FN Thomson Reuters Web of Science™ VR 1.0 PT J AU Vanderwel, MC Slot, M Lichstein, JW Reich, PB Kattge, J Atkin, OK Bloomfield, KJ Tjoelker, MG Kitajima, K AF Vanderwel, Mark C. Slot, Martijn Lichstein, Jeremy W. Reich, Peter B. Kattge, Jens Atkin, Owen K. Bloomfield, Keith J. Tjoelker, Mark G. Kitajima, Kaoru TI Global convergence in leaf respiration from estimates of thermal acclimation across time and space SO NEW PHYTOLOGIST LA English DT Article DE autotrophic respiration; carbon flux; climate change; temperature; terrestrial biosphere modelling; thermal acclimation ID CARBON-CYCLE FEEDBACK; PLANT RESPIRATION; TEMPERATURE-ACCLIMATION; SOUTHERN-POPULATIONS; DARK RESPIRATION; PINUS-BANKSIANA; CLIMATE; MODEL; PHOTOSYNTHESIS; VEGETATION AB Recent compilations of experimental and observational data have documented global temperature-dependent patterns of variation in leaf dark respiration (R), but it remains unclear whether local adjustments in respiration over time (through thermal acclimation) are consistent with the patterns in R found across geographical temperature gradients. We integrated results from two global empirical syntheses into a simple temperature-dependent respiration framework to compare the measured effects of respiration acclimation-over-time and variation-across-space to one another, and to a null model in which acclimation is ignored. Using these models, we projected the influence of thermal acclimation on: seasonal variation in R; spatial variation in mean annual R across a global temperature gradient; and future increases in R under climate change. The measured strength of acclimation-over-time produces differences in annual R across spatial temperature gradients that agree well with global variation-across-space. Our models further project that acclimation effects could potentially halve increases in R (compared with the null model) as the climate warms over the 21st Century. Convergence in global temperature-dependent patterns of R indicates that physiological adjustments arising from thermal acclimation are capable of explaining observed variation in leaf respiration at ambient growth temperatures across the globe. C1 [Vanderwel, Mark C.] Univ Regina, Dept Biol, Regina, SK S4S 0A2, Canada. [Vanderwel, Mark C.; Slot, Martijn; Lichstein, Jeremy W.; Kitajima, Kaoru] Univ Florida, Dept Biol, Gainesville, FL 32611 USA. [Slot, Martijn] Smithsonian Trop Res Inst, Balboa, Panama. [Reich, Peter B.] Univ Minnesota, Dept Forest Resources, St Paul, MN 55108 USA. [Reich, Peter B.; Tjoelker, Mark G.] Univ Western Sydney, Hawkesbury Inst Environm, Penrith, NSW 2751, Australia. [Kattge, Jens] Max Planck Inst Biogeochem, D-07745 Jena, Germany. [Atkin, Owen K.; Bloomfield, Keith J.] Australia Natl Univ, ARC Ctr Excellence Plant Energy Biol, Res Sch Biol, Canberra, ACT 2601, Australia. [Kitajima, Kaoru] Kyoto Univ, Div Forest & Biomat Sci, Kyoto 6068502, Japan. RP Vanderwel, MC (reprint author), Univ Regina, Dept Biol, Regina, SK S4S 0A2, Canada. EM mark.vanderwel@uregina.ca RI Kattge, Jens/J-8283-2016; Tjoelker, Mark/M-2413-2016; Atkin, Owen/C-8415-2009 OI Kattge, Jens/0000-0002-1022-8469; Tjoelker, Mark/0000-0003-4607-5238; Atkin, Owen/0000-0003-1041-5202 FU National Science Foundation (NSF-IOS) [1051789] FX We thank participants in the 8th New Phytologist Workshop on leaf respiration in large-scale vegetation models for valuable discussions that helped improve the final paper. We also thank three anonymous reviewers for their helpful comments. Funding for this project was provided by the National Science Foundation (NSF-IOS grant 1051789). NR 54 TC 9 Z9 9 U1 5 U2 53 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0028-646X EI 1469-8137 J9 NEW PHYTOL JI New Phytol. PD SEP PY 2015 VL 207 IS 4 BP 1026 EP 1037 DI 10.1111/nph.13417 PG 12 WC Plant Sciences SC Plant Sciences GA CO2DP UT WOS:000358965800013 PM 25898850 ER PT J AU Geng, GN Zhang, Q Martin, RV van Donkelaar, A Huo, H Che, HZ Lin, JT He, KB AF Geng, Guannan Zhang, Qiang Martin, Randall V. van Donkelaar, Aaron Huo, Hong Che, Huizheng Lin, Jintai He, Kebin TI Estimating long-term PM2.5 concentrations in China using satellite-based aerosol optical depth and a chemical transport model SO REMOTE SENSING OF ENVIRONMENT LA English DT Article DE Particulate matter; Aerosol optical depth; Satellite remote sensing ID FINE PARTICULATE MATTER; GROUND-LEVEL PM2.5; CONTIGUOUS UNITED-STATES; AIR-POLLUTION; EASTERN CHINA; NORTH CHINA; MORTALITY; HAZE; MODIS; QUALITY AB Epidemiological and health impact studies of fine particulate matter (PM2.5) have been limited in China because of the lack of spatially and temporally continuous PM2.5 monitoring data. Satellite remote sensing of aerosol optical depth (ADD) is widely used in estimating ground-level PM2.5 concentrations. We improved the method for estimating long-term surface PM2.5 concentrations using satellite remote sensing and a chemical transport model, and derived PM2.5 concentrations over China for 2006-2012. We generated a map of surface PM2.5 concentrations at 0.1 degrees x 0.1 degrees over China using the nested-grid GEOS-Chem model, most recent bottom-up emission inventory, and satellite observations from the MODIS and MISR instruments. Aerosol vertical profiles from the space-based CALIOP lidar were used to adjust the climatological drivers of the bias in the simulated results, and corrections were made for incomplete sampling. We found significant spatial agreement between the satellite-derived PM2.5 concentrations and the ground-level PM2.5 measurements collected from literatures (r = 0.74, slope = 0.77, intercept = 1121 mu g/m(3)). The population-weighted mean of PM2.5 concentrations in China is 71 mu g/m(3) and more than one billion people live in locations where PM2.5 concentrations exceed the World Health Organization Air Quality Interim Target-1 of 35 mu g/m(3). The results from our work are substantially higher than previous work, especially in heavily polluted regions. The overall population-weighted mean uncertainty over China is 17.2 mu g/m(3), as estimated using ground-level AOD measurements and vertical profiles observed from CALIOP. (C) 2015 Elsevier Inc. All rights reserved. C1 [Geng, Guannan; Zhang, Qiang] Tsinghua Univ, Ctr Earth Syst Sci, Minist Educ Key Lab Earth Syst Modeling, Beijing 100084, Peoples R China. [Geng, Guannan; Martin, Randall V.; van Donkelaar, Aaron] Dalhousie Univ, Dept Phys & Atmospher Sci, Halifax, NS B3H 4R2, Canada. [Geng, Guannan; He, Kebin] Tsinghua Univ, Sch Environm, State Key Joint Lab Environm Simulat & Pollut Con, Beijing 100084, Peoples R China. [Martin, Randall V.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Huo, Hong] Tsinghua Univ, Inst Energy Environm & Econ, Beijing 100084, Peoples R China. [Che, Huizheng] Chinese Acad Meteorol Sci, Inst Atmospher Composit, Key Lab Atmospher Chem LAC, Beijing 100081, Peoples R China. [Lin, Jintai] Peking Univ, Sch Phys, Dept Atmospher & Ocean Sci, Lab Climate & Ocean Atmosphere Studies, Beijing 100871, Peoples R China. RP Zhang, Q (reprint author), Tsinghua Univ, Ctr Earth Syst Sci, Minist Educ Key Lab Earth Syst Modeling, Beijing 100084, Peoples R China. EM qiangzhang@tsinghua.edu.cn RI Martin, Randall/C-1205-2014; Chem, GEOS/C-5595-2014; Zhang, Qiang/D-9034-2012; Lin, Jintai/A-8872-2012; che, Huizheng/B-1354-2014 OI Martin, Randall/0000-0003-2632-8402; Lin, Jintai/0000-0002-2362-2940; che, Huizheng/0000-0002-9458-3387 FU National Science Foundation of China [41222036, 41275026, 71322304, 41175127]; Collaborative Innovation Center for Regional Environmental Quality; Natural Sciences and Engineering Research Council of Canada [5265-417449-12] FX This study was supported by the National Science Foundation of China (41222036, 41275026, 71322304, and 41175127). Q. Zhang and K. B. He are supported by the Collaborative Innovation Center for Regional Environmental Quality. The work at Dalhousie was supported by the Natural Sciences and Engineering Research Council of Canada (5265-417449-12). We thank the two anonymous reviewers for their constructive comments. NR 54 TC 22 Z9 22 U1 23 U2 111 PU ELSEVIER SCIENCE INC PI NEW YORK PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA SN 0034-4257 EI 1879-0704 J9 REMOTE SENS ENVIRON JI Remote Sens. Environ. PD SEP 1 PY 2015 VL 166 BP 262 EP 270 DI 10.1016/j.rse.2015.05.016 PG 9 WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic Technology SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science & Photographic Technology GA CN7RU UT WOS:000358632500021 ER PT J AU Micheletti, T Brown, JL Walker, SL Cubas, ZS Furtado, PV Putman, SB de Moraes, W de Oliveira, MJ de Oliveira, CA Moreira, N AF Micheletti, Tatiane Brown, Janine L. Walker, Susan L. Cubas, Zalmir S. Furtado, Priscila V. Putman, Sarah B. de Moraes, Wanderlei de Oliveira, Marcos J. de Oliveira, Claudio A. Moreira, Nei TI The use of altrenogest to avoid hyperestrogenism after eCG-hCG ovulation induction in southern tigrina (Leopardus guttulus) SO THERIOGENOLOGY LA English DT Article DE Captive reproduction; Gonadotropin; Neotropical felid; Ovulation induction; Progestin ID ARTIFICIAL-INSEMINATION; DOMESTIC CAT; EXOGENOUS GONADOTROPINS; ENZYME-IMMUNOASSAY; OVARIAN ACTIVITY; CLOUDED LEOPARD; GNRH ANTAGONIST; FELIS-CATUS; EMBRYO; PROGESTERONE AB The goal of this study was to optimize an ovulation induction protocol for use with artificial insemination in the southern tigrina (Leopard us guttulus). The specific aims were to report the efficacy of using altrenogest, an oral progestin (Regumate, MSD Animal Health, Merck Animal Health), to suppress ovarian activity and prevent follicular hyperstimulation and hyperestrogenism after the administration of exogenous eCG and hCG. To monitor ovarian responses, fecal estrogen and progestogen metabolites were quantified by enzyme immunoassay in females before and after intramuscular administration of 200-IU eCG and 150-IU hCG in two trials, 4 months apart. During the first trial, there was no use of altrenogest, only the eCG-hCG ovulation induction protocol. In the second trial, the ovulation induction protocol was preceded by the administration of oral altrenogest for 14 days (minimum of 0.192 mg per kg per day). Altrenogest administration resulted in a suppression of follicular activity in three out of six females before eCG-hCG administration on the basis of lower mean estrogen concentrations (P < 0.05). It also resulted in four out of six females presenting lower fecal estrogen metabolite concentrations (P < 0.05) after ovulation induction, and two out of six individuals showed a reduction (P < 0.05) in postovulatory fecal progestogen metabolite concentrations, all when compared to the same female's cycles without the progestin. Fecal estrogen metabolite concentrations were closer to baseline in 50% of these individuals after altrenogest and eCG-hCG treatments when compared to basal concentrations before gonadotropins without the use of altrenogest. This study reported that use of altrenogest in southern tigrina can suppress ovarian, activity and avoid hyperestrogenism after administration of eCG and hCG treatment. However, not all females responded uniformly, so more studies are needed to increase the efficacy of ovulation induction for use with artificial insemination in this species. (C) 2015 Elsevier Inc. All rights reserved. C1 [Micheletti, Tatiane; Moreira, Nei] Univ Fed Parana, Dept Vet Med & Anim Sci, Palotina, Parana, Brazil. [Micheletti, Tatiane] Brazilian Inst Conservat Med TRIADE, Curitiba, Parana, Brazil. [Brown, Janine L.; Putman, Sarah B.] Smithsonian Conservat Biol Inst, Front Royal, VA USA. [Walker, Susan L.] Chester Zoo, Reprod & Welf Res Unit, Upton By Chester, England. [Cubas, Zalmir S.; de Moraes, Wanderlei; de Oliveira, Marcos J.] Itaipu Binacl, Refugio Biol Bela Vista, Foz Do Iguacu, Parana, Brazil. [Furtado, Priscila V.; de Oliveira, Claudio A.] Univ Sao Paulo, Dept Anim Reprod, Lab Dosagens Hormonais, Sao Paulo, SP, Brazil. RP Micheletti, T (reprint author), Tech Univ Dresden, Inst Forstbot & Forstzool, Pienner Str 7 Cotta Bau, D-01737 Tharandt, Germany. EM micheletti@forst.tu-dresden.de FU Brazilian's National Council for Scientific and Technological Development FX The authors would like to acknowledge everyone that helped with this project, specially all the staff from Refugio Biologico Bela Vista at Itaipu Binacional, Laboratorio de Dosagens Hormonais (LDH-USP) and Smithsonian Conservation Biology Institute, and the colleagues Aline Rafaeli Hoffmann, Alcides Ricieri Rinaldi, Debora Tramujas Ballarotti, Jackson Wolf, Luiz Ernandes Kozicki, Patricia Cubas, Renata Carolina F. Santos, Rosana de Almeida, and Romildo Romualdo Weiss for the essential support during this project's execution. They also would like to acknowledge Brazilian's National Council for Scientific and Technological Development that partially funded the first author with a temporary masters' scholarship and Smithsonian Conservation Biology Institute that provided accommodation during the samples analyses. NR 30 TC 0 Z9 0 U1 1 U2 13 PU ELSEVIER SCIENCE INC PI NEW YORK PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA SN 0093-691X EI 1879-3231 J9 THERIOGENOLOGY JI Theriogenology PD SEP 1 PY 2015 VL 84 IS 4 BP 575 EP 582 DI 10.1016/j.theriogenology.2015.04.015 PG 8 WC Reproductive Biology; Veterinary Sciences SC Reproductive Biology; Veterinary Sciences GA CO3DK UT WOS:000359036600013 PM 26001599 ER PT J AU Falcon-Lang, HJ Lucas, SG Kerp, H Krainer, K Montanez, IP Vachard, D Chaney, DS Elrick, SD Contreras, DL Kurzawe, F DiMichele, WA Looy, CV AF Falcon-Lang, Howard J. Lucas, Spencer G. Kerp, Hans Krainer, Karl Montanez, Isabel P. Vachard, Daniel Chaney, Dan S. Elrick, Scott D. Contreras, Dori L. Kurzawe, Francine DiMichele, William A. Looy, Cindy V. TI Early Permian (Asselian) vegetation from a seasonally dry coast in western equatorial Pangea: Paleoecology and evolutionary significance SO PALAEOGEOGRAPHY PALAEOCLIMATOLOGY PALAEOECOLOGY LA English DT Article DE Permian; Estuary; Volrzian conifers; Callipterids; Mangrove; New Mexico ID PALEOZOIC ICE-AGE; CENTRAL NEW-MEXICO; CENTRAL APPALACHIAN BASIN; NORTH-CENTRAL TEXAS; SOUTHERN NEW-MEXICO; SMALLER FORAMINIFERS; SEQUENCE STRATIGRAPHY; ROBLEDO MOUNTAINS; RATTENDORF GROUP; TROPICAL FLORAS AB The Pennsylvanian-Permian transition has been inferred to be a time of significant glaciation in the Southern Hemisphere, the effects of which were manifested throughout the world. In the equatorial regions of Pangea, the response of terrestrial ecosystems was highly variable geographically, reflecting the interactions of polar ice and geographic patterns on atmospheric circulation. In general, however, there was a drying trend throughout most of the western and central equatorial belt. In western Pangea, the climate proved to be considerably more seasonally dry and with much lower mean annual rainfall than in areas in the more central and easterly portions of the supercontinent. Here we describe lower Permian (upper Asselian) fossil plant assemblages from the Community Pit Formation in Prehistoric Trackways National Monument near Las Cruces, south-central New Mexico, U.S.A. The fossils occur in sediments within a 140-m-wide channel that was incised into indurated marine carbonates. The channel filling can be divided into three phases. A basal channel, limestone conglomerate facies contains allochthonous trunks of walchian conifers. A middle channel fill is composed of mictitic limestone beds containing a brackish-to-marine fauna with carbon, oxygen and strontium isotopic composition that provide independent support for salinity inferences. The middle limestone also contains a (par)autochthonous adpressed megaflora co-dominated by voltzian conifers and the callipterid Lodevia oxydata. The upper portions of the channel are filled with muddy, gypsiferous limestone that lacks plant fossils. This is the geologically oldest occurrence of voltzian conifers. It also is the westernmost occurrence of L. oxydata, a rare callipterid known only from the Pennsylvanian-Permian transition in Poland, the Appalachian Basin and New Mexico. The presence of in situ fine roots within these channel-fill limestone beds and the taphonomic constraints on the incorporation of aerial plant remains into a lime mudstone indicate that the channel sediments were periodically colonized by plants, which suggests that these species were tolerant of salinity, making these plants one of, if not the earliest unambiguous mangroves. (C) 2015 Elsevier B.V. All rights reserved. C1 [Falcon-Lang, Howard J.; Kurzawe, Francine] Univ London, Dept Earth Sci, Egham TW20 0EX, Surrey, England. [Falcon-Lang, Howard J.; Kerp, Hans] Univ Munster, Forsch Stelle Palaobot, Geol Palaontol Inst, D-48149 Munster, Germany. [Lucas, Spencer G.] New Mexico Museum Nat Hist & Sci, Albuquerque, NM 87104 USA. [Krainer, Karl] Univ Innsbruck, Inst Geol & Paleontol, A-6020 Innsbruck, Austria. [Montanez, Isabel P.] Univ Calif Davis, Dept Earth & Planetary Sci, Davis, CA 95616 USA. [Vachard, Daniel] Univ Lille 1, UMR Geosyst 8217, F-59655 Villeneuve Dascq, Ufr, France. [Chaney, Dan S.; DiMichele, William A.] Smithsonian Inst, Dept Paleobiol, Natl Museum Nat Hist, Washington, DC 20560 USA. [Elrick, Scott D.] Illinois State Geol Survey, Champaign, IL 61820 USA. [Contreras, Dori L.; Looy, Cindy V.] Univ Calif Berkeley, Dept Integrat Biol, Berkeley, CA 94720 USA. [Contreras, Dori L.; Looy, Cindy V.] Univ Calif Berkeley, Museum Paleontol, Berkeley, CA 94720 USA. RP Looy, CV (reprint author), Univ Calif Berkeley, Dept Integrat Biol, 3060 Valley Life Sci Bldg, Berkeley, CA 94720 USA. EM looy@berkeley.edu FU Bureau of Land Management (BLM Las Cruces District Office) [BLM L09AC15951]; NERC at Royal Holloway, University of London [NE/F014120/2]; NSF [EAR1024737]; NSF GRF [DGE 1106400]; Conselho Nacional de Desenvolvimento Cientifico e Tecnologico (CNPq, Brazil) [202078/2011-6]; National Museum of Natural History Small Grants program; Hellman Fellowship; University of California Museum of Paleontology FX We thank the staff of the Bureau of Land Management (BLM Las Cruces District Office and Patricia Hester, formerly BLM Regional Paleontologist) for permitting access to PTNM, and for generous financial support of this project (BLM L09AC15951). Jerry MacDonald originally discovered the fossil wood locality described here. Thanks to Dave Osleger for comments on carbonate accumulating environments. HFL gratefully acknowledges a NERC Advanced Fellowship (NE/F014120/2) held at Royal Holloway, University of London, and field support from the New Mexico Museum of Natural History and Science. SGL gratefully acknowledges the field assistance of Larry Rinehart and Justin Spielmann. IPM acknowledges support from NSF (EAR1024737). This material is in part based upon work supported by the NSF GRF under Grant No. DGE 1106400 to DLC. FK gratefully acknowledges a Conselho Nacional de Desenvolvimento Cientifico e Tecnologico (CNPq, Brazil) Postdoctoral Fellowship (202078/2011-6). WAD acknowledges support from the National Museum of Natural History Small Grants program. CVL acknowledges support from the Hellman Fellowship and the University of California Museum of Paleontology. NR 126 TC 2 Z9 2 U1 3 U2 88 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 SEP 1 PY 2015 VL 433 BP 158 EP 173 DI 10.1016/j.palaeo.2015.05.010 PG 16 WC Geography, Physical; Geosciences, Multidisciplinary; Paleontology SC Physical Geography; Geology; Paleontology GA CN5JU UT WOS:000358466400013 ER PT J AU Evans, LG Peplowski, PN McCubbin, FM Mccoy, TJ Nittler, LR Zolotov, MY Ebel, DS Lawrence, DJ Starr, RD Weider, SZ Solomon, SC AF Evans, Larry G. Peplowski, Patrick N. McCubbin, Francis M. McCoy, Timothy J. Nittler, Larry R. Zolotov, Mikhail Yu. Ebel, Denton S. Lawrence, David J. Starr, Richard D. Weider, Shoshana Z. Solomon, Sean C. TI Chlorine on the surface of Mercury: MESSENGER gamma-ray measurements and implications for the planet's formation and evolution SO ICARUS LA English DT Article DE Mercury, surface; Gamma-ray spectroscopy; Geological processes; Planetary formation ID ENSTATITE CHONDRITES; NEUTRON SPECTROMETER; LUNAR MANTLE; VOLCANISM; ELEMENTS; WATER; POTASSIUM; ABUNDANCE; SODIUM; ORIGIN AB Orbital measurements obtained by the MESSENGER Gamma-Ray Spectrometer have been analyzed to determine the surface abundance of chlorine in Mercury's northern hemisphere. The derived Cl/Si mass ratio is 0.0057 +/- 0.001, which for an assumed Si abundance of 24.6 wt% corresponds to 0.14 +/- 0.03 wt% Cl. The abundance of Cl is a factor of 2.9 +/- 1.3 higher in the north polar region (>80 degrees N) than at latitudes 0-60 degrees N, a latitudinal variation similar to that observed for Na. Our reported Cl abundances are consistent with measured bulk concentrations of neutron-absorbing elements on Mercury, particularly those observed at high northern latitudes. The Cl/K ratio on Mercury is chondritic, indicating a limited impact history akin to that of Mars, which accreted rapidly. Hypotheses for the origin of Mercury's high metal-to-silicate ratio must be able to reproduce Mercury's observed elemental abundances, including Cl. Chlorine is also an important magmatic volatile, and its elevated abundance in the northern polar region of Mercury indicates that it could have played a role in the production, ascent, and eruption of flood volcanic material in this region. We have identified several candidate primary mineralogical hosts for Cl on Mercury, including the halide minerals lawrencite (FeCl2), sylvite (KCl), and halite (NaCl), as well as Cl-bearing alkali sulfides. Amphiboles, micas, apatite, and aqueously deposited halides, in contrast, may be ruled out as mineralogical hosts of Cl on Mercury. (C) 2015 Elsevier Inc. All rights reserved. C1 [Evans, Larry G.] Comp Sci Corp, Lanham, MD 20706 USA. [Peplowski, Patrick N.; Lawrence, David J.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. [McCubbin, Francis M.] Univ New Mexico, Inst Meteorit, Dept Earth & Planetary Sci, Albuquerque, NM 87131 USA. [McCoy, Timothy J.] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20013 USA. [Nittler, Larry R.; Weider, Shoshana Z.; Solomon, Sean C.] Carnegie Inst Sci, Dept Terr Magnetism, Washington, DC USA. [Zolotov, Mikhail Yu.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA. [Ebel, Denton S.] Amer Museum Nat Hist, Dept Earth & Planetary Sci, New York, NY 10024 USA. [Starr, Richard D.] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA. [Solomon, Sean C.] Columbia Univ, Lamont Doherty Earth Observ, Palisades, NY 10964 USA. RP Evans, LG (reprint author), Comp Sci Corp, Lanham, MD 20706 USA. EM Larry.G.Evans@nasa.gov RI Peplowski, Patrick/I-7254-2012; Lawrence, David/E-7463-2015 OI Peplowski, Patrick/0000-0001-7154-8143; Lawrence, David/0000-0002-7696-6667 FU NASA [NAS5-97271, NASW-0002, NNX14AK43G, NNX10AI42G]; MESSENGER Participating Scientist Program FX This work was supported by the NASA Discovery Program under contracts NAS5-97271 to The Johns Hopkins University Applied Physics Laboratory and NASW-0002 to the Carnegie Institution of Washington. All of the data used in the present study are available in the Planetary Data System (PDS). Support was also provided to LGE, DJL, LRN, and RDS by the MESSENGER Participating Scientist Program. FMM and DSE acknowledge support from the NASA Cosmochemistry Program during this study (through grants NNX14AK43G and NNX10AI42G, respectively). We especially thank the dedicated MESSENGER operations team for their continued support of this mission. NR 73 TC 8 Z9 8 U1 2 U2 20 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 EI 1090-2643 J9 ICARUS JI Icarus PD SEP 1 PY 2015 VL 257 BP 417 EP 427 DI 10.1016/j.icarus.2015.04.039 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CN0KA UT WOS:000358101300033 ER PT J AU de Queiroz, LP Pastore, JFB Cardoso, D Snak, C Lima, ALD Gagnon, E Vatanparast, M Holland, AE Egan, AN AF de Queiroz, Luciano Paganucci Pastore, Jose Floriano B. Cardoso, Domingos Snak, Cristiane Lima, Ana Luisa de C. Gagnon, Edeline Vatanparast, Mohammad Holland, Ailsa E. Egan, Ashley N. TI A multilocus phylogenetic analysis reveals the monophyly of a recircumscribed papilionoid legume tribe Diocleae with well-supported generic relationships SO MOLECULAR PHYLOGENETICS AND EVOLUTION LA English DT Article DE Leguminosae; Papilionoideae; Phaseoleae; Phylogeny; Diocleinae ID INTERNAL TRANSCRIBED SPACERS; NUCLEAR RIBOSOMAL DNA; CHLOROPLAST DNA; SUBTRIBE DIOCLEINAE; FIELD PRESERVATION; LEGUMINOSAE; FABACEAE; SEQUENCES; PHASEOLEAE; POLLINATION AB Deciphering the phylogenetic relationships within the species-rich Millettioid clade has persisted as one of the major challenges in the systematics and evolutionary history of papilionoid legumes (Leguminosae, Papilionoideae). Historically, the predominantly neotropical lianas of subtribe Diocleinae in the Millettioid legumes have been taxonomically tangled together with the largely heterogeneous tribe Phaseoleae. This work presents a comprehensive molecular phylogenetic analysis based on nuclear and chloroplast markers and includes all genera ever referred to Diocleae except for the monospecific Philippine Luzonia, resolving several key generic relationships within the Millettioid legumes. The first of two separate analyses includes 310 matK accessions and strongly supports the reestablishment of tribe Diocleae as a branch of the Millettioid clade. This work sheds greater light on the higher-level phylogeny of Diocleae and allows the recognition of three major lineages: the Canavalia, Dioclea, and Galactia clades. The second set of phylogenetic analyses utilized nuclear (ITS/5.8S and ETS) and plastid (matK and tmT-Y) DNA sequences to reveal (i) the monophyly of Canavalia and Cleobulia; (ii) the monophyly of Bionia with the exclusion of Bionia belle; (iii) the paraphyly of Dioclea with respect to Cleobulia, Cymbosema, and Macropsychanthus; (iv) the paraphyly of Cratylia with respect to the broadly polyphyletic Camptosema; and (v) the polyphyly of Galactia with species scattered widely across the tree. (C) 2015 Elsevier Inc. All rights reserved. C1 [de Queiroz, Luciano Paganucci; Pastore, Jose Floriano B.; Cardoso, Domingos; Snak, Cristiane; Lima, Ana Luisa de C.] Univ Estadual Feira de Santana, Dept Ciencias Biol, BR-44036900 Feira De Santana, BA, Brazil. [Cardoso, Domingos] Univ Fed Bahia, Inst Biol, Dept Bot, BR-40170115 Salvador, BA, Brazil. [Gagnon, Edeline] Univ Montreal, Inst Rech Biol Vegetale, Dept Sci Biol, Montreal, PQ H1X 2B2, Canada. [Vatanparast, Mohammad; Egan, Ashley N.] Smithsonian Inst, Washington, DC 20013 USA. [Vatanparast, Mohammad] Chiba Univ, Grad Sch Sci, Dept Biol, Inage Ku, Chiba, Japan. [Holland, Ailsa E.] Queensland Herbarium, Brisbane Bot Gardens, Toowong, Qld 4066, Australia. RP de Queiroz, LP (reprint author), Univ Estadual Feira de Santana, Dept Ciencias Biol, Ave Transnordestina S-N, BR-44036900 Feira De Santana, BA, Brazil. EM luciano.paganucci@gmail.com RI de Queiroz, Luciano Paganucci/I-1378-2012; Cardoso, Domingos/D-1304-2014 OI de Queiroz, Luciano Paganucci/0000-0001-7436-0939; Cardoso, Domingos/0000-0001-7072-2656 FU Programa de Pesquisa em Biodiversidade do Semi-arido (PPBIO); Sistema Nacional de Pesquisa em Biodiversidade [SISBIOTA CNPq 563084/2010-3/FAPESB PES0053/2011]; PRONEX [FAPESB PNX0014/2009]; REFLORA [CNPq 563546/2010-7/FAPESB PES0054/2011]; CNPq Edital Universal [Process 473526/2011-5]; FAPESB [Process PET0039/2012]; Pq/CNPq; PDJ/CNPq FX We thank to John Gwaltney and Charles Bryson for providing leaf material of Lackeya multiflora from USA; Roger Graveson for the leaf material of Galactia longiflora from Saint Lucia; Roberto Salas for leaf material of Dioclea burkartii and D. paraguariensis from Argentina; Abel Conceicao for leaf material of Rhodopis planisiliqua from Dominican Republic; Elvia Souza, Patricia Jesus, M. Torres, Laura Lima, Haroldo Lima, Cassio van den Berg, Jomar Jardim, and Rafaela Forzza for the leaf material of several species from Brazil. Jefferson G. Carvalho-Sobrinho, Petala Ribeiro, Francisco Haroldo Nascimento, Ricardo Machado, Raymond Harley, Ana Maria Giulietti-Harley (UEFS), Charles Zartman (INPA), Elsa Cabral, Roberto Salas, and Andrea Cabanas (IBONE, Argentina) provided help and support during fieldwork. Seeds of species of Dioclea and Galactia from the forage germplasm collection were provided by the Centro Internacional de Agricultura Tropical (CAT, Cali, Colombia) and the transference of seeds to Brazil was kindly arranged by Luis Guillermo Santos Melendez (CAT, Programa de Recursos Geneticos), Marcelo Fragomeni Simon, and Manuela Oliveira (Embrapa, Centro Nacional de Recursos Geneticos e Biotecnologia, Brazil). DNA extraction from herbarium material of Macropsychanthus and some North-American species of Galactia was kindly allowed by Gwil Lewis (K) and Matt Lavin (MONT). Fieldwork and DNA sequencing were sponsored by Programa de Pesquisa em Biodiversidade do Semi-arido (PPBIO), Sistema Nacional de Pesquisa em Biodiversidade (SISBIOTA CNPq 563084/2010-3/FAPESB PES0053/2011), PRONEX (FAPESB PNX0014/2009), REFLORA (CNPq 563546/2010-7/FAPESB PES0054/2011), and CNPq Edital Universal (Process 473526/2011-5). DC also acknowledges FAPESB (Process PET0039/2012) for providing financial support to his research on phylogenetics. LPQ is continuously supported by a Pq/CNPq fellowship and DC and JFBP were supported by PDJ/CNPq fellowships while postdocs at Universidade Estadual de Feira de Santana. NR 104 TC 2 Z9 2 U1 3 U2 20 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 1055-7903 EI 1095-9513 J9 MOL PHYLOGENET EVOL JI Mol. Phylogenet. Evol. PD SEP PY 2015 VL 90 BP 1 EP 19 DI 10.1016/j.ympev.2015.04.016 PG 19 WC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity SC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity GA CM8PW UT WOS:000357965100001 PM 25934529 ER PT J AU Glowska, E Laniecka, I Milensky, CM AF Glowska, Eliza Laniecka, Izabella Milensky, Christopher M. TI Two new picobiin mite species (Acari: Cheyletoidea: Syringophilidae) parasitizing passerine birds in Guyana SO ACTA PARASITOLOGICA LA English DT Article DE Quill mites; Syringophilidae; Neopicobia; Rafapicobia; ectoparasites; systematics AB Two new picobiin mite species (Cheyletoidea: Syringophilidae) are described from passeriform birds in Guyana, Rafapicobia automoli sp. nov. parasitizing two furnariid species Automolus ochrolaemus (Tschudi) (type host) and Automolus rufipileatus (Pelzeln) (Passeriformes: Furnariidae) and Neopicobia herbicolae sp. nov. from Emberizoides herbicola (Vieillot) (Thraupidae). Additionally, Picumnus exilis (Lichtenstein) (Piciformes: Picidae) is recorded as a new host species for Neopicobia hepburni Glowska et Laniecka, 2014. C1 [Glowska, Eliza; Laniecka, Izabella] Adam Mickiewicz Univ, Dept Anim Morphol, Fac Biol, PL-61614 Poznan, Poland. [Milensky, Christopher M.] Smithsonian Inst, Div Birds, Washington, DC 20013 USA. RP Glowska, E (reprint author), Adam Mickiewicz Univ, Dept Anim Morphol, Fac Biol, Umultowska 89, PL-61614 Poznan, Poland. EM glowska@amu.edu.pl NR 13 TC 0 Z9 0 U1 1 U2 3 PU WALTER DE GRUYTER GMBH PI BERLIN PA GENTHINER STRASSE 13, D-10785 BERLIN, GERMANY SN 1230-2821 EI 1896-1851 J9 ACTA PARASITOL JI Acta Parasitolog. PD SEP PY 2015 VL 60 IS 3 BP 488 EP 493 DI 10.1515/ap-2015-0069 PG 6 WC Parasitology SC Parasitology GA CK6MC UT WOS:000356341200019 PM 26204188 ER PT J AU Foster, BL Ao, M Willoughby, C Soenjaya, Y Holm, E Lukashova, L Tran, AB Wimer, HF Zerfas, PM Nociti, FH Kantovitz, KR Quan, BD Sone, ED Goldberg, HA Somerman, MJ AF Foster, B. L. Ao, M. Willoughby, C. Soenjaya, Y. Holm, E. Lukashova, L. Tran, A. B. Wimer, H. F. Zerfas, P. M. Nociti, F. H., Jr. Kantovitz, K. R. Quan, B. D. Sone, E. D. Goldberg, H. A. Somerman, M. J. TI Mineralization defects in cementum and craniofacial bone from loss of bone sialoprotein SO BONE LA English DT Article DE Extracellular matrix; Mineralization; Bone; Cementum; Dentin; Cartilage ID DENTIN MATRIX PROTEIN-1; EXTRINSIC FIBER CEMENTUM; IN-VITRO; HYDROXYAPATITE FORMATION; MOUSE MODEL; SKELETAL MINERALIZATION; PERIODONTAL ATTACHMENT; EXTRACELLULAR-MATRIX; ACELLULAR CEMENTUM; SIBLING PROTEINS AB Bone sialoprotein (BSP) is a multifunctional extracellular matrix protein found in mineralized tissues, including bone, cartilage, tooth root cementum (both acellular and cellular types), and dentin. In order to define the role BSP plays in the process of biomineralization of these tissues, we analyzed cementogenesis, dentinogenesis, and osteogenesis (intramembranous and endochondral) in craniofacial bone in Bsp null mice and wild-type (WT) controls over a developmental period (1-60 days post natal; dpn) by histology, immunohistochemistry, undecalcified histochemistry, microcomputed tomography (microCT), scanning electron microscopy (SEM), transmission electron microscopy (TEM), and quantitative PCR (qPCR). Regions of intramembranous ossification in the alveolus, mandible, and calvaria presented delayed mineralization and osteoid accumulation, assessed by von Kossa and Goldner's trichrome stains at 1 and 14 dpn. Moreover, Bsp(-/-) mice featured increased cranial suture size at the early time point, 1 dpn. Immunostaining and PCR demonstrated that osteoblast markers, osterix, alkaline phosphatase, and osteopontin were unchanged in Bsp null mandibles compared to WT. Bsp(-/-) mouse molars featured a lack of functional acellular cementum formation by histology, SEM, and TEM, and subsequent loss of Sharpey's collagen fiber insertion into the tooth root structure. Bsp(-/-) mouse alveolar and mandibular bone featured equivalent or fewer osteoclasts at early ages (1 and 14 dpn), however, increased RANKL immunostaining and mRNA, and significantly increased number of osteodast-like cells (2-5 fold) were found at later ages (26 and 60 dpn), corresponding to periodontal breakdown and severe alveolar bone resorption observed following molar teeth entering occlusion. Dentin formation was unperturbed in Bsp(-/-) mouse molars, with no delay in mineralization, no alteration in dentin dimensions, and no differences in odontoblast markers analyzed. No defects were identified in endochondral ossification in the cranial base, and craniofacial morphology was unaffected in Bsp(-/-) mice. These analyses confirm a critical role for BSP in processes of cementogenesis and intramembranous ossification of craniofacial bone, whereas endochondral ossification in the cranial base was minimally affected and dentinogenesis was normal in Bsp(-/-) molar teeth. Dissimilar effects of loss of BSP on mineralization of dental and craniofacial tissues suggest local differences in the role of BSP and/or yet to be defined interactions with site-specific factors. Published by Elsevier Inc. C1 [Foster, B. L.; Ao, M.; Willoughby, C.; Tran, A. B.; Nociti, F. H., Jr.; Kantovitz, K. R.; Somerman, M. J.] Natl Inst Arthrit & Musculoskeletal & Skin Dis NI, NIH, Bethesda, MD 20892 USA. [Willoughby, C.; Goldberg, H. A.] Univ Western Ontario, Biomed Engn Program, Schulich Sch Med & Dent, London, ON N6A 5C1, Canada. [Holm, E.; Goldberg, H. A.] Univ Western Ontario, Dept Biochem, Schulich Sch Med & Dent, London, ON N6A 5C1, Canada. [Lukashova, L.] Hosp Special Surg, New York, NY 10021 USA. [Wimer, H. F.] Smithsonian Inst, Dept Vertebrate Zool, Natl Museum Nat Hist, Washington, DC 20560 USA. [Zerfas, P. M.] Off Res Serv, NIH, Div Vet Resources, Bethesda, MD 20892 USA. [Nociti, F. H., Jr.] Univ Estadual Campinas, Sch Dent, Div Periodont, Dept Prosthodont & Periodont, BR-13414903 Piracicaba, SP, Brazil. [Kantovitz, K. R.] Univ Estadual Campinas, Dept Pediat Dent, Sch Dent, BR-13414903 Piracicaba, SP, Brazil. [Quan, B. D.; Sone, E. D.] Univ Toronto, Inst Biomat & Biomed Engn, Toronto, ON M5S 3G9, Canada. [Sone, E. D.] Univ Toronto, Dept Mat Sci & Engn, Toronto, ON M5S 3G9, Canada. [Sone, E. D.] Univ Toronto, Fac Dent, Toronto, ON M5S 3G9, Canada. [Goldberg, H. A.] Univ Western Ontario, Sch Dent, Schulich Sch Med & Dent, London, ON N6A 5C1, Canada. RP Foster, BL (reprint author), Natl Inst Arthrit & Musculoskeletal & Skin Dis NI, NIH, Bldg 50 Room 4120, Bethesda, MD 20892 USA. EM brian.foster@nih.gov; fnu.aomin@nih.gov; chelseawilloughby15@gmail.com; yosoenjay@uwo.ca; eholm@uwa.ca; lukashoval@hss.edu; anne.tran2@nih.gov; helen.wimer@nih.gov; patricia.zerfas@nih.gov; nociti@unicamp.br; kamilark@yahoo.com.br; bryan.quan@utoronto.ca; eli.sone@utotonto.ca; hagoldbe@uwo.ca; Martha.somerman@nih.gov RI Foster, Brian/H-8375-2015; Kantovitz, Kamila/J-4567-2013 OI Foster, Brian/0000-0003-3444-0576; Kantovitz, Kamila/0000-0003-2045-7924 FU National Institute of Arthritis and Musculoskeletal and Skin Diseases (NIAMS)/NIH [AR 066110]; Intramural Research Program of NIAMS; Canadian Institutes of Health Research [130572]; CIHR Institute of Musculoskeletal Health and Arthritis [134216] FX This research was supported by sources including grant AR 066110 to BLF from the National Institute of Arthritis and Musculoskeletal and Skin Diseases (NIAMS)/NIH, the Intramural Research Program of NIAMS (MJS), the Canadian Institutes of Health Research (#130572; HAG), and the CIHR Institute of Musculoskeletal Health and Arthritis (#134216; EDS). We thank Kenn Holmbeck of the National Institute of Dental and Craniofacial Research (NIDCR) for assistance with microCT analysis and Nasrin Kalantari Pour (NIAMS) for assistance with histology. NR 88 TC 5 Z9 5 U1 6 U2 29 PU ELSEVIER SCIENCE INC PI NEW YORK PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA SN 8756-3282 EI 1873-2763 J9 BONE JI Bone PD SEP PY 2015 VL 78 BP 150 EP 164 DI 10.1016/j.bone.2015.05.007 PG 15 WC Endocrinology & Metabolism SC Endocrinology & Metabolism GA CK9LQ UT WOS:000356562000019 PM 25963390 ER PT J AU Hara, H Smith, DR AF Hara, Hideho Smith, David R. TI Japanese species of the sawfly genus Nesodiprion (Hymenoptera, Diprionidae) SO ZOOTAXA LA English DT Article DE Symphyta; new host record; new distribution record ID SYMPHYTA; NOV.; KEY AB Nesodiprion flavipes sp. nov. associated with Tsuga diversifolia (Maxim.) Mast. and N. kojimai sp. nov. associated with Abies veitchii Lindl. are described from Honshu, Japan. Additional taxonomic and biological information is given for other Japanese congeners, N. japonicus (Marlatt, 1898), N. albiventris Togashi, 1998, N. shinoharai Togashi, 1998, N. nigerrimus Togashi, 1998, N. kagaensis Togashi, 1998, N. niger Togashi, 2001 and N. tsugae Togashi, 2001. The males of N. shinoharai, N. kagaensis and N. tsugae are described for the first time. The host plants of N. shinoharai are Pinus spp. Nesodiprion kagaensis is newly recorded from Hokkaido, Japan, and its host plants are Pinus spp. and Larix kaempferi (Lamb.) Carriere. Larvae of N. japonicus and N. kagaensis are briefly described. A division of Nesodiprion into the following five species groups is proposed: N. tsugae group, N. niger group, N. flavipes group, N. japonicus group and N. shinoharai group. Additions to the key to Nesodiprion species by Hara & Smith (2012) are given. C1 [Hara, Hideho] Hokkaido Res Org, Forestry Res Inst, Bibai, Hokkaido 0790198, Japan. [Smith, David R.] ARS, Systemat Entomol Lab, PSI, USDA,Natl Museum Natl Hist,Smithsonian Inst, Washington, DC 20013 USA. RP Hara, H (reprint author), Hokkaido Res Org, Forestry Res Inst, Bibai, Hokkaido 0790198, Japan. EM hara-hideho@hro.or.jp; sawfly2@aol.com FU JSPS KAKENHI [20580165, 25440223] FX We deeply appreciate H. Kojima (Nagano) for offering valuable material and information and A. Shinohara (NSMT) for his kind help in various ways. Our thanks are also due N. Hirai and S. Kobayashi (OPU), T. Hirowatari (Kyushu University), K. Maeto (KU), H. Nagase (Kamakura), M. Ohara (HU), K. Ozaki (FFPRIH) and I. Togashi (Hakusan) for gifts or loans of the material for this study. We appreciate the comments and suggestions of two anonymous reviewers for improvement of the manuscript. This study was partly supported by JSPS KAKENHI Grant No. 20580165 and No. 25440223. NR 24 TC 1 Z9 1 U1 0 U2 2 PU MAGNOLIA PRESS PI AUCKLAND PA PO BOX 41383, AUCKLAND, ST LUKES 1030, NEW ZEALAND SN 1175-5326 EI 1175-5334 J9 ZOOTAXA JI Zootaxa PD AUG 31 PY 2015 VL 4007 IS 4 BP 481 EP 508 PG 28 WC Zoology SC Zoology GA CQ1LL UT WOS:000360359100002 PM 26623828 ER PT J AU Strandburg-Peshkin, A Farine, DR Couzin, ID Crofoot, MC AF Strandburg-Peshkin, Ariana Farine, Damien R. Couzin, Iain D. Crofoot, Margaret C. TI The wisdom of baboon decisions Response SO SCIENCE LA English DT Letter ID CONSENSUS DECISION; ANIMAL GROUPS C1 [Strandburg-Peshkin, Ariana; Couzin, Iain D.] Princeton Univ, Dept Ecol & Evolutionary Biol, Princeton, NJ 08544 USA. [Farine, Damien R.; Crofoot, Margaret C.] Univ Calif Davis, Dept Anthropol, Davis, CA 95616 USA. [Farine, Damien R.; Crofoot, Margaret C.] Smithsonian Trop Res Inst, Panama City, Panama. [Farine, Damien R.] Univ Oxford, Edward Grey Inst Field Ornithol, Dept Zool, Oxford OX1 3PS, England. [Couzin, Iain D.] Max Planck Inst Ornithol, Dept Collect Behav, D-78457 Constance, Germany. [Couzin, Iain D.] Univ Konstanz, Dept Biol, Chair Biodivers & Collect Behav, D-78457 Constance, Germany. RP Strandburg-Peshkin, A (reprint author), Princeton Univ, Dept Ecol & Evolutionary Biol, Princeton, NJ 08544 USA. EM astrandb@princeton.edu; damien.farine@zoo.ox.ac.uk; mccrofoot@ucdavis.edu NR 6 TC 0 Z9 0 U1 3 U2 25 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 AUG 28 PY 2015 VL 349 IS 6251 BP 935 EP 936 PG 2 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA CQ5LW UT WOS:000360646800028 PM 26315425 ER PT J AU Lea, AM Ryan, MJ AF Lea, Amanda M. Ryan, Michael J. TI SEXUAL SELECTION Irrationality in mate choice revealed by tungara frogs SO SCIENCE LA English DT Article ID MATING SIGNALS; PREFERENCE; DOMINANCE; ECONOMICS; ABSOLUTE; DECISION; UTILITY; SPACE AB Mate choice models derive from traditional microeconomic decision theory and assume that individuals maximize their Darwinian fitness by making economically rational decisions. Rational choices exhibit regularity, whereby the relative strength of preferences between options remains stable when additional options are presented. We tested female frogs with three simulated males who differed in relative call attractiveness and call rate. In binary choice tests, females' preferences favored stimulus caller B over caller A; however, with the addition of an inferior "decoy" C, females reversed their preferences and chose A over B. These results show that the relative valuation of mates is not independent of inferior alternatives in the choice set and therefore cannot be explained with the rational choice models currently used in sexual selection theory. C1 [Lea, Amanda M.; Ryan, Michael J.] Univ Texas Austin, Dept Integrat Biol, Austin, TX 78712 USA. [Ryan, Michael J.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. RP Lea, AM (reprint author), Univ Texas Austin, Dept Integrat Biol, Austin, TX 78712 USA. EM alea@utexas.edu FU NSF [1120031] FX We thank the Autoridad Nacional del Ambiente for permission to do field work in Panama; the Smithsonian Tropical Research Institute for logistical support; M. Still, S. Beckett, and A. Smejdir for assistance; and M. Jennions and an anonymous reviewer for helpful suggestions on the manuscript. M.J.R. thanks M. Bateson for early conversations on decoys. This study was supported by NSF Integrative Organismal Systems grant 1120031 to M.J.R., R. Taylor, and R. Page and an NSF Predoctoral Fellowship to A.M.L. Procedures were approved by the Institutional Animal Care and Use Committees at The University of Texas at Austin and the Smithsonian Tropical Research Institute (AUP 2011-0825-2014-02). Experimental data are provided in the supplementary materials. NR 24 TC 10 Z9 11 U1 11 U2 54 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 AUG 28 PY 2015 VL 349 IS 6251 BP 964 EP 966 DI 10.1126/science.aab2012 PG 3 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA CQ5LW UT WOS:000360646800050 PM 26315434 ER PT J AU Bahia, RG Amado, GM Maneveldt, GW Adey, WH Johnson, G Jesionek, MB Longo, LL AF Bahia, Ricardo G. Amado-Filho, Gilberto M. Maneveldt, Gavin W. Adey, Walter H. Johnson, Gabriel Jesionek, Michel B. Longo, Leila L. TI Sporolithon yoneshigueae sp nov (Sporolithales, Corallinophycidae, Rhodophyta), a new rhodolith-forming coralline alga from the southwest Atlantic SO PHYTOTAXA LA English DT Article DE genetic marker; molecular phylogeny; Sporolithaceae; taxonomy ID PTYCHOIDES HEYDRICH; RED ALGAE; SPERMONDE ARCHIPELAGO; PHYLOGENY; SEQUENCES; AFRICA; GENUS; PSBA; CERAMIACEAE; MORPHOLOGY AB The aim of this study was to describe the new rhodolith-forming coralline alga species, Sporolithon yoneshigueae sp. nov., based on both morpho-anatomical and molecular data. Specimens were collected in rhodolith beds between 28 and 66 m depths in northeastern and southeastern Brazil. The new species can be distinguished from all other species of the genus Sporolithon by its wide tetrasporangial compartment pore diameter (35-43 mu m) and the correspondingly large number (19-24) of rosette cells surrounding the tetrasporangial compartment pore. Phylogenies inferred from psbA and SSU markers support it as a new species within Sporolithon with interspecific genetic divergence varying from 8.86-10.94 %, and 3.67-4.63%, respectively. Observations from recent gathering and from herbarium collections show that specimens previously designated as Sporolithon mediterraneum in Brazil correspond to Sporolithon yoneshigueae. C1 [Bahia, Ricardo G.; Amado-Filho, Gilberto M.; Longo, Leila L.] Diretoria Pesquisa Cient, Inst Pesquisas Jardim Bot Rio de Janeiro, BR-22460030 Rio De Janeiro, RJ, Brazil. [Maneveldt, Gavin W.] Univ Western Cape, Dept Biodivers & Conservat Biol, ZA-7535 Bellville, South Africa. [Adey, Walter H.; Johnson, Gabriel] Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, Washington, DC 20560 USA. [Jesionek, Michel B.] Univ Fed Rio de Janeiro, Ctr Ciencias Saude, Inst Biol, BR-21941900 Rio De Janeiro, RJ, Brazil. RP Amado, GM (reprint author), Diretoria Pesquisa Cient, Inst Pesquisas Jardim Bot Rio de Janeiro, Rua Pacheco Leao 915, BR-22460030 Rio De Janeiro, RJ, Brazil. EM gilbertoamadofilho@gmail.com FU CNPq; CAPES; FAPERJ; South African National Research Foundation; CNPq (National Research Council-Brazil); FAPES (Fundacao de Amparo a Pesquisa do Espirito Santo); Brasoil/ANP FX We are thankful to Dr. Mariana Cabral Oliveira (Universidade de Sao Paulo) for their important suggestions to improve the manuscript quality. RGB, GMAF, LL and RGB acknowledge the Brazilian Scientific Agencies CNPq, CAPES and FAPERJ for grants, postdocs and postgraduate scholarships. GWM acknowledges research support from the South African National Research Foundation. This work is a contribution of the Rede Abrolhos/SISBIOTA and PELD Abrolhos surveys. Financial support was obtained from CNPq (National Research Council-Brazil), FAPES (Fundacao de Amparo a Pesquisa do Espirito Santo) and Brasoil/ANP. NR 55 TC 2 Z9 2 U1 0 U2 5 PU MAGNOLIA PRESS PI AUCKLAND PA PO BOX 41383, AUCKLAND, ST LUKES 1030, NEW ZEALAND SN 1179-3155 EI 1179-3163 J9 PHYTOTAXA JI Phytotaxa PD AUG 28 PY 2015 VL 224 IS 2 BP 140 EP 158 DI 10.11646/phytotaxa.224.2.2 PG 19 WC Plant Sciences SC Plant Sciences GA CP8JM UT WOS:000360139800002 ER PT J AU Babb, JF AF Babb, James F. TI Empirically constructed dynamic electric dipole polarizability function of magnesium and its applications SO PHYSICAL REVIEW A LA English DT Article ID PHOTOIONIZATION CROSS-SECTIONS; MG ISOELECTRONIC SEQUENCE; LONG-RANGE INTERACTIONS; GROUND-STATE MAGNESIUM; DER-WAALS COEFFICIENTS; RADIATIVE ATOMIC DATA; L2 CI CALCULATION; OSCILLATOR-STRENGTHS; TRANSITION-PROBABILITIES; NEUTRAL MAGNESIUM AB The dynamic electric dipole polarizability function for the magnesium atom is formed by assembling the atomic electric dipole oscillator strength distribution from combinations of theoretical and experimental data for resonance oscillator strengths and for photoionization cross sections of valence and inner shell electrons. Consistency with the oscillator strength (Thomas-Reiche-Kuhn) sum rule requires the adopted principal resonance line oscillator strength to be several percent lower than the values given in two critical tabulations, though the value adopted is consistent with a number of theoretical determinations. The static polarizability is evaluated. Comparing the resulting dynamic polarizability as a function of the photon energy with more elaborate calculations reveals the contributions of inner shell electron excitations. The present results are applied to calculate the long-range interactions between two and three magnesium atoms and the interaction between a magnesium atom and a perfectly conducting metallic plate. Extensive comparisons of prior results for the principal resonance line oscillator strength, for the static polarizability, and for the van der Waals coefficient are given in the Appendix. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Babb, JF (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS 14, Cambridge, MA 02138 USA. OI Babb, James/0000-0002-3883-9501 FU National Science Foundation FX Discussions with C. Ballance, T. G. Lee, T. Gorczyca, C. F. Fischer, S. Manson, and M. Bromley are gratefully acknowledged. This work was supported in part by grants for ITAMP from the National Science Foundation to the Smithsonian Institution and to Harvard University. I thank Dr. Y. Singh for communicating his recent result. NR 123 TC 1 Z9 1 U1 3 U2 10 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 1050-2947 EI 1094-1622 J9 PHYS REV A JI Phys. Rev. A PD AUG 27 PY 2015 VL 92 IS 2 AR 022712 DI 10.1103/PhysRevA.92.022712 PG 10 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA CP8DJ UT WOS:000360121600006 ER PT J AU Miyamoto, K Nonaka, A Oka, SI AF Miyamoto, Kei Nonaka, Ai Oka, Shin-Ichiro TI Northernmost record of a poorly known tuskfish, Choerodon margaritiferus (Perciformes: Labridae), from southern Japan, and first description of a female SO ZOOTAXA LA English DT Article DE Pisces; labrid; distribution; Okinawa; Japan AB We describe 5 specimens of Choerodon margaritiferus Fowler and Bean, 1928 (94.5-107.0 mm standard length, 1 male and 4 females) collected near Okinawa Island, southern Japan. This is the northernmost record of this species and the first record of it in Japanese waters; until now, C. margaritiferus was recorded only from the western central Pacific. This species was originally described on the basis of 1 male specimen, and all additional specimens described in the literature were also male. Morphological characters of both sexes are described, and new diagnostic characters of the female are presented. C1 [Miyamoto, Kei; Oka, Shin-Ichiro] Okinawa Churashima Fdn, Motobu, Okinawa 9050206, Japan. [Nonaka, Ai] Natl Museum Nat Hist, Smithsonian Inst, Washington, DC 20560 USA. RP Miyamoto, K (reprint author), Okinawa Churashima Fdn, Ishikawa 888, Motobu, Okinawa 9050206, Japan. EM k-miyamoto@okichura.jp NR 18 TC 0 Z9 0 U1 1 U2 4 PU MAGNOLIA PRESS PI AUCKLAND PA PO BOX 41383, AUCKLAND, ST LUKES 1030, NEW ZEALAND SN 1175-5326 EI 1175-5334 J9 ZOOTAXA JI Zootaxa PD AUG 26 PY 2015 VL 4007 IS 1 BP 82 EP 90 PG 9 WC Zoology SC Zoology GA CP6OS UT WOS:000360007600005 PM 26623789 ER PT J AU Basset, Y Barrios, H Segar, S Srygley, RB Aiello, A Warren, AD Delgado, F Coronado, J Lezcano, J Arizala, S Rivera, M Perez, F Bobadilla, R Lopez, Y Ramirez, JA AF Basset, Yves Barrios, Hector Segar, Simon Srygley, Robert B. Aiello, Annette Warren, Andrew D. Delgado, Francisco Coronado, James Lezcano, Jorge Arizala, Stephany Rivera, Marleny Perez, Filonila Bobadilla, Ricardo Lopez, Yacksecari Alejandro Ramirez, Jose TI The Butterflies of Barro Colorado Island, Panama: Local Extinction since the 1930s SO PLOS ONE LA English DT Article ID TROPICAL RAIN-FORESTS; NEOTROPICAL BUTTERFLIES; HELICONIUS BUTTERFLIES; BRITISH BUTTERFLIES; DNA BARCODES; EL-NINO; LEPIDOPTERA; ECOLOGY; CONSERVATION; ASSEMBLAGES AB Few data are available about the regional or local extinction of tropical butterfly species. When confirmed, local extinction was often due to the loss of host-plant species. We used published lists and recent monitoring programs to evaluate changes in butterfly composition on Barro Colorado Island (BCI, Panama) between an old (1923-1943) and a recent (19932013) period. Although 601 butterfly species have been recorded from BCI during the 1923-2013 period, we estimate that 390 species are currently breeding on the island, including 34 cryptic species, currently only known by their DNA Barcode Index Number. Twenty-three butterfly species that were considered abundant during the old period could not be collected during the recent period, despite a much higher sampling effort in recent times. We consider these species locally extinct from BCI and they conservatively represent 6% of the estimated local pool of resident species. Extinct species represent distant phylogenetic branches and several families. The butterfly traits most likely to influence the probability of extinction were host growth form, wing size and host specificity, independently of the phylogenetic relationships among butterfly species. On BCI, most likely candidates for extinction were small hesperiids feeding on herbs (35% of extinct species). However, contrary to our working hypothesis, extinction of these species on BCI cannot be attributed to loss of host plants. In most cases these host plants remain extant, but they probably subsist at lower or more fragmented densities. Coupled with low dispersal power, this reduced availability of host plants has probably caused the local extinction of some butterfly species. Many more bird than butterfly species have been lost from BCI recently, confirming that small preserves may be far more effective at conserving invertebrates than vertebrates and, therefore, should not necessarily be neglected from a conservation viewpoint. C1 [Basset, Yves; Srygley, Robert B.; Aiello, Annette; Coronado, James; Lezcano, Jorge; Arizala, Stephany; Perez, Filonila; Bobadilla, Ricardo; Lopez, Yacksecari; Alejandro Ramirez, Jose] Smithsonian Trop Res Inst, Panama City, Panama. [Basset, Yves; Segar, Simon] Univ South Bohemia, Fac Sci, Ceske Budejovice 37005, Czech Republic. [Basset, Yves; Segar, Simon] Acad Sci Czech Republic, Inst Entomol, Ctr Biol, CR-37005 Ceske Budejovice, Czech Republic. [Basset, Yves; Barrios, Hector; Rivera, Marleny] Univ Panama, Maestria Entomol, Panama City 080814, Panama. [Srygley, Robert B.] ARS, Northern Plains Agr Lab, USDA, Sidney, MT 59270 USA. [Warren, Andrew D.] Univ Florida, Florida Museum Nat Hist, McGuire Ctr Lepidoptera & Biodivers, Gainesville, FL 32611 USA. [Delgado, Francisco] Univ Panama, Ctr Reg Univ Veraguas, Santiago, Panama. RP Basset, Y (reprint author), Smithsonian Trop Res Inst, Apartado 0843-03092, Panama City, Panama. EM bassety@si.edu RI Segar, Simon/K-6783-2015; Basset, Yves/B-6642-2014 FU Smithsonian Institution Barcoding Opportunity [FY012, FY013]; Czech Science foundation GACR [41-14-36068G]; USB Postdoc project - EU Education for Competitiveness Operational Programme [CZ.1.07/2.3.00/30.0006]; European Social Fund; Czech State Budget; STRI; NSF Graduate Research Fellowship; OTS-Mellon award; NSF [DEB 9419543, DEB 9119619] FX Grants from the Smithsonian Institution Barcoding Opportunity FY012 and FY013 and in-kind help from the Canadian Centre for DNA Barcoding via Paul Hebert and Alex Borisenko at the Biodiversity Institute of Ontario allowed the sequencing of many of the butterfly specimens collected recently on BCI. YB was supported by Czech Science foundation GACR grant 41-14-36068G and is a member of the Sistema Nacional de Investigacion, SENACYT, Panama. SS was funded by a USB Postdoc project (reg. no. CZ.1.07/2.3.00/30.0006), funded by the EU Education for Competitiveness Operational Programme, the European Social Fund and the Czech State Budget. RBS's sampling was supported by a short-term Fellowship from STRI, an NSF Graduate Research Fellowship, and an OTS-Mellon award. Tom Kursar kindly made available the BCI butterfly data of P.D. Coley and T.A. Kursar, which were supported by NSF grants DEB 9419543 and DEB 9119619. NR 95 TC 6 Z9 7 U1 2 U2 15 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 AUG 25 PY 2015 VL 10 IS 8 AR e0136623 DI 10.1371/journal.pone.0136623 PG 22 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA CP6KK UT WOS:000359995500100 PM 26305111 ER PT J AU Farfurnik, D Jarmola, A Pham, LM Wang, ZH Dobrovitski, VV Walsworth, RL Budker, D Bar-Gill, N AF Farfurnik, D. Jarmola, A. Pham, L. M. Wang, Z. H. Dobrovitski, V. V. Walsworth, R. L. Budker, D. Bar-Gill, N. TI Optimizing a dynamical decoupling protocol for solid-state electronic spin ensembles in diamond SO PHYSICAL REVIEW B LA English DT Article ID COHERENCE TIME; RESOLUTION; SEQUENCES; CENTERS; BATH; NMR AB We demonstrate significant improvements of the spin coherence time of a dense ensemble of nitrogen-vacancy (NV) centers in diamond through optimized dynamical decoupling (DD). Cooling the sample down to 77 K suppresses longitudinal spin relaxation T-1 effects and DD microwave pulses are used to increase the transverse coherence time T-2 from similar to 0.7 ms up to similar to 30 ms. We extend previous work of single-axis (Carr-Purcell-Meiboom-Gill) DD towards the preservation of arbitrary spin states. Following a theoretical and experimental characterization of pulse and detuning errors, we compare the performance of various DD protocols. We identify that the optimal control scheme for preserving an arbitrary spin state is a recursive protocol, the concatenated version of the XY8 pulse sequence. The improved spin coherence might have an immediate impact on improvements of the sensitivities of ac magnetometry. Moreover, the protocol can be used on denser diamond samples to increase coherence times up to NV-NV interaction time scales, a major step towards the creation of quantum collective NV spin states. C1 [Farfurnik, D.; Bar-Gill, N.] Hebrew Univ Jerusalem, Racah Inst Phys, IL-9190401 Jerusalem, Israel. [Farfurnik, D.; Bar-Gill, N.] Hebrew Univ Jerusalem, Ctr Nanosci & Nanotechnol, IL-9190401 Jerusalem, Israel. [Jarmola, A.; Budker, D.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. [Pham, L. M.; Walsworth, R. L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Wang, Z. H.] Univ So Calif, Dept Chem, Los Angeles, CA 90089 USA. [Dobrovitski, V. V.] Iowa State Univ, Ames Lab, Ames, IA 50011 USA. [Walsworth, R. L.] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. [Budker, D.] Johannes Gutenberg Univ Mainz, Helmholtz Inst, D-55099 Mainz, Germany. [Bar-Gill, N.] Hebrew Univ Jerusalem, Dept Appl Phys, Rachel & Selim Sch Engn, IL-9190401 Jerusalem, Israel. RP Farfurnik, D (reprint author), Hebrew Univ Jerusalem, Racah Inst Phys, IL-9190401 Jerusalem, Israel. RI Budker, Dmitry/F-7580-2016 OI Budker, Dmitry/0000-0002-7356-4814 FU EU CIG; Minerva ARCHES award; Israel Science Foundation [750/14]; Ministry of Science and Technology, Israel; German-Israeli Project Cooperation (DIP) program; NSF [ECCS-1202258]; AFOSR/DARPA QuASAR program; U.S. Department of Energy-Basic Energy Sciences [DE-AC02-07CH11358]; CAMBR fellowship for Nanoscience and Nanotechnology; Binational Science Foundation Rahamimoff travel grant FX We thank Gonzalo A. Alvarez for fruitful discussions. This work has been supported in part by the EU CIG, the Minerva ARCHES award, the Israel Science Foundation (Grant No. 750/14), and the Ministry of Science and Technology, Israel. Additional support was provided by the German-Israeli Project Cooperation (DIP) program, the NSF through Grant No. ECCS-1202258, and the AFOSR/DARPA QuASAR program. Work at Ames Laboratory was supported by the U.S. Department of Energy-Basic Energy Sciences under Contract No. DE-AC02-07CH11358. D.F. was partially supported by the CAMBR fellowship for Nanoscience and Nanotechnology, and the Binational Science Foundation Rahamimoff travel grant. NR 39 TC 12 Z9 12 U1 3 U2 23 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 1098-0121 EI 1550-235X J9 PHYS REV B JI Phys. Rev. B PD AUG 24 PY 2015 VL 92 IS 6 AR 060301 DI 10.1103/PhysRevB.92.060301 PG 5 WC Physics, Condensed Matter SC Physics GA CS6SO UT WOS:000362212200002 ER PT J AU Holzmeyer, L Duretto, M Crayn, D Horandl, E Heslewood, M Jayanthan, J Appelhans, MS AF Holzmeyer, Laura Duretto, Marco Crayn, Darren Hoerandl, Elvira Heslewood, Margaret Jayanthan, Janani Appelhans, Marc S. TI Phylogeny of Acronychia (Rutaceae) and First Insights into Its Historical Biogeography and the Evolution of Fruit Characters SO PLOS ONE LA English DT Article ID MOLECULAR PHYLOGENY; CLADISTIC-ANALYSIS; NONCODING REGIONS; GEOGRAPHIC RANGE; CHLOROPLAST DNA; REVISION; SUBFAMILIES; DISPERSAL; INFERENCE; MELICOPE AB Background The genus Acronychia (Citrus family, Rutaceae) contains 49 species of trees and shrubs that are found mainly in rain forest. The genus has a large distributional range from mainland southern Asia to Australia and New Caledonia, but most species are endemic to either New Guinea or Australia. This study aimed to provide the first detailed molecular phylogeny of Acronychia and use it to test the taxonomic value of fruit morphological characters, and infer the historical biogeography of the genus. Methodology Phylogenetic analyses (Bayesian Inference, Maximum Likelihood) were undertaken on nucleotide sequence data from two plastid (psbA-trnH, trnL-trnF) and three nuclear markers (ETS, ITS, NIAi3) from 29 Acronychia species (59% of the genus) and representatives of related genera. Results and Conclusions The results indicate that the South-East Asian genus Maclurodendron is nested phylogenetically within Acronychia and must be synonymized to render Acronychia monophyletic. Fruit morphological characters have been used previously to infer relationships within Acronychia and our analyses show that these characters are informative for some subclades but are homoplasious for the group as a whole. Apocarpous fruits are the ancestral state in Acronychia and subapocarpous and fully syncarpous fruits are derived. The unisexual flowers of Maclurodendron are derived from bisexual flowers, which are found in all species of Acronychia as well as its relatives. Acronychia probably first evolved on Australia with range expansion to New Guinea via stepping-stone dispersal or direct land connections within the Sahul Shelf, followed by two independent dispersals to areas west of New Guinea. Most species of Acronychia occur in either Australia or New Guinea, but no species occurs in both regions. This is surprising given the close proximity of the landmasses, but might be explained by ecological factors. C1 [Holzmeyer, Laura; Hoerandl, Elvira; Appelhans, Marc S.] Univ Gottingen, Dept Systemat Biodivers & Evolut Plants, D-37073 Gottingen, Germany. [Duretto, Marco; Heslewood, Margaret] Royal Bot Gardens & Domain Trust, Natl Herbarium New South Wales, Sydney, NSW, Australia. [Crayn, Darren; Jayanthan, Janani] James Cook Univ, Australian Trop Herbarium, Cairns, Australia. [Appelhans, Marc S.] Smithsonian Inst, Dept Bot, Washington, DC 20560 USA. RP Appelhans, MS (reprint author), Univ Gottingen, Dept Systemat Biodivers & Evolut Plants, Untere Karspule 2, D-37073 Gottingen, Germany. EM marc.appelhans@biologie.uni-goettingen.de RI Research ID, CTBCC /O-3564-2014; James Cook University, TESS/B-8171-2012; Crayn, Darren/A-7386-2011 OI Crayn, Darren/0000-0001-6614-4216 FU Open Access Publication Funds of Gottingen University FX The authors acknowledge support by the Open Access Publication Funds of Gottingen University. The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 72 TC 0 Z9 0 U1 1 U2 12 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 AUG 24 PY 2015 VL 10 IS 8 AR e0136296 DI 10.1371/journal.pone.0136296 PG 22 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA CP5VA UT WOS:000359951900055 PM 26301574 ER PT J AU Ruffle, PME Kemper, F Jones, OC Sloan, GC Kraemer, KE Woods, PM Boyer, ML Srinivasan, S Antoniou, V Lagadec, E Matsuura, M McDonald, I Oliveira, JM Sargent, BA Sewilo, M Szczerba, R van Loon, JT Volk, K Zijlstra, AA AF Ruffle, Paul M. E. Kemper, F. Jones, O. C. Sloan, G. C. Kraemer, K. E. Woods, Paul M. Boyer, M. L. Srinivasan, S. Antoniou, V. Lagadec, E. Matsuura, M. McDonald, I. Oliveira, J. M. Sargent, B. A. Sewilo, M. Szczerba, R. van Loon, J. Th. Volk, K. Zijlstra, A. A. TI Spitzer infrared spectrograph point source classification in the Small Magellanic Cloud SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE techniques: spectroscopic; surveys; dust, extinction; H ii regions; Magellanic Clouds; infrared: stars ID GIANT BRANCH STARS; LONG-PERIOD VARIABLES; YOUNG STELLAR OBJECTS; WOLF-RAYET STARS; SPACE-TELESCOPE OBSERVATIONS; BINARY HD 5980; VLT-FLAMES SURVEY; ULTRAVIOLET INTERSTELLAR ABSORPTION; SPECTROSCOPIC-EXPLORER OBSERVATIONS; EMISSION-LINE STARS AB The Magellanic Clouds are uniquely placed to study the stellar contribution to dust emission. Individual stars can be resolved in these systems even in the mid-infrared, and they are close enough to allow detection of infrared excess caused by dust. We have searched the Spitzer Space Telescope data archive for all Infrared Spectrograph (IRS) staring-mode observations of the Small Magellanic Cloud (SMC) and found that 209 Infrared Array Camera (IRAC) point sources within the footprint of the Surveying the Agents of Galaxy Evolution in the Small Magellanic Cloud (SAGE-SMC) Spitzer Legacy programme were targeted, within a total of 311 staring-mode observations. We classify these point sources using a decision tree method of object classification, based on infrared spectral features, continuum and spectral energy distribution shape, bolometric luminosity, cluster membership and variability information. We find 58 asymptotic giant branch (AGB) stars, 51 young stellar objects, 4 post-AGB objects, 22 red supergiants, 27 stars (of which 23 are dusty OB stars), 24 planetary nebulae (PNe), 10 Wolf-Rayet stars, 3 H ii regions, 3 R Coronae Borealis stars, 1 Blue Supergiant and 6 other objects, including 2 foreground AGB stars. We use these classifications to evaluate the success of photometric classification methods reported in the literature. C1 [Ruffle, Paul M. E.; Jones, O. C.; McDonald, I.; Zijlstra, A. A.] Univ Manchester, Jodrell Bank, Ctr Astrophys, Manchester M13 9PL, Lancs, England. [Ruffle, Paul M. E.; Kemper, F.; Srinivasan, S.] Acad Sinica, Inst Astron & Astrophys, Taipei 10617, Taiwan. [Jones, O. C.; Volk, K.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Sloan, G. C.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. [Kraemer, K. E.] Boston Coll, Inst Sci Res, Chestnut Hill, MA 02467 USA. [Woods, Paul M.] Queens Univ Belfast, Sch Math & Phys, Astrophys Res Ctr, Belfast BT7 1NN, Antrim, North Ireland. [Boyer, M. L.] NASA, Goddard Space Flight Ctr, Observat Cosmol Lab, Greenbelt, MD 20771 USA. [Antoniou, V.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Lagadec, E.] Univ Nice Sophia Antipolis, Lab Lagrange, CNRS, Observ Cote Azur, F-06304 Nice, France. [Matsuura, M.] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales. [Matsuura, M.] UCL, Dept Phys & Astron, London WC1E 6BT, England. [Oliveira, J. M.; van Loon, J. Th.] Keele Univ, Lennard Jones Labs, Sch Phys & Geog Sci, Keele ST5 5BG, Staffs, England. [Sargent, B. A.] Rochester Inst Technol, Lab Multiwavelength Astrophys, Rochester, NY 14623 USA. [Sewilo, M.] Space Sci Inst, Boulder, CO 80301 USA. [Sewilo, M.] Johns Hopkins Univ, Dept Phys & Astron, Bloomberg Ctr 366, Baltimore, MD 21218 USA. [Szczerba, R.] N Copernicus Astron Ctr, PL-87100 Torun, Poland. EM ciska@asiaa.sinica.edu.tw RI Woods, Paul/E-6926-2011; Kemper, Francisca/D-8688-2011; Antoniou, Vallia/E-3837-2013; OI Woods, Paul/0000-0003-4340-3590; Kemper, Francisca/0000-0003-2743-8240; Antoniou, Vallia/0000-0001-7539-1593; Jones, Olivia/0000-0003-4870-5547; Kraemer, Kathleen/0000-0002-2626-7155 FU STFC; National Science Council; Ministry of Science and Technology [NSC100-2112-M-001-023-MY3, MOST103-2112-M-001-0330]; NASA ADP [NNX11AB06G]; Polish NCN grant [2011/01/B/ST9/02031, DEC-2013/08/M/ST9/00664]; National Aeronautics and Space Administration; NASA [NAS5-26555]; NASA Office of Space Science [NNX13AC07G] FX The authors wish to thank Paul Ruffle's partner Rose Wheeler, Rose provided access to Paul's notes and files, which allowed us to finish this work. PMER thanks Academia Sinica Institute of Astronomy and Astrophysics (ASIAA) for their financial support and hospitality during the preparation of this work. The authors thank David Whelan for making available Spitzer spectra of point sources described in his 2013 paper. Astrophysics at JBCA is supported by STFC. FK acknowledges support from the former National Science Council and the Ministry of Science and Technology in the form of grants NSC100-2112-M-001-023-MY3 and MOST103-2112-M-001-0330. BAS acknowledges support from NASA ADP NNX11AB06G. RSz acknowledges support from the Polish NCN grant 2011/01/B/ST9/02031. The research presented here was conducted within the scope of the HECOLS International Associated Laboratory, supported in part by the Polish NCN grant DEC-2013/08/M/ST9/00664 (E.L.; R.Sz). This work is based (in part) on observations made with the Spitzer Space Telescope, obtained from the NASA/IPAC Infrared Science Archive, both of which are operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with the National Aeronautics and Space Administration. 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 in this paper were obtained from the Mikulski Archive for Space Telescopes (MAST). STScI is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555. Support for MAST for non Hobble Space Telescope (HST) data is provided by the NASA Office of Space Science via grant NNX13AC07G and by other grants and contracts. This research has also made use of the SAGE CASJobs data base, which made possible by the Sloan Digital Sky Survey Collaboration; SAOImage DS9, developed by Smithsonian Astrophysical Observatory; the VizieR catalogue access tool. CDS, Strasbourg, France; the SIMBAD data base, operated at CDS, Strasbourg, France; and NASA's Astrophysics Data System Bibliographic Services. NR 286 TC 4 Z9 4 U1 1 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 AUG 21 PY 2015 VL 451 IS 4 BP 3504 EP 3536 DI 10.1093/mnras/stv1106 PG 33 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CQ8HA UT WOS:000360846400013 ER PT J AU Tremblay, GR O'Dea, CP Baum, SA Mittal, R McDonald, MA Combes, F Li, Y McNamara, BR Bremer, MN Clarke, TE Donahue, M Edge, AC Fabian, AC Hamer, SL Hogan, MT Oonk, JBR Quillen, AC Sanders, JS Salome, P Voit, GM AF Tremblay, G. R. O'Dea, C. P. Baum, S. A. Mittal, R. McDonald, M. A. Combes, F. Li, Y. McNamara, B. R. Bremer, M. N. Clarke, T. E. Donahue, M. Edge, A. C. Fabian, A. C. Hamer, S. L. Hogan, M. T. Oonk, J. B. R. Quillen, A. C. Sanders, J. S. Salome, P. Voit, G. M. TI Far-ultraviolet morphology of star-forming filaments in cool core brightest cluster galaxies SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies: active; galaxies: clusters: general; galaxies: clusters: intracluster medium; galaxies: star formation ID GALACTIC NUCLEUS FEEDBACK; RAY-LUMINOUS CLUSTERS; CENTRAL-DOMINANT-GALAXIES; X-RAY; FLOW CLUSTERS; MOLECULAR GAS; EMISSION-LINE; HYDRA-A; PERSEUS CLUSTER; ABELL 2597 AB We present a multiwavelength morphological analysis of star-forming clouds and filaments in the central (a parts per thousand(2)50 kpc) regions of 16 low-redshift (z < 0.3) cool core brightest cluster galaxies. New Hubble Space Telescope imaging of far-ultraviolet continuum emission from young (a parts per thousand(2)10 Myr), massive (a parts per thousand(3)5 M-aS (TM)) stars reveals filamentary and clumpy morphologies, which we quantify by means of structural indices. The FUV data are compared with X-ray, Ly alpha, narrow-band H alpha, broad-band optical/IR, and radio maps, providing a high spatial resolution atlas of star formation locales relative to the ambient hot (similar to 10(7-8) K) and warm ionized (similar to 10(4) K) gas phases, as well as the old stellar population and radio-bright active galactic nucleus (AGN) outflows. Nearly half of the sample possesses kpc-scale filaments that, in projection, extend towards and around radio lobes and/or X-ray cavities. These filaments may have been uplifted by the propagating jet or buoyant X-ray bubble, or may have formed in situ by cloud collapse at the interface of a radio lobe or rapid cooling in a cavity's compressed shell. The morphological diversity of nearly the entire FUV sample is reproduced by recent hydrodynamical simulations in which the AGN powers a self-regulating rain of thermally unstable star-forming clouds that precipitate from the hot atmosphere. In this model, precipitation triggers where the cooling-to-free-fall time ratio is t(cool)/t(ff) similar to 10. This condition is roughly met at the maximal projected FUV radius for more than half of our sample, and clustering about this ratio is stronger for sources with higher star formation rates. C1 [Tremblay, G. R.] Yale Univ, Dept Phys, New Haven, CT 06511 USA. [Tremblay, G. R.] Yale Univ, Ctr Astron & Astrophys, New Haven, CT 06511 USA. [Tremblay, G. R.] European So Observ, D-85748 Garching, Germany. [O'Dea, C. P.; Baum, S. A.] Univ Manitoba, Dept Phys & Astron, Winnipeg, MB R3T 2N2, Canada. [O'Dea, C. P.; Baum, S. A.] Rochester Inst Technol, Sch Phys & Astron, Rochester, NY 14623 USA. [Baum, S. A.] Univ Manitoba, Fac Sci, Winnipeg, MB R3T 2N2, Canada. [Baum, S. A.; Mittal, R.] Rochester Inst Technol, Chester F Carlson Ctr Imaging Sci, Rochester, NY 14623 USA. [Mittal, R.] Albert Einstein Inst, Max Planck Inst Gravitationsphys, D-30167 Hannover, Germany. [McDonald, M. A.] MIT, Kavil Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Combes, F.; Hamer, S. L.; Salome, P.] CNRS, LERMA, Observ Paris, F-75014 Paris, France. [Li, Y.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [McNamara, B. R.; Hogan, M. T.] Univ Waterloo, Dept Phys & Astron, Waterloo, ON N2L 2G1, Canada. [McNamara, B. R.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Bremer, M. N.] Univ Bristol, HH Wills Phys Lab, Bristol BS8 1TL, Avon, England. [Clarke, T. E.] US Navy, Res Lab, Remote Sensing Div, Washington, DC 20375 USA. [Donahue, M.; Voit, G. M.] Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA. [Edge, A. C.] Univ Durham, Dept Phys, Durham DH1 3LE, England. [Edge, A. C.] Inst Astron, Cambridge CB3 0HA, England. [Oonk, J. B. R.] Netherlands Inst Radio Astron, ASTRON, NL-7990 AA Dwingeloo, Netherlands. [Quillen, A. C.] Univ Rochester, Dept Phys & Astron, Rochester, NY 14627 USA. [Sanders, J. S.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. RP Tremblay, GR (reprint author), Yale Univ, Dept Phys, 217 Prospect St, New Haven, CT 06511 USA. EM grant.tremblay@yale.edu OI Edge, Alastair/0000-0002-3398-6916; Tremblay, Grant/0000-0002-5445-5401; Li, Yuan/0000-0001-5262-6150; Sanders, Jeremy/0000-0003-2189-4501; Combes, Francoise/0000-0003-2658-7893; Voit, Gerard/0000-0002-3514-0383 FU NASA [PF-150128, NAS8-03060, NNX12AH41G, NNX12AC98G, ATP12-ATP12-0017, NAS8-39073, 5-26555]; European Southern Observatory (ESO) Fellowship - European Community [229517]; National Aeronautics and Space Administration through Einstein Postdoctoral Fellowship Award [PF-150128]; NSF [AST-0908390, AST-1008134, AST-1210890, AST-1008454]; NASA through Chandra award [G06-7115B]; 6.1 Base funds FX The authors thank Drs. Richard Bower, Tim Davis, Bill Forman, Nina Hatch, Claudia Lagos, Robert Laing, Jason Spyromilio, and Aurora Simionescu for thoughtful discussions. GRT acknowledges support from a NASA Einstein Fellowship under award number PF-150128, as well as a European Southern Observatory (ESO) Fellowship partially funded by the European Community's Seventh Framework Programme (/FP7/2007-2013/) under grant agreement number 229517. Support for this work was provided by the National Aeronautics and Space Administration through Einstein Postdoctoral Fellowship Award Number PF-150128 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. YE acknowledges financial support from NSF grants AST-0908390, AST-1008134, AST-1210890, AST-1008454, NASA grants NNX12AH41G, NNX12AC98G, and ATP12-ATP12-0017, as well as computational resources from NASA, NSF XSEDE and Columbia University. TEC was partially supported by NASA through Chandra award G06-7115B issued by the Chandra X-ray Observatory Center for and on behalf of NASA under contract NAS8-39073. Basic research into radio astronomy at the Naval Research Laboratory is supported by 6.1 Base funds. This paper is based on observations made with the NASA/ESA Hobble Space Telescope, obtained at the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract 5-26555. This research made use of Astropy, a community-developed core grams package for Astronomy (Astropy Collaboration et al. 2013). We have also made extensive use of the NASA Astrophysics Data System bibliographic services and the NASA/IPAC Extragalactic Database, operated by the Jet Propulsion Laboratory, California Institute of Technology. under contract with NASA. NR 168 TC 19 Z9 19 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 AUG 21 PY 2015 VL 451 IS 4 BP 3768 EP 3800 DI 10.1093/mnras/stv1151 PG 33 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CQ8HA UT WOS:000360846400030 ER PT J AU George, LT Dwarakanath, KS Johnston-Hollitt, M Hurley-Walker, N Hindson, L Kapinska, AD Tingay, SJ Bell, M Callingham, JR For, BQ Hancock, PJ Lenc, E McKinley, B Morgan, J Offringa, A Procopio, P Staveley-Smith, L Wayth, RB Wu, C Zheng, Q Bernardi, G Bowman, JD Briggs, F Cappallo, RJ Corey, BE Deshpande, AA Emrich, D Goeke, R Greenhill, LJ Hazelton, BJ Kaplan, DL Kasper, JC Kratzenberg, E Lonsdale, CJ Lynch, MJ McWhirter, SR Mitchell, DA Morales, MF Morgan, E Oberoi, D Ord, SM Prabu, T Rogers, AEE Roshi, A Shankar, NU Srivani, KS Subrahmanyan, R Waterson, M Webster, RL Whitney, AR Williams, A Williams, CL AF George, L. T. Dwarakanath, K. S. Johnston-Hollitt, M. Hurley-Walker, N. Hindson, L. Kapinska, A. D. Tingay, S. J. Bell, M. Callingham, J. R. For, Bi-Qing Hancock, P. J. Lenc, E. McKinley, B. Morgan, J. Offringa, A. Procopio, P. Staveley-Smith, L. Wayth, R. B. Wu, Chen Zheng, Q. Bernardi, G. Bowman, J. D. Briggs, F. Cappallo, R. J. Corey, B. E. Deshpande, A. A. Emrich, D. Goeke, R. Greenhill, L. J. Hazelton, B. J. Kaplan, D. L. Kasper, J. C. Kratzenberg, E. Lonsdale, C. J. Lynch, M. J. McWhirter, S. R. Mitchell, D. A. Morales, M. F. Morgan, E. Oberoi, D. Ord, S. M. Prabu, T. Rogers, A. E. E. Roshi, A. Shankar, N. Udaya Srivani, K. S. Subrahmanyan, R. Waterson, M. Webster, R. L. Whitney, A. R. Williams, A. Williams, C. L. TI An analysis of the halo and relic radio emission from Abell 3376 from Murchison Widefield Array observations SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies: clusters: individual: Abell 3376; galaxies: clusters: intracluster medium ID X-RAY-EMISSION; GALAXY CLUSTERS; COSMIC-RAYS; NONTHERMAL EMISSION; SHOCK ACCELERATION; MAGNETIC-FIELDS; MASS FUNCTION; SKY SURVEY; GAMMA-RAY; REACCELERATION AB We have carried out multiwavelength observations of the nearby (z = 0.046) rich, merging galaxy cluster Abell 3376 with the Murchison Widefield Array (MWA). As a part of the GaLactic and Extragalactic All-sky MWA Survey, this cluster was observed at 88, 118, 154, 188, and 215 MHz. The known radio relics, towards the eastern and western peripheries of the cluster, were detected at all the frequencies. The relics, with a linear extent of similar to 1 Mpc each, are separated by similar to 2 Mpc. Combining the current observations with those in the literature, we have obtained the spectra of these relics over the frequency range 80-1400 MHz. The spectra follow power laws, with alpha = -1.17 +/- A 0.06 and -1.37 +/- A 0.08 for the west and east relics, respectively (S infinity nu(infinity)). Assuming the break frequency to be near the lower end of the spectrum we estimate the age of the relics to be similar to 0.4 Gyr. No diffuse radio emission from the central regions of the cluster (halo) was detected. The upper limit on the radio power of any possible halo that might be present in the cluster is a factor of 35 lower than that expected from the radio power and X-ray luminosity correlation for cluster haloes. From this we conclude that the cluster halo is very extended (> 500 kpc) and/or most of the radio emission from the halo has decayed. The current limit on the halo radio power is a factor of 10 lower than the existing upper limits with possible implications for models of halo formation. C1 [George, L. T.; Dwarakanath, K. S.; Deshpande, A. A.; Prabu, T.; Shankar, N. Udaya; Srivani, K. S.; Subrahmanyan, R.] Raman Res Inst, Bangalore 560080, Karnataka, India. [Johnston-Hollitt, M.; Hindson, L.; Zheng, Q.] Victoria Univ Wellington, Sch Chem & Phys Sci, Wellington 6140, New Zealand. [Hurley-Walker, N.; Tingay, S. J.; Hancock, P. J.; Morgan, J.; Wayth, R. B.; Emrich, D.; Lynch, M. J.; Ord, S. M.; Waterson, M.; Williams, A.] Curtin Univ, Int Ctr Radio Astron Res, Bentley, WA 6102, Australia. [Kapinska, A. D.; Tingay, S. J.; Callingham, J. R.; Hancock, P. J.; Mitchell, D. A.; Ord, S. M.; Subrahmanyan, R.; Webster, R. L.] ARC Ctr Excellence All Sky Astrophys CAASTRO, Redfern, NSW 2016, Australia. [Kapinska, A. D.; For, Bi-Qing; Staveley-Smith, L.; Wu, Chen] Univ Western Australia, Int Ctr Radio Astron Res, Crawley, WA 6009, Australia. [Bell, M.; Callingham, J. R.; Mitchell, D. A.] CSIRO Astron & Space Sci CASS, Epping, NSW 1710, Australia. [Callingham, J. R.; Lenc, E.] Univ Sydney, Sch Phys, Sydney Inst Astron, Sydney, NSW 2006, Australia. [McKinley, B.; Procopio, P.; Webster, R. L.] Univ Melbourne, Sch Phys, Parkville, Vic 3010, Australia. [Offringa, A.] ASTRON, NL-7990 AA Dwingeloo, Netherlands. [Bernardi, G.] Square Kilometre Array South Africa SKASA, ZA-7405 Pinelands, South Africa. [Bernardi, G.] Rhodes Univ, Dept Phys & Elect, ZA-6140 Grahamstown, South Africa. [Bernardi, G.; Greenhill, L. J.; Kasper, J. C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Bowman, J. D.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA. [Briggs, F.; Waterson, M.] Australian Natl Univ, Res Sch Astron & Astrophys, Canberra, ACT 2611, Australia. [Cappallo, R. J.; Corey, B. E.; Kratzenberg, E.; Lonsdale, C. J.; McWhirter, S. R.; Rogers, A. E. E.; Whitney, A. R.] MIT, Haystack Observ, Westford, MA 01886 USA. [Hazelton, B. J.; Morales, M. F.] Univ Washington, Dept Phys, Seattle, WA 98195 USA. [Roshi, A.] NRAO, Charlottesville, VA USA. [Roshi, A.] NRAO, Green Bank, WV USA. [Kaplan, D. L.] Univ Wisconsin, Dept Phys, Milwaukee, WI 53201 USA. [Morgan, E.; Williams, C. L.] MIT, Kavil Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Oberoi, D.] Tata Inst Fundamental Res, Natl Ctr Radio Astrophys, Pune 411007, Maharashtra, India. [Kasper, J. C.] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA. RP George, LT (reprint author), Raman Res Inst, Bangalore 560080, Karnataka, India. EM lijo@rri.res.in; dwaraka@rri.res.in RI Deshpande, Avinash/D-4868-2012; Udayashankar , N/D-4901-2012; Dwarakanath, K /D-4876-2012; Wayth, Randall/B-2444-2013; Hurley-Walker, Natasha/B-9520-2013; Emrich, David/B-7002-2013; Subrahmanyan, Ravi/D-4889-2012; M, Manjunath/N-4000-2014; Kapinska, Anna/B-3999-2014; Staveley-Smith, Lister/A-1683-2011; OI Lenc, Emil/0000-0002-9994-1593; Wayth, Randall/0000-0002-6995-4131; Hurley-Walker, Natasha/0000-0002-5119-4808; Emrich, David/0000-0002-4058-1837; M, Manjunath/0000-0001-8710-0730; Kapinska, Anna/0000-0002-5289-5729; Staveley-Smith, Lister/0000-0002-8057-0294; Callingham, Joseph/0000-0002-7167-1819; Hancock, Paul/0000-0002-4203-2946 FU US National Science Foundation [AST-0457585, PHY-0835713, 0847753, AST-0908884]; Australian Research Council (LIEF) [LE0775621, LE0882938]; US Air Force Office of Scientific Research [FA9550-0510247]; Centre for All-sky Astrophysics (an Australian Research Council Centre of Excellence) [CE110001020]; Smithsonian Astrophysical Observatory; MIT School of Science; Raman Research Institute; Australian National University; Victoria University of Wellington (New Zealand Ministry of Economic Development) [MED-E1799]; Victoria University of Wellington (IBM Shared University); CSIRO; National Collaborative Research Infrastructure Strategy, Education Investment Fund; Australia India Strategic Research Fund; Astronomy Australia Limited; NVIDIA at Harvard University; International Centre for Radio Astronomy Research (ICRAR), a Joint Venture of Curtin University; University of Western Australia by Western Australian State government FX This scientific work makes use of the Murchison Radio-astronomy Observatory, operated by the Commonwealth Scientific and Industrial Research Organisation (CSIRO), We acknowledge the Wajarri Yamatji people as the traditional owners of the Observatory site Support for the MWA comes from the US National Science Foundation (grants AST-0457585, PHY-0835713, CAREER 0847753 and AST-0908884), the Australian Research Council (LIEF grants LE0775621 and LE0882938), the US Air Force Office of Scientific Research (grant FA9550-0510247), and the Centre for All-sky Astrophysics (an Australian Research Council Centre of Excellence funded by grant CE110001020). Support is also provided by the Smithsonian Astrophysical Observatory, the MIT School of Science, the Raman Research Institute, the Australian National University, and the Victoria University of Wellington (via grant MED-E1799 from the New Zealand Ministry of Economic Development and an IBM Shared University Research Grant). The Australian Federal government provides additional support via CSIRO, National Collaborative Research Infrastructure Strategy, Education Investment Fund, and the Australia India Strategic Research Fund, and Astronomy Australia Limited, under contract to Curtin University. We acknowledge the iVEC Petabyte Data Store, the Initiative in Innovative Computing and the CUDA Center for Excellence sponsored by NVIDIA at Harvard University, and the International Centre for Radio Astronomy Research (ICRAR), a Joint Venture of Curtin University and The University of Western Australia, funded by the Western Australian State government. NR 73 TC 0 Z9 0 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 AUG 21 PY 2015 VL 451 IS 4 BP 4207 EP 4214 DI 10.1093/mnras/stv1152 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CQ8HA UT WOS:000360846400065 ER PT J AU Callingham, JR Gaensler, BM Ekers, RD Tingay, SJ Wayth, RB Morgan, J Bernardi, G Bell, ME Bhat, R Bowman, JD Briggs, F Cappallo, RJ Deshpande, AA Ewall-Wice, A Feng, L Greenhill, LJ Hazelton, BJ Hindson, L Hurley-Walker, N Jacobs, DC Johnston-Hollitt, M Kaplan, DL Kudrayvtseva, N Lenc, E Lonsdale, CJ McKinley, B McWhirter, SR Mitchell, DA Morales, MF Morgan, E Oberoi, D Offringa, AR Ord, SM Pindor, B Prabu, T Procopio, P Riding, J Srivani, KS Subrahmanyan, R Shankar, NU Webster, RL Williams, A Williams, CL AF Callingham, J. R. Gaensler, B. M. Ekers, R. D. Tingay, S. J. Wayth, R. B. Morgan, J. Bernardi, G. Bell, M. E. Bhat, R. Bowman, J. D. Briggs, F. Cappallo, R. J. Deshpande, A. A. Ewall-Wice, A. Feng, L. Greenhill, L. J. Hazelton, B. J. Hindson, L. Hurley-Walker, N. Jacobs, D. C. Johnston-Hollitt, M. Kaplan, D. L. Kudrayvtseva, N. Lenc, E. Lonsdale, C. J. McKinley, B. McWhirter, S. R. Mitchell, D. A. Morales, M. F. Morgan, E. Oberoi, D. Offringa, A. R. Ord, S. M. Pindor, B. Prabu, T. Procopio, P. Riding, J. Srivani, K. S. Subrahmanyan, R. Shankar, N. Udaya Webster, R. L. Williams, A. Williams, C. L. TI BROADBAND SPECTRAL MODELING OF THE EXTREME GIGAHERTZ-PEAKED SPECTRUM RADIO SOURCE PKS B0008-421 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: active; galaxies: individual (PKS B0008-421); radiation mechanisms: general; radio continuum: general ID COMPACT STEEP-SPECTRUM; FREE-FREE ABSORPTION; HIGH-FREQUENCY PEAKERS; SYNCHROTRON SELF-ABSORPTION; SYMMETRIC OBJECTS; SOURCE CATALOG; SOUTHERN SKY; LOUD AGN; REIONIZATION OBSERVATORIES; SOURCE EVOLUTION AB We present broadband observations and spectral modeling of PKS B0008-421. and identify it as an extreme gigahertz-peaked spectrum (GPS) source. PKS B0008-421 is characterized by the steepest known spectral slope below the turnover, close to the theoretical limit of synchrotron self-absorption, and the smallest known spectral width of any GPS source. Spectral coverage of the source spans from 0.118 to 22 GHz, which includes data from the Murchison Widefield Array and the wide bandpass receivers on the Australia Telescope Compact Array. We have implemented a Bayesian inference model fitting routine to fit the data with internal free-free absorption (FFA), single-and double-component FFA in an external homogeneous medium, FFA in an external inhomogeneous medium, or single-and double-component synchrotron self-absorption models, all with and without a high-frequency exponential break. We find that without the inclusion of a high-frequency break these models cannot accurately fit the data, with significant deviations above and below the peak in the radio spectrum. The addition of a high-frequency break provides acceptable spectral fits for the inhomogeneous FFA and double-component synchrotron self-absorption models, with the inhomogeneous FFA model statistically favored. The requirement of a high-frequency spectral break implies that the source has ceased injecting fresh particles. Additional support for the inhomogeneous FFA model as being responsible for the turnover in the spectrum is given by the consistency between the physical parameters derived from the model fit and the implications of the exponential spectral break, such as the necessity of the source being surrounded by a dense ambient medium to maintain the peak frequency near the gigahertz region. This implies that PKS B0008-421 should display an internal H I column density greater than 10(20) cm(-2). The discovery of PKS B0008-421 suggests that the next generation of low radio frequency surveys could reveal a large population of GPS sources that have ceased activity, and that a portion of the ultra-steep-spectrum source population could be composed of these GPS sources in a relic phase. C1 [Callingham, J. R.; Gaensler, B. M.; Lenc, E.] Univ Sydney, Sch Phys, Sydney Inst Astron SIfA, Sydney, NSW 2006, Australia. [Callingham, J. R.; Ekers, R. D.; Bell, M. E.; Mitchell, D. A.] CSIRO Astron & Space Sci CASS, Marsfield, NSW 2122, Australia. [Callingham, J. R.; Gaensler, B. M.; Tingay, S. J.; Wayth, R. B.; Bell, M. E.; Bhat, R.; Briggs, F.; Lenc, E.; Mitchell, D. A.; Offringa, A. R.; Ord, S. M.; Pindor, B.; Procopio, P.; Riding, J.; Subrahmanyan, R.; Webster, R. L.] ARC Ctr Excellence All Sky Astrophys CAASTRO, Sydney, NSW, Australia. [Gaensler, B. M.] Univ Toronto, Dunlap Inst Astron & Astrophys, Toronto, ON M5S 3H4, Canada. [Tingay, S. J.; Wayth, R. B.; Morgan, J.; Bhat, R.; Hurley-Walker, N.; Kudrayvtseva, N.; Ord, S. M.; Williams, A.] Curtin Univ, Int Ctr Radio Astron Res ICRAR, Bentley, WA 6102, Australia. [Bernardi, G.] Sq Kilometre Array South Africa SKA SA, ZA-7405 Pinelands, South Africa. [Bernardi, G.] Rhodes Univ, Dept Phys & Elect, ZA-6140 Grahamstown, South Africa. [Bowman, J. D.; Jacobs, D. C.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA. [Briggs, F.] Australian Natl Univ, Res Sch Astron & Astrophys, Canberra, ACT 2611, Australia. [Cappallo, R. J.; Lonsdale, C. J.; McWhirter, S. R.] MIT, Haystack Observ, Westford, MA 01886 USA. [Deshpande, A. A.; Prabu, T.; Srivani, K. S.; Subrahmanyan, R.; Shankar, N. Udaya] Raman Res Inst, Bangalore 560080, Karnataka, India. [Ewall-Wice, A.; Feng, L.; Morgan, E.; Williams, C. L.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Greenhill, L. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Hazelton, B. J.; Morales, M. F.] Univ Washington, Dept Phys, Seattle, WA 98195 USA. [Hindson, L.; Johnston-Hollitt, M.] Victoria Univ Wellington, Sch Chem & Phys Sci, Wellington 6140, New Zealand. [Kaplan, D. L.] Univ Wisconsin, Dept Phys, Milwaukee, WI 53201 USA. [McKinley, B.; Pindor, B.; Procopio, P.; Riding, J.; Webster, R. L.] Univ Melbourne, Sch Phys, Parkville, Vic 3010, Australia. [Oberoi, D.] Tata Inst Fundamental Res, Natl Ctr Radio Astrophys, Pune 411007, Maharashtra, India. [Offringa, A. R.] Netherlands Inst Radio Astron ASTRON, Dwingeloo, Netherlands. RP Callingham, JR (reprint author), Univ Sydney, Sch Phys, Sydney Inst Astron SIfA, Sydney, NSW 2006, Australia. EM j.callingham@physics.usyd.edu.au RI Deshpande, Avinash/D-4868-2012; Udayashankar , N/D-4901-2012; Wayth, Randall/B-2444-2013; Hurley-Walker, Natasha/B-9520-2013; Subrahmanyan, Ravi/D-4889-2012; M, Manjunath/N-4000-2014; OI Callingham, Joseph/0000-0002-7167-1819; Wayth, Randall/0000-0002-6995-4131; Hurley-Walker, Natasha/0000-0002-5119-4808; M, Manjunath/0000-0001-8710-0730; /0000-0002-0086-7363; Gaensler, Bryan/0000-0002-3382-9558; Lenc, Emil/0000-0002-9994-1593; Ekers, Ron/0000-0002-3532-9928 FU U.S. National Science Foundation [AST-0457585, PHY-0835713, CAREER-0847753, AST-0908884]; Australian Research Council (LIEF) [LE0775621, LE0882938]; U.S. Air Force Office of Scientific Research [FA9550-0510247]; Centre for All-sky Astrophysics (an Australian Research Council Centre of Excellence [CE110001020]; Smithsonian Astrophysical Observatory; MIT School of Science; Raman Research Institute; Australian National University; Victoria University of Wellington (via grant from the New Zealand Ministry of Economic Development) [MED-E1799]; Victoria University of Wellington (IBM Shared University Research Grant); CSIRO; National Collaborative Research Infrastructure Strategy, Education Investment Fund; Australia India Strategic Research Fund; Astronomy Australia Limited; NVIDIA at Harvard University; International Centre for Radio Astronomy Research (ICRAR), a Joint Venture of Curtin University; University of Western Australia - Western Australian State government; Commonwealth of Australia FX The authors thank Geoffrey Bicknell, David Jauncey, and Edward King for stimulating discussions about the theoretical aspects of the absorption models and the VLBI measurements of PKS B0008-421. This scientific work makes use of the Murchison Radioastronomy Observatory, operated by CSIRO. We acknowledge the Wajarri Yamatji people as the traditional owners of the Observatory site. Support for the MWA comes from the U.S. National Science Foundation (grants AST-0457585, PHY-0835713, CAREER-0847753, and AST-0908884), the Australian Research Council (LIEF grants LE0775621 and LE0882938), the U.S. Air Force Office of Scientific Research (grant FA9550-0510247), and the Centre for All-sky Astrophysics (an Australian Research Council Centre of Excellence funded by grant CE110001020). Support is also provided by the Smithsonian Astrophysical Observatory, the MIT School of Science, the Raman Research Institute, the Australian National University, and the Victoria University of Wellington (via grant MED-E1799 from the New Zealand Ministry of Economic Development and an IBM Shared University Research Grant). The Australian federal government provides additional support via the CSIRO, National Collaborative Research Infrastructure Strategy, Education Investment Fund, the Australia India Strategic Research Fund, and Astronomy Australia Limited, under contract to Curtin University. We acknowledge the iVEC Petabyte Data Store, the Initiative in Innovative Computing. and the CUDA Center for Excellence sponsored by NVIDIA at Harvard University, and the International Centre for Radio Astronomy Research (ICRAR), a Joint Venture of Curtin University and the University of Western Australia, funded by the Western Australian State government. The Australia Telescope Compact Array is part of the Australia Telescope National Facility, which is funded by the Commonwealth of Australia for operation as a National Facility managed by CSIRO. This paper includes archived data obtained through the Australia Telescope Online Archive (http://atoa.atnf.csiro.au). This research has made use of the NASA/IPAC Extragalactic Database (NED), which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. NR 96 TC 13 Z9 13 U1 0 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD AUG 20 PY 2015 VL 809 IS 2 AR 168 DI 10.1088/0004-637X/809/2/168 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CR9EC UT WOS:000361655100061 ER PT J AU Corcoran, MF Nichols, JS Pablo, H Shenar, T Pollock, AMT Waldron, WL Moffat, AFJ Richardson, ND Russell, CMP Hamaguchi, K Huenemoerder, DP Oskinova, L Hamann, WR Naze, Y Ignace, R Evans, NR Lomax, JR Hoffman, JL Gayley, K Owocki, SP Leutenegger, M Gull, TR Hole, KT Lauer, J Iping, RC AF Corcoran, M. F. Nichols, J. S. Pablo, H. Shenar, T. Pollock, A. M. T. Waldron, W. L. Moffat, A. F. J. Richardson, N. D. Russell, C. M. P. Hamaguchi, K. Huenemoerder, D. P. Oskinova, L. Hamann, W. -R. Naze, Y. Ignace, R. Evans, N. R. Lomax, J. R. Hoffman, J. L. Gayley, K. Owocki, S. P. Leutenegger, M. Gull, T. R. Hole, K. T. Lauer, J. Iping, R. C. TI A COORDINATED X-RAY AND OPTICAL CAMPAIGN OF THE NEAREST MASSIVE ECLIPSING BINARY, delta ORIONIS Aa. I. OVERVIEW OF THE X-RAY SPECTRUM SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries: close; binaries: eclipsing; stars: early-type; stars: individual (Delta Ori); stars: mass-loss; X-rays: stars ID HOT-STAR WINDS; O-TYPE STARS; RADIATION-DRIVEN WINDS; COLLIDING WINDS; EMISSION; CHANDRA; SPECTROSCOPY; SIMULATIONS; SYSTEMS; MODELS AB We present an overview of four deep phase-constrained Chandra HETGS X-ray observations of delta Ori A. Delta Ori A is actually a triple system that includes the nearest massive eclipsing spectroscopic binary, delta Ori Aa, the only such object that can be observed with little phase-smearing with the Chandra gratings. Since the fainter star, delta Ori Aa2, has a much lower X-ray luminosity than the brighter primary (delta Ori Aa1), delta Ori Aa provides a unique system with which to test the spatial distribution of the X-ray emitting gas around delta Ori Aa1 via occultation by the photosphere of, and wind cavity around, the X-ray dark secondary. Here we discuss the X-ray spectrum and X-ray line profiles for the combined observation, having an exposure time of nearly 500 ks and covering nearly the entire binary orbit. The companion papers discuss the X-ray variability seen in the Chandra spectra, present new space-based photometry and ground-based radial velocities obtained simultaneously with the X-ray data to better constrain the system parameters, and model the effects of X-rays on the optical and UV spectra. We find that the X-ray emission is dominated by embedded wind shock emission from star Aa1, with little contribution from the tertiary star Ab or the shocked gas produced by the collision of the wind of Aa1 against the surface of Aa2. We find a similar temperature distribution to previous X-ray spectrum analyses. We also show that the line half-widths are about 0.3-0.5 times the terminal velocity of the wind of star Aa1. We find a strong anti-correlation between line widths and the line excitation energy, which suggests that longer-wavelength, lower-temperature lines form farther out in the wind. Our analysis also indicates that the ratio of the intensities of the strong and weak lines of Fe XVII and Ne X are inconsistent with model predictions, which may be an effect of resonance scattering. C1 [Corcoran, M. F.; Hamaguchi, K.; Leutenegger, M.; Iping, R. C.] NASA, Goddard Space Flight Ctr, CRESST, Greenbelt, MD 20771 USA. [Corcoran, M. F.; Hamaguchi, K.; Leutenegger, M.] NASA, Goddard Space Flight Ctr, Xray Astrophys Lab, Greenbelt, MD 20771 USA. [Corcoran, M. F.] Univ Space Res Assoc, Columbia, MD 21044 USA. [Nichols, J. S.; Lauer, J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Pablo, H.; Moffat, A. F. J.; Richardson, N. D.] Univ Montreal, Dept Phys, Montreal, PQ H3C 3J7, Canada. [Pablo, H.; Moffat, A. F. J.; Richardson, N. D.] Univ Montreal, CRAQ, Montreal, PQ H3C 3J7, Canada. [Shenar, T.; Oskinova, L.; Hamann, W. -R.] Univ Potsdam, Inst Phys & Astron, D-14476 Potsdam, Germany. [Pollock, A. M. T.] European Space Agcy, XMM Newton Sci Operat Ctr, European Space Astron Ctr, E-28691 Villanueva De La Canada, Spain. [Waldron, W. L.] Eureka Sci Inc, Oakland, CA 94602 USA. [Russell, C. M. P.] NASA GSFC, Greenbelt, MD 20771 USA. [Hamaguchi, K.; Leutenegger, M.] Univ Maryland Baltimore Cty, Dept Phys, Baltimore, MD 21250 USA. [Huenemoerder, D. P.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Naze, Y.] Univ Liege, Grp Astrophys Hautes Energies, Inst Astrophys & Geophys, B-4000 Sart Tilman Par Liege, Belgium. [Ignace, R.] E Tennessee State Univ, Phys & Astron, Johnson City, TN 37614 USA. [Evans, N. R.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Lomax, J. R.] Univ Oklahoma, Homer L Dodge Dept Phys & Astron, Norman, OK 73019 USA. [Hoffman, J. L.] Univ Denver, Dept Phys & Astron, Denver, CO 80208 USA. [Gayley, K.] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA. [Owocki, S. P.] Univ Delaware, Bartol Res Inst, Newark, DE 19716 USA. [Gull, T. R.] NASA Goddard Space Flight Ctr, Lab Extraterr Planets & Stellar Astrophys, Greenbelt, MD 20771 USA. [Hole, K. T.] Weber State Univ, Dept Phys, Ogden, UT 84408 USA. [Iping, R. C.] NASA Goddard Space Flight Ctr, Observat Cosmol Lab, Greenbelt, MD 20771 USA. [Iping, R. C.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. RP Corcoran, MF (reprint author), NASA, Goddard Space Flight Ctr, CRESST, Greenbelt, MD 20771 USA. EM michael.f.corcoran@nasa.gov FU National Aeronautics and Space Administration [GO3-14015A, GO3-14015E]; National Aeronautics Space Administration [NAS8-03060]; NASA [NNG06EO90A, NNX13AF40G]; Chandra X-ray Center NASA [NAS8-03060]; NASA Postdoctoral Program at the Goddard Space Flight Center; Leibniz Graduate School for Quantitative Spectroscopy in Astrophysics; Leibniz Institute for Astrophysics Potsdam (AIP); institute of Physics and Astronomy of the University of Potsdam; Fonds National de la Recherche Scientifique (Belgium); Communaute Francaise de Belgique; PRODEX XMM and Integral contracts; "Action de Recherche Concertee" (CFWB-Academie Wallonie Europe); CRAQ (Centre de Recherche en Astrophysique du Quebec) fellowship; NSERC (Canada); FRQNT (Quebec); NSF [AST-0807477] FX We thank the MOST team for the award of observing time for delta Ori A. We also thank our anonymous referee, whose comments significantly improved this paper. M.F.C. thanks John Houck and Michael Nowak for many helpful discussions concerning data analysis with ISIS. Support for this work was provided by the National Aeronautics and Space Administration through Chandra Award Number GO3-14015A and GO3-14015E 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. M.F.C., J.S.N., W.L.W., C.M.P.R., and K.H. gratefully acknowledge this support. M.F.C. acknowledges support from NASA under cooperative agreement number NNG06EO90A. N.R.E. is grateful for support from the Chandra X-ray Center NASA Contract NAS8-03060. C.M.P.R. is 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. T.S. is grateful for financial support from the Leibniz Graduate School for Quantitative Spectroscopy in Astrophysics, a joint project of the Leibniz Institute for Astrophysics Potsdam (AIP) and the institute of Physics and Astronomy of the University of Potsdam. Y.N. acknowledges support from the Fonds National de la Recherche Scientifique (Belgium), the Communaute Francaise de Belgique, the PRODEX XMM and Integral contracts, and the "Action de Recherche Concertee" (CFWB-Academie Wallonie Europe). N.D.R. gratefully acknowledges his CRAQ (Centre de Recherche en Astrophysique du Quebec) fellowship. A.F.J.M. is grateful for financial support from NSERC (Canada) and FRQNT (Quebec). J.L.H. acknowledges support from NASA award NNX13AF40G and NSF award AST-0807477. This research has made use of NASA's Astrophysics Data System. 