near periapse. We also derive improved estimates for the system parameters, including its mass, radius, and orbital ephemeris. Our simultaneous fit to the transit, secondary eclipse, and radial velocity data allows us to determine the eccentricity (e = 0.50910 +/- 0.00048) and argument of periapse (omega = 188 degrees. 09 +/- 0 degrees.39) of HAT-P-2b's orbit with a greater precision than has been achieved for any other eccentric extrasolar planet. We also find evidence for a long-term linear trend in the radial velocity data. This trend suggests the presence of another substellar companion in the HAT-P-2 system, which could have caused HAT-P-2b to migrate inward to its present-day orbit via the Kozai mechanism. C1 [Lewis, Nikole K.; Burrows, Adam] Univ Arizona, Dept Planetary Sci & Lunar & Planetary Lab, Tucson, AZ 85721 USA. [Lewis, Nikole K.] MIT, Dept Earth Atmospher & Planetary Sci, Cambridge, MA 02139 USA. [Knutson, Heather A.; Desert, Jean-Michel; Kao, Melodie] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. [Cowan, Nicolas B.] Northwestern Univ, Ctr Interdisciplinary Explorat & Res Astrophys, Evanston, IL 60208 USA. [Cowan, Nicolas B.] Northwestern Univ, Dept Phys & Astron, Evanston, IL 60208 USA. [Laughlin, Gregory; Fortney, Jonathan J.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. [Burrows, Adam; Bakos, Gaspar A.; Hartman, Joel D.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. [Deming, Drake] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Crepp, Justin R.] Univ Notre Dame, Dept Phys, Notre Dame, IN 46556 USA. [Mighell, Kenneth J.] Natl Opt Astron Observ, Tucson, AZ 85726 USA. [Agol, Eric] Univ Washington, Dept Astron, Seattle, WA 98195 USA. [Charbonneau, David] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Fischer, Debra A.] Yale Univ, Dept Astron, New Haven, CT 06511 USA. [Hinkley, Sasha; Johnson, John Asher] CALTECH, Dept Astrophys, Pasadena, CA 91125 USA. [Howard, Andrew W.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Langton, Jonathan] Principia Coll, Dept Phys, Elsah, IL 62028 USA. [Marcy, Geoffrey W.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. RP Lewis, NK (reprint author), Univ Arizona, Dept Planetary Sci & Lunar & Planetary Lab, Tucson, AZ 85721 USA. EM nklewis@mit.edu RI Howard, Andrew/D-4148-2015; OI Howard, Andrew/0000-0001-8638-0320; Charbonneau, David/0000-0002-9003-484X; Fortney, Jonathan/0000-0002-9843-4354; /0000-0002-0802-9145; Hartman, Joel/0000-0001-8732-6166; Fischer, Debra/0000-0003-2221-0861 FU NASA; JPL/Caltech; NASA Headquarters under the NASA Earth and Space Science Fellowship Program [NNX08AX02H]; Origins Program [NNX08AF27G] 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 JPL/Caltech. N.K.L. was further supported by NASA Headquarters under the NASA Earth and Space Science Fellowship Program (NNX08AX02H), Origins Program (NNX08AF27G), and in part under contract with the California Institute of Technology (Caltech) funded by NASA through the Sagan Fellowship Program executed by the NASA Exoplanet Science Institute. 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. N.K.L. wishes to thank B. K. Jackson and J. A. Carter for many useful discussions during the preparation of this manuscript and the anonymous referee for their helpful suggestions. NR 89 TC 73 Z9 74 U1 0 U2 9 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD APR 1 PY 2013 VL 766 IS 2 AR 95 DI 10.1088/0004-637X/766/2/95 PG 22 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 108UE UT WOS:000316320900029 ER PT J AU Vanthomme, H Kolowski, J Korte, L Alonso, A AF Vanthomme, Hadrien Kolowski, Joseph Korte, Lisa Alonso, Alfonso TI Distribution of a Community of Mammals in Relation to Roads and Other Human Disturbances in Gabon, Central Africa SO CONSERVATION BIOLOGY LA English DT Article DE abundance index; camera trapping; generalized models; hunting; mosaic landscape; oil extraction; road mitigation ID SEXUAL SEGREGATION; RAIN-FORESTS; CONSERVATION; ELEPHANTS; IMPACTS; POPULATIONS; CONCESSION; ECOLOGY; MODELS AB We present the first community-level study of the associations of both roads and other human disturbances with the distribution of mammals in Gabon (central Africa). Our study site was in an oil concession within a littoral mosaic landscape. We conducted surveys along 199 line transects and installed camera traps on 99 of these transects to document mammal presence and abundance. We used generalized linear mixed-effect models to document associations between variables related to the ecosystem (land cover, topography, and hydrology), roads (coating, width of rights of way, condition, type of vehicle used on the road, traffic level, affiliation of users, and general type of road), and other human disturbances (urbanization, agriculture, hunting, logging, gathering, and industrial activities) and the abundance or presence of 17 species or groups of mammals including elephant (Loxodonta cyclotis), buffalo (Syncerus caffer), sitatunga (Tragelaphus spekei), red river hog (Potamochoerus porcus), smaller ungulates, gorilla (Gorilla gorilla), chimpanzee (Pan troglodytes), side-striped jackal (Canis adustus), carnivores, monkeys, and large rodents. Some types of roads and other human disturbances were negatively associated with the abundance or presence of elephants, buffalos, gorillas, sitatungas, some monkeys, and duikers. The pattern of associations of mammals with roads and other human disturbances was diverse and included positive associations with road presence (red river hog, some monkeys, and duikers), agriculture (sitatunga, small carnivores, and large rodents) and industrial activities (sitatunga, red river hog, red duikers, and side-striped jackal). Our results suggest that the community of mammals we studied was mostly affected by hunting, agriculture, and urbanization, which are facilitated by road presence. We recommend increased regulation of agriculture, hunting, and road building in the area. C1 [Vanthomme, Hadrien; Kolowski, Joseph; Korte, Lisa; Alonso, Alfonso] Smithsonian Conservat Biol Inst, Natl Zool Pk, Ctr Conservat Educ & Sustainabil, Washington, DC 20013 USA. RP Vanthomme, H (reprint author), Smithsonian Conservat Biol Inst, Natl Zool Pk, Ctr Conservat Educ & Sustainabil, POB 37012,MRC 0705, Washington, DC 20013 USA. EM vanthommeh@si.edu FU Shell Gabon; Smithsonian Conservation Biology Institute; Gabon Biodiversity Program [139] FX We thank A. Noungou and D. Idiata for authorizing our study (permit 0103/MEFEDD/SG/DGEF/DFC) and Shell Gabon and the Smithsonian Conservation Biology Institute for funding. We also thank J. Thompson, B. Meye, Mr. Biyogo, A. Mboutsou-Matoka, A.-E. Andoung-Ebome, and the employees of Shell Gabon and World Wildlife Fund for their help. We thank the anonymous reviewers for their constructive criticisms and comments on earlier drafts. This is contribution 139 of the Gabon Biodiversity Program. NR 39 TC 12 Z9 13 U1 12 U2 190 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0888-8892 EI 1523-1739 J9 CONSERV BIOL JI Conserv. Biol. PD APR PY 2013 VL 27 IS 2 BP 281 EP 291 DI 10.1111/cobi.12017 PG 11 WC Biodiversity Conservation; Ecology; Environmental Sciences SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 113UN UT WOS:000316694600007 PM 23410077 ER PT J AU Carrillo-Baltodano, A Collin, R AF Carrillo-Baltodano, A. Collin, R. TI Sex-change in Crepidula cf. marginalis (Gastropoda: Calyptraeidae) is a response to physical contact with conspecifics SO INTEGRATIVE AND COMPARATIVE BIOLOGY LA English DT Meeting Abstract CT Annual Meeting of the Society-for-Integrative-and-Comparative-Biology (SICB) CY JAN 03-07, 2013 CL San Francisco, CA SP Soc Integrat & Comparat Biol (SICB) C1 [Carrillo-Baltodano, A.; Collin, R.] Smithsonian Trop Res Inst, Panama City, Panama. EM carbalallan@gmail.com NR 0 TC 0 Z9 0 U1 0 U2 0 PU OXFORD UNIV PRESS INC PI CARY PA JOURNALS DEPT, 2001 EVANS RD, CARY, NC 27513 USA SN 1540-7063 J9 INTEGR COMP BIOL JI Integr. Comp. Biol. PD APR PY 2013 VL 53 SU 1 BP E259 EP E259 PG 1 WC Zoology SC Zoology GA 117ZG UT WOS:000316991402093 ER PT J AU Christy, JH AF Christy, John H. TI Extreme synchrony, amplitude modulation and phase reversals in the semilunar reproductive cycle of the intertidal false limpet Siphonaria gigas on a rocky shore in Panama SO INTEGRATIVE AND COMPARATIVE BIOLOGY LA English DT Meeting Abstract CT Annual Meeting of the Society-for-Integrative-and-Comparative-Biology (SICB) CY JAN 03-07, 2013 CL San Francisco, CA SP Soc Integrat & Comparat Biol (SICB) C1 [Christy, John H.] Smithsonian Trop Res Inst, Panama City, Panama. EM christyj@si.edu NR 0 TC 0 Z9 0 U1 0 U2 3 PU OXFORD UNIV PRESS INC PI CARY PA JOURNALS DEPT, 2001 EVANS RD, CARY, NC 27513 USA SN 1540-7063 J9 INTEGR COMP BIOL JI Integr. Comp. Biol. PD APR PY 2013 VL 53 SU 1 BP E35 EP E35 PG 1 WC Zoology SC Zoology GA 117ZG UT WOS:000316991400138 ER PT J AU Clancy, DL Davis, T Ruiz, G Cohen, CS AF Clancy, D. L. Davis, T. Ruiz, G. Cohen, C. S. TI Examining Genetic Diversity of an Invasive Colonial Ascidian in Southeast Alaska SO INTEGRATIVE AND COMPARATIVE BIOLOGY LA English DT Meeting Abstract CT Annual Meeting of the Society-for-Integrative-and-Comparative-Biology (SICB) CY JAN 03-07, 2013 CL San Francisco, CA SP Soc Integrat & Comparat Biol (SICB) C1 San Francisco State Univ, San Francisco, CA USA. Alaska Dept Fish & Game, Anchorage, AK USA. Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. EM darragh@sfsu.edu NR 0 TC 0 Z9 0 U1 0 U2 0 PU OXFORD UNIV PRESS INC PI CARY PA JOURNALS DEPT, 2001 EVANS RD, CARY, NC 27513 USA SN 1540-7063 J9 INTEGR COMP BIOL JI Integr. Comp. Biol. PD APR PY 2013 VL 53 SU 1 BP E265 EP E265 PG 1 WC Zoology SC Zoology GA 117ZG UT WOS:000316991402120 ER PT J AU Diaz, MC Thacker, RWT Redmond, N Collins, AG Marino, NEM Venezuela, U AF Diaz, M. C. Thacker, R. W. T. Redmond, N. Collins, A. G. Museo Marino, N. E. Venezuela, U. TI Don t judge a book by its cover: Discovering two new Verongida genera (Class Demospongiae, Porifera) SO INTEGRATIVE AND COMPARATIVE BIOLOGY LA English DT Meeting Abstract CT Annual Meeting of the Society-for-Integrative-and-Comparative-Biology (SICB) CY JAN 03-07, 2013 CL San Francisco, CA SP Soc Integrat & Comparat Biol (SICB) C1 U Alabama, Birmingham, AL USA. Smithsonian Inst, NMNH, Washington, DC 20560 USA. EM taxochica@gmail.com NR 0 TC 0 Z9 0 U1 0 U2 3 PU OXFORD UNIV PRESS INC PI CARY PA JOURNALS DEPT, 2001 EVANS RD, CARY, NC 27513 USA SN 1540-7063 J9 INTEGR COMP BIOL JI Integr. Comp. Biol. PD APR PY 2013 VL 53 SU 1 BP E52 EP E52 PG 1 WC Zoology SC Zoology GA 117ZG UT WOS:000316991400209 ER PT J AU Faircloth, BC Gowaty, PA Drummond, H Winker, K Glenn, TC AF Faircloth, B. C. Gowaty, P. A. Drummond, H. Winker, K. Glenn, T. C. TI Ultraconserved elements are abundant, universal markers for population genetic and behavioral studies SO INTEGRATIVE AND COMPARATIVE BIOLOGY LA English DT Meeting Abstract CT Annual Meeting of the Society-for-Integrative-and-Comparative-Biology (SICB) CY JAN 03-07, 2013 CL San Francisco, CA SP Soc Integrat & Comparat Biol (SICB) C1 Univ Calif Los Angeles, Los Angeles, CA USA. Smithsonian Trop Res Inst, Panama City, Panama. Univ Nacl Autonoma Mexico, Mexico City 04510, DF, Mexico. Univ Georgia, Athens, GA 30602 USA. EM brant@faircloth-lab.org RI Winker, Kevin/M-2042-2014 OI Winker, Kevin/0000-0002-8985-8104 NR 0 TC 0 Z9 0 U1 0 U2 9 PU OXFORD UNIV PRESS INC PI CARY PA JOURNALS DEPT, 2001 EVANS RD, CARY, NC 27513 USA SN 1540-7063 J9 INTEGR COMP BIOL JI Integr. Comp. Biol. PD APR PY 2013 VL 53 SU 1 BP E66 EP E66 PG 1 WC Zoology SC Zoology GA 117ZG UT WOS:000316991400264 ER PT J AU Hajdu, E Lobo-Hajdu, G Cosme, B De Paula, T Redmond, NE Collins, AG Thacker, RW AF Hajdu, E. Lobo-Hajdu, G. Cosme, B. De Paula, T. Redmond, N. E. Collins, A. G. Thacker, R. W. TI Towards an Evolutionary Classification of Mycalina and Latrunculina (Poecilosclerida) SO INTEGRATIVE AND COMPARATIVE BIOLOGY LA English DT Meeting Abstract CT Annual Meeting of the Society-for-Integrative-and-Comparative-Biology (SICB) CY JAN 03-07, 2013 CL San Francisco, CA SP Soc Integrat & Comparat Biol (SICB) C1 Univ Fed Rio de Janeiro, BR-21941 Rio De Janeiro, Brazil. Univ Estado Rio de Janeiro, Rio De Janeiro, Brazil. Smithsonian Inst, Washington, DC 20560 USA. Univ Alabama, Tuscaloosa, AL 35487 USA. EM eduardo.hajdu@gmail.com RI Lobo-Hajdu, G/A-6709-2008; de Paula, Thiago/B-4301-2014; Hajdu, Eduardo/C-3863-2009 OI Lobo-Hajdu, G/0000-0001-7792-9609; de Paula, Thiago/0000-0003-4468-4996; NR 0 TC 0 Z9 0 U1 0 U2 1 PU OXFORD UNIV PRESS INC PI CARY PA JOURNALS DEPT, 2001 EVANS RD, CARY, NC 27513 USA SN 1540-7063 J9 INTEGR COMP BIOL JI Integr. Comp. Biol. PD APR PY 2013 VL 53 SU 1 BP E84 EP E84 PG 1 WC Zoology SC Zoology GA 117ZG UT WOS:000316991400334 ER PT J AU Hall, MI Kamilar, JM Kirk, EC Carrano, MT Iwaniuk, AN AF Hall, M., I Kamilar, J. M. Kirk, E. C. Carrano, M. T. Iwaniuk, A. N. TI The relationship between scleral ring morphology and activity pattern in birds and dinosaurs SO INTEGRATIVE AND COMPARATIVE BIOLOGY LA English DT Meeting Abstract CT Annual Meeting of the Society-for-Integrative-and-Comparative-Biology (SICB) CY JAN 03-07, 2013 CL San Francisco, CA SP Soc Integrat & Comparat Biol (SICB) C1 Midwestern Univ, Glendale, AZ USA. UT Austin, Austin, TX USA. Smithsonian Inst, Washington, DC 20560 USA. Univ Lethbridge, Lethbridge, AB T1K 3M4, Canada. EM mhallx1@midwestern.edu RI Carrano, Matthew/C-7601-2011 OI Carrano, Matthew/0000-0003-2129-1612 NR 0 TC 0 Z9 0 U1 0 U2 13 PU OXFORD UNIV PRESS INC PI CARY PA JOURNALS DEPT, 2001 EVANS RD, CARY, NC 27513 USA SN 1540-7063 J9 INTEGR COMP BIOL JI Integr. Comp. Biol. PD APR PY 2013 VL 53 SU 1 BP E292 EP E292 PG 1 WC Zoology SC Zoology GA 117ZG UT WOS:000316991402228 ER PT J AU Klautau, M Azevedo, F Lujan, BC Russo, CAM Collins, A AF Klautau, M. Azevedo, F. Condor Lujan, B. Russo, C. A. M. Collins, A. TI Calcarea evolution: morphology and molecules SO INTEGRATIVE AND COMPARATIVE BIOLOGY LA English DT Meeting Abstract CT Annual Meeting of the Society-for-Integrative-and-Comparative-Biology (SICB) CY JAN 03-07, 2013 CL San Francisco, CA SP Soc Integrat & Comparat Biol (SICB) C1 Univ Fed Rio de Janeiro, BR-21941 Rio De Janeiro, Brazil. Smithsonian Natl Museum Nat Hist, Washington, DC USA. EM mklautau@biologia.ufrj.br NR 0 TC 0 Z9 0 U1 0 U2 2 PU OXFORD UNIV PRESS INC PI CARY PA JOURNALS DEPT, 2001 EVANS RD, CARY, NC 27513 USA SN 1540-7063 J9 INTEGR COMP BIOL JI Integr. Comp. Biol. PD APR PY 2013 VL 53 SU 1 BP E112 EP E112 PG 1 WC Zoology SC Zoology GA 117ZG UT WOS:000316991400447 ER PT J AU Kuwahara, A Meyer, C Collins, A AF Kuwahara, A. Meyer, C. Collins, A. TI Assessing Autonomous Reef Monitoring Structures (ARMS) as Biodiversity Monitors SO INTEGRATIVE AND COMPARATIVE BIOLOGY LA English DT Meeting Abstract CT Annual Meeting of the Society-for-Integrative-and-Comparative-Biology (SICB) CY JAN 03-07, 2013 CL San Francisco, CA SP Soc Integrat & Comparat Biol (SICB) C1 Humboldt State Univ, Arcata, CA USA. Smithsonian Inst, Washington, DC 20560 USA. NOAA NMFS, Silver Spring, MD USA. EM aak23@humboldt.edu NR 0 TC 0 Z9 0 U1 1 U2 11 PU OXFORD UNIV PRESS INC PI CARY PA JOURNALS DEPT, 2001 EVANS RD, CARY, NC 27513 USA SN 1540-7063 J9 INTEGR COMP BIOL JI Integr. Comp. Biol. PD APR PY 2013 VL 53 SU 1 BP E119 EP E119 PG 1 WC Zoology SC Zoology GA 117ZG UT WOS:000316991401010 ER PT J AU Maayan, I Ritzman, TB Hutchins, ED Stapley, J Lasku, E Eckalbar, WL Wilson-Rawls, J Huentelman, MJ Bermingham, E Hsieh, ST Fisher, RE Kusumi, K AF Maayan, I Ritzman, T. B. Hutchins, E. D. Stapley, J. Lasku, E. Eckalbar, W. L. Wilson-Rawls, J. Huentelman, M. J. Bermingham, E. Hsieh, S. T. Fisher, R. E. Kusumi, K. TI Comparative appendicular osteology and evolutionary genetics of Panamanian anoles with divergent locomotor strategies SO INTEGRATIVE AND COMPARATIVE BIOLOGY LA English DT Meeting Abstract CT Annual Meeting of the Society-for-Integrative-and-Comparative-Biology (SICB) CY JAN 03-07, 2013 CL San Francisco, CA SP Soc Integrat & Comparat Biol (SICB) C1 Arizona State Univ, Tempe, AZ 85287 USA. Smithsonian Trop Res Inst, Balboa, Panama. Temple Univ, Philadelphia, PA 19122 USA. Arizona Coll Med Phoenix, Phoenix, AZ USA. EM kenro.kusumi@asu.edu NR 0 TC 0 Z9 0 U1 1 U2 5 PU OXFORD UNIV PRESS INC PI CARY PA JOURNALS DEPT, 2001 EVANS RD, CARY, NC 27513 USA SN 1540-7063 J9 INTEGR COMP BIOL JI Integr. Comp. Biol. PD APR PY 2013 VL 53 SU 1 BP E320 EP E320 PG 1 WC Zoology SC Zoology GA 117ZG UT WOS:000316991402338 ER PT J AU Morrow, CC Redmond, NE Picton, BE Allcock, AL Sigwart, JD Maggs, CA AF Morrow, C. C. Redmond, N. E. Picton, B. E. Allcock, A. L. Sigwart, J. D. Maggs, C. A. TI Molecular phylogenies support homoplasy of multiple morphological characters used in the taxonomy of Heteroscleromorpha (Porifera: Demospongiae) SO INTEGRATIVE AND COMPARATIVE BIOLOGY LA English DT Meeting Abstract CT Annual Meeting of the Society-for-Integrative-and-Comparative-Biology (SICB) CY JAN 03-07, 2013 CL San Francisco, CA SP Soc Integrat & Comparat Biol (SICB) C1 Queens Univ Belfast, Belfast BT7 1NN, Antrim, North Ireland. NMNH, Washington, DC USA. Smithsonian Inst, Washington, DC 20560 USA. Natl Museums No Ireland, Holywood, North Ireland. Natl Univ Ireland Galway, Ryan Inst, Dept Zool, Galway, Ireland. EM christinemorrow@gmail.com RI Allcock, Louise/A-7359-2012 OI Allcock, Louise/0000-0002-4806-0040 NR 0 TC 0 Z9 0 U1 0 U2 3 PU OXFORD UNIV PRESS INC PI CARY PA JOURNALS DEPT, 2001 EVANS RD, CARY, NC 27513 USA SN 1540-7063 J9 INTEGR COMP BIOL JI Integr. Comp. Biol. PD APR PY 2013 VL 53 SU 1 BP E149 EP E149 PG 1 WC Zoology SC Zoology GA 117ZG UT WOS:000316991401132 ER PT J AU Potvin, J Goldbogen, JA Shadwick, RE Pyenson, ND AF Potvin, J. Goldbogen, J. A. Shadwick, R. E. Pyenson, N. D. TI Fish versus krill Comparing the energetic costs of engulfment by rorqual whales lunge-feeding on slow and fast prey SO INTEGRATIVE AND COMPARATIVE BIOLOGY LA English DT Meeting Abstract CT Annual Meeting of the Society-for-Integrative-and-Comparative-Biology (SICB) CY JAN 03-07, 2013 CL San Francisco, CA SP Soc Integrat & Comparat Biol (SICB) C1 St Louis Univ, St Louis, MO 63103 USA. Univ British Columbia, Vancouver, BC V5Z 1M9, Canada. Smithsonian Inst, Washington, DC 20560 USA. EM potvinj@slu.edu NR 0 TC 0 Z9 0 U1 1 U2 8 PU OXFORD UNIV PRESS INC PI CARY PA JOURNALS DEPT, 2001 EVANS RD, CARY, NC 27513 USA SN 1540-7063 J9 INTEGR COMP BIOL JI Integr. Comp. Biol. PD APR PY 2013 VL 53 SU 1 BP E171 EP E171 PG 1 WC Zoology SC Zoology GA 117ZG UT WOS:000316991401219 ER PT J AU Rader, JA Newsome, SD Chesser, RT Martinez Del Rio, C AF Rader, J. A. Newsome, S. D. Chesser, R. T. Martinez Del Rio, C. TI Phenotype-environment correlations in Cinclodes ovenbirds: Linking morphology to isotopic niche SO INTEGRATIVE AND COMPARATIVE BIOLOGY LA English DT Meeting Abstract CT Annual Meeting of the Society-for-Integrative-and-Comparative-Biology (SICB) CY JAN 03-07, 2013 CL San Francisco, CA SP Soc Integrat & Comparat Biol (SICB) C1 Univ Wyoming, Laramie, WY 82071 USA. Natl Museum Nat Hist, Washington, DC USA. Smithsonian Inst, Washington, DC 20560 USA. EM jrader@uwyo.edu NR 0 TC 0 Z9 0 U1 0 U2 5 PU OXFORD UNIV PRESS INC PI CARY PA JOURNALS DEPT, 2001 EVANS RD, CARY, NC 27513 USA SN 1540-7063 J9 INTEGR COMP BIOL JI Integr. Comp. Biol. PD APR PY 2013 VL 53 SU 1 BP E355 EP E355 PG 1 WC Zoology SC Zoology GA 117ZG UT WOS:000316991402478 ER PT J AU Redmond, NE Morrow, CC Thacker, RW Diaz, MC Boury-Esnualt, N Cardenas, P Hajdu, E Lobo-Hajdu, G Picton, BE Collins, AG AF Redmond, N. E. Morrow, C. C. Thacker, R. W. Diaz, M. C. Boury-Esnualt, N. Cardenas, P. Hajdu, E. Lobo-Hajdu, G. Picton, B. E. Collins, A. G. TI New 18S rDNA Sequence Data Suggest Exciting New Hypotheses for Internal Relationships of Demospongiae (Phylum Porifera). SO INTEGRATIVE AND COMPARATIVE BIOLOGY LA English DT Meeting Abstract CT Annual Meeting of the Society-for-Integrative-and-Comparative-Biology (SICB) CY JAN 03-07, 2013 CL San Francisco, CA SP Soc Integrat & Comparat Biol (SICB) C1 Smithsonian Inst, NMNH, Washington, DC 20560 USA. Queens Univ Belfast, Belfast, Antrim, North Ireland. Univ Alabama Birmingham, Birmingham, AL USA. Univ Aix Marseille, Marseille, France. Uppsala Univ, Uppsala, Sweden. Univ Fed Rio de Janeiro, Museu Nacl, BR-21941 Rio De Janeiro, Brazil. Univ Estado Rio de Janeiro, Rio De Janeiro, Brazil. EM redmondn@si.edu RI Lobo-Hajdu, G/A-6709-2008; Hajdu, Eduardo/C-3863-2009 OI Lobo-Hajdu, G/0000-0001-7792-9609; NR 0 TC 1 Z9 1 U1 0 U2 5 PU OXFORD UNIV PRESS INC PI CARY PA JOURNALS DEPT, 2001 EVANS RD, CARY, NC 27513 USA SN 1540-7063 J9 INTEGR COMP BIOL JI Integr. Comp. Biol. PD APR PY 2013 VL 53 SU 1 BP E176 EP E176 PG 1 WC Zoology SC Zoology GA 117ZG UT WOS:000316991401240 ER PT J AU Schachner, ER Lyson, TR Farmer, CG AF Schachner, E. R. Lyson, T. R. Farmer, C. G. TI Pulmonary anatomy and the evolution of turtles SO INTEGRATIVE AND COMPARATIVE BIOLOGY LA English DT Meeting Abstract CT Annual Meeting of the Society-for-Integrative-and-Comparative-Biology (SICB) CY JAN 03-07, 2013 CL San Francisco, CA SP Soc Integrat & Comparat Biol (SICB) C1 Univ Utah, Salt Lake City, UT 84112 USA. Smithsonian Inst, Washington, DC 20560 USA. EM eschachner@gmail.com NR 0 TC 0 Z9 0 U1 1 U2 4 PU OXFORD UNIV PRESS INC PI CARY PA JOURNALS DEPT, 2001 EVANS RD, CARY, NC 27513 USA SN 1540-7063 J9 INTEGR COMP BIOL JI Integr. Comp. Biol. PD APR PY 2013 VL 53 SU 1 BP E366 EP E366 PG 1 WC Zoology SC Zoology GA 117ZG UT WOS:000316991402521 ER PT J AU Seymoure, BM Mcmillan, WO Rutowski, RL AF Seymoure, B. M. Mcmillan, W. O. Rutowski, R. L. TI Convergence and Divergence of Eye Morphology in Mimetic Butterflies SO INTEGRATIVE AND COMPARATIVE BIOLOGY LA English DT Meeting Abstract CT Annual Meeting of the Society-for-Integrative-and-Comparative-Biology (SICB) CY JAN 03-07, 2013 CL San Francisco, CA SP Soc Integrat & Comparat Biol (SICB) C1 [Seymoure, B. M.; Mcmillan, W. O.; Rutowski, R. L.] Arizona State Univ, Smithsonian Trop Res Inst, Tempe, AZ 85287 USA. EM brett.seymoure@gmail.com NR 0 TC 0 Z9 0 U1 0 U2 3 PU OXFORD UNIV PRESS INC PI CARY PA JOURNALS DEPT, 2001 EVANS RD, CARY, NC 27513 USA SN 1540-7063 J9 INTEGR COMP BIOL JI Integr. Comp. Biol. PD APR PY 2013 VL 53 SU 1 BP E194 EP E194 PG 1 WC Zoology SC Zoology GA 117ZG UT WOS:000316991401312 ER PT J AU Shadwick, RE Whale, JC Lin, SC Goldbogen, JA Pyensnon, ND AF Shadwick, R. E. Whale, J. C. Lin, S. C. Goldbogen, J. A. Pyensnon, N. D. TI Mechanical design in fin whale mandibles SO INTEGRATIVE AND COMPARATIVE BIOLOGY LA English DT Meeting Abstract CT Annual Meeting of the Society-for-Integrative-and-Comparative-Biology (SICB) CY JAN 03-07, 2013 CL San Francisco, CA SP Soc Integrat & Comparat Biol (SICB) C1 Univ British Columbia, Vancouver, BC V5Z 1M9, Canada. Smithsonian Inst, Washington, DC 20560 USA. EM shadwick@zoology.ubc.ca NR 0 TC 0 Z9 0 U1 0 U2 4 PU OXFORD UNIV PRESS INC PI CARY PA JOURNALS DEPT, 2001 EVANS RD, CARY, NC 27513 USA SN 1540-7063 J9 INTEGR COMP BIOL JI Integr. Comp. Biol. PD APR PY 2013 VL 53 SU 1 BP E368 EP E368 PG 1 WC Zoology SC Zoology GA 117ZG UT WOS:000316991402530 ER PT J AU Shadwick, RE Goldbogen, JA Potvin, J Pyenson, ND Vogl, AW AF Shadwick, R. E. Goldbogen, J. A. Potvin, J. Pyenson, N. D. Vogl, A. W. TI Novel muscle and connective tissue design controls engulfment volume in lunge-feeding whales SO INTEGRATIVE AND COMPARATIVE BIOLOGY LA English DT Meeting Abstract CT Annual Meeting of the Society-for-Integrative-and-Comparative-Biology (SICB) CY JAN 03-07, 2013 CL San Francisco, CA SP Soc Integrat & Comparat Biol (SICB) C1 Univ British Columbia, Vancouver, BC V5Z 1M9, Canada. St Louis Univ, St Louis, MO 63103 USA. Smithsonian Inst, Washington, DC 20560 USA. EM shadwick@zoology.ubc.ca NR 0 TC 0 Z9 0 U1 1 U2 3 PU OXFORD UNIV PRESS INC PI CARY PA JOURNALS DEPT, 2001 EVANS RD, CARY, NC 27513 USA SN 1540-7063 J9 INTEGR COMP BIOL JI Integr. Comp. Biol. PD APR PY 2013 VL 53 SU 1 BP E195 EP E195 PG 1 WC Zoology SC Zoology GA 117ZG UT WOS:000316991401313 ER PT J AU Sheets, EA Ruiz, GM Rocha, RM Cohen, CS AF Sheets, E. A. Ruiz, G. M. Rocha, R. M. Cohen, C. S. TI Global population structure of the widely introduced tropical ascidian Botrylloides nigrum SO INTEGRATIVE AND COMPARATIVE BIOLOGY LA English DT Meeting Abstract CT Annual Meeting of the Society-for-Integrative-and-Comparative-Biology (SICB) CY JAN 03-07, 2013 CL San Francisco, CA SP Soc Integrat & Comparat Biol (SICB) C1 San Francisco State Univ, Romberg Tiburon Ctr Environm Studies, San Francisco, CA USA. San Francisco State Univ, Dept Biol, San Francisco, CA USA. Smithsonian Environm Res Ctr, Rohnert Pk, CA USA. Univ Fed Parana, Dept Zool, BR-80060000 Curitiba, Parana, Brazil. EM bethsheets@gmail.com NR 0 TC 0 Z9 0 U1 1 U2 8 PU OXFORD UNIV PRESS INC PI CARY PA JOURNALS DEPT, 2001 EVANS RD, CARY, NC 27513 USA SN 1540-7063 J9 INTEGR COMP BIOL JI Integr. Comp. Biol. PD APR PY 2013 VL 53 SU 1 BP E369 EP E369 PG 1 WC Zoology SC Zoology GA 117ZG UT WOS:000316991402536 ER PT J AU Slater, GJ Friscia, AR AF Slater, G. J. Friscia, A. R. TI Where should we expect to find Early bursts of trait evolution? A case study using Carnivora. SO INTEGRATIVE AND COMPARATIVE BIOLOGY LA English DT Meeting Abstract CT Annual Meeting of the Society-for-Integrative-and-Comparative-Biology (SICB) CY JAN 03-07, 2013 CL San Francisco, CA SP Soc Integrat & Comparat Biol (SICB) C1 Smithsonian Inst, Washington, DC 20560 USA. Univ Calif Los Angeles, Los Angeles, CA USA. EM gslater@ucla.edu NR 0 TC 0 Z9 0 U1 0 U2 0 PU OXFORD UNIV PRESS INC PI CARY PA JOURNALS DEPT, 2001 EVANS RD, CARY, NC 27513 USA SN 1540-7063 J9 INTEGR COMP BIOL JI Integr. Comp. Biol. PD APR PY 2013 VL 53 SU 1 BP E200 EP E200 PG 1 WC Zoology SC Zoology GA 117ZG UT WOS:000316991401336 ER PT J AU Starr, MJ Collin, R AF Starr, M. J. Collin, R. TI Enzyme Activity in Early Life Stages of Planktotrophic Slipper Snails (Gastropoda: Calyptraeidae) SO INTEGRATIVE AND COMPARATIVE BIOLOGY LA English DT Meeting Abstract CT Annual Meeting of the Society-for-Integrative-and-Comparative-Biology (SICB) CY JAN 03-07, 2013 CL San Francisco, CA SP Soc Integrat & Comparat Biol (SICB) C1 [Starr, M. J.; Collin, R.] Smithsonian Trop Res Inst, Panama City, Panama. EM mjs3424@louisiana.edu NR 0 TC 0 Z9 0 U1 0 U2 0 PU OXFORD UNIV PRESS INC PI CARY PA JOURNALS DEPT, 2001 EVANS RD, CARY, NC 27513 USA SN 1540-7063 J9 INTEGR COMP BIOL JI Integr. Comp. Biol. PD APR PY 2013 VL 53 SU 1 BP E375 EP E375 PG 1 WC Zoology SC Zoology GA 117ZG UT WOS:000316991402559 ER PT J AU Nawrocki, AM Collins, AG Hirano, YM Schuchert, P Cartwright, P AF Nawrocki, Annalise M. Collins, Allen G. Hirano, Yayoi M. Schuchert, Peter Cartwright, Paulyn TI Phylogenetic placement of Hydra and relationships within Aplanulata (Cnidaria: Hydrozoa) SO MOLECULAR PHYLOGENETICS AND EVOLUTION LA English DT Article DE Aplanulata; Cnidaria; Hydrozoa; Molecular phylogenetics; Hydra ID MULTIPLE SEQUENCE ALIGNMENT; EUROPEAN ATHECATE HYDROIDS; FUKAURAHYDRA-ANTHOFORMIS; SUBSTITUTION MODELS; MEDUSAE HYDROZOA; PHYLUM CNIDARIA; STEM-CELLS; RDNA DATA; N-SP; MITOCHONDRIAL AB The model organism Hydra belongs to the hydrozoan clade Aplanulata. Despite being a popular model system for development, little is known about the phylogenetic placement of this taxon or the relationships of its closest relatives. Previous studies have been conflicting regarding sister group relationships and have been unable to resolve deep nodes within the clade. In addition, there are several putative Aplanulata taxa that have never been sampled for molecular data or analyzed using multiple markers. Here, we combine the fast-evolving cytochrome oxidase 1 (CO1) mitochondrial marker with mitochondrial 16S, nuclear small ribosomal subunit (18S, SSU) and large ribosomal subunit (28S, LSU) sequences to examine relationships within the clade Aplanulata. We further discuss the relative contribution of four different molecular markers to resolving phylogenetic relationships within Aplanulata. Lastly, we report morphological synapomorphies for some of the major Aplanulata genera and families, and suggest new taxonomic classifications for two species of Aplanulata, Fukaurahydra anthoformis and Corymorpha intermedia, based on a preponderance of molecular and morphological data that justify the designation of these species to different genera. (C) 2012 Elsevier Inc. All rights reserved. C1 [Nawrocki, Annalise M.] Pomona Coll, Claremont, CA 91711 USA. [Collins, Allen G.] Smithsonian Inst, Natl Museum Nat Hist, NMFS, Natl Systemat Lab, Washington, DC 20013 USA. [Hirano, Yayoi M.] Chiba Univ, Dept Biol, Grad Sch Sci, Inage Ku, Chiba 2638522, Japan. [Schuchert, Peter] Museum Hist Nat, CH-1211 Geneva 6, Switzerland. [Nawrocki, Annalise M.; Cartwright, Paulyn] Univ Kansas, Lawrence, KS 66045 USA. RP Nawrocki, AM (reprint author), Pomona Coll, RC Seaver Biol Bldg,175 W 6th St, Claremont, CA 91711 USA. EM annarocky@gmail.com FU NSF [AToL EF-0531779, DEB-0953571, DDIG DEB-0910211]; University of Kansas Madison; Lila Self Graduate Fellowship FX We thank M.S. Barbeitos for the use of unpublished secondary structure models for 18S and 28S for Cnidaria, G.Paulay for providing specimens of H. parva, and R. Richardson for assistance with CO1 amplification of some samples. We are grateful to A.L. Crowther and three anonymous reviewers whose comments improved earlier versions of this manuscript. This work was supported by NSF Grant AToL EF-0531779 to P.C. and A.G.C., the NSF Grant DEB-0953571 to P.C., the University of Kansas Madison and Lila Self Graduate Fellowship to A.M.N., and the NSF Grant DDIG DEB-0910211 to A.M.N. and P.C. NR 69 TC 7 Z9 7 U1 0 U2 21 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 1055-7903 EI 1095-9513 J9 MOL PHYLOGENET EVOL JI Mol. Phylogenet. Evol. PD APR PY 2013 VL 67 IS 1 BP 60 EP 71 DI 10.1016/j.ympev.2012.12.016 PG 12 WC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity SC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity GA 118LY UT WOS:000317028200008 PM 23280366 ER PT J AU Grinolds, MS Hong, S Maletinsky, P Luan, L Lukin, MD Walsworth, RL Yacoby, A AF Grinolds, M. S. Hong, S. Maletinsky, P. Luan, L. Lukin, M. D. Walsworth, R. L. Yacoby, A. TI Nanoscale magnetic imaging of a single electron spin under ambient conditions SO NATURE PHYSICS LA English DT Article ID ROOM-TEMPERATURE; FORCE MICROSCOPY; RESONANCE; DIAMOND; RESOLUTION; CENTERS; ECHO AB The detection of ensembles of spins under ambient conditions has revolutionized the biological, chemical and physical sciences through magnetic resonance imaging(1) and nuclear magnetic resonance(2,3). Pushing sensing capabilities to the individual-spin level would enable unprecedented applications such as single-molecule structural imaging; however, the weak magnetic fields from single spins are undetectable by conventional far-field resonance techniques(4). In recent years, there has been a considerable effort to develop nanoscale scanning magnetometers(5-8), which are able to measure fewer spins by bringing the sensor in close proximity to its target. The most sensitive of these magnetometers generally require low temperatures for operation, but the ability to measure under ambient conditions (standard temperature and pressure) is critical for many imaging applications, particularly in biological systems. Here we demonstrate detection and nanoscale imaging of the magnetic field from an initialized single electron spin under ambient conditions using a scanning nitrogen-vacancy magnetometer. Real-space, quantitative magnetic-field images are obtained by deterministically scanning our nitrogen-vacancy magnetometer 50 nm above a target electron spin, while measuring the local magnetic field using dynamically decoupled magnetometry protocols. We discuss how this single-spin detection enables the study of a variety of room-temperature phenomena in condensed-matter physics with an unprecedented combination of spatial resolution and spin sensitivity. C1 [Grinolds, M. S.; Maletinsky, P.; Luan, L.; Lukin, M. D.; Walsworth, R. L.; Yacoby, A.] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. [Hong, S.] Harvard Univ, Sch Engn & Appl Sci, Cambridge, MA 02138 USA. [Maletinsky, P.] Univ Basel, Dept Phys, CH-4056 Basel, Switzerland. [Walsworth, R. L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Yacoby, A (reprint author), Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. EM yacoby@physics.harvard.edu RI Hong, Sungkun/D-3282-2014; Maletinsky, Patrick/L-1851-2015 OI Hong, Sungkun/0000-0003-0985-6641; Maletinsky, Patrick/0000-0003-1699-388X FU Department of Defense; National Science Foundation; Kwanjeong Scholarship Foundation; Swiss National Science Foundation; DARPA; MURI QuISM FX We gratefully acknowledge Element Six, for providing diamond samples for our NV sensors and targets. M.S.G. is supported through fellowships from the Department of Defense (NDSEG programme) and the National Science Foundation. S.H. acknowledges support from the Kwanjeong Scholarship Foundation, and P.M. thanks the Swiss National Science Foundation for fellowship funding. This work was supported by the DARPA QuEST and QuASAR programmes and the MURI QuISM. NR 31 TC 125 Z9 127 U1 12 U2 162 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 1745-2473 J9 NAT PHYS JI Nat. Phys. PD APR PY 2013 VL 9 IS 4 BP 215 EP 219 DI 10.1038/NPHYS2543 PG 5 WC Physics, Multidisciplinary SC Physics GA 118BJ UT WOS:000316997100012 ER PT J AU Wright, EL Black, CR Cheesman, AW Turner, BL Sjogersten, S AF Wright, E. L. Black, C. R. Cheesman, A. W. Turner, B. L. Sjoegersten, S. TI Impact of Simulated Changes in Water Table Depth on Ex Situ Decomposition of Leaf Litter from a Neotropical Peatland SO WETLANDS LA English DT Article DE Litter decomposition; Nutrient cycling; Tropical peatland; Vegetation communities ID DIFFERENT NUTRIENT CONDITIONS; SWAMP FOREST; COSTA-RICA; PLANT DECOMPOSITION; MICROBIAL BIOMASS; ENZYME-ACTIVITIES; CARBON STORAGE; COASTAL-PLAIN; WETLAND SOILS; PHOSPHORUS AB Although water table depth is commonly regarded as the primary determinant of litter decomposition rate in tropical peatlands, this has rarely been tested experimentally. This study explored the influence of flooding on decomposition of litter from three dominant plant species in a neotropical peatland. The non-flooded treatment reduced the mass remaining after 14 months from 84 to 81 % for Raphia taedigera, 65 to 58 % for Campnosperma panamensis, and 69 to 58 % for Cyperus sp. The proportions of carbon, nitrogen and phosphorus in the labile, semi-labile and recalcitrant carbon pools, did not reliably predict differences among species in the mass loss rate of litter. Phosphorus was rapidly lost from litter, while carbon losses, including soluble carbon, were slower, but significant for all fractions. The non-flooded treatment substantially reduced the quantity of C remaining in the residue fraction of leaf litter after 12 weeks, with 31, 19 and 6 % less remaining in the non-flooded treatment for R. taedigera, C. panamensis and Cyperus sp. This suggests that lower water table depth on litter decay increase degradation of mainly aliphatic and aromatic carbon in the residual fraction. Thus, although lowering the water table increased decomposition, the chemical composition of litter clearly influences peat accumulation. C1 [Wright, E. L.; Black, C. R.; Sjoegersten, S.] Univ Nottingham, Sch Biosci, Loughborough LE12 5RD, Leics, England. [Cheesman, A. W.; Turner, B. L.] Smithsonian Trop Res Inst, Panama City 084303092, Panama. RP Sjogersten, S (reprint author), Univ Nottingham, Sch Biosci, Sutton Bonington Campus, Loughborough LE12 5RD, Leics, England. EM sofie.sjogersten@nottingham.ac.uk RI Turner, Benjamin/E-5940-2011; Cheesman, Alexander/H-5918-2013 OI Turner, Benjamin/0000-0002-6585-0722; Cheesman, Alexander/0000-0003-3931-5766 FU UK Biotechnology and Biological Sciences Research Council; University of Nottingham; USDA-CREES National Research Initiative [2004-35107-14918] FX Emma Wright acknowledges the award of a PhD scholarship from the UK Biotechnology and Biological Sciences Research Council. The project was also supported by a University of Nottingham New Investigator grant. Alexander Cheesman was funded by a grant from the USDA-CREES National Research Initiative (No. 2004-35107-14918). We thank Darren Hepworth for laboratory assistance and staff at the Smithsonian Tropical Research Institute station in Bocas del Toro for logistical support. NR 56 TC 8 Z9 8 U1 3 U2 60 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0277-5212 J9 WETLANDS JI Wetlands PD APR PY 2013 VL 33 IS 2 BP 217 EP 226 DI 10.1007/s13157-012-0369-6 PG 10 WC Ecology; Environmental Sciences SC Environmental Sciences & Ecology GA 113AL UT WOS:000316638000003 ER PT J AU Gervais, C Languille, MA Reguer, S Gillet, M Vicenzi, EP Chagnot, S Baudelet, F Bertrand, L AF Gervais, Claire Languille, Marie-Angelique Reguer, Solenn Gillet, Martine Vicenzi, Edward P. Chagnot, Sebastien Baudelet, Francois Bertrand, Loic TI "Live" Prussian blue fading by time-resolved X-ray absorption spectroscopy SO APPLIED PHYSICS A-MATERIALS SCIENCE & PROCESSING LA English DT Article AB Prussian blue (PB) is an artists' pigment that has been frequently used in many artworks but poses several problems of conservation because of its fading under light and anoxia treatment. PB fading is due to the reduction of iron(III) into iron(II) and depends a lot on the object investigated. Due to the complexity of the structure, the precise physico-chemical mechanisms behind the redox process remain obscure. In this paper, we present a procedure to investigate light- and anoxia-induced fading of PB-paper samples by means of time resolved X-ray absorption spectroscopy performed at the Fe K-edge. A system composed of a visible light source and a flux-controlled environmental cell allowed light, gas and humidity to be modified in situ. The synchrotron X-ray beam was evidenced to induce a reduction of PB and to play a major role in the kinetics. The analysis of the PB fading kinetics of a sample submitted to various gas and light environments showed that both synchrotron beam and anoxia were influencing PB reduction in a correlated way. In comparison, light was found to play a minor role. Finally, we have demonstrated that the type of paper substrate could influence significantly the kinetics of reduction. Several hypotheses to explain the correlation between PB reduction mechanism and substrate are presented. C1 [Gervais, Claire; Vicenzi, Edward P.] Smithsonian Inst Museum Conservat Inst, Suitland, MD 20746 USA. [Languille, Marie-Angelique; Bertrand, Loic] Synchrotron SOLEIL, IPANEMA, USR CNRS MCC 3461, F-91192 Gif Sur Yvette, France. [Bertrand, Loic] Synchrotron SOLEIL, F-91192 Gif Sur Yvette, France. [Reguer, Solenn] Synchrotron SOLEIL, DiffAbs Beamline, F-91192 Gif Sur Yvette, France. [Gillet, Martine] Museum Natl Hist Nat, Ctr Rech Conservat Collect, F-75005 Paris, France. [Chagnot, Sebastien; Baudelet, Francois] Synchrotron SOLEIL, ODE Beamline, F-91192 Gif Sur Yvette, France. RP Gervais, C (reprint author), Bern Univ Arts, Fellerstr 11, CH-3027 Bern, Switzerland. EM claire.gervais@hkb.bfh.ch RI Gervais, Claire/E-5505-2012 OI Gervais, Claire/0000-0003-2433-5537 FU Swiss National Science Foundation through SNSF [138986] FX We would like to acknowledge Lucie Nataf of the ODE team and Frederic Picca for his joyful and spontaneous help in python programming. Thanks also to the team of the Soleil Chemistry Laboratory for help in preparing PB-paper samples and Matjia Strlic for sharing with us interesting points on paper aging process. We thank Robert J. Koestler for suggesting us to investigate PB fading in cultural artefacts. Claire Gervais thanks the Swiss National Science Foundation for partial funding through the SNSF Professorship grant 138986. This work has been developed as part of the IPANEMA/Smithsonian Institution agreement on science cooperation. NR 26 TC 7 Z9 7 U1 2 U2 32 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0947-8396 J9 APPL PHYS A-MATER JI Appl. Phys. A-Mater. Sci. Process. PD APR PY 2013 VL 111 IS 1 BP 15 EP 22 DI 10.1007/s00339-013-7581-y PG 8 WC Materials Science, Multidisciplinary; Physics, Applied SC Materials Science; Physics GA 105MS UT WOS:000316075700003 ER PT J AU Dunham, MM Arce, HG Allen, LE Evans, NJ Broekhoven-Fiene, H Chapman, NL Cieza, LA Gutermuth, RA Harvey, PM Hatchell, J Huard, TL Kirk, JM Matthews, BC Merin, B Miller, JF Peterson, DE Spezzi, L AF Dunham, Michael M. Arce, Hector G. Allen, Lori E. Evans, Neal J., II Broekhoven-Fiene, Hannah Chapman, Nicholas L. Cieza, Lucas A. Gutermuth, Robert A. Harvey, Paul M. Hatchell, Jennifer Huard, Tracy L. Kirk, Jason M. Matthews, Brenda C. Merin, Bruno Miller, Jennifer F. Peterson, Dawn E. Spezzi, Loredana TI THE LUMINOSITIES OF PROTOSTARS IN THE SPITZER c2d AND GOULD BELT LEGACY CLOUDS SO ASTRONOMICAL JOURNAL LA English DT Article DE stars: formation; stars: low-mass; stars: luminosity function, mass function; stars: protostars ID 1ST HYDROSTATIC CORE; YOUNG STELLAR OBJECTS; AURIGA MOLECULAR CLOUD; DUST CONTINUUM EMISSION; SELF-SIMILAR COLLAPSE; STAR-FORMING REGIONS; NEARBY DENSE CORES; INTERSTELLAR CLOUDS; SPACE-TELESCOPE; PROTOSTELLAR ENVELOPES AB Motivated by the long-standing "luminosity problem" in low-mass star formation whereby protostars are underluminous compared to theoretical expectations, we identify 230 protostars in 18 molecular clouds observed by two Spitzer Space Telescope Legacy surveys of nearby star-forming regions. We compile complete spectral energy distributions, calculate L-bol for each source, and study the protostellar luminosity distribution. This distribution extends over three orders of magnitude, from 0.01 L-circle dot to 69 L-circle dot, and has a mean and median of 4.3 L-circle dot and 1.3 L-circle dot, respectively. The distributions are very similar for Class 0 and Class I sources except for an excess of low luminosity (L-bol <= 0.5 L-circle dot) Class I sources compared to Class 0. 100 out of the 230 protostars (43%) lack any available data in the far-infrared and submillimeter (70 mu m < lambda < 850 mu m) and have L-bol underestimated by factors of 2.5 on average, and up to factors of 8-10 in extreme cases. Correcting these underestimates for each source individually once additional data becomes available will likely increase both the mean and median of the sample by 35%-40%. We discuss and compare our results to several recent theoretical studies of protostellar luminosities and show that our new results do not invalidate the conclusions of any of these studies. As these studies demonstrate that there is more than one plausible accretion scenario that can match observations, future attention is clearly needed. The better statistics provided by our increased data set should aid such future work. C1 [Dunham, Michael M.; Arce, Hector G.] Yale Univ, Dept Astron, New Haven, CT 06520 USA. [Allen, Lori E.] Natl Opt Astron Observ, Tucson, AZ 85726 USA. [Evans, Neal J., II; Harvey, Paul M.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA. [Broekhoven-Fiene, Hannah; Matthews, Brenda C.] Natl Res Council Canada, Herzberg Inst, Victoria, BC V9E 2E7, Canada. [Chapman, Nicholas L.] Northwestern Univ, Dept Phys & Astron, Ctr Interdisciplinary Explorat & Res Astrophys, Evanston, IL 60208 USA. [Cieza, Lucas A.] Univ Hawaii Manoa, Inst Astron, Honolulu, HI 96822 USA. [Gutermuth, Robert A.] Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA. [Hatchell, Jennifer] Univ Exeter, Astrophys Grp, Exeter EX4 4QL, Devon, England. [Huard, Tracy L.; Miller, Jennifer F.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Kirk, Jason M.] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales. [Merin, Bruno] ESAC ESA, Herschel Sci Ctr, E-28691 Madrid, Spain. [Miller, Jennifer F.