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 floo