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. This research also made use of the Chandra Transmission Grating Catalog and archive (http://tgcat.mit.edu). The SPH simulations presented in this paper made use of the resources provided by the NASA High-End Computing (HEC) Program through the NASA Advanced Supercomputing (NAS) Division at Ames Research Center. NR 68 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 AUG 20 PY 2015 VL 809 IS 2 AR 132 DI 10.1088/0004-637X/809/2/132 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CR9EC UT WOS:000361655100025 ER PT J AU Guillochon, J Ramirez-Ruiz, E AF Guillochon, James Ramirez-Ruiz, Enrico TI A DARK YEAR FOR TIDAL DISRUPTION EVENTS SO ASTROPHYSICAL JOURNAL LA English DT Article DE black hole physics; galaxies: active; gravitation ID MASSIVE BLACK-HOLE; OBLIQUE SHOCK BREAKOUT; GALACTIC NUCLEI; STELLAR DISRUPTION; WHITE-DWARFS; SWIFT J1644+57; DISK ACCRETION; STARS; DYNAMICS; FLARES AB Main-sequence disruptions of stars by supermassive black holes result in the production of an extended, geometrically thin debris stream winding repeatedly around the black hole. In the absence of black hole spin, inplane relativistic precession causes this stream to intersect with itself after a single winding. In this paper we show that relativistic precessions arising from black hole spin can induce deflections out of the original orbital plane that prevent the stream from self-intersecting even after many windings. This naturally leads to a " dark period" in which the flare is not observable for some time, persisting for up to a dozen orbital periods of the most bound material, which translates to years for disruptions around black holes with masses similar to 10(7)M(circle dot). When the stream eventually self-intersects, the distance from the black hole and the angle at which this collision occurs determine the rate of energy dissipation. We find that more-massive black holes (M-h greater than or similar to 10(7)M(circle dot)) tend to have more violent stream self-intersections, resulting in prompt accretion. For these tidal disruption events (TDEs), the accretion rate onto the black hole should still closely follow the original fallback rate after a fixed delay time t(delay), (M) over dot(acc) (t + t(delay) ) = (M) over dot (fb) (t). For lower black hole masses (M-h less than or similar to 10(6)), we find that flares are typically slowed down by about an order of magnitude, resulting in the majority of TDEs being sub-Eddington at peak. This also implies that current searches for TDEs are biased toward prompt flares, with slowed flares likely having been unidentified. C1 [Guillochon, James] Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, Cambridge, MA 02138 USA. [Ramirez-Ruiz, Enrico] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. RP Guillochon, J (reprint author), Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, 60 Garden St, Cambridge, MA 02138 USA. EM jguillochon@cfa.harvard.edu OI Guillochon, James/0000-0002-9809-8215 FU Aspen Center for Physics (NSF) [1066293]; Einstein grant [PF3-140108]; Packard grant; NASA ATP grant [NNX14AH37G] FX We thank J. Dexter, G. Farrar, A. Gruzinov, Y. Jiang, D. Kasen, J. Krolik, A. Loeb, M. MacLeod, M. McCourt, M. Rees, E. Rossi, N. Roth, J. Steiner, N. Stone, and E. Tejeda for useful discussions, and the Aspen Center for Physics (NSF grant 1066293) for their hospitality. We also would like to thank the anonymous referee for their helpful suggestions. This work was supported by Einstein grant PF3-140108 (J. G.), the Packard grant (E. R.), and NASA ATP grant NNX14AH37G (E. R.). NR 66 TC 21 Z9 21 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD AUG 20 PY 2015 VL 809 IS 2 AR 166 DI 10.1088/0004-637X/809/2/166 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CR9EC UT WOS:000361655100059 ER PT J AU Guo, XY Esin, A Di Stefano, R Taylor, J AF Guo, Xinyi Esin, Ann Di Stefano, Rosanne Taylor, Jeffrey TI PERIODIC SIGNALS IN BINARY MICROLENSING EVENTS SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries: general; Galaxy: general; gravitational lensing: micro; methods: data analysis; planets and satellites: general ID TIME-SERIES; DIFFERENTIAL ROTATION; PLANET PHOTOMETRY; GALACTIC HALO; LIGHT CURVES; LENSES; DISCOVERY; DATABASE; SYSTEMS; STARS AB Gravitational microlensing events are powerful tools for the study of stellar populations. In particular, they can be used to discover and study a variety of binary systems. A large number of binary lenses have already been found through microlensing surveys and a few of these systems show strong evidence of orbital motion on the timescale of the lensing event. We expect that more binary lenses of this kind will be detected in the future. For binaries whose orbital period is comparable to the event duration, the orbital motion can cause the lensing signal to deviate drastically from that of a static binary lens. The most striking property of such light curves is the presence of quasi-periodic features, which are produced as the source traverses the same regions in the rotating lens plane. These repeating features contain information about the orbital period of the lens. If this period can be extracted, then much can be learned about the lensing system even without performing time-consuming, detailed light-curve modeling. However, the relative transverse motion between the source and the lens significantly complicates the problem of period extraction. To resolve this difficulty, we present a modification of the standard Lomb-Scargle periodogram analysis. We test our method for four representative binary lens systems and demonstrate its efficiency in correctly extracting binary orbital periods. C1 [Guo, Xinyi; Di Stefano, Rosanne] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Guo, Xinyi] Pomona Coll, Dept Phys & Astron, Claremont, CA 91711 USA. [Esin, Ann; Taylor, Jeffrey] Harvey Mudd Coll, Dept Phys, Claremont, CA 91711 USA. RP Guo, XY (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. FU NSF [AST-1211843, AST-0708924, AST-0908878]; NASA [NNX12AE39GAR-13243.01-A] FX We thank Christopher Night for significant contributions to an earlier version of this work and the anonymous referee for constructive comments. This work was supported in part by support from NSF AST-1211843, AST-0708924, and AST-0908878 and NASA NNX12AE39GAR-13243.01-A. NR 35 TC 1 Z9 1 U1 1 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD AUG 20 PY 2015 VL 809 IS 2 AR 182 DI 10.1088/0004-637X/809/2/182 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CR9EC UT WOS:000361655100075 ER PT J AU Lansbury, GB Gandhi, P Alexander, DM Assef, RJ Aird, J Annuar, A Ballantyne, DR Balokovic, M Bauer, FE Boggs, SE Brandt, WN Brightman, M Christensen, FE Civano, F Comastri, A Craig, WW Del Moro, A Grefenstette, BW Hailey, CJ Harrison, FA Hickox, RC Koss, M LaMassa, SM Luo, B Puccetti, S Stern, D Treister, E Vignali, C Zappacosta, L Zhang, WW AF Lansbury, G. B. Gandhi, P. Alexander, D. M. Assef, R. J. Aird, J. Annuar, A. Ballantyne, D. R. Balokovic, M. Bauer, F. E. Boggs, S. E. Brandt, W. N. Brightman, M. Christensen, F. E. Civano, F. Comastri, A. Craig, W. W. Del Moro, A. Grefenstette, B. W. Hailey, C. J. Harrison, F. A. Hickox, R. C. Koss, M. LaMassa, S. M. Luo, B. Puccetti, S. Stern, D. Treister, E. Vignali, C. Zappacosta, L. Zhang, W. W. TI NuSTAR REVEALS EXTREME ABSORPTION IN z < 0.5 TYPE 2 QUASARS SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: active; X-rays: galaxies ID ACTIVE GALACTIC NUCLEI; HARD X-RAY; DIGITAL-SKY-SURVEY; SEYFERT 2 GALAXIES; COMPTON-THICK AGN; XMM-NEWTON OBSERVATIONS; ULTRALUMINOUS INFRARED GALAXIES; RESOLUTION SPECTRAL TEMPLATES; LUMINOUS OBSCURED QUASARS; APPROXIMATE-TO 2 AB The intrinsic column density (N-H) distribution of quasars is poorly known. At the high obscuration end of the quasar population and for redshifts z < 1, the X-ray spectra can only be reliably characterized using broad-band measurements that extend to energies above 10 keV. Using the hard X-ray observatory NuSTAR, along with archival Chandra and XMM-Newton data, we study the broad-band X-ray spectra of nine optically selected (from the SDSS), candidate Compton-thick (N-H > 1.5 x 10(24) cm(-2)) type 2 quasars (CTQSO2s); five new NuSTAR observations are reported herein, and four have been previously published. The candidate CTQSO2s lie at z < 0.5, have observed [O III] luminosities in the range 8.4< log(L-[O III]/L circle dot)< 9.6, and show evidence for extreme, Compton-thick absorption when indirect absorption diagnostics are considered. Among the nine candidate CTQSO2s, five are detected by NuSTAR in the high-energy (8-24 keV) band: two are weakly detected at the approximate to 3 sigma confidence level and three are strongly detected with sufficient counts for spectral modeling (greater than or similar to 90 net source counts at 8-24 keV). For these NuSTAR-detected sources direct (i.e., X-ray spectral) constraints on the intrinsic active galactic nucleus properties are feasible, and we measure column densities approximate to 2.5-1600 times higher and intrinsic (unabsorbed) X-ray luminosities approximate to 10-70 times higher than pre-NuSTAR constraints from Chandra and XMM-Newton. Assuming the NuSTAR-detected type 2 quasars are representative of other Compton-thick candidates, we make a correction to the N-H distribution for optically selected type 2 quasars as measured by Chandra and XMM-Newton for 39 objects. With this approach, we predict a Compton-thick fraction of f(CT) = 36(-12)(+14)%, although higher fractions (up to 76%) are possible if indirect absorption diagnostics are assumed to be reliable. C1 [Lansbury, G. B.; Gandhi, P.; Alexander, D. M.; Annuar, A.; Del Moro, A.] Univ Durham, Ctr Extragalact Astron, Dept Phys, Durham DH1 3LE, England. [Gandhi, P.] Univ Southampton, Sch Phys & Astron, Southampton SO17, Hants, England. [Assef, R. J.] Univ Diego Portales, Nucleo Astron, Fac Ingn, Santiago, Chile. [Aird, J.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Ballantyne, D. R.] Georgia Inst Technol, Sch Phys, Ctr Relativist Astrophys, Atlanta, GA 30332 USA. [Balokovic, M.; Brightman, M.; Grefenstette, B. W.; Harrison, F. A.] CALTECH, Cahill Ctr Astrophys, Pasadena, CA 91125 USA. [Bauer, F. E.] Pontificia Univ Catolica Chile, Inst Astrofis, Fac Fis, Santiago 22, Chile. [Bauer, F. E.] Millennium Inst Astrophys, Santiago 7820436, Chile. [Bauer, F. E.] Space Sci Inst, Boulder, CO 80301 USA. [Boggs, S. E.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Brandt, W. N.; Luo, B.] Penn State Univ, Dept Astron & Astrophys, Davey Lab 525, University Pk, PA 16802 USA. [Brandt, W. N.; Luo, B.] Penn State Univ, Inst Gravitat & Cosmos, University Pk, PA 16802 USA. [Christensen, F. E.; Craig, W. W.] Tech Univ Denmark, DTU Space Natl Space Inst, DK-2800 Lyngby, Denmark. [Civano, F.; LaMassa, S. M.] Yale Univ, Dept Phys, Yale Ctr Astron & Astrophys, New Haven, CT 06520 USA. [Civano, F.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. [Civano, F.; Hickox, R. C.] Dartmouth Coll, Dept Phys & Astron, Hanover, NH 03755 USA. [Comastri, A.] INAF Osservatorio Astron Bologna, I-40127 Bologna, Italy. [Craig, W. W.] Lawrence Livermore Natl Lab, Livermore, CA 94550 USA. [Hailey, C. J.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA. [Koss, M.] Swiss Fed Inst Technol, Inst Astron, Dept Phys, CH-8093 Zurich, Switzerland. [Puccetti, S.] ASDC ASI, I-00133 Rome, Italy. [Puccetti, S.; Zappacosta, L.] INAF Osservatorio Astron Roma, I-00040 Monte Porzio Catone, RM, Italy. [Stern, D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Treister, E.] Univ Concepcion, Dept Astron, Concepcion, Chile. [Vignali, C.] Univ Bologna, Dipartimento Fis & Astron, I-40127 Bologna, Italy. [Zhang, W. W.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Lansbury, GB (reprint author), Univ Durham, Ctr Extragalact Astron, Dept Phys, South Rd, Durham DH1 3LE, England. EM g.b.lansbury@durham.ac.uk RI Comastri, Andrea/O-9543-2015; Vignali, Cristian/J-4974-2012; Brandt, William/N-2844-2015; Boggs, Steven/E-4170-2015; OI Comastri, Andrea/0000-0003-3451-9970; Lansbury, George/0000-0002-5328-9827; Vignali, Cristian/0000-0002-8853-9611; Puccetti, Simonetta/0000-0002-2734-7835; Brandt, William/0000-0002-0167-2453; Boggs, Steven/0000-0001-9567-4224; Koss, Michael/0000-0002-7998-9581; Ballantyne, David/0000-0001-8128-6976 FU Science and Technology Facilities Council (STFC) [ST/K501979/1, ST/J003697/1, ST/I001573/1]; Leverhulme Trust; Gemini-CONICYT [32120009]; ERC Advanced Grant FEEDBACK at the University of Cambridge; NSF AST award [1008067]; NASA Earth and Space Science Fellowship Program [NNX14AQ07H]; CONICYT-Chile [PFB-06/2007, FONDECYT 1141218, ACT1101]; Ministry of Economy, Development, and Tourism's Millennium Science Initiative [IC120009]; Caltech NuSTAR subcontract [44A-1092750]; NASA ADP grant [NNX10AC99G]; Caltech Kingsley visitor program; ASI/INAF [I/037/12/0011/13]; NASA ADAP award [NNX12AE38G]; National Science Foundation [1211096]; Swiss National Science Foundation [PP00P2_138979/1]; NASA [NNG08FD60C]; National Aeronautics and Space Administration FX We thank the referee for a careful review, which has improved this work. We acknowledge financial support from: the Science and Technology Facilities Council (STFC) grants ST/K501979/1 (G.B.L.), ST/J003697/1 (P.G.), ST/I001573/1 (D.M.A. and A.D.M.); the Leverhulme Trust (D.M.A.); Gemini-CONICYT grant 32120009 (R.J.A.); the ERC Advanced Grant FEEDBACK at the University of Cambridge (J.A.); NSF AST award 1008067 (D.R.B.); the NASA Earth and Space Science Fellowship Program, grant NNX14AQ07H (M.B.); CONICYT-Chile grants Basal-CATA PFB-06/2007 (F.E.B.), FONDECYT 1141218 (F.E.B.), and "EMBIGGEN" Anillo ACT1101 (F.E.B.); the Ministry of Economy, Development, and Tourism's Millennium Science Initiative grant IC120009, awarded to The Millennium Institute of Astrophysics, MAS (F.E.B.); Caltech NuSTAR subcontract 44A-1092750 (W.N.B. and B.L.); NASA ADP grant NNX10AC99G (W.N.B. and B.L.); the Caltech Kingsley visitor program (A.C.); ASI/INAF grant I/037/12/0011/13 (A.C., S.P., C.V.); NASA ADAP award NNX12AE38G (R.C.H.); National Science Foundation grant 1211096 (R.C.H.); and Swiss National Science Foundation grant PP00P2_138979/1 (M.K.). We thank Andrew Ptak and Jianjun Jia for the useful correspondence. This work was supported under NASA Contract No. NNG08FD60C and made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. We thank the NuSTAR Operations, Software and Calibration teams for support with the execution and analysis of these observations. This research has made use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA). NR 112 TC 21 Z9 21 U1 1 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD AUG 20 PY 2015 VL 809 IS 2 AR 115 DI 10.1088/0004-637X/809/2/115 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CR9EC UT WOS:000361655100008 ER PT J AU Nichols, J Huenemoerder, DP Corcoran, MF Waldron, W Naze, Y Pollock, AMT Moffat, AFJ Lauer, J Shenar, T Russell, CMP Richardson, ND Pablo, H Evans, NR Hamaguchi, K Gull, T Hamann, WR Oskinova, L Ignace, R Hoffman, JL Hole, KT Lomax, JR AF Nichols, J. Huenemoerder, D. P. Corcoran, M. F. Waldron, W. Naze, Y. Pollock, A. M. T. Moffat, A. F. J. Lauer, J. Shenar, T. Russell, C. M. P. Richardson, N. D. Pablo, H. Evans, N. R. Hamaguchi, K. Gull, T. Hamann, W. -R. Oskinova, L. Ignace, R. Hoffman, Jennifer L. Hole, K. T. Lomax, J. R. TI A COORDINATED X-RAY AND OPTICAL CAMPAIGN OF THE NEAREST MASSIVE ECLIPSING BINARY, delta ORIONIS Aa. II. X-RAY VARIABILITY SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries: close; binaries: eclipsing; stars: individual ([HD 36486]delta Ori A) ID EARLY-TYPE STARS; SHORT-TERM VARIABILITY; HELIUM-LIKE IONS; O-TYPE STARS; ABSORPTION COMPONENTS; LINE INTENSITIES; COLLIDING WINDS; MAIN-SEQUENCE; ZETA-OPHIUCHI; TIME-SERIES AB We present time-resolved and phase-resolved variability studies of an extensive X-ray high-resolution spectral data set of the delta Ori Aa binary system. The four observations, obtained with Chandra ACIS HETGS, have a total exposure time of approximate to 479 ks and provide nearly complete binary phase coverage. Variability of the total X-ray flux in the range of 5-25 is is confirmed, with a maximum amplitude of about +/- 15% within a single approximate to 125 ks observation. Periods of 4.76 and 2.04 days are found in the total X-ray flux, as well as an apparent overall increase in the flux level throughout the nine-day observational campaign. Using 40 ks contiguous spectra derived from the original observations, we investigate the variability of emission line parameters and ratios. Several emission lines are shown to be variable, including S XV, Si XIII, and Ne IX. For the first time, variations of the X-ray emission line widths as a function of the binary phase are found in a binary system, with the smallest widths at phi = 0.0 when the secondary delta Ori Aa2 is at the inferior conjunction. Using 3D hydrodynamic modeling of the interacting winds, we relate the emission line width variability to the presence of a wind cavity created by a wind-wind collision, which is effectively void of embedded wind shocks and is carved out of the X-ray-producing primary wind, thus producing phase-locked X-ray variability. C1 [Nichols, J.; Lauer, J.; Evans, N. R.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Huenemoerder, D. P.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Corcoran, M. F.; Hamaguchi, K.] NASA GSFC, CRESST, Greenbelt, MD 20771 USA. [Corcoran, M. F.; Hamaguchi, K.] NASA GSFC, XRay Astrophys Lab, Greenbelt, MD 20771 USA. [Waldron, W.] Univ Space Res Assoc, Columbia, MD 21046 USA. [Naze, Y.] Eureka Sci Inc, Oakland, CA 94602 USA. [Pollock, A. M. T.] Univ Liege, FNRS Dept AGO, B-4000 Liege, Belgium. [Moffat, A. F. J.; Richardson, N. D.; Pablo, H.] European Space Agcy, XMM Newton Sci Operat Ctr, European Space Astron Ctr, E-28691 Villanueva De La Canada, Spain. [Shenar, T.; Hamann, W. -R.; Oskinova, L.] Univ Montreal, Dept Phys, Montreal, PQ H3C 3J7, Canada. [Hamaguchi, K.] Univ Potsdam, Inst Phys & Astron, D-14476 Potsdam, Germany. [Gull, T.] Univ Maryland Baltimore Cty, Dept Phys, Baltimore, MD 21250 USA. [Ignace, R.] NASA GSFC, Greenbelt, MD 20771 USA. [Hoffman, Jennifer L.] E Tennessee State Univ, Phys & Astron, Johnson City, TN 37614 USA. [Hole, K. T.] Univ Denver, Dept Phys & Astron, Denver, CO 80208 USA. [Lomax, J. R.] Weber State Univ, Dept Phys, Ogden, UT 84408 USA. [Russell, C. M. P.] Univ Oklahoma, Homer L Dodge Dept Phys & Astron, Norman, OK 73019 USA. [Russell, C. M. P.] NASA Goddard Space Flight Ctr, Xray Astrophys Lab, Greenbelt, MD 20771 USA. Oak Ridge Associated Univ, Oak Ridge, TN 37831 USA. RP Nichols, J (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. FU National Aeronautics and Space Administration through Chandra Award [GO3-14015A, G03-14015E, GO3-14015G]; National Aeronautics Space Administration [NAS8-03060]; NASA through the Smithsonian Astrophysical Observatory [SV3-73016]; Fonds National de la Recherche Scientifique (Belgium); Communaute Francaise de Belgique; PRODEX XMM and Integral contracts; Action de Recherche Concertee (CFWB-Academie Wallonie Europe); NSRC (Canada); FRQNT (Quebec); CRAQ (Centre de Recherche en Astrophysique du Quebec) fellowship; DLR [50 OR 1302]; Chandra X-ray Center NASA [NAS8-03060]; NASA [NNX13AF40G]; NSF [AST-0807477] FX The authors acknowledge the constructive comments of the anomymous referee. M.F.C., J.S.N., W.L.W., C.M.P.R., and K.H. are grateful for support provided by the National Aeronautics and Space Administration through Chandra Award Number GO3-14015A, G03-14015E, and GO3-14015G 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. D.P.H. was supported by NASA through the Smithsonian Astrophysical Observatory contract SV3-73016 to MIT for the Chandra X-ray Center and Science Instruments. Y.N. acknowledges support from the Fonds National de la Recherche Scientifique (Belgium), the Communaute Francaise de Belgique, the PRODEX XMM and Integral contracts, and the Action de Recherche Concertee (CFWB-Academie Wallonie Europe). A.F.J.M. is grateful for financial aid from NSRC (Canada) and FRQNT (Quebec). N.D.R. gratefully acknowledges his CRAQ (Centre de Recherche en Astrophysique du Quebec) fellowship. L.M.O. acknowledges support from DLR grant 50 OR 1302. N.R.E. is grateful for support from the Chandra X-ray Center NASA Contract NAS8-03060. J.L.H. acknowledges support from NASA award NNX13AF40G and NSF award AST-0807477. M.F.C., J.S.N., and K.H. also acknowledge helpful discussions with John Houck and Michael Nowak on data analysis with ISIS, and Craig Anderson for technical support. 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. This research made use of the Chandra Transmission Grating Catalog and archive (http://tgcat.mit.edu). This research also has made use of NASA's Astrophysics Data System. NR 80 TC 5 Z9 5 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD AUG 20 PY 2015 VL 809 IS 2 AR 133 DI 10.1088/0004-637X/809/2/133 PG 21 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CR9EC UT WOS:000361655100026 ER PT J AU Nunez, A Agueros, MA Covey, KR Hartman, JD Kraus, AL Bowsher, EC Douglas, ST Lopez-Morales, M Pooley, DA Posselt, B Saar, SH West, AA AF Nunez, Alejandro Agueeros, Marcel A. Covey, Kevin R. Hartman, Joel D. Kraus, Adam L. Bowsher, Emily C. Douglas, Stephanie T. Lopez-Morales, Mercedes Pooley, David A. Posselt, Bettina Saar, Steven H. West, Andrew A. TI LINKING STELLAR CORONAL ACTIVITY AND ROTATION AT 500 MYR: A DEEP CHANDRA OBSERVATION OF M37 SO ASTROPHYSICAL JOURNAL LA English DT Article DE open clusters and associations: individual (M37); stars: activity; stars: coronae; stars: rotation X-rays: individual (M37) ID X-RAY-EMISSION; SOLAR-TYPE STARS; LOW-MASS STARS; PERSEI OPEN CLUSTER; DIGITAL SKY SURVEY; MMT1 TRANSIT SURVEY; FIELD-NORTH SURVEY; ALPHA-PERSEI; MAGNETIC ACTIVITY; RADIAL-VELOCITIES AB Empirical calibrations of the stellar age-rotation-activity relation (ARAR) rely on observations of the co-eval populations of stars in open clusters. We used the Chandra X-ray Observatory to study M37, a 500-Myr-old open cluster that has been extensively surveyed for rotation periods (P-rot). M37 was observed almost continuously for five days, for a total of 440.5 ks, to measure stellar X-ray luminosities (L-X), a proxy for coronal activity, across a wide range of masses. The cluster's membership catalog was revisited to calculate updated membership probabilities from photometric data and each star's distance to the cluster center. The result is a comprehensive sample of 1699 M37 members: 426 with Prot, 278 with X-ray detections, and 76 with both. We calculate Rossby numbers, R-o = P-rot/T, where T is the convective turnover time, and ratios of the X-ray-to-bolometric luminosity, L-X/L-bol, to minimize mass dependencies in our characterization of the rotation-coronal activity relation at 500 Myr. We find that fast rotators, for which R-o< 0.09 +/- 0.01, show saturated levels of activity, with log(L-X/L-bol) = -3.06 +/- 0.04. For R-o. 0.09 +/- 0.01, activity is unsaturated and follows a power law of the form Ro b, where beta = -2.03(-0.14)(+0.17). This is the largest sample available for analyzing the dependence of coronal emission on rotation for a single-aged population, covering stellar masses in the range 0.4-1.3 M-circle dot, P-rot in the range 0.4-12.8 days, and L-X in the range 10(28.4-30.5) erg s(-1). Our results make M37 a new benchmark open cluster for calibrating the ARAR at ages of approximate to 500 Myr. C1 [Nunez, Alejandro; Agueeros, Marcel A.; Bowsher, Emily C.; Douglas, Stephanie T.] Columbia Univ, Dept Astron, New York, NY 10027 USA. [Covey, Kevin R.] Western Washington Univ, Dept Phys & Astron, Bellingham, WA 98225 USA. [Hartman, Joel D.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. [Kraus, Adam L.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA. [Lopez-Morales, Mercedes; Saar, Steven H.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02183 USA. [Pooley, David A.] Sam Houston State Univ, Dept Phys, Huntsville, TX 77341 USA. [Pooley, David A.] Eureka Sci Inc, Oakland, CA 94602 USA. [Posselt, Bettina] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [West, Andrew A.] Boston Univ, Dept Astron, Boston, MA 02215 USA. RP Nunez, A (reprint author), Columbia Univ, Dept Astron, 550 West 120th St, New York, NY 10027 USA. OI Nunez, Alejandro/0000-0002-8047-1982; Douglas, Stephanie/0000-0001-7371-2832; Posselt, Bettina/0000-0003-2317-9747; Covey, Kevin/0000-0001-6914-7797; Hartman, Joel/0000-0001-8732-6166; Agueros, Marcel/0000-0001-7077-3664 FU NASA through Chandra Award [G02-13025A]; NASA [NAS8-03060]; NSF [AST-1255419] FX We thank the referee for a careful reading of the paper. We thank Patrick Broos for his help with the AE package and Maureen van den Berg for her help with obtaining unabsorbed X-ray fluxes. Support for this work was provided by NASA through Chandra Award Number G02-13025A 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. M.A.A. acknowledges support provided by the NSF through grant AST-1255419. NR 81 TC 1 Z9 1 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD AUG 20 PY 2015 VL 809 IS 2 AR 161 DI 10.1088/0004-637X/809/2/161 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CR9EC UT WOS:000361655100054 ER PT J AU Pablo, H Richardson, ND Moffat, AFJ Corcoran, M Shenar, T Benvenuto, O Fuller, J Naze, Y Hoffman, JL Miroshnichenko, A Apellaniz, JM Evans, N Eversberg, T Gayley, K Gull, T Hamaguchi, K Hamann, WR Henrichs, H Hole, T Ignace, R Iping, R Lauer, J Leutenegger, M Lomax, J Nichols, J Oskinova, L Owocki, S Pollock, A Russell, CMP Waldron, W Buil, C Garrel, T Graham, K Heathcote, B Lemoult, T Li, D Mauclaire, B Potter, M Ribeiro, J Matthews, J Cameron, C Guenther, D Kuschnig, R Rowe, J Rucinski, S Sasselov, D Weiss, W AF Pablo, Herbert Richardson, Noel D. Moffat, Anthony F. J. Corcoran, Michael Shenar, Tomer Benvenuto, Omar Fuller, Jim Naze, Yael Hoffman, Jennifer L. Miroshnichenko, Anatoly Apellaniz, Jesus Maiz Evans, Nancy Eversberg, Thomas Gayley, Ken Gull, Ted Hamaguchi, Kenji Hamann, Wolf-Rainer Henrichs, Huib Hole, Tabetha Ignace, Richard Iping, Rosina Lauer, Jennifer Leutenegger, Maurice Lomax, Jamie Nichols, Joy Oskinova, Lida Owocki, Stan Pollock, Andy Russell, Christopher M. P. Waldron, Wayne Buil, Christian Garrel, Thierry Graham, Keith Heathcote, Bernard Lemoult, Thierry Li, Dong Mauclaire, Benjamin Potter, Mike Ribeiro, Jose Matthews, Jaymie Cameron, Chris Guenther, David Kuschnig, Rainer Rowe, Jason Rucinski, Slavek Sasselov, Dimitar Weiss, Werner TI A COORDINATED X-RAY AND OPTICAL CAMPAIGN OF THE NEAREST MASSIVE ECLIPSING BINARY, delta ORIONIS Aa. III. ANALYSIS OF OPTICAL PHOTOMETRIC (MOST) AND SPECTROSCOPIC (GROUND BASED) VARIATIONS SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries: close; binaries: eclipsing; stars: early-type; stars: individual (delta Ori A); stars: mass-loss; stars: variables: general ID APSIDAL MOTION; STARS; SYSTEM; PULSATIONS; KOI-54; SPECTRA; ORBITS; SPOTS; ORI AB We report on both high-precision photometry from the Microvariability and Oscillations of Stars (MOST) space telescope and ground-based spectroscopy of the triple system delta Ori A, consisting of a binary O9.5II+early-B (Aa1 and Aa2) with P = 5.7 days, and a more distant tertiary (O9 IV P > 400 years). This data was collected in concert with X-ray spectroscopy from the Chandra X-ray Observatory. Thanks to continuous coverage for three weeks, the MOST light curve reveals clear eclipses between Aa1 and Aa2 for the first time in non-phased data. From the spectroscopy, we have a well-constrained radial velocity (RV) curve of Aa1. While we are unable to recover RV variations of the secondary star, we are able to constrain several fundamental parameters of this system and determine an approximate mass of the primary using apsidal motion. We also detected second order modulations at 12 separate frequencies with spacings indicative of tidally influenced oscillations. These spacings have never been seen in a massive binary, making this system one of only a handful of such binaries that show evidence for tidally induced pulsations. C1 [Pablo, Herbert; Richardson, Noel D.; Moffat, Anthony F. J.] Univ Montreal, Dept Phys, Montreal, PQ H3C 3J7, Canada. [Pablo, Herbert; Richardson, Noel D.; Moffat, Anthony F. J.] Univ Montreal, CRAQ, Montreal, PQ H3C 3J7, Canada. [Corcoran, Michael; Hamaguchi, Kenji] NASA GSFC, CRESST, Greenbelt, MD 20771 USA. [Corcoran, Michael; Hamaguchi, Kenji] NASA GSFC, Xray Astrophys Lab, Greenbelt, MD 20771 USA. [Corcoran, Michael; Iping, Rosina] Univ Space Res Assoc, Columbia, MD 21046 USA. [Shenar, Tomer; Hamann, Wolf-Rainer; Oskinova, Lida] Univ Potsdam, Inst Phys & Astron, D-14476 Potsdam, Germany. [Benvenuto, Omar] Univ Nacl La Plata, Fac Ciencias Astron & Geofis, RA-1900 Buenos Aires, DF, Argentina. [Benvenuto, Omar] UNLP, CONICET, CCT, IALP, La Plata, Buenos Aires, Argentina. [Fuller, Jim] CALTECH, Walter Burke Inst Theoret Phys, TAPIR, Pasadena, CA 91125 USA. [Fuller, Jim; Leutenegger, Maurice] Univ Calif Santa Barbara, Kavli Inst Theoret Phys, Santa Barbara, CA 93106 USA. [Naze, Yael] Univ Liege, FNRS Dept AGO, B-4000 Liege, Belgium. [Hoffman, Jennifer L.] Univ Denver, Dept Phys & Astron, Denver, CO 80208 USA. [Miroshnichenko, Anatoly] Univ N Carolina, Dept Phys & Astron, Greensboro, NC 27402 USA. [Apellaniz, Jesus Maiz] Ctr Astrobiol CSIC INTA, E-28691 Villanueva De La Caada, Spain. [Evans, Nancy; Lauer, Jennifer; Nichols, Joy] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. [Eversberg, Thomas] Schnorringen Telescope Sci Inst, Waldbrol, Germany. [Gayley, Ken] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA. [Gull, Ted] NASA Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA. [Henrichs, Huib] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 XH Amsterdam, Netherlands. [Hole, Tabetha; Ignace, Richard] E Tennessee State Univ, Dept Phys & Astron, Johnson City, TN 37614 USA. [Lomax, Jamie] Univ Oklahoma, HL Dodge Dept Phys & Astron, Norman, OK 73019 USA. [Owocki, Stan] Univ Delaware, Bartol Res Inst, Newark, DE 19716 USA. [Pollock, Andy] European Space Agcy, E-28691 Madrid, Spain. [Russell, Christopher M. P.] NASA Goddard Space Flight Ctr, Xray Astrophys Lab, Greenbelt, MD 20771 USA. [Russell, Christopher M. P.] Oak Ridge Associated Univ, Oak Ridge, TN 37831 USA. [Waldron, Wayne] Eureka Sci Inc, Oakland, CA 94602 USA. [Buil, Christian] Castanet Tolosan Observ, F-31320 Castanet Tolosan, France. [Garrel, Thierry] Observ Juvignac, F-34990 Juvignac, France. [Heathcote, Bernard] Barfold Observ, Glenhope, Vic 3444, Australia. [Lemoult, Thierry] Chelles Observ, F-77500 Chelles, France. [Li, Dong] Jade Observ, Tianjin 300251, Peoples R China. [Mauclaire, Benjamin] Observ Val Arc, F-13530 Trets, France. [Ribeiro, Jose] Observ Inst Geog Exercito, Lisbon, Portugal. [Matthews, Jaymie; Kuschnig, Rainer] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada. [Cameron, Chris] Cape Breton Univ, Dept Math Phys & Geol, Sydney, NS B1P 6L2, Canada. [Guenther, David] St Marys Univ, Inst Computat Astrophys, Dept Phys & Astron, Halifax, NS B3H 3C3, Canada. [Kuschnig, Rainer] Univ Vienna, Inst Astron, A-1180 Vienna, Austria. [Rowe, Jason] NASA Ames Res Ctr, Moffett Field, CA 94035 USA. [Rucinski, Slavek] Univ Toronto, Dept Astron & Astrophys, Toronto, ON M5S 3H4, Canada. [Sasselov, Dimitar] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Pablo, H (reprint author), Univ Montreal, Dept Phys, CP 6128,Succ Ctr Ville, Montreal, PQ H3C 3J7, Canada. EM hpablo@astro.umontreal.ca; richardson@astro.umontreal.ca FU Chandra grant [GO3-14015A, GO3-14015E]; Fonds National de la Recherche Scientifique (Belgium); Communaute Francaise de Belgique; PRODEX XMMAction de Recherche Concertee (CFWB-Academie Wallonie Europe); CRAQ (Centre de Recherche en Astrophysique du Quebec); Spanish Government Ministerio de Economia y Competitividad (MINECO) [AYA2010-15 081, AYA2010-17 631, AYA2013-40 611-P]; Consejeria de Educacion of the Junta de Andalucia [P08-TIC-4075]; Austrian Science Fund (FWF); Chandra X-ray Center NASA [NAS8-03060]; NASA [NNX13AF40G]; NSF [AST-0807477] FX M.F.C., J.S.N., W.L.W., and K.H. are grateful for support via Chandra grant GO3-14015A and GO3-14015E. Y.N. acknowledges support from the Fonds National de la Recherche Scientifique (Belgium), the Communaute Francaise de Belgique, the PRODEX XMM and Integral contracts, and the Action de Recherche Concertee (CFWB-Academie Wallonie Europe). N.D.R. gratefully acknowledges his CRAQ (Centre de Recherche en Astrophysique du Quebec) fellowship. A.F.J.M., D.B.G., J.M.M., and S.M.R. are grateful for financial aid to NSERC (Canada). A.F.J.M. and H.P. also thank FRQNT (Quebec) and the Canadian Space Agency. J.M.A. acknowledges support from (a) the Spanish Government Ministerio de Economia y Competitividad (MINECO) through grants AYA2010-15 081, AYA2010-17 631, and AYA2013-40 611-P and (b) the Consejeria de Educacion of the Junta de Andalucia through grant P08-TIC-4075. R.K. and W.W. acknowledge support by the Austrian Science Fund (FWF). N.R.E. is grateful for support from the Chandra X-ray Center NASA Contract NAS8-03060. J.L.H. acknowledges support from NASA award NNX13AF40G and NSF award AST-0807477. NR 61 TC 4 Z9 4 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD AUG 20 PY 2015 VL 809 IS 2 AR 134 DI 10.1088/0004-637X/809/2/134 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CR9EC UT WOS:000361655100027 ER PT J AU Roettenbacher, RM Monnier, JD Fekel, FC Henry, GW Korhonen, H Latham, DW Muterspaugh, MW Williamson, MH Baron, F ten Brummelaar, TA Che, X Harmon, RO Schaefer, GH Scott, NJ Sturmann, J Sturmann, L Turner, NH AF Roettenbacher, Rachael M. Monnier, John D. Fekel, Francis C. Henry, Gregory W. Korhonen, Heidi Latham, David W. Muterspaugh, Matthew W. Williamson, Michael H. Baron, Fabien ten Brummelaar, Theo A. Che, Xiao Harmon, Robert O. Schaefer, Gail H. Scott, Nicholas J. Sturmann, Judit Sturmann, Laszlo Turner, Nils H. TI DETECTING THE COMPANIONS AND ELLIPSOIDAL VARIATIONS OF RS CVN PRIMARIES. II. o DRACONIS, A CANDIDATE FOR RECENT LOW-MASS COMPANION INGESTION SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries: close; stars: activity; stars: imaging; stars: individual (o Draconis); stars: variables: general ID CLOSE BINARY-SYSTEMS; CHROMOSPHERICALLY ACTIVE STARS; CHARA ARRAY; SPECTROSCOPIC BINARIES; MODEL ATMOSPHERES; PRECISION ORBITS; SIGMA-GEMINORUM; TIDAL EVOLUTION; MAIN-SEQUENCE; ROTATION AB To measure the stellar and orbital properties of the metal-poor RS CVn binary o Draconis (o Dra), we directly detect the companion using interferometric observations obtained with the Michigan InfraRed Combiner at Georgia State University's Center for High Angular Resolution Astronomy (CHARA) Array. The H-band flux ratio between the primary and secondary stars is the highest confirmed flux ratio (370 +/- 40) observed with long-baseline optical interferometry. These detections are combined with radial velocity data of both the primary and secondary stars, including new data obtained with the Tillinghast Reflector Echelle Spectrograph on the Tillinghast Reflector at the Fred Lawrence Whipple Observatory and the 2 m Tennessee State University Automated Spectroscopic Telescope at Fairborn Observatory. We determine an orbit from which we find model-independent masses and ages of the components (M-A=1.35 +/- 0.05M., MB=0.99 +/- 0.02M(circle dot), system age = 3.0. -/+ 0.5 Gyr). An average of a 23-year light curve of o Dra from the Tennessee State University Automated Photometric Telescope folded over the orbital period newly reveals eclipses and the quasi-sinusoidal signature of ellipsoidal variations. The modeled light curve for our system's stellar and orbital parameters confirm these ellipsoidal variations due to the primary star partially filling its Roche lobe potential, suggesting most of the photometric variations are not due to stellar activity (starspots). Measuring gravity darkening from the average light curve gives a best-fit of beta=0.07 +/- 0.03, a value consistent with conventional theory for convective envelope stars. The primary star also exhibits an anomalously short rotation period, which, when taken with other system parameters, suggests the star likely engulfed a low-mass companion that had recently spun-up the star. C1 [Roettenbacher, Rachael M.; Monnier, John D.; Baron, Fabien; Che, Xiao] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Fekel, Francis C.; Henry, Gregory W.; Muterspaugh, Matthew W.; Williamson, Michael H.] Tennessee State Univ, Ctr Excellence Informat Syst, Nashville, TN 37209 USA. [Korhonen, Heidi] Univ Turku, Finnish Ctr Astron ESO FINCA, FI-21500 Piikkio, Finland. [Latham, David W.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [ten Brummelaar, Theo A.; Schaefer, Gail H.; Scott, Nicholas J.; Sturmann, Judit; Sturmann, Laszlo; Turner, Nils H.] Georgia State Univ, Ctr High Angular Resolut Astron, Mt Wilson, CA 91023 USA. [Harmon, Robert O.] Ohio Wesleyan Univ, Dept Phys & Astron, Delaware, OH 43015 USA. RP Roettenbacher, RM (reprint author), Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. EM rmroett@umich.edu RI Korhonen, Heidi/E-3065-2016; OI Korhonen, Heidi/0000-0003-0529-1161; Fekel, Francis/0000-0002-9413-3896; Latham, David/0000-0001-9911-7388 FU National Science Foundation through NSF [AST-0908253, AST-1211129]; Georgia State University through the College of Arts and Sciences; University of Michigan; NSF from the Major Research Instrumentation Program [1039522]; NASA; NSF [AST-1108963]; Tennessee State University; Centers of Excellence Program; NASA Harriet G. Jenkins Pre-Doctoral Fellowship; Sigma Xi FX We thank F. C. Adams, J. A. Orosz, D. Pourbaix, and M. Rieutord for their help and comments, as well as L. Boyd of Fairborn Observatory for his support of the photometric observations. The interferometric data in this paper were obtained at the CHARA Array, funded by the National Science Foundation through NSF grants AST-0908253 and AST-1211129, and by Georgia State University through the College of Arts and Sciences. The MIRC instrument at the CHARA Array was funded by the University of Michigan. NSF grant 1039522 from the Major Research Instrumentation Program, awarded to Tennessee State University, made extracting the secondary velocities possible. Astronomy at Tennessee State University is supported by the state of Tennessee through its Centers of Excellence program. The APT program was supported by NASA, NSF, Tennessee State University, and the Centers of Excellence Program. The Nordic Optical Telescope is operated on the island of La Palma jointly by Denmark, Finland, Iceland, Norway, and Sweden, in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias. R.M.R. would like to acknowledge support from the NASA Harriet G. Jenkins Pre-Doctoral Fellowship and a Sigma Xi Grant-in-Aid of Research. J.D.M. and R.M.R. acknowledge support of NSF grant AST-1108963. This research has made use of the SIMBAD database, operated at CDS, Strasbourg, France and the Jean-Marie Mariotti Center SearchCal service8 co-developed by FIZEAU and LAOG/IPAG, and of CDS Astronomical Databases SIMBAD and VIZIER.9 NR 66 TC 4 Z9 4 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD AUG 20 PY 2015 VL 809 IS 2 AR 159 DI 10.1088/0004-637X/809/2/159 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CR9EC UT WOS:000361655100052 ER PT J AU Shenar, T Oskinova, L Hamann, WR Corcoran, MF Moffat, AFJ Pablo, H Richardson, ND Waldron, WL Huenemoerder, DP Apellaniz, JM Nichols, JS Todt, H Naze, Y Hoffman, JL Pollock, AMT Negueruela, I AF Shenar, T. Oskinova, L. Hamann, W. -R. Corcoran, M. F. Moffat, A. F. J. Pablo, H. Richardson, N. D. Waldron, W. L. Huenemoerder, D. P. Maiz Apellaniz, J. Nichols, J. S. Todt, H. Naze, Y. Hoffman, J. L. Pollock, A. M. T. Negueruela, I. TI A COORDINATED X-RAY AND OPTICAL CAMPAIGN OF THE NEAREST MASSIVE ECLIPSING BINARY, delta ORIONIS Aa. IV. A MULTIWAVELENGTH, NON-LTE SPECTROSCOPIC ANALYSIS SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries: close; binaries: eclipsing; stars: early-type; stars: individual ([HD 36486]delta Ori A); X-rays: stars ID O-TYPE STARS; RADIATION-DRIVEN WINDS; BLANKETED MODEL ATMOSPHERES; EMISSION-LINE-PROFILES; B-TYPE SUPERGIANTS; HELIUM-LIKE IONS; STELLAR WINDS; GALACTIC O; LOSS RATES; COMPOSITE SPECTRA AB Eclipsing systems of massive stars allow one to explore the properties of their components in great detail. We perform a multi-wavelength, non-LTE analysis of the three components of the massive multiple system delta Ori A, focusing on the fundamental stellar properties, stellar winds, and X-ray characteristics of the system. The primary's distance-independent parameters turn out to be characteristic for its spectral type (O9.5 II), but usage of the Hipparcos parallax yields surprisingly low values for the mass, radius, and luminosity. Consistent values follow only if delta Ori lies at about twice the Hipparcos distance, in the vicinity of the sigma-Orionis cluster. The primary and tertiary dominate the spectrum and leave the secondary only marginally detectable. We estimate the V-band magnitude difference between primary and secondary to be Delta V approximate to 2.(m)8. The inferred parameters suggest that the secondary is an early B-type dwarf (approximate to B1 V), while the tertiary is an early B-type subgiant (approximate to B0 IV). We find evidence for rapid turbulent velocities (similar to 200 km s(-1)) and wind inhomogeneities, partially optically thick, in the primary's wind. The bulk of the X-ray emission likely emerges from the primary's stellar wind (logL(X)/L-Bol approximate to -6.85), initiating close to the stellar surface at R-0 similar to 1.1 R-*. Accounting for clumping, the mass-loss rate of the primary is found to be log (M) over dot approximate to -6.4 (M-circle dot yr(-1))., which agrees with hydrodynamic predictions, and provides a consistent picture along the X-ray, UV, optical, and radio spectral domains. C1 [Shenar, T.; Oskinova, L.; Hamann, W. -R.; Todt, H.] Univ Potsdam, Inst Phys & Astron, D-14476 Potsdam, Germany. [Corcoran, M. F.] NASA Goddard Space Flight Ctr, CRESST, Greenbelt, MD 20771 USA. [Corcoran, M. F.] NASA Goddard Space Flight Ctr, Xray Astrophys Lab, Greenbelt, MD 20771 USA. [Corcoran, M. F.] Univ Space Res Assoc, Columbia, MD 21044 USA. [Moffat, A. F. J.; Pablo, H.; Richardson, N. D.] Univ Montreal, Dept Phys, Montreal, PQ H3C 3J7, Canada. [Moffat, A. F. J.; Pablo, H.; Richardson, N. D.] Univ Montreal, CRAQ, Montreal, PQ H3C 3J7, Canada. [Waldron, W. L.] Eureka Sci Inc, Oakland, CA 94602 USA. [Huenemoerder, D. P.] MIT, Kalvi Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Maiz Apellaniz, J.] INTA CSIC, Ctr Astrobiol, E-28691 Madrid, Spain. [Nichols, J. S.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Naze, Y.] Univ Liege, Inst Astrophys & Geophys, Grp Astrophys Hautes Energies, B-4000 Sart Tilman Par Liege, Belgium. [Hoffman, J. L.] Univ Denver, Dept Phys & Astron, Denver, CO 80208 USA. [Pollock, A. M. T.] European Space Agcy, XMM Newton Sci Operat Ctr, European Space Astron Ctr, E-28691 Villanueva De La Canada, Spain. [Negueruela, I.] Univ Alicante, Escuela Politecn Super, Dept Fis Ingn Sistemas & Teoria Senal, E-03080 Alicante, Spain. RP Shenar, T (reprint author), Univ Potsdam, Inst Phys & Astron, Karl Liebknecht Str 24-25, D-14476 Potsdam, Germany. FU Leibniz Graduate School for Quantitative Spectroscopy in Astrophysics; Leibniz Institute for Astrophysics Potsdam (AIP); institute of Physics and Astronomy of the University of Potsdam; DLR [50 OR 1302]; Chandra grants [GO3-14015A, GO3-14015E]; NSERC (Canada); FRQNT (Quebec); Spanish Government Ministerio de Economia y Competitividad (MINECO) [AYA2010-15 081, AYA2010-17 631]; Consejeria de Educacion of the Junta de Andaluc ia [P08-TIC-4075]; Centre du Recherche en Astrophysique du Quebec (CRAQ) fellowship; Fonds National de la Recherche Scientifique (Belgium); Communaute Francaise de Belgique; PRODEX XMM and Integral contracts; "Action de Recherche Concertee" (CFWB-Academie Wallonie Europe); NASA [NNX13AF40G]; NSF [AST-0807477]; Spanish Mineco [AYA2012-39364-C02-01/02]; European Union FX We thank the anonymous referee for constructive comments which helped to improve our paper. T.S. is grateful for financial support from the Leibniz Graduate School for Quantitative Spectroscopy in Astrophysics, a joint project of the Leibniz Institute for Astrophysics Potsdam (AIP) and the institute of Physics and Astronomy of the University of Potsdam. L.M.O. acknowledges support from DLR grant 50 OR 1302. We thank A. Valeev and S. Fabrika for kindly providing us with an optical spectrum of the system. We thank T. J. Henry and J. A. Caballero for fruitful discussions regarding system's distance. M.F.C., J.S.N., and W.L.W. are grateful for support via Chandra grants GO3-14015A and GO3-14015E. A.F.J.M. acknowledges financial aid from NSERC (Canada) and FRQNT (Quebec). J.M.A. acknowledges support from (a) the Spanish Government Ministerio de Economia y Competitividad (MINECO) through grants AYA2010-15 081 and AYA2010-17 631 and (b) the Consejeria de Educacion of the Junta de Andaluc ia through grant P08-TIC-4075. Caballero N.D.R. gratefully acknowledges his Centre du Recherche en Astrophysique du Quebec (CRAQ) fellowship. Y.N. acknowledges support from the Fonds National de la Recherche Scientifique (Belgium), the Communaute Francaise de Belgique, the PRODEX XMM and Integral contracts, and the "Action de Recherche Concertee" (CFWB-Academie Wallonie Europe). J.L.H. acknowledges support from NASA award NNX13AF40G and NSF award AST-0807477. I.N. is supported by the Spanish Mineco under grant AYA2012-39364-C02-01/02, and the European Union. NR 146 TC 13 Z9 13 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD AUG 20 PY 2015 VL 809 IS 2 AR 135 DI 10.1088/0004-637X/809/2/135 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CR9EC UT WOS:000361655100028 ER PT J AU Webb, T Noble, A DeGroot, A Wilson, G Muzzin, A Bonaventura, N Cooper, M Delahaye, A Foltz, R Lidman, C Surace, J Yee, HKC Chapman, S Dunne, L Geach, J Hayden, B Hildebrandt, H Huang, JS Pope, A Smith, MWL Perlmutter, S Tudorica, A AF Webb, Tracy Noble, Allison DeGroot, Andrew Wilson, Gillian Muzzin, Adam Bonaventura, Nina Cooper, Mike Delahaye, Anna Foltz, Ryan Lidman, Chris Surace, Jason Yee, H. K. C. Chapman, Scott Dunne, Loretta Geach, James Hayden, Brian Hildebrandt, Hendrik Huang, Jiasheng Pope, Alexandra Smith, Matthew W. L. Perlmutter, Saul Tudorica, Alex TI AN EXTREME STARBURST IN THE CORE OF A RICH GALAXY CLUSTER AT z=1.7 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: clusters: general; galaxies: evolution; galaxies: interactions; galaxies: starburst ID ACTIVE GALACTIC NUCLEI; NEAR-INFRARED PROPERTIES; STAR-FORMATION ACTIVITY; WIDE-FIELD CAMERA; SPECTROSCOPIC CONFIRMATION; COOLING FLOWS; STELLAR MASS; X-RAY; EXTRAGALACTIC SURVEY; PHOTOMETRIC SYSTEM AB We have discovered an optically rich galaxy cluster at z = 1.7089 with star formation occurring in close proximity to the central galaxy. The system, SpARCS104922.6+ 564032.5, was detected within the Spitzer Adaptation of the red-sequence Cluster Survey, and confirmed through Keck-MOSFIRE spectroscopy. The rest-frame optical richness of N-gal (500 kpc) = 30 +/- 8 implies a total halo mass, within 500 kpc, of similar to 3.8 +/- 1.2 x 10(14) M-circle dot, comparable to other clusters at or above this redshift. There is a wealth of ancillary data available, including Canada-France-Hawaii Telescope optical, UKIRT-K, Spitzer-IRAC/MIPS, and Herschel-SPIRE. This work adds submillimeter imaging with the SCUBA2 camera on the James Clerk Maxwell Telescope and near-infrared imaging with the Hubble Space Telescope. The mid/far-infrared (M/FIR) data detect an Ultra-luminous Infrared Galaxy spatially coincident with the central galaxy, with L-IR = 6.2 +/- 0.9 x 10(12) L-circle dot. The detection of polycyclic aromatic hydrocarbons at z = 1.7 in a Spitzer-IRS spectrum of the source implies the FIR luminosity is dominated by star formation (an Active Galactic Nucleus contribution of 20%) with a rate of similar to 860 +/- 130 M-circle dot yr(-1). The optical source corresponding to the IR emission is likely a chain of > 10 individual clumps arranged as " beads on a string" over a linear scale of 66 kpc. Its morphology and proximity to the Brightest Cluster Galaxy (BCG) imply a gas-rich interaction at the center of the cluster triggered the star formation. This system indicates that wet mergers may be an important process in forming the stellar mass of BCGs at early times. C1 [Webb, Tracy; Bonaventura, Nina; Delahaye, Anna] McGill Univ, Dept Phys, Montreal, PQ H3P 1T3, Canada. [Noble, Allison; Yee, H. K. C.] Univ Toronto, Dept Astron & Astrophys, Toronto, ON M5S 3H4, Canada. [DeGroot, Andrew; Wilson, Gillian; Foltz, Ryan] Univ Calif Riverside, Dept Phys & Astron, Riverside, CA 92521 USA. [Muzzin, Adam; Chapman, Scott] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Cooper, Mike] Univ Calif Irvine, Ctr Galaxy Evolut, Dept Phys & Astron, Irvine, CA 92697 USA. [Lidman, Chris] Australian Astron Observ, N Ryde, NSW 1670, Australia. [Surace, Jason] CALTECH, Spitzer Space Sci Ctr, Pasadena, CA 91125 USA. [Chapman, Scott] Dalhousie Univ, Dept Phys & Atmospher Sci, Halifax, NS B3H 2R4, Canada. [Dunne, Loretta] Univ Canterbury, Dept Phys & Astron, Christchurch 8140, New Zealand. [Dunne, Loretta] Univ Edinburgh, Insitute Astron, Royal Observ, Edinburgh EH9 3HJ, Midlothian, Scotland. [Geach, James] Univ Hertfordshire, Sci & Technol Res Inst, Ctr Astrophys Res, Hatfield AL10 9AB, Herts, England. [Hayden, Brian; Perlmutter, Saul] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Div Phys, Berkeley, CA 94720 USA. [Hildebrandt, Hendrik; Tudorica, Alex] Argelander Inst Astron, D-53121 Bonn, Germany. [Huang, Jiasheng] Chinese Acad Sci, Natl Astron Observ China, Beijing 100012, Peoples R China. [Huang, Jiasheng] Chinese Acad Sci, China Chile Joint Ctr Astron, Santiago 1515, Chile. [Huang, Jiasheng] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Pope, Alexandra] Univ Massachusetts, Dept Astron, Amherst, MA 01100 USA. [Smith, Matthew W. L.] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales. [Perlmutter, Saul] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. RP Webb, T (reprint author), McGill Univ, Dept Phys, 3600 Rue Univ, Montreal, PQ H3P 1T3, Canada. FU W. M. Keck Foundation; NASA [NAS 5-26555]; US Department of Energy, Office of Science, Office of High Energy Physics [AC02-05CH11231]; European Research Council; NSERC; NASA from the Space Telescope Science Institute [GO-13306, GO-13677, GO-13747, GO-13845, GO-14327] FX Some of the data presented herein were obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California and the National Aeronautics and Space Administration. The Observatory was made possible by the generous financial support of the W. M. Keck Foundation. The authors 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. Financial support for this work was provided by NASA through program GO-13677 from the Space Telescope Science Institute, which is operated by AURA, Inc., under NASA contract NAS 5-26555. This material is based upon work supported in part by the US Department of Energy, Office of Science, Office of High Energy Physics, under contract No. AC02-05CH11231. 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. L.D. acknowledges support from European Research Council Advanced Grant: cosmicism. T.M.A.W. acknowledges the support of an NSERC Discovery Grant. Financial support for this work was provided by NASA through programs GO-13306, GO-13677, GO-13747, GO-13845, and GO-14327 from the Space Telescope Science Institute, which is operated by AURA, Inc., under NASA contract NAS 5-26555. NR 84 TC 11 Z9 11 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD AUG 20 PY 2015 VL 809 IS 2 AR 173 DI 10.1088/0004-637X/809/2/173 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CR9EC UT WOS:000361655100066 ER PT J AU Huang, J Ouml;berg, KI AF Huang, Jane Oeberg, Karin I. TI DETECTION OF N2D+ IN A PROTOPLANETARY DISK SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE astrochemistry; ISM: molecules; protoplanetary disks ID DEUTERIUM FRACTIONATION; MOLECULAR-SPECTROSCOPY; DEUTERATED MOLECULES; INTERSTELLAR CLOUDS; COLOGNE DATABASE; DM TAURI; CHEMISTRY; CORES; LINE; ICE AB Observations of deuterium fractionation in the solar system, and in interstellar and circumstellar material, are commonly used to constrain the formation environment of volatiles. Toward protoplanetary disks, this approach has been limited by the small number of detected deuterated molecules, i.e., DCO+ and DCN. Based on ALMA Cycle 2 observations toward the disk around the T Tauri star AS 209, we report the first detection of N2D+ (J = 3-2) in a protoplanetary disk. These data are used together with previous Submillimeter Array observations of N2H+ (J = 3-2) to estimate a disk-averaged D/H ratio of 0.3-0.5, an order of magnitude higher than disk-averaged ratios previously derived for DCN/HCN and DCO+/HCO+ around other young stars. The high fractionation in N2H+ is consistent with model predictions. The presence of abundant N2D+ toward AS 209 also suggests that N2D+ and the N2D+/N2H+ ratio can be developed into effective probes of deuterium chemistry, kinematics, and ionization processes outside the CO snow line of disks. C1 [Huang, Jane; Oeberg, Karin I.