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Peterson, Dawn E.] Space Sci Inst, Boulder, CO 80301 USA. [Spezzi, Loredana] European So Observ, D-85748 Garching, Germany. RP Dunham, MM (reprint author), Yale Univ, Dept Astron, POB 208101, New Haven, CT 06520 USA. EM michael.dunham@yale.edu FU NASA/JPL Herschel OT1 grant; National Science Foundation [AST-0845619, AST-1109116]; National Aeronautics and Space Administration FX We thank Erin Kryukova, Tom Megeath, Chris McKee, Stella Offner, and Phil Myers for reading a draft in advance of publication and providing helpful comments. This work is based primarily on observations obtained with the Spitzer Space Telescope, operated by the Jet Propulsion Laboratory, California Institute of Technology. It also uses 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. These data were provided by the NASA/IPAC Infrared Science Archive, which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with NASA. This research has made use of NASA's Astrophysics Data System (ADS) Abstract Service, and the SIMBAD database, operated at CDS, Strasbourg, France. M. M. D. acknowledges the support of a NASA/JPL Herschel OT1 grant. Additional support was provided by the NSF through grant AST-0845619 to H. G. A. N.J.E. acknowledges support from the NSF through grant AST-1109116. NR 122 TC 38 Z9 38 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 APR PY 2013 VL 145 IS 4 AR 94 DI 10.1088/0004-6256/145/4/94 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 107UW UT WOS:000316247300008 ER PT J AU Hughes, AM Hull, CLH Wilner, DJ Plambeck, RL AF Hughes, A. Meredith Hull, Charles L. H. Wilner, David J. Plambeck, Richard L. TI INTERFEROMETRIC UPPER LIMITS ON MILLIMETER POLARIZATION OF THE DISKS AROUND DG Tau, GM Aur, AND MWC 480 SO ASTRONOMICAL JOURNAL LA English DT Article DE magnetic fields; polarization; protoplanetary disks; stars: formation; stars: individual (DG Tau, GM Aur, MWC 480) ID MAIN-SEQUENCE EVOLUTION; PROTOPLANETARY DISKS; CIRCUMSTELLAR DISKS; MAGNETIC-FIELDS; GRAIN ALIGNMENT; STARS; EMISSION; DUST; MM; POLARIMETRY AB Millimeter-wavelength polarization measurements offer a promising method for probing the geometry of magnetic fields in circumstellar disks. Single dish observations and theoretical work have hinted that magnetic field geometries might be predominantly toroidal, and that disks should exhibit millimeter polarization fractions of 2%-3%. While subsequent work has not confirmed these high polarization fractions, either the wavelength of observation or the target sources differed from the original observations. Here we present new polarimetric observations of three nearby circumstellar disks at 2 '' resolution with the Submillimeter Array and the Combined Array for Research in Millimeter Astronomy. We reobserve GM Aur and DG Tau, the systems in which millimeter polarization detections have been claimed. Despite higher resolution and sensitivity at wavelengths similar to the previous observations, the new observations do not show significant polarization. We also add observations of a new HAeBe system, MWC 480. These observations demonstrate that a very low (less than or similar to 0.5%) polarization fraction is probably common at large (greater than or similar to 100 AU) scales in bright circumstellar disks. We suggest that high-resolution observations may be worthwhile to probe magnetic field structure on linear distances smaller than the disk scale height, as well as in regions closer to the star that may have larger MRI-induced magnetic field strengths. C1 [Hughes, A. Meredith; Hull, Charles L. H.; Plambeck, Richard L.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Hughes, A. Meredith; Hull, Charles L. H.; Plambeck, Richard L.] Univ Calif Berkeley, Radio Astron Lab, Berkeley, CA 94720 USA. [Hughes, A. Meredith] Wesleyan Univ, Van Vleck Observ, Dept Astron, Middletown, CT 06459 USA. [Wilner, David J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Hughes, AM (reprint author), Univ Calif Berkeley, Dept Astron, 601 Campbell Hall, Berkeley, CA 94720 USA. EM amhughes@wesleyan.edu FU Miller Institute for Basic Research in Science; NSF Graduate Fellowship FX We thank Jungyeon Cho for the use of his code to model the observations. A. M. H. is supported by a fellowship from the Miller Institute for Basic Research in Science. C. L. H. H. acknowledges support from an NSF Graduate Fellowship. Support for CARMA construction was derived from the states of California, Illinois, and Maryland, the James S. McDonnell Foundation, the Gordon and Betty Moore Foundation, the Kenneth T. and Eileen L. Norris Foundation, the University of Chicago, the Associates of the California Institute of Technology, and the National Science Foundation. Ongoing CARMA development and operations are supported by the National Science Foundation under a cooperative agreement, and by the CARMA partner universities. NR 28 TC 14 Z9 14 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 J9 ASTRON J JI Astron. J. PD APR PY 2013 VL 145 IS 4 AR 115 DI 10.1088/0004-6256/145/4/115 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 107UW UT WOS:000316247300029 ER PT J AU Parker, AH Buie, MW Osip, DJ Gwyn, SDJ Holman, MJ Borncamp, DM Spencer, JR Benecchi, SD Binzel, RP Demeo, FE Fabbro, S Fuentes, CI Gay, PL Kavelaars, JJ McLeod, BA Petit, JM Sheppard, SS Stern, SA Tholen, DJ Trilling, DE Ragozzine, DA Wasserman, LH AF Parker, Alex H. Buie, Marc W. Osip, David J. Gwyn, Stephen D. J. Holman, Matthew J. Borncamp, David M. Spencer, John R. Benecchi, Susan D. Binzel, Richard P. DeMeo, Francesca E. Fabbro, Sebastian Fuentes, Cesar I. Gay, Pamela L. Kavelaars, J. J. McLeod, Brian A. Petit, Jean-Marc Sheppard, Scott S. Stern, S. Alan Tholen, David J. Trilling, David E. Ragozzine, Darin A. Wasserman, Lawrence H. CA Ice Hunters TI 2011 HM102: DISCOVERY OF A HIGH-INCLINATION L5 NEPTUNE TROJAN IN THE SEARCH FOR A POST-PLUTO NEW HORIZONS TARGET SO ASTRONOMICAL JOURNAL LA English DT Article DE minor planets, asteroids: general ID KUIPER-BELT OBJECTS; POPULATIONS; COLORS; SYSTEM; PLANE AB We present the discovery of a long-term stable L5 (trailing) Neptune Trojan in data acquired to search for candidate trans-Neptunian objects for the New Horizons spacecraft to fly by during an extended post-Pluto mission. This Neptune Trojan, 2011 HM102, has the highest inclination (29 degrees.4) of any known member of this population. It is intrinsically brighter than any single L5 Jupiter Trojan at H-V similar to 8.18. We have determined its gri colors (a first for any L5 Neptune Trojan), which we find to be similar to the moderately red colors of the L4 Neptune Trojans, suggesting similar surface properties for members of both Trojan clouds. We also present colors derived from archival data for two L4 Neptune Trojans (2006 RJ(103) and 2007 VL305), better refining the overall color distribution of the population. In this document we describe the discovery circumstances, our physical characterization of 2011 HM102, and this object's implications for the Neptune Trojan population overall. Finally, we discuss the prospects for detecting 2011 HM102 from the New Horizons spacecraft during its close approach in mid- to late-2013. C1 [Parker, Alex H.; Holman, Matthew J.; McLeod, Brian A.; Ragozzine, Darin A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Buie, Marc W.; Borncamp, David M.; Spencer, John R.; Stern, S. Alan] SW Res Inst, San Antonio, TX 78238 USA. [Osip, David J.] Las Campanas Observ, Carnegie Observ, La Serena, Chile. [Gwyn, Stephen D. J.; Fabbro, Sebastian; Kavelaars, J. J.] Natl Res Council Canada, Canadian Astron Data Ctr, Victoria, BC V9E 2E7, Canada. [Benecchi, Susan D.; Sheppard, Scott S.] Carnegie Inst Sci, Dept Terr Magnetism, Washington, DC 20015 USA. [Binzel, Richard P.; DeMeo, Francesca E.] MIT, Cambridge, MA 02139 USA. [Fuentes, Cesar I.; Trilling, David E.] No Arizona Univ, Dept Phys & Astron, Flagstaff, AZ 86011 USA. [Gay, Pamela L.] So Illinois Univ, Ctr Sci Technol Engn & Math STEM Res Educ & Outre, Carbondale, IL 62901 USA. [Petit, Jean-Marc] Univ Franche Comte, CNRS, UTINAM, F-25030 Besancon, France. [Tholen, David J.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Ragozzine, Darin A.] Univ Florida, Dept Astron, Gainesville, FL 32611 USA. [Wasserman, Lawrence H.] Lowell Observ, Flagstaff, AZ 86001 USA. RP Parker, AH (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM aparker@cfa.harvard.edu RI Fuentes, Cesar /G-7506-2016 FU NASA Keck PI Data Award; W. M. Keck Foundation; Canadian Space Agency FX This paper includes data gathered with the 6.5 m Magellan Telescopes located at the Las Campanas Observatory, Chile, as well as data collected at Subaru telescope, which is operated by the National Astronomical Observatory of Japan, and 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 Institute National des Sciences de l'Univers of the Centre National de la Recherche Scientifique of France, and the University of Hawaii. This research used the facilities of the Canadian Astronomy Data Centre operated by the National Research Council of Canada with the support of the Canadian Space Agency. Magellan time was acquired through the CfA, MIT, Carnegie, and Arizona TACS, and CFHT time was acquired through the Canada, France, and Hawaii TACs.; This work was supported in part by a NASA Keck PI Data Award, administered by the NASA Exoplanet Science Institute. Some of the data presented herein, obtained at the Subaru telescope, was made possible through a time swap from the W. M. Keck Observatory allocated to the National Aeronautics and Space Administration through the agency's scientific partnership with the California Institute of Technology and the University of California. The Observatory was made possible by the generous financial support of the W. M. Keck Foundation. NR 27 TC 8 Z9 8 U1 0 U2 8 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 APR PY 2013 VL 145 IS 4 AR 96 DI 10.1088/0004-6256/145/4/96 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 107UW UT WOS:000316247300010 ER PT J AU Wolk, SJ Rice, TS Aspin, CA AF Wolk, Scott J. Rice, Thomas S. Aspin, Colin A. TI NEAR-INFRARED PERIODIC AND OTHER VARIABLE FIELD STARS IN THE FIELD OF THE CYGNUS OB7 STAR-FORMING REGION SO ASTRONOMICAL JOURNAL LA English DT Article DE binaries: eclipsing; infrared: stars; stars: variables: general ID T-TAURI STARS; YOUNG STELLAR OBJECTS; ORION NEBULA CLUSTER; ECLIPSING BINARIES; MAGNETOSPHERIC ACCRETION; PHOTOMETRIC VARIABILITY; ABSOLUTE DIMENSIONS; MOLECULAR CLOUD; SAMPLED-DATA; AA TAU AB We present a subset of the results of a three-season, 124 night, near-infrared monitoring campaign of the dark clouds Lynds 1003 and Lynds 1004 in the Cygnus OB7 star-forming region. In this paper, we focus on the field star population. Using three seasons of UKIRT J, H, and K-band observations spanning 1.5 years, we obtained high-quality photometry on 9200 stars down to J = 17 mag, with photometric uncertainty better than 0.04 mag. After excluding known disk-bearing stars we identify 149 variables-1.6% of the sample. Of these, about 60 are strictly periodic, with periods predominantly <2 days. We conclude this group is dominated by eclipsing binaries. A few stars have long period signals of between 20 and 60 days. About 25 stars have weak modulated signals, but it was not clear if these were periodic. Some of the stars in this group may be diskless young stellar objects with relatively large variability due to cool starspots. The remaining similar to 60 stars showed variations which appear to be purely stochastic. C1 [Wolk, Scott J.; Rice, Thomas S.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Aspin, Colin A.] Univ Hawaii Manoa, Inst Astron, Hilo, HI 96720 USA. RP Wolk, SJ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. OI Wolk, Scott/0000-0002-0826-9261 FU NASA [NAS8-03060]; Spitzer Science Center [1348190]; NSF REU site grant [0757887] FX S.J.W. is supported by NASA contract NAS8-03060 (Chandra). T. S. R. was supported by grant 1348190 from the Spitzer Science Center and also the NSF REU site grant 0757887. The United Kingdom Infrared Telescope is operated by the Joint Astronomy Centre on behalf of the Science and Technology Facilities Council of the UK. We thank A. Nord, L. Rizzi, and T. Carroll for assistance in obtaining these observations. We also thank the University of Hawaii Time Allocation Committee for allocating the nights during which these observations were made. The authors wish to recognize and acknowledge the very significant cultural role and reverence that the summit of Mauna Kea has always had within the indigenous Hawaiian community. We are most fortunate to have the opportunity to conduct observations from this sacred mountain. Special thanks to Nancy Evans, Margarita Karovska, and Matthew Templeton for helping us assess the light curves. NR 50 TC 6 Z9 6 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 J9 ASTRON J JI Astron. J. PD APR PY 2013 VL 145 IS 4 AR 113 DI 10.1088/0004-6256/145/4/113 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 107UW UT WOS:000316247300027 ER PT J AU Conroy, CJ Rowe, KC Rowe, KMC Kamath, PL Aplin, KP Hui, L James, DK Moritz, C Patton, JL AF Conroy, Chris J. Rowe, Kevin C. Rowe, Karen M. C. Kamath, Pauline L. Aplin, Ken P. Hui, Lucia James, David K. Moritz, Craig Patton, James L. TI Cryptic genetic diversity in Rattus of the San Francisco Bay region, California SO BIOLOGICAL INVASIONS LA English DT Article DE Rattus; Gene flow; Rodent; Tanezumi; Microsatellite; mtDNA ID POPULATION-STRUCTURE; MITOCHONDRIAL-DNA; ENDEMIC RODENTS; HOUSE MICE; BLACK RATS; COLONIZATION; MOUSE; HYBRIDIZATION; HANTAVIRUS; MADAGASCAR AB Invasive species can have complex invasion histories, harbor cryptic levels of diversity, and pose taxonomic problems for pest management authorities. Roof rats, Rattus rattus sensu lato, are common invasive pests of the San Francisco Bay Area in California, USA. They are a significant health risk and pest management efforts impose a large financial investment from public institutions and private individuals. Recent molecular genetic and taxonomic studies of black rats in their native range in Asia have shown that the species is a complex of two karyotypic forms and four mitochondrial genetic lineages that may represent four distinct species. We used mtDNA sequences and nuclear microsatellite variation to identify which mitochondrial lineages of the R. rattus group are present in the San Francisco Bay Area and to test for gene flow among them. We recovered specimens with mtDNA sequences representing two of the major mtDNA lineages of the R. rattus group. Microsatellite variation, however, was not structured in concordance with mtDNA lineages, suggesting a more complex history involving hybridization and introgression between these lineages. Although Aplin et al. (2011) and Lack et al. (2012) reported R. rattus Lineage II in North America, this is the first detailed examination of possible gene flow amongst lineages in this region. C1 [Conroy, Chris J.; Rowe, Kevin C.; Rowe, Karen M. C.; Moritz, Craig; Patton, James L.] Univ Calif Berkeley, Museum Vertebrate Zool, Berkeley, CA 94720 USA. [Rowe, Kevin C.; Rowe, Karen M. C.] Museum Victoria, Dept Sci, Melbourne, Vic, Australia. [Kamath, Pauline L.] Univ Calif Berkeley, Dept Environm Sci Policy & Management, Berkeley, CA 94720 USA. [Aplin, Ken P.] Smithsonian Inst, Natl Museum Nat Hist, Div Mammals, Washington, DC 20013 USA. [Hui, Lucia; James, David K.] Alameda Cty Vector Control Serv Dist, Alameda, CA 94502 USA. RP Conroy, CJ (reprint author), Univ Calif Berkeley, Museum Vertebrate Zool, Berkeley, CA 94720 USA. EM ondatra@berkeley.edu RI Kamath, Pauline/H-1358-2013; Moritz, Craig/A-7755-2012; OI Kamath, Pauline/0000-0002-6458-4514; Rowe, Karen/0000-0002-6131-6418 FU MVZ; Alameda County Vector Control District FX This work benefitted from support from Denise Bonilla of the California Department of Public Health, and fieldwork by Tia Reddick, an intern with the Alameda County Vector Control District. Michael Kosoy (CDC) tested tissues for Bartonella strains, and Robert Lane (UC Berkeley) tested tissues for Borrelia. Cherilyn Acorda conducted some of the early laboratory work. This work was improved by discussions with Steve Donnellan, Ron Van Den Bussche, Hitoshi Suzuki, Jean-Francois Cosson and others at the first R. rattus consortium meeting in Bangkok in 2010. Thanks to curators and collection managers Joseph Cook and Jon Dunnum (Museum of Southwestern Biology), Larry Heaney, Bruce Patterson and Bill Stanley (Field Museum of Natural History) for access to worldwide samples of Rattus tissues. This work would not have been possible without those loans. Many thanks to Anita Pearson who personally donated many of the rats included here, especially where Lineages I and II are sympatric. Funding for laboratory analyses was kindly provided by the MVZ, and the Alameda County Vector Control District directly funded PK. NR 88 TC 10 Z9 10 U1 5 U2 45 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 1387-3547 J9 BIOL INVASIONS JI Biol. Invasions PD APR PY 2013 VL 15 IS 4 BP 741 EP 758 DI 10.1007/s10530-012-0323-9 PG 18 WC Biodiversity Conservation; Ecology SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 107FQ UT WOS:000316200700004 ER PT J AU Turner, BL Blackwell, MSA AF Turner, B. L. Blackwell, M. S. A. TI Isolating the influence of pH on the amounts and forms of soil organic phosphorus SO EUROPEAN JOURNAL OF SOIL SCIENCE LA English DT Article ID P-31 NMR-SPECTROSCOPY; MAGNETIC-RESONANCE-SPECTROSCOPY; NAOH-EDTA EXTRACTION; INOSITOL HEXAKISPHOSPHATE; POTENTIAL BIOAVAILABILITY; PASTURE SOILS; WETLAND SOILS; ARABLE SOIL; IDENTIFICATION; PHOSPHATES AB Soil pH influences the chemistry, dynamics and biological availability of phosphorus (P), but few studies have isolated the effect of pH from other soil properties. We studied phosphorus chemistry in soils along the Hoosfield acid strip (Rothamsted, UK), where a pH gradient from 3.7 to 7.8 occurs in a single soil with little variation in total phosphorus (mean +/- standard deviation 399 +/- 27mgPkg1). Soil organic phosphorus represented a consistent proportion of the total soil phosphorus (36 +/- 2%) irrespective of soil pH. However, organic phosphorus concentrations increased by about 20% in the most acidic soils (pH<4.0), through an accumulation of inositol hexakisphosphate, DNA and phosphonates. The increase in organic phosphorus in the most acidic soils was not related to organic carbon, because organic carbon concentrations declined at pH <4.0. Thus, the organic carbon to organic phosphorus ratio declined from about 70 in neutral soils to about 50 in strongly acidic soils. In contrast to organic phosphorus, inorganic phosphorus was affected strongly by soil pH, because readily-exchangeable phosphate extracted with anion-exchange membranes and a more stable inorganic phosphorus pool extracted in NaOHEDTA both increased markedly as soil pH declined. Inorganic orthophosphate concentrations were correlated negatively with amorphous manganese and positively with amorphous aluminium oxides, suggesting that soil pH influences orthophosphate stabilization via metal oxides. We conclude that pH has a relatively minor influence on the amount of organic phosphorus in soil, although some forms of organic phosphorus accumulate preferentially under strongly acidic conditions. C1 [Turner, B. L.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. [Blackwell, M. S. A.] Rothamsted Res, Okehampton EX20 2SB, Devon, England. RP Turner, BL (reprint author), Smithsonian Trop Res Inst, Apartado 0843-03092, Balboa, Ancon, Panama. EM TurnerBL@si.edu RI Turner, Benjamin/E-5940-2011 OI Turner, Benjamin/0000-0002-6585-0722 FU Biotechnology and Biological Sciences Research Council FX We thank Dayana Agudo, Alex Blumenfeld, Denise Headon, Luis Ramos and Tania Romero for analytical support, Dan Dhanoa for statistical advice, and Alison Carswell, Emma Worsfold, Philip Brookes and Andy MacDonald for assistance with sample collection, preparation and permissions. The research was made possible by the Rothamsted Long-Term Experiments, a UK National Capability funded by the Biotechnology and Biological Sciences Research Council. NR 42 TC 21 Z9 22 U1 2 U2 116 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1351-0754 J9 EUR J SOIL SCI JI Eur. J. Soil Sci. PD APR PY 2013 VL 64 IS 2 BP 249 EP 259 DI 10.1111/ejss.12026 PG 11 WC Soil Science SC Agriculture GA 112AU UT WOS:000316564700008 ER PT J AU Wang, R Paul, VJ Luesch, H AF Wang, Rui Paul, Valerie J. Luesch, Hendrik TI Seaweed extracts and unsaturated fatty acid constituents from the green alga Ulva lactuca as activators of the cytoprotective Nrf2-ARE pathway SO FREE RADICAL BIOLOGY AND MEDICINE LA English DT Article DE Oxidative stress; Reactive oxygen species; Nrf2; Keap1; Antioxidant-response element; Antioxidants; Edible seaweeds; Cytoprotective enzymes; NQO1; Ulva lactuca; Monounsaturated fatty acids; Fatty acid amides; Glutathione; Free radicals ID ANTIOXIDANT RESPONSE ELEMENT; HUMAN NEUROBLASTOMA-CELLS; MARINE NATURAL-PRODUCTS; OXIDATIVE STRESS; TRANSCRIPTIONAL REGULATION; SIGNALING PATHWAY; CANCER CHEMOPREVENTION; TERT-BUTYLHYDROQUINONE; NRF2-REGULATED GENES; SAITAMA PREFECTURE AB Increased amounts of reactive oxygen species (ROS) have been implicated in many pathological conditions, including cancer. The major machinery that the cell employs to neutralize excess ROS is through the activation of the antioxidant-response element (ARE) that controls the activation of many phase II detoxification enzymes. The transcription factor that recognizes the ARE, Nrf2, can be activated by a variety of small molecules, most of which contain an alpha,beta-unsaturated carbonyl system. In the pursuit of chemopreventive agents from marine organisms, we built, fractionated, and screened a library of 30 field-collected eukaryotic algae from Florida. An edible green alga, Ulva lactuca, yielded multiple active fractions by ARE-luciferase reporter assay. We isolated three monounsaturated fatty acid (MUFA) derivatives as active components, including a new keto-type C18 fatty acid (1), the corresponding shorter chain C16 acid (2), and an amide derivative (3) of the C18 acid. Their chemical structures were elucidated by NMR and mass spectrometry. All three contain the conjugated enone motif between C7 and C9, which is thought to be responsible for the ARE activity. Subsequent biological studies focused on 1, the most active and abundant ARE activator isolated. 08 acid 1 induced the expression of ARE-regulated cytoprotective genes, including NAD(P)H:quinone oxidoreductase 1, heme oxygenase 1, thioredoxin reductase 1, both subunits of the glutamate-cysteine ligase (catalytic subunit and modifier subunit), and the cystine/glutamate exchange transporter, in IMR-32 human neuroblastoma cells. Its cellular activity requires the presence of Nrf2 and PI3K function, based on RNA interference and pharmacological inhibitor studies, respectively. Treatment with I led only to Nrf2 activation, and not the increase in production of NRF2 mRNA. To test its ARE activity and cytoprotective potential in vivo, we treated mice with a single dose of a U. lactuca fraction that was enriched with 1, which showed ARE-activating effects similar to those observed in vitro. This could be owing to this fraction's ability to stabilize Nrf2 through inhibition of Keap1-mediated Nrf2 ubiquitination and the subsequent accumulation and nuclear translocation of Nrf2. The induction of many ARE-driven antioxidant genes in vivo and most prominently in the heart agreed with the commonly recognized cardioprotective properties of MUFAs. A significant increase in Nqo1 transcript levels was also found in other mouse tissues such as the brain, lung, and stomach. Collectively, this study provides new insight into why consumption of dietary seaweed may have health benefits, and the identified compounds add to the list of chemopreventive dietary unsaturated fatty acids. (C) 2013 Elsevier Inc. All rights reserved. C1 [Wang, Rui; Luesch, Hendrik] Univ Florida, Dept Med Chem, Gainesville, FL 32610 USA. [Paul, Valerie J.] Smithsonian Marine Stn, Ft Pierce, FL 34949 USA. RP Luesch, H (reprint author), Univ Florida, Dept Med Chem, Gainesville, FL 32610 USA. EM luesch@cop.uft.edu FU National Institutes of Health [R21CA133681, R01EY020825] FX This research was supported by the National Institutes of Health, Grants R21CA133681 and R01EY020825. We are grateful to the Florida Institute of Oceanography for providing the R/V Bellows and to the National Park Service for granting the collection permits for the Dry Tortugas National Park. We thank the crew of the R/V Bellows, K. Arthur, F. Gurgel, T. Meickle, S. Reed, R. Ritson-Williams, S. Matthew, and K. Taori, for assistance with algae collections and S. Gunasekera for extracting and fractionating the recollected U. lactuca samples. We also thank Professor J. Johnson for ARE-luc reporter constructs and ARE reporter mice; Professor S. Chanda for AP-1-(PMA)-luc plasmids; Professors N. Gray and D. Zhang for Keap1-CBD, Gal4-Neh2, and HA-Ub plasmids; Professor R. Tsien for sharing pcDNA3-mRFP through Addgene; Professor D. Borchelt and S. Fromholt for mouse genotyping; and Y. Liu for mouse oral gavaging and tissue dissection. NR 64 TC 25 Z9 28 U1 1 U2 81 PU ELSEVIER SCIENCE INC PI NEW YORK PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA SN 0891-5849 J9 FREE RADICAL BIO MED JI Free Radic. Biol. Med. PD APR PY 2013 VL 57 BP 141 EP 153 DI 10.1016/j.freeradbiomed.2012.12.019 PG 13 WC Biochemistry & Molecular Biology; Endocrinology & Metabolism SC Biochemistry & Molecular Biology; Endocrinology & Metabolism GA 105AC UT WOS:000316037000014 PM 23291594 ER PT J AU Cavers, S Dick, CW AF Cavers, Stephen Dick, Christopher W. TI Phylogeography of Neotropical trees SO JOURNAL OF BIOGEOGRAPHY LA English DT Editorial Material ID BIODIVERSITY; AMAZONIA; HISTORY; FORESTS C1 [Cavers, Stephen] CEH Edinburgh, Ctr Ecol & Hydrol, Penicuik EH26 0QB, Midlothian, Scotland. [Dick, Christopher W.] Univ Michigan, Herbarium, Dept Ecol & Evolutionary Biol, Ann Arbor, MI 48109 USA. [Dick, Christopher W.] Smithsonian Trop Res Inst, Gamboa, Panama. RP Cavers, S (reprint author), CEH Edinburgh, Ctr Ecol & Hydrol, Penicuik EH26 0QB, Midlothian, Scotland. EM scav@ceh.ac.uk RI Dick, Christopher/A-8744-2008; Cavers, Stephen/B-7806-2010 OI Cavers, Stephen/0000-0003-2139-9236 NR 25 TC 8 Z9 8 U1 3 U2 57 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0305-0270 J9 J BIOGEOGR JI J. Biogeogr. PD APR PY 2013 VL 40 IS 4 BP 615 EP 617 DI 10.1111/jbi.12097 PG 3 WC Ecology; Geography, Physical SC Environmental Sciences & Ecology; Physical Geography GA 108VY UT WOS:000316325500001 ER PT J AU Scotti-Saintagne, C Dick, CW Caron, H Vendramin, GG Guichoux, E Buonamici, A Duret, C Sire, P Valencia, R Lemes, MR Gribel, R Scotti, I AF Scotti-Saintagne, Caroline Dick, Christopher W. Caron, Henri Vendramin, Giovanni G. Guichoux, Erwan Buonamici, Anna Duret, Caroline Sire, Pierre Valencia, Renato Lemes, Maristerra R. Gribel, Rogerio Scotti, Ivan TI Phylogeography of a species complex of lowland Neotropical rain forest trees (Carapa, Meliaceae) SO JOURNAL OF BIOGEOGRAPHY LA English DT Article DE Amazonia; Carapa; historical biogeography; Mahogany family; molecular markers; Neogene diversification; phylogeography; Quaternary diversification; species complexes ID POPULATION-STRUCTURE; GENETIC-STRUCTURE; MICROSATELLITE MARKERS; GUIANENSIS MELIACEAE; COMPUTER-PROGRAM; DNA-SEQUENCES; TROPICAL TREE; CHLOROPLAST; DIVERSITY; DISPERSAL AB Aim Many tropical tree species have poorly delimited taxonomic boundaries and contain undescribed or cryptic species. We examined the genetic structure of a species complex in the tree genus Carapa in the Neotropics in order to evaluate age, geographic patterns of diversity and evolutionary relationships, and to quantify levels of introgression among currently recognized species. Location Lowland moist forests in the Guiana Shield, the Central and Western Amazon Basin, Choco and Central America. Methods Genetic structure was analysed using seven nuclear simple sequence repeats (nuSSR), five chloroplast SSRs (cpSSR), and two chloroplast DNA (cpDNA) intergenic sequences (trnHpsbA and trnCycf6). Bayesian clustering analysis of the SSR data was used to infer population genetic structure and to assign 324 samples to their most likely genetic cluster. Bayesian coalescence analyses were performed on the two cpDNA markers to estimate evolutionary relationships and divergence times. Results Two genetic clusters (nu_guianensis and nu_surinamensis) were detected, which correspond to the Neotropical species C. guianensis (sensu latu) and C. surinamensis. Fourteen cpDNA haplotypes clustered into six haplogroups distributed between the two nuclear genetic clusters. Divergence between the haplogroups was initiated in the Miocene, with some haplotype structure evolving as recently as the Pleistocene. The absence of complete lineage sorting between the nuclear and chloroplast genomes and the presence of hybrid individuals suggest that interspecific reproductive barriers are incomplete. NuSSR diversity was highest in C. guianensis and, within C. guianensis, cpDNA diversity was highest in the Central and Western Amazon Basin. Regional genetic differentiation was strong but did not conform to an isolation-by-distance process or exhibit a phylogeographical signal. Main conclusions The biogeographical history of Neotropical Carapa appears to have been influenced by events that took place during the Neogene. Our results point to an Amazonian centre of origin and diversification of Neotropical Carapa, with subsequent migration to the Pacific coast of South America and Central America. Gene flow apparently occurs among species, and introgression events are supported by inconsistencies between chloroplast and nuclear lineage sorting. The absence of phylogeographical structure may be a result of the ineffectiveness of geographical barriers among populations and of reproductive isolation mechanisms among incipient and cryptic species in this species complex. C1 [Scotti-Saintagne, Caroline; Duret, Caroline; Sire, Pierre; Scotti, Ivan] INRA UMR 0745 EcoFoG Ecol Forets Guyane, Kourou 97387, French Guiana. [Dick, Christopher W.] Univ Michigan, Dept Ecol & Evolutionary Biol, Ann Arbor, MI 48109 USA. [Dick, Christopher W.] Smithsonian Trop Res Inst, Gamboa, Panama. [Caron, Henri; Guichoux, Erwan] Univ Bordeaux, INRA, BIOGECO UMR1202, F-33610 Cestas, France. [Vendramin, Giovanni G.; Buonamici, Anna] CNR, Sez Firenze, Ist Genet Vegetale, I-50019 Florence, Italy. [Valencia, Renato] P Univ Catolica Ecuador, Escuela Ciencias Biol, Lab Ecol Plantas, Quito, Ecuador. [Valencia, Renato] P Univ Catolica Ecuador, Escuela Ciencias Biol, Herbario QCA, Quito, Ecuador. [Lemes, Maristerra R.; Gribel, Rogerio] Inst Nacl de Pesquisas da Amazonia, Lab Genet & Biol Reprod Plantas, BR-69083000 Manaus, Amazonas, Brazil. RP Scotti-Saintagne, C (reprint author), INRA UMR 0745 EcoFoG Ecol Forets Guyane, Campus Agron,BP709, Kourou 97387, French Guiana. EM caroline.scotti@ecofog.gf RI Dick, Christopher/A-8744-2008; Adapta, Inct/J-8371-2013; Gribel, Rogerio/C-5392-2013; Scotti-Saintagne, Caroline/C-3119-2009; Vendramin, Giovanni G/K-9731-2014 OI Gribel, Rogerio/0000-0002-0850-5578; Vendramin, Giovanni G/0000-0001-9921-7872 FU EU INCO 'SEEDSOURCE' project; EU PO-FEDER 'ENERGI-RAVI' program; Centre National de la Recherche Scientifique (CNRS) Programme Amazonie 'CLIPS' FX This work was financially supported by the EU INCO 'SEEDSOURCE' project, by the EU PO-FEDER 'ENERGI-RAVI' program and by the Centre National de la Recherche Scientifique (CNRS) Programme Amazonie 'CLIPS'. The authors wish to thank Saint-Omer Cazal (UMR ECOFOG, INRA, Kourou, French-Guiana), Jean-Francois Molino [Institut de Recherche pour le Developpement (IRD), UMR 'botanique et bioinformatique de l'architecture des plantes' (AMAP), Montpellier France], Daniel Sabatier (IRD, AMAP, Montpellier France), Pierre-Michel Forget (Museum National d'Histoire Naturelle, Paris), Heidy Villalobos (University of Costa Rica), Carlos Navarro (CATIE, Costa Rica), Elio Sanoja (Upata, Venezuela) and Jerome Chave (CNRS, UMR EDB, Toulouse) for sampling, Valerie Troispoux (UMR ECOFOG, INRA, Kourou, French Guiana) for molecular biology support, and David Kenfack for discussion of unpublished findings on Carapa systematics. We thank two anonymous referees for their helpful suggestions and comments, which improved the manuscript. NR 71 TC 16 Z9 16 U1 1 U2 115 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 APR PY 2013 VL 40 IS 4 BP 676 EP 692 DI 10.1111/j.1365-2699.2011.02678.x PG 17 WC Ecology; Geography, Physical SC Environmental Sciences & Ecology; Physical Geography GA 108VY UT WOS:000316325500006 ER PT J AU Rymer, PD Dick, CW Vendramin, GG Buonamici, A Boshier, D AF Rymer, Paul D. Dick, Christopher W. Vendramin, Giovanni G. Buonamici, Anna Boshier, David TI Recent phylogeographic structure in a widespread 'weedy' Neotropical tree species, Cordia alliodora (Boraginaceae) SO JOURNAL OF BIOGEOGRAPHY LA English DT Article DE Amazon Basin; Andes Mountains; Neotropics; phylogeography; samova; structure; tropical trees; vicariance ID RAIN-FOREST TREE; TROPICAL FORESTS; SOUTH-AMERICA; POPULATION-GENETICS; ATMOSPHERIC CHANGE; CEDRELA-ODORATA; DIVERSITY; DISTANCE; DIVERSIFICATION; BIODIVERSITY AB Aim Although hundreds of tree species have broad geographic ranges in the Neotropics, little is known about how such widespread species attained disjunct distributions around mountain, ocean and xeric barriers. Here, we examine the phylogeographic structure of a widespread and economically important tree, Cordia alliodora, to: (1) test the roles of vicariance and dispersal in establishing major range disjunctions, (2) determine which geographic regions and/or habitats contain the highest levels of genetic diversity, and (3) infer the geographic origin of the species. Location Twenty-five countries in Central and South America, and the West Indies. Methods Chloroplast simple sequence repeats (cpSSR; eight loci) were assayed in 67 populations (240 individuals) sampled from the full geographic range of C. alliodora. Chloroplast (trnHpsbA) and nuclear (internal transcribed spacer, ITS) DNA sequences were sampled from a geographically representative subset. Genetic structure was determined with samova, structure and haplotype networks. Analysis of molecular variance (AMOVA) and rarefaction analyses were used to compare regional haplotype diversity and differentiation. Results Although the ITS region was polymorphic it revealed limited phylogeographic structure, and trnHpsbA was monomorphic. However, structure analysis of cpSSR variation recovered three broad demes spanning Central America (Deme 1), the Greater Antilles and the Choco (Deme 2), and the Lesser Antilles and cis-Andean South America (Deme 3). samova showed two predominant demes (Deme 1+2 and Deme 3). The greatest haplotype diversity was detected east of the Andes, while significantly more genetic variation was partitioned among trans-Andean populations. Populations experiencing high precipitation seasonality (dry ecotype) had greater levels of genetic variation. Main conclusions Cordia alliodora displayed weak cis- and trans-Andean phylogeographic structure based on DNA sequence data, indicative of historical dispersal around this barrier and genetic exchange across its broad range. The cpSSR data revealed phylogeographic structure corresponding to three biogeographic zones. Patterns of genetic diversity are indicative of an origin in the seasonally dry habitats of South America. Therefore, C. alliodora fits the disperser hypothesis for widespread Neotropical species. Dispersal is evident in the West Indies and the northern Andean cordilleras. The dry ecotype harbours genetic variation that is likely to represent the source for the establishment of populations under future warmer and drier climatic scenarios. C1 [Rymer, Paul D.; Boshier, David] Univ Oxford, Dept Plant Sci, Oxford OX1 3RB, England. [Rymer, Paul D.] Univ Western Sydney, Hawkesbury Inst Environm, Richmond, NSW 2753, Australia. [Dick, Christopher W.] Univ Michigan, Dept Ecol & Evolutionary Biol, Ann Arbor, MI 48109 USA. [Dick, Christopher W.] Univ Michigan, Herbarium, Ann Arbor, MI 48109 USA. [Dick, Christopher W.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. [Vendramin, Giovanni G.; Buonamici, Anna] CNR, Ist Genet Vegetale, I-50019 Florence, Italy. RP Rymer, PD (reprint author), Univ Western Sydney, Hawkesbury Inst Environm, Locked Bag 1797, Penrith, NSW 2751, Australia. EM p.rymer@uws.edu.au RI Dick, Christopher/A-8744-2008; Vendramin, Giovanni G/K-9731-2014 OI Vendramin, Giovanni G/0000-0001-9921-7872 FU EC [FP6-2002-INCO-DEV-1]; Seedsource consortium; National Science Foundation [DEB 0640379] FX This work was funded by the EC (FP6-2002-INCO-DEV-1). We are grateful to the entire Seedsource consortium for providing support for this project. Special thanks to Stephen Cavers and two anonymous referees for intellectual contributions. This work would not have been possible without field collections from Renato Valencia and Justin Stead, and without access to herbarium material (FHO, K, U, MO, CAY) for DNA samples. Sarah Rendell and Christina Vinson provided laboratory assistance. C.D. acknowledges laboratory assistance from Saji Abraham, and National Science Foundation funding (DEB 0640379). NR 63 TC 7 Z9 8 U1 2 U2 61 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0305-0270 J9 J BIOGEOGR JI J. Biogeogr. PD APR PY 2013 VL 40 IS 4 BP 693 EP 706 DI 10.1111/j.1365-2699.2012.02727.x PG 14 WC Ecology; Geography, Physical SC Environmental Sciences & Ecology; Physical Geography GA 108VY UT WOS:000316325500007 ER PT J AU Scotti-Saintagne, C Dick, CW Caron, H Vendramin, GG Troispoux, V Sire, P Casalis, M Buonamici, A Valencia, R Lemes, MR Gribel, R Scotti, I AF Scotti-Saintagne, Caroline Dick, Christopher W. Caron, Henri Vendramin, Giovanni G. Troispoux, Valerie Sire, Pierre Casalis, Maxime Buonamici, Anna Valencia, Renato Lemes, Maristerra R. Gribel, Rogerio Scotti, Ivan TI Amazon diversification and cross-Andean dispersal of the widespread Neotropical tree species Jacaranda copaia (Bignoniaceae) SO JOURNAL OF BIOGEOGRAPHY LA English DT Article DE Amazonia; Bignoniaceae; centre of diversity; dispersal; historical biogeography; Neotropics; phylogeography; Pleistocene; tropical forest; vicariance ID RAIN-FOREST TREE; GENETIC-STRUCTURE; POPULATION-GENETICS; DIVERSITY; SPECIATION; SOFTWARE; HISTORY; DIFFERENTIATION; BIODIVERSITY; PATTERNS AB Aim The phylogeographical history of Neotropical species can be difficult to reconstruct because of superimposed Neogene and Quaternary histories, and because of taxonomic uncertainty. We analysed range-wide genetic diversity in a widespread pioneer tree species, Jacaranda copaia (Aubl.) D. Don, to characterize phylogeographical structure, date the evolutionary relationships among lineages, and evaluate the role of dispersal and vicariance in establishing the present geographical range. Location Guiana Shield; central, southern and western Amazon Basin; Choco region; Central America. Methods We analysed nine nuclear simple sequence repeat loci (nuSSR), eight chloroplast SSRs (cpSSR), and two cpDNA intergenic sequences in 341 adult trees. Genetic differentiation at nuSSRs was inferred using Bayesian clustering. Dating of chloroplast lineage divergence was obtained using a range of published mutation rates and Bayesian coalescence analyses. Population divergence dating was performed using an isolation-with-migration model for eight loci (one cp sequence and seven nuSSRs). Results Nuclear SSR variation identified three geographically overlapping clusters (nu-1, nu-2, nu-3). Twelve cpDNA haplotypes were clustered into two haplogroups (cp-1, cp-2) with the central Amazon harbouring the highest diversity. Molecular dating analysis suggests that cpDNA haplotype diversification started around the end of the Pliocene (2.61Ma on average), whereas population divergence was more recent and occurred during the mid-Quaternary (point estimates between 357 and 436ka). Main conclusions The genetic variation of J. copaia in the Neotropics was shaped mainly by Pleistocene events. Chloroplast diversity did not display the expected cis/trans Andean disjunction, indicating recent dispersal. Nuclear variation revealed that separate regions share a recent history, with a centre of diversity in the central Amazon Basin. The geographical pattern of diversity is congruent with the distribution of the two subspecies, J. copaia copaia and J. copaia spectabilis, and evidence of nuSSR admixture between the two taxa supports their classification as subspecies. C1 [Scotti-Saintagne, Caroline; Troispoux, Valerie; Sire, Pierre; Casalis, Maxime; Scotti, Ivan] INRA UMR ECOFOG, F-97387 Kourou, France. [Caron, Henri] INRA UMR BIOGECO 69, F-33312 Cestas, France. [Vendramin, Giovanni G.; Buonamici, Anna] CNR, Ist Genet Vegetale, Sez Firenze, I-50019 Florence, Italy. [Valencia, Renato] P Univ Catolica Ecuador, Lab Ecol Plantas, Escuela Ciencias Biol, Quito, Ecuador. [Lemes, Maristerra R.; Gribel, Rogerio] Inst Nacl de Pesquisas da Amazonia, Lab Genet & Biol Reprod Plantas, BR-69083000 Manaus, Amazonas, Brazil. [Dick, Christopher W.] Univ Michigan, Dept Ecol & Evolutionary Biol, Ann Arbor, MI 48109 USA. [Dick, Christopher W.] Univ Michigan, Herbarium, Ann Arbor, MI 48109 USA. [Dick, Christopher W.] Smithsonian Trop Res Inst, Gamboa, Panama. [Lemes, Maristerra R.; Gribel, Rogerio] Inst Pesquisas Jardim Bot Rio de Janeiro, Jardim Bot, BR-22460030 Rio De Janeiro, RJ, Brazil. RP Scotti-Saintagne, C (reprint author), INRA UMR 0745 EcoFoG Ecol Forets Guyane, Campus Agron,BP709, Kourou 97387, French Guiana. EM caroline.scotti@ecofog.gf RI Dick, Christopher/A-8744-2008; Adapta, Inct/J-8371-2013; Gribel, Rogerio/C-5392-2013; Scotti-Saintagne, Caroline/C-3119-2009; Vendramin, Giovanni G/K-9731-2014 OI Gribel, Rogerio/0000-0002-0850-5578; Vendramin, Giovanni G/0000-0001-9921-7872 FU EU; Agence Nationale de la recherche (ANR) FX This work was funded by the EU-funded INCO 'SEED-SOURCE' project, by the EU-funded PO-FEDER 'ENERGI-RAVI' program and the Agence Nationale de la recherche (ANR) funded programme 'BRIDGE'. The authors thank Saint-Omer Cazal (UMR ECOFOG, INRA, Kourou, French-Guiana), Jean-Francois Molino (IRD, AMAP, Montpellier, France), Daniel Sabatier (IRD, AMAP, Montpellier, France), Heidy Villalobos (University of Costa Rica) and Carlos Navarro (CATIE, Costa Rica) for sampling; Sam Davies, Cayenne herbarium (IRD, French Guiana), Manaus herbarium (EMB-RAPA and INPA, Brazil), Oxford herbarium (University Herbaria, UK) and Utrecht herbarium (National Herbarium, the Netherlands) for access to collections; and Eliane Louisanna (UMR ECOFOG, INRA, Kourou, French Guiana) for technical assistance with molecular biology. NR 67 TC 8 Z9 8 U1 1 U2 66 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0305-0270 J9 J BIOGEOGR JI J. Biogeogr. PD APR PY 2013 VL 40 IS 4 BP 707 EP 719 DI 10.1111/j.1365-2699.2012.02797.x PG 13 WC Ecology; Geography, Physical SC Environmental Sciences & Ecology; Physical Geography GA 108VY UT WOS:000316325500008 ER PT J AU Jones, FA Ceron-Souza, I Hardesty, BD Dick, CW AF Jones, F. Andrew Ceron-Souza, Ivania Hardesty, Britta Denise Dick, Christopher W. TI Genetic evidence of Quaternary demographic changes in four rain forest tree species sampled across the Isthmus of Panama SO JOURNAL OF BIOGEOGRAPHY LA English DT Article DE Climate change; coalescent theory; gene flow; genetic diversity; Last Glacial Maximum; life-history traits; microsatellites; Pleistocene refuge theory; population bottleneck; tropical forest history ID LIFE-HISTORY TRAITS; NEOTROPICAL TREE; SEED DISPERSAL; EVOLUTIONARY CONSEQUENCES; POPULATION EXPANSION; POLLINATION BIOLOGY; TROPICAL FOREST; CLIMATE-CHANGE; POLLEN RECORD; GLACIAL TIMES AB Aim We examined and compared population genetic structure in a suite of four co-occurring Panamanian tree species and performed coalescent-based analyses of demographic history to evaluate hypotheses of tropical vegetation change during the Last Glacial Maximum (LGM). Location Isthmus of Panama. Methods Nuclear microsatellite variation was assayed in multiple populations (1179 trees, 21 locations, 613 locations per species) in Jacaranda copaia (Bignoniaceae), Luehea seemannii (Malvaceae), Simarouba amara (Simaroubaceae) and Symphonia globulifera (Clusiaceae). Population structure was analysed using FST-based statistics and a Bayesian clustering approach (baps). Bayesian coalescent methods (msvar) were used to infer demographic histories. Results High levels of genetic diversity were found in all of the species (HE range, 0.560.79). Jacaranda copaia and L. seemannii showed lower FST and fewer Bayesian clusters across similar spatial scales than did S. globulifera and Simarouba amara. For each species examined, the current effective population sizes (Ne) are much lower than ancient Ne, within all inferred baps demes. In light-demanding pioneer species J. copaia, L. seemannii and S. amara, estimates of the number of generations since the bottleneck events overlap with the end of the LGM (median site posterior estimates ranged from 16 to 19ka) while Symphonia globulifera estimates are consistent with earlier population declines (median 202ka) in the early Pleistocene and late Pliocene. Main conclusions The wind-dispersed deciduous species J. copaia and L. seemannii showed lower FST and spatially extensive demes, while the animal-dispersed evergreen Symphonia globulifera and Simarouba amara showed spatially restrictive demes and higher FST. Each deme examined shows evidence of historical bottlenecks. For three of the four species which are also light-demanding pioneer species, the mean estimated time and 95% highest posterior density of the bottleneck events coincides with the end of the LGM. These results suggest that these species have undergone historical bottlenecks as a result of reduced forest cover during the Pleistocene and provide evidence of shared demographic histories among co-occurring tropical forest trees. C1 [Jones, F. Andrew] Oregon State Univ, Dept Bot & Plant Pathol, Corvallis, OR 97331 USA. [Jones, F. Andrew; Ceron-Souza, Ivania; Dick, Christopher W.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. [Hardesty, Britta Denise] CSIRO Ecosyst Sci, Atherton, Qld 4883, Australia. [Dick, Christopher W.] Univ Michigan, Dept Ecol & Evolutionary Biol, Ann Arbor, MI 48109 USA. [Dick, Christopher W.] Univ Michigan, Herbarium, Ann Arbor, MI 48109 USA. RP Jones, FA (reprint author), Oregon State Univ, Dept Bot & Plant Pathol, 2082 Cordley Hall, Corvallis, OR 97331 USA. EM jonesfr@science.oregonstate.edu RI Dick, Christopher/A-8744-2008; Hardesty, Britta Denise/A-3189-2011 OI Hardesty, Britta Denise/0000-0003-1948-5098 FU National Science Foundation [DEB 0129874, DEB 0608512, DEB 0640379]; Smithsonian Tropical Research Institute FX The authors thank M. Serrano for developing the vegetation maps of Panama. S. Aguilar and H. Mogollon carried out some of the collecting in Panama. We would like to thank the Panamanian Autoridad Nacional del Ambiente (ANAM) and the Smithsonian Tropical Research Institute (STRI) for processing research permits. National Science Foundation awards DEB 0129874, DEB 0608512 and DEB 0640379 supported this research. F.A.J. and C.W.D. acknowledge prior support from Tupper Postdoctoral Fellowships from the Smithsonian Tropical Research Institute. E. Bermingham (STRI) provided valuable initial support for this project. M. Silman, R. J. Whittaker and three anonymous referees provided feedback that greatly improved the manuscript in an earlier form. NR 73 TC 11 Z9 11 U1 1 U2 57 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0305-0270 J9 J BIOGEOGR JI J. Biogeogr. PD APR PY 2013 VL 40 IS 4 BP 720 EP 731 DI 10.1111/jbi.12037 PG 12 WC Ecology; Geography, Physical SC Environmental Sciences & Ecology; Physical Geography GA 108VY UT WOS:000316325500009 ER PT J AU Jones, PL Farris, HE Ryan, MJ Page, RA AF Jones, Patricia L. Farris, Hamilton E. Ryan, Michael J. Page, Rachel A. TI Do frog-eating bats perceptually bind the complex components of frog calls? SO JOURNAL OF COMPARATIVE PHYSIOLOGY A-NEUROETHOLOGY SENSORY NEURAL AND BEHAVIORAL PHYSIOLOGY LA English DT Article DE Phonotaxis; Physalaemus pustulosus; Sexual advertisement signal; Tungara; Trachops cirrhosus ID PARASITOID FLY; TUNGARA FROGS; NEOTROPICAL FROG; MATING SIGNALS; FIELD CRICKETS; EVOLUTION; BEHAVIOR; HEARING; PREFERENCES; TACHINIDAE AB The mating calls of male tA(0)ngara frogs, Physalaemus pustulosus, attract intended (conspecific females) and unintended (eavesdropping predators and parasites) receivers. The calls are complex, having two components: a frequency-modulated "whine" followed by 0-7 harmonic bursts or "chucks". The whine is necessary and sufficient to elicit phonotaxis from females and the chuck enhances call attractiveness when it follows a whine. Although chucks are never made alone, females perceptually bind the whine and chuck when they are spatially separated. We tested whether an unintended receiver with independent evolution of phonotaxis, the frog-eating bat, Trachops cirrhosus, has converged with frogs in its auditory grouping of the call components. In contrast to frogs, bats approached chucks broadcast alone; when the chuck was spatially separated from the whine the bats preferentially approached the whine, and bats were sensitive to whine-chuck temporal sequence. This contrast suggests that although disparate taxa may be selected to respond to the same signals, different evolutionary histories, selective regimes, and neural and cognitive architectures may result in different weighting and grouping of signal components between generalist predators and conspecific mates. C1 [Jones, Patricia L.; Ryan, Michael J.] Univ Texas Austin, Sect Integrat Biol, Austin, TX 78712 USA. [Jones, Patricia L.; Ryan, Michael J.; Page, Rachel A.] Smithsonian Trop Res Inst, Balboa, Panama. [Farris, Hamilton E.] Louisiana State Univ, Hlth Sci Ctr, Ctr Neurosci, New Orleans, LA 70112 USA. [Farris, Hamilton E.] Louisiana State Univ, Hlth Sci Ctr, Dept Otorhinolaryngol, New Orleans, LA 70112 USA. RP Jones, PL (reprint author), Univ Texas Austin, Sect Integrat Biol, Austin, TX 78712 USA. EM patricia.jones@utexas.edu FU National Science Foundation; Smithsonian Tropical Research Institute; National Institute of Health [P20RR016816] FX We thank the staff of the Smithsonian Tropical Research Institute for assistance with permits and logistics. This research was approved by the Panamanian Authorities (Autoridad Nacional del Ambiente, ANAM permit # SE/A-91-09; SE/A-95-10; SE/A-6-11; SE/A-46-11; SE/A-94-11) and the Smithsonian Institutional Animal Care and Use Committee (IACUC protocol 20100816-1012-16). Thanks to Victoria Flores, Teia Schwiezer, Jay Falk, Kristina Ottens, May Dixon and Jessica Jacobitz for help capturing and caring for bats. Thanks to Teague O'Mara for statistical advice. PLJ was funded by a National Science Foundation Graduate Research Fellowship and fellowship support from the Smithsonian Tropical Research Institute. HEF was funded by National Institute of Health grant # P20RR016816. NR 36 TC 3 Z9 3 U1 3 U2 46 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0340-7594 J9 J COMP PHYSIOL A JI J. Comp. Physiol. A -Neuroethol. Sens. Neural Behav. Physiol. PD APR PY 2013 VL 199 IS 4 BP 279 EP 283 DI 10.1007/s00359-012-0791-5 PG 5 WC Behavioral Sciences; Neurosciences; Physiology; Zoology SC Behavioral Sciences; Neurosciences & Neurology; Physiology; Zoology GA 112CJ UT WOS:000316569300003 PM 23322446 ER PT J AU Hribal, R Jewgenow, K Braun, BC Comizzoli, P AF Hribal, R. Jewgenow, K. Braun, B. C. Comizzoli, P. TI Influence of Culture Medium Composition on Relative mRNA Abundances in Domestic Cat Embryos SO REPRODUCTION IN DOMESTIC ANIMALS LA English DT Article ID IN-VITRO FERTILIZATION; BOVINE BLASTOCYSTS; DEVELOPMENTAL COMPETENCE; GENE TRANSCRIPTS; MOUSE EMBRYOS; EXPRESSION; MATURATION; OOCYTES; VIVO; CRYOPRESERVATION AB Contents Different culture conditions have been used to produce domestic cat embryos. As part of the in vitro procedures, the medium composition significantly affects the quality of the embryo development also. Quality assessments based on cleavage kinetics and blastomere symmetry are useful, but embryos also can differ in their relative gene expression patterns despite similar morphological characteristics. The aim of this study was to compare cat embryos produced with two different in vitro culture systems routinely used in two different laboratories [Smithsonian Conservation Biology Institute, Washington D.C., USA (SCBI) and Leibniz Institute for Zoo and Wildlife Research, Berlin, Germany (IZW)]. Specifically, relative mRNA expression patterns of critical genes for pre-implantation embryo development were assessed in both conditions. Embryos were produced in parallel in both culture systems by IVF using frozen-thawed ejaculated semen in the United States and fresh epididymal sperm in Germany. Success of embryo development in vitro was recorded as well as relative mRNA abundances [DNA methyltransferases 1 and 3A (DNMT1, DNMT3A), gap junction protein alpha 1 (GJA1), octamer-binding transcription factor 4 [OCT4], insulin-like growth factors 1 and 2 receptors (IGF1R, IGF2R), beta-actin (ACTB)] in pools of days 45 morulae by semi-quantitative RT-PCR assay. Percentages of cleaved embryos were similar (p>0.05) between both culture systems, regardless of the location. OCT4 mRNA abundance was higher (p<0.05) in embryos derived in the SCBI culture system compared with those from the IZW system when epididymal sperm was used for IVF. No clear correlation between the expression pattern and the culture system could be found for all other genes. It is suggested that OCT4 expression might be affected by the media composition in some conditions and can be the indicator of a better embryo quality. C1 [Hribal, R.; Jewgenow, K.; Braun, B. C.] Leibniz Inst Zoo & Wildlife Res IZW, D-10252 Berlin, Germany. [Comizzoli, P.] Smithsonian Conservat Biol Inst, Dept Reprod Sci, Washington, DC USA. RP Hribal, R (reprint author), Leibniz Inst Zoo & Wildlife Res IZW, PF 601103, D-10252 Berlin, Germany. EM hribal@izw-berlin.de RI Braun, Beate/J-8641-2016 NR 33 TC 6 Z9 8 U1 0 U2 11 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0936-6768 J9 REPROD DOMEST ANIM JI Reprod. Domest. Anim. PD APR PY 2013 VL 48 IS 2 BP 245 EP 251 DI 10.1111/j.1439-0531.2012.02139.x PG 7 WC Agriculture, Dairy & Animal Science; Reproductive Biology; Veterinary Sciences SC Agriculture; Reproductive Biology; Veterinary Sciences GA 108VH UT WOS:000316323800016 PM 22734600 ER PT J AU Clough, W AF Clough, Wayne TI Untitled SO SMITHSONIAN LA English DT Editorial Material C1 Smithsonian Inst, Washington, DC 20560 USA. RP Clough, W (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 APR PY 2013 VL 44 IS 1 BP 8 EP 8 PG 1 WC Humanities, Multidisciplinary SC Arts & Humanities - Other Topics GA 113FK UT WOS:000316651700001 ER PT J AU Jones, J Herman, D Harris, KA Kidwell, PA Fenves, SJ Moser, J Bresnahan, J Goodman, A Putnam, D Sarro, SJ AF Jones, Jerry Herman, Doug Harris, Kenneth A. Kidwell, Peggy Aldrich Fenves, Steven J. Moser, Joann Bresnahan, John Goodman, Alyssa Putnam, Donald Sarro, Steven J. TI Ask Smithsonian SO SMITHSONIAN LA English DT Editorial Material C1 [Herman, Doug] Natl Museum Amer Indian, Washington, DC USA. [Kidwell, Peggy Aldrich] Natl Museum Amer Hist, Washington, DC USA. [Moser, Joann] Smithsonian Amer Art Museum, Washington, DC 20004 USA. [Goodman, Alyssa] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 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 APR PY 2013 VL 44 IS 1 BP 94 EP 94 PG 1 WC Humanities, Multidisciplinary SC Arts & Humanities - Other Topics GA 113FK UT WOS:000316651700026 ER PT J AU Remo, JL Furnish, MD Lawrence, RJ AF Remo, John L. Furnish, Michael D. Lawrence, R. Jeffery TI Plasma-driven Z-pinch X-ray loading and momentum coupling in meteorite and planetary materials SO JOURNAL OF PLASMA PHYSICS LA English DT Article ID ISENTROPIC COMPRESSION AB X-ray momentum coupling coefficients, CM, were determined by measuring stress waveforms in planetary materials subjected to impulsive radiation loading from the Sandia National Laboratories Z-machine. Velocity interferometry (VISAR) diagnostics provided equation-of-state data. Targets were iron and stone meteorites, magnesium-rich olivine (dunite) solid and powder (similar to 5-300 mu m), and Si, Al, and Fe calibration targets. Samples were similar to 1-mm thick and, except for Si, backed by LiF single-crystal windows. X-ray spectra combined thermal radiation (blackbody 170-237 eV) and line emissions from pinch materials (Cu, Ni, Al, or stainless steel). Target fluences of 0.4-1.7 kJ/cm(2) at intensities of 43-260GW/cm(2) produced plasma pressures of 2.6-12.4 GPa. The short (similar to 5 ns) drive pulses gave rise to attenuating stress waves in the samples. The attenuating wave impulse is constant, allowing accurate C-M measurements from rear-surface motion. C-M was 1.9 - 3.1 x 10(-5) s/m for stony meteorites, 2.7 and 0.5x10(-5) s/m for solid and powdered dunite, 0.8 - 1.4 x 10(-5) s/m for iron meteorites, and 0.3, 1.8, and 2.7 x 10(-5) s/m respectively for Si, Fe, and Al calibration targets. Results are consistent with geometric scaling from recent laser hohlraum measurements. CTH hydrocode modeling of X-ray coupling to porous silica corroborated experimental measurements and supported extrapolations to other materials. CTH-modeled C-M for porous materials was low and consistent with experimental results. Analytic modeling (BBAY) of X-ray radiation-induced momentum coupling to selected materials was also performed, often producing higher C-M values than experimental results. Reasons for the higher values include neglect of solid ejecta mechanisms, turbulent mixing of heterogeneous phases, variances in heats of melt/vaporization, sample inhomogeneities, wave interactions at the sample/window boundary, and finite sample/window sizes. The measurements validate application of CM to (inhomogeneous) planetary materials from high-intensity soft X-ray radiation. C1 [Remo, John L.] Harvard Univ, Dept Astron, Cambridge, MA 02138 USA. [Remo, John L.] Harvard Univ, Dept Earth & Planetary Sci, Cambridge, MA 02138 USA. [Remo, John L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Furnish, Michael D.; Lawrence, R. Jeffery] Sandia Natl Labs, Albuquerque, NM 87185 USA. RP Remo, JL (reprint author), Harvard Univ, Dept Astron, Cambridge, MA 02138 USA. EM mdfurni@sandia.gov FU National Nuclear Security Administration under the Stewardship Science Academic Affairs Program through Department of Energy (DOE) [DE-FG52-66NA26215, FG52-09NA29549]; National Nuclear Security Administration under the High Energy Density Laboratory Plasmas program through DOE [FG52-09NA29457]; Harvard University; Lockheed Martin Corp., for the US DOE's NNSA [DE-AC04-94AL85000] FX We thank R. G. Adams for his assistance in carrying out the dunite shot, and J. L. Porter for his hospitality at Sandia National Laboratories (SNL). C. Coverdale and B. Jones welcomed these measurements as ride-along shots with their experiments on the Z-facility. We thank M. I. Petaev for providing chemical abundances of the meteorite targets. JLR was supported by the National Nuclear Security Administration under the Stewardship Science Academic Affairs Program through Department of Energy (DOE) grants Nos. DE-FG52-66NA26215, FG52-09NA29549, and under the High Energy Density Laboratory Plasmas program through DOE grant No. FG52-09NA29457 with Harvard University. This research is solely the authors' views and may not represent views of the DOE, Harvard University, or SNL. SNL is a multi-program laboratory managed and operated by Sandia Corp., a wholly owned subsidiary of Lockheed Martin Corp., for the US DOE's NNSA under contract DE-AC04-94AL85000. NR 24 TC 2 Z9 2 U1 2 U2 15 PU CAMBRIDGE UNIV PRESS PI NEW YORK PA 32 AVENUE OF THE AMERICAS, NEW YORK, NY 10013-2473 USA SN 0022-3778 J9 J PLASMA PHYS JI J. Plasma Phys. PD APR PY 2013 VL 79 BP 121 EP 141 DI 10.1017/S0022377812000712 PN 2 PG 21 WC Physics, Fluids & Plasmas SC Physics GA 105LT UT WOS:000316072400002 ER PT J AU Wei, N Dick, CW Lowe, AJ Gardner, MG AF Wei, Na Dick, Christopher W. Lowe, Andrew J. Gardner, Michael G. TI POLYMORPHIC MICROSATELLITE LOCI FOR VIROLA SEBIFERA (MYRISTICACEAE) DERIVED FROM SHOTGUN 454 PYROSEQUENCING SO APPLICATIONS IN PLANT SCIENCES LA English DT Article DE microsatellite loci; Myristicaceae; shotgun 454 pyrosequencing; Virola sebifera ID VERTEBRATES AB Premise of the study: Polymorphic microsatellite loci were characterized in the dioecious neotropical rainforest tree Virola sebifera. The markers will be used to study ecological and genetic impacts of hunting and landscape change in this vertebrate-dispersed, insect-pollinated tree species. Methods and Results: Simple sequence repeat (SSR) markers were screened from genomic libraries of South American V. sebifera obtained by shotgun 454 pyrosequencing. Primer pairs were tested on Panamanian samples (N = 42). Approximately 52% of the 61 tested SSR markers amplified, and 16% were polymorphic. Ten selected polymorphic SSR loci contained seven to 15 alleles per locus, and polymorphic information content averaged 0.694. Observed heterozygosity ranged from 0.465 to 0.905, and expected heterozygosity was between 0.477 and 0.876. Conclusions: The 10 polymorphic loci will be useful in studying gene flow and genetic structure at local and regional spatial scales in V. sebifera. C1 [Wei, Na; Dick, Christopher W.] Univ Michigan, Dept Ecol & Evolut Biol, Ann Arbor, MI 48109 USA. [Dick, Christopher W.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. [Lowe, Andrew J.; Gardner, Michael G.] Univ Adelaide, Australian Ctr Evolutionary Biol & Biodivers, Sch Earth & Environm Sci, Adelaide, SA 5001, Australia. [Lowe, Andrew J.; Gardner, Michael G.] Univ Adelaide, Inst Environm, Adelaide, SA 5001, Australia. [Lowe, Andrew J.] Sci Resource Ctr, Dept Environm & Nat Resources, Adelaide, SA 5005, Australia. [Gardner, Michael G.] Flinders Univ S Australia, Sch Biol Sci, Adelaide, SA 5001, Australia. [Gardner, Michael G.] S Australian Museum, Evolutionary Biol Unit, Adelaide, SA 5000, Australia. RP Wei, N (reprint author), Univ Michigan, Dept Ecol & Evolut Biol, 830 North Univ Ave, Ann Arbor, MI 48109 USA. EM weina@umich.edu RI Dick, Christopher/A-8744-2008 FU University of Michigan FX The authors thank C. Scotti-Saintagne and I. Scotti for contributing Virola sebifera DNA samples and collection information. The work was supported by a Rackham Graduate Student Research Grant from the University of Michigan. NR 10 TC 4 Z9 4 U1 0 U2 3 PU BOTANICAL SOC AMER INC PI ST LOUIS PA PO BOX 299, ST LOUIS, MO 63166-0299 USA SN 2168-0450 J9 APPL PLANT SCI JI Appl. Plant Sci. PD APR PY 2013 VL 1 IS 4 AR 1200295 DI 10.3732/apps.1200295 PG 3 WC Plant Sciences SC Plant Sciences GA AQ1QM UT WOS:000342556100001 ER PT J AU Evans, S AF Evans, Susan TI Personal Beliefs and National Stories: Theater in Museums as a Tool for Exploring Historical Memory SO CURATOR-THE MUSEUM JOURNAL LA English DT Article AB How does what we remember about history relate to true historical understanding, and how can the museum become a location for these conversations? During the summer of 2011, the National Museum of American History challenged audiences to consider issues of historical memory and national history through the performance of an interactive museum theater program, The Time Trial of John Brown. Using the Time Trial approach as a case study, this article reveals that interactive theater in museums can provide a platform from which audiences assert their own historical understanding while learning firsthand about their role in creating a shared knowledge of American history. As the role of museums evolves in the twenty-first century, new attention must be paid to this personal process of examining and creating history and memory through performance. It is through performance and participation that history and memory are both examined and created by the audience. C1 Smithsonian Inst, Natl Museum Amer Hist, Off Educ & Publ Programs, Washington, DC 20013 USA. RP Evans, S (reprint author), Smithsonian Inst, Natl Museum Amer Hist, Off Educ & Publ Programs, 14th St & Constitut Ave NW,NMAH MRC 603, Washington, DC 20013 USA. EM EvansSN@si.edu NR 17 TC 1 Z9 1 U1 0 U2 0 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0011-3069 EI 2151-6952 J9 CURATOR JI Curator PD APR PY 2013 VL 56 IS 2 BP 189 EP 197 DI 10.1111/cura.12019 PG 9 WC Humanities, Multidisciplinary SC Arts & Humanities - Other Topics GA V41AV UT WOS:000209520000003 ER PT J AU Watson, B Werb, SR AF Watson, Bill Werb, Shari Rosenstein TI One Hundred Strong: A Colloquium on Transforming Natural History Museums in the Twenty-first Century SO CURATOR-THE MUSEUM JOURNAL LA English DT Article AB In February 2012, the Smithsonian's National Museum of Natural History (NMNH) convened 100 colleagues from 43 organizations to initiate a collaborative learning research agenda focused on examining important areas for innovation to better serve twenty-first-century audiences. The conference organizers anticipated that scientists, educators, exhibit professionals, and other members of the natural history community would identify and prioritize research questions about what, how, why, when, and where people learn about natural history. We prepared to engage in a conversation about how natural history museums could change what they do. The participants' overwhelming passion for their work, and for natural history museums and their transformative potential for society, quickly turned the conversation toward how natural history museums should change what they are. The result was an emergent learning research agenda situated within a broader vision for natural history museums. C1 [Watson, Bill] Smithsonian Inst, Natl Museum Nat Hist, Learning Experiences & Evaluat, Washington, DC 20560 USA. [Werb, Shari Rosenstein] Smithsonian Inst, Natl Museum Nat Hist, Educ & Outreach, Washington, DC 20560 USA. RP Watson, B (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Learning Experiences & Evaluat, Washington, DC 20560 USA. EM WatsonB@si.edu; werbs@si.edu NR 14 TC 10 Z9 10 U1 0 U2 0 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0011-3069 EI 2151-6952 J9 CURATOR JI Curator PD APR PY 2013 VL 56 IS 2 BP 255 EP 265 DI 10.1111/cura.12023 PG 11 WC Humanities, Multidisciplinary SC Arts & Humanities - Other Topics GA V41AV UT WOS:000209520000007 ER PT J AU Estrada, C Wcislo, WT Van Bael, SA AF Estrada, Catalina Wcislo, William T. Van Bael, Sunshine A. TI Symbiotic fungi alter plant chemistry that discourages leaf-cutting ants SO NEW PHYTOLOGIST LA English DT Article DE Atta colombica; Colletotrichum tropicale; Cucumis sativus; endophytic fungi; leaf-cutting ants; plant defenses; symbiosis ID ATTA-CEPHALOTES L; REICH HYMENOPTERA-FORMICIDAE; INDUCED SYSTEMIC RESISTANCE; ENDOPHYTIC FUNGI; COLLETOTRICHUM-LAGENARIUM; VOLATILE ANTIMICROBIALS; NEEDLE ENDOPHYTES; POLYPHAGOUS MOTH; THEOBROMA-CACAO; SPRUCE BUDWORM AB Fungal symbionts that live asymptomatically inside plant tissues (endophytes) can influence plantinsect interactions. Recent work has shown that damage by leaf-cutting ants, a major Neotropical defoliator, is reduced to almost half in plants with high densities of endophytes. We investigated changes in the phenotype of leaves that could influence ants' behavior to result in the reduction of foliar damage. We produced cucumber seedlings with high and low densities of one common endophyte species, Colletotrichum tropicale. We used the leaves in bioassays and to compare chemical and physical leaf characteristics important for ants' food selection. Ants cut about one-third more area of cucumber leaves with lower densities of endophytes and removed c. 20% more paper disks impregnated with the extracts of those leaves compared with leaves and disks from plants hosting the fungus. Colletotrichum tropicale colonization did not cause detectable changes in the composition of volatile compounds, cuticular waxes, nutrients or leaf toughness. Our study shows that endophytes changed leaf chemistry and suggests that compounds with relative low volatility released after leaf wounding are a major factor influencing foraging decisions by ants when choosing between plants with low or high endophyte loads. C1 [Estrada, Catalina; Wcislo, William T.; Van Bael, Sunshine A.] Smithsonian Trop Res Inst, Balboa 084303092, Panama. [Van Bael, Sunshine A.] Tulane Univ, Dept Ecol & Evolutionary Biol, New Orleans, LA 70118 USA. RP Estrada, C (reprint author), Smithsonian Trop Res Inst, Balboa 084303092, Panama. EM estradac@si.edu FU Smithsonian Institute Scholarly Studies Program; Restricted Endowment Funds; Smithsonian Institute; NSF [DEB-0949602]; SENACYT [FID10-091] FX We thank: M. Caballero, H. Espinosa, M. Franco, A. Conception, F. Santos, E. Rojas, T. Hammer, J. Urriola, C. Gill and R. Walter for laboratory support; N. Gomez and K. Tidgewell for advice in chemical analyses; P. Galgani, R. Urriola, A. Ruiz and J. Ceballos for logistic support; and three anonymous reviewers for comments on the manuscript. This work was funded by the Smithsonian Institute Scholarly Studies Program to W. T. W. and S. A. V., Restricted Endowment Funds to C. E., S. A. V., W. T. W., a Smithsonian Institute Postdoctoral Fellowship to C. E., NSF DEB-0949602 to S. A. V. and W. T. W., and SENACYT FID10-091 to S. A. V. and W. T. W. Permission was granted to for this research by Panama's Authority on the Environment (ANAM). NR 88 TC 26 Z9 26 U1 1 U2 120 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0028-646X EI 1469-8137 J9 NEW PHYTOL JI New Phytol. PD APR PY 2013 VL 198 IS 1 BP 241 EP 251 DI 10.1111/nph.12140 PG 11 WC Plant Sciences SC Plant Sciences GA 096YH UT WOS:000315440400025 PM 23406415 ER PT J AU Condit, R Engelbrecht, BMJ Pino, D Perez, R Turner, BL AF Condit, Richard Engelbrecht, Bettina M. J. Pino, Delicia Perez, Rolando Turner, Benjamin L. TI Species distributions in response to individual soil nutrients and seasonal drought across a community of tropical trees SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA LA English DT Article DE tropical soil resources; phosphorus limitation; climate response; environmental control; plant communities ID RAIN-FOREST; HABITAT SPECIALIZATION; DISTRIBUTION PATTERNS; PHOSPHORUS; NITROGEN; DIVERSITY; MECHANISMS; VEGETATION; GRADIENTS; MORTALITY AB Tropical forest vegetation is shaped by climate and by soil, but understanding how the distributions of individual tree species respond to specific resources has been hindered by high diversity and consequent rarity. To study species over an entire community, we surveyed trees and measured soil chemistry across climatic and geological gradients in central Panama and then used a unique hierarchical model of species occurrence as a function of rainfall and soil chemistry to circumvent analytical difficulties posed by rare species. The results are a quantitative assessment of the responses of 550 tree species to eight environmental factors, providing a measure of the importance of each factor across the entire tree community. Dry-season intensity and soil phosphorus were the strongest predictors, each affecting the distribution of more than half of the species. Although we anticipated clear-cut responses to dry-season intensity, the finding that many species have pronounced associations with either high or low phosphorus reveals a previously unquantified role for this nutrient in limiting tropical tree distributions. The results provide the data necessary for understanding distributional limits of tree species and predicting future changes in forest composition. C1 [Condit, Richard; Engelbrecht, Bettina M. J.; Perez, Rolando; Turner, Benjamin L.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. [Engelbrecht, Bettina M. J.; Pino, Delicia] Univ Bayreuth, Dept Plant Ecol, D-95440 Bayreuth, Germany. RP Condit, R (reprint author), Smithsonian Trop Res Inst, Apartado 0843-03092, Balboa, Ancon, Panama. EM conditr@gmail.com RI Turner, Benjamin/E-5940-2011 OI Turner, Benjamin/0000-0002-6585-0722 FU US National Science Foundation [0948585]; US Department of Defense; US Agency for International Development; Deutsche Forschungsgemeinschaft; Smithsonian Tropical Research Institute FX We thank the dozens of field and laboratory assistants who have measured trees, collected soil, and run extractions, and we thank J. Dalling and T. Brenes for comments on the manuscript. Funding was provided by US National Science Foundation Grant 0948585, the US Department of Defense, the US Agency for International Development, and the Deutsche Forschungsgemeinschaft. The Smithsonian Tropical Research Institute provided financial support for soil analyses and tree inventories, as well serving as the base of operations. NR 46 TC 83 Z9 91 U1 15 U2 144 PU NATL ACAD SCIENCES PI WASHINGTON PA 2101 CONSTITUTION AVE NW, WASHINGTON, DC 20418 USA SN 0027-8424 J9 P NATL ACAD SCI USA JI Proc. Natl. Acad. Sci. U. S. A. PD MAR 26 PY 2013 VL 110 IS 13 BP 5064 EP 5068 DI 10.1073/pnas.1218042110 PG 5 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 131XN UT WOS:000318031900049 PM 23440213 ER PT J AU Kirrander, A Rittenhouse, S Ascoli, M Eyler, EE Gould, PL Sadeghpour, HR AF Kirrander, Adam Rittenhouse, Seth Ascoli, Marco Eyler, Edward E. Gould, Phillip L. Sadeghpour, H. R. TI Approach to form long-range ion-pair molecules in an ultracold Rb gas SO PHYSICAL REVIEW A LA English DT Article ID NEGATIVE-ION; STATES; SPECTROSCOPY AB We propose a realizable and efficient approach for exciting long-range ion-pair molecules, known as heavy Rydberg states, in an ultracold Rb-85 gas via Feshbach resonances. Heavy Rydberg states, the molecular analogs of electronic Rydberg states, with the electron replaced by an atomic anion, offer opportunities for novel physics, including the formation of ultracold anions and strongly coupled plasmas. We map the positions, lifetimes, and Franck-Condon factors of heavy Rydberg resonances across a wide range of excitation energies, and we calculate the rates of formation for the most promising transitions through long-lived intermediate interferometric resonances. DOI: 10.1103/PhysRevA.87.031402 C1 [Kirrander, Adam] Univ Edinburgh, Sch Chem, Edinburgh EH9 3JJ, Midlothian, Scotland. [Kirrander, Adam; Rittenhouse, Seth; Sadeghpour, H. R.] Harvard Smithsonian Ctr Astrophys, ITAMP, Cambridge, MA 02138 USA. [Rittenhouse, Seth] Western Washington Univ, Dept Phys & Astron, Bellingham, WA 98225 USA. [Ascoli, Marco; Eyler, Edward E.; Gould, Phillip L.] Univ Connecticut, Dept Phys, Storrs, CT 06269 USA. RP Kirrander, A (reprint author), Univ Edinburgh, Sch Chem, West Mains Rd, Edinburgh EH9 3JJ, Midlothian, Scotland. EM adam.kirrander@ed.ac.uk FU National Science Foundation through a grant for the Institute for Theoretical Atomic, Molecular, and Optical Physics at Harvard University and Smithsonian Astrophysical Observatory; National Science Foundation FX This work was supported by the National Science Foundation through a grant for the Institute for Theoretical Atomic, Molecular, and Optical Physics at Harvard University and Smithsonian Astrophysical Observatory and by a National Science Foundation grant to the University of Connecticut. We are grateful to Z. Pavlovic for the calculations of the wave functions for the Feshbach resonances. The authors acknowledge helpful discussions with S. Yelin and E. Kuznetsova, as well as G. Pichler (H.R.S.), K. Lawley and T. Ridley (A.K.), and B.L. Johnson (S.R.). NR 28 TC 6 Z9 6 U1 0 U2 16 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 MAR 22 PY 2013 VL 87 IS 3 AR 031402 DI 10.1103/PhysRevA.87.031402 PG 4 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA 113IH UT WOS:000316659400002 ER PT J AU Papa, R Kapan, DD Counterman, BA Maldonado, K Lindstrom, DP Reed, RD Nijhout, HF Hrbek, T McMillan, WO AF Papa, Riccardo Kapan, Durrell D. Counterman, Brian A. Maldonado, Karla Lindstrom, Daniel P. Reed, Robert D. Nijhout, H. Frederik Hrbek, Tomas McMillan, W. Owen TI Multi-Allelic Major Effect Genes Interact with Minor Effect QTLs to Control Adaptive Color Pattern Variation in Heliconius erato SO PLOS ONE LA English DT Article ID BUTTERFLY WING PATTERNS; MULLERIAN MIMICRY; LINKAGE MAP; WARNING-COLOR; CONVERGENT EVOLUTION; NATURAL-SELECTION; BICYCLUS-ANYNANA; EYESPOT; ADAPTATION; REVEALS AB Recent studies indicate that relatively few genomic regions are repeatedly involved in the evolution of Heliconius butterfly wing patterns. Although this work demonstrates a number of cases where homologous loci underlie both convergent and divergent wing pattern change among different Heliconius species, it is still unclear exactly how many loci underlie pattern variation across the genus. To address this question for Heliconius erato, we created fifteen independent crosses utilizing the four most distinct color pattern races and analyzed color pattern segregation across a total of 1271 F2 and backcross offspring. Additionally, we used the most variable brood, an F2 cross between H. himera and the east Ecuadorian H. erato notabilis, to perform a quantitative genetic analysis of color pattern variation and produce a detailed map of the loci likely involved in the H. erato color pattern radiation. Using AFLP and gene based markers, we show that fewer major genes than previously envisioned control the color pattern variation in H. erato. We describe for the first time the genetic architecture of H. erato wing color pattern by assessing quantitative variation in addition to traditional linkage mapping. In particular, our data suggest three genomic intervals modulate the bulk of the observed variation in color. Furthermore, we also identify several modifier loci of moderate effect size that contribute to the quantitative wing pattern variation. Our results are consistent with the two-step model for the evolution of mimetic wing patterns in Heliconius and support a growing body of empirical data demonstrating the importance of major effect loci in adaptive change. C1 [Papa, Riccardo; Maldonado, Karla; Hrbek, Tomas] Univ Puerto Rico, Dept Biol, Rio Piedras, PR 00931 USA. [Papa, Riccardo; Maldonado, Karla; Hrbek, Tomas] Univ Puerto Rico, Ctr Appl Trop Ecol & Conservat, Rio Piedras, PR 00931 USA. [Kapan, Durrell D.] Calif Acad Sci, Dept Entomol, San Francisco, CA 94118 USA. [Kapan, Durrell D.] Calif Acad Sci, Ctr Comparat Genom, San Francisco, CA 94118 USA. [Kapan, Durrell D.] Univ Hawaii Manoa, Pacific Biosci Res Ctr, Ctr Conservat & Res Training, Honolulu, HI 96822 USA. [Counterman, Brian A.] Mississippi State Univ, Dept Biol Sci, Mississippi State, MS 39762 USA. [Lindstrom, Daniel P.] Univ Guam, Dept Biol, Mangilao, GU USA. [Reed, Robert D.] Cornell Univ, Dept Ecol & Evolutionary Biol, Ithaca, NY USA. [Nijhout, H. Frederik] Duke Univ, Dept Biol, Durham, NC USA. [Hrbek, Tomas] Univ Fed Amazonas, Inst Biol Sci, Dept Biol, Manaus, Amazonas, Brazil. [McMillan, W. Owen] Smithsonian Trop Res Inst, Panama City, Panama. RP Papa, R (reprint author), Univ Puerto Rico, Dept Biol, Rio Piedras, PR 00931 USA. EM rpapa.lab@gmail.com RI Hrbek, Tomas/J-6988-2012 OI Hrbek, Tomas/0000-0003-3239-7068 FU National Science Foundation [IOS 1052541, DEB-0844244, DEB-9806792]; University of Puerto Rico Rio Piedras' Center for Applied Tropical Ecology and Conservation FX Funding for this study was provided by National Science Foundation grants (IOS 1052541, DEB-0844244, DEB-9806792) to WOM. The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript.; We thank the Ministerio del Ambiente in Ecuador for permission to collect butterflies and Germania Estevez for help and guidance during collecting trips. We give a special thanks to Ana Maria Quiles and many volunteers of the butterfly rearing crew for help rearing larvae and maintaining the Heliconius insectaries at the University of Puerto Rico. Undergraduate and graduate students participating in this project were supported in part by the University of Puerto Rico Rio Piedras' Center for Applied Tropical Ecology and Conservation. AFLP's were generated the Genotyping and Sequencing Center at University of Puerto Rico Rio Piedras. NR 90 TC 19 Z9 19 U1 1 U2 40 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 MAR 22 PY 2013 VL 8 IS 3 AR e57033 DI 10.1371/journal.pone.0057033 PG 19 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 111VQ UT WOS:000316549400008 PM 23533571 ER PT J AU Krediet, CJ Ritchie, KB Paul, VJ Teplitski, M AF Krediet, Cory J. Ritchie, Kim B. Paul, Valerie J. Teplitski, Max TI Coral-associated micro-organisms and their roles in promoting coral health and thwarting diseases SO PROCEEDINGS OF THE ROYAL SOCIETY B-BIOLOGICAL SCIENCES LA English DT Review DE coral microbiology; commensal bacteria; microbiota ID PATHOGEN SERRATIA-MARCESCENS; ACROPORA-DIGITIFERA GENOME; MUCUS-ASSOCIATED BACTERIA; NITROGEN-FIXING BACTERIA; SCLERACTINIAN CORAL; PORITES-ASTREOIDES; MICROBIAL ACTIVITY; PHAGE THERAPY; CELL BIOLOGY; REEF CORALS AB Over the last decade, significant advances have been made in characterization of the coral microbiota. Shifts in its composition often correlate with the appearance of signs of diseases and/or bleaching, thus suggesting a link between microbes, coral health and stability of reef ecosystems. The understanding of interactions in coral-associated microbiota is informed by the on-going characterization of other microbiomes, which suggest that metabolic pathways and functional capabilities define the 'core' microbiota more accurately than the taxonomic diversity of its members. Consistent with this hypothesis, there does not appear to be a consensus on the specificity in the interactions of corals with microbial commensals, even though recent studies report potentially beneficial functions of the coral-associated bacteria. They cycle sulphur, fix nitrogen, produce antimicrobial compounds, inhibit cell-to-cell signalling and disrupt virulence in opportunistic pathogens. While their beneficial functions have been documented, it is not certain whether or how these microbes are selected by the hosts. Therefore, understanding the role of innate immunity, signal and nutrient exchange in the establishment of coral microbiota and in controlling its functions will probably reveal ancient, evolutionarily conserved mechanisms that dictate the outcomes of host-microbial interactions, and impact the resilience of the host. C1 [Krediet, Cory J.; Teplitski, Max] Univ Florida IFAS, Gainesville, FL 32610 USA. [Ritchie, Kim B.] Mote Marine Lab, Sarasota, FL 34236 USA. [Ritchie, Kim B.; Teplitski, Max] Univ Florida, Soil & Water Sci Dept, Inst Food & Agr Sci, Gainesville, FL 32611 USA. [Teplitski, Max] Smithsonian Marine Stn, Ft Pierce, FL 34949 USA. RP Teplitski, M (reprint author), Univ Florida IFAS, Gainesville, FL 32610 USA. EM maxtep@ufl.edu FU Protect Our Reefs program; proceeds from the sales of 'Protect Our Reefs' specialty license plates; Smithsonian Institution FX The preparation of this manuscript was supported by grants from Protect Our Reefs program to the co-authors. Protect Our Reefs program is funded by the proceeds from the sales of 'Protect Our Reefs' specialty license plates and is managed by Mote Marine Laboratory through a peer-reviewed process. M. T. is supported by the 2012 George E. Burch Fellowship in Theoretical Medicine and Affiliated Sciences at the Smithsonian Institution. This is contribution 903 of the Smithsonian Marine Station at Fort Pierce. NR 102 TC 56 Z9 57 U1 14 U2 251 PU ROYAL SOC PI LONDON PA 6-9 CARLTON HOUSE TERRACE, LONDON SW1Y 5AG, ENGLAND SN 0962-8452 J9 P ROY SOC B-BIOL SCI JI Proc. R. Soc. B-Biol. Sci. PD MAR 22 PY 2013 VL 280 IS 1755 AR 20122328 DI 10.1098/rspb.2012.2328 PG 9 WC Biology; Ecology; Evolutionary Biology SC Life Sciences & Biomedicine - Other Topics; Environmental Sciences & Ecology; Evolutionary Biology GA 081YC UT WOS:000314357600001 PM 23363627 ER PT J AU Gutierrez, EE Helgen, KM AF Gutierrez, Eliecer E. Helgen, Kristofer M. TI Outdated taxonomy blocks conservation SO NATURE LA English DT Letter C1 [Gutierrez, Eliecer E.; Helgen, Kristofer M.] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA. RP Gutierrez, EE (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA. EM gutierreze@si.edu RI Gutierrez, Eliecer/D-5703-2014 OI Gutierrez, Eliecer/0000-0001-6790-8185 NR 2 TC 9 Z9 9 U1 1 U2 19 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 0028-0836 EI 1476-4687 J9 NATURE JI Nature PD MAR 21 PY 2013 VL 495 IS 7441 BP 314 EP 314 PG 1 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 113EY UT WOS:000316650500025 PM 23518556 ER PT J AU Vieira, JD Marrone, DP Chapman, SC De Breuck, C Hezaveh, YD Weiss, A Aguirre, JE Aird, KA Aravena, M Ashby, MLN Bayliss, M Benson, BA Biggs, AD Bleem, LE Bock, JJ Bothwell, M Bradford, CM Brodwin, M Carlstrom, JE Chang, CL Crawford, TM Crites, AT de Haan, T Dobbs, MA Fomalont, EB Fassnacht, CD George, EM Gladders, MD Gonzalez, AH Greve, TR Gullberg, B Halverson, NW High, FW Holder, GP Holzapfel, WL Hoover, S Hrubes, JD Hunter, TR Keisler, R Lee, AT Leitch, EM Lueker, M Luong-Van, D Malkan, M McIntyre, V McMahon, JJ Mehl, J Menten, KM Meyer, SS Mocanu, LM Murphy, EJ Natoli, T Padin, S Plagge, T Reichardt, CL Rest, A Ruel, J Ruhl, JE Sharon, K Schaffer, KK Shaw, L Shirokoff, E Spilker, JS Stalder, B Staniszewski, Z Stark, AA Story, K Vanderlinde, K Welikala, N Williamson, R AF Vieira, J. D. Marrone, D. P. Chapman, S. C. De Breuck, C. Hezaveh, Y. D. Weiss, A. Aguirre, J. E. Aird, K. A. Aravena, M. Ashby, M. L. N. Bayliss, M. Benson, B. A. Biggs, A. D. Bleem, L. E. Bock, J. J. Bothwell, M. Bradford, C. M. Brodwin, M. Carlstrom, J. E. Chang, C. L. Crawford, T. M. Crites, A. T. de Haan, T. Dobbs, M. A. Fomalont, E. B. Fassnacht, C. D. George, E. M. Gladders, M. D. Gonzalez, A. H. Greve, T. R. Gullberg, B. Halverson, N. W. High, F. W. Holder, G. P. Holzapfel, W. L. Hoover, S. Hrubes, J. D. Hunter, T. R. Keisler, R. Lee, A. T. Leitch, E. M. Lueker, M. Luong-Van, D. Malkan, M. McIntyre, V. McMahon, J. J. Mehl, J. Menten, K. M. Meyer, S. S. Mocanu, L. M. Murphy, E. J. Natoli, T. Padin, S. Plagge, T. Reichardt, C. L. Rest, A. Ruel, J. Ruhl, J. E. Sharon, K. Schaffer, K. K. Shaw, L. Shirokoff, E. Spilker, J. S. Stalder, B. Staniszewski, Z. Stark, A. A. Story, K. Vanderlinde, K. Welikala, N. Williamson, R. TI Dusty starburst galaxies in the early Universe as revealed by gravitational lensing SO NATURE LA English DT Article ID SOUTH-POLE TELESCOPE; SUBMILLIMETER GALAXY; MOLECULAR GAS; DEEP-FIELD; REDSHIFT; COUNTS; MODEL AB In the past decade, our understanding of galaxy evolution has been revolutionized by the discovery that luminous, dusty starburst galaxies were 1,000 times more abundant in the early Universe than at present(1,2). It has, however, been difficult to measure the complete redshift distribution of these objects, especially at the highest redshifts (z>4). Here we report a redshift survey at a wavelength of three millimetres, targeting carbon monoxide line emission from the star-forming molecular gas in the direction of extraordinarily bright millimetre-wave-selected sources. High-resolution imaging demonstrates that these sources are strongly gravitationally lensed by foreground galaxies. We detect spectral lines in 23 out of 26 sources and multiple lines in 12 of those 23 sources, from which we obtain robust, unambiguous redshifts. At least 10 of the sources are found to lie at z > 4, indicating that the fraction of dusty starburst galaxies at high redshifts is greater than previously thought. Models of lens geometries in the sample indicate that the background objects are ultra-luminous infrared galaxies, powered by extreme bursts of star formation. C1 [Vieira, J. D.; Bock, J. J.; Lueker, M.; Padin, S.; Shirokoff, E.; Staniszewski, Z.] CALTECH, Pasadena, CA 91125 USA. [Marrone, D. P.; Bothwell, M.; Spilker, J. S.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Chapman, S. C.] Dalhousie Univ, Dept Phys & Atmospher Sci, Halifax, NS B3H 3J5, Canada. [Chapman, S. C.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [De Breuck, C.; Aravena, M.; Biggs, A. D.; Gullberg, B.] European So Observ, D-85748 Garching, Germany. [Hezaveh, Y. D.; de Haan, T.; Dobbs, M. A.; Holder, G. P.; Shaw, L.; Vanderlinde, K.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada. [Weiss, A.; Menten, K. M.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Aguirre, J. E.] Univ Penn, Philadelphia, PA 19104 USA. [Aird, K. A.; Hrubes, J. D.; Luong-Van, D.] Univ Chicago, Chicago, IL 60637 USA. [Ashby, M. L. N.; Stalder, B.; Stark, A. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Bayliss, M.; Ruel, J.] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. [Benson, B. A.; Bleem, L. E.; Carlstrom, J. E.; Chang, C. L.; Crawford, T. M.; Crites, A. T.; Gladders, M. D.; High, F. W.; Hoover, S.; Keisler, R.; Leitch, E. M.; McMahon, J. J.; Mehl, J.; Meyer, S. S.; Mocanu, L. M.; Natoli, T.; Padin, S.; Plagge, T.; Sharon, K.; Schaffer, K. K.; Story, K.; Williamson, R.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Benson, B. A.; Carlstrom, J. E.; Chang, C. L.; Hoover, S.; McMahon, J. J.; Meyer, S. S.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA. [Bleem, L. E.; Carlstrom, J. E.; Keisler, R.; Meyer, S. S.; Natoli, T.; Story, K.] Univ Chicago, Dept Phys, Chicago, IL 60637 USA. [Bock, J. J.; Bradford, C. M.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Brodwin, M.] Univ Missouri, Dept Phys & Astron, Kansas City, MO 64110 USA. [Carlstrom, J. E.; Crawford, T. M.; Crites, A. T.; Gladders, M. D.; High, F. W.; Leitch, E. M.; Mehl, J.; Meyer, S. S.; Mocanu, L. M.; Padin, S.; Plagge, T.; Sharon, K.; Williamson, R.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. [Carlstrom, J. E.; Chang, C. L.] Argonne Natl Lab, Argonne, IL 60439 USA. [Fomalont, E. B.; Hunter, T. R.] Natl Radio Astron Observ, Charlottesville, VA 22903 USA. [Fassnacht, C. D.] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA. [George, E. M.; Holzapfel, W. L.; Lee, A. T.; Reichardt, C. L.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. [Gonzalez, A. H.] Univ Florida, Dept Astron, Gainesville, FL 32611 USA. [Greve, T. R.] UCL, Dept Phys & Astron, London WC1E 6BT, England. [Halverson, N. W.] Univ Colorado, Dept Astrophys & Planetary Sci, Boulder, CO 80309 USA. [Halverson, N. W.] Univ Colorado, Dept Phys, Boulder, CO 80309 USA. [Lee, A. T.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Dept Phys, Berkeley, CA 94720 USA. [Malkan, M.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. [McIntyre, V.] CSIRO, Australia Telescope Natl Facil, Epping, NSW 1710, Australia. [McMahon, J. J.] Univ Michigan, Dept Phys, Ann Arbor, MI 48109 USA. [Murphy, E. J.] Observ Carnegie Inst Sci, Pasadena, CA 91101 USA. [Rest, A.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Ruhl, J. E.; Staniszewski, Z.] Case Western Reserve Univ, Dept Phys, Ctr Educ & Res Cosmol & Astrophys, Cleveland, OH 44106 USA. [Sharon, K.