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RP Huang, J (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. FU Simons Collaboration on the Origins of Life (SCOL); Alfred P. Sloan Foundation; David and Lucile Packard Foundation FX This paper makes use of the following ALMA data: ADS/JAO.ALMA#2013.1.00226. ALMA is a partnership of ESO (representing its member states), NSF (USA) and NINS (Japan), together with NRC (Canada) and NSC and ASIAA (Taiwan), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by ESO, AUI/NRAO and NAOJ. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. We thank Adam Leroy and the NAASC for assistance with calibration and imaging, Ryan Loomis and Viviana Guzman for helpful discussions on the data, and the referee for useful comments on the paper. K.I.O. also acknowledges funding from the Simons Collaboration on the Origins of Life (SCOL), the Alfred P. Sloan Foundation, and the David and Lucile Packard Foundation. NR 39 TC 1 Z9 1 U1 2 U2 3 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 AUG 20 PY 2015 VL 809 IS 2 AR L26 DI 10.1088/2041-8205/809/2/L26 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CQ6LI UT WOS:000360715500009 ER PT J AU Loomis, RA Cleeves, LI Oberg, KI Guzman, VV Andrews, SM AF Loomis, Ryan A. Cleeves, L. Ilsedore Oeberg, Karin I. Guzman, Viviana V. Andrews, Sean M. TI THE DISTRIBUTION AND CHEMISTRY OF H2CO IN THE DM TAU PROTOPLANETARY DISK SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE astrochemistry; circumstellar matter; ISM: molecules; protoplanetary disks; radio Lines: ISM ID CO SNOW LINE; ORGANIC-MOLECULES; H-2 FLUORESCENCE; CHEMICAL-MODEL; IMAGING SURVEY; COSMIC-RAYS; TW-HYDRAE; HD 163296; LY-ALPHA; X-RAY AB H2CO ice on dust grains is an important precursor of complex organic molecules (COMs). H2CO gas can be readily observed in protoplanetary disks and may be used to trace COM chemistry. However, its utility as a COM probe is currently limited by a lack of constraints on the relative contributions of two different formation pathways: on icy grain surfaces and in the gas phase. We use archival Atacama Large (sub-) Millimeter Array observations of the resolved distribution of H2CO emission in the disk around the young low-mass star DM Tau to assess the relative importance of these formation routes. The observed H2CO emission has a centrally peaked and radially broad brightness profile (extending out to 500 AU). We compare these observations with disk chemistry models with and without grain-surface formation reactions and find that both gas and grain-surface chemistry are necessary to explain the spatial distribution of the emission. Gas-phase H2CO production is responsible for the observed central peak, while grain-surface chemistry is required to reproduce the emission exterior to the CO snow line (where H2CO mainly forms through the hydrogenation of CO ice before being non-thermally desorbed). These observations demonstrate that both gas and grain-surface pathways contribute to the observed H2CO in disks and that their relative contributions depend strongly on distance from the host star. C1 [Loomis, Ryan A.; Oeberg, Karin I.; Guzman, Viviana V.] Harvard Univ, Dept Astron, Cambridge, MA 02138 USA. [Cleeves, L. Ilsedore] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Andrews, Sean M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Loomis, RA (reprint author), Harvard Univ, Dept Astron, Cambridge, MA 02138 USA. EM rloomis@cfa.harvard.edu OI Cleeves, L. Ilsedore/0000-0003-2076-8001 FU National Science Foundation Graduate Research Fellowship; NSF grant [AST-1008800]; Rackham Predoctoral Fellowship; Simons Collaboration on the Origins of Life (SCOL); Alfred P. Sloan Foundation; David and Lucile Packard Foundation FX We thank the anonymous referee for useful comments. We thank David Wilner and Charlie Qi for productive and insightful conversations. R.A.L. gratefully acknowledges funding from an National Science Foundation Graduate Research Fellowship. L.I.C. acknowledges support by NSF grant AST-1008800 and the Rackham Predoctoral Fellowship. K.I.O. also acknowledges funding from the Simons Collaboration on the Origins of Life (SCOL), the Alfred P. Sloan Foundation, and the David and Lucile Packard Foundation. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. This paper makes use of the following ALMA data: ADS/JAO. ALMA# 2011.0.00629.S. ALMA is a partnership of ESO (representing its member states), NSF (USA) and NINS (Japan), together with NRC (Canada) and NSC and ASIAA (Taiwan), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by ESO, AUI/NRAO and NAOJ. NR 52 TC 3 Z9 3 U1 1 U2 3 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 AUG 20 PY 2015 VL 809 IS 2 AR L25 DI 10.1088/2041-8205/809/2/L25 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CQ6LI UT WOS:000360715500008 ER PT J AU Laporta, GZ Linton, YM Wilkerson, RC Bergo, ES Nagaki, SS Sant'Ana, DC Sallum, MAM AF Laporta, Gabriel Zorello Linton, Yvonne-Marie Wilkerson, Richard C. Bergo, Eduardo Sterlino Nagaki, Sandra Sayuri Sant'Ana, Denise Cristina Mureb Sallum, Maria Anice TI Malaria vectors in South America: current and future scenarios SO PARASITES & VECTORS LA English DT Article DE Anopheles darlingi; Albitarsis Complex; Climate change; Ecological niche model; Plasmodium falciparum ID NYSSORHYNCHUS ALBITARSIS DIPTERA; POLYMERASE CHAIN-REACTION; CLIMATE-CHANGE; ANOPHELES-NYSSORHYNCHUS; POTENTIAL DISTRIBUTION; PLASMODIUM-FALCIPARUM; CULICIDAE; COMPLEX; BRAZIL; TRANSMISSION AB Background: Malaria remains a significant public health issue in South America. Future climate change may influence the distribution of the disease, which is dependent on the distribution of those Anopheles mosquitoes competent to transmit Plasmodium falciparum. Herein, predictive niche models of the habitat suitability for P. falciparum, the current primary vector Anopheles darlingi and nine other known and/or potential vector species of the Neotropical Albitarsis Complex, were used to document the current situation and project future scenarios under climate changes in South America in 2070. Methods: To build each ecological niche model, we employed topography, climate and biome, and the currently defined distribution of P. falciparum, An. darlingi and nine species comprising the Albitarsis Complex in South America. Current and future (i.e., 2070) distributions were forecast by projecting the fitted ecological niche model onto the current environmental situation and two scenarios of simulated climate change. Statistical analyses were performed between the parasite and each vector in both the present and future scenarios to address potential vector roles in the dynamics of malaria transmission. Results: Current distributions of malaria vector species were associated with that of P. falciparum, confirming their role in transmission, especially An. darlingi, An. marajoara and An. deaneorum. Projected climate changes included higher temperatures, lower water availability and biome modifications. Regardless of future scenarios considered, the geographic distribution of P. falciparum was exacerbated in 2070 South America, with the distribution of the pathogen covering 35-46 % of the continent. As the current primary vector An. darlingi showed low tolerance for drier environments, the projected climate change would significantly reduce suitable habitat, impacting both its distribution and abundance. Conversely, climate generalist members of the Albitarsis Complex showed significant spatial and temporal expansion potential in 2070, and we conclude these species will become more important in the dynamics of malaria transmission in South America. Conclusions: Our data suggest that climate and landscape effects will elevate the importance of members of the Albitarsis Complex in malaria transmission in South America in 2070, highlighting the need for further studies addressing the bionomics, ecology and behaviours of the species comprising the Albitarsis Complex. C1 [Laporta, Gabriel Zorello; Nagaki, Sandra Sayuri; Sant'Ana, Denise Cristina; Mureb Sallum, Maria Anice] Univ Sao Paulo, Fac Saude Publ, Dept Epidemiol, BR-01255 Sao Paulo, SP, Brazil. [Laporta, Gabriel Zorello] Univ Sao Paulo, Fac Med, Lab Informat Med, Sao Paulo, SP, Brazil. [Laporta, Gabriel Zorello] Fac Med ABC, Setor Posgrad Pesquisa & Inovacao, Santo Andre, SP, Brazil. [Linton, Yvonne-Marie; Wilkerson, Richard C.] Walter Reed Army Inst Res, Div Entomol, Silver Spring, MD USA. [Linton, Yvonne-Marie; Wilkerson, Richard C.] Smithsonian Inst, Walter Reed Biosystemat Unit, Museum Support Ctr, Suitland, MD USA. [Linton, Yvonne-Marie; Wilkerson, Richard C.] Smithsonian Inst, Dept Entomol, Natl Museum Nat Hist, Washington, DC 20560 USA. [Linton, Yvonne-Marie] Uniformed Serv Univ Hlth Sci, Dept Preventat Med & Biostat, Bethesda, MD 20814 USA. [Bergo, Eduardo Sterlino] Secretaria Estado Saude Sao Paulo, Superintendencia Controle Endemias SUCEN, Araraquara, SP, Brazil. RP Laporta, GZ (reprint author), Univ Sao Paulo, Fac Saude Publ, Dept Epidemiol, BR-01255 Sao Paulo, SP, Brazil. EM gabrielzorelo@usp.br RI Laporta, Gabriel/B-8662-2012; Nagaki, Sandra/G-7069-2016; OI Laporta, Gabriel/0000-0001-7412-9390 FU Sao Paulo Research Foundation (FAPESP) [2014/26229-7]; Brazilian National Council for Scientific and Technological Development (CNPq) [301666/2011-3]; National Institute of Health, USA [R01 AI50139-02]; FAPESP [2014/09774-1, 2015/09669-6] FX We gratefully acknowledge financial support from the Sao Paulo Research Foundation (FAPESP, Grant no. 2014/26229-7), the Brazilian National Council for Scientific and Technological Development (CNPq, Grant no. 301666/2011-3) to MAMS; RCW was partially supported by an award from the National Institute of Health, USA (grant R01 AI50139-02 to Jan Conn). GZL is currently financially supported by FAPESP Grant no. 2014/09774-1 and FAPESP Grant no. 2015/09669-6. Funders of this study had no role in the design, collection, analysis or interpretation of the results, nor in the writing of this report or the decision to publish it. Part of this research was performed under a Memorandum of Understanding between the Walter Reed Army Institute of Research and the Smithsonian Institution, with institutional support provided by both organizations. The material to be published reflects the views of the authors and should not be construed to represent those of the US Department of the Army or the US Department of Defense. This manuscript was prepared whilst YML held a National Research Council (NRC) Senior Research Associateship Award at the Walter Reed Army Institute of Research. NR 55 TC 6 Z9 6 U1 2 U2 37 PU BIOMED CENTRAL LTD PI LONDON PA 236 GRAYS INN RD, FLOOR 6, LONDON WC1X 8HL, ENGLAND SN 1756-3305 J9 PARASITE VECTOR JI Parasites Vectors PD AUG 19 PY 2015 VL 8 AR 426 DI 10.1186/s13071-015-1038-4 PG 13 WC Parasitology SC Parasitology GA CP3DE UT WOS:000359756200003 PM 26283539 ER PT J AU McCarthy, MC Tamassia, F Thorwirth, S AF McCarthy, M. C. Tamassia, F. Thorwirth, S. TI High-resolution rotational spectroscopy of iminosilylene, HNSi SO MOLECULAR PHYSICS LA English DT Article DE vibrational excitation; quantum chemical calculations; rotational spectroscopy; molecular structure ID CORRELATED MOLECULAR CALCULATIONS; SILICON-NITROGEN CHEMISTRY; GAUSSIAN-BASIS SETS; EQUILIBRIUM STRUCTURE; HYPERFINE-STRUCTURE; 2ND DERIVATIVES; CARBON CHAINS; ATOMS; HSIN; PERTURBATION AB By means of Fourier transform microwave spectroscopy of a supersonic beam, the fundamental rotational transition of isotopic and vibrationally excited iminosilylene, HNSi, has been detected. In addition to seven isotopic species, vibrational satellite transitions from more than 30 vibrationally excited states, including the three fundamental modes, have been detected. Those from nu(2) are particularly intense, enabling detection of transitions from as high as (0,22(0),0) (i.e. similar to 10,000 cm(-1) above ground). At high spectral resolution, well-resolved nitrogen quadrupole structure has been observed in nearly every transition. Excitation of nu(1) or nu(3) changes eQq(N) little, but eQq(N) systematically decreases with increasing excitation of the nu(2) bend, from a value of 0.376(5) MHz for (0,0(0),0) to -2.257(5) MHz for (0,20(0),0). With the large amount of new data in hand, it has also been possible to determine the leading vibration-rotation constants (alpha(i) and gamma(i)) for nu(2) or nu(3) to high precision, and derive a revised semi-empirical equilibrium structure for this fundamental triatomic molecule. Various electronic and molecular properties of iminosilylene have been calculated at the coupled cluster level of theory, and these generally agree well with experiment and previous calculations. An unsuccessful search for HSiN, a highly polar isomer calculated to lie nearly 3 eV above HNSi, is also reported. C1 [McCarthy, M. C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [McCarthy, M. C.] Harvard Univ, Sch Engn & Appl Sci, Cambridge, MA 02138 USA. [Tamassia, F.] Univ Bologna, Dipartimento Chim Ind Toso Montanari, Bologna, Italy. [Thorwirth, S.] Univ Cologne, Inst Phys 1, 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 FU NSF [CHE-1058063]; Universita di Bologna; MIUR [20129ZFHFE]; Deutsche Forschungsgemeinschaft [TH 1301/3-1, TH 1301/3-2] FX The work in Cambridge is supported by NSF [grant number CHE-1058063]; F. Tamassia acknowledges the Universita di Bologna and MIUR [grant number 20129ZFHFE] (PRIN 2012 funds under the project 'STAR: Spectroscopic and computational Techniques for Astrophysical and Atmospheric Research') for financial support; S. Thorwirth gratefully acknowledges support from the Deutsche Forschungsgemeinschaft [grant number TH 1301/3-1], [grant number TH 1301/3-2]. NR 58 TC 1 Z9 1 U1 1 U2 3 PU TAYLOR & FRANCIS LTD PI ABINGDON PA 4 PARK SQUARE, MILTON PARK, ABINGDON OX14 4RN, OXON, ENGLAND SN 0026-8976 EI 1362-3028 J9 MOL PHYS JI Mol. Phys. PD AUG 18 PY 2015 VL 113 IS 15-16 SI SI BP 2204 EP 2216 DI 10.1080/00268976.2015.1019583 PG 13 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA CQ9BN UT WOS:000360906000018 ER PT J AU Koepfli, KP Pollinger, J Godinho, R Robinson, J Lea, A Hendricks, S Schweizer, RM Thalmann, O Silva, P Fan, ZX Yurchenko, AA Dobrynin, P Makunin, A Cahill, JA Shapiro, B Alvares, F Brito, JC Geffen, E Leonard, JA Helgen, KM Johnson, WE O'Brien, SJ Van Valkenburgh, B Wayne, RK AF Koepfli, Klaus-Peter Pollinger, John Godinho, Raquel Robinson, Jacqueline Lea, Amanda Hendricks, Sarah Schweizer, Rena M. Thalmann, Olaf Silva, Pedro Fan, Zhenxin Yurchenko, Andrey A. Dobrynin, Pavel Makunin, Alexey Cahill, James A. Shapiro, Beth Alvares, Francisco Brito, Jose C. Geffen, Eli Leonard, Jennifer A. Helgen, Kristofer M. Johnson, Warren E. O'Brien, Stephen J. Van Valkenburgh, Blaire Wayne, Robert K. TI Genome-wide Evidence Reveals that African and Eurasian Golden Jackals Are Distinct Species SO CURRENT BIOLOGY LA English DT Article ID NEOFELIS-NEBULOSA; CLOUDED LEOPARD; CLIMATE-CHANGE; EVOLUTION; CARNIVORA; CANIDS; DIVERGENCE; DELIMITATION; SEQUENCE; MAMMALIA AB The golden jackal of Africa (Canis aureus) has long been considered a conspecific of jackals distributed throughout Eurasia, with the nearest source populations in the Middle East. However, two recent reports found that mitochondrial haplotypes of some African golden jackals aligned more closely to gray wolves (Canis lupus) [1,2], which is surprising given the absence of gray wolves in Africa and the phenotypic divergence between the two species. Moreover, these results imply the existence of a previously unrecognized phylogenetically distinct species despite a long history of taxonomic work on African canids. To test the distinct-species hypothesis and understand the evolutionary history that would account for this puzzling result, we analyzed extensive genomic data including mitochondrial genome sequences, sequences from 20 autosomal loci (17 introns and 3 exon segments), microsatellite loci, X- and Y-linked zinc-finger protein gene (ZFX and ZFY) sequences, and whole-genome nuclear sequences in African and Eurasian golden jackals and gray wolves. Our results provide consistent and robust evidence that populations of golden jackals from Africa and Eurasia represent distinct monophyletic lineages separated for more than one million years, sufficient to merit formal recognition as different species: C. anthus (African golden wolf) and C. aureus (Eurasian golden jackal). Using morphologic data, we demonstrate a striking morphologic similarity between East African and Eurasian golden jackals, suggesting parallelism, which may have misled taxonomists and likely reflects uniquely intense interspecific competition in the East African carnivore guild. Our study shows how ecology can confound taxonomy if interspecific competition constrains size diversification. C1 [Koepfli, Klaus-Peter] Smithsonian Conservat Biol Inst, Natl Zool Pk, Washington, DC 20008 USA. [Koepfli, Klaus-Peter; Yurchenko, Andrey A.; Dobrynin, Pavel; Makunin, Alexey; O'Brien, Stephen J.] St Petersburg State Univ, Theodosius Dobzhansky Ctr Genome Bioinformat, St Petersburg 199034, Russia. [Pollinger, John; Robinson, Jacqueline; Schweizer, Rena M.; Van Valkenburgh, Blaire; Wayne, Robert K.] Univ Calif Los Angeles, Dept Ecol & Evolutionary Biol, Los Angeles, CA 90095 USA. [Godinho, Raquel; Silva, Pedro; Alvares, Francisco; Brito, Jose C.] Univ Porto, CIBIO InBIO Ctr Invest Biodiversidade & Recursos, P-4485661 Vairao, Portugal. [Godinho, Raquel; Silva, Pedro; Alvares, Francisco; Brito, Jose C.] Univ Porto, Fac Ciencias, Dept Biol, P-4169007 Oporto, Portugal. [Godinho, Raquel] Univ Johannesburg, Dept Zool, ZA-2006 Auckland Pk, South Africa. [Lea, Amanda] Duke Univ, Dept Biol, Durham, NC 27708 USA. [Hendricks, Sarah] Univ Idaho, Dept Biol Sci, Inst Bioinformat & Evolutionary Studies, Moscow, ID 83844 USA. [Thalmann, Olaf] Univ Turku, Div Genet & Physiol, Dept Biol Sci, Turku 20014, Finland. [Thalmann, Olaf] Univ Oulu, Dept Biol, Oulu 90014, Finland. [Fan, Zhenxin] Sichuan Univ, Coll Life Sci, Sichuan Key Lab Conservat Biol Endangered Wildlif, Chengdu 610064, Peoples R China. [Cahill, James A.; Shapiro, Beth] Univ Calif Santa Cruz, Dept Ecol & Evolutionary Biol, Santa Cruz, CA 95064 USA. [Geffen, Eli] Tel Aviv Univ, Dept Zool, IL-69978 Tel Aviv, Israel. [Leonard, Jennifer A.] Conservat & Evolutionary Genet Grp EBD CSIC, Estn Biol Donana, Seville 41092, Spain. [Helgen, Kristofer M.] Smithsonian Inst, Natl Museum Amer Hist, Div Mammals, Washington, DC 20013 USA. [Johnson, Warren E.] Smithsonian Conservat Biol Inst, Natl Zool Pk, Front Royal, VA 22630 USA. [O'Brien, Stephen J.] Nova SE Univ, Oceanog Ctr, Dania, FL 33004 USA. RP Koepfli, KP (reprint author), Smithsonian Conservat Biol Inst, Natl Zool Pk, 3001 Connecticut Ave NW, Washington, DC 20008 USA. EM koepflik@si.edu; rwayne@ucla.edu RI Makunin, Alexey/N-2055-2015; Yurchenko, Andrey/N-2698-2015; Brito, Jose/A-7831-2010; CSIC, EBD Donana/C-4157-2011; Leonard, Jennifer/A-7894-2010; OI Makunin, Alexey/0000-0002-9555-5097; Yurchenko, Andrey/0000-0002-2239-6902; Brito, Jose/0000-0001-5444-8132; CSIC, EBD Donana/0000-0003-4318-6602; Leonard, Jennifer/0000-0003-0291-7819; Alvares, Francisco/0000-0002-4033-6989; Shapiro, Beth/0000-0002-2733-7776 FU Russian Ministry of Science Mega-grant [11.G34.31.0068]; FCT [IF/00564/2012, IF/00459/2013]; National Geographic Society [CRE 7629-04, CRE 8412-08]; CIBIO; Project "Genomics Applied to Genetic Resources"; North Portugal Regional Operational Programme (ON.2 - O Novo Norte), under the National Strategic Reference Framework, through the European Regional Development Fund; National Science Foundation Graduate Research Fellowship; Marie Curie Intra-European Fellowship within the 7th European Community Framework Program FX K.-P.K., A.A.Y., P.D., A.M., and S.J.O. were supported by Russian Ministry of Science Mega-grant 11.G34.31.0068. R.G. and J.C.B. were supported by FCT contracts (IF/00564/2012 and IF/00459/2013, respectively). Fieldwork of J.C.B. and F.A. in North Africa was supported by the National Geographic Society (CRE 7629-04 and CRE 8412-08) and CIBIO, respectively. Microsatellite lab work was partially funded by Project "Genomics Applied to Genetic Resources" cofinanced by North Portugal Regional Operational Programme 2007/2013 (ON.2 - O Novo Norte), under the National Strategic Reference Framework, through the European Regional Development Fund. R.M.S. was supported by a National Science Foundation Graduate Research Fellowship. O.T. is financed by a Marie Curie Intra-European Fellowship within the 7th European Community Framework Program and is grateful to M. Webster. We thank the Tel Aviv University Zoological Museum for providing samples of golden jackals and gray wolves used in this study. We gratefully acknowledge Frank Zachos (Naturhistorisches Museum Wien) for providing samples of golden jackals from Serbia and for constructive comments on the manuscript. We also thank N. Ferrand for helpful comments on the manuscript. We thank Michael Campana (Smithsonian Conservation Biology Institute) for conducting additional phylogenetic analyses on the mitochondrial genome dataset. We are grateful to Pauline Charruau-Dau and rev.com for providing translations of Frederic Cuvier's description of Canis anthus. We also thank D. Gordon E. Robertson for permission to use the photograph of a golden jackal from Serengeti National Park, Tanzania, for the graphical abstract. Finally, we thank four anonymous reviewers for providing excellent comments that improved the manuscript. NR 29 TC 15 Z9 15 U1 3 U2 36 PU CELL PRESS PI CAMBRIDGE PA 600 TECHNOLOGY SQUARE, 5TH FLOOR, CAMBRIDGE, MA 02139 USA SN 0960-9822 EI 1879-0445 J9 CURR BIOL JI Curr. Biol. PD AUG 17 PY 2015 VL 25 IS 16 BP 2158 EP 2165 DI 10.1016/j.cub.2015.06.060 PG 8 WC Biochemistry & Molecular Biology; Cell Biology SC Biochemistry & Molecular Biology; Cell Biology GA CP4WB UT WOS:000359882200028 PM 26234211 ER PT J AU Farine, DR Spencer, KA Boogert, NJ AF Farine, Damien R. Spencer, Karen A. Boogert, Neeltje J. TI Early-Life Stress Triggers Juvenile Zebra Finches to Switch Social Learning Strategies SO CURRENT BIOLOGY LA English DT Article ID DIFFUSION ANALYSIS; NETWORK STRUCTURE; SELECTION; INNOVATIONS; PERSPECTIVE; PERFORMANCE; CONFORMITY; PLASTICITY; STARLINGS; DYNAMICS AB Stress during early life can cause disease and cognitive impairment in humans and non-humans alike [1]. However, stress and other environmental factors can also program developmental pathways [2, 3]. We investigate whether differential exposure to developmental stress can drive divergent social learning strategies [4, 5] between siblings. In many species, juveniles acquire essential foraging skills by copying others: they can copy peers (horizontal social learning), learn from their parents (vertical social learning), or learn from other adults (oblique social learning) [6]. However, whether juveniles' learning strategies are condition dependent largely remains a mystery. We found that juvenile zebra finches living in flocks socially learned novel foraging skills exclusively from adults. By experimentally manipulating developmental stress, we further show that social learning targets are phenotypically plastic. While control juveniles learned foraging skills from their parents, their siblings, exposed as nestlings to experimentally elevated stress hormone levels, learned exclusively from unrelated adults. Thus, early-life conditions triggered individuals to switch strategies from vertical to oblique social learning. This switch could arise from stress-induced differences in developmental rate, cognitive and physical state, or the use of stress as an environmental cue. Acquisition of alternative social learning strategies may impact juveniles' fit to their environment and ultimately change their developmental trajectories. C1 [Farine, Damien R.] Univ Oxford, Dept Zool, Edward Grey Inst Field Ornithol, Oxford OX1 3PS, England. [Farine, Damien R.] Univ Calif Davis, Dept Anthropol, Davis, CA 95616 USA. [Farine, Damien R.] Smithsonian Trop Res Inst, Panama City 084303092, Panama. [Spencer, Karen A.; Boogert, Neeltje J.] Univ St Andrews, Sch Psychol & Neurosci, St Andrews KY16 9JP, Fife, Scotland. [Boogert, Neeltje J.] Univ Cambridge, Dept Zool, Cambridge CB2 3EJ, England. RP Farine, DR (reprint author), Univ Oxford, Dept Zool, Edward Grey Inst Field Ornithol, S Parks Rd, Oxford OX1 3PS, England. EM damien.farine@zoo.ox.ac.uk FU NSF [NSF-IOS1250895]; BBSRC [BB/L006081/1]; BBSRC David Phillips Research Fellowship; Netherlands Organization for Scientific Research (NWO) FX We thank Ben Sheldon, Kevin Laland, Will Hoppitt, Lucy Aplin, Bram Kuijper, and Willem Frankenhuis for their constructive feedback, James Sturdy for his help scoring the videos, and Roland Stump for his help setting up the PIT/RFID system. D.R.F. was funded by grants from the NSF (NSF-IOS1250895) to Margaret Crofoot and BBSRC (BB/L006081/1) to Ben Sheldon, K.A.S. was funded by a BBSRC David Phillips Research Fellowship, and N.J.B. was funded by a Netherlands Organization for Scientific Research (NWO) Rubicon grant. NR 40 TC 10 Z9 10 U1 8 U2 43 PU CELL PRESS PI CAMBRIDGE PA 600 TECHNOLOGY SQUARE, 5TH FLOOR, CAMBRIDGE, MA 02139 USA SN 0960-9822 EI 1879-0445 J9 CURR BIOL JI Curr. Biol. PD AUG 17 PY 2015 VL 25 IS 16 BP 2184 EP 2188 DI 10.1016/j.cub.2015.06.071 PG 5 WC Biochemistry & Molecular Biology; Cell Biology SC Biochemistry & Molecular Biology; Cell Biology GA CP4WB UT WOS:000359882200032 PM 26212879 ER PT J AU Bastin, JF Barbier, N Rejou-Mechain, M Fayolle, A Gourlet-Fleury, S Maniatis, D de Haulleville, T Baya, F Beeckman, H Beina, D Couteron, P Chuyong, G Dauby, G Doucet, JL Droissart, V Dufrene, M Ewango, C Gillet, JF Gonmadje, CH Hart, T Kavali, T Kenfack, D Libalah, M Malhi, Y Makana, JR Pelissier, R Ploton, P Serckx, A Sonke, B Stevart, T Thomas, DW De Canniere, C Bogaert, J AF Bastin, J. -F. Barbier, N. Rejou-Mechain, M. Fayolle, A. Gourlet-Fleury, S. Maniatis, D. de Haulleville, T. Baya, F. Beeckman, H. Beina, D. Couteron, P. Chuyong, G. Dauby, G. Doucet, J. -L. Droissart, V. Dufrene, M. Ewango, C. Gillet, J. F. Gonmadje, C. H. Hart, T. Kavali, T. Kenfack, D. Libalah, M. Malhi, Y. Makana, J. -R. Pelissier, R. Ploton, P. Serckx, A. Sonke, B. Stevart, T. Thomas, D. W. De Canniere, C. Bogaert, J. TI Seeing Central African forests through their largest trees SO SCIENTIFIC REPORTS LA English DT Article ID TROPICAL FOREST; BIOMASS; SIZE; DISTRIBUTIONS; DIVERSITY AB Large tropical trees and a few dominant species were recently identified as the main structuring elements of tropical forests. However, such result did not translate yet into quantitative approaches which are essential to understand, predict and monitor forest functions and composition over large, often poorly accessible territories. Here we show that the above-ground biomass (AGB) of the whole forest can be predicted from a few large trees and that the relationship is proved strikingly stable in 175 1-ha plots investigated across 8 sites spanning Central Africa. We designed a generic model predicting AGB with an error of 14% when based on only 5% of the stems, which points to universality in forest structural properties. For the first time in Africa, we identified some dominant species that disproportionally contribute to forest AGB with 1.5% of recorded species accounting for over 50% of the stock of AGB. Consequently, focusing on large trees and dominant species provides precise information on the whole forest stand. This offers new perspectives for understanding the functioning of tropical forests and opens new doors for the development of innovative monitoring strategies. C1 [Bastin, J. -F.; De Canniere, C.] Univ Libre Bruxelles, Landscape Ecol & Plant Prod Syst Unit, B-1050 Brussels, Belgium. [Bastin, J. -F.; Fayolle, A.; de Haulleville, T.; Doucet, J. -L.; Dufrene, M.; Gillet, J. F.; Bogaert, J.] Univ Liege, Gembloux Agrobio Tech, BIOSE Dept, B-5030 Gembloux, Belgium. [Bastin, J. -F.; Serckx, A.] Ecole Reg Post Univ Amenagement & Gest Integres, Forets & Terr Tropicaux, Kinshasa, Zaire. [Barbier, N.; Rejou-Mechain, M.; Couteron, P.; Droissart, V.; Libalah, M.; Pelissier, R.; Ploton, P.] IRD, UMR AMAP, F-34000 Montpellier, France. [Rejou-Mechain, M.; Gourlet-Fleury, S.; Gonmadje, C. H.] Campus Int Baillarguet, CIRAD, UPR BSEF, F-34398 Montpellier, France. [Maniatis, D.; Malhi, Y.] Univ Oxford, Sch Geog & Environm, Environm Change Inst, Oxford, England. [de Haulleville, T.; Beeckman, H.] Royal Museum Cent Africa, Lab Wood Biol & Xylarium, Tervuren, Belgium. [Baya, F.] Minist Eaux Forets Chasse & Peche, Bangui, Cent Afr Republ. [Beina, D.] Univ Bangui Cerphameta, Bangui, Cent Afr Republ. [Chuyong, G.] Univ Buea, Dept Anim & Plant Sci, Buea, Cameroon. [Dauby, G.] Univ Libre Bruxelles, Fac Sci, Lab Evolut Biol & Ecol, Brussels, Belgium. [Ewango, C.; Makana, J. -R.] Wildlife Conservat Soc, CEFRECOF, Kinshasa, Zaire. [Gonmadje, C. H.] Natl Herbarium, Yaounde, Cameroon. [Gonmadje, C. H.] CIFOR, Cent African Reg Off, Yaounde 2008, Cameroon. [Hart, T.] Lukuru Wildlife Res Fdn, Kinshasa, Gombe, Zaire. [Kavali, T.] Wildlife Conservat Soc, DRC Program, Kinshasa, Zaire. [Kenfack, D.] Smithsonian Inst, Dept Bot, MRC 166, CTFS ForestGEO, Washington, DC 20013 USA. [Serckx, A.] Univ Liege, Behav Biol Unit, Liege, Belgium. [Serckx, A.] Royal Belgian Inst Nat Sci, Conservat Biol Unit, Brussels, Belgium. [Serckx, A.] Max Planck Inst Evolutionary Anthropol, Dept Primatol, Leipzig, Germany. [Libalah, M.; Sonke, B.] Univ Yaounde, Dept Biol, Plant Systemat & Ecol Lab, Yaounde 1, Cameroon. [Stevart, T.] Africa & Madagascar Dept, Missouri Bot Garden, St Louis, MO USA. [Thomas, D. W.] Oregon State Univ, Dept Bot & Plant Pathol, Corvallis, OR 97331 USA. RP Bastin, JF (reprint author), Univ Libre Bruxelles, Landscape Ecol & Plant Prod Syst Unit, CP264-2, B-1050 Brussels, Belgium. EM bastin.jf@gmail.com RI Barbier, Nicolas/A-5489-2010; Pelissier, Raphael/C-1224-2008 OI Barbier, Nicolas/0000-0002-5323-3866; Pelissier, Raphael/0000-0003-4845-5090 FU FRIA (FNRS); ERAIFT (WBI); WWF; CoForTips project [ANR-12-EBID-0002]; COBIMFO project (Congo Basin integrated monitoring for forest carbon mitigation and biodiversity) - Belgian Science Policy Office (Belspo); French Foreign Affairs; CIRAD; SCAC FX J.-F.B. and A. S. were supported by the FRIA (FNRS), ERAIFT (WBI) and WWF; M. R.-M. was supported by the CoForTips project (ANR-12-EBID-0002); T. d. H. was supported by the COBIMFO project (Congo Basin integrated monitoring for forest carbon mitigation and biodiversity) funded by the Belgian Science Policy Office (Belspo); C. H. G was supported by the "Sud Expert Plantes" project of French Foreign Affairs, CIRAD and SCAC. We thank the ARF Project (Appui a la Recherche Forestiere) in CAR for providing access to the M'Baiki site and to the database. We also would like to thank Dr. Valery Gond, for providing and sharing the map used in Fig. 1. NR 30 TC 21 Z9 21 U1 3 U2 18 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 AUG 17 PY 2015 VL 5 AR 13156 DI 10.1038/srep13156 PG 8 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA CO9YA UT WOS:000359531500002 PM 26279193 ER PT J AU van den Doel, PB Prieto, VR van Rossum-Fikkert, SE Schaftenaar, W Latimer, E Howard, L Chapman, S Masters, N Osterhaus, ADME Ling, PD Dastjerdi, A Martina, B AF van den Doel, Petra B. Rodriguez Prieto, Victor van Rossum-Fikkert, Sarah E. Schaftenaar, Willem Latimer, Erin Howard, Lauren Chapman, Sarah Masters, Nic Osterhaus, Albert D. M. E. Ling, Paul D. Dastjerdi, Akbar Martina, Byron TI A novel antigen capture ELISA for the specific detection of IgG antibodies to elephant endotheliotropic herpes virus SO BMC VETERINARY RESEARCH LA English DT Article DE EEHV; Asian elephant; Glycoprotein B; ELISA; Seroprevalence ID ASIAN ELEPHANTS; SEROLOGICAL EVIDENCE; AFRICAN ELEPHANTS; GLYCOPROTEIN-B; SIMPLEX-VIRUS; MAXIMUS; INFECTION AB Background: Elephants are classified as critically endangered animals by the International Union for Conservation of Species (IUCN). Elephant endotheliotropic herpesvirus (EEHV) poses a large threat to breeding programs of captive Asian elephants by causing fatal haemorrhagic disease. EEHV infection is detected by PCR in samples from both clinically ill and asymptomatic elephants with an active infection, whereas latent carriers can be distinguished exclusively via serological assays. To date, identification of latent carriers has been challenging, since there are no serological assays capable of detecting seropositive elephants. Results: Here we describe a novel ELISA that specifically detects EEHV antibodies circulating in Asian elephant plasma/serum. Approximately 80 % of PCR positive elephants display EEHV-specific antibodies. Monitoring three Asian elephant herds from European zoos revealed that the serostatus of elephants within a herd varied from non-detectable to high titers. The antibody titers showed typical herpes-like rise-and-fall patterns in time which occur in all seropositive animals in the herd more or less simultaneously. Conclusions: This study shows that the developed ELISA is suitable to detect antibodies specific to EEHV. It allows study of EEHV seroprevalence in Asian elephants. Results confirm that EEHV prevalence among Asian elephants (whether captive-born or wild-caught) is high. C1 [van den Doel, Petra B.; Osterhaus, Albert D. M. E.; Martina, Byron] Erasmus MC, Erasmus Med Ctr, ViroSci Lab, NL-3015 GE Rotterdam, Netherlands. [Osterhaus, Albert D. M. E.; Martina, Byron] Artemis One Hlth Res Inst, Utrecht, Netherlands. [Rodriguez Prieto, Victor] Univ Complutense Madrid, Dept Anim Hlth, VISAVET Ctr, Madrid, Spain. [van Rossum-Fikkert, Sarah E.] Erasmus MC, Dept Genet, Rotterdam, Netherlands. [Schaftenaar, Willem] Rotterdam Zoo, Vet Serv, Rotterdam, Netherlands. [Latimer, Erin] Smithsonians Natl Zoo, Smithsonian Conservat Biol Inst, Washington, DC USA. [Howard, Lauren] Houston Zoo Inc, Dept Anim Hlth, Houston, TX USA. [Chapman, Sarah] Twycross Zoo, East Midland Zool Soc, Atherstone, Warwick, England. [Masters, Nic] Zool Soc London, Vet Serv, London, England. [Ling, Paul D.] Baylors Coll Med, Dept Mol Virol & Microbiol, Houston, TX USA. [Dastjerdi, Akbar] Anim & Plant Hlth Agcy, Addlestone, Surrey, England. RP Martina, B (reprint author), Erasmus MC, Erasmus Med Ctr, ViroSci Lab, Room Ee1714,Dr Molewaterpl 50, NL-3015 GE Rotterdam, Netherlands. EM b.martina@erasmusmc.nl RI APHA, Staff publications/E-6082-2010; Dastjerdi, Akbar/E-1803-2011; Account for bibliometric studies, IT VISAVET/C-3115-2014 OI Account for bibliometric studies, IT VISAVET/0000-0003-3319-0050 FU Zoological Society of London FX Zoological Society of London NR 29 TC 1 Z9 1 U1 2 U2 16 PU BIOMED CENTRAL LTD PI LONDON PA 236 GRAYS INN RD, FLOOR 6, LONDON WC1X 8HL, ENGLAND SN 1746-6148 J9 BMC VET RES JI BMC Vet. Res. PD AUG 14 PY 2015 VL 11 AR 203 DI 10.1186/s12917-015-0522-6 PG 10 WC Veterinary Sciences SC Veterinary Sciences GA CO9BH UT WOS:000359466500001 PM 26268467 ER PT J AU Caldwell, RL Ross, R Rodaniche, A Huffard, CL AF Caldwell, Roy L. Ross, Richard Rodaniche, Arcadio Huffard, Christine L. TI Behavior and Body Patterns of the Larger Pacific Striped Octopus SO PLOS ONE LA English DT Article ID ABDOPUS-ACULEATUS DORBIGNY; WUNDERPUS-PHOTOGENICUS; VULCANOCTOPUS-HYDROTHERMALIS; CEPHALOPODA OCTOPODIDAE; MATING-BEHAVIOR; CYANEA GRAY; N.-GEN.; VULGARIS; WILD; CUTTLEFISH AB Over thirty years ago anecdotal accounts of the undescribed Larger Pacific Striped Octopus suggested behaviors previously unknown for octopuses. Beak-to-beak mating, dens shared by mating pairs, inking during mating and extended spawning were mentioned in publications, and enticed generations of cephalopod biologists. In 2012-2014 we were able to obtain several live specimens of this species, which remains without a formal description. All of the unique behaviors listed above were observed for animals in aquaria and are discussed here. We describe the behavior, body color patterns, and postures of 24 adults maintained in captivity. Chromatophore patterns of hatchlings are also shown. C1 [Caldwell, Roy L.] Univ Calif Berkeley, Dept Integrat Biol, Berkeley, CA 94720 USA. [Caldwell, Roy L.; Ross, Richard; Huffard, Christine L.] Calif Acad Sci, San Francisco, CA 94118 USA. [Rodaniche, Arcadio] Smithsonian Trop Res Inst, Panama City, Panama. [Huffard, Christine L.] Monterey Bay Aquarium Res Inst, Moss Landing, CA USA. RP Caldwell, RL (reprint author), Univ Calif Berkeley, Dept Integrat Biol, Berkeley, CA 94720 USA. EM rlcaldwell@berkeley.edu FU University of California Museum of Paleontology FX Funding was provided to RLC by the University of California Museum of Paleontology. This funding group had no influence on the authors' study design, interpretation, or communication. NR 60 TC 6 Z9 6 U1 20 U2 66 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 AUG 12 PY 2015 VL 10 IS 8 AR e0134152 DI 10.1371/journal.pone.0134152 PG 17 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA CO9JT UT WOS:000359492300033 PM 26266543 ER PT J AU Kelehear, C Jones, HI Wood, BA Shine, R AF Kelehear, Crystal Jones, Hugh I. Wood, Benjamin A. Shine, Richard TI Wild Cane Toads (Rhinella marina) Expel Foreign Matter from the Coelom via the Urinary Bladder in Response to Internal Injury, Endoparasites and Disease SO PLOS ONE LA English DT Article ID IMPLANTED DUMMY TRANSMITTERS; BUFO-MARINUS; RHABDIAS-PSEUDOSPHAEROCEPHALA; TRANSINTESTINAL EXPULSION; TROPICAL AUSTRALIA; FROGS; BUFONIDAE; DYNAMICS; ANURA; ACANTHOCEPHALA AB Dissections of > 1,200 wild-caught cane toads (Rhinella marina) in tropical Australia confirm a laboratory report that anurans can expel foreign objects from the coelom by incorporating them into the urinary bladder. The foreign objects that we found inside bladders included a diverse array of items (e.g., grass seeds, twigs, insect prey, parasites), many of which may have entered the coelom via rupture of the gut wall. In some cases, the urinary bladder was fused to other organs including liver, fat bodies, ovaries, Bidder's organs, lungs, mesentery, stomach wall, gall bladder, and the abdominal wall. Acanthocephalan parasites (of a range of developmental stages) were identified from the walls of the urinary bladders of three cane toads. This organ may play a significant role in destroying or excreting metazoan parasites, as well as inanimate objects. C1 [Kelehear, Crystal; Shine, Richard] Univ Sydney, Sch Biol Sci, Camperdown, NSW, Australia. [Jones, Hugh I.] Univ Western Australia, Sch Pathol & Lab Med, Crawley, WA, Australia. [Wood, Benjamin A.] Queen Elizabeth Med Ctr, PathWest Lab Med, Nedlands, WA, Australia. RP Kelehear, C (reprint author), Smithsonian Trop Res Inst, Panama City, Panama. EM crystal.kelehear@hotmail.com FU Australian Research Council [FL120100074] FX This work was supported by Australian Research Council (http://www.arc.gov.au) Grant FL120100074 to RS. The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 29 TC 0 Z9 0 U1 3 U2 9 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 AUG 12 PY 2015 VL 10 IS 8 AR e0134036 DI 10.1371/journal.pone.0134036 PG 9 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA CO9JT UT WOS:000359492300031 PM 26267862 ER PT J AU Wappler, T Guilbert, E Labandeira, CC Hornschemeyer, T Wedmann, S AF Wappler, Torsten Guilbert, Eric Labandeira, Conrad C. Hoernschemeyer, Thomas Wedmann, Sonja TI Morphological and Behavioral Convergence in Extinct and Extant Bugs: The Systematics and Biology of a New Unusual Fossil Lace Bug from the Eocene SO PLOS ONE LA English DT Article ID GREEN RIVER FORMATION; HEMIPTERA HETEROPTERA; AMBER HEMIPTERA; SP N.; TINGIDAE; CANTACADERINAE; GENUS; COLORADO; USA; RECONSTRUCTION AB The bug Gyaclavator kohlsi Wappler, Guilbert, Wedmann et Labandeira, gen. et sp. nov., represents a new extinct genus of lace bugs (Insecta: Heteroptera: Tingidae) occurring in latest early Eocene deposits of the Green River Formation, from the southern Piceance Basin of Northwestern Colorado, in North America. Gyaclavator can be placed within the Tingidae with certainty, perhaps it is sistergroup to Cantacaderinae. If it belongs to Cantacaderinae, it is the first fossil record of this group for North America. Gyaclavator has unique, conspicuous antennae bearing a specialized, highly dilated distiflagellomere, likely important for intra-or intersex reproductive competition and attraction. This character parallels similar antennae in leaf-footed bugs (Coreidae), and probably is associated with a behavioral convergence as well. C1 [Wappler, Torsten; Wedmann, Sonja] Forschungsstn Grube Messel, Senckenberg Forschungsinst, Messel, Germany. [Wappler, Torsten; Wedmann, Sonja] Forschungsstn Grube Messel, Nat Museum Frankfurt, Messel, Germany. [Wappler, Torsten; Wedmann, Sonja] Senckenberg Biodiversitat & Klima Forschungszentr, Frankfurt, Germany. [Wappler, Torsten] Univ Bonn, Steinmann Inst Geol, Mineral, Palaontol, Bonn, Germany. [Guilbert, Eric] Museum Natl Hist Nat, CNRS, UMR 7205, Dept Systemat & Evolut, Paris, France. [Labandeira, Conrad C.] Smithsonian Inst, Dept Paleobiol, Natl Museum Nat Hist, Washington, DC 20560 USA. [Labandeira, Conrad C.] Univ Maryland, Dept Entomol & Behav, Ecol Evolut & Systemat Program, College Pk, MD 20742 USA. [Labandeira, Conrad C.] Capital Normal Univ, Coll Life Sci, Beijing, Peoples R China. [Hoernschemeyer, Thomas] Univ Gottingen, Johann Friedrich Blumenbach Inst Zool & Anthropol, Abt Morphol & Systemat, Zool Museum, D-37073 Gottingen, Germany. RP Wappler, T (reprint author), Forschungsstn Grube Messel, Senckenberg Forschungsinst, Messel, Germany. EM twappler@uni-bonn.de; sonja.wedmann@senckenberg.de RI Wappler, Torsten/D-4287-2011; OI Wappler, Torsten/0000-0003-1592-0988; Wedmann, Sonja/0000-0002-9778-4125; Hornschemeyer, Thomas/0000-0002-4924-5389 FU Deutsche Forschungsgemeinschaft (DFG) [WE 2942/6-1, WE 2942/6-2, HO 2306/6-1, HO 2306/6-2]; Hesse's Ministry of Higher Education, Research, and the Arts FX This research was possible thanks to grants of the Deutsche Forschungsgemeinschaft (DFG, grant no WE 2942/6-1 to S. W., grant no WE 2942/6-2 to S. W. and T. W., and grant no HO 2306/6-1 6-2 to T. H.) (www.dfg.de) and by the research funding programme "LOEWE-Landes-Offensive zur Entwicklung Wissenschaftlich-okonomischer Exzellenz" of Hesse's Ministry of Higher Education, Research, and the Arts. (https://wissenschaft.hessen.de/). The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 76 TC 3 Z9 4 U1 2 U2 12 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 AUG 12 PY 2015 VL 10 IS 8 AR e0133330 DI 10.1371/journal.pone.0133330 PG 17 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA CO9JT UT WOS:000359492300014 PM 26267108 ER PT J AU Zhou, G Bayliss, D Hartman, JD Rabus, M Bakos, GA Jordan, A Brahm, R Penev, K Csubry, Z Mancini, L Espinoza, N de Val-Borro, M Bhatti, W Ciceri, S Henning, T Schmidt, B Murphy, SJ Butler, RP Arriagada, P Shectman, S Crane, J Thompson, I Suc, V Noyes, RW AF Zhou, G. Bayliss, D. Hartman, J. D. Rabus, M. Bakos, G. A. Jordan, A. Brahm, R. Penev, K. Csubry, Z. Mancini, L. Espinoza, N. de Val-Borro, M. Bhatti, W. Ciceri, S. Henning, T. Schmidt, B. Murphy, S. J. Butler, R. P. Arriagada, P. Shectman, S. Crane, J. Thompson, I. Suc, V. Noyes, R. W. TI A 0.24+0.18 M-circle dot double-lined eclipsing binary from the HATSouth survey SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE binaries: eclipsing; stars: individual: HATS551-027 ID LOW-MASS STARS; MAIN-SEQUENCE STARS; CM-DRACONIS; M-DWARFS; HOT JUPITER; FUNDAMENTAL PROPERTIES; ABSOLUTE DIMENSIONS; EVOLUTIONARY MODELS; CIRCUMBINARY PLANET; RADIUS RELATION AB We report the discovery and characterization of a new M-dwarf binary, with component masses and radii of M-1 = 0.244(-0.003)(+0.003) M-circle dot, R-1 = 0.261(-0.009)(+0.006) R-circle dot, M-2 = 0.179(-0.001)(+0.002) M-circle dot, R-2 = 0.218(-0.011)(+0.007) R-circle dot, and orbital period of similar to 4.1 d. The M-dwarf binary HATS551-027 (LP 837-20) was identified as an eclipsing binary by the HATSouth survey, and characterized by a series of high-precision photometric observations of the eclipse events, and spectroscopic determinations of the atmospheric parameters and radial velocity orbits. HATS551-027 is one of few systems with both stellar components lying in the fully convective regime of very low mass stars, and can serve as a test for stellar interior models. The radius of HATS551-027A is consistent with models to 1 sigma, whilst HATS551-027B is inflated by 9 per cent at 2s significance. We measure the effective temperatures for the two stellar components to be T-eff,T- (1) = 3190 +/- 100 K and T-eff, (2) = 2990 +/- 110 K; both are slightly cooler than theoretical models predict, but consistent with other M-dwarfs of similar masses that have previously been studied. We also measure significant Ha emission from both components of the binary system, and discuss this in the context of the correlation between stellar activity and the discrepancies between the observed and model temperatures. C1 [Zhou, G.; Bayliss, D.; Schmidt, B.] Australian Natl Univ, Res Sch Astron & Astrophys, Canberra, ACT 2611, Australia. [Hartman, J. D.; Bakos, G. A.; Penev, K.; Csubry, Z.; de Val-Borro, M.; Bhatti, W.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. [Rabus, M.; Jordan, A.; Brahm, R.; Espinoza, N.; Suc, V.] Pontificia Univ Catolica Chile, Inst Astrofis, Santiago 7820436, Chile. [Mancini, L.; Ciceri, S.; Henning, T.] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Murphy, S. J.] Heidelberg Univ, Zentrum Astron, Astron Rech Inst, D-69120 Heidelberg, Germany. [Butler, R. P.; Arriagada, P.] Carnegie Inst Sci, Dept Terr Magnetism, Washington, DC 20015 USA. [Shectman, S.; Crane, J.; Thompson, I.] Observ Carnegie Inst Washington, Pasadena, CA 91101 USA. [Noyes, R. W.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Zhou, G (reprint author), Australian Natl Univ, Res Sch Astron & Astrophys, Canberra, ACT 2611, Australia. EM george.zhou@anu.edu.au OI Jordan, Andres/0000-0002-5389-3944 FU NSF MRI grant [NSF/AST-0723074]; NASA [NNX12AH91H, NNX13AQ62G]; ARC Laureate Fellowship [FL0992131]; Millennium Science Initiative, Chilean Ministry of Economy [IC120009]; FONDECYT [1130857]; BASAL CATA [PFB-06]; CONICYT-PCHA/Doctorado Nacional; La Silla Observatory [P087.A-9014(A), P088.A-9008(A), P089.A9008(A), P087.C-0508(A), 089.A-9006(A).]; Robert Martin Ayers Sciences Fund; [NSF/AST-1108686] FX Development of the HATSouth project was funded by NSF MRI grant NSF/AST-0723074, operations are supported by NASA grant NNX12AH91H, and follow-up observations receive partial support from grant NSF/AST-1108686. Work at the Australian National University is supported by ARC Laureate Fellowship Grant FL0992131. Follow-up observations with the MPG 2.2 m/FEROS instrument were performed under MPIA guaranteed time (P087.A-9014(A), P088.A-9008(A), P089.A-9008(A)) and Chilean time (P087.C-0508(A)). AJ acknowledges support from project IC120009 'Millennium Institute of Astrophysics (MAS)' of the Millennium Science Initiative, Chilean Ministry of Economy, FONDECYT project 1130857, and BASAL CATA PFB-06. VS acknowledges support form BASAL CATA PFB-06. RB and NE acknowledge support from CONICYT-PCHA/Doctorado Nacional and Fondecyt project 1130857. KP acknowledges support from NASA grant: NNX13AQ62G. This work is based on observations made with ESO Telescopes at the La Silla Observatory under programme IDs P087.A-9014(A), P088.A-9008(A), P089.A9008(A), P087.C-0508(A), and 089.A-9006(A). We acknowledge the use of the AAVSO Photometric All-Sky Survey (APASS), funded by the Robert Martin Ayers Sciences Fund, and the SIMBAD data base, operated at CDS, Strasbourg, France. Operations at the MPG/ESO 2.2 m Telescope are jointly performed by the Max Planck Gesellschaft and the European Southern Observatory. The imaging system GROND has been built by the high-energy group of MPE in collaboration with the LSW Tautenburg and ESO. We thank Regis Lachaume for his technical assistance during the observations at the MPG 2.2 m Telescope. Australian access to the Magellan Telescopes was supported through the National Collaborative Research Infrastructure Strategy of the Australian Federal Government. We thank Albert Jahnke, Toni Hanke (HESS), Peter Conroy (MSO) for their contributions to the HATSouth project. The HATSouth network is operated by a collaboration consisting of Princeton University (PU), the Max Planck Institut fur Astronomie (MPIA), the Australian National University (ANU), and the Pontificia Universidad Catolica de Chile (PUC). The station at Las Campanas Observatory (LCO) of the Carnegie Institution is operated by PU in conjunction with PUC, the station at the High Energy Spectroscopic Survey (HESS) site is operated in conjunction with MPIA, and the station at Siding Spring Observatory (SSO) is operated jointly with ANU. This paper includes data gathered with the 6.5 metre Magellan Telescopes located at Las Campanas Observatory, Chile. NR 75 TC 4 Z9 4 U1 1 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 AUG 11 PY 2015 VL 451 IS 3 BP 2263 EP 2277 DI 10.1093/mnras/stv1070 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CQ8CL UT WOS:000360833700002 ER PT J AU Sobey, C Young, NJ Hessels, JWT Weltevrede, P Noutsos, A Stappers, BW Kramer, M Bassa, C Lyne, AG Kondratiev, VI Hassall, TE Keane, EF Bilous, AV Breton, RP Griessmeier, JM Karastergiou, A Pilia, M Serylak, M ter Veen, S van Leeuwen, J Alexov, A Anderson, J Asgekar, A Avruch, IM Bell, ME Bentum, MJ Bernardi, G Best, P Birzan, L Bonafede, A Breitling, F Broderick, J Bruggen, M Corstanje, A Carbone, D de Geus, E de Vos, M van Duin, A Duscha, S Eisloffel, J Falcke, H Fallows, RA Fender, R Ferrari, C Frieswijk, W Garrett, MA Gunst, AW Hamaker, JP Heald, G Hoeft, M Horandel, J Jutte, E Kuper, G Maat, P Mann, G Markoff, S McFadden, R McKay-Bukowski, D McKean, JP Mulcahy, DD Munk, H Nelles, A Norden, MJ Orru, E Paas, H Pandey-Pommier, M Pandey, VN Pietka, G Pizzo, R Polatidis, AG Rafferty, D Renting, A Rottgering, H Rowlinson, A Scaife, AMM Schwarz, D Sluman, J Smirnov, O Steinmetz, M Stewart, A Swinbank, J Tagger, M Tang, Y Tasse, C Thoudam, S Toribio, C Vermeulen, R Vocks, C van Weeren, RJ Wijers, RAMJ Wise, MW Wucknitz, O Yatawatta, S Zarka, P AF Sobey, C. Young, N. J. Hessels, J. W. T. Weltevrede, P. Noutsos, A. Stappers, B. W. Kramer, M. Bassa, C. Lyne, A. G. Kondratiev, V. I. Hassall, T. E. Keane, E. F. Bilous, A. V. Breton, R. P. Griessmeier, J. -M. Karastergiou, A. Pilia, M. Serylak, M. ter Veen, S. van Leeuwen, J. Alexov, A. Anderson, J. Asgekar, A. Avruch, I. M. Bell, M. E. Bentum, M. J. Bernardi, G. Best, P. Birzan, L. Bonafede, A. Breitling, F. Broderick, J. Brueggen, M. Corstanje, A. Carbone, D. de Geus, E. de Vos, M. van Duin, A. Duscha, S. Eisloeffel, J. Falcke, H. Fallows, R. A. Fender, R. Ferrari, C. Frieswijk, W. Garrett, M. A. Gunst, A. W. Hamaker, J. P. Heald, G. Hoeft, M. Horandel, J. Juette, E. Kuper, G. Maat, P. Mann, G. Markoff, S. McFadden, R. McKay-Bukowski, D. McKean, J. P. Mulcahy, D. D. Munk, H. Nelles, A. Norden, M. J. Orru, E. Paas, H. Pandey-Pommier, M. Pandey, V. N. Pietka, G. Pizzo, R. Polatidis, A. G. Rafferty, D. Renting, A. Rottgering, H. Rowlinson, A. Scaife, A. M. M. Schwarz, D. Sluman, J. Smirnov, O. Steinmetz, M. Stewart, A. Swinbank, J. Tagger, M. Tang, Y. Tasse, C. Thoudam, S. Toribio, C. Vermeulen, R. Vocks, C. van Weeren, R. J. Wijers, R. A. M. J. Wise, M. W. Wucknitz, O. Yatawatta, S. Zarka, P. TI LOFAR discovery of a quiet emission mode in PSR B0823+26 SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE stars: neutron; pulsars: individual: PSR B0823+26 ID RADIO TELESCOPE OBSERVATION; SINGLE-PULSE OBSERVATIONS; GALACTIC MAGNETIC-FIELD; FREQUENCY-DEPENDENCE; FARADAY-ROTATION; SPIN-DOWN; X-RAY; SUBPULSE MODULATION; TIMING OBSERVATIONS; CRAB PULSAR AB PSR B0823+26, a 0.53-s radio pulsar, displays a host of emission phenomena over time-scales of seconds to (at least) hours, including nulling, subpulse drifting, and mode-changing. Studying pulsars like PSR B0823+26 provides further insight into the relationship between these various emission phenomena and what they might teach us about pulsar magnetospheres. Here we report on the LOFAR (Low-Frequency Array) discovery that PSR B0823+26 has a weak and sporadically emitting 'quiet' (Q) emission mode that is over 100 times weaker (on average) and has a nulling fraction forty-times greater than that of the more regularly-emitting 'bright' (B) mode. Previously, the pulsar has been undetected in the Q mode, and was assumed to be nulling continuously. PSR B0823+26 shows a further decrease in average flux just before the transition into the B mode, and perhaps truly turns off completely at these times. Furthermore, simultaneous observations taken with the LOFAR, Westerbork, Lovell, and Effelsberg telescopes between 110 MHz and 2.7 GHz demonstrate that the transition between the Q mode and B mode occurs within one single rotation of the neutron star, and that it is concurrent across the range of frequencies observed. C1 [Sobey, C.; Noutsos, A.; Kramer, M.; Wucknitz, O.