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Schaffer, K. K.] Sch Art Inst Chicago, Liberal Arts Dept, Chicago, IL 60603 USA. [Shaw, L.] Yale Univ, Dept Phys, New Haven, CT 06520 USA. [Welikala, N.] Univ Paris 11, Inst Astrophys Spatiale, F-91405 Orsay, France. [Welikala, N.] CNRS, F-91405 Orsay, France. RP Vieira, JD (reprint author), CALTECH, 1200 East Calif Blvd, Pasadena, CA 91125 USA. EM vieira@caltech.edu RI Holzapfel, William/I-4836-2015; Williamson, Ross/H-1734-2015; OI Williamson, Ross/0000-0002-6945-2975; Marrone, Daniel/0000-0002-2367-1080; Aird, Kenneth/0000-0003-1441-9518; Reichardt, Christian/0000-0003-2226-9169; De Breuck, Carlos/0000-0002-6637-3315; Hunter, Todd/0000-0001-6492-0090; Stark, Antony/0000-0002-2718-9996 FU National Science Foundation; Kavli Foundation; Gordon and Betty Moore Foundation; NASA from the Space Telescope Science Institute; NSERC; CRC; ClfAR FX The SPT is supported by the National Science Foundation, the Kavli Foundation and the Gordon and Betty Moore Foundation. ALMA is a partnership of ESO (representing its member states), NSF (USA) and NINS (Japan), together with NRC (Canada) and NSC and ASIAA (Taiwan), in cooperation with Chile. The Joint ALMA Observatory is operated by ESO, AUI/NRAO and NAOJ. The National Radio Astronomy Observatory is a facility of the NSF operated under cooperative agreement by Associated Universities, Inc. Partial support for this work was provided by NASA from the Space Telescope Science Institute. This work is based in part on observations made with Herschel, a European Space Agency Cornerstone Mission with significant participation by NASA. Work at McGill University is supported by NSERC, the CRC programme and ClfAR. NR 27 TC 109 Z9 109 U1 1 U2 16 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 0028-0836 EI 1476-4687 J9 NATURE JI Nature PD MAR 21 PY 2013 VL 495 IS 7441 BP 344 EP 347 DI 10.1038/nature12001 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 113EY UT WOS:000316650500037 PM 23485967 ER PT J AU Safavi-Naini, A Rittenhouse, ST Blume, D Sadeghpour, HR AF Safavi-Naini, A. Rittenhouse, Seth T. Blume, D. Sadeghpour, H. R. TI Nonuniversal bound states of two identical heavy fermions and one light particle SO PHYSICAL REVIEW A LA English DT Article ID INTERACTING PARTICLES; DYNAMICS AB We study the behavior of the bound-state energy of a system consisting of two identical heavy fermions of mass M and a light particle of mass m. The heavy fermions interact with the light particle through a short-range two-body potential with positive s-wave scattering length a(s). We impose a short-range boundary condition on the logarithmic derivative of the hyperradial wave function and show that, in the regime where Efimov states are absent, a nonuniversal three-body state cuts through the universal three-body states previously described by Kartavtsev and Malykh [O. I. Kartavtsev and A. V. Malykh, J. Phys. B 40, 1429 (2007)]. The presence of the nonuniversal state alters the behavior of the universal states in certain regions of the parameter space. We show that the existence of the nonuniversal state is predicted accurately by a simple quantum defect theory model that utilizes hyperspherical coordinates. An empirical two-state model is employed to quantify the coupling of the nonuniversal state to the universal states. DOI: 10.1103/PhysRevA.87.032713 C1 [Safavi-Naini, A.] MIT, Dept Phys, Cambridge, MA 02139 USA. [Safavi-Naini, A.; Rittenhouse, Seth T.; Blume, D.; Sadeghpour, H. R.] Harvard Smithsonian Ctr Astrophys, ITAMP, Cambridge, MA 02138 USA. [Rittenhouse, Seth T.] Western Washington Univ, Dept Phys & Astron, Bellingham, WA 98225 USA. [Blume, D.] Washington State Univ, Dept Phys & Astron, Pullman, WA 99164 USA. RP Safavi-Naini, A (reprint author), MIT, Dept Phys, Cambridge, MA 02139 USA. EM safavin@mit.edu FU National Science Foundation (NSF) [PHY-1205443] FX This work was supported by the National Science Foundation (NSF) through a grant for the Institute for Theoretical Atomic, Molecular and Optical Physics at Harvard University and Smithsonian Astrophysical Observatory. D.B. acknowledges support by the NSF through Grant No. PHY-1205443. We acknowledge insightful correspondence with S. Endo and P. Naidon. NR 30 TC 6 Z9 6 U1 3 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 MAR 21 PY 2013 VL 87 IS 3 AR 032713 DI 10.1103/PhysRevA.87.032713 PG 6 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA 110AB UT WOS:000316412900005 ER PT J AU Akimkin, V Zhukovska, S Wiebe, D Semenov, D Pavlyuchenkov, Y Vasyunin, A Birnstiel, T Henning, T AF Akimkin, V. Zhukovska, S. Wiebe, D. Semenov, D. Pavlyuchenkov, Ya Vasyunin, A. Birnstiel, T. Henning, Th TI PROTOPLANETARY DISK STRUCTURE WITH GRAIN EVOLUTION: THE ANDES MODEL SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; astrochemistry; circumstellar matter; stars: formation; stars: pre-main sequence ID T-TAURI STARS; SPECTRAL ENERGY-DISTRIBUTIONS; HERBIG AE/BE STARS; POLYCYCLIC AROMATIC-HYDROCARBONS; RADIATION THERMOCHEMICAL MODELS; PHOTON-DOMINATED REGIONS; CIRCUMSTELLAR DISKS; ACCRETION DISKS; DM-TAURI; MOLECULAR-HYDROGEN AB We present a self-consistent model of a protoplanetary disk: "ANDES" ("AccretioN disk with Dust Evolution and Sedimentation"). ANDES is based on a flexible and extendable modular structure that includes (1) a 1+1D frequency-dependent continuum radiative transfer module, (2) a module to calculate the chemical evolution using an extended gas-grain network with UV/X-ray-driven processes and surface reactions, (3) a module to calculate the gas thermal energy balance, and (4) a 1+1D module that simulates dust grain evolution. For the first time, grain evolution and time-dependent molecular chemistry are included in a protoplanetary disk model. We find that grain growth and sedimentation of large grains onto the disk midplane lead to a dust-depleted atmosphere. Consequently, dust and gas temperatures become higher in the inner disk (R less than or similar to 50 AU) and lower in the outer disk (R greater than or similar to 50 AU), in comparison with the disk model with pristine dust. The response of disk chemical structure to the dust growth and sedimentation is twofold. First, due to higher transparency a partly UV-shielded molecular layer is shifted closer to the dense midplane. Second, the presence of big grains in the disk midplane delays the freeze-out of volatile gas-phase species such as CO there, while in adjacent upper layers the depletion is still effective. Molecular concentrations and thus column densities of many species are enhanced in the disk model with dust evolution, e.g., CO2, NH2CN, HNO, H2O, HCOOH, HCN, and CO. We also show that time-dependent chemistry is important for a proper description of gas thermal balance. C1 [Akimkin, V.; Wiebe, D.; Pavlyuchenkov, Ya] RAS, Inst Astron, Moscow 117901, Russia. [Zhukovska, S.; Semenov, D.; Henning, Th] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Vasyunin, A.] Univ Virginia, Dept Chem, Charlottesville, VA 22903 USA. [Birnstiel, T.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Birnstiel, T.] Excellence Cluster Universe, D-85748 Garching, Germany. RP Akimkin, V (reprint author), RAS, Inst Astron, Pyatnitskaya Str 48, Moscow 117901, Russia. EM akimkin@inasan.ru; zhukovska@mpia.de; dwiebe@inasan.ru; semenov@mpia.de; pavyar@inasan.ru; anton.vasyunin@gmail.com; tbirnstiel@cfa.harvard.edu; henning@mpia.de RI Semenov, Dmitry/B-7446-2012; Vasyunin, Anton/N-9112-2016; Akimkin, Vitaly/N-8883-2016; Pavlyuchenkov, Yaroslav/C-7622-2017 OI Semenov, Dmitry/0000-0002-3913-7114; Birnstiel, Tilman/0000-0002-1899-8783; Vasyunin, Anton/0000-0003-1684-3355; FU RFBR [10-02-00612, 12-02-31248, NSh-3602.2012.2]; Deutsche Forschungsgemeinschaft [SPP 1573, SPP 1385]; National Science Foundation (US) for the astrochemistry program at the University of Virginia FX This research made use of NASA's Astrophysics Data System. This work is supported by the RFBR grants 10-02-00612, 12-02-31248, Federal Targeted Program "Scientific resources of Innovation-Driven Russia" for 2009-2013 and NSh-3602.2012.2. S.Z. is supported by the Deutsche Forschungsgemeinschaft through SPP 1573: "Physics of the Interstellar Medium." D.S. acknowledges support by the Deutsche Forschungsgemeinschaft through SPP 1385: "The first ten million years of the solar system-a planetary materials approach" (SE 1962/1-1 and 1-2). A.V. acknowledges the support of the National Science Foundation (US) for the astrochemistry program at the University of Virginia. We thank Kees Dullemond, Andras Zsom, Ewine F. van Dishoeck, and Simon Bruderer for valuable discussions. We highly appreciate the comments and suggestions of an anonymous referee that helped us a lot to improve the quality of the paper. NR 131 TC 26 Z9 26 U1 2 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 MAR 20 PY 2013 VL 766 IS 1 AR 8 DI 10.1088/0004-637X/766/1/8 PG 24 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 105GH UT WOS:000316054000008 ER PT J AU Bhattacharya, S Habib, S Heitmann, K Vikhlinin, A AF Bhattacharya, Suman Habib, Salman Heitmann, Katrin Vikhlinin, Alexey TI DARK MATTER HALO PROFILES OF MASSIVE CLUSTERS: THEORY VERSUS OBSERVATIONS SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: clusters: general; galaxies: halos; methods: numerical ID OBSERVATIONS COSMOLOGICAL INTERPRETATION; RELAXED GALAXY CLUSTERS; WEAK LENSING ANALYSIS; POWER SPECTRUM; REDSHIFT DEPENDENCE; DENSITY PROFILES; GAS FRACTION; CHANDRA; SIMULATIONS; EVOLUTION AB Dark-matter-dominated cluster-scale halos act as an important cosmological probe and provide a key testing ground for structure formation theory. Focusing on their mass profiles, we have carried out (gravity-only) simulations of the concordance.CDM cosmology, covering a mass range of 2 x 10(12) to 2 x 10(15) h(-1) M-circle dot and a redshift range of z = 0-2, while satisfying the associated requirements of resolution and statistical control. When fitting to the Navarro-Frenk-White profile, our concentration-mass (c-M) relation differs in normalization and shape in comparison to previous studies that have limited statistics in the upper end of the mass range. We show that the flattening of the c-M relation with redshift is naturally expressed if c is viewed as a function of the peak height parameter, nu. Unlike the c-M relation, the slope of the c-nu relation is effectively constant over the redshift range z = 0-2, while the amplitude varies by similar to 30% for massive clusters. This relation is, however, not universal: using a simulation suite covering the allowed wCDM parameter space, we show that the c-nu relation varies by about +/- 20% as cosmological parameters are varied. At fixed mass, the c(M) distribution is well fit by a Gaussian with sigma(c)/< c > similar or equal to 1/3, independent of the radius at which the concentration is defined, the halo dynamical state, and the underlying cosmology. We compare the.CDM predictions with observations of halo concentrations from strong lensing, weak lensing, galaxy kinematics, and X-ray data, finding good agreement for massive clusters (M-vir > 4 x 10(14) h(-1) M-circle dot), but with some disagreements at lower masses. Because of uncertainty in observational systematics and modeling of baryonic physics, the significance of these discrepancies remains unclear. C1 [Bhattacharya, Suman; Habib, Salman; Heitmann, Katrin] Argonne Natl Lab, Div High Energy Phys, Argonne, IL 60439 USA. [Bhattacharya, Suman; Habib, Salman; Heitmann, Katrin] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Habib, Salman; Heitmann, Katrin] Argonne Natl Lab, Div Math & Comp Sci, Argonne, IL 60439 USA. [Vikhlinin, Alexey] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Vikhlinin, Alexey] Space Res Inst IKI, Moscow 117997, Russia. RP Bhattacharya, S (reprint author), Argonne Natl Lab, Div High Energy Phys, Argonne, IL 60439 USA. FU Los Alamos National Laboratory Institutional Computing initiative; DOE [W-7405-ENG-36] FX It is a pleasure to acknowledge discussions and collaborations with Joanne Cohn, Zarija Lukic, Darren Reed, Alexey Voevodkin, and Martin White. We acknowledge several motivating conversations with Masahiro Takada (S.H.) and Mike Gladders (S.H. and K.H.). We thank Volker Springel for discussions and for making GADGET-2 publicly available. We are indebted to Patricia Fasel and Adrian Pope for their contributions to the HACC analysis framework. We thank Anatoly Klypin and Francisco Prada for pointing out a numerical error in an earlier version of the Appendix (now corrected) and for discussions of results obtained by our two groups. A special acknowledgment is due to the resource allocation awarded to us on the hybrid supercomputer Cerrillos and other clusters under the Los Alamos National Laboratory Institutional Computing initiative. Part of this research was supported by the DOE under contract W-7405-ENG-36. The authors acknowledge support from the LDRD programs at Los Alamos National Laboratory and Argonne National Laboratory, where analysis was performed on the Eureka cluster. S.B. and K.H. were supported in part by NASA. NR 83 TC 69 Z9 69 U1 0 U2 7 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAR 20 PY 2013 VL 766 IS 1 AR 32 DI 10.1088/0004-637X/766/1/32 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 105GH UT WOS:000316054000032 ER PT J AU Ciaravella, A Webb, DF Giordano, S Raymond, JC AF Ciaravella, A. Webb, D. F. Giordano, S. Raymond, J. C. TI BRIGHT RAY-LIKE FEATURES IN THE AFTERMATH OF CORONAL MASS EJECTIONS: WHITE LIGHT VERSUS ULTRAVIOLET SPECTRA SO ASTROPHYSICAL JOURNAL LA English DT Article DE Sun: corona; Sun: coronal mass ejections (CMEs); Sun: UV radiation ID CURRENT SHEET; MAGNETIC RECONNECTION; SOLAR-FLARES; MORPHOLOGY; PLASMA; ACCELERATION; OUTFLOWS; DENSITY; FIELD AB Current sheets (CSs) are important signatures of magnetic reconnection in the eruption of confined solar magnetic structures. Models of coronal mass ejections (CMEs) involve formation of a CS connecting the ejected flux rope with the post-eruption magnetic loops. CSs have been identified in white light (WL) images of CMEs as narrow rays trailing the outward moving CME core, and in ultraviolet spectra as narrow bright features emitting the [Fe XVIII] line. In this work, samples of rays detected in WL images or in ultraviolet spectra have been analyzed. Temperatures, widths, and line intensities of the rays have been measured, and their correlation to the CME properties has been studied. The samples show a wide range of temperatures with hot, coronal, and cool rays. In some cases, the UV spectra support the identification of rays as CSs, but they show that some WL rays are cool material from the CME core. In many cases, both hot and cool material are present, but offset from each other along the Ultraviolet Coronagraph Spectrometer slit. We find that about 18% of the WL rays show very hot gas consistent with the CS interpretation, while about 23% show cold gas that we attribute to cool prominence material draining back from the CME core. The remaining events have ordinary coronal temperatures, perhaps because they have relaxed back to a quiescent state. C1 [Ciaravella, A.] INAF Osservatorio Astron Palermo, I-90134 Palermo, Italy. [Webb, D. F.] Boston Coll, Inst Sci Res, Newton, MA 02459 USA. [Giordano, S.] INAF Osservatorio Astron Torino, I-10025 Pino Torinese, Italy. [Raymond, J. C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Ciaravella, A (reprint author), INAF Osservatorio Astron Palermo, Pza Parlamento 1, I-90134 Palermo, Italy. OI Ciaravella, Angela/0000-0002-3127-8078; Giordano, Silvio/0000-0002-3468-8566 FU NASA [NNX09AB17G-R, NNX11AB61G] FX This work was performed under NASA grants NNX09AB17G-R and NNX11AB61G to the Smithsonian Astrophysical Observatory. It was initiated during a series of workshops on Understanding the role of current sheets in solar eruptive phenomena at the International Space Sciences Institute (ISSI). We also benefited from the SOHO/LASCO CME catalog, generated and maintained by the Center for Solar Physics and Space Weather, The Catholic University of America in cooperation with NRL and NASA. NR 41 TC 13 Z9 15 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 MAR 20 PY 2013 VL 766 IS 1 AR 65 DI 10.1088/0004-637X/766/1/65 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 105GH UT WOS:000316054000065 ER PT J AU D'Onghia, E Vogelsberger, M Hernquist, L AF D'Onghia, Elena Vogelsberger, Mark Hernquist, Lars TI SELF-PERPETUATING SPIRAL ARMS IN DISK GALAXIES SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: kinematics and dynamics; galaxies: spiral; methods: numerical ID STAR-FORMATION; MILKY-WAY; INSTABILITIES; SUBSTRUCTURE; DYNAMICS; FEEDBACK AB The causes of spiral structure in galaxies remain uncertain. Leaving aside the grand bisymmetric spirals with their own well-known complications, here we consider the possibility that multi-armed spiral features originate from density inhomogeneities orbiting within disks. Using high-resolution N-body simulations, we follow the motions of stars under the influence of gravity, and show that mass concentrations with properties similar to those of giant molecular clouds can induce the development of spiral arms through a process termed swing amplification. However, unlike in earlier work, we demonstrate that the eventual response of the disk can be highly non-linear, significantly modifying the formation and longevity of the resulting patterns. Contrary to expectations, ragged spiral structures can thus survive at least in a statistical sense long after the original perturbing influence has been removed. C1 [D'Onghia, Elena; Vogelsberger, Mark; Hernquist, Lars] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [D'Onghia, Elena] Univ Wisconsin, Dept Astron, Madison, WI 53706 USA. RP D'Onghia, E (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM edonghia@cfa.harvard.edu NR 43 TC 69 Z9 69 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 MAR 20 PY 2013 VL 766 IS 1 AR 34 DI 10.1088/0004-637X/766/1/34 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 105GH UT WOS:000316054000034 ER PT J AU Gilliland, RL Marcy, GW Rowe, JF Rogers, L Torres, G Fressin, F Lopez, ED Buchhave, LA Christensen-Dalsgaard, J Desert, JM Henze, CE Isaacson, H Jenkins, J Lissauer, JJ Chaplin, WJ Basu, S Metcalfe, TS Elsworth, Y Handberg, R Hekker, S Huber, D Karoff, C Kjeldsen, H Lund, MN Lundkvist, M Miglio, A Charbonneau, D Ford, EB Fortney, JJ Haas, MR Howard, AW Howell, SB Ragozzine, D Thompson, SE AF Gilliland, Ronald L. Marcy, Geoffrey W. Rowe, Jason F. Rogers, Leslie Torres, Guillermo Fressin, Francois Lopez, Eric D. Buchhave, Lars A. Christensen-Dalsgaard, Jorgen Desert, Jean-Michel Henze, Christopher E. Isaacson, Howard Jenkins, Jonm. Lissauer, Jack J. Chaplin, William J. Basu, Sarbani Metcalfe, Travis S. Elsworth, Yvonne Handberg, Rasmus Hekker, Saskia Huber, Daniel Karoff, Christoffer Kjeldsen, Hans Lund, Mikkel N. Lundkvist, Mia Miglio, Andrea Charbonneau, David Ford, Eric B. Fortney, Jonathan J. Haas, Michael R. Howard, Andrew W. Howell, Steve B. Ragozzine, Darin Thompson, Susan E. TI KEPLER-68: THREE PLANETS, ONE WITH A DENSITY BETWEEN THAT OF EARTH AND ICE GIANTS SO ASTROPHYSICAL JOURNAL LA English DT Article DE planetary systems; stars: fundamental parameters; stars: individual (Kepler-68, KIC 11295426, 2MASS J19240775+4902249) ID SOLAR-TYPE STARS; TESTING BLEND SCENARIOS; SPITZER-SPACE-TELESCOPE; EXOPLANET HD 189733B; FINE GUIDANCE SENSOR; SUN-LIKE STAR; TRANSITING PLANET; INITIAL CHARACTERISTICS; EXTRASOLAR PLANETS; ASTEROSEISMIC DATA AB NASA's Kepler Mission has revealed two transiting planets orbiting Kepler-68. Follow-up Doppler measurements have established the mass of the innermost planet and revealed a third Jovian-mass planet orbiting beyond the two transiting planets. Kepler-68b, in a 5.4 day orbit, has M-P = 8.3(-2.4)(+2.2) M-circle plus, R-P = 2.31(-0.09)(+0.06) R-circle plus, and rho(P) = 3.32(-0.98)(+0.86) g cm(-3), giving Kepler-68b a density intermediate between that of the ice giants and Earth. Kepler-68c is Earth-sized, with a radius R-P = 0.953(-0.042)(+0.037) R-circle plus and transits on a 9.6 day orbit; validation of Kepler-68c posed unique challenges. Kepler-68d has an orbital period of 580 +/- 15 days and a minimum mass of M-P sin i = 0.947 +/- 0.035M(J). Power spectra of the Kepler photometry at one minute cadence exhibit a rich and strong set of asteroseismic pulsation modes enabling detailed analysis of the stellar interior. Spectroscopy of the star coupled with asteroseismic modeling of the multiple pulsation modes yield precise measurements of stellar properties, notably T-eff = 5793 +/- 74 K, M-star = 1.079 +/- 0.051 M-circle dot, R-star = 1.243 +/- 0.019 R-circle dot, and rho(star) = 0.7903 +/- 0.0054 g cm(-3), all measured with fractional uncertainties of only a few percent. Models of Kepler-68b suggest that it is likely composed of rock and water, or has a H and He envelope to yield its density similar to 3 g cm(-3). C1 [Gilliland, Ronald L.] Penn State Univ, Dept Astron, University Pk, PA 16802 USA. [Gilliland, Ronald L.] Penn State Univ, Ctr Exoplanets & Habitable Worlds, University Pk, PA 16802 USA. [Marcy, Geoffrey W.; Isaacson, Howard] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Rowe, Jason F.; Henze, Christopher E.; Lissauer, Jack J.; Huber, Daniel; Haas, Michael R.; Howell, Steve B.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Rogers, Leslie] CALTECH, Pasadena, CA 91125 USA. [Torres, Guillermo; Fressin, Francois; Desert, Jean-Michel; Charbonneau, David] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Lopez, Eric D.; Fortney, Jonathan J.] Univ Calif Santa Cruz, Santa Cruz, CA 95064 USA. [Buchhave, Lars A.] Univ Copenhagen, Niels Bohr Inst, DK-2100 Copenhagen, Denmark. [Christensen-Dalsgaard, Jorgen; Handberg, Rasmus; Karoff, Christoffer; Kjeldsen, Hans; Lund, Mikkel N.; Lundkvist, Mia] Stellar Astrophys Ctr, Dept Phys & Astron, DK-8000 Aarhus C, Denmark. [Christensen-Dalsgaard, Jorgen] Natl Ctr Atmospher Res, High Altitude Observ, Boulder, CO 80307 USA. [Jenkins, Jonm.; Thompson, Susan E.] NASA, Ames Res Ctr, SETI Inst, Moffett Field, CA 94035 USA. [Chaplin, William J.; Elsworth, Yvonne; Miglio, Andrea] Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England. [Basu, Sarbani] Yale Univ, Dept Astron, New Haven, CT 06511 USA. [Metcalfe, Travis S.] White Dwarf Res Corp, Boulder, CO 80301 USA. [Hekker, Saskia] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 XH Amsterdam, Netherlands. [Ford, Eric B.; Ragozzine, Darin] Univ Florida, Dept Astron, Gainesville, FL 32611 USA. [Howard, Andrew W.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. RP Gilliland, RL (reprint author), Penn State Univ, Dept Astron, 525 Davey Lab, University Pk, PA 16802 USA. EM gillil@stsci.edu RI Howard, Andrew/D-4148-2015; OI Howard, Andrew/0000-0001-8638-0320; Charbonneau, David/0000-0002-9003-484X; Fortney, Jonathan/0000-0002-9843-4354; Buchhave, Lars A./0000-0003-1605-5666; Metcalfe, Travis/0000-0003-4034-0416; Karoff, Christoffer/0000-0003-2009-7965; Basu, Sarbani/0000-0002-6163-3472; /0000-0001-6545-639X; Lund, Mikkel Norup/0000-0001-9214-5642; Lundkvist, Mia Sloth/0000-0002-8661-2571; Handberg, Rasmus/0000-0001-8725-4502 FU NASA's Science Mission Directorate; W.M. Keck Foundation; NASA, JPL/Caltech; Space Telescope Science Institute [HF-51313.01-A]; NASA [NAS 5-26555, NNX12AC75G, AST-1105930, NNX09AG09A]; Danish National Research Foundation; ASTERISK project (ASTERoseismic Investigations with SONG and Kepler); European Research Council [267864]; NSF [AST-1105930] FX Funding for this tenth Discovery mission is provided by NASA's Science Mission Directorate. The many people contributing to the development of this mission are gratefully acknowledged. We thank Elizabeth Adams, Eric Agol, Natalie Batalha, William Borucki, Stephen Bryson, William Cochran, Andrea Dupree, Debra Fischer, and David Monet for discussion and contributions. The anonymous referee made comments serving to improve the paper. Some of the data used here 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 NASA. The W.M. Keck Foundation provided generous financial support to the Keck Observatory. 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. Partial support for this work was provided by NASA through an award issued by JPL/Caltech. Support for L.A.R. was provided through Hubble Fellowship grant No. HF-51313.01-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. G.T. acknowledges partial support for this work from NASA grant NNX12AC75G (Kepler Participating Scientist Program). Funding for the Stellar Astrophysics Centre is provided by The Danish National Research Foundation. The research is supported by the ASTERISK project (ASTERoseismic Investigations with SONG and Kepler) funded by the European Research Council (grant agreement No. 267864). Asteroseismic analysis was supported in part by White Dwarf Research Corporation through the Pale Blue Dot project (http://whitedwarf.org/palebluedot). S.B. acknowledges support from NSF grant AST-1105930. R.L.G. has been partially supported by NASA co-operative agreement NNX09AG09A. NR 107 TC 58 Z9 58 U1 0 U2 18 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAR 20 PY 2013 VL 766 IS 1 AR 40 DI 10.1088/0004-637X/766/1/40 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 105GH UT WOS:000316054000040 ER PT J AU Huang, JS Faber, SM Willmer, CNA Rigopoulou, D Koo, D Newman, J Shu, C Ashby, MLN Barmby, P Coil, A Luo, Z Magdis, G Wang, T Weiner, B Willner, SP Zheng, XZ Fazio, GG AF Huang, J-S Faber, S. M. Willmer, C. N. A. Rigopoulou, D. Koo, D. Newman, J. Shu, C. Ashby, M. L. N. Barmby, P. Coil, A. Luo, Z. Magdis, G. Wang, T. Weiner, B. Willner, S. P. Zheng, X. Z. Fazio, G. G. TI MULTI-WAVELENGTH STUDY OF A COMPLETE IRAC 3.6 mu m SELECTED GALAXY SAMPLE: A FAIR CENSUS OF RED AND BLUE POPULATIONS AT REDSHIFTS 0.4-1.2 SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology: observations; galaxies: distances and redshifts; galaxies: evolution; galaxies: luminosity function, mass function ID STAR-FORMING GALAXIES; EXTENDED GROTH STRIP; BAND LUMINOSITY FUNCTION; LYMAN BREAK GALAXIES; ESTIMATING PHOTOMETRIC REDSHIFTS; SPECTRAL ENERGY-DISTRIBUTIONS; ARTIFICIAL NEURAL-NETWORKS; DARK-MATTER HALOES; DIGITAL SKY SURVEY; DEEP FIELD SOUTH AB We present a multi-wavelength study of a 3.6 mu m selected galaxy sample in the Extended Groth Strip (EGS). The sample is complete for galaxies with stellar mass >10(9.5) M-circle dot and redshift 0.4 < z < 1.2. In this redshift range, the Infrared Array Camera 3.6 mu m band measures the rest-frame near-infrared band, permitting nearly unbiased selection with respect to both quiescent and star-forming galaxies. The numerous spectroscopic redshifts available in the EGS are used to train an artificial neural network to estimate photometric redshifts. The distribution of photometric redshift errors is Gaussian with standard deviation similar to 0.025(1 + z), and the fraction of redshift failures (>3 sigma errors) is about 3.5%. A new method of validation based on pair statistics confirms the estimate of standard deviation even for galaxies lacking spectroscopic redshifts. Basic galaxy properties measured include rest-frame U - B colors, B- and K-band absolute magnitudes, and stellar masses. We divide the sample into quiescent and star-forming galaxies according to their rest-frame U - B colors and 24-3.6 mu m flux density ratios and derive rest K-band luminosity functions and stellar mass functions for quiescent, star-forming, and all galaxies. The results show that massive, quiescent galaxies were in place by z approximate to 1, but lower mass galaxies generally ceased their star formation at later epochs. C1 [Huang, J-S] Chinese Acad Sci, Natl Astron Observ, Beijing 100012, Peoples R China. [Huang, J-S; Ashby, M. L. N.; Wang, T.; Willner, S. P.; Fazio, G. G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Faber, S. M.; Koo, D.] Univ Calif Santa Cruz, Univ Calif Observ, Lick Observ, Santa Cruz, CA 95064 USA. [Willmer, C. N. A.; Weiner, B.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Rigopoulou, D.; Magdis, G.] Univ Oxford, Dept Astrophys, Oxford OX1 3RH, England. [Newman, J.] Univ Pittsburgh, Dept Phys & Astron, Pittsburgh, PA 15260 USA. [Shu, C.; Luo, Z.] Shanghai Normal Univ, Shanghai Key Lab Astrophys, Shanghai 200234, Peoples R China. [Barmby, P.] Univ Western Ontario, Dept Phys & Astron, London, ON N6A 3K7, Canada. [Coil, A.] Univ Calif San Diego, Dept Phys, La Jolla, CA 92093 USA. [Coil, A.] Univ Calif San Diego, Ctr Astrophys & Space Sci, La Jolla, CA 92093 USA. [Wang, T.] Nanjing Univ, Sch Astron & Space Sci, Nanjing 210008, Jiangsu, Peoples R China. [Zheng, X. Z.] Purple Mt Observ, Nanjing, Jiangsu, Peoples R China. RP Huang, JS (reprint author), Chinese Acad Sci, Natl Astron Observ, Beijing 100012, Peoples R China. RI Magdis, Georgios/C-7295-2014; Barmby, Pauline/I-7194-2016 OI Magdis, Georgios/0000-0002-4872-2294; Barmby, Pauline/0000-0003-2767-0090 FU NASA by JPL/Caltech; Chinese National Nature Science foundation [10878003, 10833005] FX 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. Part of the work was done during J.-S. Huang's visit to Shanghai Normal University supported by the Chinese National Nature Science foundation Nos. 10878003 and 10833005. NR 107 TC 10 Z9 10 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 MAR 20 PY 2013 VL 766 IS 1 AR 21 DI 10.1088/0004-637X/766/1/21 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 105GH UT WOS:000316054000021 ER PT J AU McJunkin, M France, K Burgh, EB Herczeg, GJ Schindhelm, E Brown, JM Brown, A AF McJunkin, Matthew France, Kevin Burgh, Eric B. Herczeg, Gregory J. Schindhelm, Eric Brown, Joanna M. Brown, Alexander TI PROBING THE INNER REGIONS OF PROTOPLANETARY DISKS WITH CO ABSORPTION LINE SPECTROSCOPY SO ASTROPHYSICAL JOURNAL LA English DT Article DE protoplanetary disks; stars: individual: (AA Tau, HN Tau, DE Tau, RECX-15, RW Aur, SU Aur) ID T-TAURI STARS; MAIN-SEQUENCE STARS; MOLECULAR-HYDROGEN EMISSION; FAR-ULTRAVIOLET CONTINUUM; ETA-CHAMAELEONTIS CLUSTER; YOUNG CIRCUMSTELLAR DISKS; SPACE-TELESCOPE SURVEY; 4TH POSITIVE EMISSION; H-2 EMISSION; MAGNETOSPHERIC ACCRETION AB Carbon monoxide (CO) is the most commonly used tracer of molecular gas in the inner regions of protoplanetary disks. CO can be used to constrain the excitation and structure of the circumstellar environment. Absorption line spectroscopy provides an accurate assessment of a single line of sight through the protoplanetary disk system, giving more straightforward estimates of column densities and temperatures than CO and molecular hydrogen (H-2) emission line studies. We analyze new observations of ultraviolet CO absorption from the Hubble Space Telescope along the sightlines to six classical T Tauri stars. Gas velocities consistent with the stellar velocities, combined with the moderate-to-high disk inclinations, argue against the absorbing CO gas originating in a fast-moving disk wind. We conclude that the far-ultraviolet observations provide a direct measure of the disk atmosphere or possibly a slow disk wind. The CO absorption lines are reproduced by model spectra with column densities in the range N((CO)-C-12) similar to 10(16)-10(18) cm(-2) and N((CO)-C-13) similar to 10(15)-10(17) cm(-2), rotational temperatures T-rot(CO) similar to 300-700 K, and Doppler b-values, b similar to 0.5-1.5 km s(-1). We use these results to constrain the line-of-sight density of the warm molecular gas (n(CO) similar to 70-4000 cm(-3)) and put these observations in context with protoplanetary disk models. C1 [McJunkin, Matthew; France, Kevin; Burgh, Eric B.; Brown, Alexander] Univ Colorado, Ctr Astrophys & Space Astron, Boulder, CO 80309 USA. [Herczeg, Gregory J.] Peking Univ, Kavli Inst Astron & Astrophys, Beijing 100871, Peoples R China. [Schindhelm, Eric] SW Res Inst, Boulder, CO 80302 USA. [Brown, Joanna M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP McJunkin, M (reprint author), Univ Colorado, Ctr Astrophys & Space Astron, 389 UCB, Boulder, CO 80309 USA. EM matthew.mcjunkin@colorado.edu OI Herczeg, Gregory/0000-0002-7154-6065 FU NASA [NNX08AC146, NAS5-98043]; HST guest observing program [11616] FX We thank M. Eidelsberg for providing the CO oscillator strengths and rovibrational line wavelengths used in this work. This work made use of data from HST guest observing program 11616 and was supported by NASA grants NNX08AC146 and NAS5-98043 to the University of Colorado at Boulder. NR 74 TC 9 Z9 9 U1 0 U2 15 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAR 20 PY 2013 VL 766 IS 1 AR 12 DI 10.1088/0004-637X/766/1/12 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 105GH UT WOS:000316054000012 ER PT J AU Stawarz, L Tanaka, YT Madejski, G O'Sullivan, SP Cheung, CC Feain, IJ Fukazawa, Y Gandhi, P Hardcastle, MJ Kataoka, J Ostrowski, M Reville, B Siemiginowska, A Simionescu, A Takahashi, T Takei, Y Takeuchi, Y Werner, N AF Stawarz, L. Tanaka, Y. T. Madejski, G. O'Sullivan, S. P. Cheung, C. C. Feain, I. J. Fukazawa, Y. Gandhi, P. Hardcastle, M. J. Kataoka, J. Ostrowski, M. Reville, B. Siemiginowska, A. Simionescu, A. Takahashi, T. Takei, Y. Takeuchi, Y. Werner, N. TI GIANT LOBES OF CENTAURUS A RADIO GALAXY OBSERVED WITH THE SUZAKU X-RAY SATELLITE SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: active; galaxies: individual (Centaurus A); galaxies: jets; intergalactic medium; magnetic fields; X-rays: galaxies ID ACTIVE GALACTIC NUCLEI; ENERGY COSMIC-RAYS; DOUBLE-DOUBLE MORPHOLOGY; DEEP FIELD-SOUTH; MAGNETIC-FIELD; PARTICLE-ACCELERATION; CENTER REGION; CLUSTER ENVIRONMENTS; NUMBER COUNTS; FERMI-LAT AB We report on Suzaku observations of selected regions within the southern giant lobe of the radio galaxy Centaurus A. In our analysis we focus on distinct X-ray features detected with the X-ray Imaging Spectrometer within the range 0.5-10 keV, some of which are likely associated with fine structure of the lobe revealed by recent high-quality radio intensity and polarization maps. With the available photon statistics, we find that the spectral properties of the detected X-ray features are equally consistent with thermal emission from hot gas with temperatures kT > 1 keV, or with a power-law radiation continuum characterized by photon indices Gamma similar to 2.0 +/- 0.5. However, the plasma parameters implied by these different models favor a synchrotron origin for the analyzed X-ray spots, indicating that a very efficient acceleration of electrons up to greater than or similar to 10 TeV energies is taking place within the giant structure of Centaurus A, albeit only in isolated and compact regions associated with extended and highly polarized radio filaments. We also present a detailed analysis of the diffuse X-ray emission filling the whole field of view of the instrument, resulting in a tentative detection of a soft excess component best fitted by a thermal model with a temperature of kT similar to 0.5 keV. The exact origin of the observed excess remains uncertain, although energetic considerations point to thermal gas filling the bulk of the volume of the lobe and mixed with the non-thermal plasma, rather than to the alternative scenario involving a condensation of the hot intergalactic medium around the edges of the expanding radio structure. If correct, this would be the first detection of the thermal content of the extended lobes of a radio galaxy in X-rays. The corresponding number density of the thermal gas in such a case is n(g) similar to 10(-4) cm(-3), while its pressure appears to be in almost exact equipartition with the volume-averaged non-thermal pressure provided by the radio-emitting electrons and the lobes' magnetic field. A prominent large-scale fluctuation of the Galactic foreground emission, resulting in excess foreground X-ray emission aligned with the lobe, cannot be ruled out. Although tentative, our findings potentially imply that the structure of the extended lobes in active galaxies is likely to be highly inhomogeneous and non-uniform, with magnetic reconnection and turbulent acceleration processes continuously converting magnetic energy to internal energy of the plasma particles, leading to possibly significant spatial and temporal variations in the plasma beta parameter around the volume-averaged equilibrium condition beta similar to 1. C1 [Stawarz, L.; Gandhi, P.; Takahashi, T.; Takei, Y.] Inst Space & Astronaut Sci JAXA, Chuo Ku, Sagamihara, Kanagawa 2525210, Japan. [Stawarz, L.; Ostrowski, M.] Jagiellonian Univ, Astron Observ, PL-30244 Krakow, Poland. [Tanaka, Y. T.; Fukazawa, Y.] Hiroshima Univ, Dept Phys Sci, Hiroshima 7398526, Japan. [Madejski, G.] Stanford Univ, Dept Phys, Kavli Inst Particle Astrophys & Cosmol, WW Hansen Expt Phys Lab, Stanford, CA 94305 USA. [Madejski, G.] Stanford Univ, SLAC Natl Accelerator Lab, Stanford, CA 94305 USA. [O'Sullivan, S. P.] Univ Sydney, Sch Phys A28, Sydney Inst Astron, Sydney, NSW 2006, Australia. [Cheung, C. C.] Natl Acad Sci, Washington, DC 20001 USA. [Feain, I. J.] CSIRO Astron & Space Sci, ATNF, Epping, NSW 1710, Australia. [Hardcastle, M. J.] Univ Hertfordshire, Sch Phys Astron & Math, Hatfield AL10 9AB, Herts, England. [Kataoka, J.; Takeuchi, Y.] Waseda Univ, Res Inst Sci & Engn, Shinjuku Ku, Tokyo 1698555, Japan. [Reville, B.] Univ Oxford, Clarendon Lab, Oxford OX1 3PU, England. [Siemiginowska, A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Simionescu, A.; Werner, N.] Stanford Univ, KIPAC, Stanford, CA 94305 USA. [Simionescu, A.; Werner, N.] Stanford Univ, Dept Phys, Stanford, CA 94305 USA. RP Stawarz, L (reprint author), Inst Space & Astronaut Sci JAXA, Chuo Ku, 3-1-1 Yoshinodai, Sagamihara, Kanagawa 2525210, Japan. EM stawarz@astro.isas.jaxa.jp RI XRAY, SUZAKU/A-1808-2009; OI Hardcastle, Martin/0000-0003-4223-1117 FU Polish NSC grant [DEC-2012/04/A/ST9/00083]; Australian Research Council [FL100100033]; NASA [DPR S-15633-Y.]; European Research Council under the European Community's Seventh Framework Programme/ERC [247039] FX L.S. and M.O. were supported by Polish NSC grant DEC-2012/04/A/ST9/00083. S.O'S. acknowledges the support of the Australian Research Council through grant FL100100033. Work by C.C.C. at NRL is supported in part by NASA DPR S-15633-Y. B.R. has received funding from the European Research Council under the European Community's Seventh Framework Programme (FP7/2007-2013)/ERC grant agreement no. 247039. NR 95 TC 18 Z9 18 U1 0 U2 8 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAR 20 PY 2013 VL 766 IS 1 AR 48 DI 10.1088/0004-637X/766/1/48 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 105GH UT WOS:000316054000048 ER PT J AU Tremmel, M Fragos, T Lehmer, BD Tzanavaris, P Belczynski, K Kalogera, V Basu-Zych, AR Farr, WM Hornschemeier, A Jenkins, L Ptak, A Zezas, A AF Tremmel, M. Fragos, T. Lehmer, B. D. Tzanavaris, P. Belczynski, K. Kalogera, V. Basu-Zych, A. R. Farr, W. M. Hornschemeier, A. Jenkins, L. Ptak, A. Zezas, A. TI MODELING THE REDSHIFT EVOLUTION OF THE NORMAL GALAXY X-RAY LUMINOSITY FUNCTION SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries: close; galaxies: stellar content; stars: evolution; X-rays: binaries; X-rays: diffuse background; X-rays: galaxies ID DEEP FIELD-SOUTH; STAR-FORMATION HISTORY; BLACK-HOLE BINARIES; ACTIVE GALACTIC NUCLEI; INITIAL MASS FUNCTIONS; SIMILAR-TO 1; FORMING GALAXIES; STELLAR-MASS; HOT GAS; EXPLOSION MECHANISM AB Emission from X-ray binaries (XRBs) is a major component of the total X-ray luminosity of normal galaxies, so X-ray studies of high-redshift galaxies allow us to probe the formation and evolution of XRBs on very long timescales (similar to 10 Gyr). In this paper, we present results from large-scale population synthesis models of binary populations in galaxies from z = 0 to similar to 20. We use as input into our modeling the Millennium II Cosmological Simulation and the updated semi-analytic galaxy catalog by Guo et al. to self-consistently account for the star formation history (SFH) and metallicity evolution of each galaxy. We run a grid of 192 models, varying all the parameters known from previous studies to affect the evolution of XRBs. We use our models and observationally derived prescriptions for hot gas emission to create theoretical galaxy X-ray luminosity functions (XLFs) for several redshift bins. Models with low common envelope efficiencies, a 50% twins mass ratio distribution, a steeper initial mass function exponent, and high stellar wind mass-loss rates best match observational results from Tzanavaris & Georgantopoulos, though they significantly underproduce bright early-type and very bright (L-x > 10(41)) late-type galaxies. These discrepancies are likely caused by uncertainties in hot gas emission and SFHs, active galactic nucleus contamination, and a lack of dynamically formed low-mass XRBs. In our highest likelihood models, we find that hot gas emission dominates the emission for most bright galaxies. We also find that the evolution of the normal galaxy X-ray luminosity density out to z = 4 is driven largely by XRBs in galaxies with X-ray luminosities between 10(40) and 10(41) erg s(-1). C1 [Tremmel, M.] Univ Washington, Dept Astron, Seattle, WA 98195 USA. [Fragos, T.; Zezas, A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Lehmer, B. D.; Tzanavaris, P.] Johns Hopkins Univ, Baltimore, MD 21218 USA. [Lehmer, B. D.; Tzanavaris, P.; Basu-Zych, A. R.; Hornschemeier, A.; Jenkins, L.; Ptak, A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Belczynski, K.] Univ Warsaw, Astron Observ, PL-00478 Warsaw, Poland. [Belczynski, K.] Univ Texas Brownsville, Ctr Gravitat Wave Astron, Brownsville, TX 78520 USA. [Kalogera, V.; Farr, W. M.] Northwestern Univ, Ctr Interdisciplinary Res & Explorat Astrophys, Evanston, IL 60208 USA. [Kalogera, V.; Farr, W. M.] Northwestern Univ, Dept Phys & Astron, Evanston, IL 60208 USA. [Zezas, A.] Univ Crete, Dept Phys, Iraklion 71003, Crete, Greece. [Zezas, A.] Fdn Res & Technol, IESL, Iraklion 71110, Crete, Greece. RP Tremmel, M (reprint author), Univ Washington, Dept Astron, Box 351580, Seattle, WA 98195 USA. EM mjt29@astro.washington.edu RI Zezas, Andreas/C-7543-2011; Fragos, Tassos/A-3581-2016 OI Zezas, Andreas/0000-0001-8952-676X; Fragos, Tassos/0000-0003-1474-1523 FU CfA; ITC; NASA at Goddard Space Flight Center; MSHE [N203 404939]; NASA ADP [NNX12AL39G] FX The authors thank the anonymous referee whose comments and suggestions have helped to improve this paper. T.F. acknowledges support from the CfA and the ITC prize fellowship programs. B.D.L. thanks the Einstein Fellowship program. P.T. acknowledges support through a NASA Post-doctoral Program Fellowship at Goddard Space Flight Center, administered by Oak Ridge Associated Universities through a contract with NASA. Resources supporting this work were provided by the Northwestern University Quest High Performance Computing (HPC) cluster and by the NASA High-End Computing (HEC) Program through the NASA Center for Climate Simulation (NCCS) at Goddard Space Flight Center. K.B. acknowledges support from MSHE grant N203 404939. V.K. acknowledges support for this work from NASA ADP grant NNX12AL39G (sub-contract to Northwestern University) NR 77 TC 12 Z9 12 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 MAR 20 PY 2013 VL 766 IS 1 AR 19 DI 10.1088/0004-637X/766/1/19 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 105GH UT WOS:000316054000019 ER PT J AU Woodman, N AF Woodman, Neal TI The identity of the enigmatic "Black Shrew" (Sorex niger Ord, 1815) SO PROCEEDINGS OF THE BIOLOGICAL SOCIETY OF WASHINGTON LA English DT Article DE Eulipotyphla; Guthrie's Geography; nomenclature; Soricidae; Soricomorpha; Suncus montanus; taxonomy; Zoology of North America AB The scientific name Sorex niger Ord, 1815 (Mammalia, Soricidae) was originally applied to a North American species that George Ord called the "Black Shrew." The origin of the name "Black Shrew," however, was obscure, and Samuel Rhoads subsequently wrote that the species represented by this name could not be determined The names Sorex niger Ord and Black, Shrew have since been mostly forgotten. Two of Ord's contemporaries, however, noted that Ord's use of these names probably alluded to Benjamin Smith Barton's Black Shrew, whose discovery near Philadelphia was announced by Barton in 1806. Examination of two unpublished illustrations of the Black Shrew made by Barton indicates that the animal depicted is Blarina brevicauda (Say, 1822). Had the connection between Ord's and Barton's names been made more clearly, one of the most common mammals in eastern North America would bear a different scientific name today. This connection also would have affected the validity of Sorex niger Horsfield, 1851. While Sorex niger Ord remains a nomen nudum, the animal it referenced can now be identified. C1 US Geol Survey, Patuxent Wildlife Res Ctr, Natl Museum Nat Hist, Smithsonian Inst, Washington, DC 20013 USA. RP Woodman, N (reprint author), US Geol Survey, Patuxent Wildlife Res Ctr, Natl Museum Nat Hist, Smithsonian Inst, Washington, DC 20013 USA. EM woodmann@si.edu RI sebastianovitsch, stepan/G-8507-2013 NR 40 TC 1 Z9 1 U1 0 U2 6 PU BIOL SOC WASHINGTON PI WASHINGTON PA NAT MUSEUM NAT HIST SMITHSONIAN INST, WASHINGTON, DC 20560 USA SN 0006-324X J9 P BIOL SOC WASH JI Proc. Biol. Soc. Wash. PD MAR 19 PY 2013 VL 126 IS 1 BP 1 EP 10 PG 10 WC Biology SC Life Sciences & Biomedicine - Other Topics GA 114AX UT WOS:000316713400001 ER PT J AU Olson, SL AF Olson, Storrs L. TI Fossil woodpeckers from Bermuda with the description of a new species of Colaptes (Ayes: Picidae) SO PROCEEDINGS OF THE BIOLOGICAL SOCIETY OF WASHINGTON LA English DT Article DE Aegolius; flicker; fossil birds; Holocene; owls; Pleistocene; Sphyrapicus varius; Strigidae; Yellow-bellied Sapsucker ID QUATERNARY DEPOSITS; AVES; GENUS AB Fossils of woodpeckers (Picidae) occur on Bermuda in late Pleistocene and Holocene deposits. Most of these are from a flicker (Colaptes), presumably. derived from the North American Colaptes auratus that was smaller than all mainland forms of that species. The Bermuda flicker was larger than C. a: gundlachi of Grand Cayman and is named as a new species Colaptes oceanicus, that probably persisted into the colonial period (1600s). Three fossils are referred to the migratory Yellow-bellied Sapsucker (Sphyrapicus varius), which winters in small numbers on Bermuda. One distal end of a tarsometatarsus of a woodpecker appears to differ from either of the previous species, but its identity was not further determined. Colaptes oceanicus would probably have excavated nest holes in the resident palm trees (Sabal bermudana) and in rotten limbs and stumps of hardwoods. These excavations would have been crucial for the evolution of the small owl Aegolius gradyi and probably provided shelter for other Bermuda organisms as well. C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Div Birds,NHB MRC 116, Washington, DC 20013 USA. RP Olson, SL (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Div Birds,NHB MRC 116, POB 37012, Washington, DC 20013 USA. EM olsons@si.edu NR 19 TC 0 Z9 0 U1 1 U2 4 PU BIOL SOC WASHINGTON PI WASHINGTON PA NAT MUSEUM NAT HIST SMITHSONIAN INST, WASHINGTON, DC 20560 USA SN 0006-324X J9 P BIOL SOC WASH JI Proc. Biol. Soc. Wash. PD MAR 19 PY 2013 VL 126 IS 1 BP 17 EP 24 PG 8 WC Biology SC Life Sciences & Biomedicine - Other Topics GA 114AX UT WOS:000316713400003 ER PT J AU Petit, RE Harasewych, MG AF Petit, Richard E. Harasewych, M. G. TI Rediscovery of Cancellaria corrosa Reeve, 1856 (Gastropoda: Cancellariidae) in the tropical eastern Pacific SO PROCEEDINGS OF THE BIOLOGICAL SOCIETY OF WASHINGTON LA English DT Article DE Cancellaria acalypta; Cancellaria corrosa; Cancellaria decussata; Cancellaria gemmulata; eastern Pacific; neogastropod taxonomy AB Cancellaria corrosa Reeve, 1856, a species described from an unknown locality and believed by early authors to inhabit "China Seas," has been found to be a component of the sublittoral fauna of western Central America. A more detailed description of the shell and radula of this species is provided. As specimens have been misidentified in collections as C. decussata Sowerby I, 1832 or C. gemmulata Sowerby I, 1832, features useful to distinguish these species are provided. Examination of the fossil literature for the region indicates that the lineage giving rise to C. corrosa has been present since at least the middle Miocene. C1 [Harasewych, M. G.] Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, Washington, DC 20013 USA. RP Petit, RE (reprint author), 806 St Charles Rd, North Myrtle Beach, SC 29582 USA. EM r.e.petit@att.net; Harasewych@si.edu NR 17 TC 1 Z9 1 U1 0 U2 0 PU BIOL SOC WASHINGTON PI WASHINGTON PA NAT MUSEUM NAT HIST SMITHSONIAN INST, WASHINGTON, DC 20560 USA SN 0006-324X EI 1943-6327 J9 P BIOL SOC WASH JI Proc. Biol. Soc. Wash. PD MAR 19 PY 2013 VL 126 IS 1 BP 83 EP 89 PG 7 WC Biology SC Life Sciences & Biomedicine - Other Topics GA 114AX UT WOS:000316713400007 ER PT J AU Kharol, SK Martin, RV Philip, S Vogel, S Henze, DK Chen, D Wang, Y Zhang, Q Heald, CL AF Kharol, S. K. Martin, R. V. Philip, S. Vogel, S. Henze, D. K. Chen, D. Wang, Y. Zhang, Q. Heald, C. L. TI Persistent sensitivity of Asian aerosol to emissions of nitrogen oxides SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article DE PM2; 5; NOx; SO2; NH3; GEOS-Chem ID UNITED-STATES; GEOS-CHEM; SATELLITE-OBSERVATIONS; ATMOSPHERIC AMMONIA; PARTICULATE MATTER; CHINA; AIR; INVENTORY; POLLUTION; STRATEGY AB We use a chemical transport model and its adjoint to examine the sensitivity of secondary inorganic aerosol formation to emissions of precursor trace gases from Asia. Sensitivity simulations indicate that secondary inorganic aerosol mass concentrations are most sensitive to ammonia (NH3) emissions in winter and to sulfur dioxide (SO2) emissions during the rest of the year. However, in the annual mean, the perturbations on Asian population-weighted ground-level secondary inorganic aerosol concentrations of 34% due to changing nitrogen oxide (NOx) emissions are comparable to those from changing either SO2 (41%) or NH3 (25%) emissions. The persistent sensitivity to NOx arises from the regional abundance of NH3 over Asia that promotes ammonium nitrate formation. IASI satellite observations corroborate the NH3 abundance. Projected emissions for 2020 indicate continued sensitivity to NOx emissions. We encourage more attention to NOx controls in addition to SO2 and NH3 controls to reduce ground-level East Asian aerosol. Citation: Kharol, S. K., R. V. Martin, S. Philip, S. Vogel, D. K. Henze, D. Chen, Y. Wang, Q. Zhang, and C. L. Heald (2013), Persistent sensitivity of Asian aerosol to emissions of nitrogen oxides, Geophys. Res. Lett., 40, 1021-1026, doi:10.1002/grl.50234. C1 [Kharol, S. K.; Martin, R. V.; Philip, S.] Dalhousie Univ, Dept Phys & Atmospher Sci, Halifax, NS B3H 3J5, Canada. [Martin, R. V.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Vogel, S.; Henze, D. K.] Univ Colorado, Dept Mech Engn, Boulder, CO 80309 USA. [Chen, D.] Univ Calif Los Angeles, Dept Atmospher & Ocean Sci, Los Angeles, CA USA. [Wang, Y.; Zhang, Q.] Tsinghua Univ, Key Lab Earth Syst Modeling, Minist Educ, Ctr Earth Syst Sci, Beijing 100084, Peoples R China. [Heald, C. L.] MIT, Dept Civil & Environm Engn, Cambridge, MA 02139 USA. [Heald, C. L.] MIT, Dept Earth Atmospher & Planetary Sci, Cambridge, MA USA. RP Kharol, SK (reprint author), Dalhousie Univ, Dept Phys & Atmospher Sci, Halifax, NS B3H 3J5, Canada. EM shaileshan2000@yahoo.co.in RI Heald, Colette/A-6813-2011; Martin, Randall/C-1205-2014; Chem, GEOS/C-5595-2014; Wang, Yuxuan/C-6902-2014; Zhang, Qiang/D-9034-2012; Chen, Dan/R-4486-2016 OI Martin, Randall/0000-0003-2632-8402; Wang, Yuxuan/0000-0002-1649-6974; FU NSERC; NOAA; NASA; U.S. EPA FX This work was supported by NSERC. IASI NH3 data were provided by L. Clarisse, D. Hurtmans, C. Clerbaux, and P.-F. Coheur (ULB-LATMOS). C.L.H. acknowledges support from NOAA. D.K.H. recognizes support from NASA and the U.S. EPA. NR 33 TC 18 Z9 18 U1 3 U2 42 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 EI 1944-8007 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD MAR 16 PY 2013 VL 40 IS 5 BP 1021 EP 1026 DI 10.1002/grl.50234 PG 6 WC Geosciences, Multidisciplinary SC Geology GA 134VG UT WOS:000318242900041 ER PT J AU Lee, RKL Owen, RB Renaut, RW Behrensmeyer, AK Potts, R Sharp, WD AF Lee, Ray K. L. Owen, R. Bernhart Renaut, Robin W. Behrensmeyer, Anna K. Potts, Richard Sharp, Warren D. TI Facies, geochemistry and diatoms of late Pleistocene Olorgesailie tufas, southern Kenya Rift SO PALAEOGEOGRAPHY PALAEOCLIMATOLOGY PALAEOECOLOGY LA English DT Article DE Pleistocene; Tufa; Diatoms; Geochemistry; Sedimentology; Olorgesailie ID EAST-AFRICAN CLIMATE; FRESH-WATER WETLAND; NORTHERN KENYA; ENVIRONMENTAL-CHANGE; SPRING DEPOSITS; STABLE-ISOTOPES; CALCAREOUS TUFA; HUMAN-EVOLUTION; OLDUVAI GORGE; CENTRAL SPAIN AB This research reconstructs paleoenvironments of late Pleistocene tufas at Olorgesailie in the southern Kenya Rift and examines the relationship between climate, tectonism and tufa precipitation. The deposits crop out at three main sites, forming at 290 kyr and at least twice between 220 and 12 kyr ago. Ten carbonate facies comprise the bulk of the tufas, which accumulated at spring vents, in swamps and shallow lakes, along fissures, and along fluvial channels. The tufas contain diatoms dominated by shallow-water, swamp and fluvial taxa associated with fresh to mildly saline conditions. delta C-13 isotopes are relatively enriched (0.25 to 1.96 parts per thousand) compared with other East African tufas, but uniform within each set of tufa deposits, suggesting similar sources of CO2 derived from similar plants and soil organic matter during each interval of deposition. 8130 ranges from -7.17 parts per thousand to +5.16 parts per thousand suggesting variable evaporation and rainfall/groundwater sources or changing water temperatures. Variable REE patterns suggest spatial and/or temporal contrasts in groundwater chemistry. The former springs may have developed in response to climate changes, but there are no clear correlations with known East African wet phases. The deposition of tufa probably also relates to basin breakup and faulting, which likely influenced groundwater movements. Increased permineralized silica in plants in tufas and non-carbonate sediments reflects the introduction of deeper groundwaters than those during earlier Olorgesailie Formation times. Whether climatically or tectonically controlled, the tufa spring sites would have provided a supply of potable water, at least intermittently, during the Pleistocene, and would have provided attractive places for wildlife and possibly for Middle Stone Age human inhabitants of the region, especially during relatively dry times. (C) 2013 Elsevier B.V. All rights reserved. C1 [Lee, Ray K. L.; Owen, R. Bernhart] Hong Kong Baptist Univ, Dept Geog, Kowloon Tong, Hong Kong, Peoples R China. [Renaut, Robin W.] Univ Saskatchewan, Dept Geol Sci, Saskatoon, SK S7N 5E2, Canada. [Behrensmeyer, Anna K.] Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20013 USA. [Potts, Richard] Smithsonian Inst, Natl Museum Nat Hist, Human Origins Program, Washington, DC 20013 USA. [Potts, Richard] Natl Museums Kenya, Dept Earth Sci, Palaeontol Sect, Nairobi, Kenya. [Sharp, Warren D.] Berkeley Geochronol Ctr, Berkeley, CA 94709 USA. RP Owen, RB (reprint author), Hong Kong Baptist Univ, Dept Geog, Kowloon Tong, Hong Kong, Peoples R China. EM owen@hkbu.edu.hk OI Owen, Richard Bernhart/0000-0001-5267-5366 FU Research Grant Council of Hong Kong [201911]; NSERC (Canada) [629-08]; National Science Foundation (HOMINID grant) [BCS-0218511]; National Science Foundation [BCS-0302157]; Smithsonian Human Origins Program; Peter Buck Fund for Human Origins Research FX The authors would like to thank the National Museums of Kenya. The research was undertaken under permits from the Ministry of Science and Technology, Republic of Kenya. Funding for Lee and Owen was provided by the Research Grant Council of Hong Kong (grant 201911). Renaut was supported by NSERC (Canada) Discovery Grant 629-08. Behrensmeyer, Potts and Sharp were supported by the National Science Foundation (HOMINID grant BCS-0218511 to RP; grant BCS-0302157 to WS), the Smithsonian Human Origins Program, and the Peter Buck Fund for Human Origins Research. We thank Concha Arenas and Elizabeth Turner for their very helpful reviews of the original manuscript. NR 110 TC 7 Z9 7 U1 1 U2 22 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0031-0182 EI 1872-616X J9 PALAEOGEOGR PALAEOCL JI Paleogeogr. Paleoclimatol. Paleoecol. PD MAR 15 PY 2013 VL 374 BP 197 EP 217 DI 10.1016/j.palaeo.2013.01.019 PG 21 WC Geography, Physical; Geosciences, Multidisciplinary; Paleontology SC Physical Geography; Geology; Paleontology GA 122MR UT WOS:000317322700017 ER PT J AU Dumas, P Jimenez, H Peignon, C Wantiez, L Adjeroud, M AF Dumas, Pascal Jimenez, Haizea Peignon, Christophe Wantiez, Laurent Adjeroud, Mehdi TI Small-Scale Habitat Structure Modulates the Effects of No-Take Marine Reserves for Coral Reef Macroinvertebrates SO PLOS ONE LA English DT Article ID NEW-CALEDONIA; FRENCH-POLYNESIA; SPATIAL-PATTERNS; FISH COMMUNITIES; PROTECTED AREAS; SOUTH-PACIFIC; FISHERIES; BIODIVERSITY; AUSTRALIA; SUSTAINABILITY AB No-take marine reserves are one of the oldest and most versatile tools used across the Pacific for the conservation of reef resources, in particular for invertebrates traditionally targeted by local fishers. Assessing their actual efficiency is still a challenge in complex ecosystems such as coral reefs, where reserve effects are likely to be obscured by high levels of environmental variability. The goal of this study was to investigate the potential interference of small-scale habitat structure on the efficiency of reserves. The spatial distribution of widely harvested macroinvertebrates was surveyed in a large set of protected vs. unprotected stations from eleven reefs located in New Caledonia. Abundance, density and individual size data were collected along random, small-scale (20 x 1 m) transects. Fine habitat typology was derived with a quantitative photographic method using 17 local habitat variables. Marine reserves substantially augmented the local density, size structure and biomass of the target species. Density of Trochus niloticus and Tridacna maxima doubled globally inside the reserve network; average size was greater by 10 to 20% for T. niloticus. We demonstrated that the apparent success of protection could be obscured by marked variations in population structure occurring over short distances, resulting from small-scale heterogeneity in the reef habitat. The efficiency of reserves appeared to be modulated by the availability of suitable habitats at the decimetric scale ("microhabitats") for the considered sessile/low-mobile macroinvertebrate species. Incorporating microhabitat distribution could significantly enhance the efficiency of habitat surrogacy, a valuable approach in the case of conservation targets focusing on endangered or emblematic macroinvertebrate or relatively sedentary fish species C1 [Dumas, Pascal] IRD, UR CoReUs 2 227, Fisheries Dept Vanuatu, Port Vila, Vanuatu. [Jimenez, Haizea; Peignon, Christophe; Adjeroud, Mehdi] IRD, UR CoReUs 2 227, Noumea, New Caledonia. [Jimenez, Haizea] Smithsonian Environm Res Ctr, Marine Invas Res Lab, Tiburon, CA USA. [Wantiez, Laurent] Univ Nouvelle Caledonie, LIVE, Noumea, New Caledonia. RP Dumas, P (reprint author), IRD, UR CoReUs 2 227, Fisheries Dept Vanuatu, Port Vila, Vanuatu. EM pascal-paul.dumas@ird.fr RI Wantiez, Laurent/L-3343-2013; Adjeroud, Mehdi/J-6411-2016; OI Wantiez, Laurent/0000-0001-5024-2057; Adjeroud, Mehdi/0000-0002-6825-8759; Dumas, Pascal/0000-0001-7369-8989 FU french PAMPA-LITEAU III programme; IRD (Institut de Recherche pour le developpement) FX This study was funded by french PAMPA-LITEAU III programme (http://www.ifremer.fr/pampa) and IRD (Institut de Recherche pour le developpement). The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 66 TC 2 Z9 2 U1 2 U2 46 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 MAR 15 PY 2013 VL 8 IS 3 AR e58998 DI 10.1371/journal.pone.0058998 PG 9 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 109ZC UT WOS:000316409800051 PM 23554965 ER PT J AU Feist, J Reid, MTH Kling, MF AF Feist, Johannes Reid, M. T. Homer Kling, Matthias F. TI Nanoplasmonic near-field synthesis SO PHYSICAL REVIEW A LA English DT Article ID HIGH-HARMONIC-GENERATION; CYCLE LASER FIELDS; ELECTRON LOCALIZATION; ATTOSECOND PHYSICS; NONLINEAR OPTICS; PULSES; POLARIZATION; ENHANCEMENT; EMISSION AB The temporal response of resonances in nanoplasmonic structures typically converts an incoming few-cycle field into a much longer near-field at the spot where nonlinear physical phenomena including electron emission, recollision, and high-harmonic generation can take place. We show that for practically useful structures pulse shaping of the incoming pulse can be used to synthesize the plasmon-enhanced field and enable single-cycle-driven nonlinear physical phenomena. Our method is demonstrated for the generation of an isolated attosecond pulse by plasmon-enhanced high harmonic generation. We furthermore show that optimal control techniques can be used even if the response of the plasmonic structure is not known a priori. DOI: 10.1103/PhysRevA.87.033816 C1 [Feist, Johannes] Harvard Smithsonian Ctr Astrophys, ITAMP, Cambridge, MA 02138 USA. [Feist, Johannes] Univ Autonoma Madrid, Dept Fis Teor Mat Condensada, E-28049 Madrid, Spain. [Reid, M. T. Homer] MIT, Dept Math, Cambridge, MA 02139 USA. [Kling, Matthias F.] Max Planck Inst Quantum Opt, D-85748 Garching, Germany. [Kling, Matthias F.] Kansas State Univ, JR Macdonald Lab, Manhattan, KS 66506 USA. RP Feist, J (reprint author), Harvard Smithsonian Ctr Astrophys, ITAMP, 60 Garden St, Cambridge, MA 02138 USA. EM johannes.feist@uam.es RI Kling, Matthias/D-3742-2014; Feist, Johannes/J-7394-2012; OI Feist, Johannes/0000-0002-7972-0646; Kling, Matthias/0000-0002-1710-0775 FU NSF; European Research Council [290981]; U.S. Department of Energy [DE-SC0008146, DE-FG02-86ER13491]; BMBF via PhoNa; DFG [Kl-1439/4, Kl-1439/5]; Cluster of Excellence: Munich Center for Advanced Photonics (MAP); Defense Advanced Research Projects Agency (DARPA) [N66001-09-1-2070-DOD]; AFOSR Multidisciplinary Research Program of the University Research Initiative (MURI) for Complex and Robust On-chip Nanophotonics [FA9550-09-1-0704] FX J.F. is grateful for support by the NSF through a grant to ITAMP and by the European Research Council under Grant No. 290981 (PLASMONANOQUANTA). M.F.K. is grateful for support by the U.S. Department of Energy under DE-SC0008146 and DE-FG02-86ER13491, the BMBF via PhoNa, and the DFG via Kl-1439/4, and Kl-1439/5, and the Cluster of Excellence: Munich Center for Advanced Photonics (MAP). M.T.H.R. is grateful for support by the Defense Advanced Research Projects Agency (DARPA) under grant N66001-09-1-2070-DOD and by the AFOSR Multidisciplinary Research Program of the University Research Initiative (MURI) for Complex and Robust On-chip Nanophotonics under grant FA9550-09-1-0704. NR 48 TC 5 Z9 5 U1 0 U2 38 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 MAR 15 PY 2013 VL 87 IS 3 AR 033816 DI 10.1103/PhysRevA.87.033816 PG 6 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA 108TG UT WOS:000316318500006 ER PT J AU Blanco, J Konstantinov, A AF Blanco, Javier Konstantinov, Alexander TI Review of the New World species of the genus Argopistes Motschulsky (Coleoptera: Chrysomelidae: Galerucinae: Alticini) SO ZOOTAXA LA English DT Review DE Flea beetles; new species; USA; Caribbean AB The New World species of the genus Argopistes Motschulsky, 1860 are reviewed, illustrated and a key for their identification is provided. Two new species are described: A. turnbowi (Bahamas Islands) and A. woodleyi (Dominican Republic). The lectotype of A. scyrtoides LeConte is designated. C1 [Blanco, Javier] Natl Museum Nat Hist, Smithsonian Inst, Dept Entomol, Washington, DC 20013 USA. [Konstantinov, Alexander] Natl Museum Nat Hist, Smithsonian Inst, USDA, Systemat Entomol Lab,ARS, Washington, DC 20013 USA. RP Blanco, J (reprint author), Natl Museum Nat Hist, Smithsonian Inst, Dept Entomol, POB 37012, Washington, DC 20013 USA. EM Javier.Blanco@uspto.gov; alex.konstantinov@ars.usda.gov NR 9 TC 1 Z9 1 U1 0 U2 5 PU MAGNOLIA PRESS PI AUCKLAND PA PO BOX 41383, AUCKLAND, ST LUKES 1030, NEW ZEALAND SN 1175-5326 J9 ZOOTAXA JI Zootaxa PD MAR 13 PY 2013 VL 3626 IS 2 BP 249 EP 267 PG 19 WC Zoology SC Zoology GA 104GU UT WOS:000315980700003 PM 26176135 ER PT J AU Regier, JC Mitter, C Zwick, A Bazinet, AL Cummings, MP Kawahara, AY Sohn, JC Zwickl, DJ Cho, S Davis, DR Baixeras, J Brown, J Parr, C Weller, S Lees, DC Mitter, KT AF Regier, Jerome C. Mitter, Charles Zwick, Andreas Bazinet, Adam L. Cummings, Michael P. Kawahara, Akito Y. Sohn, Jae-Cheon Zwickl, Derrick J. Cho, Soowon Davis, Donald R. Baixeras, Joaquin Brown, John Parr, Cynthia Weller, Susan Lees, David C. Mitter, Kim T. TI A Large-Scale, Higher-Level, Molecular Phylogenetic Study of the Insect Order Lepidoptera (Moths and Butterflies) SO PLOS ONE LA English DT Article ID CODING NUCLEAR GENES; EVOLUTION; CLASSIFICATION; BOOTSTRAP; GLOSSATA; LIFE; TREE; HOMOLOGIES; SUPPORT AB Background: Higher-level relationships within the Lepidoptera, and particularly within the species-rich subclade Ditrysia, are generally not well understood, although recent studies have yielded progress. We present the most comprehensive molecular analysis of lepidopteran phylogeny to date, focusing on relationships among superfamilies. Methodology / Principal Findings: 483 taxa spanning 115 of 124 families were sampled for 19 protein-coding nuclear genes, from which maximum likelihood tree estimates and bootstrap percentages were obtained using GARLI. Assessment of heuristic search effectiveness showed that better trees and higher bootstrap percentages probably remain to be discovered even after 1000 or more search replicates, but further search proved impractical even with grid computing. Other analyses explored the effects of sampling nonsynonymous change only versus partitioned and unpartitioned total nucleotide change; deletion of rogue taxa; and compositional heterogeneity. Relationships among the non-ditrysian lineages previously inferred from morphology were largely confirmed, plus some new ones, with strong support. Robust support was also found for divergences among non-apoditrysian lineages of Ditrysia, but only rarely so within Apoditrysia. Paraphyly for Tineoidea is strongly supported by analysis of nonsynonymous-only signal; conflicting, strong support for tineoid monophyly when synonymous signal was added back is shown to result from compositional heterogeneity. Conclusions / Significance: Support for among-superfamily relationships outside the Apoditrysia is now generally strong. Comparable support is mostly lacking within Apoditrysia, but dramatically increased bootstrap percentages for some nodes after rogue taxon removal, and concordance with other evidence, strongly suggest that our picture of apoditrysian phylogeny is approximately correct. This study highlights the challenge of finding optimal topologies when analyzing hundreds of taxa. It also shows that some nodes get strong support only when analysis is restricted to nonsynonymous change, while total change is necessary for strong support of others. Thus, multiple types of analyses will be necessary to fully resolve lepidopteran phylogeny. C1 [Regier, Jerome C.] Univ Maryland, Inst Biosci & Biotechnol Res, College Pk, MD 20742 USA. [Regier, Jerome C.; Mitter, Charles; Sohn, Jae-Cheon; Mitter, Kim T.] Univ Maryland, Dept Entomol, College Pk, MD 20742 USA. [Zwick, Andreas] State Museum Nat Hist, Stuttgart, Germany. [Bazinet, Adam L.; Cummings, Michael P.] Univ Maryland, Lab Mol Evolut, Ctr Bioinformat & Computat Biol, College Pk, MD 20742 USA. [Kawahara, Akito Y.] Univ Florida, Florida Museum Nat Hist, Gainesville, FL 32611 USA. [Zwickl, Derrick J.] Univ Arizona, Dept Ecol & Evolutionary Biol, Tucson, AZ USA. [Cho, Soowon] Chungbuk Natl Univ, Dept Plant Med, Chonju, South Korea. [Davis, Donald R.] Smithsonian Inst, Dept Entomol, Washington, DC 20560 USA. [Baixeras, Joaquin] Univ Valencia, Cavanilles Inst Biodivers & Evolutionary Biol, Valencia, Spain. [Brown, John] ARS, Systemat Entomol Lab, USDA, Beltsville, MD USA. [Parr, Cynthia] Smithsonian Inst, Encyclopedia Life, Washington, DC 20560 USA. [Weller, Susan] Univ Minnesota, Dept Entomol, St Paul, MN USA. [Lees, David C.] Nat Hist Museum, Dept Life Sci, London SW7 5BD, England. RP Regier, JC (reprint author), Univ Maryland, Inst Biosci & Biotechnol Res, College Pk, MD 20742 USA. EM regier@umd.edu; cmitter@umd.edu RI Yakovlev, Roman/J-7243-2013; Baixeras, Joaquin/L-1734-2014; Zwick, Andreas/A-5735-2015 OI Baixeras, Joaquin/0000-0002-6092-0496; FU U. S. National Science Foundation's Assembling the Tree of Life program [1042845, 0531626, 0531769] FX Financial support was provided by the U. S. National Science Foundation's Assembling the Tree of Life program, award numbers 1042845, 0531626, and 0531769. The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 67 TC 93 Z9 97 U1 6 U2 114 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 MAR 12 PY 2013 VL 8 IS 3 AR e58568 DI 10.1371/journal.pone.0058568 PG 23 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 107WV UT WOS:000316252500031 PM 23554903 ER PT J AU Weisrock, DW Macey, JR Matsui, M Mulcahy, DG Papenfuss, TJ AF Weisrock, David W. Macey, J. Robert Matsui, Masafumi Mulcahy, Daniel G. Papenfuss, Theodore J. TI Molecular phylogenetic reconstruction of the endemic Asian salamander family Hynobiidae (Amphibia, Caudata) SO ZOOTAXA LA English DT Article ID RIBOSOMAL-RNA GENES; MITOCHONDRIAL GENOME; TOKYOENSIS AMPHIBIA; ALLOZYMIC VARIATION; JAPAN AMPHIBIA; EVOLUTION; INFERENCE; SEQUENCE; URODELA; DNA AB The salamander family Hynobiidae contains over 50 species and has been the subject of a number of molecular phylogenetic investigations aimed at reconstructing branches across the entire family. In general, studies using the greatest amount of sequence data have used reduced taxon sampling, while the study with the greatest taxon sampling has used a limited sequence data set. Here, we provide insights into the phylogenetic history of the Hynobiidae using both dense taxon sampling and a large mitochondrial DNA sequence data set. We report exclusive new mitochondrial DNA data of 2566 aligned bases (with 151 excluded sites, of included sites 1157 are variable with 957 parsimony informative). This is sampled from two genic regions encoding a 12S-16S region (the 3' end of 12S rRNA, tRNA(VAl), and the 5' end of 16S rRNA), and a ND2-COI region (ND2, tRNA(Trp), tRNA(Ala), tRNA(Asn), the origin for light strand replication-O-L, tRNA(Cys), tRNA(Tyr), and the 5' end of COI). Analyses using parsimony, Bayesian, and maximum likelihood optimality criteria produce similar phylogenetic trees, with discordant branches generally receiving low levels of branch support. Monophyly of the Hynobiidae is strongly supported across all analyses, as is the sister relationship and deep divergence between the genus Onychodactylus with all remaining hynobiids. Within this latter grouping our phylogenetic results identify six clades that are relatively divergent from one another, but for which there is minimal support for their phylogenetic placement. This includes the genus Batrachuperus, the genus Hynobius, the genus Pachyhynobius, the genus Salamandrella, a clade containing the genera Ranodon and Paradactylodon, and a clade containing the genera Liua and Pseudohynobius. This latter clade receives low bootstrap support in the parsimony analysis, but is consistent across all three analytical methods. Our results also clarify a number of well-supported relationships within the larger Batrachuperus and Hynobius clades. While the relationships identified in this study do much to clarify the phylogenetic history of the Hynobiidae, the poor resolution among major hynobiid clades, and the contrast of mtDNA-derived relationships with recent phylogenetic results from a small number of nuclear genes, highlights the need for continued phylogenetic study with larger numbers of nuclear loci. C1 [Weisrock, David W.] Univ Kentucky, Dept Biol, Lexington, KY 40506 USA. [Macey, J. Robert] Merritt Coll, Dept Biol, Oakland, CA 94619 USA. [Macey, J. Robert; Papenfuss, Theodore J.] Univ Calif Berkeley, Museum Vertebrate Zool, Berkeley, CA 94720 USA. [Matsui, Masafumi] Kyoto Univ, Grad Sch Human & Environm Studies, Kyoto 6068501, Japan. [Mulcahy, Daniel G.] Natl Museum Nat Hist, Smithsonian Inst, Suitland, MD 20746 USA. RP Weisrock, DW (reprint author), Univ Kentucky, Dept Biol, 101 Thomas Hunt Morgan Bldg, Lexington, KY 40506 USA. EM dweis2@uky.edu RI Weisrock, David/G-3587-2015 FU National Science Foundation [BSR-9106898, DEB-9318642, DEB-9726064]; National Geographic Society [4110-89, 4872-93] FX We thank Zhili Fang, Tatjana N. Dujsebayeva, Natalia B. Ananjeva, H. G. Kami, and Kh. Monkhbayar for field assistance, and Eric Routman for providing the Cryptobranchus sample We thank the National Science Foundation (BSR-9106898 to Allan Larson; DEB-9318642 to Jonathan B. Losos, Kevin de Queiroz, and Allan Larson; DEB-9726064 to Allan Larson, J. R. Macey, and T. J. Papenfuss) and the National Geographic Society (4110-89 and 4872-93 to T. J. Papenfuss and J. R. Macey) for financial support. We thank Kraig Adler for facilitating contacts among scientists. We most of all thank Allan Larson for guidance, as this project was dear, and now complete - we dedicate this paper to Allan Larson who has long been on the breaking edge of salamander Genetics that is now known as Genomics. NR 61 TC 7 Z9 7 U1 3 U2 18 PU MAGNOLIA PRESS PI AUCKLAND PA PO BOX 41383, AUCKLAND, ST LUKES 1030, NEW ZEALAND SN 1175-5326 EI 1175-5334 J9 ZOOTAXA JI Zootaxa PD MAR 12 PY 2013 VL 3626 IS 1 BP 77 EP 93 PG 17 WC Zoology SC Zoology GA 104GQ UT WOS:000315980300003 PM 26176127 ER PT J AU Grishin, NV Burns, JM Janzen, DH Hallwachs, W Hajibabaei, M AF Grishin, Nick V. Burns, John M. Janzen, Daniel H. Hallwachs, Winnie Hajibabaei, Mehrdad TI OXYNETRA: FACIES AND DNA BARCODES POINT TO A NEW SPECIES FROM COSTA RICA (HESPERIIDAE: PYRGINAE: PYRRHOPYGINI) SO JOURNAL OF THE LEPIDOPTERISTS SOCIETY LA English DT Article DE cryptic species; sexual dimorphism; genitalia (male and female); mimicry; Prunus annularis ID SKIPPER BUTTERFLIES AB Oxynetra stangelandi Grishin & Burns, new species, from high elevations of Area de Conservacion Guanacaste (ACG) in northwestern Costa Rica, is most similar to Oxynetra hopfferi Staudinger, known from mountains of central and southern Costa Rica and western Panama. These hesperiid species differ mainly in body color pattern and in DNA barcodes. We compare their barcodes, nucleotide by nucleotide, together with barcodes of a congener and a species of the related genus Olafia, and use the barcode data to show phylogenetic relationships. We describe the new species, its discovery, its male and female genitalia, and its life history as a cloud forest herbivore of Prunus annularis (Rosaceae). In ACG, no other skippers feed on this plant species, and no other skippers of the tribe Pyrrhopygini feed on plants in the family Rosaceae. Various stages of O. stangelandi belong to mimicry complexes. Although our adults, which are reared from wild-caught caterpillars, are split between the sexes (4 males, 6 females), there are scarcely any females of Oxynetra in the world's museums. C1 [Grishin, Nick V.] Univ Texas Southwestern, Howard Hughes Med Inst, Dallas, TX 75390 USA. [Grishin, Nick V.] Univ Texas Southwestern, Dept Biophys, Dallas, TX 75390 USA. [Grishin, Nick V.] Univ Texas Southwestern, Dept Biochem, Dallas, TX 75390 USA. [Burns, John M.] Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol, Washington, DC 20013 USA. [Janzen, Daniel H.; Hallwachs, Winnie] Univ Penn, Dept Biol, Philadelphia, PA 19104 USA. [Hajibabaei, Mehrdad] Univ Guelph, Dept Integrat Biol, Biodivers Inst Ontario, Guelph, ON N1G 2W1, Canada. RP Grishin, NV (reprint author), Univ Texas Southwestern, Howard Hughes Med Inst, Dallas, TX 75390 USA. EM grishin@chop.swmed.edu; burnsj@si.edu; djanzen@sas.upenn.edu; whallwac@sas.upenn.edu; mhajibab@uoguelph.ca FU U.S. National Science Foundation [BSR 9024770, DEB 9306296, 9400829, 9705072, 0072730, 0515699]; Wege Foundation; International Conservation Fund of Canada; Jessie B. Cox Charitable Trust; Blue Moon Fund; Guanacaste Dry Forest Conservation Fund; Area de Conservacion Guanacaste; University of Pennsylvania; Government of Canada through Genome Canada; Ontario Genomics Institute; NSERC Canada FX We are grateful to Mike Stangeland for bringing phenotypic differences of the new species to our attention; Blanca Huertas and David Lees (BMNH), Wolfram Mey (ZMHB), and Matthias Nuss (MTD) for providing unrestricted access to specimens under their care and help in the collections; Gerardo Lamas and Bernard Hermier for sharing images of Oxynetra type specimens; Kim Garwood and Isidro A. Chacon for providing photographs of Oxynetra hopfferi specimens; Ernst Brockmann for barcode sequences of Oxynetra confusa and Olafia roscius; Donald Harvey for dissecting genitalia; Karie Darrow for photographing genitalia of four Oxynetra species, plus adults of the two South American species; Zobeida Fuentes and ACG parataxonomists Harry Ramirez, Mariano Pereira, Dunia Garcia, Manuel Pereira, and Freddy Quesada for finding and rearing Oxynetra caterpillars and for identifying their foodplant; Isidro A. Chacon for a specimen of O. hopfferi; many of the above as well as Andy Warren for discussing various aspects of this study; and two anonymous reviewers for helpful comments. The study has been supported by U.S. National Science Foundation grants BSR 9024770 and DEB 9306296, 9400829, 9705072, 0072730, 0515699, and grants from the Wege Foundation, International Conservation Fund of Canada, Jessie B. Cox Charitable Trust, Blue Moon Fund, Guanacaste Dry Forest Conservation Fund, Area de Conservacion Guanacaste, and University of Pennsylvania (DHJ); by the Government of Canada through Genome Canada and the Ontario Genomics Institute, and by NSERC Canada (MH). NR 15 TC 4 Z9 5 U1 0 U2 3 PU LEPIDOPTERISTS SOC PI LOS ANGELES PA 900 EXPOSITION BLVD, LOS ANGELES, CA 90007-4057 USA SN 0024-0966 J9 J LEPID SOC JI J. Lepid. Soc. PD MAR 11 PY 2013 VL 67 IS 1 BP 1 EP 14 PG 14 WC Entomology SC Entomology GA 302KB UT WOS:000330602300001 ER PT J AU Davis, DR Diaz, R Overholt, WA AF Davis, Donald R. Diaz, Rodrigo Overholt, William A. TI SYSTEMATICS AND BIOLOGY OF CREMASTOBOMBYCIA CHROMOLAENAE, NEW SPECIES (GRACILLARIIDAE), A NATURAL ENEMY OF CHROMOLAENA ODORATA (L.) KING AND H. ROBINSON (ASTERACEAE) SO JOURNAL OF THE LEPIDOPTERISTS SOCIETY LA English DT Article DE biocontrol agent; biogeography; genital morphology; invasive plant species; larval biology AB A new species, Cremastobombycia chromolaenae, is described from Florida and Texas, USA. The larva is a leaf miner on Chromolaena odorata (L.) King and H. Robinson, a 2-3 in tall perennial shrub of the family Asteraceae, whose native range extends from southern Florida south to northern Argentina (Fig. 1). The plant is also known to occur in Africa, Asia, and Australia where it is considered exotic and in some countries has become a major weed. The larvae of C. chromolaenae are hypometamorphic and possess two distinct larval body forms and feeding behaviors-an early stage sap-feeding form with a flattened body and prognathous mouthparts and a later stage tissue-feeding form with a more cylindrical body and possessing hypognathous mouthparts. Based on head capsule counts and measurements, the larvae undergo five instars, with the first three instars being of the sap-feeding form and the last two tissue-feeding instars. The larval mine begins as a short, serpentine track which enlarges to a rounded, whitish, and eventually tentiform blotch. Cremastobombycia chromolaenae may have value as a biocontrol agent in those areas where the host plant has become a major problem. C1 [Davis, Donald R.] Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol, Washington, DC 20013 USA. [Diaz, Rodrigo; Overholt, William A.] Univ Florida, Biol Control Res & Containment Lab, Ft Pierce, FL 34945 USA. RP Davis, DR (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol, POB 37012,MRC 105, Washington, DC 20013 USA. EM davisd@si.edu; rrdg@ufl.edu; billover@ufl.edu NR 16 TC 2 Z9 2 U1 1 U2 2 PU LEPIDOPTERISTS SOC PI LOS ANGELES PA 900 EXPOSITION BLVD, LOS ANGELES, CA 90007-4057 USA SN 0024-0966 J9 J LEPID SOC JI J. Lepid. Soc. PD MAR 11 PY 2013 VL 67 IS 1 BP 35 EP 41 PG 7 WC Entomology SC Entomology GA 302KB UT WOS:000330602300004 ER PT J AU Castillo, RF Ubelaker, DH Acosta, JAL de la Fuente, GAC AF Fernandez Castillo, Rafael Ubelaker, Douglas H. Lorente Acosta, Jose Antonio Canadas de la Fuente, Guillermo A. TI Effects of temperature on bone tissue. Histological study of the changes in the bone matrix SO FORENSIC SCIENCE INTERNATIONAL LA English DT Article DE Burned bones; Forensic science; Forensic anthropology; Cremains; Thermal ID MINERALIZATION DENSITY DISTRIBUTION; FORENSIC ANTHROPOLOGY; CREMATED BONE; HUMAN REMAINS; COLLAGEN; COLOR; FIRE AB The analysis of burned human remains has given rise to many publications in the literature and has caused great interest among forensic specialists and physical anthropologists due to the difficulty in its analysis and interpretation. The main goal of this study has been to measure the changes that occur in bone matrix as a consequence of the increased temperature and establishing categories of histological morphology in relation to fire temperature. To this end, a total of 150 bone cylinders from the ilium obtained by bone biopsy. These samples have been obtained from forensic cadavers and burned at controlled temperatures between 100 and 1100 degrees C in an oven. The samples were fixed in methyl methacrylate and stained with hematoxylin-eosin, Goldner's trichrome and toluidine blue stains. The samples were studied using an optical microscope at 100x. Our study classifies the morphological changes that occur in bone matrix in four stages as a result of the temperature. (C) 2012 Elsevier Ireland Ltd. All rights reserved. C1 [Fernandez Castillo, Rafael] Univ Granada, Lab Anthropol, Fac Med, E-18071 Granada, Spain. [Ubelaker, Douglas H.] NMNH, Dept Anthropol, Smithsonian Inst, Washington, DC 20560 USA. [Lorente Acosta, Jose Antonio] Univ Granada, Dept Legal Med, Fac Med, E-18071 Granada, Spain. [Canadas de la Fuente, Guillermo A.] Univ Granada, Sch Hlth Sci, Granada 18012, Spain. RP Castillo, RF (reprint author), Univ Granada, Dept Anthropol, Avda Madrid S-N, E-18071 Granada, Spain. EM rafaelfernandez@ugr.es; ubelaked@si.edu; jlorente@ugr.es; gacf@ugr.es RI Castillo, Rafael/H-2178-2013; Canadas-De la Fuente, Guillermo/I-3679-2015 OI Castillo, Rafael/0000-0002-1814-5254; NR 33 TC 3 Z9 3 U1 3 U2 26 PU ELSEVIER IRELAND LTD PI CLARE PA ELSEVIER HOUSE, BROOKVALE PLAZA, EAST PARK SHANNON, CO, CLARE, 00000, IRELAND SN 0379-0738 J9 FORENSIC SCI INT JI Forensic Sci.Int. PD MAR 10 PY 2013 VL 226 IS 1-3 BP 33 EP 37 DI 10.1016/j.forsciint.2012.11.012 PG 5 WC Medicine, Legal SC Legal Medicine GA 115DF UT WOS:000316792100016 PM 23287528 ER PT J AU Barro, G Faber, SM Perez-Gonzalez, PG Koo, DC Williams, CC Kocevski, DD Trump, JR Mozena, M McGrath, E van der Wel, A Wuyts, S Bell, EF Croton, DJ Daniel, C Dekel, A Ashby, MLN Cheung, E Ferguson, HC Fontana, A Fang, J Giavalisco, M Grogin, NA Guo, YC Hathi, NP Hopkins, PF Huang, KH Koekemoer, AM Kartaltepe, JS Lee, KS Newman, JA Porter, LA Primack, JR Ryan, RE Rosario, D Somerville, RS Salvato, M Hsu, LT AF Barro, Guillermo Faber, S. M. Perez-Gonzalez, Pablo G. Koo, David C. Williams, Christina C. Kocevski, Dale D. Trump, Jonathan R. Mozena, Mark McGrath, Elizabeth van der Wel, Arjen Wuyts, Stijn Bell, Eric F. Croton, Darren J. Daniel, Ceverino Dekel, Avishai Ashby, M. L. N. Cheung, Edmond Ferguson, Henry C. Fontana, Adriano Fang, Jerome Giavalisco, Mauro Grogin, Norman A. Guo, Yicheng Hathi, Nimish P. Hopkins, Philip F. Huang, Kuang-Han Koekemoer, Anton M. Kartaltepe, Jeyhan S. Lee, Kyoung-Soo Newman, Jeffrey A. Porter, Lauren A. Primack, Joel R. Ryan, Russell E. Rosario, David Somerville, Rachel S. Salvato, Mara Hsu, Li-Ting TI CANDELS: THE PROGENITORS OF COMPACT QUIESCENT GALAXIES AT z similar to 2 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: high-redshift; galaxies: photometry; galaxies: starburst ID STAR-FORMING GALAXIES; ACTIVE GALACTIC NUCLEUS; SUPERMASSIVE BLACK-HOLES; HUBBLE-SPACE-TELESCOPE; LESS-THAN 2; EXTRAGALACTIC LEGACY SURVEY; HIGH-REDSHIFT GALAXIES; MASS-SIZE RELATION; STELLAR MASS; PHOTOMETRIC REDSHIFT AB We combine high-resolution Hubble Space Telescope/WFC3 images with multi- wavelength photometry to track the evolution of structure and activity of massive (M-* > 10(10)M(circle dot)) galaxies at redshifts z = 1.4-3 in two fields of the Cosmic Assembly Near-infrared Deep Extragalactic Legacy Survey. We detect compact, star- forming galaxies (cSFGs) whose number densities, masses, sizes, and star formation rates (SFRs) qualify them as likely progenitors of compact, quiescent, massive galaxies (cQGs) at z = 1.5-3. At z greater than or similar to 2, cSFGs present SFR = 100-200M(circle dot) yr(-1), yet their specific star formation rates (sSFR similar to 10(-9) yr(-1)) are typically half that of other massive SFGs at the same epoch, and host X-ray luminous active galactic nuclei (AGNs) 30 times (similar to 30%) more frequently. These properties suggest that cSFGs are formed by gas- rich processes (mergers or disk- instabilities) that induce a compact starburst and feed an AGN, which, in turn, quench the star formation on dynamical timescales (few 10(8) yr). The cSFGs are continuously being formed at z = 2-3 and fade to cQGs down to z similar to 1.5. After this epoch, cSFGs are rare, thereby truncating the formation of new cQGs. Meanwhile, down to z = 1, existing cQGs continue to enlarge to match local QGs in size, while less-gas-rich mergers and other secular mechanisms shepherd (larger) SFGs as later arrivals to the red sequence. In summary, we propose two evolutionary tracks of QG formation: an early (z greater than or similar to 2), formation path of rapidly quenched cSFGs fading into cQGs that later enlarge within the quiescent phase, and a late-arrival (z less than or similar to 2) path in which larger SFGs form extended QGs without passing through a compact state. C1 [Barro, Guillermo; Faber, S. M.; Koo, David C.; Kocevski, Dale D.; Trump, Jonathan R.; Mozena, Mark; McGrath, Elizabeth; Cheung, Edmond; Fang, Jerome; Guo, Yicheng] Univ Calif Santa Cruz, UCO Lick Observ, Santa Cruz, CA 95064 USA. [Barro, Guillermo; Faber, S. M.; Koo, David C.; Kocevski, Dale D.; Trump, Jonathan R.; Mozena, Mark; McGrath, Elizabeth; Cheung, Edmond; Fang, Jerome; Guo, Yicheng] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. [Perez-Gonzalez, Pablo G.] Univ Complutense Madrid, Dept Astrofis, Fac CC Fis, E-28040 Madrid, Spain. [Perez-Gonzalez, Pablo G.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Williams, Christina C.; Giavalisco, Mauro; Guo, Yicheng] Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA. [van der Wel, Arjen] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Wuyts, Stijn; Rosario, David; Salvato, Mara; Hsu, Li-Ting] Max Planck Inst Extraterr Phys, D-85741 Garching, Germany. [Bell, Eric F.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Croton, Darren J.] Swinburne Univ Technol, Ctr Astrophys & Supercomp, Hawthorn, Vic 3122, Australia. [Daniel, Ceverino; Dekel, Avishai] Hebrew Univ Jerusalem, Racah Inst Phys, IL-91904 Jerusalem, Israel. [Ashby, M. L. N.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Ferguson, Henry C.; Grogin, Norman A.; Huang, Kuang-Han; Koekemoer, Anton M.; Ryan, Russell E.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Fontana, Adriano] INAF Osservatorio Astron Roma, I-00040 Rome, Italy. [Hathi, Nimish P.] Observ Carnegie Inst Washington, Pasadena, CA 91101 USA. [Hopkins, Philip F.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Kartaltepe, Jeyhan S.] Natl Opt Astron Observ, Tucson, AZ 85719 USA. [Lee, Kyoung-Soo] Purdue Univ, Dept Phys, W Lafayette, IN 47907 USA. [Newman, Jeffrey A.] Univ Pittsburgh, Dept Phys & Astron, Pittsburgh, PA 15260 USA. [Porter, Lauren A.; Primack, Joel R.] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Santa Cruz, CA 95064 USA. [Somerville, Rachel S.] Rutgers State Univ, Dept Phys & Astron, Piscataway, NJ 08854 USA. RP Barro, G (reprint author), Univ Calif Santa Cruz, UCO Lick Observ, Santa Cruz, CA 95064 USA. RI Perez-Gonzalez, Pablo/J-2871-2016; Hathi, Nimish/J-7092-2014; OI Perez-Gonzalez, Pablo/0000-0003-4528-5639; Hathi, Nimish/0000-0001-6145-5090; Koekemoer, Anton/0000-0002-6610-2048; fontana, adriano/0000-0003-3820-2823; Bell, Eric/0000-0002-5564-9873 NR 129 TC 138 Z9 139 U1 0 U2 11 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAR 10 PY 2013 VL 765 IS 2 AR 104 DI 10.1088/0004-637X/765/2/104 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 103MP UT WOS:000315921500029 ER PT J AU Berger, E Zauderer, BA Levan, A Margutti, R Laskar, T Fong, W Mangano, V Fox, DB Tunnicliffe, RL Chornock, R Tanvir, NR Menten, KM Hjorth, J Roth, K Dupuy, TJ AF Berger, E. Zauderer, B. A. Levan, A. Margutti, R. Laskar, T. Fong, W. Mangano, V. Fox, D. B. Tunnicliffe, R. L. Chornock, R. Tanvir, N. R. Menten, K. M. Hjorth, J. Roth, K. Dupuy, T. J. TI THE AFTERGLOW AND ULIRG HOST GALAXY OF THE DARK SHORT GRB 120804A SO ASTROPHYSICAL JOURNAL LA English DT Article DE gamma-ray burst: general; gamma-ray burst: individual (GRB120804A) ID GAMMA-RAY BURSTS; SPECTRAL ENERGY-DISTRIBUTIONS; ACTIVE GALACTIC NUCLEI; STAR-FORMATION RATES; S-SELECTED GALAXIES; DIGITAL SKY SURVEY; DEEP-FIELD-SOUTH; LUMINOSITY FUNCTION; RADIO-SOURCE; LARGE ARRAY AB We present the optical discovery and subarcsecond optical and X-ray localization of the afterglow of the short GRB 120804A, as well as optical, near-IR, and radio detections of its host galaxy. X-ray observations with Swift/XRT, Chandra, and XMM-Newton extending to delta t approximate to 19 days reveal a single power-law decline. The optical afterglow is faint, and comparison to the X-ray flux indicates that GRB 120804A is "dark," with a rest-frame extinction of A(V)(host) approximate to 2.5 mag (at z = 1.3). The intrinsic neutral hydrogen column density inferred from the X-ray spectrum, N-H,N- int(z = 1.3) approximate to 2 x 10(22) cm(-2), is commensurate with the large extinction. The host galaxy exhibits red optical/near-IR colors. Equally important, JVLA observations at approximate to 0.9-11 days reveal a constant flux density of F-nu (5.8 GHz) = 35 +/- 4 mu Jy and an optically thin spectrum, unprecedented for GRB afterglows, but suggestive instead of emission from the host galaxy. The optical/near-IR and radio fluxes are well fit with the scaled spectral energy distribution of the local ultraluminous infrared galaxy (ULIRG) Arp 220 at z approximate to 1.3, with a resulting star formation rate of x approximate to 300 M-circle dot yr(-1). The inferred extinction and small projected offset (2.2 +/- 1.2 kpc) are also consistent with the ULIRG scenario, as is the presence of a companion galaxy at the same redshift and with a separation of about 11 kpc. The limits on radio afterglow emission, in conjunction with the observed X-ray and optical emission, require a circumburst density of n similar to 10(-3) cm(-3), an isotropic-equivalent energy scale of E-gamma,E- iso approximate to E-K,E- iso approximate to 7 x 10(51) erg, and a jet opening angle of theta(j) >= 11 degrees. The expected fraction of luminous infrared galaxies in the short GRB host sample is similar to 0.01 and similar to 0.25 (for pure stellar mass and star formation weighting, respectively). Thus, the observed fraction of two events in about 25 hosts (GRBs 120804A and 100206A) appears to support our previous conclusion that short GRBs track both stellar mass and star formation activity. C1 [Berger, E.; Zauderer, B. A.; Margutti, R.; Laskar, T.; Fong, W.; Chornock, R.; Dupuy, T. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Levan, A.; Tunnicliffe, R. L.] Univ Warwick, Dept Phys, Coventry CV4 7AL, W Midlands, England. [Mangano, V.] Ist Astrofis Spaziale & Fis Cosm, INAF, I-90146 Palermo, Italy. [Fox, D. B.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Tanvir, N. R.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. [Menten, K. M.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Hjorth, J.] Univ Copenhagen, Dark Cosmol Ctr, Niels Bohr Inst, DK-2100 Copenhagen O, Denmark. [Roth, K.] Gemini Observ, Hilo, HI 96720 USA. RP Berger, E (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Hjorth, Jens/M-5787-2014 OI Hjorth, Jens/0000-0002-4571-2306 FU National Science Foundation [AST-1107973, PHY11-25915]; NASA/Swift AO7 [NNX12AD69G]; Danish National Research Foundation; ESA Member States; USA (NASA); [ASI-INAF I/004/11/0] FX We thank Karina Caputi, Ranga Chary, Francesca Civano, Martin Elvis, and Jane Rigby for useful discussions about ULIRGs and AGNs. We also thank Brian Metzger for information on the magnetar scenario. The Berger GRB group at Harvard is supported by the National Science Foundation under Grant AST-1107973 and by NASA/Swift AO7 grant NNX12AD69G. E.B. acknowledges partial support of this research while in residence at the Kavli Institute for Theoretical Physics under National Science Foundation Grant PHY11-25915. The Dark Cosmology Centre is funded by the Danish National Research Foundation. V.M. acknowledges funding through contract ASI-INAF I/004/11/0. Observations were obtained with the JVLA (program 12A-394) operated by the National Radio Astronomy Observatory, a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. The paper includes data gathered with the 6.5 m Magellan Telescopes located at Las Campanas Observatory, Chile; with ESO Telescopes at the La Silla Paranal Observatory under program ID 089.D-0450; with the Gemini Observatory, which is operated by the Association of Universities for Research in Astronomy, Inc., under a cooperative agreement with the NSF on behalf of the Gemini partnership: the National Science Foundation (United States), the Science and Technology Facilities Council (United Kingdom), the National Research Council (Canada), CONICYT (Chile), the Australian Research Council (Australia), Ministerio da Ciencia, Tecnologia e Inovacao (Brazil) and Ministerio de Ciencia, Tecnologia e Innovacion Productiva (Argentina). This work is based in part on observations obtained with XMM-Newton, an ESA science mission with instruments and contributions directly funded by ESA Member States and the USA (NASA). NR 58 TC 15 Z9 16 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 MAR 10 PY 2013 VL 765 IS 2 AR 121 DI 10.1088/0004-637X/765/2/121 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 103MP UT WOS:000315921500046 ER PT J AU Carter, JA Agol, E AF Carter, Joshua A. Agol, Eric TI THE QUASIPERIODIC AUTOMATED TRANSIT SEARCH ALGORITHM SO ASTROPHYSICAL JOURNAL LA English DT Article DE methods: numerical; planetary systems; techniques: photometric ID TIMING VARIATIONS; PLANETARY TRANSITS; EXTRASOLAR PLANETS; TERRESTRIAL PLANETS; LIGHT CURVES; SYSTEM; PHOTOMETRY; MASS AB We present a new algorithm for detecting transiting extrasolar planets in time-series photometry. The Quasiperiodic Automated Transit Search (QATS) algorithm relaxes the usual assumption of strictly periodic transits by permitting a variable, but bounded, interval between successive transits. We show that this method is capable of detecting transiting planets with significant transit timing variations without any loss of significance-"smearing"-as would be incurred with traditional algorithms; however, this is at the cost of a slightly increased stochastic background. The approximate times of transit are standard products of the QATS search. Despite the increased flexibility, we show that QATS has a run-time complexity that is comparable to traditional search codes and is comparably easy to implement. QATS is applicable to data having a nearly uninterrupted, uniform cadence and is therefore well suited to the modern class of space-based transit searches (e.g., Kepler, CoRoT). Applications of QATS include transiting planets in dynamically active multi-planet systems and transiting planets in stellar binary systems. C1 [Carter, Joshua A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Agol, Eric] Univ Washington, Dept Astron, Seattle, WA 98195 USA. RP Carter, JA (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. OI Carter, Joshua/0000-0001-8152-2561; /0000-0002-0802-9145 FU NASA through Hubble Fellowship [HF-51267.01-A]; Space Telescope Science Institute; Association of Universities for Research in Astronomy, Inc., for NASA [NAS 5-26555.]; NSF [AST 0645416] FX The authors are grateful for helpful discussions with A. Kel'Manov, the Kepler TTV/Multibody working group, J. Jenkins, A. Ofir, and E. Petigura. The authors thank the participants of the Sagan Exoplanet Workshop for testing an implementation of the QATS algorithm. J. Carter thanks C. Carter, E. Carter, and the staff at Phillips House for their inspiration, labor and care during the writing of a portion of this manuscript. J. Carter acknowledges support by NASA through Hubble Fellowship grant HF-51267.01-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. E. Agol acknowledges support from NSF Career grant AST 0645416, and thanks Ian Agol for pointing out the usefulness of the Farey sequence in computing the QATS spectrum. NR 31 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 MAR 10 PY 2013 VL 765 IS 2 DI 10.1088/0004-637X/765/2/132 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 103MP UT WOS:000315921500057 ER PT J AU Fraine, JD Deming, D Gillon, M Jehin, E Demory, BO Benneke, B Seager, S Lewis, NK Knutson, H Desert, JM AF Fraine, Jonathan D. Deming, Drake Gillon, Michael Jehin, Emmanuel Demory, Brice-Olivier Benneke, Bjoern Seager, Sara Lewis, Nikole K. Knutson, Heather Desert, Jean-Michel TI SPITZER TRANSITS OF THE SUPER-EARTH GJ1214b AND IMPLICATIONS FOR ITS ATMOSPHERE SO ASTROPHYSICAL JOURNAL LA English DT Article DE infrared: planetary systems; planets and satellites: atmospheres; planets and satellites: composition; techniques: photometric ID METAL-RICH ATMOSPHERE; EXOPLANET GJ 1214B; TRANSMISSION SPECTROSCOPY; HD 189733B; MU-M; SPECTRUM; PLANETS; SEARCH; NEPTUNE; CURVES AB We observed the transiting super-Earth exoplanet GJ1214b using warm Spitzer at 4.5 mu m wavelength during a 20 day quasi-continuous sequence in 2011 May. The goals of our long observation were to accurately define the infrared transit radius of this nearby super-Earth, to search for the secondary eclipse, and to search for other transiting planets in the habitable zone of GJ1214. We here report results from the transit monitoring of GJ1214b, including a reanalysis of previous transit observations by Desert et al. In total, we analyze 14 transits of GJ1214b at 4.5 mu m, 3 transits at 3.6 mu m, and 7 new ground-based transits in the I + z band. Our new Spitzer data by themselves eliminate cloudless solar composition atmospheres for GJ1214b, and methane-rich models from Howe & Burrows. Using our new Spitzer measurements to anchor the observed transit radii of GJ1214b at long wavelengths, and adding new measurements in I + z, we evaluate models from Benneke & Seager and Howe & Burrows using chi(2) analysis. We find that the best-fit model exhibits an increase in transit radius at short wavelengths due to Rayleigh scattering. Pure water atmospheres are also possible. However, a flat line ( no atmosphere detected) remains among the best of the statistically acceptable models, and better than pure water atmospheres. We explore the effect of systematic differences among results from different observational groups, and we find that the Howe & Burrows tholin-haze model remains the best fit, even when systematic differences among observers are considered. C1 [Fraine, Jonathan D.; Deming, Drake] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Gillon, Michael; Jehin, Emmanuel] Univ Liege, Inst Astrophys & Geophys, Liege, Belgium. [Demory, Brice-Olivier; Benneke, Bjoern; Seager, Sara] MIT, Dept Earth Atmospher & Planetary Sci, Cambridge, MA 02139 USA. [Demory, Brice-Olivier; Benneke, Bjoern; Seager, Sara] MIT, Dept Phys, Cambridge, MA 02139 USA. [Lewis, Nikole K.] Univ Arizona, Dept Planetary Sci, Tucson, AZ 85721 USA. [Lewis, Nikole K.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA. [Knutson, Heather] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. [Desert, Jean-Michel] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Fraine, JD (reprint author), Univ Maryland, Dept Astron, College Pk, MD 20742 USA. EM jfraine@astro.umd.edu OI Demory, Brice-Olivier/0000-0002-9355-5165 FU NASA, JPL/Caltech; NASA 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 through an award issued by JPL/Caltech. We thank the Spitzer staff for their hard work and dedication in implementing these difficult observations, and the anonymous referee for a careful review of this paper. NR 38 TC 37 Z9 37 U1 1 U2 7 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAR 10 PY 2013 VL 765 IS 2 AR 127 DI 10.1088/0004-637X/765/2/127 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 103MP UT WOS:000315921500052 ER PT J AU Hermes, JJ Montgomery, MH Winget, DE Brown, WR Gianninas, A Kilic, M Kenyon, SJ Bell, KJ Harrold, ST AF Hermes, J. J. Montgomery, M. H. Winget, D. E. Brown, Warren R. Gianninas, A. Kilic, Mukremin Kenyon, Scott J. Bell, Keaton J. Harrold, Samuel T. TI DISCOVERY OF PULSATIONS, INCLUDING POSSIBLE PRESSURE MODES, IN TWO NEW EXTREMELY LOW MASS, He-CORE WHITE DWARFS SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries: close; Galaxy: stellar content; stars: individual (SDSS J111215.82+111745.0,SDSS J151826.68+065813.2); stars: variables: general; white dwarfs ID ZZ-CETI STARS; DRIVING MECHANISM; MERGER SYSTEMS; TELESCOPE; SPECTROGRAPH; EVOLUTION; HELIUM; LIMITS; I. AB We report the discovery of the second and third pulsating extremely low mass (ELM) white dwarfs (WDs), SDSS J111215.82+111745.0 (hereafter J1112) and SDSS J151826.68+065813.2 (hereafter J1518). Both have masses < 0.25 M-circle dot and effective temperatures below 10,000 K, establishing these putatively He-core WDs as a cooler class of pulsating hydrogen-atmosphere WDs (DAVs, or ZZ Ceti stars). The short-period pulsations evidenced in the light curve of J1112 may also represent the first observation of acoustic (p-mode) pulsations in any WD, which provide an exciting opportunity to probe this WD in a complimentary way compared to the long-period g-modes that are also present. J1112 is a T-eff = 9590 +/- 140 K and log g = 6.36 +/- 0.06 WD. The star displays sinusoidal variability at five distinct periodicities between 1792 and 2855 s. In this star, we also see short-period variability, strongest at 134.3 s, well short of the expected g-modes for such a low-mass WD. The other new pulsating WD, J1518, is a Teff = 9900 +/- 140 K and log g = 6.80 +/- 0.05 WD. The light curve of J1518 is highly non-sinusoidal, with at least seven significant periods between 1335 and 3848 s. Consistent with the expectation that ELM WDs must be formed in binaries, these two new pulsating He-core WDs, in addition to the prototype SDSS J184037.78+642312.3, have close companions. However, the observed variability is inconsistent with tidally induced pulsations and is so far best explained by the same hydrogen partial-ionization driving mechanism at work in classic C/O-core ZZ Ceti stars. C1 [Hermes, J. J.; Montgomery, M. H.; Winget, D. E.; Bell, Keaton J.; Harrold, Samuel T.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA. [Hermes, J. J.; Montgomery, M. H.; Winget, D. E.; Bell, Keaton J.; Harrold, Samuel T.] McDonald Observ, Ft Davis, TX 79734 USA. [Brown, Warren R.; Kenyon, Scott J.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. [Gianninas, A.; Kilic, Mukremin] Univ Oklahoma, Homer L Dodge Dept Phys & Astron, Norman, OK 73019 USA. RP Hermes, JJ (reprint author), Univ Texas Austin, Dept Astron, RLM 15308, Austin, TX 78712 USA. EM jjhermes@astro.as.utexas.edu RI Alexandros, Gianninas/B-8352-2016; OI Alexandros, Gianninas/0000-0002-8655-4308; Kenyon, Scott/0000-0003-0214-609X NR 43 TC 37 Z9 37 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 MAR 10 PY 2013 VL 765 IS 2 AR 102 DI 10.1088/0004-637X/765/2/102 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 103MP UT WOS:000315921500027 ER PT J AU Lazzati, D Morsony, BJ Margutti, R Begelman, MC AF Lazzati, Davide Morsony, Brian J. Margutti, Raffaella Begelman, Mitchell C. TI PHOTOSPHERIC EMISSION AS THE DOMINANT RADIATION MECHANISM IN LONG-DURATION GAMMA-RAY BURSTS SO ASTROPHYSICAL JOURNAL LA English DT Article DE gamma-ray burst: general; hydrodynamics; methods: numerical; relativistic processes ID PEAK-ENERGY; PROMPT EMISSION; COMPREHENSIVE ANALYSIS; JETS; LUMINOSITY; MODEL; EFFICIENCY; SPECTRA; GRB; THERMALIZATION AB We present the results of a set of numerical simulations of long-duration gamma-ray burst jets associated with massive, compact stellar progenitors. The simulations extend to large radii and allow us to locate the region in which the peak frequency of the advected radiation is set before the radiation is released at the photosphere. Light curves and spectra are calculated for different viewing angles as well as different progenitor structures and jet properties. We find that the radiation released at the photosphere of matter-dominated jets is able to reproduce the observed Amati and energy-Lorentz factor correlations. Our simulations also predict a correlation between the burst energy and the radiative efficiency of the prompt phase, consistent with observations. C1 [Lazzati, Davide] NC State Univ, Dept Phys, Raleigh, NC 27695 USA. [Morsony, Brian J.] Univ Wisconsin, Dept Astron, Madison, WI 53706 USA. [Margutti, Raffaella] Harvard Smithsonian Ctr Astrophys, ITC, Cambridge, MA 02138 USA. [Begelman, Mitchell C.] Univ Colorado, JILA, Boulder, CO 80309 USA. [Begelman, Mitchell C.] NIST, Boulder, CO 80309 USA. [Begelman, Mitchell C.] Univ Colorado, Dept Astrophys & Planetary Sci, Boulder, CO 80309 USA. RP Lazzati, D (reprint author), NC State Univ, Dept Phys, 2401 Stinson Dr, Raleigh, NC 27695 USA. FU Fermi GI program [NNX10AP55G, NNX12AO74G]; NSF Astronomy and Astrophysics Postdoctoral Fellowship [AST-1102796] FX We thank S. E. Woosley and A. Heger for making their pre-SN models available, Lorenzo Amati for sharing his up-to-date data on the Amati correlation before publication, and Gabriele Ghisellini and Dimitrios Giannios for valuable discussions. 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. This work was supported in part by the Fermi GI program grants NNX10AP55G and NNX12AO74G (DL). B.J.M. is supported by an NSF Astronomy and Astrophysics Postdoctoral Fellowship under award AST-1102796. NR 49 TC 34 Z9 34 U1 0 U2 7 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAR 10 PY 2013 VL 765 IS 2 AR 103 DI 10.1088/0004-637X/765/2/103 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 103MP UT WOS:000315921500028 ER PT J AU Nardini, E Wang, JF Fabbiano, G Elvis, M Pellegrini, S Risaliti, G Karovska, M Zezas, A AF Nardini, E. Wang, Junfeng Fabbiano, G. Elvis, M. Pellegrini, S. Risaliti, G. Karovska, M. Zezas, A. TI THE EXCEPTIONAL SOFT X-RAY HALO OF THE GALAXY MERGER NGC 6240 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: active; galaxies: halos; galaxies: individual (NGC 6240); galaxies: starburst; X-rays: galaxies ID ACTIVE GALACTIC NUCLEUS; ULTRALUMINOUS INFRARED GALAXIES; HOT INTERSTELLAR-MEDIUM; HUBBLE-SPACE-TELESCOPE; ELLIPTIC GALAXIES; ANTENNAE GALAXIES; MERGING GALAXIES; MOLECULAR GAS; STARBURST GALAXIES; STAR-FORMATION AB We report on a recent similar to 150 ks long Chandra observation of the ultraluminous infrared galaxy merger NGC 6240, which allows a detailed investigation of the diffuse galactic halo. Extended soft X-ray emission is detected at the 3 sigma confidence level over a diamond-shaped region with projected physical size of similar to 110 x 80 kpc, and a single-component thermal model provides a reasonably good fit to the observed X-ray spectrum. The hot gas has a temperature of similar to 7.5 million K, an estimated density of 2.5 x 10(-3) cm(-3), and a total mass of similar to 10(10)M(circle dot), resulting in an intrinsic 0.4-2.5 keV luminosity of 4 x 10(41) erg s(-1). The average temperature of 0.65 keV is quite high to be obviously related to either the binding energy in the dark-matter gravitational potential of the system or the energy dissipation and shocks following the galactic collision, yet the spatially resolved spectral analysis reveals limited variations across the halo. The relative abundance of the main alpha-elements with respect to iron is several times the solar value, and nearly constant as well, implying a uniform enrichment by type II supernovae out to the largest scales. Taken as a whole, the observational evidence is not compatible with a superwind originated by a recent, nuclear starburst, but rather hints at widespread, enhanced star formation proceeding at a steady rate over the entire dynamical timescale (similar to 200 Myr). The preferred scenario is that of a starburst-processed gas component gently expanding into, and mixing with, a pre-existing halo medium of lower metallicity (Z similar to 0.1 solar) and temperature (kT similar to 0.25 keV). This picture cannot be probed more extensively with the present data, and the ultimate fate of the diffuse, hot gas remains uncertain. Under some favorable conditions, at least a fraction of it might be retained after the merger completion, and evolve into the hot halo of a young elliptical galaxy. C1 [Nardini, E.; Wang, Junfeng; Fabbiano, G.; Elvis, M.; Risaliti, G.; Karovska, M.; Zezas, A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Pellegrini, S.] Univ Bologna, Dipartimento Fis & Astron, I-40127 Bologna, Italy. [Risaliti, G.] INAF Osservatorio Astrofis Arcetri, I-50125 Florence, Italy. [Zezas, A.] Univ Crete, Dept Phys, GR-71003 Iraklion, Crete, Greece. RP Nardini, E (reprint author), Keele Univ, Sch Phys & Geog Sci, Astrophys Grp, Keele ST5 5BG, Staffs, England. EM e.nardini@keele.ac.uk RI Zezas, Andreas/C-7543-2011; OI Zezas, Andreas/0000-0001-8952-676X; Risaliti, Guido/0000-0002-3556-977X FU NASA [GO1-12123X, NAS8-03060, NAS5-26555]; Chandra X-ray Center (CXC) FX This research is supported by NASA grant GO1-12123X (PI: G. Fabbiano). We thank the anonymous referee for a careful reading, and constructive comments that helped to improve the clarity of this paper. We acknowledge support from the Chandra X-ray Center (CXC), which is operated by the Smithsonian Astrophysical Observatory (SAO) for and on behalf of NASA under contract NAS8-03060. We have made use of software provided by the CXC in the application packages ciao and Sherpa, and of SAOImage DS9, developed by SAO. The X-ray data were retrieved from the Chandra Data Archive, and the HST image was obtained from the MAST data archive at the Space Telescope Science Institute. STScI is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555. NR 113 TC 10 Z9 10 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 MAR 10 PY 2013 VL 765 IS 2 AR 141 DI 10.1088/0004-637X/765/2/141 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 103MP UT WOS:000315921500066 ER PT J AU Kauffmann, J Pillai, T Zhang, QZ AF Kauffmann, Jens Pillai, Thushara Zhang, Qizhou TI THE GALACTIC CENTER CLOUD G0.253+0.016: A MASSIVE DENSE CLOUD WITH LOW STAR FORMATION POTENTIAL SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE Galaxy: center; ISM: clouds; stars: formation ID INFRARED-DARK CLOUDS; MOLECULAR CLOUDS; DUST CONTINUUM; SIZE RELATION; MILKY-WAY; II.; CORES; GAS; FRAGMENTATION; EMISSION AB We present the first interferometric molecular line and dust emission maps for the Galactic Center (GC) cloud G0.253+0.016, observed using CARMA and the SMA. This cloud is very dense, and concentrates a mass exceeding the Orion Molecular Cloud Complex (2 x 10(5) M-circle dot) into a radius of only 3 pc, but it is essentially starless. G0.253+0.016 therefore violates "star formation laws" presently used to explain trends in galactic and extragalactic star formation by a factor similar to 45. Our observations show a lack of dense cores of significant mass and density, thus explaining the low star formation activity. Instead, cores with low densities and line widths less than or similar to 1 kms(-1)-probably the narrowest lines reported for the GC region to date-are found. Evolution over several 10(5) yr is needed before more massive cores, and possibly an Arches-like stellar cluster, could form. Given the disruptive dynamics of the GC region, and the potentially unbound nature of G0.253+0.016, it is not clear that this evolution will happen. C1 [Kauffmann, Jens; Pillai, Thushara] CALTECH, Dept Astron, Pasadena, CA 91125 USA. [Zhang, Qizhou] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Kauffmann, J (reprint author), CALTECH, Dept Astron, 1200 East Calif Blvd, Pasadena, CA 91125 USA. EM jens.kauffmann@astro.caltech.edu OI Zhang, Qizhou/0000-0003-2384-6589 FU Smithsonian Institution; Academia Sinica; Gordon and Betty Moore Foundation; Kenneth T. and Eileen L. Norris Foundation; James S. McDonnell Foundation; Associates of the California Institute of Technology; University of Chicago; state of California; state of Illinois; state of Maryland; National Science Foundation (NSF) [AST 05-40399]; CARMA partner universities; National Aeronautics and Space Administration; CARMA; Dewey, Cheetham & Howe (Cambridge, MA) 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.; Support for CARMA construction was derived from the Gordon and Betty Moore Foundation, the Kenneth T. and Eileen L. Norris Foundation, the James S. McDonnell Foundation, the Associates of the California Institute of Technology, the University of Chicago, the states of California, Illinois, and Maryland, and the National Science Foundation (NSF). Ongoing CARMA development and operations are supported by the NSF and the CARMA partner universities.; We thank S. Longmore for giving us access to Longmore et al. (2012) in advance of publication, D. Lis and K. Menten for enlightening discussions, and the anonymous referee for making the Letter more readable. J.K. is grateful to D. Li and P. Goldsmith, his hosts at JPL, for making this work possible. Part of the research was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. T.P. acknowledges support from CARMA, which is supported by the National Science Foundation through grant AST 05-40399. J.K. acknowledges support from Dewey, Cheetham & Howe (Cambridge, MA). NR 36 TC 34 Z9 34 U1 0 U2 1 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 MAR 10 PY 2013 VL 765 IS 2 AR L35 DI 10.1088/2041-8205/765/2/L35 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 097QR UT WOS:000315489100011 ER PT J AU Veach, TJ Groppi, CE Hedden, A AF Veach, Todd J. Groppi, Christopher E. Hedden, Abigail TI VIBRATIONALLY EXCITED HCN AROUND AFGL 2591: A PROBE OF PROTOSTELLAR STRUCTURE SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE ISM: molecules; stars: formation; stars: individual (AFGL 2591); stars: kinematics and dynamics; stars: protostars; submillimeter: stars ID YOUNG; EMISSION; WATER; DISKS; STARS; CS AB Vibrationally excited molecules with submillimeter rotational transitions are potentially excellent probes of physical conditions near protostars. This study uses observations of the upsilon = 1 and upsilon = 2 ro-vibrational modes of HCN (4-3) to probe this environment. The presence or absence and relative strengths of these ro-vibrational lines probe the gas excitation mechanism and physical conditions in warm, dense material associated with protostellar disks. We present pilot observations from the Heinrich Hertz Submillimeter Telescope and follow-up observations from the Submillimeter Array. All vibrationally excited HCN (4-3) upsilon = 0, upsilon = 1, and upsilon = 2 lines were observed. The existence of the three upsilon = 2 lines at approximately equal intensity imply collisional excitation with a density of greater than (10(10) cm(-3)) and a temperature of >1000 K for the emitting gas. This warm, high-density material should directly trace structures formed in the protostellar envelope and disk environment. Further, the line shapes of the upsilon = 2 emission may suggest a Keplerian disk. This Letter demonstrates the utility of this technique which is of particular interest due to the recent inauguration of the Atacama Large Millimeter Array. C1 [Veach, Todd J.] Arizona State Univ, Dept Phys, Tempe, AZ 85287 USA. [Groppi, Christopher E.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA. [Hedden, Abigail] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Veach, TJ (reprint author), Arizona State Univ, Dept Phys, Tempe, AZ 85287 USA. EM tveach@asu.edu RI Groppi, Christopher/L-5284-2013 OI Groppi, Christopher/0000-0002-2021-1628 FU Smithsonian Institution; Academia Sinica FX The SMT is operated by the Arizona Radio Observatory (ARO), Steward Observatory, University of Arizona. The Submillimeter Array (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. NR 14 TC 6 Z9 6 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 MAR 10 PY 2013 VL 765 IS 2 AR L34 DI 10.1088/2041-8205/765/2/L34 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 097QR UT WOS:000315489100010 ER PT J AU Zapata, LA Schmid-Burgk, J Perez-Goytia, N Ho, PTP Rodriguez, LF Loinard, L Cruz-Gonzalez, I AF Zapata, Luis A. Schmid-Burgk, Johannes Perez-Goytia, Nadia Ho, Paul T. P. Rodriguez, Luis F. Loinard, Laurent Cruz-Gonzalez, Irene TI A 10,000 YEAR OLD EXPLOSION IN DR21 SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE ISM: individual objects (DR21); ISM: jets and outflows; ISM: molecules; stars: formation; techniques: imaging spectroscopy ID DR-21; REGIONS; ORION; ARRAY AB Sensitive high angular resolution (similar to 2 '') CO(2-1) line observations made with the Submillimeter Array of the flow emanating from the high-mass star-forming region DR21 located in the Cygnus X molecular cloud are presented. These new interferometric observations indicate that this well known enigmatic outflow appears to have been produced by an explosive event that took place about 10,000 years ago, and that might be related to the disintegration of a massive stellar system such as the one that occurred in Orion Becklin-Neugebauer/Kleinman-Low 500 years ago, but about 20 times more energetic. This result therefore argues in favor of the idea that the disintegration of young stellar systems perhaps is a frequent phenomenon present during the formation of massive stars. However, many more theoretical and observational studies are still needed to confirm our hypothesis. C1 [Zapata, Luis A.; Perez-Goytia, Nadia; Rodriguez, Luis F.; Loinard, Laurent] UNAM, Ctr Radioastron Astrofis, Morelia 58089, Michoacan, Mexico. [Schmid-Burgk, Johannes] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Ho, Paul T. P.] Acad Sinica, Inst Astron & Astrophys, Taipei 115, Taiwan. [Ho, Paul T. P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Cruz-Gonzalez, Irene] Univ Nacl Autonoma Mexico, Inst Astron, Mexico City 04510, DF, Mexico. RP Zapata, LA (reprint author), UNAM, Ctr Radioastron Astrofis, Apdo Postal 3-72 Xangari, Morelia 58089, Michoacan, Mexico. FU DGAPA; UNAM; CONACyT, Mexico; Alexander von Humboldt Stiftung FX L.A.Z., L.L., and L.F.R. acknowledge financial support from DGAPA, UNAM, and CONACyT, Mexico. L.L. is indebted to the Alexander von Humboldt Stiftung for financial support. We are very grateful to Chris Davis for having provided us with his H2 image of the DR21 outflow. This study makes use of Spitzer telescope infrared images from the archive. We are very thankful for the suggestions of an anonymous referee which helped to improve our manuscript. NR 15 TC 9 Z9 9 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 MAR 10 PY 2013 VL 765 IS 2 AR L29 DI 10.1088/2041-8205/765/2/L29 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 097QR UT WOS:000315489100005 ER PT J AU Onofrio, R AF Onofrio, Roberto TI ON WEAK INTERACTIONS AS SHORT-DISTANCE MANIFESTATIONS OF GRAVITY SO MODERN PHYSICS LETTERS A LA English DT Article DE Weak interactions; gravitation; fundamental constants ID EARTHS GRAVITATIONAL-FIELD; NEWTONIAN GRAVITATION; GENERAL RELATIVITY; SPACETIME FOAM; QUANTUM STATES; CONSTANT; TORSION; PROTON; FORCES AB We conjecture that weak interactions are peculiar manifestations of quantum gravity at the Fermi scale, and that the Fermi constant is related to the Newtonian constant of gravitation. In this framework one may understand the violations of fundamental symmetries by the weak interactions, in particular parity violations, as due to fluctuations of the spacetime geometry at a Planck scale coinciding with the Fermi scale. As a consequence, gravitational phenomena should play a more important role in the microworld, and experimental settings are suggested to test this hypothesis. C1 [Onofrio, Roberto] Univ Padua, Dipartimento Fis & Astron Galileo Galilei, I-35131 Padua, Italy. [Onofrio, Roberto] Harvard Smithsonian Ctr Astrophys, ITAMP, Cambridge, MA 02138 USA. RP Onofrio, R (reprint author), Univ Padua, Dipartimento Fis & Astron Galileo Galilei, Via Marzolo 8, I-35131 Padua, Italy. EM onofrior@gmail.com NR 32 TC 8 Z9 8 U1 0 U2 38 PU WORLD SCIENTIFIC PUBL CO PTE LTD PI SINGAPORE PA 5 TOH TUCK LINK, SINGAPORE 596224, SINGAPORE SN 0217-7323 J9 MOD PHYS LETT A JI Mod. Phys. Lett. A PD MAR 7 PY 2013 VL 28 IS 7 AR 1350022 DI 10.1142/S0217732313500223 PG 7 WC Physics, Nuclear; Physics, Particles & Fields; Physics, Mathematical SC Physics GA 116TS UT WOS:000316906500006 ER PT J AU Martinez, O Lattanzi, V Thorwirth, S McCarthy, MC AF Martinez, Oscar, Jr. Lattanzi, Valerio Thorwirth, Sven McCarthy, Michael C. TI Detection of protonated vinyl cyanide, CH2CHCNH+, a prototypical branched nitrile cation SO JOURNAL OF CHEMICAL PHYSICS LA English DT Article ID TITANS UPPER-ATMOSPHERE; ION MOLECULE CHEMISTRY; ROTATIONAL SPECTROSCOPY; 2ND DERIVATIVES; BASIS-SETS; SPECTRA; ACRYLONITRILE; PERTURBATION; EQUILIBRIUM; PREDICTION AB The rotational spectrum of protonated vinyl cyanide, CH2CHCNH+, a prototypical branched nitrile species and likely intermediate in astronomical sources and in the planetary atmosphere of Titan, has been detected in a pulsed-discharge supersonic molecular beam by means of Fourier transform microwave spectroscopy. Fifteen lines arising from 11 a-type rotational transitions have been observed between 9 and 46 GHz, several with partially resolved nitrogen hyperfine structure. From this data set, the leading spectroscopic constants, including all three rotational constants, have been determined to high accuracy. The agreement between experimental rotational constants and those calculated at the CCSD(T) level of theory is of order 0.1%. An even better estimate was obtained through empirical scaling using calculated and experimental rotational constants of isoelectronic vinyl acetylene. Measurement of a small nitrogen quadrupole coupling constant in protonated vinyl cyanide is consistent with a quadruply bound nitrogen atom and a H+-N C-R type structure. Because vinyl cyanide is abundant in molecule-rich astronomical sources and possesses a high proton affinity, and because protonated vinyl cyanide is unreactive with hydrogen and other well-known interstellar species, this cation is an excellent candidate for astronomical detection. The present work suggests that other organic molecules containing the nitrile group and closely related species such as protonated vinyl acetylene can probably be detected with the same instrumentation. (C) 2013 American Institute of Physics. [http://dx.doi.org/10.1063/1.4793316] C1 [Martinez, Oscar, Jr.; Lattanzi, Valerio; McCarthy, Michael C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Martinez, Oscar, Jr.; Lattanzi, Valerio; McCarthy, Michael C.] Harvard Univ, Sch Engn & Appl Sci, Cambridge, MA 02138 USA. [Thorwirth, Sven] Univ Cologne, Inst Phys 1, D-50937 Cologne, Germany. RP Martinez, O (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Thorwirth, Sven/C-6217-2011; OI Thorwirth, Sven/0000-0001-8200-6710; McCarthy, Michael/0000-0001-9142-0008 FU National Science Foundation (NSF) [CHE-1058063]; Deutsche Forschungsgemeinschaft (DFG) [TH 1301/3-1, TH 1301/3-2] FX We thank C. A. Gottlieb for helpful conversations, and D. Kokkin and E. S. Palmer for technical assistance. The work in Cambridge is supported from National Science Foundation (NSF) Grant No. CHE-1058063. S.T. gratefully acknowledges funding from the Deutsche Forschungsgemeinschaft (DFG) through Grant Nos. TH 1301/3-1 and TH 1301/3-2. NR 45 TC 4 Z9 4 U1 2 U2 26 PU AMER INST PHYSICS PI MELVILLE PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1, MELVILLE, NY 11747-4501 USA SN 0021-9606 J9 J CHEM PHYS JI J. Chem. Phys. PD MAR 7 PY 2013 VL 138 IS 9 AR 094316 DI 10.1063/1.4793316 PG 7 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA 102WD UT WOS:000315874200034 PM 23485303 ER PT J AU Lee, MY Munroe, TA Shao, KT AF Lee, Mao-Ying Munroe, Thomas A. Shao, Kwang-Tsao TI Symphurus orientalis (Bleeker) redefined based on morphological and molecular characters (Pleuronectiformes: Cynoglossidae) SO ZOOTAXA LA English DT Article DE Symphurus orientalis; Symphurus novemfasciatus; flatfish; redescription; synonym; tonguefish; species complex; cryptic species ID 16S RIBOSOMAL-RNA; PACIFIC TONGUEFISH PLEURONECTIFORMES; DNA BARCODING REVEALS; WESTERN PACIFIC; HYDROTHERMAL VENTS; TAXONOMIC STATUS; IDENTIFICATION; PERCIFORMES; AUSTRALIA; TELEOSTEI AB Aphoristia (= Symphurus) orientalis Bleeker 1879, collected from an unspecified depth and location in Japanese waters, is the first described species of symphurine tonguefish from Indo-Pacific waters. The original description with accompanying illustration is based on the unique holotype specimen and provides limited diagnostic characters for this taxon. Subsequent to its description, the holotype of A. orientalis has been lost. Limited diagnostic information and loss of the holotype have caused considerable confusion to subsequent systematic studies regarding the identity of this and similar tonguefish species occurring in the Indo-West Pacific region. Several, often-cited, taxonomic accounts purportedly redescribing S. orientalis are erroneous because they include more than one species in these redescriptions. These erroneous redescriptions not only confused the species concept of S. orientalis (Bleeker), but also confounded the systematics of similar Indo-West Pacific tonguefishes. Symphurus novemfasciatus Shen and Lin, described on two specimens collected in southern Taiwan, shares many morphological and pigmentation features similar to those of S. orientalis. Morphological data from a large series of tonguefishes collected in Taiwanese and Japanese waters, as well as molecular data from a smaller number of specimens from these locations, including the type locality of S. novemfasciatus, confirm the presence of only one species, S. orientalis (Bleeker), among these specimens. Symphurus novemfasciatus Shen and Lin is therefore regarded as a junior subjective synonym of S. orientalis. Symphurus orientalis is redefined based on a large series of specimens identified by a consistent set of morphological criteria, and a neotype is designated to stabilize nomenclature and systematics of this species. Symphurus orientalis differs from congeners by its combination of: a predominant 1-2-2-2-2 pattern of interdigitation of proximal dorsal-fin pterygiophores and neural spines, 12 caudal-fin rays, 9 abdominal and 52-55 total vertebrae, four hypurals, 96-101 dorsal-fin rays, 82-89 anal-fin rays, 87-99 longitudinal scale rows, 37-42 transverse scales, 5-11 (usually) distinct, complete or incomplete, blackish-brown crossbands on the ocular side, uniformly white blind side, and conspicuous bluish-black peritoneum. Documenting morphological variation for S. orientalis represents the most important step towards clarification of the identity of this and other symphurine tonguefish species from this region. Reliable identification of specimens of S. orientalis also provides the foundation for evaluating the status of several other, poorly-known, nominal species of Indo-West Pacific tonguefishes that have features similar to those of S. orientalis. Improved identifications will lead to better knowledge on the geographic distribution of S. orientalis and these other species, as well as to improve estimates of biodiversity and the biogeography of Indo-West Pacific symphurine tonguefishes. C1 [Lee, Mao-Ying] Natl Taiwan Ocean Univ, Dept Aquaculture, Keelung 20224, Taiwan. [Munroe, Thomas A.] NOAA, Natl Marine Fisheries Serv, Natl Systemat Lab, Smithsonian Inst,Natl Museum Nat Hist, Washington, DC 20013 USA. [Shao, Kwang-Tsao] Acad Sinica, Biodivers Res Ctr, Lab Fish Ecol & Evolut, Taipei 11529, Taiwan. RP Shao, KT (reprint author), Acad Sinica, Biodivers Res Ctr, Lab Fish Ecol & Evolut, Taipei 11529, Taiwan. EM coleoptera@gmail.com; munroet@si.edu; zoskt@gate.sinica.edu.tw FU National Science Council [NSC 96-2628-B-001-006-MY3, NSC 99-2621-B-001-008-MY3]; Biodiversity Research Center, Academia Sinica. FX This work represents a portion of a collecting activities grant investigating the biodiversity and systematics of deep-sea fishes in Taiwanese waters supported by the National Science Council (NSC 96-2628-B-001-006-MY3 and NSC 99-2621-B-001-008-MY3) and awarded to K.-T. Shao, Biodiversity Research Center, Academia Sinica. We thank H.-M. Yeh, Coastal and Offshore Resource Research Center, Fisheries Research Institute, who kindly provided trawl station data from research vessels. H.-C. Ho, P.-F. Lee, Y.-C. Liao and L.-P. Lin assisted with collecting specimens and kindly provided other specimens used in this study. K.-C. Hsu advised M.-Y. Lee regarding molecular aspects of this research study. A. Collins, NSL, kindly provided information and helpful editorial suggestions regarding molecular approaches used in this study. L.-P. Lin and C.-W. Chang assisted with loans and shipments of specimens. M. Nizinski provided assistance and support during M.-Y. Lee's visit to the National Museum of Natural History, Smithsonian Institution. H. Endo, N. Nakayama, and R. Asaoka provided assistance and support during M.-Y. Lee's visit to the Department of Biology, Faculty of Science, Kochi University. They also provided two important fresh specimens of S. orientalis from Japan to help with molecular comparisons. K. Matsuura and G. Shinohara provided loan of Suruga Bay specimens during M.-Y. Lee's visit to the Department of Zoology, National Science Museum. K. Murphy (USNM) assisted with specimen and catalogue information. K. Nakaya, Hokkaido University, provided the photograph of the holotype of S. septemstriatus. K. Vinnikov, University of Hawaii at Manoa, graciously provided translations of Russian literature. L. Willis, NMFS-NSL, assisted with literature. H.-M. Chen provided comments on an early draft of the manuscript. M.-Y. Lee extends his appreciation to all members of the Laboratory of Fish Ecology and Evolution for their support, especially H. Lee for helping to draw the distribution map and assistance during this study. NR 117 TC 4 Z9 4 U1 1 U2 1 PU MAGNOLIA PRESS PI AUCKLAND PA PO BOX 41383, AUCKLAND, ST LUKES 1030, NEW ZEALAND SN 1175-5326 EI 1175-5334 J9 ZOOTAXA JI Zootaxa PD MAR 7 PY 2013 VL 3620 IS 3 BP 379 EP 403 PG 25 WC Zoology SC Zoology GA 103RS UT WOS:000315937200003 PM 26120714 ER PT J AU Geipel, I Jung, K Kalko, EKV AF Geipel, Inga Jung, Kirsten Kalko, Elisabeth K. V. TI Perception of silent and motionless prey on vegetation by echolocation in the gleaning bat Micronycteris microtis SO PROCEEDINGS OF THE ROYAL SOCIETY B-BIOLOGICAL SCIENCES LA English DT Article DE prey perception; echolocation; acoustic clutter; narrow-space active gleaning insectivorous bat; Micronycteris microtis ID LONG-EARED BATS; MYOTIS-NATTERERI; EPTESICUS-NILSSONII; PLECOTUS-AURITUS; MEGADERMA-LYRA; SENSORY BASIS; EATING BATS; BEHAVIOR; PHYLLOSTOMIDAE; CHIROPTERA AB Gleaning insectivorous bats that forage by using echolocation within dense forest vegetation face the sensorial challenge of acoustic masking effects. Active perception of silent and motionless prey in acoustically cluttered environments by echolocation alone has thus been regarded impossible. The gleaning insectivorous bat Micronycteris microtis however, forages in dense understory vegetation and preys on insects, including dragonflies, which rest silent and motionless on vegetation. From behavioural experiments, we show that M. microtis uses echolocation as the sole sensorial modality for successful prey perception within a complex acoustic environment. All individuals performed a stereotypical three-dimensional hovering flight in front of prey items, while continuously emitting short, multiharmonic, broadband echolocation calls. We observed a high precision in target localization which suggests that M. microtis perceives a detailed acoustic image of the prey based on shape, surface structure and material. Our experiments provide, to our knowledge, the first evidence that a gleaning bat uses echolocation alone for successful detection, classification and precise localization of silent and motionless prey in acoustic clutter. Overall, we conclude that the three-dimensional hovering flight of M. microtis in combination with a frequent emission of short, high-frequency echolocation calls is the key for active prey perception in acoustically highly cluttered environments. C1 [Geipel, Inga; Jung, Kirsten; Kalko, Elisabeth K. V.] Univ Ulm, Inst Expt Ecol, D-89069 Ulm, Germany. [Kalko, Elisabeth K. V.] Smithsonian Trop Res Inst, Panama City, Panama. RP Geipel, I (reprint author), Univ Ulm, Inst Expt Ecol, Albert Einstein Allee 11, D-89069 Ulm, Germany. EM inga.geipel@uni-ulm.de FU University of Ulm; STRI FX We thank T. Jonsson for his continuous support and helpful comments. We thank M. Tschapka, J. Ratcliffe, H.