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Sobey, C.; Hessels, J. W. T.; Bassa, C.; Kondratiev, V. I.; Pilia, M.; van Leeuwen, J.; Asgekar, A.; Bentum, M. J.; de Geus, E.; de Vos, M.; van Duin, A.; Duscha, S.; Falcke, H.; Fallows, R. A.; Frieswijk, W.; Garrett, M. A.; Gunst, A. W.; Hamaker, J. P.; Heald, G.; Kuper, G.; Maat, P.; McFadden, R.; McKean, J. P.; Munk, H.; Norden, M. J.; Orru, E.; Pandey, V. N.; Pizzo, R.; Polatidis, A. G.; Renting, A.; Sluman, J.; Tang, Y.; Toribio, C.; Vermeulen, R.; Wise, M. W.; Yatawatta, S.] ASTRON Netherlands Inst Radio Astron, NL-7990 AA Dwingeloo, Netherlands. [Young, N. J.] Univ Witwatersrand, Sch Phys, ZA-2050 Johannesburg, South Africa. [Young, N. J.; Weltevrede, P.; Stappers, B. W.; Kramer, M.; Lyne, A. G.] Univ Manchester, Sch Phys & Astron, Jodrell Bank, Ctr Astrophys, Manchester M13 9PL, Lancs, England. [Hessels, J. W. T.; van Leeuwen, J.; Carbone, D.; Markoff, S.; Swinbank, J.; Wijers, R. A. M. J.; Wise, M. W.] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 XH Amsterdam, Netherlands. [Kondratiev, V. I.] Russian Acad Sci, PN Lebedev Phys Inst, Ctr Astro Space, Moscow 117997, Russia. [Hassall, T. E.; Breton, R. P.; Broderick, J.; Mulcahy, D. D.; Scaife, A. M. M.] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England. [Keane, E. F.] Swinburne Univ Technol, Ctr Astrophys & Supercomputing, Hawthorn, Vic 3122, Australia. [Keane, E. F.] ARC Ctr Excellence All Sky Astrophys CAASTRO, Redfern, NSW 2016, Australia. [Bilous, A. V.; ter Veen, S.; Corstanje, A.; Falcke, H.; Horandel, J.; Nelles, A.; Thoudam, S.] Radboud Univ Nijmegen, Dept Astrophys IMAPP, NL-6500 GL Nijmegen, Netherlands. [Griessmeier, J. -M.; Tagger, M.] Univ Orleans, CNRS, LPC2E, F-45071 Orleans 2, France. [Griessmeier, J. -M.] Univ Orleans, CNRS, Observ Paris, Stn Radioastron Nancay,INSU,OSUC,USR 704, F-18330 Nancay, France. [Karastergiou, A.; Fender, R.; Stewart, A.] Univ Oxford, Astrophys, Oxford OX1 3RH, England. [Serylak, M.] Univ Western Cape, Dept Phys & Astron, ZA-7535 Bellville, South Africa. [Alexov, A.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Anderson, J.] Helmholtz Zentrum Potsdam, GFZ, Dept Geodesy & Remote Sensing 1, D-14473 Potsdam, Germany. [Asgekar, A.] Shell Technol Ctr, Bangalore 560099, Karnataka, India. [Avruch, I. M.] SRON Netherlands Inst Space Res, NL-9700 AV Groningen, Netherlands. [Avruch, I. M.; Heald, G.; McKean, J. P.] Univ Groningen, Kapteyn Astron Inst, NL-9700 AV Groningen, Netherlands. [Bell, M. E.; Rowlinson, A.] CSIRO, Australia Telescope Natl Facil, Epping, NSW 1710, Australia. [Bentum, M. J.] Univ Twente, NL-7500 AE Enschede, Netherlands. [Bernardi, G.; van Weeren, R. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Best, P.] Univ Edinburgh, Royal Observ, Inst Astron, Edinburgh EH9 3HJ, Midlothian, Scotland. [Birzan, L.; Garrett, M. A.; Rafferty, D.; Rottgering, H.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [Bonafede, A.; Brueggen, M.] Univ Hamburg, D-21029 Hamburg, Germany. [Breitling, F.; Mann, G.; Steinmetz, M.; Vocks, C.] Leibniz Inst Astrophys Potsdam AIP, D-14482 Potsdam, Germany. [de Geus, E.] SmarterVis BV, NL-9401 JX Assen, Netherlands. [Eisloeffel, J.; Hoeft, M.] Thuringer Landessternwarte, D-07778 Tautenburg, Germany. [Ferrari, C.] Univ Nice Sophia Antipolis, CNRS, Observ Cote Azur, Lab Lagrange,UMR7293, F-06300 Nice, France. [Juette, E.] Ruhr Univ Bochum, Astron Inst, D-44780 Bochum, Germany. [McKay-Bukowski, D.] Univ Oulu, Sodankyla Geophys Observ, FI-99600 Sodankyla, Finland. [McKay-Bukowski, D.] STFC Rutherford Appleton Lab, Didcot OX11 0QX, Oxon, England. [Paas, H.] Univ Groningen, Ctr Informat Technol, NL-9747 AJ Groningen, Netherlands. [Pandey-Pommier, M.] Observ Lyon, Ctr Rech Astrophys Lyon, F-69561 St Genis Laval, France. [Schwarz, D.] Univ Bielefeld, Fak Phys, D-33501 Bielefeld, Germany. [Smirnov, O.] Rhodes Univ, Dept Phys & Elect, ZA-6140 Grahamstown, South Africa. [Smirnov, O.] SKA South Africa, ZA-7405 Pinelands, South Africa. [Tasse, C.; Zarka, P.] Observ Paris, UMR CNRS 8109, LESIA, F-92195 Meudon, France. RP Sobey, C (reprint author), Max Planck Inst Radioastron, Hugel 69, D-53121 Bonn, Germany. EM sobey@astron.nl RI Kondratiev, Vladislav/N-1105-2015; Breton, Rene/A-5536-2017; Yatawatta, Sarod/E-6037-2013; OI Kondratiev, Vladislav/0000-0001-8864-7471; Breton, Rene/0000-0001-8522-4983; Swinbank, John/0000-0001-9445-1846; Wijers, Ralph/0000-0002-3101-1808; Yatawatta, Sarod/0000-0001-5619-4017; Bilous, Anna/0000-0002-7177-6987; van Weeren, Reinout/0000-0002-0587-1660 FU Deutsche Forschungsgemeinschaft (DFG) [FOR 1254]; National Research Foundation (NRF); NWO Vidi fellowship; ERC [337062]; STFC consolidated grant; Agence Nationale de la Recherche [ANR-09-JCJC-0001-01] FX We thank the Deutsche Forschungsgemeinschaft (DFG) for funding this work within the research unit FOR 1254 'Magnetisation of Interstellar and Intergalactic Media: The Prospects of Low-Frequency Radio Observations'. NY acknowledges support from the National Research Foundation (NRF). JWTH acknowledges funding from an NWO Vidi fellowship and ERC Starting Grant 'DRAGNET' (337062). The LOFAR was designed and constructed by ASTRON, the Netherlands Institute for Radio Astronomy, and has facilities in several countries that are owned by various parties (each with their own funding sources), and that are collectively operated by the International LOFAR Telescope (ILT) foundation under a joint scientific policy. The WSRT is operated by ASTRON/NWO. Observations with the Lovell Telescope are supported through an STFC consolidated grant. This work is partly based on observations with the 100-m telescope of the Max-Planck-Institut fur Radioastronomie at Effelsberg. We would like to thank R. Karuppusamy for his help with the Effelsberg observations. CF acknowledges financial support by the Agence Nationale de la Recherche through grant ANR-09-JCJC-0001-01. The majority of the plots were created using the PSRCHIVE PYTHON interface, and the PYTHON package MATPLOTLIB (Hunter 2007). NR 86 TC 7 Z9 7 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 AUG 11 PY 2015 VL 451 IS 3 BP 2493 EP 2506 DI 10.1093/mnras/stv1066 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CQ8CL UT WOS:000360833700018 ER PT J AU Devaney, J Barrett, B Barrett, F Redmond, J O'Halloran, J AF Devaney, John Barrett, Brian Barrett, Frank Redmond, John O'Halloran, John TI Forest Cover Estimation in Ireland Using Radar Remote Sensing: A Comparative Analysis of Forest Cover Assessment Methodologies SO PLOS ONE LA English DT Article ID LAND-COVER; ALOS-PALSAR; TROPICAL DEFORESTATION; MAPPING DEFORESTATION; BRAZILIAN AMAZONIA; BOREAL FORESTS; SPATIAL DATA; CLASSIFICATION; BACKSCATTER; BIOMASS AB Quantification of spatial and temporal changes in forest cover is an essential component of forest monitoring programs. Due to its cloud free capability, Synthetic Aperture Radar (SAR) is an ideal source of information on forest dynamics in countries with near-constant cloud-cover. However, few studies have investigated the use of SAR for forest cover estimation in landscapes with highly sparse and fragmented forest cover. In this study, the potential use of L-band SAR for forest cover estimation in two regions (Longford and Sligo) in Ireland is investigated and compared to forest cover estimates derived from three national (Forestry2010, Prime2, National Forest Inventory), one pan-European (Forest Map 2006) and one global forest cover (Global Forest Change) product. Two machine-learning approaches (Random Forests and Extremely Randomised Trees) are evaluated. Both Random Forests and Extremely Randomised Trees classification accuracies were high (98.1-98.5%), with differences between the two classifiers being minimal (<0.5%). Increasing levels of post classification filtering led to a decrease in estimated forest area and an increase in overall accuracy of SAR-derived forest cover maps. All forest cover products were evaluated using an independent validation dataset. For the Longford region, the highest overall accuracy was recorded with the Forestry2010 dataset (97.42%) whereas in Sligo, highest overall accuracy was obtained for the Prime2 dataset (97.43%), although accuracies of SAR-derived forest maps were comparable. Our findings indicate that spaceborne radar could aid inventories in regions with low levels of forest cover in fragmented landscapes. The reduced accuracies observed for the global and pan-continental forest cover maps in comparison to national and SAR-derived forest maps indicate that caution should be exercised when applying these datasets for national reporting. C1 [Devaney, John; O'Halloran, John] Univ Coll Cork UCC, Sch Biol Earth & Environm Sci BEES, Cork, Ireland. [Barrett, Brian] Univ Coll Cork UCC, Sch Geog & Archaeol, Cork, Ireland. [Barrett, Frank; Redmond, John] Dept Agr Food & Marine, Forest Serv, Johnstown Castle, Wexford, Ireland. RP Devaney, J (reprint author), Smithsonian Environm Res Ctr, 647 Contees Wharf, Edgewater, MD 21037 USA. EM devaneyj@si.edu OI Devaney, John/0000-0002-7676-0378 FU Science, Technology, Research and Innovation for the Environment (STRIVE) Programme [2011-CCRP-FS-1.1]; Irish Government under National Development Plan (NDP) FX This study has been prepared as part of the Science, Technology, Research and Innovation for the Environment (STRIVE) Programme (Grant No. 2011-CCRP-FS-1.1). The programme is financed by the Irish Government under the National Development Plan (NDP) 2007-2013 and is administered by the Environmental Protection Agency (www.epa.ie). The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 89 TC 0 Z9 0 U1 3 U2 35 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 AUG 11 PY 2015 VL 10 IS 8 AR e0133583 DI 10.1371/journal.pone.0133583 PG 27 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA CO7PP UT WOS:000359353300008 PM 26262681 ER PT J AU Sherratt, E Castaneda, MD Garwood, RJ Mahler, DL Sanger, TJ Herrel, A de Queiroz, K Losos, JB AF Sherratt, Emma Castaneda, Maria del Rosario Garwood, Russell J. Mahler, D. Luke Sanger, Thomas J. Herrel, Anthony de Queiroz, Kevin Losos, Jonathan B. TI Amber fossils demonstrate deep-time stability of Caribbean lizard communities SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA LA English DT Article DE adaptive radiation; ecomorph; Hispaniola; Miocene; Anolis ID DOMINICAN AMBER; ANOLIS-LIZARDS; PHYLOGENETIC-RELATIONSHIPS; IGUANIAN LIZARDS; MORPHOLOGICAL DIVERSIFICATION; ECOLOGICAL OPPORTUNITY; ISLAND LIZARDS; EVOLUTION; DIVERSITY; SERIES AB Whether the structure of ecological communities can exhibit stability over macroevolutionary timescales has long been debated. The similarity of independently evolved Anolis lizard communities on environmentally similar Greater Antillean islands supports the notion that community evolution is deterministic. However, a dearth of Caribbean Anolis fossils-only three have been described to date-has precluded direct investigation of the stability of anole communities through time. Here we report on an additional 17 fossil anoles in Dominican amber dating to 15-20 My before the present. Using data collected primarily by X-ray microcomputed tomography (X-ray micro-CT), we demonstrate that the main elements of Hispaniolan anole ecomorphological diversity were in place in the Miocene. Phylogenetic analysis yields results consistent with the hypothesis that the ecomorphs that evolved in the Miocene are members of the same ecomorph clades extant today. The primary axes of ecomorphological diversity in the Hispaniolan anole fauna appear to have changed little between the Miocene and the present, providing evidence for the stability of ecological communities over macroevolutionary timescales. C1 [Sherratt, Emma] Univ New England, Sch Environm & Rural Sci, Armidale, NSW 2351, Australia. [Sherratt, Emma; Castaneda, Maria del Rosario; Losos, Jonathan B.] Harvard Univ, Dept Organism & Evolutionary Biol, Cambridge, MA 02138 USA. [Sherratt, Emma; Castaneda, Maria del Rosario; Losos, Jonathan B.] Harvard Univ, Museum Comparat Zool, Cambridge, MA 02138 USA. [Garwood, Russell J.] Univ Manchester, Sch Earth Atmospher & Environm Sci, Manchester M13 9PL, Lancs, England. [Mahler, D. Luke] Univ Calif Davis, Ctr Populat Biol, Davis, CA 95616 USA. [Sanger, Thomas J.] Univ Florida, Dept Mol Genet & Microbiol, Gainesville, FL 32610 USA. [Herrel, Anthony] Museum Natl Hist Nat, Dept Ecol & Gest Biodiversite, UMR 7179, F-75231 Paris, France. [Herrel, Anthony] Univ Ghent, Evolutionary Morphol Vertebrates, B-9000 Ghent, Belgium. [de Queiroz, Kevin] Smithsonian Inst, Natl Museum Amer Hist, Dept Vertebrate Zool, Washington, DC 20560 USA. RP Sherratt, E (reprint author), Univ New England, Sch Environm & Rural Sci, Armidale, NSW 2351, Australia. EM emma.sherratt@gmail.com RI Herrel, Anthony/C-3712-2013; Sherratt, Emma/A-9931-2011 OI Herrel, Anthony/0000-0003-0991-4434; Sherratt, Emma/0000-0003-2164-7877 FU National Science Foundation FX We thank those who allowed us access to amber fossils for study: G. Bechly, J. Calbeto, L. Costeur, M. Cusanovich, G. Greco, M. Greco, D. Grimaldi, M. Halonen, and J. Work. We especially thank E. Morone for providing access to more than half of the fossils examined for this study. We thank J. Klaczko, and G. Gartner for providing support and discussions and J. Casart for assisting with data collection. Scan data were also provided by R. Boistel, M. Polcyn, L. Jacobs, M. Colbert, and R. Ketcham. We thank the National Science Foundation for support. NR 56 TC 4 Z9 4 U1 5 U2 26 PU NATL ACAD SCIENCES PI WASHINGTON PA 2101 CONSTITUTION AVE NW, WASHINGTON, DC 20418 USA SN 0027-8424 J9 P NATL ACAD SCI USA JI Proc. Natl. Acad. Sci. U. S. A. PD AUG 11 PY 2015 VL 112 IS 32 BP 9961 EP 9966 DI 10.1073/pnas.1506516112 PG 6 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA CO6RY UT WOS:000359285100060 PM 26216976 ER PT J AU Ali, ZS Parsons, AR Zheng, HX Pober, JC Liu, A Aguirre, JE Bradley, RF Bernardi, G Carilli, CL Cheng, C DeBoer, DR Dexter, MR Grobbelaar, J Horrell, J Jacobs, DC Klima, P MacMahon, DHE Maree, M Moore, DF Razavi, N Stefan, II Walbrugh, WP Walker, A AF Ali, Zaki S. Parsons, Aaron R. Zheng, Haoxuan Pober, Jonathan C. Liu, Adrian Aguirre, James E. Bradley, Richard F. Bernardi, Gianni Carilli, Chris L. Cheng, Carina DeBoer, David R. Dexter, Matthew R. Grobbelaar, Jasper Horrell, Jasper Jacobs, Daniel C. Klima, Pat MacMahon, David H. E. Maree, Matthys Moore, David F. Razavi, Nima Stefan, Irina I. Walbrugh, William P. Walker, Andre TI PAPER-64 CONSTRAINTS ON REIONIZATION: THE 21 cm POWER SPECTRUM AT z=8.4 SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology: observations; dark ages, reionization, first stars; early universe; instrumentation: interferometers; intergalactic medium ID STAR-FORMING GALAXIES; ULTRA DEEP FIELD; SIMILAR-TO 20; NORTH CELESTIAL POLE; COSMIC REIONIZATION; INTERGALACTIC MEDIUM; FOREGROUND REMOVAL; CENTIMETER FLUCTUATIONS; REDUNDANCY CALIBRATION; CROSS-CORRELATION AB In this paper, we report new limits on 21 cm emission from cosmic reionization based on a 135 day observing campaign with a 64-element deployment of the Donald C. Backer Precision Array for Probing the Epoch of Reionization in South Africa. This work extends the work presented in Parsons et al. with more collecting area, a longer observing period, improved redundancy-based calibration, improved fringe-rate filtering, and updated power-spectral analysis using optimal quadratic estimators. The result is a new 2 sigma upper limit on Delta(2)(k) of (22.4 mK)(2) in the range 0.15 < k < 0.5h Mpc(-1) at z = 8.4. This represents a three-fold improvement over the previous best upper limit. As we discuss in more depth in a forthcoming paper, this upper limit supports and extends previous evidence against extremely cold reionization scenarios. We conclude with a discussion of implications for future 21 cm reionization experiments, including the newly funded Hydrogen Epoch of Reionization Array. C1 [Ali, Zaki S.; Parsons, Aaron R.; Liu, Adrian; Cheng, Carina] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Parsons, Aaron R.; DeBoer, David R.; Dexter, Matthew R.; MacMahon, David H. E.] Univ Calif Berkeley, Radio Astron Lab, Berkeley, CA 94720 USA. [Zheng, Haoxuan] MIT, Dept Phys, Cambridge, MA 02139 USA. [Pober, Jonathan C.] Univ Washington, Dept Phys, Seattle, WA 98195 USA. [Liu, Adrian] Berkeley Ctr Cosmol Phys, Berkeley, CA USA. [Aguirre, James E.; Moore, David F.] Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA. [Bradley, Richard F.] Univ Virginia, Dept Elect & Comp Engn, Charlottesville, VA USA. [Bradley, Richard F.; Klima, Pat] Natl Radio Astron Observ, Charlottesville, VA USA. [Bradley, Richard F.] Univ Virginia, Dept Astron, Charlottesville, VA 22903 USA. [Bernardi, Gianni; Grobbelaar, Jasper; Horrell, Jasper; Maree, Matthys; Walbrugh, William P.; Walker, Andre] Sq Kilometer Array, Cape Town, South Africa. [Bernardi, Gianni] Rhodes Univ, Dept Phys & Elect, Grahamstown, South Africa. [Bernardi, Gianni] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Carilli, Chris L.] Natl Radio Astron Observ, Socorro, NM 87801 USA. [Carilli, Chris L.; Razavi, Nima; Stefan, Irina I.] Univ Cambridge, Cavendish Lab, Cambridge CB3 0HE, England. [Jacobs, Daniel C.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ USA. RP Ali, ZS (reprint author), Univ Calif Berkeley, Dept Astron, 601 Campbell Hall, Berkeley, CA 94720 USA. OI Pober, Jonathan/0000-0002-3492-0433 FU National Science Foundation (NSF) [0804508, 1129258, 1125558]; NSF [1352519, 1302774, 1401708]; Mount Cuba Astronomical Association FX PAPER is supported by grants from the National Science Foundation (NSF; awards 0804508, 1129258, and 1125558). A.R.P., J.C.P., and D.C.J. would like to acknowledge NSF support (awards 1352519, 1302774, and 1401708, respectively). J.E.A. would like to acknowledge a generous grant from the Mount Cuba Astronomical Association for computing resources. We graciously thank SKA-SA for site infrastructure and observing support. We also thank interns Monde Manzini and Ruvano Casper from Durban University of Technology, who helped expand the array from 32 to 64 antennas. Thanks also to Josh Dillon for helpful discussions on optimal quadratic estimators. NR 107 TC 64 Z9 64 U1 1 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD AUG 10 PY 2015 VL 809 IS 1 AR 61 DI 10.1088/0004-637X/809/1/61 PG 21 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CR9DN UT WOS:000361653500061 ER PT J AU Bai, XN Caprioli, D Sironi, L Spitkovsky, A AF Bai, Xue-Ning Caprioli, Damiano Sironi, Lorenzo Spitkovsky, Anatoly TI MAGNETOHYDRODYNAMIC-PARTICLE-IN-CELL METHOD FOR COUPLING COSMIC RAYS WITH A THERMAL PLASMA: APPLICATION TO NON-RELATIVISTIC SHOCKS SO ASTROPHYSICAL JOURNAL LA English DT Article DE acceleration of particles; instabilities; magnetohydrodynamics (MHD); methods: numerical; plasmas; shock waves ID UNSPLIT GODUNOV METHOD; MAGNETIC-FIELD AMPLIFICATION; HYBRID SIMULATIONS; SUPERNOVA-REMNANTS; ION-ACCELERATION; FILAMENTATION INSTABILITY; CONSTRAINED TRANSPORT; ASTROPHYSICAL SHOCKS; PROTOPLANETARY DISKS; COLLISIONLESS SHOCKS AB We formulate a magnetohydrodynamic-particle-in-cell (MHD-PIC) method for describing the interaction between collisionless cosmic ray (CR) particles and a thermal plasma. The thermal plasma is treated as a fluid, obeying equations of ideal MHD, while CRs are treated as relativistic Lagrangian particles subject to the Lorentz force. Backreaction from CRs to the gas is included in the form of momentum and energy feedback. In addition, we include the electromagnetic feedback due to CR-induced Hall effect that becomes important when the electron-ion drift velocity of the background plasma induced by CRs approaches the Alfven velocity. Our method is applicable on scales much larger than the ion inertial length, bypassing the microscopic scales that must be resolved in conventional PIC methods, while retaining the full kinetic nature of the CRs. We have implemented and tested this method in the Athena MHD code, where the overall scheme is second-order accurate and fully conservative. As a first application, we describe a numerical experiment to study particle acceleration in non-relativistic shocks. Using a simplified prescription for ion injection, we reproduce the shock structure and the CR energy spectra obtained with more self-consistent hybrid-PIC simulations, but at substantially reduced computational cost. We also show that the CR-induced Hall effect reduces the growth rate of the Bell instability and affects the gas dynamics in the vicinity of the shock front. As a step forward, we are able to capture the transition of particle acceleration from non-relativistic to relativistic regimes, with momentum spectrum f (p) proportional to p(-4) connecting smoothly through the transition, as expected from the theory of Fermi acceleration. C1 [Bai, Xue-Ning; Sironi, Lorenzo] Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, 60 Garden St,MS 51, Cambridge, MA 02138 USA. [Caprioli, Damiano; Spitkovsky, Anatoly] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. RP Bai, XN (reprint author), Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, 60 Garden St,MS 51, Cambridge, MA 02138 USA. EM xbai@cfa.harvard.edu RI Caprioli, Damiano/I-6582-2012 OI Caprioli, Damiano/0000-0003-0939-8775 FU NASA through Hubble Fellowship grant - Space Telescope Science Institute [HST-HF2-51301.001-A]; NASA [NAS 5-26555, NNX14AQ34G, NAS8-03060]; NASA through Einstein Fellowship grant - Chandra X-ray Center [PF1-120090]; Simons Foundation [267233, 291817]; XSEDE grant [TG-AST140001] FX We thank the anonymous referee for a very useful report that led to several improvements to the paper, particularly on code implementation, convergence checks, and overall clarity. X.-N.B. is supported by NASA through Hubble Fellowship grant HST-HF2-51301.001-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. D.C. is supported by NASA grant NNX14AQ34G. L.S. is supported by NASA through Einstein 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. This work was partially supported by Simons Foundation (grants 267233 and 291817 to AS), and was facilitated by Max Planck/Princeton Center for Plasma Physics. Computation for this work was performed on computational resources supported by PICSciE and the OIT's High Performance Computing Center at Princeton University. This work also used resources on Stampede at Texas Advanced Computing Center through XSEDE grant TG-AST140001. NR 65 TC 9 Z9 9 U1 1 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 AUG 10 PY 2015 VL 809 IS 1 AR 55 DI 10.1088/0004-637X/809/1/55 PG 22 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CR9DN UT WOS:000361653500055 ER PT J AU Barclay, T Quintana, EV Adams, FC Ciardi, DR Huber, D Foreman-Mackey, D Montet, BT Caldwell, D AF Barclay, Thomas Quintana, Elisa V. Adams, Fred C. Ciardi, David R. Huber, Daniel Foreman-Mackey, Daniel Montet, Benjamin T. Caldwell, Douglas TI THE FIVE PLANETS IN THE KEPLER-296 BINARY SYSTEM ALL ORBIT THE PRIMARY: A STATISTICAL AND ANALYTICAL ANALYSIS SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries: general; methods: data analysis; methods: statistical; planetary systems; stars: individual (Kepler-296, KIC 11497958, KOI-1422); techniques: photometric ID POTENTIAL TRANSIT SIGNALS; CANDIDATE HOST STARS; EARTH-SIZED PLANET; SOLAR-TYPE STARS; HABITABLE ZONE; BAYESIAN-INFERENCE; MISSION DATA; DENSE CORES; DARK CLOUDS; M DWARFS AB Kepler-296 is a binary star system with two M-dwarf components separated by 0 ''.2. Five transiting planets have been confirmed to be associated with the Kepler-296 system; given the evidence to date, however, the planets could in principle orbit either star. This ambiguity has made it difficult to constrain both the orbital and physical properties of the planets. Using both statistical and analytical arguments, this paper shows that all five planets are highly likely to orbit the primary star in this system. We performed a Markov-Chain Monte Carlo simulation using a five transiting planet model, leaving the stellar density and dilution with uniform priors. Using importance sampling, we compared the model probabilities under the priors of the planets orbiting either the brighter or the fainter component of the binary. A model where the planets orbit the brighter component, Kepler-296A, is strongly preferred by the data. Combined with our assertion that all five planets orbit the same star, the two outer planets in the system, Kepler-296 Ae and Kepler-296 Af, have radii of 1.53 +/- 0.26 and 1.80 +/- 0.31 R-circle plus, respectively, and receive incident stellar fluxes of 1.40 +/- 0.23 and 0.62 +/- 0.10 times the incident flux the Earth receives from the Sun. This level of irradiation places both planets within or close to the circumstellar habitable zone of their parent star. C1 [Barclay, Thomas; Quintana, Elisa V.; Caldwell, Douglas] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Barclay, Thomas] Bay Area Environm Res Inst, Petaluma, CA 94952 USA. [Adams, Fred C.] Univ Michigan, Dept Phys, Ann Arbor, MI 48109 USA. [Ciardi, David R.] CALTECH, NASA Exoplanet Sci Inst, Pasadena, CA 91125 USA. [Huber, Daniel] Univ Sydney, Sch Phys, Sydney Inst Astron SIfA, Sydney, NSW 2006, Australia. [Huber, Daniel; Caldwell, Douglas] SETI Inst, Mountain View, CA 94043 USA. [Huber, Daniel] Aarhus Univ, Dept Phys & Astron, Stellar Astrophys Ctr, DK-8000 Aarhus C, Denmark. [Foreman-Mackey, Daniel] NYU, Dept Phys, Ctr Cosmol & Particle Phys, New York, NY 10003 USA. [Montet, Benjamin T.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA. [Montet, Benjamin T.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Barclay, T (reprint author), NASA, Ames Res Ctr, M-S 244-30, Moffett Field, CA 94035 USA. OI Montet, Benjamin/0000-0001-7516-8308; Ciardi, David/0000-0002-5741-3047 FU NASA Science Mission Directorate; Association of Universities for Research in Astronomy, Inc., under NASA [NAS5-26555]; NASA Office of Space Science [NNX09AF08G]; NASA Keck PI Data Award; W. M. Keck Foundation; NASA Senior Fellowship at the Ames Research Center; National Science Foundation Graduate Research Fellowship [DGE1144469]; Australian Research Council [DE140101364]; National Aeronautics and Space Administration [NNX14AB92G] FX This paper includes data collected by the Kepler mission. Funding for the Kepler mission is provided by the NASA Science Mission Directorate. We would like to express our gratitude to all those who have worked on the Kepler pipeline over the many years of the Kepler mission. Some Kepler data presented in this paper were obtained from the Mikulski Archive for Space Telescopes (MAST) at the Space Telescope Science Institute (STScI). 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. This research has made use of the NASA Exoplanet Archive, which is operated by the California Institute of Technology, under contract with the National Aeronautics and Space Administration under the Exoplanet Exploration Program. This research made use of APLpy, an open-source plotting package for Python hosted at http://aplpy.github.com. This work was supported by a NASA Keck PI Data Award, administered by the NASA Exoplanet Science Institute. Some of the 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 Maunakea has always had within the indigenous Hawaiian community. We are most fortunate to have the opportunity to conduct observations from this mountain. E.V.Q. is supported by a NASA Senior Fellowship at the Ames Research Center, administered by Oak Ridge Associated Universities through a contract with NASA. B.T.M. is supported by the National Science Foundation Graduate Research Fellowship under Grant No. DGE1144469. D.H. acknowledges support by the Australian Research Council's Discovery Projects funding scheme (project number DE140101364) and support by the National Aeronautics and Space Administration under Grant NNX14AB92G issued through the Kepler Participating Scientist Program. NR 62 TC 13 Z9 13 U1 3 U2 11 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD AUG 10 PY 2015 VL 809 IS 1 DI 10.1088/0004-637X/809/1/7 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CR9DN UT WOS:000361653500007 ER PT J AU Barnacka, A Geller, MJ Dell'Antonio, IP Benbow, W AF Barnacka, Anna Geller, Margaret J. Dell'Antonio, Ian P. Benbow, Wystan TI RESOLVING THE HIGH-ENERGY UNIVERSE WITH STRONG GRAVITATIONAL LENSING: THE CASE OF PKS 1830-211 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: jets; gamma-rays: jets; gravitational lensing: strong; methods: data analysis; techniques: high angular resolution; quasars: individual (PKS 1820-211) ID LARGE-AREA TELESCOPE; GAMMA-RAY FLARES; MOLECULAR ABSORPTION-LINES; SYNCHROTRON-PROTON BLAZAR; RADIO-SOURCE PKS1830-211; FERMI-DETECTED BLAZARS; TIME-DELAY DISTANCES; HUBBLE CONSTANT; LUMINOUS BLAZARS; M87 JET AB Gravitational lensing is a potentially powerful tool for elucidating the origin of gamma-ray emission from distant sources. Cosmic lenses magnify the emission from distant sources and produce time delays between mirage images. Gravitationally induced time delays depend on the position of the emitting regions in the source plane. The Fermi/LAT telescope continuously monitors the entire sky and detects gamma-ray flares, including those from gravitationally lensed blazars. Therefore, temporal resolution at gamma-ray energies can be used to measure these time delays, which, in turn, can be used to resolve the origin of the gamma-ray flares spatially. We provide a guide to the application and Monte Carlo simulation of three techniques for analyzing these unresolved light curves: the autocorrelation function, the double power spectrum, and the maximum peak method. We apply these methods to derive time delays from the gamma-ray light curve of the gravitationally lensed blazar PKS 1830-211. The result of temporal analysis combined with the properties of the lens from radio observations yield an improvement in spatial resolution at gamma-ray energies by a factor of 10,000. We analyze four active periods. For two of these periods the emission is consistent with origination from the core, and for the other two the data suggest that the emission region is displaced from the core by more than similar to 1.5 kpc. For the core emission, the gamma-ray time delays, 23 +/- 0.5 days and 19.7 +/- 1.2 days, are consistent with the radio time delay of 26(-5)(+4) days. C1 [Barnacka, Anna; Geller, Margaret J.; Benbow, Wystan] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Barnacka, Anna] Jagiellonian Univ, Astron Observ, Krakow, Poland. [Dell'Antonio, Ian P.] Brown Univ, Dept Phys, Providence, RI 02912 USA. RP Barnacka, A (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS 20, Cambridge, MA 02138 USA. EM abarnacka@cfa.harvard.edu OI Barnacka, Anna/0000-0001-5655-4158; Geller, Margaret/0000-0002-9146-4876 FU Department of Energy Office of Science; NASA; Smithsonian Astrophysical Observatory; NCN grant [DEC-2011/01/M/ST9/01891]; Smithsonian Institution FX A. B. is supported by the Department of Energy Office of Science, NASA & the Smithsonian Astrophysical Observatory with financial support from the NCN grant DEC-2011/01/M/ ST9/01891. M.J.G. is supported by the Smithsonian Institution. NR 109 TC 5 Z9 5 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD AUG 10 PY 2015 VL 809 IS 1 AR 100 DI 10.1088/0004-637X/809/1/100 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CR9DN UT WOS:000361653500100 ER PT J AU Bromley, BC Kenyon, SJ AF Bromley, Benjamin C. Kenyon, Scott J. TI EVOLUTION OF A RING AROUND THE PLUTO-CHARON BINARY SO ASTROPHYSICAL JOURNAL LA English DT Article DE Kuiper belt: general; planet-disk interactions; planets and satellites: formation; planets and satellites: individual (Pluto); planets and satellites: rings ID GIANT IMPACT ORIGIN; TRANSITING CIRCUMBINARY PLANETS; ECCENTRIC STELLAR BINARIES; BODY-COAGULATION CODE; SATURNS RINGS; ACCRETION DISKS; PLANETESIMAL SWARM; TIDAL EVOLUTION; GASEOUS NEBULA; KUIPER-BELT AB We consider the formation of satellites around the Pluto-Charon binary. An early collision between the two partners likely produced the binary and a narrow ring of debris, out of which arose the moons Styx, Nix, Kerberos, and Hydra. How the satellites emerged from the compact ring is uncertain. Here we show that a particle ring spreads from physical collisions and collective gravitational scattering, similar to migration. Around a binary, these processes take place in the reference frames of "most circular" orbits, akin to circular ones in a Keplerian potential. Ring particles damp to these orbits and avoid destructive collisions. Damping and diffusion also help particles survive dynamical instabilities driven by resonances with the binary. In some situations, particles become trapped near resonances that sweep outward with the tidal evolution of the Pluto-Charon binary. With simple models and numerical experiments, we show how the Pluto-Charon impact ring may have expanded into a broad disk, out of which grew the circumbinary moons. In some scenarios, the ring can spread well beyond the orbit of Hydra, the most distant moon, to form a handful of smaller satellites. If these small moons exist, New Horizons will find them. C1 [Bromley, Benjamin C.] Univ Utah, Dept Phys & Astron, Salt Lake City, UT 84112 USA. [Kenyon, Scott J.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Bromley, BC (reprint author), Univ Utah, Dept Phys & Astron, 115 S 1400 E,Rm 201, Salt Lake City, UT 84112 USA. EM bromley@physics.utah.edu; skenyon@cfa.harvard.edu OI Kenyon, Scott/0000-0003-0214-609X FU NASA [NNX10AF35G, NNX11AM37G] FX We are grateful for the comments of an anonymous referee that resulted in a number of improvements to our presentation. We thank NASA for support through the Astrophysics Theory and Origins of Solar Systems programs (grant NNX10AF35G) and through the Outer Planets Program (grant NNX11AM37G). We are also grateful to NASA for a generous allotment of supercomputer time on the "discover" cluster. NR 131 TC 1 Z9 1 U1 0 U2 8 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD AUG 10 PY 2015 VL 809 IS 1 AR 88 DI 10.1088/0004-637X/809/1/88 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CR9DN UT WOS:000361653500088 ER PT J AU Ciardi, DR Van Eyken, JC Barnes, JW Beichman, CA Carey, SJ Crockett, CJ Eastman, J Johns-Krull, CM Howell, SB Kane, SR Mclane, JN Plavchan, P Prato, L Stauffer, J Van Belle, GT Von Braun, K AF Ciardi, David R. Van Eyken, Julian C. Barnes, Jason W. Beichman, Charles A. Carey, Sean J. Crockett, Christopher J. Eastman, Jason Johns-Krull, Christopher M. Howell, Steve B. Kane, Stephen R. Mclane, Jacob N. . Plavchan, Peter Prato, L. Stauffer, John Van Belle, Gerard T. Von Braun, Kaspar TI FOLLOW-UP OBSERVATIONS OF PTFO 8-8695: A 3 MYR OLD T TAURI STAR HOSTING A JUPITER-MASS PLANETARY CANDIDATE SO ASTROPHYSICAL JOURNAL LA English DT Article DE planetary systems; stars: individual (PTFO 8-8695, 2MASS J05250755+0134243, CVSO 30); stars: pre-main sequence ID SPIN-ORBIT MISALIGNMENT; RADIAL-VELOCITY; ORION PROJECT; LIGHT-CURVE; TRANSIT; VARIABILITY; SYSTEM; SEARCH; BINARY; OCCULTATIONS AB We present Spitzer 4.5 mu m light curve observations, Keck NIRSPEC radial velocity observations, and LCOGT optical light curve observations of PTFO 8-8695, which may host a Jupiter-sized planet in a very short orbital period (0.45 days). Previous work by van Eyken et al. and Barnes et al. predicts that the stellar rotation axis and the planetary orbital plane should precess with a period of 300-600 days. As a consequence, the observed transits should change shape and depth, disappear, and reappear with the precession. Our observations indicate the long-term presence of the transit events (> 3 years), and that the transits indeed do change depth, disappear and reappear. The Spitzer observations and the NIRSPEC radial velocity observations (with contemporaneous LCOGT optical light curve data) are consistent with the predicted transit times and depths for the M-k = 0.34 M-circle dot precession model and demonstrate the disappearance of the transits. An LCOGT optical light curve shows that the transits do reappear approximately 1 year later. The observed transits occur at the times predicted by a straight-forward propagation of the transit ephemeris. The precession model correctly predicts the depth and time of the Spitzer transit and the lack of a transit at the time of the NIRSPEC radial velocity observations. However, the precession model predicts the return of the transits approximately 1 month later than observed by LCOGT. Overall, the data are suggestive that the planetary interpretation of the observed transit events may indeed be correct, but the precession model and data are currently insufficient to confirm firmly the planetary status of PTFO 8-8695b. C1 [Ciardi, David R.; Van Eyken, Julian C.; Beichman, Charles A.] NASA Exoplanet Sci Inst Caltech, Pasadena, CA 91125 USA. [Van Eyken, Julian C.] Univ Calif Santa Barbara, LCOGT, Santa Barbara, CA 93106 USA. [Barnes, Jason W.; Eastman, Jason] Cumbres Observ Global Telescope Network, Goleta, CA USA. [Barnes, Jason W.] Univ Idaho, Moscow, ID 83843 USA. [Carey, Sean J.; Stauffer, John] Spitzer Sci Ctr Caltech, Pasadena, CA USA. [Crockett, Christopher J.] Sci News, Washington, DC 20036 USA. [Eastman, Jason] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Johns-Krull, Christopher M.] Rice Univ, Houston, TX USA. [Howell, Steve B.] NASA Ames Res Ctr, Mountain View, CA USA. [Kane, Stephen R.] San Francisco State Univ, San Francisco, CA 94132 USA. [Mclane, Jacob N. .; Prato, L.; Van Belle, Gerard T.; Von Braun, Kaspar] Lowell Observ, Flagstaff, AZ 86001 USA. [Plavchan, Peter] Missouri State Univ, Springfield, MO USA. RP Ciardi, DR (reprint author), NASA Exoplanet Sci Inst Caltech, Pasadena, CA 91125 USA. EM ciardi@ipac.caltech.edu RI Barnes, Jason/B-1284-2009; OI Barnes, Jason/0000-0002-7755-3530; Eastman, Jason/0000-0003-3773-5142; Ciardi, David/0000-0002-5741-3047 FU W. M. Keck Foundation; Las Cumbres Observatory Global Telescope Network; NASA; National Aeronautics and Space Administration under the Exoplanet Exploration Program; National Aeronautics and Space Administration FX D.R.C. would like to dedicate this paper to his dad Robert A. Ciardi (1940-2013). Robert Ciardi had a passion for learning and knowledge and, in particular, for science. While not able to pursue a career in science for himself, he never stopped thinking and growing, and through his love and encouragement, D.R.C. was able to pursue his own love of exploration and science. In many ways, Robert Ciardi was more excited about this discovery than the authors on this paper. He will be greatly missed. Thank you, Dad. Some of the data presented herein were obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California and the National Aeronautics and Space Administration. The Observatory was made possible by the generous financial support of the W. M. Keck Foundation. The authors wish to recognize and acknowledge the 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 research has made use of the LCOGT Archive, which is operated by the California Institute of Technology, under contract with the Las Cumbres Observatory Global Telescope Network. 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. This research has made use of the NASA Exoplanet Archive, which is operated by the California Institute of Technology, under contract with the National Aeronautics and Space Administration under the Exoplanet Exploration Program. Portions of this work were performed at the California Institute of Technology under contract with the National Aeronautics and Space Administration. NR 58 TC 8 Z9 8 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD AUG 10 PY 2015 VL 809 IS 1 AR 42 DI 10.1088/0004-637X/809/1/42 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CR9DN UT WOS:000361653500042 ER PT J AU Fukui, A Gould, A Sumi, T Bennett, DP Bond, IA Han, C Suzuki, D Beaulieu, JP Batista, V Udalski, A Street, RA Tsapras, Y Hundertmark, M Abe, F Bhattacharya, A Freeman, M Itow, Y Ling, CH Koshimoto, N Masuda, K Matsubara, Y Muraki, Y Ohnishi, K Philpott, LC Rattenbury, N Saito, T Sullivan, DJ Tristram, PJ Yonehara, A Choi, JY Christie, GW DePoy, DL Dong, SB Drummond, J Gaudi, BS Hwang, KH Kavka, A Lee, CU McCormick, J Natusch, T Ngan, H Park, H Pogge, RW Shin, IG Tan, TG Yee, JC Szymanski, MK Pietrzynski, G Soszynski, I Poleski, R Kozlowski, S Pietrukowicz, P Ulaczyk, K Wyrzykowski, L Bramich, DM Browne, P Dominik, M Horne, K Ipatov, S Kains, N Snodgrass, C Steele, IA AF Fukui, A. Gould, A. Sumi, T. Bennett, D. P. Bond, I. A. Han, C. Suzuki, D. Beaulieu, J. -P. Batista, V. Udalski, A. Street, R. A. Tsapras, Y. Hundertmark, M. Abe, F. Bhattacharya, A. Freeman, M. Itow, Y. Ling, C. H. Koshimoto, N. Masuda, K. Matsubara, Y. Muraki, Y. Ohnishi, K. Philpott, L. C. Rattenbury, N. Saito, T. Sullivan, D. J. Tristram, P. J. Yonehara, A. Choi, J. -Y. Christie, G. W. DePoy, D. L. Dong, Subo Drummond, J. Gaudi, B. S. Hwang, K. -H. Kavka, A. Lee, C. -U. McCormick, J. Natusch, T. Ngan, H. Park, H. Pogge, R. W. Shin, I-G. Tan, T. -G. Yee, J. C. Szymanski, M. K. Pietrzynski, G. Soszynski, I. Poleski, R. Kozlowski, S. Pietrukowicz, P. Ulaczyk, K. Wyrzykowski, L. Bramich, D. M. Browne, P. Dominik, M. Horne, K. Ipatov, S. Kains, N. Snodgrass, C. Steele, I. A. CA MOA Collaboration FUN Collaboration OGLE Collaboration RoboNet Collaboration TI OGLE-2012-BLG-0563Lb: A SATURN-MASS PLANET AROUND AN M DWARF WITH THE MASS CONSTRAINED BY SUBARU AO IMAGING SO ASTROPHYSICAL JOURNAL LA English DT Article DE planetary systems; planets and satellites: detection; planets and satellites: gaseous planets; stars: late-type; techniques: high angular resolution; techniques: photometric ID MAGNIFICATION MICROLENSING EVENTS; SOLAR-TYPE STARS; MILKY-WAY BULGE; GALACTIC BULGE; JUPITER/SATURN ANALOG; MODEL ATMOSPHERES; HIGH-RESOLUTION; EXTINCTION MAP; MAIN-SEQUENCE; GIANT PLANETS AB We report the discovery of a microlensing exoplanet OGLE-2012-BLG-0563Lb with the planet-star mass ratio of similar to 1 x 10(-3). Intensive photometric observations of a high-magnification microlensing event allow us to detect a clear signal of the planet. Although no parallax signal is detected in the light curve, we instead succeed at detecting the flux from the host star in high-resolution JHK'-band images obtained by the Subaru/AO188 and Infrared Camera and Spectrograph instruments, allowing us to constrain the absolute physical parameters of the planetary system. With the help of spectroscopic information about the source star obtained during the high-magnification state by Bensby et al., we find that the lens system is located at 1.3(-0.8)(+0.6) kpc from us, and consists of an M dwarf (0.34(-0.20)(+0.12)M(circle dot)) orbited by a Saturn-mass planet (0.39(-0.23)(+0.14)M(Jup)) at the projected separation of 0.74(-0.42)(+0.26)AU (close model) or 4.3(-2.5)(+1.5)AU (wide model). The probability of contamination in the host star's flux, which would reduce the masses by a factor of up to three, is estimated to be 17%. This possibility can be tested by future high-resolution imaging. We also estimate the (J - K-s) and (H - K-s) colors of the host star, which are marginally consistent with a low metallicity mid-to-early M dwarf, although further observations are required for the metallicity to be conclusive. This is the fifth sub-Jupiter-mass (0.2 < m(p)/M-Jup < 1) microlensing planet around an M dwarf with the mass well constrained. The relatively rich harvest of sub-Jupiters around M dwarfs is contrasted with a possible paucity of similar to 1-2 Jupiter-mass planets around the same type of star, which can be explained by the planetary formation process in the core-accretion scheme. C1 [Fukui, A.] Natl Inst Nat Sci, Natl Astron Observ Japan, Okayama Astrophys Observ, Kamogatacho, Okayama 7190232, Japan. [Sumi, T.; Koshimoto, N.] Osaka Univ, Grad Sch Sci, Dept Earth & Space Sci, Toyonaka, Osaka 5600043, Japan. [Bennett, D. P.; Suzuki, D.; Bhattacharya, A.] Univ Notre Dame, Dept Phys, Notre Dame, IN 46556 USA. [Bond, I. A.; Ling, C. H.] Massey Univ, Inst Informat & Math Sci, Auckland, New Zealand. [Abe, F.; Itow, Y.; Masuda, K.; Matsubara, Y.; Muraki, Y.] Nagoya Univ, Solar Terr Environm Lab, Nagoya, Aichi 4648601, Japan. [Freeman, M.; Rattenbury, N.] Univ Auckland, Dept Phys, Auckland, New Zealand. [Sullivan, D. J.] Victoria Univ, Sch Chem & Phys Sci, Wellington, New Zealand. [Ohnishi, K.] Nagano Natl Coll Technol, Nagano 3818550, Japan. [Philpott, L. C.] Univ British Columbia, Dept Earth Ocean & Atmospher Sci, Vancouver, BC V6T 1Z4, Canada. [Saito, T.] Tokyo Metropolitan Coll Ind Technol, Tokyo 1168523, Japan. [Tristram, P. J.] Mt John Univ Observ, Lake Tekapo 8770, New Zealand. [Yonehara, A.] Kyoto Sangyo Univ, Dept Phys, Fac Sci, Kita Ku, Kyoto, Kyoto 6038555, Japan. [Gould, A.; Gaudi, B. S.; Kavka, A.; Pogge, R. W.; Yee, J. C.; Poleski, R.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. [Han, C.; Choi, J. -Y.; Hwang, K. -H.; Park, H.; Shin, I-G.] Chungbuk Natl Univ, Inst Astrophys, Dept Phys, Cheongju 371763, South Korea. [Christie, G. W.; Natusch, T.; Ngan, H.] Auckland Observ, Auckland, New Zealand. [DePoy, D. L.] Texas A&M Univ, Dept Phys, College Stn, TX 77843 USA. [Dong, Subo] Peking Univ, Kavli Inst Astron & Astrophys, Beijing 100871, Peoples R China. [Drummond, J.] Possum Observ, Patutahi, New Zealand. [Lee, C. -U.] Korea Astron & Space Sci Inst, Taejon 305348, South Korea. [McCormick, J.] Farm Cove Observ, Ctr Backyard Astrophys, Auckland, New Zealand. [Natusch, T.] AUT Univ, Auckland, New Zealand. [Tan, T. -G.] Perth Exoplanet Survey Telescope, Perth, WA, Australia. [Yee, J. C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Udalski, A.; Szymanski, M. K.; Pietrzynski, G.; Soszynski, I.; Poleski, R.; Kozlowski, S.; Pietrukowicz, P.; Ulaczyk, K.; Wyrzykowski, L.] Univ Warsaw Observ, PL-00478 Warsaw, Poland. [Beaulieu, J. -P.; Batista, V.] Univ Paris 06, Inst Astrophys Paris, CNRS, UMR7095, F-75014 Paris, France. [Street, R. A.; Tsapras, Y.] Las Cumbres Observ, Global Telescope Network, Goleta, CA 93117 USA. [Tsapras, Y.] Univ Heidelberg ZAH, Zentrum Astron, Astron Rechen Inst, D-69120 Heidelberg, Germany. [Tsapras, Y.] Queen Mary Univ London, Sch Phys & Astron, London E1 4NS, England. [Bramich, D. M.] Qatar Fdn, Qatar Environm & Energy Res Inst, Doha, Qatar. [Browne, P.; Dominik, M.; Horne, K.] Univ St Andrews, Sch Phys & Astron, SUPA, St Andrews KY16 9SS, Fife, Scotland. [Hundertmark, M.] Univ Copenhagen, Niels Bohr Inst, DK-2100 Copenhagen O, Denmark. [Hundertmark, M.] Univ Copenhagen, Nat Hist Museum, Ctr Star & Planet Format, DK-1350 Copenhagen K, Denmark. [Ipatov, S.] Russian Acad Sci, Vernadsky Inst Geochem & Analyt Chem, Moscow 119991, Russia. [Ipatov, S.] Russian Acad Sci, Space Res Inst, Moscow 119991, Russia. [Kains, N.] European So Observ, D-85748 Garching, Germany. [Kains, N.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Snodgrass, C.] Open Univ, Dept Phys Sci, Planetary & Space Sci, Milton Keynes MK7 6AA, Bucks, England. [Snodgrass, C.] Max Planck Inst Solar Syst Res, D-37077 Gottingen, Germany. [Steele, I. A.] Liverpool John Moores Univ, Astrophys Res Inst, Liverpool L3 5RF, Merseyside, England. RP Fukui, A (reprint author), Natl Inst Nat Sci, Natl Astron Observ Japan, Okayama Astrophys Observ, 3037-5 Ooaza Honjyo, Kamogatacho, Okayama 7190232, Japan. EM gould@astronomy.ohio-state.edu; gwchristie@christie.org.nz; depoy@physics.tamu.edu; farmcoveobs@xtra.co.nz; tim.natusch@aut.ac.nz RI Hundertmark, Markus/C-6190-2015; Watanabe, Makoto/E-3667-2016; Kozlowski, Szymon/G-4799-2013; OI Hundertmark, Markus/0000-0003-0961-5231; Watanabe, Makoto/0000-0002-3656-4081; Kozlowski, Szymon/0000-0003-4084-880X; Dominik, Martin/0000-0002-3202-0343; Tan, Thiam-Guan/0000-0001-5603-6895; Snodgrass, Colin/0000-0001-9328-2905 FU Astrobiology Project of the Center for Novel Science Initiatives (CNSI), National Institutes of Natural Sciences (NINS) [AB261005]; JSPS [JSPS23103002, JSPS24253004, JSPS26247023]; Creative Research Initiative Program of National Research Foundation of Korea [2009-0081561]; "Strategic Priority Research Program-The Emergence of Cosmological Structures" of the Chinese Academy of Sciences [09000000]; National Science Centre, Poland [MAESTRO 2014/14/A/ST9/00121]; European Union [268421]; Qatar Foundation from QNRF grant [NPRP-09-476-1-078]; [JSPS25103508]; [23340064] FX This paper is based in part on data collected at Subaru Telescope, which is operated by the National Astronomical Observatory of Japan. A.F. thanks Oscar A. Gonzalez for kindly providing VVV data. A.F. was supported by the Astrobiology Project of the Center for Novel Science Initiatives (CNSI), National Institutes of Natural Sciences (NINS; Grant Number AB261005). T.S. acknowledges the financial support from the JSPS, JSPS23103002, JSPS24253004, and JSPS26247023. The MOA project is supported by grants JSPS25103508 and 23340064. NJR is a Royal Society of New Zealand Rutherford Discovery Fellow. Work by C.H. was supported by Creative Research Initiative Program (2009-0081561) of National Research Foundation of Korea. S.D. is supported by "the Strategic Priority Research Program-The Emergence of Cosmological Structures" of the Chinese Academy of Sciences (grant No. 09000000). The OGLE project has received funding from the National Science Centre, Poland, grant MAESTRO 2014/14/A/ST9/00121 to A.U. C.S. received funding from the European Union Seventh Framework Programme (FP7/2007-2013) under grant agreement No. 268421. K.A., D.M.B., M.D., K.H., M.H., C.L., C.S., R.A.S., and Y.T. would like to thank the Qatar Foundation for support from QNRF grant NPRP-09-476-1-078. NR 69 TC 10 Z9 10 U1 0 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD AUG 10 PY 2015 VL 809 IS 1 AR 74 DI 10.1088/0004-637X/809/1/74 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CR9DN UT WOS:000361653500074 ER PT J AU Gopalan, G Vrtilek, SD Bornn, L AF Gopalan, Giri Vrtilek, Saeqa Dil Bornn, Luke TI CLASSIFYING X-RAY BINARIES: A PROBABILISTIC APPROACH SO ASTROPHYSICAL JOURNAL LA English DT Article DE methods: data analysis; methods: statistical; pulsars: general; stars: black holes; stars: neutron; X-rays: binaries ID LINEAR ALGEBRA; PERFORMANCE; MISSION; CATALOG AB In X-ray binary star systems consisting of a compact object that accretes material from an orbiting secondary star, there is no straightforward means to decide whether the compact object is a black hole or a neutron star. To assist in this process, we develop a Bayesian statistical model that makes use of the fact that X-ray binary systems appear to cluster based on their compact object type when viewed from a three-dimensional coordinate system derived from X-ray spectral data where the first coordinate is the ratio of counts in the mid-to low-energy band (color 1), the second coordinate is the ratio of counts in the high-to low-energy band (color 2), and the third coordinate is the sum of counts in all three bands. We use this model to estimate the probabilities of an X-ray binary system containing a black hole, non-pulsing neutron star, or pulsing neutron star. In particular, we utilize a latent variable model in which the latent variables follow a Gaussian process prior distribution, and hence we are able to induce the spatial correlation which we believe exists between systems of the same type. The utility of this approach is demonstrated by the accurate prediction of system types using Rossi X-ray Timing Explorer All Sky Monitor data, but it is not flawless. In particular, non-pulsing neutron systems containing "bursters" that are close to the boundary demarcating systems containing black holes tend to be classified as black hole systems. As a byproduct of our analyses, we provide the astronomer with the public R code which can be used to predict the compact object type of XRBs given training data. C1 [Gopalan, Giri; Bornn, Luke] Harvard Univ, Dept Stat, Cambridge, MA 02138 USA. [Vrtilek, Saeqa Dil] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Bornn, Luke] Simon Fraser Univ, Dept Stat & Actuarial Sci, Burnaby, BC V5A 1S6, Canada. RP Gopalan, G (reprint author), Harvard Univ, Dept Stat, One Oxford St, Cambridge, MA 02138 USA. FU Smithsonian Institution CGPS grant FX We acknowledge the Harvard ICHASC for their helpful feedback. Additionally, G.G. and S.D.V. acknowledge partial support through a Smithsonian Institution CGPS grant to SDV. NR 27 TC 0 Z9 0 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD AUG 10 PY 2015 VL 809 IS 1 AR 40 DI 10.1088/0004-637X/809/1/40 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CR9DN UT WOS:000361653500040 ER PT J AU Greiner, J Fox, DB Schady, P Kruhler, T Trenti, M Cikota, A Bolmer, J Elliott, J Delvaux, C Perna, R Afonso, P Kann, DA Klose, S Savaglio, S Schmidl, S Schweyer, T Tanga, M Varela, K AF Greiner, J. Fox, D. B. Schady, P. Kruehler, T. Trenti, M. Cikota, A. Bolmer, J. Elliott, J. Delvaux, C. Perna, R. Afonso, P. Kann, D. A. Klose, S. Savaglio, S. Schmidl, S. Schweyer, T. Tanga, M. Varela, K. TI GAMMA-RAY BURSTS TRACE UV METRICS OF STAR FORMATION OVER 3 < z < 5 SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology: observations; galaxies: high-redshift; galaxies: luminosity function; mass function; galaxies: star formation; gamma-ray burst: general ID MASS-METALLICITY RELATION; LY-ALPHA EMITTERS; GALAXY LUMINOSITY FUNCTION; DEEP FIELD CAMPAIGN; GRB HOST GALAXIES; APPROXIMATE-TO 3; FORMING GALAXIES; OPTICAL AFTERGLOW; FORMATION RATES; SPITZER OBSERVATIONS AB We present the first uniform treatment of long duration gamma-ray burst (GRB) host galaxy detections and upper limits over the redshift range 3 < z < 5, a key epoch for observational and theoretical efforts to understand the processes, environments, and consequences of early cosmic star formation (SF). We contribute deep imaging observations of 13 GRB positions yielding the discovery of 8 new host galaxies. We use this data set in tandem with previously published observations of 31 further GRB positions to estimate or constrain the host galaxy rest-frame ultraviolet (UV; lambda = 1600 angstrom) absolute magnitudes M-UV. We then use the combined set of 44 M-UV estimates and limits to construct the M-UV luminosity function (LF) for GRB host galaxies over 3 < z < 5 and compare it to expectations from Lyman break galaxy (LBG) photometric surveys with the Hubble Space Telescope. Adopting standard prescriptions for the luminosity dependence of galaxy dust obscuration (and hence, total SF rate), we find that our LF is compatible with LBG observations over a factor of 600x in host luminosity, from M-UV = -22.5 mag to >-15.6 mag, and with extrapolations of the assumed Schechter-type LF well beyond this range. We review proposed astrophysical and observational biases for our sample, and find that they are for the most part minimal. We therefore conclude, as the simplest interpretation of our results, that GRBs successfully trace UV metrics of cosmic SF over the range 3 < z < 5. Our findings suggest that GRBs provide an accurate picture of star formation processes from z approximate to 3 out to the highest redshifts. C1 [Greiner, J.; Schady, P.; Bolmer, J.; Elliott, J.; Delvaux, C.; Savaglio, S.; Schweyer, T.; Tanga, M.; Varela, K.