-U. Schnitzler, M. Beecher, B. Fenton and an anonymous referee for their helpful and valuable comments improving the manuscript. Bats were captured with the permission from local authorities (ANAM, scientific permit no. SE/A-32-07). Financial support was provided by University of Ulm (I.G. and E.K.V.K) and STRI (E.K.V.K). NR 54 TC 20 Z9 20 U1 3 U2 96 PU ROYAL SOC PI LONDON PA 6-9 CARLTON HOUSE TERRACE, LONDON SW1Y 5AG, ENGLAND SN 0962-8452 J9 P ROY SOC B-BIOL SCI JI Proc. R. Soc. B-Biol. Sci. PD MAR 7 PY 2013 VL 280 IS 1754 AR 20122830 DI 10.1098/rspb.2012.2830 PG 7 WC Biology; Ecology; Evolutionary Biology SC Life Sciences & Biomedicine - Other Topics; Environmental Sciences & Ecology; Evolutionary Biology GA 072IN UT WOS:000313663700016 PM 23325775 ER PT J AU Padilla-Torres, SD Ferraz, G Luz, SLB Zamora-Perea, E Abad-Franch, F AF Padilla-Torres, Samael D. Ferraz, Goncalo Luz, Sergio L. B. Zamora-Perea, Elvira Abad-Franch, Fernando TI Modeling Dengue Vector Dynamics under Imperfect Detection: Three Years of Site-Occupancy by Aedes aegypti and Aedes albopictus in Urban Amazonia SO PLOS ONE LA English DT Article ID POPULATION-DYNAMICS; PUERTO-RICO; TRANSMISSION; MOSQUITOS; CULICIDAE; DIPTERA; OVITRAP; BRAZIL; FEVER; INFESTATION AB Aedes aegypti and Ae. albopictus are the vectors of dengue, the most important arboviral disease of humans. To date, Aedes ecology studies have assumed that the vectors are truly absent from sites where they are not detected; since no perfect detection method exists, this assumption is questionable. Imperfect detection may bias estimates of key vector surveillance/control parameters, including site-occupancy (infestation) rates and control intervention effects. We used a modeling approach that explicitly accounts for imperfect detection and a 38-month, 55-site detection/non-detection dataset to quantify the effects of municipality/state control interventions on Aedes site-occupancy dynamics, considering meteorological and dwelling-level covariates. Ae. aegypti site-occupancy estimates (mean 0.91; range 0.79-0.97) were much higher than reported by routine surveillance based on ` rapid larval surveys' (0.03; 0.02-0.11) and moderately higher than directly ascertained with oviposition traps (0.68; 0.50-0.91). Regular control campaigns based on breeding-site elimination had no measurable effects on the probabilities of dwelling infestation by dengue vectors. Site-occupancy fluctuated seasonally, mainly due to the negative effects of high maximum (Ae. aegypti) and minimum (Ae. albopictus) summer temperatures (June-September). Rainfall and dwelling-level covariates were poor predictors of occupancy. The marked contrast between our estimates of adult vector presence and the results from ` rapid larval surveys' suggests, together with the lack of effect of local control campaigns on infestation, that many Aedes breeding sites were overlooked by vector control agents in our study setting. Better sampling strategies are urgently needed, particularly for the reliable assessment of infestation rates in the context of control program management. The approach we present here, combining oviposition traps and site-occupancy models, could greatly contribute to that crucial aim. C1 [Padilla-Torres, Samael D.; Ferraz, Goncalo] Inst Nacl de Pesquisas da Amazonia, Grad Program Ecol, Manaus, Amazonas, Brazil. [Ferraz, Goncalo] Inst Nacl de Pesquisas da Amazonia, Smithsonian Trop Res Inst, Biol Dynam Forest Fragments Project, Manaus, Amazonas, Brazil. [Luz, Sergio L. B.; Zamora-Perea, Elvira; Abad-Franch, Fernando] Inst Leonidas & Maria Deane Fiocruz Amazonia, Manaus, Amazonas, Brazil. RP Abad-Franch, F (reprint author), Inst Leonidas & Maria Deane Fiocruz Amazonia, Manaus, Amazonas, Brazil. EM fernando@amazonia.fiocruz.br RI Ferraz, Goncalo/C-3860-2008; Abad-Franch, Fernando/L-4741-2013 OI Ferraz, Goncalo/0000-0001-8748-0462; FU PDTSP-Dengue Program (Fiocruz-CNPq); Instituto Leonidas e Maria Deane; Fiocruz-Fapeam agreement; Brazilian National Research Council (CAPES/CNPq) [190023/10-4]; Research Program on Infectious Disease Ecology in the Amazon (RP-IDEA) of the Instituto Leonidas e Maria Deane - Fiocruz Amazonia [17] FX Research partially funded by the PDTSP-Dengue Program (Fiocruz-CNPq), the Instituto Leonidas e Maria Deane, the Fiocruz-Fapeam agreement, and the Brazilian National Research Council (CAPES/CNPq; scholarship 190023/10-4 to SDP-T). The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript.; We thank RM Mota, DLN Leite, and AC Barbosa for field assistance. RS Rocha and the Manaus municipal and state Health Departments provided data on routine control-surveillance activities. We particularly thank the residents who participated in the study - and patiently let us keep running our vector monitoring system. SA Juliano, LL Bailey, RE Gurtler, and BW Nelson provided insightful comments on earlier versions of this manuscript. This work is contribution number 17 of the Research Program on Infectious Disease Ecology in the Amazon (RP-IDEA) of the Instituto Leonidas e Maria Deane - Fiocruz Amazonia. NR 60 TC 5 Z9 5 U1 6 U2 51 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 MAR 5 PY 2013 VL 8 IS 3 AR e58420 DI 10.1371/journal.pone.0058420 PG 11 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 099RC UT WOS:000315637900140 PM 23472194 ER PT J AU Wang, BB Luo, TM Tadesse, S Tardif, S Ross, C Schulkin, J Power, M Rosen, T Norwitz, E AF Wang, Bingbing Luo, Tianmeng Tadesse, Serkalem Tardif, Suzette Ross, Corinna Schulkin, Jay Power, Michael Rosen, Todd Norwitz, Errol TI Expression of CRH and CRH Regulating Proteins in Placentas of Non-Human Primates SO REPRODUCTIVE SCIENCES LA English DT Meeting Abstract CT 60th Annual Scientific Meeting of the Society-for-Gynecologic-Investigation (SGI) CY MAR 20-23, 2013 CL Orlando, FL SP Soc Gynecol Invest C1 [Luo, Tianmeng; Tadesse, Serkalem; Norwitz, Errol] Tufts Univ, Boston, MA 02111 USA. [Wang, Bingbing; Rosen, Todd] UMDNJ, Robert Wood Johnson Med Sch, New Brunswick, NJ USA. [Schulkin, Jay] Univ Washington, Seattle, WA 98195 USA. [Tardif, Suzette; Ross, Corinna; Power, Michael] UT Hlth Sci Ctr, San Antonio, TX USA. Smithsonian Conservat Biol Inst, Conservat Ecol Ctr, Washington, DC USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU SAGE PUBLICATIONS INC PI THOUSAND OAKS PA 2455 TELLER RD, THOUSAND OAKS, CA 91320 USA SN 1933-7191 EI 1933-7205 J9 REPROD SCI JI Reprod. Sci. PD MAR PY 2013 VL 20 IS S3 SU 3 BP 136A EP 136A PG 1 WC Obstetrics & Gynecology; Reproductive Biology SC Obstetrics & Gynecology; Reproductive Biology GA 287LK UT WOS:000329543100249 ER PT J AU Annan, A Baldwin, HJ Corman, VM Klose, SM Owusu, M Nkrumah, EE Badu, EK Anti, P Agbenyega, O Meyer, B Oppong, S Sarkodie, YA Kalko, EKV Lina, PHC Godlevska, EV Reusken, C Seebens, A Gloza-Rausch, F Vallo, P Tschapka, M Drosten, C Drexler, JF AF Annan, Augustina Baldwin, Heather J. Corman, Victor Max Klose, Stefan M. Owusu, Michael Nkrumah, Evans Ewald Badu, Ebenezer Kofi Anti, Priscilla Agbenyega, Olivia Meyer, Benjamin Oppong, Samuel Sarkodie, Yaw Adu Kalko, Elisabeth K. V. Lina, Peter H. C. Godlevska, Elena V. Reusken, Chantal Seebens, Antje Gloza-Rausch, Florian Vallo, Peter Tschapka, Marco Drosten, Christian Drexler, Jan Felix TI Human Betacoronavirus 2c EMC/2012-related Viruses in Bats, Ghana and Europe SO EMERGING INFECTIOUS DISEASES LA English DT Article ID ACUTE RESPIRATORY SYNDROME; CORONAVIRUSES AB We screened fecal specimens of 4,758 bats from Ghana and 272 bats from 4 European countries for betacoronaviruses. Viruses related to the novel human betacoronavirus EMC/2012 were detected in 46 (24.9%) of 185 Nycteris bats and 40 (14.7%) of 272 Pipistrellus bats. Their genetic relatedness indicated EMC/2012 originated from bats. C1 [Annan, Augustina; Owusu, Michael] Kumasi Ctr Collaborat Res Trop Med, Kumasi, Ghana. [Baldwin, Heather J.] Macquarie Univ, Sydney, NSW 2109, Australia. [Baldwin, Heather J.; Klose, Stefan M.; Kalko, Elisabeth K. V.; Vallo, Peter; Tschapka, Marco] Univ Ulm, D-89069 Ulm, Germany. [Corman, Victor Max; Meyer, Benjamin; Gloza-Rausch, Florian; Drosten, Christian; Drexler, Jan Felix] Univ Bonn, Med Ctr, Bonn, Germany. [Nkrumah, Evans Ewald; Badu, Ebenezer Kofi; Anti, Priscilla; Agbenyega, Olivia; Oppong, Samuel; Sarkodie, Yaw Adu] Kwame Nkrumah Univ Sci & Technol, Kumasi, Ghana. [Kalko, Elisabeth K. V.; Tschapka, Marco] Smithsonian Trop Res Inst, Balboa, Panama. [Lina, Peter H. C.] Nat Biodivers Ctr, Leiden, Netherlands. [Godlevska, Elena V.] Schmalhausen Inst Zool, Kiev, Ukraine. [Reusken, Chantal] Netherlands Ctr Infect Dis Control, Bilthoven, Netherlands. [Seebens, Antje; Gloza-Rausch, Florian] Ctr Bat Protect & Informat, Noctalis, Bad Segeberg, Germany. [Vallo, Peter] Acad Sci Czech Republic, Vvi, Brno, Czech Republic. RP Drexler, JF (reprint author), Univ Bonn, Inst Virol, Med Ctr, D-53127 Bonn, Germany. EM drexler@virology-bonn.de RI Drexler, Jan Felix/C-1004-2014; Vallo, Peter/F-9650-2014; Godlevska, Lena/O-4131-2016; Meyer, Bernhard/Q-9413-2016; OI Godlevska, Lena/0000-0001-6792-6543; Owusu, Michael/0000-0001-5066-150X; Corman, Victor Max/0000-0002-3605-0136 FU European Union [223498, 278976]; German Research Foundation (DFG) [DR 772/3-1, KA1241/18-1] FX This study was supported by the European Union FP7 projects EMPERIE (contract number 223498) and ANTIGONE (contract number 278976) and by the German Research Foundation (DFG grant DR 772/3-1, KA1241/18-1). NR 15 TC 130 Z9 131 U1 4 U2 32 PU CENTERS DISEASE CONTROL PI ATLANTA PA 1600 CLIFTON RD, ATLANTA, GA 30333 USA SN 1080-6040 EI 1080-6059 J9 EMERG INFECT DIS JI Emerg. Infect. Dis PD MAR PY 2013 VL 19 IS 3 BP 456 EP 459 DI 10.3201/eid1903.121503 PG 4 WC Immunology; Infectious Diseases SC Immunology; Infectious Diseases GA 268LU UT WOS:000328173000014 PM 23622767 ER PT J AU Harris, AJ Wen, J Xiang, QY AF Harris, A. J. Wen, Jun Xiang, Qiu-Yun (Jenny) TI Inferring the biogeographic origins of inter-continental disjunct endemics using a Bayes-DIVA approach SO JOURNAL OF SYSTEMATICS AND EVOLUTION LA English DT Review DE arcto-Tertiary; biogeography; disjunction; endemic species; Northern Hemisphere; RASP; S-DIVA; temperate forest ID DISPERSAL-VICARIANCE ANALYSIS; EASTERN NORTH-AMERICA; HISTORICAL BIOGEOGRAPHY; SEQUENCE DATA; LAND-BRIDGE; FLORISTIC DISJUNCTION; MITOCHONDRIAL GENOMES; MOLECULAR PHYLOGENY; GEOGRAPHIC RANGE; TEMPERATE PLANTS AB The arcto-Tertiary relictual flora is comprised of many genera that occur non-contiguously in the temperate zones of eastern Asia, Europe, eastern North America, and western North America. Within each distributional area, species are typically endemic and may thus be widely separated from closely related species within the other areas. It is widely accepted that this common pattern of distribution resulted from of the fragmentation of a once more-continuous arcto-Tertiary forest. The historical biogeographic events leading to the present-day disjunction have often been investigated using a phylogenetic approach. Limitations to these previous studies have included phylogenetic uncertainty and uncertainty in ancestral range reconstructions. However, the recently described Bayes-DIVA method handles both types of uncertainty. Thus, we used Bayes-DIVA analysis to reconstruct the stem lineage distributions for 185 endemic lineages from 23 disjunct genera representing 17 vascular plant families. In particular, we asked whether endemic lineages within each of the four distributional areas more often evolved from (1) widespread ancestors, (2) ancestors dispersed from other areas, or (3) endemic ancestors. We also considered which of these three biogeographic mechanisms may best explain the origins of arcto-Tertiary disjunct endemics in the neotropics. Our results show that eastern Asian endemics more often evolved from endemic ancestors compared to endemics in Europe and eastern and western North America. Present-day endemic lineages in the latter areas more often arose from widespread ancestors. Our results also provide anecdotal evidence for the importance of dispersal in the biogeographic origins of arcto-Tertiary species endemic in the neotropics. C1 [Harris, A. J.] Oklahoma State Univ, Dept Bot, Stillwater, OK 74078 USA. [Wen, Jun] Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, Washington, DC 20013 USA. [Xiang, Qiu-Yun (Jenny)] N Carolina State Univ, Dept Plant Biol, Raleigh, NC 27695 USA. RP Harris, AJ (reprint author), Oklahoma State Univ, Dept Bot, Stillwater, OK 74078 USA. EM aj.harris@okstate.edu; jenny_xiang@ncsu.edu FU NSF [DEB-0444125]; CAS/SAFEA International Partnership Program for Creative Research Teams FX We are highly indebted to Peter FRITSCH (California Academy of Sciences, USA) and Andrew SCHNABEL (Indiana University South Bend, USA) for providing data. We also gratefully acknowledge Yu YAN (Sichuan University, China) and Linda WATSON (Oklahoma State University, USA) for helpful discussion on methodology and manuscript preparation, respectively. We would like to thank Mark FISHBEIN, Angela REIN, and Ben HAACK (all three at Oklahoma State University), as well as two anonymous reviewers for their assistance in improving the manuscript. The work has benefited from a former NSF grant (Grant No. DEB-0444125) and a CAS/SAFEA International Partnership Program for Creative Research Teams. NR 135 TC 21 Z9 23 U1 2 U2 26 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1674-4918 EI 1759-6831 J9 J SYST EVOL JI J. Syst. Evol. PD MAR PY 2013 VL 51 IS 2 BP 117 EP 133 DI 10.1111/jse.12007 PG 17 WC Plant Sciences SC Plant Sciences GA 227QH UT WOS:000325127900001 ER PT J AU Shi, WT Wen, J Lutz, S AF Shi, Wenting Wen, Jun Lutz, Susan TI Pollen morphology of the Maddenia clade of Prunus and its taxonomic and phylogenetic implications SO JOURNAL OF SYSTEMATICS AND EVOLUTION LA English DT Article DE Laurocerasus; Maddenia; Padus; pollen morphology; Prunus; Pygeum ID ROSACEAE; SEQUENCES AB Maddenia (Rosaceae) was long recognized as a distinct genus closely related to Prunus and was recently merged with the latter. The Maddenia clade of Prunus has been revised taxonomically with four species from eastern Asia recognized. Recent molecular studies have provided evidence that this group is nested within Prunus, having a close relationship with the Padus-Laurocerasus complex. To further test the phylogenetic position of Maddenia, this study investigates pollen morphology of all former Maddenia species and 28 other Prunus species, using scanning electron microscopy and light microscopy. The Prunus species sampled here represent major subgenera: Amygdalus, Cerasus, Laurocerasus, Padus, and Prunus s.s. We found that pollen grains of these groups are all monad and tricolporate with striate or rugulate sculpturing. The pollen evidence supports a close relationship between Maddenia and species of Padus and Laurocerasus subgroups (excluding the Pygeum group), all of which have elongated, thicker, and less directional muri. Pollen of the subgenera of Cerasus, Amygdalus, and Prunus has generally thinner, highly directional, and predominantly parallel muri. The pollen grains of the Pygeum subgroup are quite distinct from the other groups of Prunus. Pygeum pollen has rugulate exines with much shorter and rod-shaped muri. C1 [Shi, Wenting; Wen, Jun; Lutz, Susan] Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, Washington, DC 20013 USA. RP Wen, J (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, MRC 166, Washington, DC 20013 USA. EM wenj@si.edu FU NSF [0515431]; Smithsonian Endowment Grant Program FX This study was derived from an undergraduate research internship project at the National Museum of Natural History of the Smithsonian Institution, through the Washington Program at University of California, Davis. We thank Professor Dan POTTER (UC, Davis) for his encouragement and support for the internship project, Siew-Wai CHIN (UC, Davis) for providing the parsimonious tree, and Limin LU (Institute of Botany, Chinese Academy of Sciences), Scott WHITTAKER (SEM Lab, Smithsonian Institution) and Stanley YANKOWSKI (Botany Dept., Smithsonian Institution) for technical assistance. The Prunus systematic studies were supported by NSF Award number 0515431 and the Smithsonian Endowment Grant Program. NR 31 TC 6 Z9 6 U1 1 U2 8 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1674-4918 J9 J SYST EVOL JI J. Syst. Evol. PD MAR PY 2013 VL 51 IS 2 BP 164 EP 183 DI 10.1111/j.1759-6831.2012.00233.x PG 20 WC Plant Sciences SC Plant Sciences GA 227QH UT WOS:000325127900005 ER PT J AU Petchey, F Ulm, S David, B McNiven, IJ Asmussen, B Tomkins, H Dolby, N Aplin, K Richards, T Rowe, C Leavesley, M Mandui, H AF Petchey, Fiona Ulm, Sean David, Bruno McNiven, Ian J. Asmussen, Brit Tomkins, Helene Dolby, Nic Aplin, Ken Richards, Thomas Rowe, Cassandra Leavesley, Matthew Mandui, Herman TI High-resolution radiocarbon dating of marine materials in archaeological contexts: radiocarbon marine reservoir variability between Anadara, Gafrarium, Batissa, Polymesoda spp. and Echinoidea at Caution Bay, Southern Coastal Papua New Guinea SO ARCHAEOLOGICAL AND ANTHROPOLOGICAL SCIENCES LA English DT Article DE Radiocarbon; Marine reservoir correction; Gafarium; Anadara; Polymesoda; Caution Bay; Batissa; Echinoidea; Lapita ID DELTA-R VALUES; OXYGEN-ISOTOPE VARIATION; SOUTHWEST PACIFIC-OCEAN; AGE CALIBRATION; C-14; MOLLUSKS; ISLAND; RECORD; CARBON; REEF AB The remains of shellfish dominate many coastal archaeological sites in the Pacific and provide a wealth of information about economy, culture, environment and climate. Shells are therefore the logical sample type to develop local and regional radiocarbon chronologies. The calibration of radiocarbon (C-14) dates on marine animals is not straightforward, however, requiring an understanding of habitat and dietary preferences as well as detailed knowledge of local ocean conditions. The most complex situations occur where terrestrial influences impinge on the marine environment resulting in both the enrichment and depletion of C-14 (Ulm Geoarchaeology 17(4):319-348, 2002; Petchey and Clark Quat Geochronol 6:539-549, 2011). A sampling protocol that combines a high-resolution excavation methodology, selection of short-lived samples identified to species level, and a tri-isotope approach using C-14, delta C-13 and delta O-18, has given us the ability to identify C-14 source variation that would otherwise have been obscured. Here, we present new research that details high-resolution mapping of marine C-14 reservoir variation between Gafrarium tumidum, Gafrarium pectinatum, Anadara granosa, Anadara antiquata, Batissa violacea, Polymesoda erosa and Echinoidea fromthe Bogi 1 archaeological site, Caution Bay, southern coastal Papua New Guinea. These isotopes highlight specific dietary, habitat and behavioural variations that are key to obtaining chronological information from shell radiocarbon determinations. C1 [Petchey, Fiona] Univ Waikato, Waikato Radiocarbon Dating Lab, Hamilton, New Zealand. [Ulm, Sean; Tomkins, Helene] James Cook Univ, Sch Arts & Social Sci, Dept Anthropol Archaeol & Sociol, Cairns, Qld 4870, Australia. [David, Bruno; McNiven, Ian J.; Dolby, Nic; Richards, Thomas; Rowe, Cassandra] Monash Univ, Sch Geog & Environm Sci, Clayton, Vic 3800, Australia. [Asmussen, Brit] Queensland Museum, South Brisbane, Qld 4101, Australia. [Aplin, Ken] Natl Museum Nat Hist, Smithsonian Inst, Washington, DC 20013 USA. [Leavesley, Matthew] Univ Papua New Guinea, Port Moresby, NCD, Papua N Guinea. [Mandui, Herman] Natl Museum & Art Gallery Papua New Guinea, Boroko, NCD, Papua N Guinea. RP Petchey, F (reprint author), Univ Waikato, Waikato Radiocarbon Dating Lab, Private Bag 3240, Hamilton, New Zealand. EM f.petchey@waikato.ac.nz; sean.ulm@jcu.edu.au; bruno.david@monash.edu; ian.mcniven@monash.edu; brit.asmussen@qm.qld.gov.au; helen.tomkins@my.jcu.edu.au; nicdolby@gmail.com; thomas.richards@monash.edu; cassandra.rowe@monash.edu; matthew.leavesley@gmail.com RI James Cook University, TESS/B-8171-2012; Ulm, Sean/A-3854-2010; Rowe, Cassandra/M-6009-2015; OI Ulm, Sean/0000-0001-6653-9963; Rowe, Cassandra/0000-0001-8938-5733; Asmussen, Brit/0000-0001-8443-1892; David, Bruno/0000-0002-8567-6135 FU Australian Research Council; QEII Fellowship [DP0877782]; Australian Research Council [FT120100656] FX We wish to thank: Thomas Samson for ethnographic information. Mr Sese Kevau, Mr Vagi Daure, Ms Daro Daroa for their expertise in local shellfish information. BD thanks the Australian Research Council for grant and QEII Fellowship DP0877782. SU is the recipient of an Australian Research Council Future Fellowship (project number FT120100656). NR 71 TC 11 Z9 11 U1 0 U2 11 PU SPRINGER HEIDELBERG PI HEIDELBERG PA TIERGARTENSTRASSE 17, D-69121 HEIDELBERG, GERMANY SN 1866-9557 EI 1866-9565 J9 ARCHAEOL ANTHROP SCI JI Archaeol. Anthropol. Sci. PD MAR PY 2013 VL 5 IS 1 BP 69 EP 80 DI 10.1007/s12520-012-0108-1 PG 12 WC Anthropology; Archaeology; Geosciences, Multidisciplinary SC Anthropology; Archaeology; Geology GA 223VT UT WOS:000324840400005 ER PT J AU Tarr, K Shay, W AF Tarr, Kimberly Shay, Wendy TI How Film (and Video) Found Its Way into "Our Nation's Attic": A Conversation about the Origins of Audiovisual Collecting and Archiving at the Smithsonian Institution SO MOVING IMAGE LA English DT Editorial Material C1 [Shay, Wendy] Smithsonian Inst, Natl Museum Amer Hist, Arch Ctr, Washington, DC 20560 USA. RP Tarr, K (reprint author), NYU, Audiovisual Preservat Program, New York, NY 10003 USA. NR 3 TC 0 Z9 0 U1 0 U2 1 PU UNIV MINNESOTA PRESS PI MINNEAPOLIS PA MILL PLACE, SUITE 290 111 THIRD AVE S, MINNEAPOLIS, MN 55401-2520 USA SN 1532-3978 J9 MOV IMAGE JI Mov. Image PD SPR PY 2013 VL 13 IS 1 BP 178 EP 184 PG 7 WC Film, Radio, Television SC Film, Radio & Television GA 211NI UT WOS:000323914600008 ER PT J AU Frodeman, R Holbrook, JB Bourexis, PS Cook, SB Diederick, L Tankersley, RA AF Frodeman, Robert Holbrook, J. Britt Bourexis, Patricia S. Cook, Susan B. Diederick, Laura Tankersley, Richard A. TI Broader Impacts 2.0: Seeing-and Seizing-the Opportunity SO BIOSCIENCE LA English DT Editorial Material C1 [Frodeman, Robert; Holbrook, J. Britt] Univ N Texas, Ctr Study Interdisciplinar, Denton, TX 76203 USA. [Bourexis, Patricia S.] Study Grp, Kill Devil Hills, NC USA. [Cook, Susan B.] Indian River State Coll, Ctr Ocean Sci Educ Excellence Florida, Ft Pierce, FL USA. [Diederick, Laura] Smithsonian Marine Stn, Ft Pierce, FL USA. [Tankersley, Richard A.] Florida Inst Technol, Dept Biol Sci, Melbourne, FL 32901 USA. RP Tankersley, RA (reprint author), Florida Inst Technol, Dept Biol Sci, Melbourne, FL 32901 USA. EM rtankers@fit.edu RI Holbrook, J. Britt/C-6813-2011 OI Holbrook, J. Britt/0000-0002-5804-0692 NR 0 TC 5 Z9 5 U1 0 U2 8 PU AMER INST BIOLOGICAL SCI PI WASHINGTON PA 1444 EYE ST, NW, STE 200, WASHINGTON, DC 20005 USA SN 0006-3568 J9 BIOSCIENCE JI Bioscience PD MAR PY 2013 VL 63 IS 3 BP 153 EP 154 DI 10.1525/bio.2013.63.3.2 PG 2 WC Biology SC Life Sciences & Biomedicine - Other Topics GA 186MI UT WOS:000322048200002 ER PT J AU Zapico, SC Ubelaker, DH AF Zapico, Sara C. Ubelaker, Douglas H. TI Applications of physiological bases of ageing to forensic sciences. Estimation of age-at-death SO AGEING RESEARCH REVIEWS LA English DT Review DE Age estimation; Ageing; Chemical methods; Aspartic acid racemization; Molecular biology methods; DNA mutations ID ASPARTIC-ACID RACEMIZATION; HUMAN MITOCHONDRIAL-DNA; 3RD MOLAR DEVELOPMENT; GLYCATION END-PRODUCTS; COLLAGEN CROSS-LINKING; PULP/TOOTH AREA RATIO; HUMAN CORTICAL BONE; HUMAN LENS PROTEINS; FREE-RADICAL THEORY; HUMAN ROOT DENTIN AB Age-at-death estimation is one of the main challenges in forensic sciences since it contributes to the identification of individuals. There are many anthropological techniques to estimate the age at death in children and adults. However, in adults this methodology is less accurate and requires population specific references. For that reason, new methodologies have been developed. Biochemical methods are based on the natural process of ageing, which induces different biochemical changes that lead to alterations in cells and tissues. In this review, we describe different attempts to estimate the age in adults based on these changes. Chemical approaches imply modifications in molecules or accumulation of some products. Molecular biology approaches analyze the modifications in DNA and chromosomes. Although the most accurate technique appears to be aspartic acid racemization, it is important to take into account the other techniques because the forensic context and the human remains available will determine the possibility to apply one or another methodology. (C) 2013 Elsevier B.V. All rights reserved. C1 [Zapico, Sara C.; Ubelaker, Douglas H.] Natl Museum Nat Hist, Smithsonian Inst, Dept Anthropol, MRC 112, Washington, DC 20013 USA. RP Zapico, SC (reprint author), Natl Museum Nat Hist, Smithsonian Inst, Dept Anthropol, MRC 112, 10th & Constitut Ave,NW,POB 37012, Washington, DC 20013 USA. EM Casado-ZapicoS@si.edu FU Smithsonian Institution FX Sara C. Zapico is supported by a Peter Buck Postdoctoral Fellowship from the Smithsonian Institution. NR 191 TC 8 Z9 9 U1 3 U2 39 PU ELSEVIER IRELAND LTD PI CLARE PA ELSEVIER HOUSE, BROOKVALE PLAZA, EAST PARK SHANNON, CO, CLARE, 00000, IRELAND SN 1568-1637 EI 1872-9649 J9 AGEING RES REV JI Ageing Res. Rev. PD MAR PY 2013 VL 12 IS 2 BP 605 EP 617 DI 10.1016/j.arr.2013.02.002 PG 13 WC Cell Biology; Geriatrics & Gerontology SC Cell Biology; Geriatrics & Gerontology GA 175LX UT WOS:000321233300013 ER PT J AU Sheehy, D AF Sheehy, Daniel TI Music of Latin America and the Caribbean SO LATIN AMERICAN MUSIC REVIEW-REVISTA DE MUSICA LATINOAMERICANA LA English DT Book Review C1 [Sheehy, Daniel] Smithsonian Inst, Washington, DC 20560 USA. RP Sheehy, D (reprint author), Smithsonian Inst, Washington, DC 20560 USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU UNIV TEXAS PRESS PI AUSTIN PA JOURNAL DIV, 2100 COMAL, AUSTIN, TX 78722 USA SN 0163-0350 J9 LAT AM MUSIC REV JI Lat. Am. Music Rev.-Rev. Music Latinoam. PD SPR-SUM PY 2013 VL 34 IS 1 BP 114 EP 116 PG 3 WC Music SC Music GA 178WQ UT WOS:000321478500006 ER PT J AU Fowler, AE Forsstrom, T von Numers, M Vesakoski, O AF Fowler, Amy E. Forsstrom, Tiia von Numers, Mikael Vesakoski, Outi TI The North American mud crab Rhithropanopeus harrisii (Gould, 1841) in newly colonized Northern Baltic Sea: distribution and ecology SO AQUATIC INVASIONS LA English DT Article DE Xanthidae; Finland; biological invasion; introduced species; demography ID LARVAL DEVELOPMENT; MONDEGO-RIVER; ODRA ESTUARY; TEMPERATURE; POPULATION; SALINITY; TRIDENTATUS; PORTUGAL; DECAPODA; BIOLOGY AB Here we present the known distribution and population demography of the most northern known population of the North American white-fingered mud crab, Rhithropanopeus harrisii, from southwest Finland in the Baltic Sea. This species was first reported in Finland in 2009 from the archipelago close to Turku and has been found from 82 locations within a 30 km radius since then. Due to the presence of young of year, juveniles, and gravid females observed at three sites in Finland, R. harrisii has established successful populations that are able to overwinter under ice and can opportunistically occupy diverse habitats, such as shafts of dead marsh plants, self-made burrows in muddy bottoms, and the brown algae Fucus vesiculosus in hard bottoms. In its native range, a rhizocephalan barnacle parasitizes R. harrisii, but this parasite was not found in the introduced Finnish population. While R. harrisii is expected to expand its range along the coast of the northern Baltic Sea, the ultimate impact of this species on food web dynamics, both as a predator and prey item, remains to be seen. C1 [Fowler, Amy E.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. [Fowler, Amy E.] Villanova Univ, Dept Biol, Villanova, PA 19085 USA. [Forsstrom, Tiia; Vesakoski, Outi] Univ Turku, Dept Biol, FIN-20014 Turku, Finland. [von Numers, Mikael] Abo Akad Univ, Dept Biosci Environm & Marine Biol, FI-20520 Turku, Finland. [Vesakoski, Outi] Univ Turku, Finland Archipelago Res Inst, FI-20014 Turku, Finland. RP Fowler, AE (reprint author), Smithsonian Environm Res Ctr, POB 28, Edgewater, MD 21037 USA. EM amy.fowler@villanova.edu; ttfors@utu.fi; mnumers@abo.fi; Outi.Vesakoski@utu.fi RI Forsstrom, Tiia/B-8288-2014 OI Forsstrom, Tiia/0000-0001-8407-0994 FU Global Invasions Network; National Science Foundation FX We are grateful to Henry Hellstrom and Ville Peltonen for providing us with crabs, Riikka Puntila from Finnish Game and Fishery Research Institute for providing data from public webpages, and Maiju Lehtiniemi and Tarja Katajisto for cooperation during summer 2011 and for planning future studies of R. harrisii ecology in Finland. Pauli Huunonen and Olavi Sahlsten kindly provided their observations. AF would also like to thank her two postdoctoral advisors at the Smithsonian Environmental Research Center, Greg Ruiz and Whitman Miller, for their suggestions, advice, and support on this project. We are also grateful to the two anonymous reviewers and the editor, Mark Hanson, for their comments. A Research Coordination Network grant funded by the Global Invasions Network, with support from the National Science Foundation, was awarded to AF for this research. NR 32 TC 13 Z9 14 U1 0 U2 33 PU REGIONAL EURO-ASIAN BIOLOGICAL INVASIONS CENTRE-REABIC PI HELSINKI PA PL 3, HELSINKI, 00981, FINLAND SN 1798-6540 J9 AQUAT INVASIONS JI Aquat. Invasions PD MAR PY 2013 VL 8 IS 1 BP 89 EP 96 DI 10.3391/ai.2013.8.1.10 PG 8 WC Ecology; Marine & Freshwater Biology SC Environmental Sciences & Ecology; Marine & Freshwater Biology GA 172IN UT WOS:000320995600010 ER PT J AU Shen, XL Li, S Chen, N Li, SZ McShea, WJ Lu, Z AF Shen, Xiaoli Li, Sheng Chen, Nyima Li, Shengzhi McShea, William J. Lu, Zhi TI Does science replace traditions? Correlates between traditional Tibetan culture and local bird diversity in Southwest China (vol 145, pg 160, 2012) SO BIOLOGICAL CONSERVATION LA English DT Correction C1 [Shen, Xiaoli; Li, Sheng; Lu, Zhi] Peking Univ, Sch Life Sci, Ctr Nat & Soc, Beijing 100871, Peoples R China. [Chen, Nyima; Li, Shengzhi; Lu, Zhi] Shan Shui Conservat Ctr, Beijing 100871, Peoples R China. [Shen, Xiaoli; McShea, William J.] Natl Zool Pk, Smithsonian Conservat Biol Inst, Front Royal, VA 22630 USA. RP Shen, XL (reprint author), Natl Zool Pk, Smithsonian Conservat Biol Inst, 1500 Remount Rd, Front Royal, VA 22630 USA. EM xlshen.pku@gmail.com NR 1 TC 0 Z9 0 U1 2 U2 7 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 0006-3207 J9 BIOL CONSERV JI Biol. Conserv. PD MAR PY 2013 VL 159 BP 553 EP 553 DI 10.1016/j.biocon.2013.03.001 PG 1 WC Biodiversity Conservation; Ecology; Environmental Sciences SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 160DF UT WOS:000320096300066 ER PT J AU Hendy, AJW AF Hendy, Austin J. W. TI SPATIAL AND STRATIGRAPHIC VARIATION OF MARINE PALEOENVIRONMENTS IN THE MUDDLE-UPPER MIOCENE GATUN FORMATION, ISTHMUS OF PANAMA SO PALAIOS LA English DT Article ID FAUNAL GRADIENT ANALYSIS; SERIES UPPER ORDOVICIAN; NEW-ZEALAND; SEQUENCE STRATIGRAPHY; CINCINNATIAN SERIES; SOUTH-AMERICA; TARANAKI BASINS; NEOGENE; DIVERSITY; WANGANUI AB The middle-upper Miocene (Serravallian-Tortonian) Gatun Formation of Panama is one of the most diverse marine fossil assemblages in the Caribbean, and has been widely used as a baseline in studies investigating the effects of the late Neogene closure of the Central American Seaway. Despite being the focus of exhaustive paleoecological sampling studies, previous studies have not revealed the fine-scale spatial and temporal variation in the composition of the Gatun fauna. High-resoluton faunal inventories were conducted from over 600 stratigraphic horizons in the Gatun Formation, capturing more than 200 species, which represent mostly widespread or common, and typically macroscopic taxa. Cluster and detrended correspondence analyses (DCA) reveal a stratigraphic pattern of variation in the faunal composition of individual horizons as well as differences between sampling sites. Stratigraphic curves of DCA axis scores indicate relative shifts in water depth and sedimentation through the stratigraphy and among localities. Overall the Gatun reveals both coarse- and fine-scale temporal variations in paleobathymetry, reflecting long-term shifts in basin subsidence and accommodation space that is potentially overprinted by fifth- or sixth-order glacio-eustatic cycles. The formation accumulated during an overall phase of increasing accommodation space, with major intervals of transgression (lower Gatun), regression (middle Gatun), and further transgression to mid-shelf depths (upper Gatun). Shallowing through the middle part of the Gatun is largely the result of an increase in supply of pyroclastic and volcaniclastic sediments from the adjacent volcanic arc. These findings have implications for understanding the tectonic evolution of the Canal Basin. C1 [Hendy, Austin J. W.] Smithsonian Trop Res Inst, Ctr Trop Paleontol & Archaeol, Panama City, Panama. [Hendy, Austin J. W.] Univ Florida, Florida Museum Nat Hist, Gainesville, FL 32611 USA. RP Hendy, AJW (reprint author), Smithsonian Trop Res Inst, Ctr Trop Paleontol & Archaeol, Panama City, Panama. EM ahendy@flmnh.ufl.edu FU U.S. National Science Foundation (NSF) [0966884] FX This work was funded by U.S. National Science Foundation (NSF) grant 0966884 (International Science and Engineering [OISE], Division of Earth Sciences [EAR], Research on Learning in Formal and Informal Settings [DRL], the Smithsonian Institution, and the Autoridad del Canal de Panama (ACP). I appreciate the encouragement of C. Jaramillo and the Smithsonian Tropical Research Institute in undertaking this research. I am grateful for the assistance of J.D. Carrillo Sanchez, G. Gerado, K. Hendy, J.C. Moreno, J. Ortiz, A. Rojas-Briceno, and M.C. Vallejo in the measurement of stratigraphic sections and collection of field data. The ACP are thanked for providing safe access to the Atlantic Locks excavation site, and making available core material for inspection. Ricardo Perez is acknowledged for donating the Toyota vehicles used for fieldwork, and the Direccion de Recursos Minerales are thanked for providing collecting permits. This is a contribution of the NSF Partnerships for International Research and Education Panama Canal Project. NR 79 TC 12 Z9 13 U1 0 U2 9 PU SEPM-SOC SEDIMENTARY GEOLOGY PI TULSA PA 6128 EAST 38TH ST, STE 308, TULSA, OK 74135-5814 USA SN 0883-1351 J9 PALAIOS JI Palaios PD MAR-APR PY 2013 VL 28 IS 3-4 BP 210 EP 227 DI 10.2110/palo.2012.p12-024r PG 18 WC Geology; Paleontology SC Geology; Paleontology GA 168AW UT WOS:000320679100007 ER PT J AU Nash, MC Opdyke, BN Troitzsch, U Russell, BD Adey, WH Kato, A Diaz-Pulido, G Brent, C Gardner, M Prichard, J Kline, DI AF Nash, M. C. Opdyke, B. N. Troitzsch, U. Russell, B. D. Adey, W. H. Kato, A. Diaz-Pulido, G. Brent, C. Gardner, M. Prichard, J. Kline, D. I. TI Dolomite-rich coralline algae in reefs resist dissolution in acidified conditions SO NATURE CLIMATE CHANGE LA English DT Article ID OCEAN ACIDIFICATION; MAGNESIAN CALCITES; POLYSACCHARIDE; PRODUCTIVITY; NUCLEATION; CARBONATES; TURBULENT AB Coral reef ecosystems develop best in high-flow environments but their fragile frameworks are also vulnerable to high wave energy. Wave-resistant algal rims, predominantly made up of the crustose coralline algae (CCA) Porolithon onkodes and P. pachydermum(1,2), are therefore critical structural elements for the survival of many shallow coral reefs. Concerns are growing about the susceptibility of CCA to ocean acidification because CCA Mg-calcite skeletons are more susceptible to dissolution under low pH conditions than coral aragonite skeletons(3). However, the recent discovery(4) of dolomite (Mg0.5Ca0.5(CO3)), a stable carbonate(5), in P. onkodes cells necessitates a reappraisal of the impacts of ocean acidification on these CCA. Here we show, using a dissolution experiment, that dried dolomite-rich CCA have 6-10 times lower rates of dissolution than predominantly Mg-calcite CCA in both high-CO2 (similar to 700 ppm) and control (similar to 380 ppm) environments, respectively. We reveal this stabilizing mechanism to be a combination of reduced porosity due to dolomite infilling and selective dissolution of other carbonate minerals. Physical break-up proceeds by dissolution of Mg-calcite walls until the dolomitized cell eventually drops out intact. Dolomite-rich CCA frameworks are common in shallow coral reefs globally and our results suggest that it is likely that they will continue to provide protection and stability for coral reef frameworks as CO2 rises. C1 [Nash, M. C.] Australian Natl Univ, Res Sch Phys, Acton, ACT 0200, Australia. [Opdyke, B. N.; Troitzsch, U.; Brent, C.; Gardner, M.; Prichard, J.] Australian Natl Univ, Res Sch Earth Sci, Acton, ACT 0200, Australia. [Russell, B. D.] Univ Adelaide, Sch Earth & Environm Sci, Southern Seas Ecol Labs, Adelaide, SA 5005, Australia. [Adey, W. H.] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20013 USA. [Kato, A.] Hiroshima Univ, Takehara Fisheries Res Stn, Ctr Educ & Res Field Sci, Hiroshima 7250024, Japan. [Diaz-Pulido, G.] Griffith Univ, Griffith Sch Environm, Nathan, Qld 4111, Australia. [Diaz-Pulido, G.] Griffith Univ, Australian Rivers Inst, Nathan, Qld 4111, Australia. [Kline, D. I.] Univ Calif San Diego, Scripps Inst Oceanog, La Jolla, CA 92093 USA. [Kline, D. I.] Univ Queensland, Sch Biol Sci, Coral Reef Ecosyst Lab, Brisbane, Qld 4072, Australia. RP Nash, MC (reprint author), Australian Natl Univ, Res Sch Phys, GPO Box 4, Acton, ACT 0200, Australia. EM merinda.nash@anu.edu.au RI Kato, Aki/I-2630-2013; OI Kato, Aki/0000-0001-6124-9676; Russell, Bayden/0000-0003-1282-9978 NR 28 TC 37 Z9 37 U1 3 U2 77 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 1758-678X J9 NAT CLIM CHANGE JI Nat. Clim. Chang. PD MAR PY 2013 VL 3 IS 3 BP 268 EP 272 DI 10.1038/NCLIMATE1760 PG 5 WC Environmental Sciences; Environmental Studies; Meteorology & Atmospheric Sciences SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences GA 150NY UT WOS:000319399000023 ER PT J AU Yao, NY Laumann, CR Gorshkov, AV Weimer, H Jiang, L Cirac, JI Zoller, P Lukin, MD AF Yao, N. Y. Laumann, C. R. Gorshkov, A. V. Weimer, H. Jiang, L. Cirac, J. I. Zoller, P. Lukin, M. D. TI Topologically protected quantum state transfer in a chiral spin liquid SO NATURE COMMUNICATIONS LA English DT Article ID SUPERCONDUCTING FLUX QUBIT; POLAR-MOLECULES; NUCLEAR-SPIN; DIAMOND; MEMORY; COMPUTATION; COMPUTERS; CIRCUITS; PHYSICS; ANYONS AB Topology plays a central role in ensuring the robustness of a wide variety of physical phenomena. Notable examples range from the current-carrying edge states associated with the quantum Hall and the quantum spin Hall effects to topologically protected quantum memory and quantum logic operations. Here we propose and analyse a topologically protected channel for the transfer of quantum states between remote quantum nodes. In our approach, state transfer is mediated by the edge mode of a chiral spin liquid. We demonstrate that the proposed method is intrinsically robust to realistic imperfections associated with disorder and decoherence. Possible experimental implementations and applications to the detection and characterization of spin liquid phases are discussed. C1 [Yao, N. Y.; Laumann, C. R.; Weimer, H.; Lukin, M. D.] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. [Laumann, C. R.; Weimer, H.] Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom & Mol Phys, Cambridge, MA 02138 USA. [Gorshkov, A. V.; Jiang, L.] CALTECH, Inst Quantum Informat, Pasadena, CA 91125 USA. [Cirac, J. I.] Max Planck Inst Quantum Opt, D-85748 Garching, Germany. [Zoller, P.] Austrian Acad Sci, Inst Quantum Opt & Quantum Informat, A-6020 Innsbruck, Austria. [Zoller, P.] Univ Innsbruck, Inst Theoret Phys, A-6020 Innsbruck, Austria. RP Yao, NY (reprint author), Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. EM nyao@fas.harvard.edu RI Yao, Norman/A-3929-2009; Gorshkov, Alexey/A-9848-2008; Zoller, Peter/O-1639-2014 OI Yao, Norman/0000-0003-0194-7266; Gorshkov, Alexey/0000-0003-0509-3421; Zoller, Peter/0000-0003-4014-1505 FU NSF; DOE [FG02-97ER25308]; CUA; DARPA; AFOSR MURI; NIST; Lawrence Golub Fellowship; Lee A. DuBridge Foundation; Sherman Fairchild Foundation; IQIM; Gordon and Betty Moore Foundation; National Science Foundation; Smithsonian Astrophysical Observatory; German Academic Exchange Service (DAAD) FX We gratefully acknowledge conversations with T. Kitagawa, S. Bennett, P. Maurer, E. Altman, E. Demler, S. Sachdev, M. Freedman and J. Preskill. This work was supported, in part, by the NSF, DOE (FG02-97ER25308), CUA, DARPA, AFOSR MURI, NIST, Lawrence Golub Fellowship, Lee A. DuBridge Foundation, the Sherman Fairchild Foundation, IQIM and the Gordon and Betty Moore Foundation. H. W. was supported by the National Science Foundation through a grant for the Institute for Theoretical Atomic, Molecular and Optical Physics at Harvard University and the Smithsonian Astrophysical Observatory and by a fellowship within the Postdoc Programme of the German Academic Exchange Service (DAAD). NR 55 TC 15 Z9 15 U1 0 U2 28 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 MAR PY 2013 VL 4 AR 1585 DI 10.1038/ncomms2531 PG 8 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 143NJ UT WOS:000318873900039 PM 23481393 ER PT J AU Flechas, SV Medina, EM Crawford, AJ Sarmiento, C Cardenas, ME Amezquita, A Restrepo, S AF Flechas, S. V. Medina, E. M. Crawford, A. J. Sarmiento, C. Cardenas, M. E. Amezquita, A. Restrepo, S. TI Characterization of the First Batrachochytrium dendrobatidis Isolate from the Colombian Andes, an Amphibian Biodiversity Hotspot SO ECOHEALTH LA English DT Article DE Chytridiomycota; Colombia; Andes; multi-locus genotyping; morphological description ID CHYTRIDIOMYCOSIS; FROG; EXTINCTION; PATHOGEN; DECLINES; BACTERIA; SEQUENCE; AMERICA; DISEASE AB The pathogenic chytrid fungus, Batrachochytrium dendrobatidis (Bd), constitutes a significant threat to more than 790 amphibian species occurring in Colombia. To date there is no molecular or morphological description of strains infecting Colombian populations. Here we report the genetic and morphological characterization of the first Colombian isolate of Bd (strain EV001). Our goals were threefold: (1) to characterize the morphology of EV001 using light and scanning electron microscopy, (2) to genotype this strain by direct sequencing of 17 polymorphic nuclear markers developed previously, and (3) to compare our findings with published reports on strains from other areas of the globe. We found that EV001 is morphologically consistent with previously described strains. Multi-locus genotyping suggested that EV001 is grouped genetically with Panamanian strains and is most similar to strain JEL203 isolated from a captive individual. This finding fills an important gap in our knowledge of Neotropical strains of Bd and provides a baseline for further evolutionary and functional analyses. C1 [Flechas, S. V.; Medina, E. M.; Crawford, A. J.; Sarmiento, C.; Cardenas, M. E.; Amezquita, A.; Restrepo, S.] Univ Los Andes, Dept Biol Sci, Bogota, Colombia. [Crawford, A. J.; Sarmiento, C.] Smithsonian Trop Res Inst, Ancon, Panama. RP Flechas, SV (reprint author), Univ Los Andes, Dept Biol Sci, Carrera 1 18A-10, Bogota, Colombia. EM s-flecha@uniandes.edu.co OI Restrepo, Silvia/0000-0001-9016-1040; Sarmiento, Carolina/0000-0002-8575-7170 FU International Centre for Genetic Engineering and Biotechnology (CRP-ICGEB) [CRP/COL09-01]; Fundacion para la Promocion de la Ciencia y la Tecnologia, Banco de la Republica [2635]; Association of Zoos and Aquariums [CEF 08-836] FX This study was completed with financial support from the International Centre for Genetic Engineering and Biotechnology (CRP-ICGEB) (CRP/COL09-01), the Fundacion para la Promocion de la Ciencia y la Tecnologia, Banco de la Republica (Project No 2635) and the Association of Zoos and Aquariums (CEF 08-836). For assistance in the field we especially thank L. M. Arenas. NR 39 TC 1 Z9 1 U1 0 U2 24 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 1612-9202 J9 ECOHEALTH JI EcoHealth PD MAR PY 2013 VL 10 IS 1 BP 72 EP 76 DI 10.1007/s10393-013-0823-9 PG 5 WC Biodiversity Conservation; Ecology; Environmental Sciences SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 143CM UT WOS:000318843900009 PM 23529763 ER PT J AU Campbell, BA Putzig, NE Carter, LM Morgan, GA Phillips, RJ Plaut, JJ AF Campbell, Bruce A. Putzig, Nathaniel E. Carter, Lynn M. Morgan, Gareth A. Phillips, Roger. J. Plaut, Jeffrey J. TI Roughness and near-surface density of Mars from SHARAD radar echoes SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article DE Mars; radar; topography ID MEDUSAE FOSSAE FORMATION; SCALE ROUGHNESS; MOLA DATA; ICE; SCATTERING; REFLECTIVITY; TOPOGRAPHY; EVOLUTION; GLACIERS; REGION AB We present a technique for estimating Mars topographic roughness on horizontal scales from about 10 m to 100 m using Shallow Radar (SHARAD) sounding data. Our results offer a view of surface properties complementary to Mars Orbiter Laser Altimeter (MOLA) pulse-width or baseline roughness maps and can be compared to SHARAD peak-echo properties to infer deviations from the average near-surface density. Latitudinal averaging of SHARAD-derived roughness over Arabia and Noachis Terrae shows good agreement with MOLA-derived roughness and provides clear evidence for latitude-dependent mantling deposits previously inferred from image data. In northwestern Gordii Dorsum, we find that bulk density in at least the upper few meters is significantly lower than in other units of the Medusae Fossae Formation. We observe the same behavior indicative of low near-surface density in wind-eroded crater fill in the southern highlands. Combining surface-properties analysis, subsurface sounding, and high-resolution optical images, we show that the Pavonis Mons fan-shaped deposit differs significantly from lobate debris aprons which SHARAD has shown to be ice-cored. There are no internal radar reflections from the smooth-facies portion of the Pavonis Mons fan-shaped deposit, and we suggest that these deposits are either quite thin or have little dielectric (i.e., density) contrast with the underlying terrain. Future application of these techniques can identify other low-density units across Mars, assist in the mapping of regional volatile-rich mantling units, and provide new constraints on the physical properties of the polar layered terrain. C1 [Campbell, Bruce A.; Morgan, Gareth A.] Smithsonian Inst, Ctr Earth & Planetary Studies, Washington, DC 20013 USA. [Putzig, Nathaniel E.; Phillips, Roger. J.] SW Res Inst, Boulder, CO USA. [Carter, Lynn M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Plaut, Jeffrey J.] CALTECH, Jet Prop Lab, Pasadena, CA USA. RP Campbell, BA (reprint author), Smithsonian Inst, Ctr Earth & Planetary Studies, MRC 315,POB 37012, Washington, DC 20013 USA. EM campbellb@si.edu RI Carter, Lynn/D-2937-2012 FU NASA Mars Reconnaissance Orbiter project FX The authors thank two anonymous reviewers for their constructive comments. Funding for this work was provided in part by the NASA Mars Reconnaissance Orbiter project. The Shallow Radar (SHARAD) was provided by the Italian Space Agency, and its operations are led by the Department of Information Engineering, Electronics, and Telecommunications, University of Rome "La Sapienza." NR 44 TC 10 Z9 10 U1 1 U2 17 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 MAR PY 2013 VL 118 IS 3 BP 436 EP 450 DI 10.1002/jgre.20050 PG 15 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 134VJ UT WOS:000318243300005 ER PT J AU Wilson, LB Koval, A Sibeck, DG Szabo, A Cattell, CA Kasper, JC Maruca, BA Pulupa, M Salem, CS Wilber, M AF Wilson, L. B., III Koval, A. Sibeck, D. G. Szabo, A. Cattell, C. A. Kasper, J. C. Maruca, B. A. Pulupa, M. Salem, C. S. Wilber, M. TI Shocklets, SLAMS, and field-aligned ion beams in the terrestrial foreshock SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID EARTHS BOW SHOCK; AMPLITUDE MAGNETIC-STRUCTURES; QUASI-PARALLEL SHOCKS; LOW-FREQUENCY WAVES; UPSTREAM SOLAR-WIND; ISEE-2 OBSERVATIONS; SUPRATHERMAL IONS; REFLECTED IONS; RE-FORMATION; PLASMA AB We present Wind spacecraft observations of ion distributions showing field-aligned beams (FABs) and large-amplitude magnetic fluctuations composed of a series of shocklets and short large-amplitude magnetic structures (SLAMS). The FABs are found to have T-b similar to 80 - 850 eV, V-b/V-sw similar to 1.3 - 2.4, T-perpendicular to,T-b/T-parallel to,T-b similar to 1-8, and n(b)/n(o) similar to 0.2-11%. Saturation amplitudes for ion/ion resonant and non-resonant instabilities are too small to explain the observed SLAMS amplitudes. We show two examples where groups of SLAMS can act like a local quasi-perpendicular shock reflecting ions to produce the FABs, a scenario distinct from the more common production at the quasi-perpendicular bow shock. The SLAMS exhibit a foot-like magnetic enhancement with a leading magnetosonic whistler train, consistent with previous observations. Strong ion and electron heating are observed within the series of shocklets and SLAMS with temperatures increasing by factors greater than or similar to 5 and greater than or similar to 3, respectively. Both the core and halo electron components show strong perpendicular heating inside the feature. C1 [Wilson, L. B., III; Koval, A.; Sibeck, D. G.; Szabo, A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA. [Cattell, C. A.] Univ Minnesota, Sch Phys & Astron, Minneapolis, MN 55455 USA. [Kasper, J. C.; Maruca, B. A.] Harvard Univ, Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Pulupa, M.; Salem, C. S.; Wilber, M.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Koval, A.] Univ Maryland Baltimore Cty, Goddard Planetary Heliophys Inst, Baltimore, MD 21228 USA. RP Wilson, LB (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD USA. EM lynn.b.wilsoniii@gmail.com RI Kasper, Justin/D-1152-2010; Wilson III, Lynn/D-4425-2012; OI Kasper, Justin/0000-0002-7077-930X; Wilson III, Lynn/0000-0002-4313-1970; Cattell, Cynthia/0000-0002-3805-320X; Pulupa, Marc/0000-0002-1573-7457 FU Wind MODA grants; NESSF [NNX07AU72H, NNX07AI05G]; Dr. Leonard Burlaga/Arctowski Medal Fellowship FX We thank R. P. Lin (3DP), K. W. Ogilvie (SWE), and R. P. Lepping (MFI) for the use of data from their instruments. Data from ACE, GOES, Interball, and OMNI data were obtained from CDAWeb. All data sets from the Wind spacecraft were produced under Wind MO&DA grants. This research was supported by NESSF grant NNX07AU72H, grant NNX07AI05G, and the Dr. Leonard Burlaga/Arctowski Medal Fellowship. NR 52 TC 12 Z9 12 U1 1 U2 6 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9380 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD MAR PY 2013 VL 118 IS 3 BP 957 EP 966 DI 10.1029/2012JA018186 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 135FP UT WOS:000318274000001 ER PT J AU Giordano, S Ciaravella, A Raymond, JC Ko, YK Suleiman, R AF Giordano, S. Ciaravella, A. Raymond, J. C. Ko, Y-K Suleiman, R. TI UVCS/SOHO catalog of coronal mass ejections from 1996 to 2005: Spectroscopic proprieties SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID CME CURRENT SHEETS; SHOCK-WAVE DRIVEN; ULTRAVIOLET SPECTROSCOPY; 3-DIMENSIONAL STRUCTURE; RADIO OBSERVATIONS; SOHO OBSERVATIONS; SOLAR CORONA; UV; RECONNECTION; TEMPERATURE AB Ultraviolet spectra of the extended solar corona have been routinely obtained by SOHO/UltraViolet Coronagraph Spectrometer (UVCS) since 1996. Sudden variations of spectral parameters are mainly due to the detection of coronal mass ejections (CMEs) crossing the instrumental slit. We present a catalog of CME ultraviolet spectra based upon a systematic search of events in the Large Angle and Spectrometric Coronagraph (LASCO) CME catalog, and we discuss their statistical properties. Our catalog includes 1059 events through the end of 2005, covering nearly a full solar cycle. It is available online at the URL http://solarweb.oato.inaf.it/UVCS_CME and embedded in the online LASCO CME catalog (http://cdaw.gsfc.nasa.gov/CME_list). The emission lines observed provide diagnostics of CME plasma parameters, such as the light-of-sight velocity, density, and temperature and allow to link the CME onset data to the extended corona white-light images. The catalog indicates whether there are clear signatures of features such as shock waves, current sheets, O VI flares, helical motions, and which part of the CME structures (front, cavity, or prominence material) are detected. The most common detected structure is the cool prominence material (in about 70% of the events). For each event, the catalog also contains movies, images, plots, and information relevant to address detailed scientific investigations. The number of events detected in UV is about one tenth of the LASCO CMEs and about one fourth of the halo events. We find that UVCS tends to detect faster, more massive, and energetic CME than LASCO, and for about 40% of the events, it has been possible to determine the plasma light-of-sight velocity. C1 [Giordano, S.] Osserv Astron Torino, INAF, I-10025 Pino Torinese, Italy. [Ciaravella, A.] Osserv Astron Palermo, INAF, Palermo, Italy. [Raymond, J. C.; Suleiman, R.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Ko, Y-K] USN, Res Lab, Div Space Sci, Washington, DC 20375 USA. RP Giordano, S (reprint author), Osserv Astron Torino, INAF, I-10025 Pino Torinese, Italy. EM giordano@oato.inaf.it OI Ciaravella, Angela/0000-0002-3127-8078; Giordano, Silvio/0000-0002-3468-8566 FU National Aeronautics and Space Administration (NASA) [NNG06GG78G, NNX09AB17G, NNX11AB61G] FX This work was supported by National Aeronautics and Space Administration (NASA) grants NNG06GG78G, NNX09AB17G, and NNX11AB61G to the Smithsonian Astrophysical Observatory. The LASCO CME catalog is generated and maintained at the CDAW Data Center by NASA and the Catholic University of America in cooperation with the Naval Research Laboratory. SOHO is a project of international cooperation between the European Space Agency (ESA) and the NASA. UVCS is a joint project of NASA, Italian Space Agency (ASI), and the Swiss Funding Agencies. We thank Antonio Volpicelli for help to release the online catalog. NR 63 TC 7 Z9 7 U1 0 U2 5 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 MAR PY 2013 VL 118 IS 3 BP 967 EP 981 DI 10.1002/jgra.50166 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 135FP UT WOS:000318274000002 ER PT J AU Carter, PJ Marsh, TR Steeghs, D Groot, PJ Nelemans, G Levitan, D Rau, A Copperwheat, CM Kupfer, T Roelofs, GHA AF Carter, P. J. Marsh, T. R. Steeghs, D. Groot, P. J. Nelemans, G. Levitan, D. Rau, A. Copperwheat, C. M. Kupfer, T. Roelofs, G. H. A. TI A search for the hidden population of AM CVn binaries in the Sloan Digital Sky Survey SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE accretion, accretion discs; binaries: close; novae, cataclysmic variables; stars: individual: SDSS J104325.08+563258.1; stars: individual: SDSS J173047.59+554518.5; white dwarfs ID CANUM-VENATICORUM BINARIES; DOUBLE WHITE-DWARFS; ORBITAL PERIOD; CATACLYSMIC VARIABLES; DATA RELEASE; SPECTROSCOPIC ANALYSIS; PG 1346+082; CP ERIDANI; STARS; SDSS AB We present the latest results from a spectroscopic survey designed to uncover the hidden population of AM Canum Venaticorum (AM CVn) binaries in the photometric data base of the Sloan Digital Sky Survey (SDSS). We selected similar to 2000 candidates based on their photometric colours, a relatively small sample which is expected to contain the majority of all AM CVn binaries in the SDSS (expected to be similar to 50). We present two new candidate AM CVn binaries discovered using this strategy: SDSS J104325.08+563258.1 and SDSS J173047.59+554518.5. We also present spectra of 29 new cataclysmic variables, 23 DQ white dwarfs and 21 DZ white dwarfs discovered in this survey. The survey is now approximately 70 per cent complete, and the discovery of seven new AM CVn binaries indicates a lower space density than previously predicted. From the essentially complete g <= 19 sample, we derive an observed space density of (5 +/- 3) x 10(-7) pc(-3); this is lower than previous estimates by a factor of 3. The sample has been cross-matched with the GALEX All-Sky Imaging Survey data base, and with Data Release 9 of the United Kingdom Infrared Telescope (UKIRT) Infrared Deep Sky Survey (UKIDSS). The addition of UV photometry allows new colour cuts to be applied, reducing the size of our sample to similar to 1100 objects. Optimizing our follow-up should allow us to uncover the remaining AM CVn binaries present in the SDSS, providing the larger homogeneous sample required to more reliably estimate their space density. C1 [Carter, P. J.; Marsh, T. R.; Steeghs, D.; Copperwheat, C. M.] Univ Warwick, Dept Phys, Coventry CV4 7AL, W Midlands, England. [Groot, P. J.; Nelemans, G.; Kupfer, T.] Radboud Univ Nijmegen, Dept Astrophys IMAPP, NL-6500 GL Nijmegen, Netherlands. [Nelemans, G.] Katholieke Univ Leuven, Inst Astron, B-3001 Louvain, Belgium. [Levitan, D.] CALTECH, Div Phys Math & Astron, Pasadena, CA 91125 USA. [Rau, A.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Roelofs, G. H. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Carter, PJ (reprint author), Univ Warwick, Dept Phys, Coventry CV4 7AL, W Midlands, England. EM philip.carter@warwick.ac.uk RI Steeghs, Danny/C-5468-2009; Nelemans, Gijs/D-3177-2012; Groot, Paul/K-4391-2016 OI Steeghs, Danny/0000-0003-0771-4746; Nelemans, Gijs/0000-0002-0752-2974; Groot, Paul/0000-0002-4488-726X FU Science and Technology Facilities Council (STFC) [ST/F002599/1]; Alfred P. Sloan Foundation; National Science Foundation; US Department of Energy; National Aeronautics and Space Administration; Japanese Monbukagakusho; Max Planck Society; Higher Education Funding Council for England FX We thank the anonymous referee for useful comments and suggestions. PJC acknowledges the support of a Science and Technology Facilities Council (STFC) studentship. TRM, DS and CMC acknowledge support from the Science and Technology Facilities Council (STFC) grant no. ST/F002599/1. Funding for the SDSS and SDSS-II has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, the US 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 website is http://www.sdss.org/. GALEX is a NASA Small Explorer. The mission was developed in cooperation with the Centre National dEtudes Spatiales of France and the Korean Ministry of Science and Technology. This research has made use of the SIM-BAD data base, operated at CDS, Strasbourg, France, and NASA's Astrophysics Data System Bibliographic Services. Several figures make use of P. Bergeron's synthetic white dwarf colours, taken from http://www.astro.umontreal.ca/similar to bergeron/CoolingModels. Fig. 12 makes use of white dwarf model spectra kindly provided by Detlev Koester. NR 81 TC 21 Z9 21 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 2013 VL 429 IS 3 BP 2143 EP 2160 DI 10.1093/mnras/sts485 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 135ET UT WOS:000318271300020 ER PT J AU Keith, MJ Coles, W Shannon, RM Hobbs, GB Manchester, RN Bailes, M Bhat, NDR Burke-Spolaor, S Champion, DJ Chaudhary, A Hotan, AW Khoo, J Kocz, J Oslowski, S Ravi, V Reynolds, JE Sarkissian, J van Straten, W Yardley, DRB AF Keith, M. J. Coles, W. Shannon, R. M. Hobbs, G. B. Manchester, R. N. Bailes, M. Bhat, N. D. R. Burke-Spolaor, S. Champion, D. J. Chaudhary, A. Hotan, A. W. Khoo, J. Kocz, J. Oslowski, S. Ravi, V. Reynolds, J. E. Sarkissian, J. van Straten, W. Yardley, D. R. B. TI Measurement and correction of variations in interstellar dispersion in high-precision pulsar timing SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE methods: data analysis; pulsars: general; ISM: structure ID MILLISECOND PULSARS; MAGNETIC-FIELD; SCATTERING; LIMITS; ARRAY; SCINTILLATION; PACKAGE; TEMPO2; WAVES AB Signals from radio pulsars show a wavelength-dependent delay due to dispersion in the interstellar plasma. At a typical observing wavelength, this delay can vary by tens of microseconds on 5-yr time-scales, far in excess of signals of interest to pulsar timing arrays, such as that induced by a gravitational wave background. Measurement of these delay variations is not only crucial for the detection of such signals, but also provides an unparalleled measurement of the turbulent interstellar plasma at astronomical unit (au) scales. In this paper we demonstrate that without consideration of wavelength-independent red noise, 'simple' algorithms to correct for interstellar dispersion can attenuate signals of interest to pulsar timing arrays. We present a robust method for this correction, which we validate through simulations, and apply it to observations from the Parkes Pulsar Timing Array. Correction for dispersion variations comes at a cost of increased band-limited white noise. We discuss scheduling to minimize this additional noise, and factors, such as scintillation, that can exacerbate the problem. Comparison with scintillation measurements confirms previous results that the spectral exponent of electron density variations in the interstellar medium often appears steeper than expected. We also find a discrete change in dispersion measure of PSR J1603-7202 of similar to 2 x 10(-3) cm(-3) pc for about 250 d. We speculate that this has a similar origin to the 'extreme scattering events' seen in other sources. In addition, we find that four pulsars show a wavelength-dependent annual variation, indicating a persistent gradient of electron density on an au spatial scale, which has not been reported previously. C1 [Keith, M. J.; Shannon, R. M.; Hobbs, G. B.; Manchester, R. N.; Chaudhary, A.; Hotan, A. W.; Khoo, J.; Oslowski, S.; Ravi, V.; Reynolds, J. E.; Sarkissian, J.; Yardley, D. R. B.] CSIRO Astron & Space Sci, Australia Telescope Natl Facil, Epping, NSW 1710, Australia. [Coles, W.] Univ Calif San Diego, La Jolla, CA 92093 USA. [Bailes, M.; Bhat, N. D. R.; Kocz, J.; Oslowski, S.; van Straten, W.] Swinburne Univ Technol, Ctr Astrophys & Supercomp, Hawthorn, Vic 3122, Australia. [Bhat, N. D. R.] Curtin Univ Technol, Int Ctr Radio Astron Res, Bentley, WA 6102, Australia. [Burke-Spolaor, S.] CALTECH, Jet Prop Lab, NASA, Pasadena, CA 91109 USA. [Champion, D. J.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Kocz, J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Ravi, V.] Univ Melbourne, Sch Phys, Melbourne, Vic 3010, Australia. [Yardley, D. R. B.] Univ Sydney, Sch Phys A29, Sydney Inst Astron, Sydney, NSW 2006, Australia. RP Keith, MJ (reprint author), CSIRO Astron & Space Sci, Australia Telescope Natl Facil, POB 76, Epping, NSW 1710, Australia. EM mkeith@pulsarastronomy.net OI Champion, David/0000-0003-1361-7723; Shannon, Ryan/0000-0002-7285-6348; Kocz, Jonathon/0000-0003-0249-7586; van Straten, Willem/0000-0003-2519-7375; Oslowski, Stefan/0000-0003-0289-0732 FU Australian Research Council [DP0878388, FF0348478]; Commonwealth of Australia FX This work has been carried out as part of the Parkes Pulsar Timing Array project. GBH is the recipient of an Australian Research Council QEII Fellowship (project DP0878388), the PPTA project was initiated with support from RNM's Federation Fellowship (FF0348478). The Parkes radio telescope is part of the Australia Telescope which is funded by the Commonwealth of Australia for operation as a National Facility managed by CSIRO. NR 32 TC 60 Z9 60 U1 0 U2 1 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 2013 VL 429 IS 3 BP 2161 EP 2174 DI 10.1093/mnras/sts486 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 135ET UT WOS:000318271300021 ER PT J AU Camero-Arranz, A Rea, N Bucciantini, N McLaughlin, MA Slane, P Gaensler, BM Torres, DF Stella, L de Ona, E Israel, GL Camilo, F Possenti, A AF Camero-Arranz, A. Rea, N. Bucciantini, N. McLaughlin, M. A. Slane, P. Gaensler, B. M. Torres, D. F. Stella, L. de Ona, E. Israel, G. L. Camilo, F. Possenti, A. TI The extended X-ray emission around RRAT J1819-1458 SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE stars: magnetic field; stars: neutron; pulsars: individual: RRAT J1819-1458; X-rays: stars ID RADIO TRANSIENT J1819-1458; SUPERNOVA-REMNANTS; SCATTERING HALOS; WIND NEBULAE; DISCOVERY; EVOLUTION; DISTANCE; PULSARS AB We present new imaging and spectral analysis of the recently discovered extended X-ray emission around the high magnetic field rotating radio transient RRAT J1819-1458. We used two Chandra observations performed for this object in 2008 May 31 and 2011 May 28, respectively. The diffuse X-ray emission was detected with a significance of similar to 19 sigma in the image obtained by combining the two observations. Neither long-term spectral nor timing variability has been observed from the source or the nebula. RRAT J1819-1458 shows an unusual high X-ray efficiency of eta(X) = L-X(0.3 5 keV)/(E) over dot(rot) similar to 0.15 at converting spin-down power into X-ray luminosity. The most favourable scenario for the origin of this extended X-ray emission is either a pulsar wind nebula or a scattering halo. A magnetically powered scenario for the extended emission is viable only in the case of a Compton nebula, while it can be tentatively disfavoured in the case of synchrotron emission. C1 [Camero-Arranz, A.; Rea, N.; Torres, D. F.; de Ona, E.] Fac Ciencies, Inst Ciencies Espai IEEC CSIC, E-08193 Barcelona, Spain. [Bucciantini, N.] INAF Osservatorio Astrofis Arcetri, I-50125 Florence, Italy. [Bucciantini, N.] INFN Sez Firenze, I-50019 Florence, Italy. [McLaughlin, M. A.] W Virginia Univ, Dept Phys, Morgantown, WV 26501 USA. [Slane, P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Gaensler, B. M.] Univ Sydney, Redfern, NSW 2016, Australia. [Torres, D. F.] Passeig Lluis Co, ICREA, E-08010 Barcelona, Spain. [Stella, L.; Israel, G. L.] INAF Osservatorio Astron Roma, I-00040 Rome, Italy. [Camilo, F.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA. [Camilo, F.] Arecibo Observ, Arecibo, PR 00612 USA. [Possenti, A.] INAF Osservatorio Astron Cagliari, I-09012 Capoterra, Italy. RP Camero-Arranz, A (reprint author), Fac Ciencies, Inst Ciencies Espai IEEC CSIC, Campus UAB,Torre C5,2A Planta, E-08193 Barcelona, Spain. EM camero.ascension@gmail.com RI Gaensler, Bryan/F-8655-2010; Rea, Nanda/I-2853-2015; Torres, Diego/O-9422-2016; OI Rea, Nanda/0000-0003-2177-6388; Torres, Diego/0000-0002-1522-9065; Bucciantini, Niccolo'/0000-0002-8848-1392; Israel, GianLuca/0000-0001-5480-6438; Gaensler, Bryan/0000-0002-3382-9558; de Ona Wilhelmi, Emma/0000-0002-5401-0744 FU Formosa programme [TW2010005 Q19]; iLINK programme [2011-0303]; CSIC; NASA [NAS8-03060]; Chandra Observer Support Award [GO1-12091X]; National Aeronautics and Space Administration; National Science Foundation; [AYA2009-07391]; [SGR2009-811] FX This work was supported by the grants AYA2009-07391 and SGR2009-811, as well as the Formosa programme TW2010005 Q19 and iLINK programme 2011-0303. NR is supported by a Ramon y Cajal research position in CSIC. PS acknowledges support from NASA Contract NAS8-03060. This work was supported by Chandra Observer Support Award GO1-12091X. This publication makes use of data products from the TwoMicron 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 also thank Michael Kramer, Marta Burgay, Andrew Lyne, Shami Chatterjee and Andrea Tiengo. NR 23 TC 5 Z9 6 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 2013 VL 429 IS 3 BP 2493 EP 2499 DI 10.1093/mnras/sts531 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 135ET UT WOS:000318271300047 ER PT J AU Marinucci, A Risaliti, G Wang, JF Bianchi, S Elvis, M Matt, G Nardini, E Braito, V AF Marinucci, Andrea Risaliti, Guido Wang, Junfeng Bianchi, Stefano Elvis, Martin Matt, Giorgio Nardini, Emanuele Braito, Valentina TI X-ray absorption variability in NGC 4507 SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE Galaxies: active; Galaxies: Seyfert ID ACTIVE GALACTIC NUCLEI; PHOTON IMAGING CAMERA; SEYFERT 2 GALAXIES; XMM-NEWTON; OBSCURED AGN; LINE; ABSORBER; SPECTRUM; COMPLEX; REGION AB We present a complete spectral analysis of an XMM-Newton and Chandra campaign of the obscured AGN in NGC 4507, consisting of six observations spanning a period of six months, ranging from 2010 June to December. We detect strong absorption variability on time-scales between 1.5 and 4 months, suggesting that the obscuring material consists of gas clouds at parsec-scale distance. The lack of significant variability on shorter time-scales suggests that this event is not due to absorption by broad-line region (BLR) clouds, which was instead found in other studies of similar sources. This shows that a single, universal structure of the absorber (either BLR clouds, or the parsec-scale torus) is not enough to reproduce the observed complexity of the X-ray absorption features of this AGN. C1 [Marinucci, Andrea; Bianchi, Stefano; Matt, Giorgio] Univ Roma Tre, Dipartimento Fis, I-00146 Rome, Italy. [Marinucci, Andrea; Risaliti, Guido; Wang, Junfeng; Elvis, Martin; Nardini, Emanuele] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Risaliti, Guido; Braito, Valentina] INAF Osservatorio Astrofis Arcetri, Florence, Italy. INAF Osservatorio Astron Brera, I-23807 Merate, Italy. RP Marinucci, A (reprint author), Univ Roma Tre, Dipartimento Fis, Via Vasca Navale 84, I-00146 Rome, Italy. EM marinucci@fis.uniroma3.it RI Bianchi, Stefano/B-4804-2010; OI Bianchi, Stefano/0000-0002-4622-4240; Braito, Valentina/0000-0002-2629-4989; Risaliti, Guido/0000-0002-3556-977X FU NASA [NNX11AC85G, GO2-13124X] FX The authors thank both the referees for their comments that greatly improved this paper. This work was partially supported by NASA grants NNX11AC85G and GO2-13124X. NR 47 TC 8 Z9 8 U1 0 U2 4 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 2013 VL 429 IS 3 BP 2581 EP 2586 DI 10.1093/mnras/sts534 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 135ET UT WOS:000318271300055 ER PT J AU Brenneman, LW Risaliti, G Elvis, M Nardini, E AF Brenneman, L. W. Risaliti, G. Elvis, M. Nardini, E. TI An examination of the spectral variability in NGC 1365 with Suzaku SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE accretion, accretion discs; galaxies: active; galaxies: individual: NGC 1365; X-rays: galaxies ID BLACK-HOLE SPIN; ACTIVE GALACTIC NUCLEI; FLUORESCENT IRON LINES; X-RAY BINARIES; XMM-NEWTON; MCG-6-30-15; ABSORPTION; GALAXIES; HARD; EMISSION AB We present jointly analysed data from three deep Suzaku observations of NGC 1365. These high-signal-to-noise spectra enable us to examine the nature of this variable, obscured active galactic nucleus (AGN) in unprecedented detail on time-scales ranging from hours to years. We find that in addition to the power-law continuum and absorption from ionized gas seen in most AGN, inner disc reflection and variable absorption from neutral gas within the broad emission line region are both necessary components in all three observations. We confirm the clumpy nature of the cold absorbing gas, though we note that occultations of the inner disc and corona are much more pronounced in the high-flux state (2008) than in the low-flux state (2010) of the source. The onset and duration of the 'dips' in the X-ray light curve in 2010 are both significantly longer than in 2008, however, indicating that either the distance to the gas from the black hole is larger or the nature of the gas has changed between epochs. We also note significant variations in the power-law flux over time-scales similar to the cold absorber, both within and between the three observations. The warm absorber does not vary significantly within observations, but does show variations in column density of a factor of >= 10 on time-scales of <= 2 weeks that seem unrelated to the changes in the continuum, reflection or cold absorber. By assuming a uniform iron abundance for the reflection and absorption, we have also established that Fe/solar = 3.5(-0.1)(+0.3) is sufficient to model the broad-band spectrum without invoking an additional partial-covering absorber. Such a measurement is consistent with previous published constraints from the 2008 Suzaku observation alone, and with results from other Seyfert AGN in the literature. C1 [Brenneman, L. W.; Risaliti, G.; Elvis, M.; Nardini, E.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Risaliti, G.] INAF Osservatorio Astrofis Arcetri, I-50125 Florence, Italy. RP Brenneman, LW (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM lbrenneman@head.cfa.harvard.edu RI XRAY, SUZAKU/A-1808-2009; OI Risaliti, Guido/0000-0002-3556-977X FU Suzaku mission through NASA [NNXlOAR44G] FX We gratefully acknowledge support from the Suzaku mission through NASA grant NNXlOAR44G, as well as the dedicated work of the NASA/GSFC Suzaku GOF team on data calibration. This work made use of archived Suzaku data maintained by HEASARC at NASA/GSFC. LB thanks Chris Reynolds and Mike Nowak for useful discussions that contributed to the data analysis in this paper, and Dominic Walton for providing the XSTAR grid used in this work, as well as insightful comments on the manuscript. We also thank the anonymous referee, whose critique greatly improved this work. NR 47 TC 18 Z9 18 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 2013 VL 429 IS 3 BP 2662 EP 2676 DI 10.1093/mnras/sts555 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 135ET UT WOS:000318271300062 ER PT J AU Burr, DM Perron, JT Lamb, MP Irwin, RP Collins, GC Howard, AD Sklar, LS Moore, JM Adamkovics, M Baker, VR Drummond, SA Black, BA AF Burr, Devon M. Perron, J. Taylor Lamb, Michael P. Irwin, Rossman P., III Collins, Geoffrey C. Howard, Alan D. Sklar, Leonard S. Moore, Jeffrey M. Adamkovics, Mate Baker, Victor R. Drummond, Sarah A. Black, Benjamin A. TI Fluvial features on Titan: Insights from morphology and modeling SO GEOLOGICAL SOCIETY OF AMERICA BULLETIN LA English DT Article ID HUYGENS LANDING SITE; UNIDIRECTIONAL WATER FLOWS; CASSINI RADAR; RIVER INCISION; SEDIMENT TRANSPORT; SOUTH-POLE; BED CONFIGURATIONS; TERMINAL VELOCITY; TECTONIC ACTIVITY; METHANE CYCLE AB Fluvial features on Titan have been identified in synthetic aperture radar (SAR) data taken during spacecraft flybys by the Cassini Titan Radar Mapper (RADAR) and in Descent Imager/Spectral Radiometer (DISR) images taken during descent of the Huygens probe to the surface. Interpretations using terrestrial analogs and process mechanics extend our perspective on fluvial geomorphology to another world and offer insight into their formative processes. At the landscape scale, the varied morphologies of Titan's fluvial networks imply a variety of mechanical controls, including structural influence, on channelized flows. At the reach scale, the various morphologies of individual fluvial features, implying a broad range of fluvial processes, suggest that (paleo-)flows did not occupy the entire observed width of the features. DISR images provide a spatially limited view of uplands dissected by valley networks, also likely formed by overland flows, which are not visible in lower-resolution SAR data. This high-resolution snapshot suggests that some fluvial features observed in SAR data may be river valleys rather than channels, and that uplands elsewhere on Titan may also have fine-scale fluvial dissection that is not resolved in SAR data. Radar-bright terrain with crenulated bright and dark bands is hypothesized here to be a signature of fine-scale fluvial dissection. Fluvial deposition is inferred to occur in braided channels, in (paleo)lake basins, and on SAR-dark plains, and DISR images at the surface indicate the presence of fluvial sediment. Flow sufficient to move sediment is inferred from observations and modeling of atmospheric processes, which support the inference from surface morphology of precipitation-fed fluvial processes. With material properties appropriate for Titan, terrestrial hydraulic equations are applicable to flow on Titan for fully turbulent flow and rough boundaries. For low-Reynolds-number flow over smooth boundaries, however, knowledge of fluid kinematic viscosity is necessary. Sediment movement and bed form development should occur at lower bed shear stress on Titan than on Earth. Scaling bedrock erosion, however, is hampered by uncertainties regarding Titan material properties. Overall, observations of Titan point to a world pervasively influenced by fluvial processes, for which appropriate terrestrial analogs and formulations may provide insight. C1 [Burr, Devon M.; Drummond, Sarah A.] Univ Tennessee, Dept Earth & Planetary Sci, Knoxville, TN 37996 USA. [Perron, J. Taylor; Black, Benjamin A.] MIT, Dept Earth Atmospher & Planetary Sci, Cambridge, MA 02139 USA. [Lamb, Michael P.] CALTECH, Pasadena, CA 91125 USA. [Irwin, Rossman P., III] Smithsonian Inst, Natl Air & Space Museum, Ctr Earth & Planetary Studies, Washington, DC 20013 USA. [Collins, Geoffrey C.] Wheaton Coll, Dept Phys & Astron, Norton, MA 02766 USA. [Howard, Alan D.] Univ Virginia, Dept Environm Sci, Charlottesville, VA 22904 USA. [Sklar, Leonard S.] San Francisco State Univ, Dept Geosci, San Francisco, CA 94132 USA. [Moore, Jeffrey M.] NASA, Space Sci Div, Ames Res Ctr, Moffett Field, CA 94035 USA. [Adamkovics, Mate] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Baker, Victor R.] Univ Arizona, Dept Hydrol & Water Resources, Tucson, AZ 85721 USA. RP Burr, DM (reprint author), Univ Tennessee, Dept Earth & Planetary Sci, 1412 Circle Dr, Knoxville, TN 37996 USA. EM dburr1@utk.edu RI Lamb, Michael/B-6478-2012; Perron, J. Taylor/D-8983-2012; OI Perron, J. Taylor/0000-0002-0404-8701; Sklar, Leonard/0000-0001-9626-733X; Howard, Alan/0000-0002-5423-1600 FU Cassini Data Analysis Program; Outer Planets Research Program; University of Tennessee FX Support for Burr, Irwin, Perron, Drummond, and Black was provided by a Cassini Data Analysis Program grant to Burr. Collins and Sklar were supported by an Outer Planets Research Program grant to Collins. Moore and Howard were supported by an Outer Planets Research Program grant to Moore. We acknowledge support from the University of Tennessee Exhibit, Performance, and Publication Expense Fund. We thank Tom Farr for processing the synthetic aperture radar (SAR) images in Figure 4. We gratefully acknowledge Trent Hare for his Titan ArcGIS project and Randy Kirk and Alex Hayes for helpful information. We thank the editors for their assistance in helping us shape this publication appropriately, and Bob Craddock, Ralph Lorenz, and an anonymous reviewer for providing useful comments. Most of all, we thank the Cassini and Huygens spacecraft mission teams for their successful efforts to produce the data used in this manuscript. NR 201 TC 33 Z9 33 U1 1 U2 31 PU GEOLOGICAL SOC AMER, INC PI BOULDER PA PO BOX 9140, BOULDER, CO 80301-9140 USA SN 0016-7606 EI 1943-2674 J9 GEOL SOC AM BULL JI Geol. Soc. Am. Bull. PD MAR-APR PY 2013 VL 125 IS 3-4 BP 299 EP 321 DI 10.1130/B30612.1 PG 23 WC Geosciences, Multidisciplinary SC Geology GA 130IJ UT WOS:000317907000003 ER PT J AU Loinard, L Zapata, LA Rodriguez, LF Pech, G Chandler, CJ Brogan, CL Wilner, DJ Ho, PTP Parise, B Hartmann, LW Zhu, ZH Takahashi, S Trejo, A AF Loinard, Laurent Zapata, Luis A. Rodriguez, Luis F. Pech, Gerardo Chandler, Claire J. Brogan, Crystal L. Wilner, David J. Ho, Paul T. P. Parise, Berengere Hartmann, Lee W. Zhu, Zhaohuan Takahashi, Satoko Trejo, Alfonso TI ALMA and VLA observations of the outflows in IRAS 16293-2422 SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE techniques: interferometric; stars: formation; stars: individual: IRAS 16293-2422; ISM: jets and outflows ID 1ST HYDROSTATIC CORE; SOLAR-TYPE PROTOSTAR; SUBMILLIMETER ARRAY; MULTIPLE SYSTEM; PROPER MOTIONS; STAR-FORMATION; RADIO-SOURCES; IRAS-16293-2422; INFALL; OPHIUCHUS AB We present Atacama Large Millimeter/submillimeter Array (ALMA) and Very Large Array (VLA) observations of the molecular and ionized gas at 0.1-0.3 arcsec resolution in the Class 0 protostellar system IRAS 16293-2422. These data clarify the origins of the protostellar outflows from the deeply embedded sources in this complex region. Source A2 is confirmed to be at the origin of the well-known large-scale north-east-south-west flow. The most recent VLA observations reveal a new ejection from that protostar, demonstrating that it drives an episodic jet. The central compact part of the other known large-scale flow in the system, oriented roughly east-west, is well delineated by the CO(6-5) emission imaged with ALMA and is confirmed to be driven from within component A. Finally, a one-sided blueshifted bubble-like outflow structure is detected here for the first time from source B to the northwest of the system. Its very short dynamical time-scale (similar to 200 yr), low velocity and moderate collimation support the idea that source B is the youngest object in the system, and possibly one of the youngest protostars known. C1 [Loinard, Laurent; Zapata, Luis A.; Rodriguez, Luis F.; Pech, Gerardo] Univ Nacl Autonoma Mexico, Ctr Radiostron & Astrofis, Morelia 58089, Michoacan, Mexico. [Loinard, Laurent; Parise, Berengere] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Chandler, Claire J.] Natl Radio Astron Observ, Socorro, NM 87801 USA. [Brogan, Crystal L.] Natl Radio Astron Observ, Charlottesville, VA 22903 USA. [Wilner, David J.; Ho, Paul T. P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Ho, Paul T. P.; Takahashi, Satoko; Trejo, Alfonso] Acad Sinica, Inst Astron & Astrophys, Taipei 115, Taiwan. [Hartmann, Lee W.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Zhu, Zhaohuan] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. RP Loinard, L (reprint author), Univ Nacl Autonoma Mexico, Ctr Radiostron & Astrofis, Morelia 58089, Michoacan, Mexico. EM l.loinard@crya.unam.mx FU DGAPA; UNAM; CONACyT (Mexico); Alexander von Humboldt Stiftung; DFG Emmy Noether [PA1692/1-1] FX LL, LAZ, LFR and GP acknowledge the support of DGAPA, UNAM and of CONACyT (Mexico). LL is indebted to the Alexander von Humboldt Stiftung for financial support. BP is supported by the DFG Emmy Noether grant PA1692/1-1. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. This Letter makes use of the following ALMA data: ADS/JAO.ALMA#2011.0.00007.SV. ALMAis a partnership of ESO (representing its member states), NSF (USA) and NINS (Japan), together with NRC (Canada) and NSC, and ASIAA (Taiwan), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by ESO, AUI/NRAO and NAOJ. NR 32 TC 17 Z9 17 U1 1 U2 1 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 2013 VL 430 IS 1 BP L10 EP L14 DI 10.1093/mnrasl/sls038 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 135FU UT WOS:000318274500003 ER PT J AU Fabian, AC Kara, E Walton, DJ Wilkins, DR Ross, RR Lozanov, K Uttley, P Gallo, LC Zoghbi, A Miniutti, G Boller, T Brandt, WN Cackett, EM Chiang, CY Dwelly, T Malzac, J Miller, JM Nardini, E Ponti, G Reis, RC Reynolds, CS Steiner, JF Tanaka, Y Young, AJ AF Fabian, A. C. Kara, E. Walton, D. J. Wilkins, D. R. Ross, R. R. Lozanov, K. Uttley, P. Gallo, L. C. Zoghbi, A. Miniutti, G. Boller, T. Brandt, W. N. Cackett, E. M. Chiang, C. -Y. Dwelly, T. Malzac, J. Miller, J. M. Nardini, E. Ponti, G. Reis, R. C. Reynolds, C. S. Steiner, J. F. Tanaka, Y. Young, A. J. TI Long XMM observation of the narrow-line Seyfert 1 galaxy IRAS 13224-3809: rapid variability, high spin and a soft lag SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE accretion, accretion discs; black hole physics; line: profiles; X-rays: general ID X-RAY REFLECTION; BLACK-HOLE SPIN; IRON-K; SPECTRAL PROPERTIES; EMISSION-LINES; IRAS-13224-3809; REVERBERATION; NEWTON AB The narrow-line Seyfert 1 galaxy IRAS 13224-3809 has been observed with XMM-Newton for 500 ks. The source is rapidly variable on time-scales down to a few 100 s. The spectrum shows strong broad Fe - K and L emission features which are interpreted as arising from reflection from the inner parts of an accretion disc around a rapidly spinning black hole. Assuming a power law emissivity for the reflected flux and that the innermost radius corresponds to the innermost stable circular orbit, the black hole spin is measured to be 0.989 with a statistical precision better than 1 per cent. Systematic uncertainties are discussed. A soft X-ray lag of 100 s confirms this scenario. The bulk of the power-law continuum source is located at a radius of 2-3 gravitational radii. C1 [Fabian, A. C.; Kara, E.; Walton, D. J.; Wilkins, D. R.; Lozanov, K.; Chiang, C. -Y.; Malzac, J.; Steiner, J. F.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Ross, R. R.] Coll Holy Cross, Dept Phys, Worcester, MA 01610 USA. [Uttley, P.] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1090 GE Amsterdam, Netherlands. [Gallo, L. C.] St Marys Univ, Dept Astron & Phys, Halifax, NS B3H 3C3, Canada. [Zoghbi, A.; Reynolds, C. S.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Miniutti, G.] Ctr Astrobiol CSIC INTA, Dep Astrofis, LAEFF, E-28691 Madrid, Spain. [Boller, T.; Ponti, G.; Tanaka, Y.] Max Planck Inst Extraterr Phys, D-85741 Garching, Germany. [Brandt, W. N.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Cackett, E. M.] Wayne State Univ, Dept Phys & Astron, Detroit, MI 48201 USA. [Dwelly, T.] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England. [Miller, J. M.; Reis, R. C.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Nardini, E.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Young, A. J.] Univ Bristol, HH Wills Phys Lab, Bristol BS8 1TL, Avon, England. RP Fabian, AC (reprint author), Univ Cambridge, Inst Astron, Madingley Rd, Cambridge CB3 0HA, England. EM acf@ast.cam.ac.uk RI Miniutti, Giovanni/L-2721-2014; Brandt, William/N-2844-2015; Zoghbi, Abderahmen/A-8445-2017; OI Miniutti, Giovanni/0000-0003-0707-4531; Brandt, William/0000-0002-0167-2453; Zoghbi, Abderahmen/0000-0002-0572-9613; reis, rubens/0000-0002-6618-2412; Chiang, Chia-Ying/0000-0002-9630-4003 FU Royal Society; NASA [PF1-120087]; Gates Cambridge Scholarship FX We thank Jelle Kaastra for a helpful referee report. ACF thanks the Royal Society for support. RCR thanks the Michigan Society of Fellows and NASA for support through the Einstein Fellowship Programme, grant number PF1-120087. EK is supported by the Gates Cambridge Scholarship. NR 40 TC 40 Z9 40 U1 1 U2 11 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 2013 VL 429 IS 4 BP 2917 EP 2923 DI 10.1093/mnras/sts504 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 135FD UT WOS:000318272600010 ER PT J AU Madej, OK Jonker, PG Groot, PJ van Haaften, LM Nelemans, G Maccarone, TJ AF Madej, O. K. Jonker, P. G. Groot, P. J. van Haaften, L. M. Nelemans, G. Maccarone, T. J. TI Time-resolved X-Shooter spectra and RXTE light curves of the ultra-compact X-ray binary candidate 4U 0614+091 SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE binaries: close; white dwarfs; X-rays: individual: 4U 0614+091 ID ORBITAL PERIOD; NEUTRON-STAR; OPTICAL SPECTROSCOPY; ACCRETION DISKS; EXO 0748-676; BLACK-HOLES; MASS; HELIUM; DONOR; EVOLUTION AB In this paper we present X-Shooter time-resolved spectroscopy and RXTE PCA light curves of the ultra-compact X-ray binary candidate 4U 0614+091. The X-Shooter data are compared to the GMOS data analysed previously by Nelemans et al. We confirm the presence of CIII and OII emission features at approximate to 4650 angstrom and approximate to 5000 angstrom. The emission lines do not show evident Doppler shifts that could be attributed to the motion of the donor star/hotspot around the centre of mass of the binary. We note a weak periodic signal in the red-wing/blue-wing flux ratio of the emission feature at approximate to 4650 angstrom. The signal occurs at P = 30.23 +/- 0.03 min in the X-Shooter and at P = 30.468 +/- 0.006 min in the GMOS spectra when the source was in the low/hard state. Due to aliasing effects the period in the GMOS and X-Shooter data could well be the same. We deem it likely that the orbital period is thus close to 30 min; however, as several photometric periods have been reported for this source in the literature already, further confirmation of the 30 min period is warranted. We compare the surface area of the donor star and the disc of 4U 0614+091 with the surface area of the donor star and the disc in typical hydrogen-rich low-mass X-ray binaries and the class of AM Canum Venaticorum stars and argue that the optical emission in 4U 0614+091 is likely dominated by the disc emission. Assuming that the accretion disc in 4U 0614+091 is optically thick and the opening angle of the disc is similar to the one derived for the hydrogen-rich low-mass X-ray binaries we conclude that the donor star may in fact stay in the disc shadow. Additionally, we search for periodic signals in all the publicly available RXTE PCA light curves of 4U 0614+091 which could be associated with the orbital period of this source. A modulation at the orbital period with an amplitude of approximate to 10 per cent such as those that have been found in other ultra-compact X-ray binaries (4U 0513-40, 4U 1820-30) is not present in 4U 0614+091. We propose that the X-ray modulation found in 4U 0513-40 and 4U 1820-30 could be a signature of an outflow launched during the high/soft state near the stream impact region. C1 [Madej, O. K.; Jonker, P. G.; Groot, P. J.; van Haaften, L. M.; Nelemans, G.] Radboud Univ Nijmegen, Dept Astrophys, IMAPP, NL-6500 GL Nijmegen, 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. [Nelemans, G.] Katholieke Univ Leuven, Inst Astron, B-3001 Louvain, Belgium. [Maccarone, T. J.] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England. RP Madej, OK (reprint author), Radboud Univ Nijmegen, Dept Astrophys, IMAPP, POB 9010, NL-6500 GL Nijmegen, Netherlands. EM O.Madej@sron.nl RI Nelemans, Gijs/D-3177-2012; Groot, Paul/K-4391-2016 OI Nelemans, Gijs/0000-0002-0752-2974; Groot, Paul/0000-0002-4488-726X FU VIDI grant from the Netherlands Organization for Scientific Research FX We thank the referee for the useful comments. OKM and PGJ would like to thank: Rob Hynes, Manuel Torres, Frank Verbunt for useful discussions, Lucas Ellerbroek, Andrea Modigliani and Wolfram Freudling for the help with X-Shooter data reduction, Tom Marsh for the use of MOLLY and LTE emission line models, Keith Horne for the use of the eclipse mapping code. PGJ acknowledges support from a VIDI grant from the Netherlands Organization for Scientific Research. We acknowledge the RXTE/ASM and MAXI teams for the X-ray monitoring data. NR 53 TC 4 Z9 4 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 2013 VL 429 IS 4 BP 2986 EP 2996 DI 10.1093/mnras/sts550 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 135FD UT WOS:000318272600017 ER PT J AU Li, GJ Loeb, A AF Li, Gongjie Loeb, Abraham TI Accumulated tidal heating of stars over multiple pericentre passages near SgrA SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE black hole physics; binaries: close; stars: oscillations; galaxies: nuclei ID MASSIVE BLACK-HOLE; GALACTIC-CENTER; CAPTURE BINARIES; STELLAR ORBITS; HYPERVELOCITY STARS; EXTRASOLAR PLANETS; DYNAMICAL TIDES; NEUTRON-STARS; YOUNG STARS; DISRUPTION AB We consider the long-term tidal heating of a star by the supermassive black hole at the Galactic centre, SgrA*. We show that gravitational interaction with background stars leads to a linear growth of the tidal excitation energy with the number of pericentre passages near SgrA*. The accumulated heat deposited by excitation of modes within the star over many pericentre passages can lead to a runaway disruption of the star at a pericentre distance that is four to five times farther than the standard tidal disruption radius. The accumulated heating may explain the lack of massive (greater than or similar to 10M(circle dot)) S-stars closer than several tens of au from SgrA*. C1 [Li, Gongjie; Loeb, Abraham] Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, Cambridge, MA 02138 USA. RP Li, GJ (reprint author), Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, 60 Garden St, Cambridge, MA 02138 USA. EM gli@cfa.harvard.edu FU NSF [AST-0907890]; NASA [NNX08AL43G, NNA09DB30A] FX We thank Charlie Conroy, James Fuller, Bence Kocsis, Leo Meyer, Sterl Phinney, Eliot Quataert and Nick Stone for helpful comments. GL benefitted significantly from the MESA 2012 summer school. This work was supported in part by NSF grant AST-0907890 and NASA grants NNX08AL43G and NNA09DB30A. NR 59 TC 7 Z9 7 U1 0 U2 0 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 2013 VL 429 IS 4 BP 3040 EP 3046 DI 10.1093/mnras/sts567 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 135FD UT WOS:000318272600021 ER EF