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Greiner, J.] Tech Univ Munich, Excellence Cluster Universe, D-85748 Garching, Germany. [Fox, D. B.] Penn State Univ, Dept Astron & Astrophys, Ctr Theoret & Observat Cosmol, University Pk, PA 16802 USA. [Fox, D. B.] Penn State Univ, Ctr Particle & Gravitat Astrophys, University Pk, PA 16802 USA. [Kruehler, T.] European So Observ, Santiago 19, Chile. [Trenti, M.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Trenti, M.] Univ Cambridge, Kavli Inst Cosmol, Cambridge CB3 0HA, England. [Trenti, M.] Univ Melbourne, Sch Phys, Melbourne, Vic 3010, Australia. [Cikota, A.] Univ Innsbruck, Inst Astro & Teilchenphys, A-6020 Innsbruck, Austria. [Bolmer, J.; Schweyer, T.] Tech Univ Munich, Dept Phys, D-85748 Garching, Germany. [Elliott, J.] Harvard Smithsonian Ctr Astrophys, Astrophys Data Syst, Cambridge, MA 02138 USA. [Perna, R.] SUNY Stony Brook, Dept Phys & Astron, Stony Brook, NY 11794 USA. [Afonso, P.] Amer River Coll, Dept Phys & Astron, Sacramento, CA 95841 USA. [Kann, D. A.; Klose, S.; Schmidl, S.] Thuringer Landessternwarte Tautenburg, D-07778 Tautenburg, Germany. [Savaglio, S.] Univ Calabria, I-87036 Arcavacata Di Rende, Italy. RP Greiner, J (reprint author), Max Planck Inst Extraterr Phys, Giessenbachstr, D-85748 Garching, Germany. EM jcg@mpe.mpg.de; dfox@psu.edu; pschady@mpe.mpg.de; tkruehle@eso.org; michele.trenti@unimelb.edu.au; aleksandar.cikota@student.uibk.ac.at; jan@bolmer.de; jonathan.elliott@cfa.harvard.edu; delvaux@mpe.mpg.de; rosalba.perna@stonybrook.edu; afonsop@arc.losrios.edu; klose@tls-tautenburg.de; sandra.savaglio@googlemail.com; schmidl@tls-tautenburg.de; mohit@mpe.mpg.de; kvarela@mpe.mpg.de OI Trenti, Michele/0000-0001-9391-305X; Savaglio, Sandra/0000-0003-2354-3238 FU Sofja Kovalevskaja Award from the Alexander von Humboldt Foundation Germany; NSF [AST 1414246, HST-GO-13831.011-A]; DFG [KI 766/16-1, SA 2001/2-1]; Thuringer Ministerium fur Bildung, Wissenschaft und Kultur [FKZ 12010-514]; Bundesministerium fur Wirtschaft and Technologie through DLR (Deutsches Zentrum fur Luft- und Raumfahrt e.V.) [FKZ 50 OR 1211]; EXTraS; European Union [607452]; Leibniz-Prize (DFG) [HA 1850/28-1] FX The authors acknowledge astrostatistical consulting support from E. Feigelson. D.B.F. expresses appreciation to MPE Directors K. Nandra and R. Bender for administrative support of his sabbatical stay at MPE, where this collaboration was initiated. P.S. and M.T. acknowledge support through the Sofja Kovalevskaja Award to P. Schady from the Alexander von Humboldt Foundation Germany. R.P. acknowledges co-funding through NSF grant No. AST 1414246 and HST-GO-13831.011-A.S.K. acknowledges support by DFG grant KI 766/16-1 and SSc support by the Thuringer Ministerium fur Bildung, Wissenschaft und Kultur under FKZ 12010-514. S.Sa. acknowledges support from the Bundesministerium fur Wirtschaft and Technologie through DLR (Deutsches Zentrum fur Luft- und Raumfahrt e.V.) FKZ 50 OR 1211. K.V. acknowledges support by DFG grant SA 2001/2-1, and C.D. acknowledges support through EXTraS, funded from the European Union's Seventh Framework Programme for research, technological development and demonstration under grant agreement No. 607452. A.C. is grateful for support of his visit to MPE Garching. Partial funding for GROND (hardware and personnel) was generously granted from the Leibniz-Prize to Prof. G. Hasinger (DFG grant HA 1850/28-1). NR 125 TC 14 Z9 14 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD AUG 10 PY 2015 VL 809 IS 1 AR 76 DI 10.1088/0004-637X/809/1/76 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CR9DN UT WOS:000361653500076 ER PT J AU MacGregor, MA Wilner, DJ Andrews, SM Lestrade, JF Maddison, S AF MacGregor, Meredith A. Wilner, David J. Andrews, Sean M. Lestrade, Jean-Franois Maddison, Sarah TI THE EPSILON ERIDANI SYSTEM RESOLVED BY MILLIMETER INTERFEROMETRY SO ASTROPHYSICAL JOURNAL LA English DT Article DE circumstellar matter; stars: individual (epsilon Eridani); submillimeter: planetary systems ID MAIN-SEQUENCE STARS; ELEMENT-OF ERIDANI; YOUNG SOLAR-SYSTEM; DEBRIS DISK; ALMA OBSERVATIONS; SUBMILLIMETER GALAXIES; COLLISIONAL CASCADES; ALPHA CENTAURI; KUIPER-BELT; PLANET AB We present observations of. Eridani from the Submillimeter Array (SMA) at 1.3 mm and from the Australia Telescope Compact Array at 7 mm that reach an angular resolution of similar to 4 '' (13 AU). These first millimeter interferometer observations of epsilon Eridani, which hosts the closest debris disk to the Sun, reveal two distinct emission components: (1) the well-known outer dust belt, which, although patchy, is clearly resolved in the radial direction, and (2) an unresolved source coincident with the position of the star. We use direct model-fitting of the millimeter visibilities to constrain the basic properties of these two components. A simple Gaussian shape for the outer belt fit to the SMA data results in a radial location of 64.4(-3.0)(+2.4) AU and FWHM of 20.2(-8.2)(+6.0) AU (fractional width Delta R/R = 0.3). Similar results are obtained taking a power law radial emission profile for the belt, though the power law index cannot be usefully constrained. Within the noise obtained (0.2 mJy beam(-1)), these data are consistent with an axisymmetric belt model and show no significant azimuthal structure that might be introduced by unseen planets in the system. These data also limit any stellocentric offset of the belt to <9 AU, which disfavors the presence of giant planets on highly eccentric (>0.1) and wide (10's of AU) orbits. The flux density of the unresolved central component exceeds predictions for the stellar photosphere at these long wavelengths, by a marginally significant amount at 1.3 mm but by a factor of a few at 7 mm (with brightness temperature 13000 +/- 1600 K for a source size of the optical stellar radius). We attribute this excess emission to ionized plasma from a stellar corona or chromosphere. C1 [MacGregor, Meredith A.; Wilner, David J.; Andrews, Sean M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Lestrade, Jean-Franois] CNRS, LERMA, Observ Paris, F-75014 Paris, France. [Maddison, Sarah] Swinburne Univ, Ctr Astrophys & Supercomp, Melbourne, Vic, Australia. RP MacGregor, MA (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM mmacgregor@cfa.harvard.edu OI MacGregor, Meredith/0000-0001-7891-8143 FU National Science Foundation Graduate Research Fellowship [DGE1144152]; Swinburne Centre for Astrophysics Supercomputing; Universite Claude Bernard Lyon 1; Smithsonian Institution; Academia Sinica FX M.A.M acknowledges support from a National Science Foundation Graduate Research Fellowship (DGE1144152) and from the Swinburne Centre for Astrophysics & Supercomputing. D.J.W. thanks the Swinburne Visiting Researcher Scheme. S.T.M. acknowledges the support of the visiting professorship scheme from the Universite Claude Bernard Lyon 1. The Submillimeter Array is a joint project between the Smithsonian Astrophysical Observatory and the Academia Sinica Institute of Astronomy and Astrophysics and is funded by the Smithsonian Institution and the Academia Sinica. We thank Mark Gurwell and Scott Paine for discussions about the Submillimeter Array primary beam shape. NR 53 TC 8 Z9 8 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD AUG 10 PY 2015 VL 809 IS 1 AR 47 DI 10.1088/0004-637X/809/1/47 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CR9DN UT WOS:000361653500047 ER PT J AU Montet, BT Morton, TD Foreman-Mackey, D Johnson, JA Hogg, DW Bowler, BP Latham, DW Bieryla, A Mann, AW AF Montet, Benjamin T. Morton, Timothy D. Foreman-Mackey, Daniel Johnson, John Asher Hogg, David W. Bowler, Brendan P. Latham, David W. Bieryla, Allyson Mann, Andrew W. TI STELLAR AND PLANETARY PROPERTIES OF K2 CAMPAIGN 1 CANDIDATES AND VALIDATION OF 17 PLANETS, INCLUDING A PLANET RECEIVING EARTH-LIKE INSOLATION SO ASTROPHYSICAL JOURNAL LA English DT Article DE catalogs; planetary systems; planets and satellites: detection; stars: fundamental parameters ID INTEGRAL-FIELD SPECTROGRAPH; FALSE-POSITIVE RATE; DIGITAL SKY SURVEY; M DWARFS; ADAPTIVE OPTICS; LIGHT CURVES; HOST-STARS; KEPLER; COOL; SYSTEM AB The extended Kepler mission, K2, is now providing photometry of new fields every three months in a search for transiting planets. In a recent study, Foreman-Mackey and collaborators presented a list of 36 planet candidates orbiting 31 stars in K2 Campaign 1. In this contribution, we present stellar and planetary properties for all systems. We combine ground-based seeing-limited survey data and adaptive optics imaging with an automated transit analysis scheme to validate 21 candidates as planets, 17 for the first time, and identify 6 candidates as likely false positives. Of particular interest is K2-18 (EPIC 201912552), a bright (K = 8.9) M2.8 dwarf hosting a 2.23 +/- 0.25 R-circle plus planet with T-eq = 272 +/- 15 K and an orbital period of 33 days. We also present two new open-source software packages which enable this analysis. The first, isochrones, is a flexible tool for fitting theoretical stellar models to observational data to determine stellar properties using a nested sampling scheme to capture the multimodal nature of the posterior distributions of the physical parameters of stars that may plausibly be evolved. The second is vespa, a new general-purpose procedure to calculate false positive probabilities and statistically validate transiting exoplanets. C1 [Montet, Benjamin T.; Bowler, Brendan P.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA. [Montet, Benjamin T.; Johnson, John Asher; Latham, David W.; Bieryla, Allyson] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Morton, Timothy D.] Princeton Univ, Dept Astrophys, Princeton, NJ 08544 USA. [Foreman-Mackey, Daniel; Hogg, David W.] NYU, Dept Phys, Ctr Cosmol & Particle Phys, New York, NY 10003 USA. [Foreman-Mackey, Daniel; Hogg, David W.] NYU, Ctr Data Sci, New York, NY 10003 USA. [Hogg, David W.] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Mann, Andrew W.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA. RP Montet, BT (reprint author), CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA. EM btm@astro.caltech.edu OI Montet, Benjamin/0000-0001-7516-8308; Latham, David/0000-0001-9911-7388 FU NASA [NAS5-26555]; NASA Office of Space Science [NNX13AC07G]; NASA Science Mission directorate; Alfred P. Sloan Foundation; National Science Foundation; U.S. Department of Energy Office of Science; National Science Foundation Graduate Research Fellowship [DGE-1144469]; David and Lucile Packard Foundation; National Science Foundation [IIS-1124794]; National Aeronautics and Space Administration [NNX12AI50G, NNX14AE11G]; Moore-Sloan Data Science Environment at NYU; University of Arizona; Brazilian Participation Group; Brookhaven National Laboratory; Carnegie Mellon University; University of Florida; French Participation Group; German Participation Group; Harvard University; Instituto de Astrofisica de Canarias; Michigan State/Notre Dame/JINA Participation Group; Johns Hopkins University; Lawrence Berkeley National Laboratory; Max Planck Institute for Astrophysics; Max Planck Institute for Extraterrestrial Physics; New Mexico State University; New York University; Ohio State University; Pennsylvania State University; University of Portsmouth; Princeton University; Spanish Participation Group; University of Tokyo; University of Utah; Vanderbilt University; University of Virginia; University of Washington; Yale University FX We thank Roberto Sanchis-Ojeda (Berkeley), Dan Huber (Sydney) and Jeff Coughlin (SETI) for conversations and suggestions which improved the quality of this manuscript. We also thank Keivan Stassun (Vanderbilt) for his insights into stellar parameters and the rate of subgiant contamination for both Kepler and K2, which significantly improved this work. We thank the anonymous referee for their comments and suggestions. We are grateful to the entire Kepler team, past and present. Their tireless efforts were all essential to the tremendous success of the mission and the successes of K2 present and future. Some of the data presented in this paper were obtained from the Mikulski Archive for Space Telescopes (MAST). STScI is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555. for MAST for non-HST data is provided by the NASA Office of Space Science via grant NNX13AC07G and by other grants and contracts. This paper includes data collected by the Kepler mission. Funding for the Kepler mission is provided by the NASA Science Mission directorate. This paper includes data collected by the Sloan Digital Sky Survey. 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, 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. B.T.M. is supported by the National Science Foundation Graduate Research Fellowship under Grant No. DGE-1144469. J.A.J. is supported by generous grants from the David and Lucile Packard Foundation and the Alfred P. Sloan Foundation. D.F. M. and D.W.H. were partially supported by the National Science Foundation (grant IIS-1124794), the National Aeronautics and Space Administration (grant NNX12AI50G), and the Moore-Sloan Data Science Environment at NYU. T. D. M. is supported by the National Aeronautics and Space Administration (grant NNX14AE11G). NR 73 TC 21 Z9 21 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD AUG 10 PY 2015 VL 809 IS 1 AR 25 DI 10.1088/0004-637X/809/1/25 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CR9DN UT WOS:000361653500025 ER PT J AU Oronsaye, SI Ord, SM Bhat, NDR Tremblay, SE McSweeney, SJ Tingay, SJ van Straten, W Jameson, A Bernardi, G Bowman, JD Briggs, F Cappallo, RJ Deshpande, AA Greenhill, LJ Hazelton, BJ Johnston-Hollitt, M Kaplan, DL Lonsdale, CJ McWhirter, SR Mitchell, DA Morales, MF Morgan, E Oberoi, D Prabu, T Shankar, NU Srivani, KS Subrahmanyan, R Wayth, RB Webster, RL Williams, A Williams, CL AF Oronsaye, S. I. Ord, S. M. Bhat, N. D. R. Tremblay, S. E. McSweeney, S. J. Tingay, S. J. van Straten, W. Jameson, A. Bernardi, G. Bowman, J. D. Briggs, F. Cappallo, R. J. Deshpande, A. A. Greenhill, L. J. Hazelton, B. J. Johnston-Hollitt, M. Kaplan, D. L. Lonsdale, C. J. McWhirter, S. R. Mitchell, D. A. Morales, M. F. Morgan, E. Oberoi, D. Prabu, T. Shankar, N. Udaya Srivani, K. S. Subrahmanyan, R. Wayth, R. B. Webster, R. L. Williams, A. Williams, C. L. TI SIMULTANEOUS OBSERVATIONS OF GIANT PULSES FROM THE CRAB PULSAR, WITH THE MURCHISON WIDEFIELD ARRAY AND PARKES RADIO TELESCOPE: IMPLICATIONS FOR THE GIANT PULSE EMISSION MECHANISM SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM: individual objects (Crab Nebula); ISM: structure; pulsars: general; pulsars: individual (Crab pulsar); scattering ID NEBULA PULSAR; INTERSTELLAR SCINTILLATION; STATISTICAL PROPERTIES; NP 0532; UNIVERSE; SCATTERING; SPECTRA; VARIABILITY; FREQUENCIES; DISPERSION AB We report on observations of giant pulses from the Crab pulsar performed simultaneously with the Parkes radio telescope and the incoherent combination of the Murchison Widefield Array (MWA) antenna tiles. The observations were performed over a duration of approximately one hour at a center frequency of 1382 MHz with 340 MHz bandwidth at Parkes, and at a center frequency of 193 MHz with 15 MHz bandwidth at the MWA. Our analysis has led to the detection of 55 giant pulses at the MWA and 2075 at Parkes above a threshold of 3.5 sigma and 6.5 sigma, respectively. We detected 51% of the MWA giant pulses at the Parkes radio telescope, with spectral indices in the range of -3.6 > alpha > -4.9 (S-nu alpha nu(alpha)). We present a Monte Carlo analysis supporting the conjecture that the giant pulse emission in the Crab is intrinsically broadband, the less than 100% correlation being due to the relative sensitivities of the two instruments and the width of the spectral index distribution. Our observations are consistent with the hypothesis that the spectral index of giant pulses is drawn from normal distribution of standard deviation 0.6, but with a mean that displays an evolution with frequency from -3.00 at 1382 MHz, to -2.85 at 192 MHz. C1 [Oronsaye, S. I.; Ord, S. M.; Bhat, N. D. R.; Tremblay, S. E.; McSweeney, S. J.; Tingay, S. J.; Wayth, R. B.; Williams, A.] Curtin Univ, ICRAR, Bentley, WA 6102, Australia. [Oronsaye, S. I.; Ord, S. M.; Bhat, N. D. R.; Tremblay, S. E.; Tingay, S. J.; van Straten, W.; Jameson, A.; Mitchell, D. A.; Subrahmanyan, R.; Wayth, R. B.; Webster, R. L.] ARC Ctr Excellence All Sky Astrophys CAASTRO, Sydney, NSW, Australia. [van Straten, W.; Jameson, A.] Swinburne Univ Technol, Ctr Astrophys & Supercomp, Hawthorn, Vic 3122, Australia. [Bernardi, G.] SKASA, ZA-7405 Pinelands, South Africa. [Bernardi, G.; Greenhill, L. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Bernardi, G.] Rhodes Univ, Dept Phys & Elect, ZA-6140 Grahamstown, South Africa. [Bowman, J. D.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA. [Briggs, F.] Australian Natl Univ, Res Sch Astron & Astrophys, Canberra, ACT 2611, Australia. [Cappallo, R. J.; Lonsdale, C. J.; McWhirter, S. R.] MIT, Haystack Observ, Westford, MA 01886 USA. [Deshpande, A. A.; Prabu, T.; Shankar, N. Udaya; Srivani, K. S.; Subrahmanyan, R.] Raman Res Inst, Bangalore 560080, Karnataka, India. [Hazelton, B. J.; Morales, M. F.] Univ Washington, Dept Phys, Seattle, WA 98195 USA. [Johnston-Hollitt, M.] Victoria Univ Wellington, Sch Chem & Phys Sci, Wellington 6140, New Zealand. [Kaplan, D. L.] Univ Wisconsin, Dept Phys, Milwaukee, WI 53201 USA. [Mitchell, D. A.] CASS, Epping, NSW 1710, Australia. [Morgan, E.; Williams, C. L.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Oberoi, D.] Tata Inst Fundamental Res, Natl Ctr Radio Astrophys, Pune 411007, Maharashtra, India. [Webster, R. L.] Univ Melbourne, Sch Phys, Parkville, Vic 3010, Australia. RP Oronsaye, SI (reprint author), Curtin Univ, ICRAR, Bentley, WA 6102, Australia. RI Deshpande, Avinash/D-4868-2012; Wayth, Randall/B-2444-2013; Subrahmanyan, Ravi/D-4889-2012; M, Manjunath/N-4000-2014; Udayashankar , N/D-4901-2012; OI Wayth, Randall/0000-0002-6995-4131; M, Manjunath/0000-0001-8710-0730; van Straten, Willem/0000-0003-2519-7375 FU U.S. National Science Foundation [AST-0457585, PHY-0835713, CAREER-0847753, AST-0908884]; Australian Research Council [LE0775621, LE0882938]; U.S. Air Force Office of Scientific Research [FA9550-0510247]; Centre for All-sky Astrophysics (Australian Research Council Centre of Excellence) [CE110001020]; Smithsonian Astrophysical Observatory; MIT School of Science; Raman Research Institute; Australian National University; Victoria University of Wellington (New Zealand Ministry of Economic Development) [MED-E1799]; Australian Federal government via the Commonwealth Scientific and Industrial Research Organisation (CSIRO); National Collaborative Research Infrastructure Strategy; Education Investment Fund; Australia India Strategic Research Fund; Astronomy Australia Limited; NVIDIA at Harvard University; International Centre for Radio Astronomy Research (ICRAR); Joint Venture of Curtin University; University of Western Australia - Western Australian State government; Australian Research Council Centre of Excellence for All-sky Astrophysics (CAASTRO) [CE110001020]; Victoria University of Wellington (IBM Shared University Research Grant) FX We would like to thank Haydon Knight for useful contributions during the preparation of this paper. This scientific work makes use of the Murchison Radio-astronomy Observatory, operated by CSIRO. We acknowledge the Wajarri Yamatji people as the traditional owners of the Observatory site. Support for the MWA comes from the U.S. National Science Foundation (grants AST-0457585, PHY-0835713, CAREER-0847753, and AST-0908884), the Australian Research Council (LIEF grants LE0775621 and LE0882938), the U.S. Air Force Office of Scientific Research (grant FA9550-0510247), and the Centre for All-sky Astrophysics (an Australian Research Council Centre of Excellence funded by grant CE110001020). Support is also provided by the Smithsonian Astrophysical Observatory, the MIT School of Science, the Raman Research Institute, the Australian National University, and the Victoria University of Wellington (via grant MED-E1799 from the New Zealand Ministry of Economic Development and an IBM Shared University Research Grant). The Australian Federal government provides additional support via the Commonwealth Scientific and Industrial Research Organisation (CSIRO), National Collaborative Research Infrastructure Strategy, Education Investment Fund, and the Australia India Strategic Research Fund, and Astronomy Australia Limited, under contract to Curtin University. We acknowledge the iVEC Petabyte Data Store, the Initiative in Innovative Computing and the CUDA Center for Excellence sponsored by NVIDIA at Harvard University, and the International Centre for Radio Astronomy Research (ICRAR), a Joint Venture of Curtin University and The University of Western Australia, funded by the Western Australian State government. This research was conducted by the Australian Research Council Centre of Excellence for All-sky Astrophysics (CAASTRO), through project number CE110001020. NR 57 TC 5 Z9 5 U1 1 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD AUG 10 PY 2015 VL 809 IS 1 AR 51 DI 10.1088/0004-637X/809/1/51 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CR9DN UT WOS:000361653500051 ER PT J AU Osten, RA Wolk, SJ AF Osten, Rachel A. Wolk, Scott J. TI CONNECTING FLARES AND TRANSIENT MASS-LOSS EVENTS IN MAGNETICALLY ACTIVE STARS SO ASTROPHYSICAL JOURNAL LA English DT Article DE stars: activity; stars: flare; stars: late-type; stars: mass-loss ID EXTREME-ULTRAVIOLET-EXPLORER; X-RAY FLARES; ANGULAR-MOMENTUM LOSS; MAIN-SEQUENCE STARS; AD LEONIS; FREQUENCY-DISTRIBUTIONS; ENERGY PARTITION; STELLAR FLARES; ALPHA EMISSION; SOLAR-FLARES AB We explore the ramification of associating the energetics of extreme magnetic reconnection events with transient mass-loss in a stellar analogy with solar eruptive events. We establish energy partitions relative to the total bolometric radiated flare energy for different observed components of stellar flares and show that there is rough agreement for these values with solar flares. We apply an equipartition between the bolometric radiated flare energy and kinetic energy in an accompanying mass ejection, seen in solar eruptive events and expected from reconnection. This allows an integrated flare rate in a particular waveband to be used to estimate the amount of associated transient mass-loss. This approach is supported by a good correspondence between observational flare signatures on high flaring rate stars and the Sun, which suggests a common physical origin. If the frequent and extreme flares that young solar-like stars and low-mass stars experience are accompanied by transient mass-loss in the form of coronal mass ejections, then the cumulative effect of this mass-loss could be large. We find that for young solar-like stars and active M dwarfs, the total mass lost due to transient magnetic eruptions could have significant impacts on disk evolution, and thus planet formation, and also exoplanet habitability. C1 [Osten, Rachel A.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Wolk, Scott J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Osten, Rachel A.] Johns Hopkins Univ, Ctr Astrophys Sci, Baltimore, MD 21218 USA. RP Osten, RA (reprint author), Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA. EM osten@stsci.edu FU NASA (Chandra) [NAS8-03060] FX R.A.O. acknowledges the useful discussions which took place at the International Space Science Institute workshop on Energy Partition in Solar and Stellar Flares for helping to frame elements of the study. S.J.W. was supported by NASA contract NAS8-03060 (Chandra). NR 70 TC 9 Z9 9 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD AUG 10 PY 2015 VL 809 IS 1 AR 79 DI 10.1088/0004-637X/809/1/79 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CR9DN UT WOS:000361653500079 ER PT J AU Pober, JC Ali, ZS Parsons, AR McQuinn, M Aguirre, JE Bernardi, G Bradley, RF Carilli, CL Cheng, C DeBoer, DR Dexter, MR Furlanetto, SR Grobbelaar, J Horrell, J Jacobs, DC Klima, PJ Kohn, SA Liu, A MacMahon, DHE Maree, M Mesinger, A Moore, DF Razavi-Ghods, N Stefan, II Walbrugh, WP Walker, A Zheng, HX AF Pober, Jonathan C. Ali, Zaki S. Parsons, Aaron R. McQuinn, Matthew Aguirre, James E. Bernardi, Gianni Bradley, Richard F. Carilli, Chris L. Cheng, Carina DeBoer, David R. Dexter, Matthew R. Furlanetto, Steven R. Grobbelaar, Jasper Horrell, Jasper Jacobs, Daniel C. Klima, Patricia J. Kohn, Saul A. Liu, Adrian MacMahon, David H. E. Maree, Matthys Mesinger, Andrei Moore, David F. Razavi-Ghods, Nima Stefan, Irina I. Walbrugh, William P. Walker, Andre Zheng, Haoxuan TI PAPER-64 CONSTRAINTS ON REIONIZATION. II. THE TEMPERATURE OF THE z=8.4 INTERGALACTIC MEDIUM SO ASTROPHYSICAL JOURNAL LA English DT Article DE dark ages, reionization, first stars; galaxies: high-redshift; intergalactic medium ID STAR-FORMING GALAXIES; LY-ALPHA EMITTERS; MURCHISON-WIDEFIELD-ARRAY; FORMATION RATE INDICATOR; CM POWER SPECTRUM; X-RAY BINARIES; COSMIC REIONIZATION; 21-CM FLUCTUATIONS; REDSHIFT Z; EPOCH AB We present constraints on both the kinetic temperature of the intergalactic medium (IGM) at z = 8.4, and on models for heating the IGM at high-redshift with X-ray emission from the first collapsed objects. These constraints are derived using a semi-analytic method to explore the new measurements of the 21 cm power spectrum from the Donald C. Backer Precision Array for Probing the Epoch of Reionization (PAPER), which were presented in a companion paper, Ali et al. Twenty-one cm power spectra with amplitudes of hundreds of mK2 can be generically produced if the kinetic temperature of the IGM is significantly below the temperature of the cosmic microwave background (CMB); as such, the new results from PAPER place lower limits on the IGM temperature at z = 8.4. Allowing for the unknown ionization state of the IGM, our measurements find the IGM temperature to be above approximate to 5 K for neutral fractions between 10% and 85%, above approximate to 7 K for neutral fractions between 15% and 80%, or above approximate to 10 K for neutral fractions between 30% and 70%. We also calculate the heating of the IGM that would be provided by the observed high redshift galaxy population, and find that for most models, these galaxies are sufficient to bring the IGM temperature above our lower limits. However, there are significant ranges of parameter space that could produce a signal ruled out by the PAPER measurements; models with a steep drop-off in the star formation rate density at high redshifts or with relatively low values for the X-ray to star formation rate efficiency of high redshift galaxies are generally disfavored. The PAPER measurements are consistent with (but do not constrain) a hydrogen spin temperature above the CMB temperature, a situation which we find to be generally predicted if galaxies fainter than the current detection limits of optical/NIR surveys are included in calculations of X-ray heating. C1 [Pober, Jonathan C.] Univ Washington, Dept Phys, Seattle, WA 98195 USA. [Ali, Zaki S.; Parsons, Aaron R.; Cheng, Carina; Liu, Adrian] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Parsons, Aaron R.; DeBoer, David R.; Dexter, Matthew R.; MacMahon, David H. E.] Univ Calif Berkeley, Radio Astron Lab, Berkeley, CA 94720 USA. [McQuinn, Matthew] Univ Washington, Dept Astron, Seattle, WA 98195 USA. [Aguirre, James E.; Kohn, Saul A.; Moore, David F.] Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA. [Bernardi, Gianni; Grobbelaar, Jasper; Horrell, Jasper; Maree, Matthys; Walbrugh, William P.; Walker, Andre] SKA SA, Pinelands, South Africa. [Bernardi, Gianni] Rhodes Univ, Dept Phys & Elect, ZA-6140 Grahamstown, South Africa. [Bernardi, Gianni] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Bradley, Richard F.] Univ Virginia, Dept Elect & Comp Engn, Charlottesville, VA USA. [Bradley, Richard F.; Klima, Patricia J.] Natl Radio Astron Observ, Charlottesville, VA USA. [Bradley, Richard F.] Univ Virginia, Dept Astron, Charlottesville, VA 22903 USA. [Carilli, Chris L.] Natl Radio Astron Observ, Socorro, NM 87801 USA. [Carilli, Chris L.; Razavi-Ghods, Nima; Stefan, Irina I.] Univ Cambridge, Cavendish Lab, Cambridge CB3 0HE, England. [Furlanetto, Steven R.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA USA. [Jacobs, Daniel C.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ USA. [Liu, Adrian] Berkeley Ctr Cosmol Phys, Berkeley, CA USA. [Mesinger, Andrei] Scuola Normale Super Pisa, Pisa, Italy. [Zheng, Haoxuan] MIT, Dept Phys, Cambridge, MA 02139 USA. RP Pober, JC (reprint author), Univ Washington, Dept Phys, Seattle, WA 98195 USA. OI Pober, Jonathan/0000-0002-3492-0433 FU National Science Foundation (NSF) [0804508, 1129258, 1125558]; NSF [1302774, 1352519, 1401708]; Mount Cuba Astronomical Association FX PAPER is supported by grants from the National Science Foundation (NSF; awards 0804508, 1129258, and 1125558). J.C.P., A.R.P., and D.C.J. would like to acknowledge NSF support (awards 1302774, 1352519, and 1401708, respectively). J.E.A. would like to acknowledge a generous grant from the Mount Cuba Astronomical Association for computing resources. We graciously thank SKA-SA for onsite infrastructure and observing support. In addition we would like to thank our South African interns Monde Manzini and Ruvano Casper from Durban University of Technology (DUT), who helped build out the array from 32 antennas to the 64 antennas this analysis was based on. The authors would also like to thank Anson D'Aloisio, Adam Lidz, Jordan Mirocha, and Jonathan Pritchard for very helpful and fruitful conversations, Brant Robertson for providing the quantitative error contours in the R15 model, and our reviewer for helpful suggestions for better quantifying the effects of certain approximations in our work. NR 71 TC 23 Z9 23 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD AUG 10 PY 2015 VL 809 IS 1 AR 62 DI 10.1088/0004-637X/809/1/62 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CR9DN UT WOS:000361653500062 ER PT J AU Rugheimer, S Kaltenegger, L Segura, A Linsky, J Mohanty, S AF Rugheimer, S. Kaltenegger, L. Segura, A. Linsky, J. Mohanty, S. TI EFFECT OF UV RADIATION ON THE SPECTRAL FINGERPRINTS OF EARTH-LIKE PLANETS ORBITING M STARS SO ASTROPHYSICAL JOURNAL LA English DT Article DE astrobiology; planets and satellites: atmospheres; planets and satellites: terrestrial planets; stars: low-mass ID EXOPLANET HOST STARS; WEBB-SPACE-TELESCOPE; EXTRA-SOLAR PLANETS; DIGITAL SKY SURVEY; HIGH-LEVEL CLOUDS; K-BAND SPECTRA; M-DWARFS; HABITABLE ZONE; SUPER-EARTHS; MAGNETIC ACTIVITY AB We model the atmospheres and spectra of Earth-like planets orbiting the entire grid of M dwarfs for active and inactive stellar models with T-eff = 2300 K to T-eff = 3800 K and for six observed MUSCLES M dwarfs with UV radiation data. We set the Earth-like planets at the 1 AU equivalent distance and show spectra from the visible to IR (0.4-20 mu m) to compare detectability of features in different wavelength ranges with the. James Webb Space Telescope and other future ground- and spaced-based missions to characterize exo-Earths. We focus on the effect of UV activity levels on detectable atmospheric features that indicate habitability on Earth, namely, H2O, O-3, CH4, N2O, and CH3Cl. To observe signatures of life-O-2/O-3 in combination with reducing species like CH4-we find that early and active M dwarfs are the best targets of the M star grid for future telescopes. The O-2 spectral feature at 0.76 mu m is increasingly difficult to detect in reflected light of later M dwarfs owing to low stellar flux in that wavelength region. N2O, another biosignature detectable in the IR, builds up to observable concentrations in our planetary models around M dwarfs with low UV flux. CH3Cl could become detectable, depending on the depth of the overlapping N2O feature. We present a spectral database of Earth-like planets around cool stars for directly imaged planets as a framework for interpreting future light curves, direct imaging, and secondary eclipse measurements of the atmospheres of terrestrial planets in the habitable zone. to design and assess future telescope capabilities. C1 [Rugheimer, S.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Rugheimer, S.; Kaltenegger, L.] Cornell Univ, Carl Sagan Inst, Ithaca, NY 14853 USA. [Kaltenegger, L.] MPIA, D-69117 Heidelberg, Germany. [Segura, A.] Univ Nacl Autonoma Mexico, Inst Ciencias Nucl, Mexico City 04510, DF, Mexico. [Linsky, J.] Univ Colorado, JILA, Boulder, CO 80309 USA. [Linsky, J.] NIST, Boulder, CO 80309 USA. [Mohanty, S.] Univ London Imperial Coll Sci Technol & Med, Blackett Lab 1010, London SW7 2AZ, England. RP Rugheimer, S (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. OI Rugheimer, Sarah/0000-0003-1620-7658 FU DFG [ENP KA 3142/1-1]; Simons Foundation [290357]; NASA [NAS5-26555]; NASA Office of Space Science [NAG5-7584] FX We especially thank Andrew West and Evgenya L. Shkolnik for useful conversations about M dwarfs. We also would like to thank Kevin France for discussions concerning the MUSCLES database. This work has made use of the MUSCLES M dwarf UV radiation field database. We would also like to acknowledge support from DFG funding ENP KA 3142/1-1 and the Simons Foundation (290357, Kaltenegger).; The UV radiation field for AD Leo was 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 NAG5-7584 and by other grants and contracts. NR 93 TC 16 Z9 16 U1 5 U2 25 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD AUG 10 PY 2015 VL 809 IS 1 AR 57 DI 10.1088/0004-637X/809/1/57 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CR9DN UT WOS:000361653500057 ER PT J AU Sesar, B Bovy, J Bernard, EJ Caldwell, N Cohen, JG Fouesneau, M Johnson, CI Ness, M Ferguson, AMN Martin, NF Price-Whelan, AM Rix, HW Schlafly, EF Burgett, WS Chambers, KC Flewelling, H Hodapp, KW Kaiser, N Magnier, EA Platais, I Tonry, JL Waters, C Wyse, RFG AF Sesar, Branimir Bovy, Jo Bernard, Edouard J. Caldwell, Nelson Cohen, Judith G. Fouesneau, Morgan Johnson, Christian I. Ness, Melissa Ferguson, Annette M. N. Martin, Nicolas F. Price-Whelan, Adrian M. Rix, Hans-Walter Schlafly, Edward F. Burgett, William S. Chambers, Kenneth C. Flewelling, Heather Hodapp, Klaus W. Kaiser, Nick Magnier, Eugene A. Platais, Imants Tonry, John L. Waters, Christopher Wyse, Rosemary F. G. TI THE NATURE AND ORBIT OF THE OPHIUCHUS STREAM SO ASTROPHYSICAL JOURNAL LA English DT Article DE Galaxy: halo; Galaxy: kinematics and dynamics; Galaxy: structure; globular clusters: general ID DIGITAL SKY SURVEY; STELLAR STREAM; TIDAL STREAMS; PROPER-MOTION; GLOBULAR-CLUSTERS; ORPHAN STREAM; STAR-CLUSTERS; USNO-B; MILKY; CATALOG AB The Ophiuchus stream is a recently discovered stellar tidal stream in the Milky Way. We present high-quality spectroscopic data for 14 stream member stars obtained using the Keck and MMT telescopes. We confirm the stream as a fast moving (v(los) similar to 290 km s(-1)), kinematically cold group (sigma v(los) less than or similar to 1 km s(-1)) of alpha-enhanced and metal-poor stars ([alpha/Fe] similar to 0.4 dex, [Fe/H] similar to -2.0 dex). Using a probabilistic technique, we model the stream simultaneously in line-of-sight velocity, color-magnitude, coordinate, and proper motion space, and so determine its distribution in 6D phase-space. We find that the stream extends in distance from 7.5 to 9 kpc from the Sun; it is 50 times longer than wide, merely appearing highly foreshortened in projection. The analysis of the stellar population contained in the stream suggests that it is similar to 12 Gyr old, and that its initial stellar mass was similar to 2 x 10(4) M-circle dot (or at least greater than or similar to 7 x 10(3) M-circle dot). Assuming a fiducial Milky Way potential, we fit an orbit to the stream that matches the observed phase-space distribution, except for some tension in the proper motions: the stream has an orbital period of similar to 350 Myr, and is on a fairly eccentric orbit (e similar to 0.66) with a pericenter of similar to 3.5 kpc and an apocenter of similar to 17 kpc. The phase-space structure and stellar population of the stream show that its progenitor must have been a globular cluster that was disrupted only similar to 240 Myr ago. We do not detect any significant overdensity of stars along the stream that would indicate the presence of a progenitor, and conclude that the stream is all that is left of the progenitor. C1 [Sesar, Branimir; Fouesneau, Morgan; Ness, Melissa; Martin, Nicolas F.; Rix, Hans-Walter; Schlafly, Edward F.] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Bovy, Jo] Inst Adv Study, Princeton, NJ 08540 USA. [Bernard, Edouard J.; Ferguson, Annette M. N.] Univ Edinburgh, Inst Astron, SUPA, Royal Observ, Edinburgh EH9 3HJ, Midlothian, Scotland. [Caldwell, Nelson; Johnson, Christian I.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Cohen, Judith G.] CALTECH, Div Phys Math & Astron, Pasadena, CA 91125 USA. [Martin, Nicolas F.] Univ Strasbourg, CNRS, UMR 7550, Observ Astron Strasbourg, F-67000 Strasbourg, France. [Price-Whelan, Adrian M.] Columbia Univ, Dept Astron, New York, NY 10027 USA. [Burgett, William S.] GMTO Corp, Pasadena, CA 91101 USA. [Chambers, Kenneth C.; Flewelling, Heather; Hodapp, Klaus W.; Kaiser, Nick; Magnier, Eugene A.; Tonry, John L.; Waters, Christopher] Univ Hawaii Manoa, Inst Astron, Honolulu, HI 96822 USA. [Platais, Imants; Wyse, Rosemary F. G.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. RP Sesar, B (reprint author), Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany. EM bsesar@mpia.de OI Bernard, Edouard/0000-0002-8722-225X; Chambers, Kenneth /0000-0001-6965-7789; Schlafly, Edward Ford/0000-0002-3569-7421 FU European Research Council under the European Union [321035]; Clay Fellowship; National Aeronautics and Space Administration through the Planetary Science Division of the NASA Science Mission Directorate [NNX08AR22G]; National Science Foundation [AST-1238877, 11-44155]; W. M. Keck Foundation FX B.S. acknowledges funding from the European Research Council under the European Union's Seventh Framework Programme (FP 7) ERC Grant Agreement n. [321035]. C.I.J. gratefully acknowledges support from the Clay Fellowship, administered by the Smithsonian Astrophysical Observatory. A.P.W. is supported by a National Science Foundation Graduate Research Fellowship under Grant No. 11-44155. The Pan-STARRS1 Surveys (PS1) have been made possible through contributions by 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, the 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, the National Science Foundation Grant No. AST-1238877, the University of Maryland, Eotvos Lorand University (ELTE), and the Los Alamos National Laboratory. Some of the data presented herein were obtained at the W.M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California and the National Aeronautics and Space Administration. The Observatory was made possible by the generous financial support of the W. M. Keck Foundation. The authors 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. Observations reported here were obtained at the MMT Observatory, a joint facility of the Smithsonian Institution and the University of Arizona. NR 65 TC 6 Z9 6 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD AUG 10 PY 2015 VL 809 IS 1 AR 59 DI 10.1088/0004-637X/809/1/59 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CR9DN UT WOS:000361653500059 ER PT J AU Sullivan, PW Winn, JN Berta-Thompson, ZK Charbonneau, D Deming, D Dressing, CD Latham, DW Levine, AM McCullough, PR Morton, T Ricker, GR Vanderspek, R Woods, D AF Sullivan, Peter W. Winn, Joshua N. Berta-Thompson, Zachory K. Charbonneau, David Deming, Drake Dressing, Courtney D. Latham, David W. Levine, Alan M. McCullough, Peter R. Morton, Timothy Ricker, George R. Vanderspek, Roland Woods, Deborah TI THE TRANSITING EXOPLANET SURVEY SATELLITE: SIMULATIONS OF PLANET DETECTIONS AND ASTROPHYSICAL FALSE POSITIVES SO ASTROPHYSICAL JOURNAL LA English DT Article DE planets and satellites: detection; space vehicles: instruments; surveys ID INTERMEDIATE-MASS STARS; FINITE INTEGRATION TIME; MAIN-SEQUENCE STARS; LUMINOSITY FUNCTION; ECLIPSING BINARIES; PHOTOMETRIC SURVEYS; EXTRASOLAR PLANETS; SPACE-TELESCOPE; GALACTIC DISK; DATA RELEASE AB The Transiting Exoplanet Survey Satellite (TESS) is a NASA-sponsored Explorer mission that will perform a wide-field survey for planets that transit bright host stars. Here, we predict the properties of the transiting planets that TESS will detect along with the EB stars that produce false-positive photometric signals. The predictions are based on Monte Carlo simulations of the nearby population of stars, occurrence rates of planets derived from Kepler, and models for the photometric performance and sky coverage of the TESS cameras. We expect that TESS will find approximately 1700 transiting planets from 2 x 10(5) pre-selected target stars. This includes 556 planets smaller than twice the size of Earth, of which 419 are hosted by M dwarf stars and 137 are hosted by FGK dwarfs. Approximately 130 of the R < 2 R-circle plus planets will have host stars brighter than K-s = 9. Approximately 48 of the planets with R < 2 R-circle plus lie within or near the habitable zone (0.2 < S/S-circle plus < 2); between 2 and 7 such planets have host stars brighter than K-s = 9. We also expect approximately 1100 detections of planets with radii 2-4 R-circle plus, and 67 planets larger than 4 R-circle plus. Additional planets larger than 2 R-circle plus can be detected around stars that are not among the pre-selected target stars, because TESS will also deliver full-frame images at a 30-minute cadence. The planet detections are accompanied by over 1000 astrophysical false positives. We discuss how TESS data and ground-based observations can be used to distinguish the false positives from genuine planets. We also discuss the prospects for follow-up observations to measure the masses and atmospheres of the TESS planets. C1 [Sullivan, Peter W.; Winn, Joshua N.] MIT, Dept Phys, Cambridge, MA 02139 USA. [Sullivan, Peter W.; Winn, Joshua N.; Berta-Thompson, Zachory K.; Levine, Alan M.; Ricker, George R.; Vanderspek, Roland] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Charbonneau, David; Dressing, Courtney D.; Latham, David W.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Deming, Drake] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [McCullough, Peter R.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [McCullough, Peter R.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Morton, Timothy] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. [Woods, Deborah] MIT, Lincoln Lab, Lexington, MA 02420 USA. RP Sullivan, PW (reprint author), MIT, Dept Phys, 77 Massachusetts Ave, Cambridge, MA 02139 USA. OI Berta-Thompson, Zachory/0000-0002-3321-4924 FU National Aeronautics and Space Administration; National Science Foundation FX We are grateful to the referee, Scott Gaudi, for providing constructive criticism that has led to improvements in this paper. We thank the members of the TESS Science Team for their contributions to the mission. In particular, Jacob Bean, Tabetha Boyajian, Eric Gaidos, Daniel Huber, Geoffrey Marcy, Roberto Sanchis-Ojeda, and Keivan Stassun provided helpful comments on the manuscript, and discussions with Jon Jenkins helped inform our approach to the simulations. We acknowledge Anthony Smith, Kristin Clark, and Michael Chrisp at MIT-Lincoln Laboratory for their respective roles in the project management, systems engineering, and optical design for the TESS payload. In addition, Barry Burke and Vyshnavi Suntharalingam at MIT-LL provided useful input to the PSF model. We thank Leo Girardi for adding the TESS bandpass to the TRILEGAL simulation and for providing a perl script to facilitate the queries. We also thank Gibor Basri for sharing the stellar variability data from Kepler. This publication makes use of data products from the 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. NR 82 TC 39 Z9 39 U1 1 U2 16 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD AUG 10 PY 2015 VL 809 IS 1 AR 77 DI 10.1088/0004-637X/809/1/77 PG 29 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CR9DN UT WOS:000361653500077 ER PT J AU Valencic, LA Smith, RK AF Valencic, Lynne A. Smith, Randall K. TI INTERSTELLAR DUST PROPERTIES FROM A SURVEY OF X-RAY HALOS SO ASTROPHYSICAL JOURNAL LA English DT Article DE dust, extinction; X-rays: ISM ID COLOR-MAGNITUDE DIAGRAMS; GLOBULAR-CLUSTER SYSTEM; PULSAR 4U 1538-52; SOURCE CYGNUS X-2; OPTICAL COUNTERPART; NEUTRON-STAR; CENTAURUS X-3; BLACK-HOLE; METAL-RICH; GRS 1915+105 AB Interstellar dust grains produce X-ray halos around bright sources due to small-angle X-ray scattering. Numerous studies have examined these halos, but no systematic study has yet tested the available halo data against the large number of well-defined dust models in circulation. We have therefore obtained the largest sample to date of X-ray dust halos from XMM-Newton and Chandra, and fitted them with 14 commonly used dust grain models, including comparisons with the optical extinction, A(V), where available in the literature. Our main conclusions are summarized as follows. (1) Comparing A(V) with N-H values measured via X-ray spectral fits, we find a ratio of A(V)/N-H (10(21) cm(-2)) = 0.48 +/- 0.06, in agreement with previous work. (2) Out of 35 halos, 27 could be fit by one or more grain models, with the most successful models having maximum grain radius a(max) < 0.4 mu m and fewer large grains than the less successful models. This suggests that the diffuse ISM does not contain a signicant presence of grains with a(max) > 0.5 mu m. (3) Most halos were best fit assuming a single dust cloud dominated the scattering, rather than smoothly distributed dust along the sightline. (4) Eight sources could not be fit with the models considered here, most of which were along distant (d > 5 kpc) sight lines through the Galactic thin disk. (5) Some sight lines had halos with observed X-ray scattering optical depth tau(sca)/AV that were signicantly different than expected. This may result from an inhomogeneous dust distribution across the halo extraction area. C1 [Valencic, Lynne A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Valencic, Lynne A.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Smith, Randall K.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Valencic, LA (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM lynne.a.valencic@nasa.gov FU NASA [NNX10AE04G, NNX10AD10G]; Chandra grant [GO7-8142B] FX The authors thank the anonymous referee for many insightful comments that significantly improved this work. They also gratefully acknowledge helpful discussions with Eli Dwek and Fred Seward. Financial support for this work was made possible by NASA Grants NNX10AE04G and NNX10AD10G and Chandra grant GO7-8142B. NR 146 TC 5 Z9 5 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD AUG 10 PY 2015 VL 809 IS 1 AR 66 DI 10.1088/0004-637X/809/1/66 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CR9DN UT WOS:000361653500066 ER PT J AU Welsh, WF Orosz, JA Short, DR Cochran, WD Endl, M Brugamyer, E Haghighipour, N Buchhave, LA Doyle, LR Fabrycky, DC Hinse, TC Kane, SR Kostov, V Mazeh, T Mills, SM Muller, TWA Quarles, B Quinn, SN Ragozzine, D Shporer, A Steffen, JH Tal-Or, L Torres, G Windmiller, G Borucki, WJ AF Welsh, William F. Orosz, Jerome A. Short, Donald R. Cochran, William D. Endl, Michael Brugamyer, Erik Haghighipour, Nader Buchhave, Lars A. Doyle, Laurance R. Fabrycky, Daniel C. Hinse, Tobias Cornelius Kane, Stephen R. Kostov, Veselin Mazeh, Tsevi Mills, Sean M. Mueller, Tobias W. A. Quarles, Billy Quinn, Samuel N. Ragozzine, Darin Shporer, Avi Steffen, Jason H. Tal-Or, Lev Torres, Guillermo Windmiller, Gur Borucki, William J. TI KEPLER 453 b-THE 10th KEPLER TRANSITING CIRCUMBINARY PLANET SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries: close; binaries: eclipsing; planets and satellites: detection; planets and satellites: dynamical evolution and stability; stars: individual (KIC 9632895, Kepler-453) ID MAIN-SEQUENCE STARS; CLOSE BINARY-SYSTEMS; LOW-MASS; LIGHT CURVES; HIERARCHICAL TRIPLE; ECLIPSING BINARIES; ROTATION PERIODS; STELLAR ROTATION; TIDAL EVOLUTION; HABITABLE ZONES AB We present the discovery of Kepler-453 b, a 6.2 R-circle plus planet in a low-eccentricity, 240.5 day orbit about an eclipsing binary. The binary itself consists of a 0.94 and 0.195 M-circle dot pair of stars with an orbital period of 27.32 days. The plane of the planet's orbit is rapidly precessing, and its inclination only becomes sufficiently aligned with the primary star in the latter portion of the Kepler data. Thus three transits are present in the second half of the light curve, but none of the three conjunctions that occurred during the first half of the light curve produced observable transits. The precession period is similar to 103 years, and during that cycle, transits are visible only similar to 8.9% of the time. This has the important implication that for every system like Kepler-453 that we detect, there are similar to 11.5 circumbinary systems that exist but are not currently exhibiting transits. The planet's mass is too small to noticeably perturb the binary, and consequently its mass is not measurable with these data; however, our photodynamical model places a 1 sigma upper limit of 16 M-circle plus. With a period 8.8 times that of the binary, the planet is well outside the dynamical instability zone. It does, however, lie within the habitable zone of the binary, making it the third of 10 Kepler circumbinary planets to do so. C1 [Welsh, William F.; Orosz, Jerome A.; Short, Donald R.; Windmiller, Gur] San Diego State Univ, Dept Astron, San Diego, CA 92182 USA. [Cochran, William D.; Endl, Michael; Brugamyer, Erik] Univ Texas Austin, McDonald Observ, Austin, TX 78712 USA. [Haghighipour, Nader] Univ Hawaii Manoa, Inst Astron, Honolulu, HI 96822 USA. [Haghighipour, Nader] Univ Hawaii Manoa, NASA Astrobiol Inst, Honolulu, HI 96822 USA. [Buchhave, Lars A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Buchhave, Lars A.] Univ Copenhagen, Nat Hist Museum Denmark, Ctr Star & Planet Format, DK-1350 Copenhagen, Denmark. [Doyle, Laurance R.] SETI Inst, Mountain View, CA 94043 USA. [Doyle, Laurance R.] Principia Coll, IMoP, Elsah, IL 62028 USA. [Fabrycky, Daniel C.; Mills, Sean M.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. [Hinse, Tobias Cornelius] Korea Astron & Space Sci Inst, Taejon 305348, South Korea. [Hinse, Tobias Cornelius] Armagh Observ, Armagh BT61 9DG, North Ireland. [Kane, Stephen R.] San Francisco State Univ, Dept Phys & Astron, San Francisco, CA 94132 USA. [Kostov, Veselin] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Mazeh, Tsevi; Tal-Or, Lev] Tel Aviv Univ, Raymond & Beverly Sackler Fac Exact Sci, Sch Phys & Astron, IL-69978 Tel Aviv, Israel. [Mueller, Tobias W. A.] Univ Tubingen, Inst Astron & Astrophys, D-72076 Tubingen, Germany. [Quarles, Billy; Borucki, William J.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Quinn, Samuel N.] Georgia State Univ, Dept Phys & Astron, Atlanta, GA 30303 USA. [Ragozzine, Darin] Florida Inst Technol, Dept Phys & Space Sci, Melbourne, FL 32901 USA. [Shporer, Avi] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Shporer, Avi] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. [Steffen, Jason H.] Northwestern Univ, CIERA, Evanston, IL 60208 USA. [Torres, Guillermo] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Orosz, JA (reprint author), San Diego State Univ, Dept Astron, 5500 Campanile Dr, San Diego, CA 92182 USA. EM wwelsh@mail.sdsu.edu; jorosz@mail.sdsu.edu OI Buchhave, Lars A./0000-0003-1605-5666 FU Institute for Astronomy; NASA Astrobiology Institute at the University of Hawaii-Manoa; National Science Foundation [AST-1109928]; NASA's Kepler Participating Scientist Program [NNX12AD23G]; Origins of Solar Systems Program [NNX13AI76G]; Korea Research Council for Fundamental Science and Technology (KRCF) through the Young Research Scientist Fellowship Program; KASI (Korea Astronomy and Space Science Institute) [2013-9-400-0/2014-1-400-06]; Northern Ireland Department of Culture, Arts and Leisure (DCAL); NASA ADAP grant [NNX13AF20G]; NASA Origins grant [NNX12AQ62G]; Astrobiology Institute under Institute for Astronomy, University of Hawaii [NNA09DA77]; HST grant [HST-GO-12548.06-A]; NASA from the Space Telescope Science Institute [HST-GO-12548.06-A]; NASA [NAS5-26555]; European Research Council under the EU's Seventh Framework Programme (ERC Grant) [291352]; NASA Postdoctoral Program; NSF grant [AST-1007992]; NASA, Science Mission Directorate FX We thank the ApJ Editors for their patience and the anonymous referee for suggestions that helped improve this paper. We thank Amy McQuillan of Tel Aviv University for assistance with the measurement of the ACF, and Justice Bruursema for assisting with the WIYN observations. W.F.W. thanks the Institute for Astronomy and the NASA Astrobiology Institute at the University of Hawaii-Manoa for their support and kind hospitality during his sabbatical visit when part of this project was carried out. W.F.W. and J.A.O. gratefully acknowledge support from the National Science Foundation via grant AST-1109928, and from NASA's Kepler Participating Scientist Program (NNX12AD23G) and Origins of Solar Systems Program (NNX13AI76G). T.C.H. gratefully acknowledges financial support from the Korea Research Council for Fundamental Science and Technology (KRCF) through the Young Research Scientist Fellowship Program and financial support from KASI (Korea Astronomy and Space Science Institute) grant number 2013-9-400-0/2014-1-400-06. Numerical computations were partly carried out using the SFI/HEA Irish Centre for High-End Computing (ICHEC) and the KMTNet computing cluster at the Korea Astronomy and Space Science Institute. Astronomical research at the Armagh Observatory is funded by the Northern Ireland Department of Culture, Arts and Leisure (DCAL). N.H. acknowledges support from the NASA ADAP grant NNX13AF20G, NASA Origins grant NNX12AQ62G, Astrobiology Institute under Cooperative Agreement NNA09DA77 at the Institute for Astronomy, University of Hawaii, and HST grant HST-GO-12548.06-A. Support for program HST-GO-12548.06-A 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. T.M. gratefully acknowledges support of from the European Research Council under the EU's Seventh Framework Programme (ERC Grant Agreement No. 291352). B.Q. gratefully acknowledges the support of the NASA Postdoctoral Program. J.H.S. acknowledges the support from NASA's Kepler Participating Scientist Program (NNX12AD23G). G.T. acknowledges partial support from NSF grant AST-1007992. The authors acknowledge the outstanding work of David Ciardi (NExScI/Caltech) in organizing and maintaining the Kepler Community Follow-up Observing Program (CFOP) website.26 We also thank Phil Lucas for organizing the UKIRT J-band observations of the Kepler field available on the CFOP website. This research has made use of the NASA Exoplanet Archive, which is operated by the California Institute of Technology, under contract with the National Aeronautics and Space Administration under the Exoplanet Exploration Program. Kepler was competitively selected as the 10th mission of the Discovery Program. Funding for this mission is provided by NASA, Science Mission Directorate. NR 79 TC 20 Z9 20 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD AUG 10 PY 2015 VL 809 IS 1 AR 26 DI 10.1088/0004-637X/809/1/26 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CR9DN UT WOS:000361653500026 ER PT J AU Willis, S Guzman, A Marengo, M Smith, HA Martinez, R Allen, L AF Willis, S. Guzman, A. Marengo, M. Smith, H. A. Martinez, R. Allen, L. TI THE SCHMIDT LAW IN SIX GALACTIC MASSIVE STAR-FORMING REGIONS SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM: clouds; stars: formation ID NEARBY MOLECULAR CLOUDS; SPITZER-SPACE-TELESCOPE; HERSCHEL HI-GAL; MILKY-WAY; NGC 6334; FORMATION RATES; ARRAY CAMERA; COMPLEX; GALAXIES; EXTINCTION AB We present a census of young stars in five massive star-forming regions in the 4th Galactic quadrant, G305, G326-4, G326-6, G333 (RCW 106), and G351, and combine this census with an earlier census of young stars in NGC 6334. Each region was observed at J, H, and K-s with the NOAO Extremely Wide-Field Infrared Imager and combined with deep observations taken with the Infrared Array Camera (IRAC) on board the Spitzer Space Telescope at the wavelengths 3.6 and 4.5 mu m. We derived a five band point-source catalog containing >200,000 infrared sources in each region. We have identified a total of 2871 YSO candidates, 363 Class I YSOs, and 2508 Class II YSOs. We mapped the column density of each cloud using observations from Herschel between 160 and 500 mu m and near-infrared extinction maps in order to determine the average gas surface density above A(V) > 2. We study the surface density of the YSOs and the star-formation rate as a function of the column density within each cloud and compare them to the results for nearby star-forming regions. We find a range in power-law indices across the clouds, with the dispersion in the local relations in an individual cloud much lower than the average over the six clouds. We find the average over the six clouds to be Sigma(SFR) similar to Sigma(2.15 +/- 0.41)(gas) and power-law exponents ranging from 1.77 to 2.86, similar to the values derived within nearby star-forming regions, including Taurus and Orion. The large dispersion in the power-law relations between individual Milky Way molecular clouds reinforces the idea that there is not a direct universal connection between Sigma(gas) and a cloud's observed star-formation rate. C1 [Willis, S.; Marengo, M.] Iowa State Univ, Dept Phys & Astron, Ames, IA 50010 USA. [Willis, S.; Guzman, A.; Smith, H. A.; Martinez, R.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Allen, L.] Natl Opt Astron Observ, Tucson, AZ 85719 USA. RP Willis, S (reprint author), Iowa State Univ, Dept Phys & Astron, Ames, IA 50010 USA. EM swillis@cfa.harvard.edu OI Guzman, Andres/0000-0003-0990-8990 FU NASA [1407, NNX12AI55G, NNX10AD68G]; JPL-RSA [1369565]; National Aeronautics and Space Administration's Earth Science Technology Office [NCC5-626] FX This work is based on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under NASA contract 1407. This research made use of Montage, funded by the National Aeronautics and Space Administration's Earth Science Technology Office, Computation Technologies Project, under cooperative agreement NCC5-626 between NASA and the California Institute of Technology. Montage is maintained by the NASA/IPAC Infrared Science Archive. S.W. acknowledges partial support from NASA grants NNX12AI55G and NNX10AD68G, and JPL-RSA 1369565. S.W. and H.A.S. acknowledge partial support from NASA Grants NNX12AI55G and NNX10AD68G, and JPL-RSA 1369565. NR 52 TC 2 Z9 2 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD AUG 10 PY 2015 VL 809 IS 1 AR 87 DI 10.1088/0004-637X/809/1/87 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CR9DN UT WOS:000361653500087 ER PT J AU Kaplan, DL Tingay, SJ Manoharan, PK Macquart, JP Hancock, P Morgan, J Mitchell, DA Ekers, RD Wayth, RB Trott, C Murphy, T Oberoi, D Cairns, IH Feng, L Kudryavtseva, N Bernardi, G Bowman, JD Briggs, F Cappallo, RJ Deshpande, AA Gaensler, BM Greenhill, LJ Walker, NH Hazelton, BJ Hollitt, MJ Lonsdale, CJ McWhirter, SR Morales, MF Morgan, E Ord, SM Prabu, T Shankar, NU Srivani, KS Subrahmanyan, R Webster, RL Williams, A Williams, CL AF Kaplan, D. L. Tingay, S. J. Manoharan, P. K. Macquart, J. P. Hancock, P. Morgan, J. Mitchell, D. A. Ekers, R. D. Wayth, R. B. Trott, C. Murphy, T. Oberoi, D. Cairns, I. H. Feng, L. Kudryavtseva, N. Bernardi, G. Bowman, J. D. Briggs, F. Cappallo, R. J. Deshpande, A. A. Gaensler, B. M. Greenhill, L. J. Walker, N. Hurley Hazelton, B. J. Hollitt, M. Johnston Lonsdale, C. J. McWhirter, S. R. Morales, M. F. Morgan, E. Ord, S. M. Prabu, T. Shankar, N. Udaya Srivani, K. S. Subrahmanyan, R. Webster, R. L. Williams, A. Williams, C. L. TI MURCHISON WIDEFIELD ARRAY OBSERVATIONS OF ANOMALOUS VARIABILITY: A SERENDIPITOUS NIGHT-TIME DETECTION OF INTERPLANETARY SCINTILLATION SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE radio continuum: galaxies; scattering; Sun: coronal mass ejections (CMEs); Sun: heliosphere; techniques: interferometric ID RADIO-SOURCES; INTERSTELLAR SCINTILLATION; CATALOG; VELOCITIES AB We present observations of high-amplitude rapid (2 s) variability toward two bright, compact extragalactic radio sources out of several hundred of the brightest radio sources in one of the 30 degrees x 30 degrees Murchison Widefield Array (MWA) Epoch of Reionization fields using the MWA at 155 MHz. After rejecting intrinsic, instrumental, and ionospheric origins we consider the most likely explanation for this variability to be interplanetary scintillation (IPS), likely the result of a large coronal mass ejection propagating from the Sun. This is confirmed by roughly contemporaneous observations with the Ooty Radio Telescope. We see evidence for structure on spatial scales ranging from <1000 to >10(6) km. The serendipitous night-time nature of these detections illustrates the new regime that the MWA has opened for IPS studies with sensitive night-time, wide-field, low-frequency observations. This regime complements traditional dedicated strategies for observing IPS and can be utilized in real-time to facilitate dedicated follow-up observations. At the same time, it allows large-scale surveys for compact (arcsec) structures in low-frequency radio sources despite the 2' resolution of the array. C1 [Kaplan, D. L.] Univ Wisconsin, Dept Phys, Milwaukee, WI 53201 USA. [Tingay, S. J.; Macquart, J. P.; Hancock, P.; Morgan, J.; Wayth, R. B.; Trott, C.; Kudryavtseva, N.; Walker, N. Hurley; Ord, S. M.; Williams, A.] Curtin Univ, Int Ctr Radio Astron Res, Bentley, WA 6102, Australia. [Tingay, S. J.; Macquart, J. P.; Hancock, P.; Mitchell, D. A.; Wayth, R. B.; Trott, C.; Murphy, T.; Gaensler, B. M.; Ord, S. M.; Subrahmanyan, R.; Webster, R. L.] Tata Inst Fundamental Res, ARC Ctr Excellence All Sky Astrophys CAASTRO, Ooty 643001, India. [Manoharan, P. K.; Oberoi, D.] Tata Inst Fundamental Res, Natl Ctr Radio Astrophys, Radio Astron Ctr, Ooty 643001, India. [Mitchell, D. A.; Ekers, R. D.] CASS, Epping, NSW 1710, Australia. [Murphy, T.; Cairns, I. H.; Gaensler, B. M.] Univ Sydney, Sydney Inst Astron, Sch Phys, Sydney, NSW 2006, Australia. [Feng, L.; Morgan, E.; Williams, C. L.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Bernardi, G.] SKA SA, ZA-7405 Pinelands, South Africa. [Bernardi, G.] Rhodes Univ, Dept Phys & Elect, ZA-6140 Grahamstown, South Africa. [Bernardi, G.; Greenhill, L. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Bowman, J. D.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA. [Briggs, F.] Australian Natl Univ, Res Sch Astron & Astrophys, Canberra, ACT 2611, Australia. [Cappallo, R. J.; Lonsdale, C. J.; McWhirter, S. R.] MIT, Haystack Observ, Westford, MA 01886 USA. [Deshpande, A. A.; Prabu, T.; Shankar, N. Udaya; Srivani, K. S.; Subrahmanyan, R.] Raman Res Inst, Bangalore 560080, Karnataka, India. [Gaensler, B. M.] Univ Toronto, Dunlap Inst Astron & Astrophys, Toronto, ON M5S 3H4, Canada. [Hazelton, B. J.; Morales, M. F.] Univ Washington, Dept Phys, Seattle, WA 98195 USA. [Hollitt, M. Johnston] Victoria Univ Wellington, Sch Chem & Phys Sci, Wellington 6140, New Zealand. [Webster, R. L.] Univ Melbourne, Sch Phys, Parkville, Vic 3010, Australia. RP Kaplan, DL (reprint author), Univ Wisconsin, Dept Phys, Milwaukee, WI 53201 USA. EM kaplan@uwm.edu RI Wayth, Randall/B-2444-2013; Trott, Cathryn/B-5325-2013; Deshpande, Avinash/D-4868-2012; Udayashankar , N/D-4901-2012; Hurley-Walker, Natasha/B-9520-2013; Subrahmanyan, Ravi/D-4889-2012; M, Manjunath/N-4000-2014; OI Wayth, Randall/0000-0002-6995-4131; Cairns, Iver/0000-0001-6978-9765; Trott, Cathryn/0000-0001-6324-1766; Hurley-Walker, Natasha/0000-0002-5119-4808; M, Manjunath/0000-0001-8710-0730; Gaensler, Bryan/0000-0002-3382-9558; Kaplan, David/0000-0001-6295-2881; Murphy, Tara/0000-0002-2686-438X; Kudryavtseva, Nadia/0000-0002-1372-0942; Ekers, Ron/0000-0002-3532-9928; Hancock, Paul/0000-0002-4203-2946 FU U.S. National Science Foundation [AST-0457585, PHY-0835713, CAREER-0847753, AST-0908884]; Australian Research Council (LIEF) [LE0775621, LE0882938]; U.S. Air Force Office of Scientific Research [FA9550-0510247]; Centre for All-sky Astrophysics (an Australian Research Council Centre of Excellence) [CE110001020]; NSF [AST-1412421]; ISRO; Smithsonian Astrophysical Observatory; MIT School of Science; Raman Research Institute; Australian National University; Victoria University of Wellington from the New Zealand Ministry of Economic Development [MED-E1799]; Victoria University of Wellington from the IBM; Australian Federal government via the Commonwealth Scientific and Industrial Research Organisation (CSIRO); National Collaborative Research Infrastructure Strategy, Education Investment Fund; Australia India Strategic Research Fund; Astronomy Australia Limited; NVIDIA at Harvard University; International Centre for Radio Astronomy Research (ICRAR); Western Australian State government FX We thank an anonymous referee for a thorough and thoughtful review. We thank B. Jackson, C. Loi, and A. Rowlinson for helpful conversations. This scientific work makes use of the Murchison Radio-astronomy Observatory, operated by CSIRO. We acknowledge the Wajarri Yamatji people as the traditional owners of the Observatory site. Support for the MWA comes from the U.S. National Science Foundation (grants AST-0457585, PHY-0835713, CAREER-0847753, and AST-0908884), the Australian Research Council (LIEF grants LE0775621 and LE0882938), the U.S. Air Force Office of Scientific Research (grant FA9550-0510247), and the Centre for All-sky Astrophysics (an Australian Research Council Centre of Excellence funded by grant CE110001020). D.L.K. is additionally supported by NSF grant AST-1412421. P.K.M. acknowledges partial support from ISRO. Support is also provided by the Smithsonian Astrophysical Observatory, the MIT School of Science, the Raman Research Institute, the Australian National University, and the Victoria University of Wellington (via grant MED-E1799 from the New Zealand Ministry of Economic Development and an IBM Shared University Research Grant). The Australian Federal government provides additional support via the Commonwealth Scientific and Industrial Research Organisation (CSIRO), National Collaborative Research Infrastructure Strategy, Education Investment Fund, and the Australia India Strategic Research Fund, and Astronomy Australia Limited, under contract to Curtin University. We acknowledge the iVEC Petabyte Data Store, the Initiative in Innovative Computing and the CUDA Center for Excellence sponsored by NVIDIA at Harvard University, and the International Centre for Radio Astronomy Research (ICRAR), a Joint Venture of Curtin University and The University of Western Australia, funded by the Western Australian State government. This research made use of APLpy, an open-source plotting package for Python hosted at http://aplpy.github.com. NR 40 TC 4 Z9 5 U1 0 U2 7 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 AUG 10 PY 2015 VL 809 IS 1 AR L12 DI 10.1088/2041-8205/809/1/L12 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CO7EJ UT WOS:000359321900012 ER PT J AU Taniguchi, Y Kajisawa, M Kobayashi, MAR Nagao, T Shioya, Y Scoville, NZ Sanders, DB Capak, PL Koekemoer, AM Toft, S McCracken, HJ Le Fevre, O Tasca, L Sheth, K Renzini, A Lilly, S Carollo, M Kovac, K Ilbert, O Schinnerer, E Fu, H Tresse, L Griffiths, RE Civano, F AF Taniguchi, Yoshiaki Kajisawa, Masaru Kobayashi, Masakazu A. R. Nagao, Tohru Shioya, Yasuhiro Scoville, Nick Z. Sanders, David B. Capak, Peter L. Koekemoer, Anton M. Toft, Sune McCracken, Henry J. Le Fevre, Olivier Tasca, Lidia Sheth, Kartik Renzini, Alvio Lilly, Simon Carollo, Marcella Kovac, Katarina Ilbert, Olivier Schinnerer, Eva Fu, Hai Tresse, Laurence Griffiths, Richard E. Civano, Francesca TI DISCOVERY OF MASSIVE, MOSTLY STAR FORMATION QUENCHED GALAXIES WITH EXTREMELY LARGE Ly alpha EQUIVALENT WIDTHS AT z similar to 3 SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE cosmology: observations; early universe; galaxies: evolution; galaxies: formation; galaxies: high-redshift ID EVOLUTION SURVEY COSMOS; QUIESCENT GALAXIES; STELLAR POPULATIONS; EMITTING GALAXIES; DROPOUT GALAXIES; SOURCE CATALOG; FIELD; REDSHIFT; EMITTERS; PROGENITORS AB We report a discovery of six massive galaxies with both extremely large Ly alpha equivalent widths (EWs) and evolved stellar populations at z similar to 3. These MAssive Extremely STrong Ly alpha emitting Objects (MAESTLOs) have been discovered in our large-volume systematic survey for strong Ly alpha emitters (LAEs) with 12 optical intermediate-band data taken with Subaru/Suprime-Cam in the COSMOS field. Based on the spectral energy distribution fitting analysis for these LAEs, it is found that these MAESTLOs have (1) large rest-frame EWs of EW0 (Ly alpha) similar to 100-300 angstrom, (2) M-star similar to 10(10.5) -10(11.1) M-circle dot, and (3) relatively low specific star formation rates of SFR/M-star similar to 0.03-1 Gyr(-1). Three of the six MAESTLOs have extended Ly alpha emission with a radius of several kiloparsecs, although they show very compact morphology in the HST/ACS images, which correspond to the rest-frame UV continuum. Since the MAESTLOs do not show any evidence for active galactic nuclei, the observed extended Ly alpha emission is likely to be caused by a star formation process including the superwind activity. We suggest that this new class of LAEs, MAESTLOs, provides a missing link from star-forming to passively evolving galaxies at the peak era of the cosmic star formation history. C1 [Taniguchi, Yoshiaki; Kajisawa, Masaru; Kobayashi, Masakazu A. R.; Nagao, Tohru; Shioya, Yasuhiro] Ehime Univ, Res Ctr Space & Cosm Evolut, Bunkyo Cho, Matsuyama, Ehime 7908577, Japan. [Kajisawa, Masaru] Ehime Univ, Grad Sch Sci & Engn, Bunkyo Cho, Matsuyama, Ehime 7908577, Japan. [Scoville, Nick Z.; Capak, Peter L.] CALTECH, Dept Astron, Pasadena, CA 91125 USA. [Sanders, David B.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Capak, Peter L.] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. [Koekemoer, Anton M.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Toft, Sune] Univ Copenhagen, Dark Cosmol Ctr, Niels Bohr Inst, DK-2100 Copenhagen, Denmark. [McCracken, Henry J.] Univ Paris 06, Inst Astrophys Paris, CNRS, UMR7095, F-75014 Paris, France. [Le Fevre, Olivier; Tasca, Lidia; Ilbert, Olivier; Tresse, Laurence] Aix Marseille Univ, LAM, CNRS, UMR 7326, F-13388 Marseille, France. [Sheth, Kartik] Natl Radio Astron Observ, Charlottesville, VA 22903 USA. [Renzini, Alvio] Univ Padua, Dipartimento Astron, I-35122 Padua, Italy. [Lilly, Simon; Carollo, Marcella; Kovac, Katarina] Swiss Fed Inst Technol, Dept Phys, CH-8093 Zurich, Switzerland. [Schinnerer, Eva] MPI Astron, D-69117 Heidelberg, Germany. [Fu, Hai] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52245 USA. [Griffiths, Richard E.] Univ Hawaii, Phys & Astron, Hilo, HI 96720 USA. [Civano, Francesca] Yale Ctr Astron & Astrophys, New Haven, CT 06520 USA. [Civano, Francesca] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Taniguchi, Y (reprint author), Ehime Univ, Res Ctr Space & Cosm Evolut, Bunkyo Cho, Matsuyama, Ehime 7908577, Japan. EM tani@cosmos.phys.sci.ehime-u.ac.jp FU JSPS [15340059, 17253001, 19340046, 23244031, 23654068, 25707010] FX We would like to thank both the Subaru and HST staff for their invaluable help, as well as all members of the COSMOS team. We would also like to thank the anonymous referee for valuable suggestions and comments. We also thank Alex Hagen for kindly providing us with the information of their LAEs. This work was financially supported in part by JSPS (Y.T.: 15340059, 17253001, 19340046, and 23244031; T.N.: 23654068 and 25707010). Data analysis was in part carried out on the common use data analysis computer system at the Astronomy Data Center, ADC, of the National Astronomical Observatory of Japan. NR 36 TC 5 Z9 5 U1 0 U2 0 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 AUG 10 PY 2015 VL 809 IS 1 AR L7 DI 10.1088/2041-8205/809/1/L7 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CO7EJ UT WOS:000359321900007 ER PT J AU Arora, BS Morgan, J Ord, SM Tingay, SJ Hurley-Walker, N Bell, M Bernardi, G Bhat, NDR Briggs, F Callingham, JR Deshpande, AA Dwarakanath, KS Ewall-Wice, A Feng, L For, BQ Hancock, P Hazelton, BJ Hindson, L Jacobs, D Johnston-Hollitt, M Kapinska, AD Kudryavtseva, N Lenc, E McKinley, B Mitchell, D Oberoi, D Offringa, AR Pindor, B Procopio, P Riding, J Staveley-Smith, L Wayth, RB Wu, C Zheng, Q Bowman, JD Cappallo, RJ Corey, BE Emrich, D Goeke, R Greenhill, LJ Kaplan, DL Kasper, JC Kratzenberg, E Lonsdale, CJ Lynch, MJ McWhirter, SR Morales, MF Morgan, E Prabu, T Rogers, AEE Roshi, A Shankar, NU Srivani, KS Subrahmanyan, R Waterson, M Webster, RL Whitney, AR Williams, A Williams, CL AF Arora, B. S. Morgan, J. Ord, S. M. Tingay, S. J. Hurley-Walker, N. Bell, M. Bernardi, G. Bhat, N. D. R. Briggs, F. Callingham, J. R. Deshpande, A. A. Dwarakanath, K. S. Ewall-Wice, A. Feng, L. For, B. -Q. Hancock, P. Hazelton, B. J. Hindson, L. Jacobs, D. Johnston-Hollitt, M. Kapinska, A. D. Kudryavtseva, N. Lenc, E. McKinley, B. Mitchell, D. Oberoi, D. Offringa, A. R. Pindor, B. Procopio, P. Riding, J. Staveley-Smith, L. Wayth, R. B. Wu, C. Zheng, Q. Bowman, J. D. Cappallo, R. J. Corey, B. E. Emrich, D. Goeke, R. Greenhill, L. J. Kaplan, D. L. Kasper, J. C. Kratzenberg, E. Lonsdale, C. J. Lynch, M. J. McWhirter, S. R. Morales, M. F. Morgan, E. Prabu, T. Rogers, A. E. E. Roshi, A. Shankar, N. Udaya Srivani, K. S. Subrahmanyan, R. Waterson, M. Webster, R. L. Whitney, A. R. Williams, A. Williams, C. L. TI Ionospheric Modelling using GPS to Calibrate the MWA. I: Comparison of First Order Ionospheric Effects between GPS Models and MWA Observations SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF AUSTRALIA LA English DT Article DE atmospheric effects; techniques: interferometric ID TOTAL ELECTRON-CONTENT AB We compare first-order (refractive) ionospheric effects seen by the MWA with the ionosphere as inferred from GPS data. The first-order ionosphere manifests itself as a bulk position shift of the observed sources across an MWA field of view. These effects can be computed from global ionosphere maps provided by GPS analysis centres, namely the CODE. However, for precision radio astronomy applications, data from local GPS networks needs to be incorporated into ionospheric modelling. For GPS observations, the ionospheric parameters are biased by GPS receiver instrument delays, among other effects, also known as receiver DCBs. The receiver DCBs need to be estimated for any non-CODE GPS station used for ionosphere modelling. In this work, single GPS station-based ionospheric modelling is performed at a time resolution of 10 min. Also the receiver DCBs are estimated for selected Geoscience Australia GPS receivers, located at Murchison Radio Observatory, Yarragadee, Mount Magnet and Wiluna. The ionospheric gradients estimated from GPS are compared with that inferred from MWA. The ionospheric gradients at all the GPS stations show a correlation with the gradients observed with the MWA. The ionosphere estimates obtained using GPS measurements show promise in terms of providing calibration information for the MWA. C1 [Arora, B. S.; Morgan, J.; Ord, S. M.; Tingay, S. J.; Hurley-Walker, N.; Bhat, N. D. R.; Hancock, P.; Kudryavtseva, N.; Wayth, R. B.; Emrich, D.; Lynch, M. J.; Williams, A.] Curtin Univ, Int Ctr Radio Astron Res, Bentley, WA 6102, Australia. [Callingham, J. R.; Lenc, E.] Univ Sydney, Sch Phys, Sydney Inst Astron, Sydney, NSW 2006, Australia. [Bernardi, G.] SKA SA, ZA-7405 Pinelands, South Africa. [Bernardi, G.] Rhodes Univ, Dept Phys & Elect, ZA-6140 Grahamstown, South Africa. [Bernardi, G.; Greenhill, L. J.; Kasper, J. C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Briggs, F.; McKinley, B.; Offringa, A. R.] Australian Natl Univ, Res Sch Astron & Astrophys, Canberra, ACT 2611, Australia. [Callingham, J. R.; Mitchell, D.] CSIRO Astron & Space Sci, Epping, NSW 1710, Australia. [Callingham, J. R.; Hancock, P.; Kapinska, A. D.; Lenc, E.; McKinley, B.; Mitchell, D.; Procopio, P.; Staveley-Smith, L.; Wayth, R. B.; Subrahmanyan, R.; Webster, R. L.] ARC Ctr Excellence All Sky Astrophys CAASTRO, Redfern, NSW 2016, Australia. [Deshpande, A. A.; Dwarakanath, K. S.; Prabu, T.; Shankar, N. Udaya; Srivani, K. S.; Subrahmanyan, R.] Raman Res Inst, Bangalore 560080, Karnataka, India. [Ewall-Wice, A.; Feng, L.; Goeke, R.; Morgan, E.; Williams, C. L.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [For, B. -Q.; Kapinska, A. D.; Staveley-Smith, L.; Wu, C.] Univ Western Australia, ICRAR, Crawley, WA 6009, Australia. [Hazelton, B. J.; Morales, M. F.] Univ Washington, Dept Phys, Seattle, WA 98195 USA. [Hindson, L.; Johnston-Hollitt, M.; Zheng, Q.] Victoria Univ Wellington, Sch Chem & Phys Sci, Wellington 6140, New Zealand. [Jacobs, D.; Bowman, J. D.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA. [Mitchell, D.; Pindor, B.; Procopio, P.; Riding, J.; Webster, R. L.] Univ Melbourne, Sch Phys, Parkville, Vic 3010, Australia. [Oberoi, D.] Tata Inst Fundamental Res, Natl Ctr Radio Astrophys, Pune 411007, Maharashtra, India. [Cappallo, R. J.; Corey, B. E.; Kratzenberg, E.; Lonsdale, C. J.; McWhirter, S. R.; Rogers, A. E. E.; Whitney, A. R.] MIT, Haystack Observ, Westford, MA 01886 USA. [Kaplan, D. L.] Univ Wisconsin, Dept Phys, Milwaukee, WI 53201 USA. [Kasper, J. C.] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA. [Roshi, A.] Natl Radio Astron Observ, Charlottesville, VA 22903 USA. [Waterson, M.] Jodrell Bank Observ, SKA Org Headquarters, Macclesfield SK11 9DL, Cheshire, England. RP Arora, BS (reprint author), Curtin Univ, Int Ctr Radio Astron Res, Bentley, WA 6102, Australia. EM balwinderarora@gmail.com RI Wayth, Randall/B-2444-2013; Dwarakanath, K /D-4876-2012; Hurley-Walker, Natasha/B-9520-2013; Emrich, David/B-7002-2013; Subrahmanyan, Ravi/D-4889-2012; M, Manjunath/N-4000-2014; Kapinska, Anna/B-3999-2014; Deshpande, Avinash/D-4868-2012; Udayashankar , N/D-4901-2012; Staveley-Smith, Lister/A-1683-2011 OI Lenc, Emil/0000-0002-9994-1593; Kudryavtseva, Nadia/0000-0002-1372-0942; Callingham, Joseph/0000-0002-7167-1819; Hancock, Paul/0000-0002-4203-2946; /0000-0002-0086-7363; Wayth, Randall/0000-0002-6995-4131; Hurley-Walker, Natasha/0000-0002-5119-4808; Emrich, David/0000-0002-4058-1837; M, Manjunath/0000-0001-8710-0730; Kapinska, Anna/0000-0002-5289-5729; Staveley-Smith, Lister/0000-0002-8057-0294 FU US National Science Foundation [AST-0457585, PHY-0835713, CAREER-0847753, AST-0908884]; Australian Research Council [LE0775621, LE0882938]; US Air Force Office of Scientific Research [FA9550-0510247]; Centre for All-sky Astrophysics (an Australian Research Council Centre of Excellence) [CE110001020]; Smithsonian Astrophysical Observatory; MIT School of Science; Raman Research Institute; Australian National University; Victoria University of Wellington from New Zealand Ministry of Economic Development [MED-E1799]; Victoria University of Wellington from IBM Shared University Research Grant [MED-E1799]; NVIDIA at Harvard University; International Centre for Radio Astronomy Research (ICRAR); Joint Venture of Curtin University; University of Western Australia; Western Australian State government; CSIRO; National Collaborative Research Infrastructure Strategy; Education Investment Fund; Australia India Strategic Research Fund; Astronomy Australia Limited FX The authors wish to thank Anthony Willis from National Research Council of Canada for the valuable discussions. This scientific work makes use of the MRO, operated by Commonwealth Scientific and Industrial Research Organisation (CSIRO). We acknowledge the Wajarri Yamatji people as the traditional owners of the Observatory site. Support for the MWA comes from the US National Science Foundation (grants AST-0457585, PHY-0835713, CAREER-0847753, and AST-0908884), the Australian Research Council (LIEF grants LE0775621 and LE0882938), the US Air Force Office of Scientific Research (grant FA9550-0510247), and the Centre for All-sky Astrophysics (an Australian Research Council Centre of Excellence funded by grant CE110001020). Support is also provided by the Smithsonian Astrophysical Observatory, the MIT School of Science, the Raman Research Institute, the Australian National University, and the Victoria University of Wellington (via grant MED-E1799 from the New Zealand Ministry of Economic Development and an IBM Shared University Research Grant). The Australian Federal government provides additional support via the CSIRO, National Collaborative Research Infrastructure Strategy, Education Investment Fund, and the Australia India Strategic Research Fund, and Astronomy Australia Limited, under contract to Curtin University. We acknowledge the iVEC Petabyte Data Store, the Initiative in Innovative Computing and the CUDA Center for Excellence sponsored by NVIDIA at Harvard University, and the International Centre for Radio Astronomy Research (ICRAR), a Joint Venture of Curtin University and The University of Western Australia, funded by the Western Australian State government. NR 50 TC 4 Z9 4 U1 1 U2 9 PU CAMBRIDGE UNIV PRESS PI NEW YORK PA 32 AVENUE OF THE AMERICAS, NEW YORK, NY 10013-2473 USA SN 1323-3580 EI 1448-6083 J9 PUBL ASTRON SOC AUST JI Publ. Astron. Soc. Aust. PD AUG 10 PY 2015 VL 32 AR e029 DI 10.1017/pasa.2015.29 PG 21 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CO8RU UT WOS:000359439300001 ER PT J AU Waring, BG Alvarez-Cansino, L Barry, KE Becklund, KK Dale, S Gei, MG Keller, AB Lopez, OR Markesteijn, L Mangan, S Riggs, CE Rodriguez-Ronderos, ME Segnitz, RM Schnitzer, SA Powers, JS AF Waring, Bonnie G. Alvarez-Cansino, Leonor Barry, Kathryn E. Becklund, Kristen K. Dale, Sarah Gei, Maria G. Keller, Adrienne B. Lopez, Omar R. Markesteijn, Lars Mangan, Scott Riggs, Charlotte E. Rodriguez-Ronderos, Maria Elizabeth Segnitz, R. Max Schnitzer, Stefan A. Powers, Jennifer S. TI Pervasive and strong effects of plants on soil chemistry: a meta-analysis of individual plant 'Zinke' effects SO PROCEEDINGS OF THE ROYAL SOCIETY B-BIOLOGICAL SCIENCES LA English DT Article DE individual plant effects; plant-soil interactions; spatial heterogeneity ID ORGANIC-MATTER DYNAMICS; PUBLICATION BIAS; DECIDUOUS TREES; FOREST; DECOMPOSITION; NUTRIENTS; NITROGEN; CARBON; INPUTS; HETEROGENEITY AB Plant species leave a chemical signature in the soils below them, generating fine-scale spatial variation that drives ecological processes. Since the publication of a seminal paper on plant-mediated soil heterogeneity by Paul Zinke in 1962, a robust literature has developed examining effects of individual plants on their local environments (individual plant effects). Here, we synthesize this work using meta-analysis to show that plant effects are strong and pervasive across ecosystems on six continents. Overall, soil properties beneath individual plants differ from those of neighbours by an average of 41%. Although the magnitudes of individual plant effects exhibit weak relationships with climate and latitude, they are significantly stronger in deserts and tundra than forests, and weaker in intensively managed ecosystems. The ubiquitous effects of plant individuals and species on local soil properties imply that individual plant effects have a role in plant soil feedbacks, linking individual plants with biogeochemical processes at the ecosystem scale. C1 [Waring, Bonnie G.; Becklund, Kristen K.; Gei, Maria G.; Riggs, Charlotte E.; Powers, Jennifer S.] Univ Minnesota, Dept Ecol Evolut & Behav, St Paul, MN 55108 USA. [Powers, Jennifer S.] Univ Minnesota, Dept Plant Biol, St Paul, MN 55108 USA. [Alvarez-Cansino, Leonor; Schnitzer, Stefan A.] Marquette Univ, Dept Biol Sci, Milwaukee, WI 53201 USA. [Alvarez-Cansino, Leonor; Lopez, Omar R.; Markesteijn, Lars; Mangan, Scott; Schnitzer, Stefan A.; Powers, Jennifer S.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. [Alvarez-Cansino, Leonor] Univ Bayreuth, Dept Plant Ecol, D-95440 Bayreuth, Germany. [Barry, Kathryn E.; Rodriguez-Ronderos, Maria Elizabeth] Univ Wisconsin, Dept Biol Sci, Milwaukee, WI 53211 USA. [Dale, Sarah] Nurture Lakeland, Staveley, Cumbria, England. [Keller, Adrienne B.] Indiana Univ, Dept Biol, Bloomington, IN USA. [Lopez, Omar R.] Inst Invest Cient & Serv Alta Tecnol, Clayton, Panama. [Markesteijn, Lars] Univ Oxford, Dept Zool, Oxford OX1 3PS, England. [Mangan, Scott] Washington Univ, Dept Biol, St Louis, MO 63130 USA. [Segnitz, R. Max] Stanford Univ, Dept Biol, Stanford, CA 94305 USA. RP Powers, JS (reprint author), Univ Minnesota, Dept Ecol Evolut & Behav, St Paul, MN 55108 USA. EM powers@umn.edu OI Waring, Bonnie/0000-0002-8457-5164 FU NSF [DEB-1019441, DEB-1053237, DEB-0845071, DEB-1019436]; Sistema Nacional de Investigacion (SNI) de SENACYT FX This work was supported by NSF grants DEB-1019441 and DEB-1053237 to J.S.P., and grants nos DEB-0845071 and DEB-1019436 to S.A.S., and funding from Sistema Nacional de Investigacion (SNI) de SENACYT to O.R.L. NR 44 TC 5 Z9 5 U1 4 U2 28 PU ROYAL SOC PI LONDON PA 6-9 CARLTON HOUSE TERRACE, LONDON SW1Y 5AG, ENGLAND SN 0962-8452 EI 1471-2954 J9 P ROY SOC B-BIOL SCI JI Proc. R. Soc. B-Biol. Sci. PD AUG 7 PY 2015 VL 282 IS 1812 BP 91 EP 98 AR 20151001 DI 10.1098/rspb.2015.1001 PG 8 WC Biology; Ecology; Evolutionary Biology SC Life Sciences & Biomedicine - Other Topics; Environmental Sciences & Ecology; Evolutionary Biology GA CS7ZM UT WOS:000362305500011 PM 26224711 ER PT J AU Erwin, DH AF Erwin, Douglas H. TI David M. Raup (1933-2015) OBITUARY SO NATURE LA English DT Biographical-Item C1 [Erwin, Douglas H.] Natl Museum Nat Hist, Dept Palaeobiol, Smithsonian Inst, Washington, DC 20560 USA. [Erwin, Douglas H.] Santa Fe Inst, Santa Fe, NM USA. RP Erwin, DH (reprint author), Natl Museum Nat Hist, Dept Palaeobiol, Smithsonian Inst, Washington, DC 20560 USA. EM erwind@si.edu NR 1 TC 0 Z9 0 U1 1 U2 6 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 0028-0836 EI 1476-4687 J9 NATURE JI Nature PD AUG 6 PY 2015 VL 524 IS 7563 BP 36 EP 36 PG 1 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA CO2QS UT WOS:000359002300021 PM 26245575 ER PT J AU Lemaitre, R Tavares, M AF Lemaitre, Rafael Tavares, Marcos TI New taxonomic and distributional information on hermit crabs (Crustacea: Anomura: Paguroidea) from the Gulf of Mexico, Caribbean Sea, and Atlantic coast of South America SO ZOOTAXA LA English DT Article DE Crustacea; Paguroidea; hermit crabs; new records; taxonomy; distribution; Gulf of Mexico; Caribbean Sea; Brazil; Atlantic South America ID GENUS PAGURISTES CRUSTACEA; A. MILNE-EDWARDS; FAMILY PAGURIDAE CRUSTACEA; TROPICAL WESTERN ATLANTIC; DECAPODA ANOMURA; PROVENZANOI GROUP; AREOPAGURISTES RAHAYU; TOMOPAGURUS CRUSTACEA; ANNOTATED CHECKLIST; MOLECULAR ANALYSIS AB A collection of Paguroidea recently obtained during deep-water expeditions along the coast of Brazil, forms the basis of this report. Of the 14 species reported from Brazil, 11 represent range extensions to the south, and one, Michelopagurus atlanticus (Bouvier, 1922), is a first record for the western Atlantic. The specimens were compared with types and western Atlantic materials deposited in various major museums. A diagnosis and illustrations are presented for each of seven species found to be poorly or insufficiently known. New material and information is reported for two additional species that occur in Brazil but not found in the recent deep-water collections: Clibanarius symmetricus (Randall, 1840) and Mixtopagurus paradoxus A. Milne-Edwards, 1880. Remarkable and unique color photographs of live or fresh specimens of Allodardanus bredini Haig & Provenzano, 1965, Bathynarius anomalus (A. Milne-Edwards & Bouvier, 1893), Pylopagurus discoidalis (A. Milne-Edwards, 1880), Paguristes spinipes A. Milne-Edwards, 1880, Parapagurus pilosimanus Smith, 1876, and P. alaminos Lemaitre, 1986, are presented. A review of published records and museum collections of the terrestrial Coenobita clypeatus (Fabricius, 1787), has shown that the southern range limit of this species does not extend beyond the southern Caribbean and Trinidad and Tobago, and thus does not occur on the Brazilian coast as previously believed. A distribution map of C. clypeatus is provided based on specimens in the collections of the National Museum of Natural History, Smithsonian Institution. New distribution records in the Gulf of Mexico and southern Caribbean, and morphological information, are included for Pagurus rotundimanus Wass, 1963, a species originally described from the Florida Keys but rarely reported since. Relevant remarks on the taxonomy, morphology, and distribution of all these species are included. The revised list of Paguroidea known from Brazil is updated, and now includes a total of 62 species in the families Pylochelidae (1), Diogenidae (27), Paguridae (28), and Parapaguridae (6). A synopsis of primary taxonomic works on western Atlantic Paguroidea is also presented. C1 [Lemaitre, Rafael] Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, Suitland, MD 20746 USA. [Tavares, Marcos] Univ Sao Paulo, Museu Zool, BR-04263000 Sao Paulo, SP, Brazil. RP Lemaitre, R (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, 4210 Silver Hill Rd, Suitland, MD 20746 USA. EM lemaitrr@si.edu; mdst@usp.br RI Museu de Zoologia da USP, MZ-USP/Q-2192-2016 FU Conselho Nacional de Desenvolvimento Cientifico e Tecnologico or CNpQ [301806/2010-1]; Petroleo Brasileiro S.A. or PETROBRAS [4600224970]; National Geographic Society's Committee for Research and Exploration [9102-12] FX This study was made possibly, in part, by research grants for studies on the systematics of decapod crustaceans provided to MT by Conselho Nacional de Desenvolvimento Cientifico e Tecnologico or CNpQ (Grant #301806/2010-1) and Petroleo Brasileiro S.A. or PETROBRAS (Grant #4600224970); and grants for DROP provided by the Smithsonian Institution's Consortium for Understanding and Sustaining a Biodiverse Planet, and the National Geographic Society's Committee for Research and Exploration (Grant #9102-12). We profusely thank the following individuals and their institutions: B.B. Brown, photographer with the Willemstad Seaquarium in Curacao, for allowing use of his outstanding images; P. Clark and H. Taylor (both NHM), for providing information and the photograph of Broderip's gastropod shells with the Coenobita specimens; D.L. Felder (ULLZ), for sharing photographs and information of specimens form his collections; Joel Braga (MZUSP), for photographs of species of Parapagurus; and J. Harasewych (USNM), for identification of the shells of Melongena melongena. The enthusiasm and cooperation of the DROP team in Curacao who collected specimens on board the Curasub and provided valuable information, are gratefully acknowledged; these include: C. Baldwin and C. Castillo (both USNM), B. B. Brown, and A. "Dutch" Schrier. Valuable specimens and/or information were also supplied by: M. Wicksten (Texas A&M University, College Station Texas); G. Navas and A. Bermudez (both Universidad de Cartagena, Colombia); and F. Mantelatto and M. Negri (both Faculty of Philosophy, Sciences and Letters at Ribeirao Preto, University of Sao Paulo) for specimens and information. This study is Ocean Heritage Foundation/Curacao Sea Aquarium/Substation Curacao contribution #16. NR 186 TC 3 Z9 3 U1 1 U2 19 PU MAGNOLIA PRESS PI AUCKLAND PA PO BOX 41383, AUCKLAND, ST LUKES 1030, NEW ZEALAND SN 1175-5326 EI 1175-5334 J9 ZOOTAXA JI Zootaxa PD AUG 4 PY 2015 VL 3994 IS 4 BP 451 EP 506 PG 56 WC Zoology SC Zoology GA CO7SD UT WOS:000359361200001 PM 26250287 ER PT J AU Bizau, JM Cubaynes, D Guilbaud, S Al Shorman, MM Gharaibeh, MF Ababneh, IQ Blancard, C McLaughlin, BM AF Bizau, J. M. Cubaynes, D. Guilbaud, S. Al Shorman, M. M. Gharaibeh, M. F. Ababneh, I. Q. Blancard, C. McLaughlin, B. M. TI K-shell photoionization of O+ and O2+ ions: Experiment and theory SO PHYSICAL REVIEW A LA English DT Article ID X-RAY SPECTROSCOPY; PHOTOABSORPTION CROSS-SECTIONS; LOW-LYING STATES; R-MATRIX THEORY; INTERSTELLAR-MEDIUM; OSCILLATOR-STRENGTHS; OXYGEN IONS; RESONANCE PHOTOIONIZATION; ISOELECTRONIC SEQUENCE; ELECTRON-IMPACT AB Absolute cross sections for the single and double K-shell photoionization of carbonlike O2+ and nitrogenlike O+ ions were measured in the 526-620-eV photon energy range by employing the ion-photon merged-beam technique at the SOLEIL synchrotron radiation facility. High-resolution spectroscopy up to E/Lambda E approximate to 5300 was achieved. Rich resonance structures observed in the experimental spectra are analyzed and identified with the aid of R-matrix and multiconfiguration Dirac-Fock (MCDF) methods. For these two atomic oxygen ions of particular astrophysical interest we characterized the strong 1s -> 2p and the weaker 1s -> np (n > 2) resonances observed. A detailed comparison of the energies of the 1s -> 2p resonances in the first members of the oxygen isonuclear sequence measured by synchrotron based experiments and the Chandra and XMM-Newton x-ray satellites is presented. C1 [Bizau, J. M.; Cubaynes, D.; Guilbaud, S.; Al Shorman, M. M.] Univ Paris 11, CNRS UMR 8214, ISMO, F-91405 Orsay, France. [Bizau, J. M.; Cubaynes, D.] Synchrotron SOLEIL LOrme Merisiers, F-91192 Gif Sur Yvette, France. [Gharaibeh, M. F.] Qatar Univ, Dept Math Stat & Phys, Doha, Qatar. [Ababneh, I. Q.] Jordan Univ Sci & Technol, Dept Phys, Irbid 22110, Jordan. [Blancard, C.] CEA DAM DIF, F-91297 Arpajon, France. [McLaughlin, B. M.] Queens Univ Belfast, Sch Math & Phys, CTAMOP, Belfast BT7 1NN, Antrim, North Ireland. [McLaughlin, B. M.] Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom & Mol Phys, Cambridge, MA 02138 USA. RP Bizau, JM (reprint author), Univ Paris 11, CNRS UMR 8214, ISMO, Batiment 350, F-91405 Orsay, France. EM jean-marc.bizau@u-psud.fr; b.mclaughlin@qub.ac.uk FU Scientific Research Support Fund, Jordan [Bas/2/02/2010]; SESAME - Lounsbery Foundation; U.S. National Science Foundation; RTRA network Triangle de la Physique; Queen's University Belfast; Office of Science of the U.S. Department of Energy [DE-AC05-00OR22725] FX The authors thank the SOLEIL staff and in particular E. Antonsson of the PLEIADES beam line for helpful assistance during the measurements, and J. Bozek and M. Patanen for their help in the energy calibration of the beam line. M.F.G. acknowledges funding from the Scientific Research Support Fund, Jordan, under Contract No. Bas/2/02/2010. I.Q.A. acknowledges financial support from the SESAME - Lounsbery Foundation for a training fellowship. B.M.M. acknowledges support from the U.S. National Science Foundation through a grant to ITAMP at the Harvard-Smithsonian Center for Astrophysics, the RTRA network Triangle de la Physique, and a visiting research fellowship (VRF) from Queen's University Belfast. We thank E. T. Kennedy for a careful reading of the manuscript and constructive comments. J. C. Raymond and R. K. Smith at the Harvard-Smithsonian Center for Astrophysics are acknowledged for many helpful discussions on the astrophysical applications. The R-matrix computational work was carried out at the National Energy Research Scientific Computing Center in Oakland, CA, USA and at the High Performance Computing Center Stuttgart (HLRS) of the University of Stuttgart, Stuttgart, Germany. This research also used resources of the Oak Ridge Leadership Computing Facility at the Oak Ridge National Laboratory, which is supported by the Office of Science of the U.S. Department of Energy under Contract No. DE-AC05-00OR22725. NR 58 TC 5 Z9 5 U1 5 U2 21 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 AUG 3 PY 2015 VL 92 IS 2 AR 023401 DI 10.1103/PhysRevA.92.023401 PG 14 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA CO1MO UT WOS:000358919600006 ER PT J AU Li, DH Shi, W Munroe, TA Gong, L Kong, XY AF Li, Dong-He Shi, Wei Munroe, Thomas A. Gong, Li Kong, Xiao-Yu TI Concerted Evolution of Duplicate Control Regions in the Mitochondria of Species of the Flatfish Family Bothidae (Teleostei: Pleuronectiformes) SO PLOS ONE LA English DT Article ID MAXIMUM-LIKELIHOOD; DNA-SEQUENCE; GENOME; REPLICATION; SNAKE; REARRANGEMENTS; PLATYSTERNON; MITOGENOME; PHYLOGENY; ORIGINS AB Mitogenomes of flatfishes (Pleuronectiformes) exhibit the greatest diversity of gene rearrangements in teleostean fishes. Duplicate control regions (CRs) have been found in the mito-genomes of two flatfishes, Samariscus latus (Samaridae) and Laeops lanceolata (Bothidae), which is rare in teleosts. It has been reported that duplicate CRs have evolved in a concerted fashion in fishes and other animals, however, whether concerted evo-lution exists in flatfishes remains unknown. In this study, based on five newly sequenced and six previously reported mitogenomes of lefteye flounders in the Bothidae, we explored whether duplicate CRs and concerted evolution exist in these species. Results based on the present study and previous reports show that four out of eleven bothid species examined have duplicate CRs of their mitogenomes. The core regions of the duplicate CRs of mitogenomes in the same species have identical, or nearly identical, sequences when compared to each other. This pattern fits the typical characteristics of concerted evolution. Additionally, phylogenetic and ancestral state reconstruction analysis also provided evidence to support the hypothesis that duplicate CRs evolved concertedly. The core region of concerted evolution is situated at the conserved domains of the CR of the mitogenome from the termination associated sequences (TASs) to the conserved sequence blocks (CSBs). Commonly, this region is con-sidered to regulate mitochondrial replication and transcription. Thus, we hypothesize that the cause of concerted evolution of the duplicate CRs in the mtDNAs of these four bothids may be related to some function of the conserved sequences of the CRs during mitochondrial rep-lication and transcription. We hope our results will provide fresh insight into the molecular mechanisms related to replication and evolution of mitogenomes. C1 [Li, Dong-He; Shi, Wei; Gong, Li; Kong, Xiao-Yu] Chinese Acad Sci, Key Lab Trop Marine Bio resources & Ecol, South China Sea Inst Oceanol, Guangzhou 510301, Guangdong, Peoples R China. [Li, Dong-He; Shi, Wei; Gong, Li; Kong, Xiao-Yu] Chinese Acad Sci, Guangdong Prov Key Lab Appl Marine Biol, South China Sea Inst Oceanol, Guangzhou 510301, Guangdong, Peoples R China. [Li, Dong-He; Shi, Wei; Gong, Li] South China Sea Bioresource Exploitat & Utilizat, Guangzhou 510301, Guangdong, Peoples R China. [Li, Dong-He; Gong, Li] Univ Chinese Acad Sci, Beijing 100049, Peoples R China. [Munroe, Thomas A.] NOAA, Natl Systemat Lab NMFS, Smithsonian Inst NHB, Washington, DC 20013 USA. RP Shi, W (reprint author), Chinese Acad Sci, Key Lab Trop Marine Bio resources & Ecol, South China Sea Inst Oceanol, Guangzhou 510301, Guangdong, Peoples R China. EM shiwei@scsio.ac.cn; xykong@scsio.ac.cn FU Natural Science Foundation of China [31471979, 41206134, 30870283]; Science and Technology Planning Project of Guangdong Province, China [2014B030301064] FX This work was supported by the Natural Science Foundation of China (grant numbers 31471979, 41206134, 30870283) and Science and Technology Planning Project of Guangdong Province, China (2014B030301064). NR 49 TC 2 Z9 2 U1 2 U2 8 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 AUG 3 PY 2015 VL 10 IS 8 AR e0134580 DI 10.1371/journal.pone.0134580 PG 13 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA CO1UY UT WOS:000358942400029 PM 26237419 ER PT J AU Archambault, S Archer, A Beilicke, M Benbow, W Bird, R Biteau, J Bouvier, A Bugaev, V Cardenzana, JV Cerruti, M Chen, X Ciupik, L Connolly, MP Cui, W Dickinson, HJ Dumm, J Eisch, JD Errando, M Falcone, A Feng, Q Finley, JP Fleischhack, H Fortin, P Fortson, L Furniss, A Gillanders, GH Griffin, S Griffiths, ST Grube, J Gyuk, G Hakansson, N Hanna, D Holder, J Humensky, TB Johnson, CA Kaaret, P Kar, P Kertzman, M Khassen, Y Kieda, D Krause, M Krennrich, F Kumar, S Lang, MJ Maier, G McArthur, S McCann, A Meagher, K Millis, J Moriarty, P Mukherjee, R Nieto, D de Bhroithe, AO Ong, RA Otte, AN Park, N Pohl, M Popkow, A Prokoph, H Pueschel, E Quinn, J Ragan, K Reyes, LC Reynolds, PT Richards, GT Roache, E Santander, M Sembroski, GH Shahinyan, K Smith, AW Staszak, D Telezhinsky, I Tucci, JV Tyler, J Varlotta, A Vincent, S Wakely, SP Weinstein, A Welsing, R Wilhelm, A Williams, DA Zitzer, B Hughes, ZD AF Archambault, S. Archer, A. Beilicke, M. Benbow, W. Bird, R. Biteau, J. Bouvier, A. Bugaev, V. Cardenzana, J. V. Cerruti, M. Chen, X. Ciupik, L. Connolly, M. P. Cui, W. Dickinson, H. J. Dumm, J. Eisch, J. D. Errando, M. Falcone, A. Feng, Q. Finley, J. P. Fleischhack, H. Fortin, P. Fortson, L. Furniss, A. Gillanders, G. H. Griffin, S. Griffiths, S. T. Grube, J. Gyuk, G. Hakansson, N. Hanna, D. Holder, J. Humensky, T. B. Johnson, C. A. Kaaret, P. Kar, P. Kertzman, M. Khassen, Y. Kieda, D. Krause, M. Krennrich, F. Kumar, S. Lang, M. J. Maier, G. McArthur, S. McCann, A. Meagher, K. Millis, J. Moriarty, P. Mukherjee, R. Nieto, D. de Bhroithe, A. O'Faolain Ong, R. A. Otte, A. N. Park, N. Pohl, M. Popkow, A. Prokoph, H. Pueschel, E. Quinn, J. Ragan, K. Reyes, L. C. Reynolds, P. T. Richards, G. T. Roache, E. Santander, M. Sembroski, G. H. Shahinyan, K. Smith, A. W. Staszak, D. Telezhinsky, I. Tucci, J. V. Tyler, J. Varlotta, A. Vincent, S. Wakely, S. P. Weinstein, A. Welsing, R. Wilhelm, A. Williams, D. A. Zitzer, B. Hughes, Z. D. CA Veritas Collaboration TI VERITAS DETECTION OF gamma-RAY FLARING ACTIVITY FROM THE BL LAC OBJECT 1ES 1727+502 DURING BRIGHT MOONLIGHT OBSERVATIONS SO ASTROPHYSICAL JOURNAL LA English DT Article DE BL Lacertae objects: individual (1ES 1727+502); galaxies: active; gamma rays: galaxies; radiation mechanisms: non-thermal ID LARGE-AREA TELESCOPE; SELF-COMPTON MODEL; SPECTRAL ENERGY-DISTRIBUTION; LACERTAE OBJECTS; GALACTIC NUCLEI; HOST GALAXIES; SOURCE CATALOG; CRAB-NEBULA; TEV BLAZARS; FERMI ERA AB During moonlit nights, observations with ground-based Cherenkov telescopes at very high energies (VHEs, E > 100 GeV) are constrained since the photomultiplier tubes (PMTs) in the telescope camera are extremely sensitive to the background moonlight. Observations with the VERITAS telescopes in the standard configuration are performed only with a moon illumination less than 35% of full moon. Since 2012, the VERITAS collaboration has implemented a new observing mode under bright moonlight, by either reducing the voltage applied to the PMTs (reduced-high-voltage; RHV configuration), or by utilizing UV-transparent filters. While these operating modes result in lower sensitivity and increased energy thresholds, the extension of the available observing time is useful for monitoring variable sources such as blazars and sources requiring spectral measurements at the highest energies. In this paper we report the detection of gamma-ray flaring activity from the BL Lac object 1ES 1727+502 during RHV observations. This detection represents the first evidence of VHE variability from this blazar. The integral flux is (1.1 +/- 0.2) x 10(-11) cm(-2) s(-1) above 250 GeV, which is about five times higher than the low-flux state. The detection triggered additional VERITAS observations during standard dark-time. Multiwavelength observations with the FLWO 48 '' telescope, and the Swift and Fermi satellites are presented and used to produce the first spectral energy distribution (SED) of this object during gamma-ray flaring activity. The SED is then fitted with a standard synchrotron-self-Compton model, placing constraints on the properties of the emitting region and of the acceleration mechanism at the origin of the relativistic particle population in the jet. C1 [Archambault, S.; Griffin, S.; Hanna, D.; Ragan, K.; Staszak, D.; Tyler, J.] McGill Univ, Dept Phys, 3600 Univ St, Montreal, PQ H3A 2T8, Canada. [Archer, A.; Beilicke, M.; Bugaev, V.] Washington Univ, Dept Phys, St Louis, MO 63130 USA. [Benbow, W.; Cerruti, M.; Fortin, P.; Roache, E.] Harvard Smithsonian Ctr Astrophys, Fred Lawrence Whipple Observ, Amado, AZ 85645 USA. [Bird, R.; Khassen, Y.; Pueschel, E.; Quinn, J.] Univ Coll Dublin, Sch Phys, Dublin 4, Ireland. [Biteau, J.; Bouvier, A.; Furniss, A.; Johnson, C. A.; Williams, D. A.; Hughes, Z. D.] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Santa Cruz, CA 95064 USA. [Biteau, J.; Bouvier, A.; Furniss, A.; Johnson, C. A.; Williams, D. A.; Hughes, Z. D.] Univ Calif Santa Cruz, Dept Phys, Santa Cruz, CA 95064 USA. [Cardenzana, J. V.; Dickinson, H. J.; Eisch, J. D.; Krennrich, F.; Weinstein, A.] Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA. [Chen, X.; Hakansson, N.; Pohl, M.; Telezhinsky, I.; Wilhelm, A.] Univ Potsdam, Inst Phys & Astron, D-14476 Potsdam, Germany. [Chen, X.; Fleischhack, H.; Krause, M.; Maier, G.; de Bhroithe, A. O'Faolain; Pohl, M.; Prokoph, H.; Telezhinsky, I.; Vincent, S.; Welsing, R.; Wilhelm, A.] DESY, D-15738 Zeuthen, Germany. [Ciupik, L.; Grube, J.; Gyuk, G.] Adler Planetarium & Astron Museum, Dept Astron, Chicago, IL 60605 USA. [Connolly, M. P.; Gillanders, G. H.; Lang, M. J.; Moriarty, P.] Natl Univ Ireland Galway, Sch Phys, Galway, Ireland. [Cui, W.; Feng, Q.; Finley, J. P.; Sembroski, G. H.; Tucci, J. V.; Varlotta, A.] Purdue Univ, Dept Phys & Astron, W Lafayette, IN 47907 USA. [Dumm, J.; Fortson, L.; Shahinyan, K.] Univ Minnesota, Sch Phys & Astron, Minneapolis, MN 55455 USA. [Errando, M.; Mukherjee, R.; Santander, M.] Columbia Univ, Barnard Coll, Dept Phys & Astron, New York, NY 10027 USA. [Falcone, A.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Griffiths, S. T.; Kaaret, P.] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA. [Holder, J.; Kumar, S.] Univ Delaware, Dept Phys & Astron, Newark, DE 19716 USA. [Holder, J.; Kumar, S.] Univ Delaware, Bartol Res Inst, Newark, DE 19716 USA. [Humensky, T. B.; Nieto, D.] Columbia Univ, Dept Phys, New York, NY 10027 USA. [Kar, P.; Kieda, D.; Smith, A. W.] Univ Utah, Dept Phys & Astron, Salt Lake City, UT 84112 USA. [Kertzman, M.] Depauw Univ, Dept Phys & Astron, Greencastle, IN 46135 USA. [McArthur, S.; Park, N.; Wakely, S. P.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA. [McCann, A.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Meagher, K.; Otte, A. N.; Richards, G. T.] Georgia Inst Technol, Sch Phys, Atlanta, GA 30332 USA. [Meagher, K.; Otte, A. N.; Richards, G. T.] Georgia Inst Technol, Ctr Relativist Astrophys, Atlanta, GA 30332 USA. [Millis, J.] Anderson Univ, Dept Phys Sci & Engn, Anderson, IN 46012 USA. [Ong, R. A.; Popkow, A.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. [Reyes, L. C.] Calif Polytech State Univ San Luis Obispo, Dept Phys, San Luis Obispo, CA 94307 USA. [Reynolds, P. T.] Cork Inst Technol, Dept Appl Sci, Cork, Ireland. [Zitzer, B.] Argonne Natl Lab, Argonne, IL 60439 USA. RP Archambault, S (reprint author), McGill Univ, Dept Phys, 3600 Univ St, Montreal, PQ H3A 2T8, Canada. EM matteo.cerruti@cfa.harvard.edu; griffins@physics.mcgill.ca RI Nieto, Daniel/J-7250-2015; OI Nieto, Daniel/0000-0003-3343-0755; Pueschel, Elisa/0000-0002-0529-1973 FU U.S. Department of Energy Office of Science; U.S. National Science Foundation; Smithsonian Institution; NSERC in Canada; Science Foundation Ireland (SFI) [10/RFP/AST2748]; STFC in the U.K. FX The authors wish to thank Kari Nilsson for useful discussions about the host-galaxy contribution, as well as the anonymous referee for his/her comments which improved the present work. This research is supported by grants from the U.S. Department of Energy Office of Science, the U.S. National Science Foundation and the Smithsonian Institution, by NSERC in Canada, by Science Foundation Ireland (SFI 10/RFP/AST2748) and by STFC in the U.K. We acknowledge the excellent work of the technical support staff at the Fred Lawrence Whipple Observatory and at the collaborating institutions in the construction and operation of the instrument. The VERITAS Collaboration is grateful to Trevor Weekes for his seminal contributions and leadership in the field of VHE gamma-ray astrophysics, which made this study possible. NR 88 TC 6 Z9 6 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 AUG 1 PY 2015 VL 808 IS 2 AR 110 DI 10.1088/0004-637X/808/2/110 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DF0BA UT WOS:000371002400005 ER PT J AU Buchhave, LA Latham, DW AF Buchhave, Lars A. Latham, David W. TI THE METALLICITIES OF STARS WITH AND WITHOUT TRANSITING PLANETS SO ASTROPHYSICAL JOURNAL LA English DT Article DE planetary systems; surveys; techniques: spectroscopic ID HOST STARS; KEPLER; MASS; SPECTROSCOPY AB Host star metallicities have been used to infer observational constraints on planet formation throughout the history of the exoplanet field. The giant planet metallicity correlation has now been widely accepted, but questions remain as to whether the metallicity correlation extends to the small terrestrial-sized planets. Here, we report metallicities for a sample of 518 stars in the Kepler field that have no detected transiting planets and compare their metallicity distribution to a sample of stars that hosts small planets (R-p < 1.7 R-circle plus). Importantly, both samples have been analyzed in a homogeneous manner using the same set of tools (Stellar Parameters Classification tool). We find the average metallicity of the sample of stars without detected transiting planets to be [m/H](SNTP,dwarf) = -0.02 +/- 0.02 dex and the sample of stars hosting small planets to be [m/H](STP) = -0.02 +/- 0.02 dex. The average metallicities of the two samples are indistinguishable within the uncertainties, and the two-sample Kolmogorov-Smirnov test yields a p-value of 0.68 (0.41 sigma), indicating a failure to reject the null hypothesis that the two samples are drawn from the same parent population. We conclude that the homogeneous analysis of the data presented here supports the hypothesis that stars hosting small planets have a metallicity similar to stars with no known transiting planets in the same area of the sky. C1 [Buchhave, Lars A.; Latham, David W.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Buchhave, Lars A.] Univ Copenhagen, Nat Hist Museum Denmark, Ctr Star & Planet Format, DK-1350 Copenhagen, Denmark. RP Buchhave, LA (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. OI Buchhave, Lars A./0000-0003-1605-5666; Latham, David/0000-0001-9911-7388 NR 26 TC 17 Z9 17 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD AUG 1 PY 2015 VL 808 IS 2 AR 187 DI 10.1088/0004-637X/808/2/187 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DF0BA UT WOS:000371002400083 ER PT J AU Civano, F Hickox, RC Puccetti, S Comastri, A Mullaney, JR Zappacosta, L LaMassa, SM Aird, J Alexander, DM Ballantyne, DR Bauer, FE Brandt, WN Boggs, SE Christensen, FE Craig, WW Del-Moro, A Elvis, M Forster, K Gandhi, P Grefenstette, BW Hailey, CJ Harrison, FA Lansbury, GB Luo, B Madsen, K Saez, C Stern, D Treister, E Urry, MC Wik, DR Zhang, W AF Civano, F. Hickox, R. C. Puccetti, S. Comastri, A. Mullaney, J. R. Zappacosta, L. LaMassa, S. M. Aird, J. Alexander, D. M. Ballantyne, D. R. Bauer, F. E. Brandt, W. N. Boggs, S. E. Christensen, F. E. Craig, W. W. Del-Moro, A. Elvis, M. Forster, K. Gandhi, P. Grefenstette, B. W. Hailey, C. J. Harrison, F. A. Lansbury, G. B. Luo, B. Madsen, K. Saez, C. Stern, D. Treister, E. Urry, M. C. Wik, D. R. Zhang, W. TI THE NuSTAR EXTRAGALACTIC SURVEYS: OVERVIEW AND CATALOG FROM THE COSMOS FIELD SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: nuclei; X-rays: general ID ACTIVE GALACTIC NUCLEI; X-RAY LUMINOSITY; MEDIUM-SENSITIVITY SURVEY; POINT-SOURCE CATALOG; CHANDRA DEEP SURVEY; COMPTON-THICK AGN; SWIFT-BAT SURVEY; ALL-SKY SURVEY; XMM-NEWTON; HELLAS2XMM SURVEY AB To provide the census of the sources contributing to the X-ray background peak above 10 keV, Nuclear Spectroscopic Telescope Array (NuSTAR) is performing extragalactic surveys using a three-tier "wedding cake" approach. We present the NuSTAR survey of the COSMOS field, the medium sensitivity, and medium area tier, covering 1.7 deg(2) and overlapping with both Chandra and XMM-Newton data. This survey consists of 121 observations for a total exposure of similar to 3 Ms. To fully exploit these data, we developed a new detection strategy, carefully tested through extensive simulations. The survey sensitivity at 20% completeness is 5.9, 2.9, and 6.4 x 10(-14) erg cm(-2) s(-1) in the 3-24, 3-8, and 8-24 keV bands, respectively. By combining detections in 3 bands, we have a sample of 91 NuSTAR sources with 10(42)-10(45.5) erg s(-1) luminosities and redshift z = 0.04-2.5. Thirty-two sources are detected in the 8-24 keV band with fluxes similar to 100 times fainter than sources detected by Swift-BAT. Of the 91 detections, all but 4 are associated with a Chandra and/or XMM-Newton point-like counterpart. One source is associated with an extended lower energy X-ray source. We present the X-ray (hardness ratio and luminosity) and optical-to-X-ray properties. The observed fraction of candidate Compton-thick active galactic nuclei measured from the hardness ratio is between 13%-20%. We discuss the spectral properties of NuSTAR J100259+0220.6 (ID 330) at z = 0.044, with the highest hardness ratio in the entire sample. The measured column density exceeds 10(24) cm(-2), implying the source is Compton-thick. This source was not previously recognized as such without the >10 keV data. C1 [Civano, F.; LaMassa, S. M.; Urry, M. C.] Yale Ctr Astron & Astrophys, 260 Whitney Ave, New Haven, CT 06520 USA. [Civano, F.; Hickox, R. C.] Dartmouth Coll, Dept Phys & Astron, Wilder Lab 6127, Hanover, NH 03755 USA. [Civano, F.; Elvis, M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Puccetti, S.] ASDC ASI, I-00133 Rome, Italy. [Comastri, A.] INAF Osservatorio Astron Bologna, I-40127 Bologna, Italy. [Mullaney, J. R.] Univ Sheffield, Dept Phys & Astron, Sheffield S3 7RH, S Yorkshire, England. [Zappacosta, L.] INAF Osservatorio Astron Roma, I-00040 Monte Porzio Catone, RM, Italy. [Aird, J.; Alexander, D. M.; Del-Moro, A.; Gandhi, P.; Lansbury, G. B.] Univ Durham, Dept Phys, Durham DH1 3LE, England. [Aird, J.] Univ Cambridge, Inst Astron, Madingley Rd, Cambridge CB3 0HA, England. [Ballantyne, D. R.] Georgia Inst Technol, Sch Phys, Ctr Relativist Astrophys, Atlanta, GA 30332 USA. [Bauer, F. E.; Luo, B.; Saez, C.] Pontificia Univ Catolica Chile, Inst Astrofis, Fac Fis, Santiago 22, Chile. [Bauer, F. E.; Luo, B.] Millennium Inst Astrophys, Santiago, Chile. [Bauer, F. E.] Space Sci Inst, Boulder, CO 80301 USA. [Brandt, W. N.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Brandt, W. N.] Penn State Univ, Inst Gravitat & Cosmos, University Pk, PA 16802 USA. [Brandt, W. N.] Penn State Univ, Dept Phys, University Pk, PA 16802 USA. [Boggs, S. E.; Craig, W. W.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Christensen, F. E.] Tech Univ Denmark, DTU Space Natl Space Inst, DK-2800 Lyngby, Denmark. [Craig, W. W.] Lawrence Livermore Natl Lab, Livermore, CA USA. [Forster, K.; Grefenstette, B. W.; Harrison, F. A.; Madsen, K.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA. [Gandhi, P.] Univ Southampton, Sch Phys Astron, Southampton SO17 1BJ, Hants, England. [Hailey, C. J.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA. [Stern, D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Treister, E.] Univ Concepcion, Dept Astron, Concepcion, Chile. [Wik, D. R.; Zhang, W.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Civano, F (reprint author), Yale Ctr Astron & Astrophys, 260 Whitney Ave, New Haven, CT 06520 USA. RI Boggs, Steven/E-4170-2015; OI Boggs, Steven/0000-0001-9567-4224; Puccetti, Simonetta/0000-0002-2734-7835; Comastri, Andrea/0000-0003-3451-9970; Ballantyne, David/0000-0001-8128-6976; Urry, Meg/0000-0002-0745-9792 FU National Aeronautics and Space Administration; NASA [11-ADAP110218, GO3-14150C]; Science and Technology Facilities Council [ST/I001573/1]; NSF [AST 1008067]; NuSTAR grant [44A-1092750]; NASA ADP grant [NNX10AC99G]; V. M. Willaman Endowment; CONICYT-Chile [Basal-CATA PFB-06/2007]; FONDECYT [1141218, 1120061]; "EMBIGGEN" Anillo [ACT1101]; Ministry of Economy, Development, and Tourism's Millennium Science Initiative [IC120009]; Center of Excellence in Astrophysics and Associated Technologies; ASI/INAF [I/037/12/0] FX We thank the anonymous referee for interesting comments and A. Goulding and M. Rose for useful discussions. This work made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. We thank the NuSTAR Operations, Software and Calibration teams for support with the execution and analysis of these observations. This research has made use of the NuSTAR Data Analysis Software (NUSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA). We acknowledge support from the NASA grants 11-ADAP110218 and GO3-14150C (FC); from the Science and Technology Facilities Council ST/I001573/1 (ADM, DMA); NSF award AST 1008067 (DRB); NuSTAR grant 44A-1092750, NASA ADP grant NNX10AC99G, and the V. M. Willaman Endowment (WNB, BL); CONICYT-Chile grants Basal-CATA PFB-06/2007 (FEB), FONDECYT 1141218 (FEB), and "EMBIGGEN" Anillo ACT1101 (FEB, ET); the Ministry of Economy, Development, and Tourism's Millennium Science Initiative through grant IC120009, awarded to The Millennium Institute of Astrophysics, MAS (FEB); the Center of Excellence in Astrophysics and Associated Technologies (PFB 06) and by the FONDECYT regular grant 1120061 (ET); financial support under ASI/INAF contract I/037/12/0 (LZ). NR 96 TC 10 Z9 10 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD AUG 1 PY 2015 VL 808 IS 2 AR 185 DI 10.1088/0004-637X/808/2/185 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DF0BA UT WOS:000371002400081 ER PT J AU Dumusque, X Pepe, F Lovis, C Latham, DW AF Dumusque, Xavier Pepe, Francesco Lovis, Christophe Latham, David W. TI CHARACTERIZATION OF A SPURIOUS ONE-YEAR SIGNAL IN HARPS DATA SO ASTROPHYSICAL JOURNAL LA English DT Article DE instrumentation: detectors; instrumentation: spectrographs; methods: data analysis; planets and satellites: terrestrial planets; techniques: radial velocities ID EARTH-LIKE PLANETS; SOLAR-LIKE OSCILLATIONS; ALPHA-CENTAURI-B; RADIAL-VELOCITY; MASS PLANET; I.; SEARCH; STARS; SUN AB The HARPS spectrograph is showing an extreme stability, close to the m s(-1) level, over more than 10 years of data. However, the radial velocities of some stars are contaminated by a spurious one-year signal with an amplitude that can be as high as a few m s(-1). This signal is in opposition of phase with the revolution of Earth around the Sun and can be explained by the deformation of spectral lines crossing block stitchings of the CCD when the spectrum of an observed star is alternatively blueshifted and redshifted due to the motion of Earth around the Sun. This annual perturbation can be suppressed by either removing those affected spectral lines from the correlation mask used by the cross-correlation technique to derive precise radial velocities, or by simply fitting a yearly sinusoid to the radial velocity data. This is mandatory if we want to detect long-period low-amplitude signals in the HARPS radial velocities of quiet solar-type stars. C1 [Dumusque, Xavier; Latham, David W.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Pepe, Francesco; Lovis, Christophe] Univ Geneva, Astron Observ, CH-1290 Sauverny, Switzerland. RP Dumusque, X (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM xdumusque@cfa.harvard.edu FU NASA from MIT [5710003554] FX We thank the referee for valuable comments and suggestions that improved the first version of the paper. X.D. thanks NASA's Transiting Exoplanet Survey Satellite (TESS) mission for partial support via sub-award 5710003554 from MIT to SAO. We are grateful to all of the technical and scientific collaborators of the HARPS Consortium, ESO Headquarters, and ESO La Silla who have contributed their extraordinary passion and valuable work to the success of the HARPS project. NR 25 TC 8 Z9 8 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD AUG 1 PY 2015 VL 808 IS 2 AR 171 DI 10.1088/0004-637X/808/2/171 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DF0BA UT WOS:000371002400066 ER PT J AU Favre, C Bergin, EA Neill, JL Crockett, NR Zhang, QZ Lis, DC AF Favre, Cecile Bergin, Edwin A. Neill, Justin L. Crockett, Nathan R. Zhang, Qizhou Lis, Dariusz C. TI THE DISTRIBUTION OF DEUTERATED FORMALDEHYDE WITHIN ORION-KL SO ASTROPHYSICAL JOURNAL LA English DT Article DE astrochemistry; ISM: abundances; ISM: individual objects (Orion-KL); ISM: molecules; line: identification ID EXTRAORDINARY SOURCES HEXOS; LIMITED MILLIMETER SURVEY; LINE SURVEY; SUBMILLIMETER ARRAY; HERSCHEL OBSERVATIONS; THERMAL-DESORPTION; ORGANIC-MOLECULES; PROPER MOTIONS; STAR-FORMATION; HOT CORE AB We report the first high angular resolution imaging (3 ''.4 x 3 ''.0) of deuterated formaldehyde (HDCO) toward Orion- KL, carried out with the Submillimeter Array. We find that the spatial distribution of the formaldehyde emission systematically differs from that of methanol: while methanol is found toward the inner part of the region, HDCO is found in colder gas that wraps around the methanol emission on four sides. The HDCO/H2CO ratios are determined to be 0.003- 0.009 within the region, up to an order of magnitude higher than the D/H measured for methanol. These findings strengthen the previously suggested hypothesis that there are differences in the chemical pathways leading to HDCO (via deuterated gas- phase chemistry) and deuterated methanol (through conversion of formaldehyde into methanol on the surface of icy grain mantles). C1 [Favre, Cecile; Bergin, Edwin A.; Neill, Justin L.] Univ Michigan, Dept Astron, 500 Church St, Ann Arbor, MI 48109 USA. [Zhang, Qizhou] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. [Lis, Dariusz C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Lis, Dariusz C.] Univ Paris 06, Sorbonne Univ, CNRS, LERMA,Observ Paris,PSL Res Univ, F-75014 Paris, France. CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA. EM cfavre@umich.edu OI Zhang, Qizhou/0000-0003-2384-6589 FU NASA by JPL/Caltech FX Support for this work was provided by NASA (Herschel OT funding) through an award issued by JPL/Caltech. This paper makes use of SMA data. C.F. thanks Tzu-Cheng Peng for helpful discussions. NR 76 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 EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD AUG 1 PY 2015 VL 808 IS 2 AR 155 DI 10.1088/0004-637X/808/2/155 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DF0BA UT WOS:000371002400050 ER PT J AU Jiang, XJ Liu, HYB Zhang, QZ Wang, JZ Zhang, ZY Li, J Gao, Y Gu, QS AF Jiang, Xue-Jian Liu, Hauyu Baobab Zhang, Qizhou Wang, Junzhi Zhang, Zhi-Yu Li, Juan Gao, Yu Gu, Qiusheng TI SMA OBSERVATIONS OF C2H IN HIGH-MASS STAR-FORMING REGIONS SO ASTROPHYSICAL JOURNAL LA English DT Article DE astrochemistry; ISM: abundances; molecular processes; stars: early-type; stars: formation; stars: individual (G10.6-0.4, ON1, W33, and AFGL 490) ID SPATIALLY-RESOLVED CHEMISTRY; CARBON-CHAIN MOLECULES; H-II REGIONS; OB CLUSTERS; INFRARED OBSERVATIONS; INTERSTELLAR CLOUDS; PHYSICAL STRUCTURE; DENSITY STRUCTURE; DUST CONTINUUM; HII REGION AB C2H is a representative hydrocarbon that is abundant and ubiquitous in the interstellar medium. To study its chemical properties, we present Submillimeter Array observations of the C2H N = 3-2 and. HC3N J = 30-29 transitions. and the 1.1 mm continuum emission toward four OB cluster-forming regions, AFGL 490, ON 1, W33 Main, and G10.6-0.4, which cover a bolometric luminosity range of similar to 10(3)-10(6) L-circle dot. We found that on large scales, the C2H emission traces the dense molecular envelope. However, for all observed sources, the peaks of C2H emission are offset by several times. 104 AU from the peaks of 1.1 mm continuum emission, where the most luminous stars are located. By comparing the distribution and profiles of C2H hyperfine lines and the 1.1 mm continuum emission, we find that the C2H column density (and abundance) around the 1.1 mm continuum peaks is lower than those in the ambient gas envelope. Chemical models suggest that C2H might be transformed to other species owing to increased temperature and density;. thus, its reduced abundance could be the signpost of the heated molecular gas in the similar to 10(4) AU vicinity around the embedded high-mass stars. Our results support such theoretical prediction for centrally embedded similar to 10(3)-10(6) L-circle dot OB star-forming cores, while future higher-resolution observations are required to examine the C2H transformation around the localized sites of high-mass star formation. C1 [Jiang, Xue-Jian; Gao, Yu] Chinese Acad Sci, Purple Mt Observ, 2 W Beijing Rd, Nanjing 210008, Jiangsu, Peoples R China. [Jiang, Xue-Jian; Gao, Yu] Chinese Acad Sci, Key Lab Radio Astron, 2 W Beijing Rd, Nanjing 210008, Jiangsu, Peoples R China. [Jiang, Xue-Jian; Zhang, Qizhou] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Jiang, Xue-Jian; Gu, Qiusheng] Nanjing Univ, Minist Educ, Key Lab Modern Astron & Astrophys, Nanjing 210093, Jiangsu, Peoples R China. [Jiang, Xue-Jian; Gu, Qiusheng] Collaborat Innovat Ctr Modern Astron & Space Expl, Nanjing 210093, Jiangsu, Peoples R China. [Liu, Hauyu Baobab] Acad Sinica, Inst Astron & Astrophys, Taipei 106, Taiwan. [Wang, Junzhi; Li, Juan] Chinese Acad Sci, Shanghai Astron Observ, Shanghai 200030, Peoples R China. [Zhang, Zhi-Yu] Univ Edinburgh, Royal Observ, Inst Astron, Edinburgh EH9 3HJ, Midlothian, Scotland. [Zhang, Zhi-Yu] ESO, D-85748 Munich, Germany. RP Jiang, XJ (reprint author), Chinese Acad Sci, Purple Mt Observ, 2 W Beijing Rd, Nanjing 210008, Jiangsu, Peoples R China. EM xjjiang@pmo.ac.cn OI Zhang, Qizhou/0000-0003-2384-6589; Liu, Hauyu Baobab/0000-0003-2300-2626; Zhang, Zhiyu/0000-0002-7299-2876 FU National Natural Science Foundation of China [11390373, 11273015, 11133001, 11328301]; Strategic Priority Research Program "The Emergence of Cosmological Structures" of the Chinese Academy of Sciences [XDB09000000]; National Basic Research Program (973 program) [2013CB834905]; Specialized Research Fund for the Doctoral Program of Higher Education [20100091110009]; European Research Council (ERC) FX We acknowledge the SMA staff for their help during and after the observations. X.J. thanks Keping Qiu for informative discussions on the source ON 1. This work is supported under the National Natural Science Foundation of China (grants 11390373, 11273015, 11133001, and 11328301), the Strategic Priority Research Program "The Emergence of Cosmological Structures" of the Chinese Academy of Sciences (grant XDB09000000), the National Basic Research Program (973 program No. 2013CB834905), and Specialized Research Fund for the Doctoral Program of Higher Education (20100091110009). Z.-Y.Z. acknowledges support from the European Research Council (ERC) in the form of Advanced Grant. COSMICISM. This research made use of Matplotlib (Hunter 2007) and APLpy, an open-source plotting package for Python hosted at http://aplpy.github.com. NR 74 TC 2 Z9 2 U1 1 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD AUG 1 PY 2015 VL 808 IS 2 AR 114 DI 10.1088/0004-637X/808/2/114 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DF0BA UT WOS:000371002400009 ER PT J AU Jones, DE Kashyap, VL van Dyk, DA AF Jones, David E. Kashyap, Vinay L. van Dyk, David A. TI DISENTANGLING OVERLAPPING ASTRONOMICAL SOURCES USING SPATIAL AND SPECTRAL INFORMATION SO ASTROPHYSICAL JOURNAL LA English DT Article DE methods: statistical; techniques: image processing; X-rays: stars ID BAYESIAN-ANALYSIS; UNCERTAINTIES; COMPUTATION; CALIBRATION; MIXTURES; COUNTS; MODELS; FIELDS; LIMITS AB We present a powerful new algorithm that combines both spatial information (event locations and the point-spread function) and spectral information (photon energies) to separate photons from overlapping sources. We use Bayesian statistical methods to simultaneously infer the number of overlapping sources, to probabilistically separate the photons among the sources, and to fit the parameters describing the individual sources. Using the Bayesian joint posterior distribution, we are able to coherently quantify the uncertainties associated with all these parameters. The advantages of combining spatial and spectral information are demonstrated through a simulation study. The utility of the approach is then illustrated by analysis of observations of FK Aqr and FL Aqr with the XMM-Newton Observatory and the central region of the Orion Nebula Cluster with the Chandra X-ray Observatory. C1 [Jones, David E.] Harvard Univ, Dept Stat, 1 Oxford St, Cambridge, MA 02138 USA. [Kashyap, Vinay L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [van Dyk, David A.] Univ London Imperial Coll Sci Technol & Med, Dept Math, Stat Sect, London SW7 2AZ, England. RP Jones, DE (reprint author), Harvard Univ, Dept Stat, 1 Oxford St, Cambridge, MA 02138 USA. EM djones@fas.harvard.edu FU Smithsonian Competitive Grants Program for Science Fund [40488100HH0043]; CHASC International Astrostatistics Center; NSF [DMS 1208791, DMS 1209232]; Harvard Statistics Department; NASA [NAS8-03060]; Chandra grant [AR0-11001X]; Wolfson Research Merit Award by British Royal Society; Marie-Curie Career Integration Grant by European Commission FX This work was supported by the Smithsonian Competitive Grants Program for Science Fund 40488100HH0043 and was conducted under the auspices of the CHASC International Astrostatistics Center. CHASC is supported by NSF grants DMS 1208791 and DMS 1209232. D.E.J. acknowledges support from the Harvard Statistics Department, V.L.K. from a NASA contract to the Chandra X-Ray Center NAS8-03060 and from Chandra grant AR0-11001X, and D.v.D. from a Wolfson Research Merit Award provided by the British Royal Society and from a Marie-Curie Career Integration Grant provided by the European Commission. In addition, we thank CHASC members for many helpful discussions, especially Xiao-Li Meng, Andreas Zezas, Aneta Siemiginowska, Lazhi Wang, and Alex Blocker. NR 38 TC 1 Z9 1 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD AUG 1 PY 2015 VL 808 IS 2 AR 137 DI 10.1088/0004-637X/808/2/137 PG 24 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DF0BA UT WOS:000371002400032 ER PT J AU Mullaney, JR Del-Moro, A Aird, J Alexander, DM Civano, FM Hickox, RC Lansbury, GB Ajello, M Assef, R Ballantyne, DR Balokovic, M Bauer, FE Brandt, WN Boggs, SE Brightman, M Christensen, FE Comastri, A Craig, WW Elvis, M Forster, K Gandhi, P Grefenstette, BW Hailey, CJ Harrison, FA Koss, M LaMassa, SM Luo, B Madsen, KK Puccetti, S Saez, C Stern, D Treister, E Urry, CM Wik, DR Zappacosta, L Zhang, W AF Mullaney, J. R. Del-Moro, A. Aird, J. Alexander, D. M. Civano, F. M. Hickox, R. C. Lansbury, G. B. Ajello, M. Assef, R. Ballantyne, D. R. Balokovic, M. Bauer, F. E. Brandt, W. N. Boggs, S. E. Brightman, M. Christensen, F. E. Comastri, A. Craig, W. W. Elvis, M. Forster, K. Gandhi, P. Grefenstette, B. W. Hailey, C. J. Harrison, F. A. Koss, M. LaMassa, S. M. Luo, B. Madsen, K. K. Puccetti, S. Saez, C. Stern, D. Treister, E. Urry, C. M. Wik, D. R. Zappacosta, L. Zhang, W. TI THE NuSTAR EXTRAGALACTIC SURVEYS: INITIAL RESULTS AND CATALOG FROM THE EXTENDED CHANDRA DEEP FIELD SOUTH SO ASTROPHYSICAL JOURNAL LA English DT Article DE astronomical databases: miscellaneous; galaxies: active; galaxies: evolution; X-rays: galaxies; X-rays: general ID ACTIVE GALACTIC NUCLEI; POINT-SOURCE CATALOG; HARD X-RAYS; MS SOURCE CATALOGS; SWIFT-BAT SURVEY; NUMBER COUNTS; BACKGROUND SPECTRUM; LUMINOSITY FUNCTION; SPACE DENSITY; BLACK-HOLES AB We present the initial results and the source catalog from the Nuclear Spectroscopic Telescope Array (NuSTAR) survey of the Extended Chandra Deep Field South (hereafter, ECDFS)-currently the deepest contiguous component of the NuSTAR extragalactic survey program. The survey covers the full approximate to 30' x 30' area of this field to a maximum depth of approximate to 360 ks (approximate to 220 ks when corrected for vignetting at 3-24 keV), reaching sensitivity limits of approximate to 1.3 x 10(-14) erg s(-1) cm(-2) (3-8 keV), approximate to 3.4 x 10(-14) erg s(-1) cm(-2) (8-24 keV), and approximate to 3.0 x 10(-14) erg s(-1) cm(-2) (3-24 keV). A total of 54 sources are detected over the full field, although five of these are found to lie below our significance threshold once contaminating flux from neighboring (i.e., blended) sources is taken into account. Of the remaining 49 that are significant, 19 are detected in the 8-24 keV band. The 8-24 to 3-8 keV band ratios of the 12 sources that are detected in both bands span the range 0.39-1.7, corresponding to a photon index range of Gamma approximate to 0.5-2.3, with a median photon index of (Gamma) over bar = 1.70 +/- 0.52. The redshifts of the 49 sources in our main sample span the range z = 0.21-2.7, and their rest-frame 10-40 keV luminosities (derived from the observed 8-24 keV fluxes) span the range L10-40 keV (0.7-300) 10 erg s(-1), sampling below the "knee" of the X-ray luminosity function out to z similar to 0.8-1. Finally, we identify one NuSTAR source that has neither a Chandra nor an XMM-Newton counterpart, but that shows evidence of nuclear activity at infrared wavelengths and thus may represent a genuine, new X-ray source detected by NuSTAR in the ECDFS. C1 [Mullaney, J. R.; Del-Moro, A.; Aird, J.; Alexander, D. M.; Lansbury, G. B.; Gandhi, P.] Univ Durham, Dept Phys, Ctr Extragalact Astron, South Rd, Durham DH1 3LE, England. [Mullaney, J. R.] Univ Sheffield, Dept Phys & Astron, Sheffield S3 7RH, S Yorkshire, England. [Aird, J.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Civano, F. M.; LaMassa, S. M.; Urry, C. M.] Yale Ctr Astron & Astrophys, New Haven, CT 06520 USA. [Civano, F. M.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. [Civano, F. M.; Hickox, R. C.] Dartmouth Coll, Dept Phys & Astron, Wilder Lab 6127, Hanover, NH 03755 USA. [Ajello, M.; Boggs, S. E.; Craig, W. W.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Assef, R.] Univ Diego Portales, Nucleo Astron, Fac Ingn, Santiago, Chile. [Ballantyne, D. R.] Georgia Inst Technol, Sch Phys, Ctr Relativist Astrophys, Atlanta, GA 30332 USA. [Balokovic, M.; Brightman, M.; Forster, K.; Grefenstette, B. W.; Harrison, F. A.; Madsen, K. K.] CALTECH, Cahill Ctr Astrophys, Pasadena, CA 91125 USA. [Bauer, F. E.] Pontificia Univ Catolica Chile, Fac Fis, Inst Astrofis, Santiago 22, Chile. [Bauer, F. E.] Millennium Inst Astrophys, Santiago, Chile. [Bauer, F. E.] Space Sci Inst, Boulder, CO 80301 USA. [Brandt, W. N.; Luo, B.] Penn State Univ, Dept Astron & Astrophys, Davey Lab 525, University Pk, PA 16802 USA. [Brandt, W. N.; Luo, B.] Penn State Univ, Inst Gravitat & Cosmos, University Pk, PA 16802 USA. [Brandt, W. N.] Penn State Univ, Dept Phys, University Pk, PA 16802 USA. [Christensen, F. E.] Tech Univ Denmark, Natl Space Inst, DTU Space, DK-2800 Lyngby, Denmark. [Comastri, A.] INAF Osservatorio Astron Bologna, I-40127 Bologna, Italy. [Elvis, M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Gandhi, P.] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England. [Hailey, C. J.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA. [Koss, M.] Swiss Fed Inst Technol, Dept Phys, Inst Astron, CH-8093 Zurich, Switzerland. [Puccetti, S.] ASDC ASI, I-00133 Rome, Italy. [Puccetti, S.; Zappacosta, L.] INAF, Osservatorio Astron Roma, I-00040 Monte Porzio Catone, Rome, Italy. [Saez, C.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Stern, D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Treister, E.] Univ Concepcion, Dept Astron, Concepcion, Chile. [Wik, D. R.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Wik, D. R.] Johns Hopkins Univ, Baltimore, MD 21218 USA. [Zhang, W.] West Virginia Wesleyan Coll, Phys & Engn Dept, Buckhannon, WV 26201 USA. RP Mullaney, JR (reprint author), Univ Durham, Dept Phys, Ctr Extragalact Astron, South Rd, Durham DH1 3LE, England. RI Boggs, Steven/E-4170-2015; OI Boggs, Steven/0000-0001-9567-4224; Puccetti, Simonetta/0000-0002-2734-7835; Koss, Michael/0000-0002-7998-9581; Comastri, Andrea/0000-0003-3451-9970; Ballantyne, David/0000-0001-8128-6976; Urry, Meg/0000-0002-0745-9792; Lansbury, George/0000-0002-5328-9827 FU National Aeronautics and Space Administration; Science and Technology Facilities Council [ST/I001573/1]; Institute of Advanced Study, Durham University; ERC; NASA [11-ADAP11-0218, GO3-14150C]; NSF [AST 1008067]; NuSTAR [44A-1092750]; NASA ADP [NNX10AC99G]; V. M. Willaman Endowment; CONICYT-Chile [Basal-CATA PFB-06/2007]; FONDECYT [1141218, 1120061]; "EMBIGGEN" Anillo [ACT1101]; Ministry of Economy, Development, and Tourism's Millennium Science Initiative [IC120009]; Center of Excellence in Astrophysics and Associated Technologies [PFB 06]; ASI/INAF [I/037/12/0 011/13]; NASA Headquarters under the NASA Earth and Space Science Fellowship Program [NNX14AQ07H] FX We thank the anonymous referee for their careful reading of the manuscript and comments that improved the clarity of the text. This work made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. We thank the NuSTAR Operations, Software, and Calibration teams for support with the execution and analysis of these observations. This research has made use of the NuSTAR Data Analysis Software (NUSTARDAS), jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA). A.D.M. and D.M.A. gratefully acknowledge financial support from the Science and Technology Facilities Council (ST/I001573/1). J.A. acknowledges support from a COFUND Junior Research Fellowship from the Institute of Advanced Study, Durham University, and ERC Advanced Grant FEEDBACK at the University of Cambridge. F.M.C. acknowledges support from NASA grants 11-ADAP11-0218 and GO3-14150C. D.R.B. is supported in part by NSF award AST 1008067. W.N.B. and B.L. thank NuSTAR grant 44A-1092750, NASA ADP grant NNX10AC99G, and the V. M. Willaman Endowment. We acknowledge support from CONICYT-Chile grants Basal-CATA PFB-06/2007 (FEB), FONDECYT 1141218 (FEB) and 1120061 (ET), and "EMBIGGEN" Anillo ACT1101 (FEB, ET); and the Ministry of Economy, Development, and Tourism's Millennium Science Initiative through grant IC120009, awarded to The Millennium Institute of Astrophysics, MAS (FEB). Support for the work of E.T. was also provided by the Center of Excellence in Astrophysics and Associated Technologies (PFB 06). A.C., S.P., and L.Z. acknowledge support from the ASI/INAF grant I/037/12/0 011/13. A.C. acknowledges the Caltech Kingsley visitor program. M.B. acknowledges support from NASA Headquarters under the NASA Earth and Space Science Fellowship Program, grant NNX14AQ07H. NR 79 TC 7 Z9 7 U1 1 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD AUG 1 PY 2015 VL 808 IS 2 AR 184 DI 10.1088/0004-637X/808/2/184 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DF0BA UT WOS:000371002400080 ER PT J AU Simon, JB Hughes, AM Flaherty, KM Bai, XN Armitage, PJ AF Simon, Jacob B. Hughes, A. Meredith Flaherty, Kevin M. Bai, Xue-Ning Armitage, Philip J. TI SIGNATURES OF MRI-DRIVEN TURBULENCE IN PROTOPLANETARY DISKS: PREDICTIONS FOR ALMA OBSERVATIONS SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; line: profiles; magnetohydrodynamics (MHD); protoplanetary disks; turbulence ID ANGULAR-MOMENTUM TRANSPORT; 3-DIMENSIONAL MAGNETOHYDRODYNAMIC SIMULATIONS; VERTICAL MAGNETIC-FIELD; UNSPLIT GODUNOV METHOD; T TAURI DISKS; ACCRETION DISKS; MAGNETOROTATIONAL-INSTABILITY; CONSTRAINED TRANSPORT; OUTER REGIONS; HD 163296 AB Spatially resolved observations of molecular line emission have the potential to yield unique constraints on the nature of turbulence within protoplanetary disks. Using a combination of local non-ideal magnetohydrodynamics (MHD) simulations and radiative transfer calculations, tailored to properties of the disk around HD 163296, we assess the ability of ALMA to detect turbulence driven by the magnetorotational instability (MRI). Our local simulations show that the MRI produces small-scale turbulent velocity fluctuations that increase in strength with height above the mid-plane. For a set of simulations at different disk radii, we fit a Maxwell-Boltzmann distribution to the turbulent velocity and construct a turbulent broadening parameter as a function of radius and height. We input this broadening into radiative transfer calculations to quantify observational signatures of MRI-driven disk turbulence. We find that the ratio of the peak line flux to the flux at line center is a robust diagnostic of turbulence that is only mildly degenerate with systematic uncertainties in disk temperature. For the CO(3-2) line, which we expect to probe the most magnetically active slice of the disk column, variations in the predicted peak-to-trough ratio between our most and least turbulent models span a range of approximately 15%. Additional independent constraints can be derived from the morphology of spatially resolved line profiles, and we estimate the resolution required to detect turbulence on different spatial scales. We discuss the role of lower optical depth molecular tracers, which trace regions closer to the disk mid-plane where velocities in MRI-driven models are systematically lower. C1 [Simon, Jacob B.] Southwest Res Inst, Dept Space Studies, Boulder, CO 80302 USA. [Simon, Jacob B.; Armitage, Philip J.] Univ Colorado, JILA, Boulder, CO 80309 USA. [Simon, Jacob B.; Armitage, Philip J.] NIST, Boulder, CO 80309 USA. [Hughes, A. Meredith; Flaherty, Kevin M.] Wesleyan Univ, Van Vleck Observ, Dept Astron, Middletown, CT 06459 USA. [Bai, Xue-Ning] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Armitage, Philip J.] Univ Colorado, Dept Astrophys & Planetary Sci, Boulder, CO 80309 USA. RP Simon, JB (reprint author), Southwest Res Inst, Dept Space Studies, Boulder, CO 80302 USA. EM jbsimon.astro@gmail.com FU NASA [NNX13AI58G, NNX13AI32G, NAS 5-26555, NAS5-26555]; NSF [AST 1313021]; Space Telescope Science Institute [HST-AR-12814]; California Institute of Technology (Caltech); Jet Propulsion Laboratory (JPL) - NASA; NASA from the Space Telescope Science Institute [HST-HF-51301.01-A]; XSEDE [TG-AST120062, TG-AST140001] FX We thank Daniel R. Wik, Matt Kunz, Steve Balbus, Jeremy Goodman, and Richard Nelson for useful discussions and suggestions regarding this work. We also thank the referee, whose suggestions greatly enhanced the quality of this work. We acknowledge support from NASA through grants NNX13AI58G (P.J.A.) and NNX13AI32G (A.M.H., K.M.F.), from the NSF through grant AST 1313021 (P.J.A.), and from grant HST-AR-12814 (P.J.A.) awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., for NASA, under contact NAS 5-26555. J.B.S.'s support was provided in part under contract with the California Institute of Technology (Caltech) and the Jet Propulsion Laboratory (JPL) funded by NASA through the Sagan Fellowship Program executed by the NASA Exoplanet Science Institute. 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. This research was supported by an allocation of advanced computing resources provided by the National Science Foundation. The computations were performed on Kraken at the National Institute for Computational Sciences and Maverick at the Texas Advanced Computing Center through XSEDE grant TG-AST120062 and on Stampede at the Texas Advanced Computing Center through XSEDE grant TG-AST140001. NR 86 TC 8 Z9 8 U1 1 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD AUG 1 PY 2015 VL 808 IS 2 AR 180 DI 10.1088/0004-637X/808/2/180 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DF0BA UT WOS:000371002400076 ER PT J AU Strader, J Dupree, AK Smith, GH AF Strader, Jay Dupree, A. K. Smith, Graeme H. TI THE 10830 angstrom HELIUM LINE AMONG EVOLVED STARS IN THE GLOBULAR CLUSTER M4 SO ASTROPHYSICAL JOURNAL LA English DT Article DE globular clusters: individual (M4); stars: chromospheres ID RED GIANT STARS; MULTIPLE STELLAR POPULATIONS; OMEGA-CENTAURI; MAIN-SEQUENCE; CHROMOSPHERIC ACTIVITY; ABUNDANCE VARIATIONS; MASS OUTFLOW; ATMOSPHERES; PHOTOMETRY; METALLICITIES AB Helium is a pivotal element in understanding the multiple main sequences and extended horizontal branches observed in some globular clusters. Here we present a spectroscopic study of helium in the nearby globular cluster Messier 4 (M4). We have obtained spectra of the chromospheric He I 10830 angstrom line in 16 red horizontal branch (RHB), red giant branch, and asymptotic giant branch stars. Clear He I absorption or emission is present in most of the stars. Effective temperature is the principal parameter that correlates with 10830 angstrom line strength. Stars with T-eff < 4450 K do not exhibit the helium line. RHB stars, which are the hottest stars in our sample, all have strong He I line absorption. A number of these stars show very broad 10830 angstrom lines with shortward extensions indicating outflows as high as 80-100 km s(-1) and the possibility of mass loss. We have also derived [Na/Fe] and [Al/Fe] abundances to see whether these standard tracers of "second generation" cluster stars are correlated with He I line strength. Unlike the case for our previous study of omega Cen, no clear correlation is observed. This may be because the sample does not cover the full range of abundance variations found in M4, or simply because the physical conditions in the chromosphere, rather than the helium abundance, primarily determine the He I 10830 angstrom line strength. A larger sample of high-quality He I spectra of both "first" and "second" generation red giants within a narrow range of T-eff and luminosity is needed to test for the subtle spectroscopic variations in He I expected in M4. C1 [Strader, Jay] Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA. [Dupree, A. K.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Smith, Graeme H.] Univ Calif Santa Cruz, UCO Lick Observ, Santa Cruz, CA 95064 USA. RP Strader, J (reprint author), Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA. EM strader@pa.msu.edu; adupree@cfa.harvard.edu; graeme@ucolick.org FU National Aeronautics and Space Administration; National Science Foundation FX We thank an anonymous referee for comments that improved the paper. We thank Ben Hendricks for generously providing us with photometry and his differential reddening map of the field of M4. We also thank Christian Johnson for facilitating the Python reduction of a MIKE spectrum. This publication makes use of data products from 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. This paper is partially nased 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 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). NR 45 TC 0 Z9 0 U1 1 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD AUG 1 PY 2015 VL 808 IS 2 AR 124 DI 10.1088/0004-637X/808/2/124 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DF0BA UT WOS:000371002400019 ER PT J AU Tamura, Y Kawabe, R Shimajiri, Y Tsukagoshi, T Nakajima, Y Oasa, Y Wilner, DJ Chandler, CJ Saigo, K Tomida, K Yun, MS Taniguchi, A Kohno, K Hatsukade, B Aretxaga, I Austermann, JE Dickman, R Ezawa, H Goss, WM Hayashi, M Hughes, DH Hiramatsu, M Inutsuka, S Ogasawara, R Ohashi, N Oshima, T Scott, KS Wilson, GW AF Tamura, Y. Kawabe, R. Shimajiri, Y. Tsukagoshi, T. Nakajima, Y. Oasa, Y. Wilner, D. J. Chandler, C. J. Saigo, K. Tomida, K. Yun, M. S. Taniguchi, A. Kohno, K. Hatsukade, B. Aretxaga, I. Austermann, J. E. Dickman, R. Ezawa, H. Goss, W. M. Hayashi, M. Hughes, D. H. Hiramatsu, M. Inutsuka, S. Ogasawara, R. Ohashi, N. Oshima, T. Scott, K. S. Wilson, G. W. TI EXTREMELY BRIGHT SUBMILLIMETER GALAXIES BEYOND THE LUPUS-I STAR-FORMING REGION SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: evolution; galaxies: formation; galaxies: high-redshift; galaxies: starburst; ISM: individual objects (Lupus-I Molecular Cloud); submillimeter: galaxies ID 1ST HYDROSTATIC CORE; DEEP FIELD SOUTH; RADIATION HYDRODYNAMIC MODEL; STRONGLY LENSED GALAXIES; CLERK MAXWELL TELESCOPE; ALL-SKY SURVEY; GOODS-S FIELD; NUMBER COUNTS; INTERSTELLAR-MEDIUM; SOURCE CATALOG AB We report detections of two candidate distant submillimeter galaxies (SMGs), MM J154506.4-344318 and MM J154132.7-350320, which are discovered in the AzTEC/ASTE 1.1 mm survey toward the Lupus-I star-forming region. The two objects have 1.1 mm flux densities of 43.9 and 27.1 mJy, and have Herschel/SPIRE counterparts as well. The Submillimeter Array counterpart to the former SMG is identified at 890 mu m and 1.3 mm. Photometric redshift estimates using all available data from the mid-infrared to the radio suggest that the redshifts of the two SMGs are z(photo) similar or equal to 4-5 and 3, respectively. Near-infrared objects are found very close to the SMGs and they are consistent with low-z ellipticals, suggesting that the high apparent luminosities can be attributed to gravitational magnification. The cumulative number counts at S-1.1mm >= 25 mJy, combined with the other two 1.1 mm brightest sources, are 0.70(-0.34)(+0.56) deg(-2), which is consistent with a model prediction that accounts for flux magnification due to strong gravitational lensing. Unexpectedly, a z > 3 SMG and a Galactic dense starless core (e.g., a first hydrostatic core) could be similar in the mid-infrared to millimeter spectral energy distributions and spatial structures at least at greater than or similar to 1 ''. This indicates that it is necessary to distinguish the two possibilities by means of broadband photometry from the optical to centimeter and spectroscopy to determine the redshift, when a compact object is identified toward Galactic star-forming regions. C1 [Tamura, Y.; Kohno, K.] Univ Tokyo, Inst Astron, Mitaka, Tokyo 1810015, Japan. [Kawabe, R.; Hayashi, M.] Natl Astron Observ Japan, Mitaka, Tokyo 1818588, Japan. [Kawabe, R.] Grad Univ Adv Studies SOKENDAI, Sch Sci, Dept Astron, Mitaka, Tokyo 1818588, Japan. [Kawabe, R.] Joint ALMA Observ, Santiago 7630355, Chile. [Shimajiri, Y.] Univ Paris Diderot, Lab AIM, CEA DSM CNRS, IRFU Serv Astrophys,CEA Saclay, F-91191 Gif Sur Yvette, France. [Shimajiri, Y.; Oshima, T.] Natl Astron Observ Japan, Nobeyama Radio Observ, Minamisa Ku, Nagano 3841305, Japan. [Tsukagoshi, T.] Ibaraki Univ, Inst Astrophys & Planetary Sci, Mito, Ibaraki 3108512, Japan. [Nakajima, Y.] Hitotsubashi Univ, Tokyo 1868601, Japan. [Oasa, Y.] Saitama Univ, Fac Educ, Saitama 3888570, Japan. [Wilner, D. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Chandler, C. J.; Dickman, R.; Goss, W. M.] Natl Radio Astron Observ, Socorro, NM 87801 USA. [Saigo, K.; Hatsukade, B.; Ezawa, H.; Hiramatsu, M.; Ogasawara, R.] Natl Astron Observ Japan, Chile Observ, Mitaka, Tokyo 1818588, Japan. [Tomida, K.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. [Tomida, K.] Univ Tokyo, Dept Phys, Bunkyo Ku, Tokyo 1130033, Japan. [Yun, M. S.; Wilson, G. W.] Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA. [Kohno, K.] Univ Tokyo, Res Ctr Early Universe, Bunkyo Ku, Tokyo 1130033, Japan. [Aretxaga, I.] Inst Nacl Astrofis Opt & Electr, Puebla 72000, Mexico. [Austermann, J. E.] Univ Colorado, Ctr Astrophys & Space Astron, Boulder, CO 80309 USA. [Hayashi, M.] Grad Univ Adv Studies SOKENDAI, Sch Math & Phys Sci, Kanagawa 2400193, Japan. [Inutsuka, S.] Nagoya Univ, Dept Phys, Nagoya, Aichi 4648602, Japan. [Ohashi, N.] Natl Astron Observ Japan, Subaru Telescope, Hilo, HI 96720 USA. [Scott, K. S.] Natl Radio Astron Observ, North Amer ALMA Sci Ctr, Charlottesville, VA 22903 USA. RP Tamura, Y (reprint author), Univ Tokyo, Inst Astron, Mitaka, Tokyo 1810015, Japan. EM ytamura@ioa.s.u-tokyo.ac.jp OI Tomida, Kengo/0000-0001-8105-8113 FU KAKENHI [25103503]; JSPS [09J05537, 09J00159]; Commonwealth of Australia; Smithsonian Institution; Academia Sinica; NASA; National Aeronautics and Space Administration; National Science Foundation FX We acknowledge the anonymous referee for many useful suggetions. We are grateful to the ASTE team for making the observations possible. We thank M. Bethermin and I. Shimizu for making the model number counts available. The study is partially supported by KAKENHI (No. 25103503). Y.S. and K.T. are supported by the JSPS Research Fellowship for Young Scientists (Nos. 09J05537 and 09J00159, respectively). This work is based on observations and archival data made with the following telescopes and facilities. The ASTE telescope is operated by National Astronomical Observatory of Japan. The Australia Telescope Compact Array is part of the Australia Telescope National Facility, which is funded by the Commonwealth of Australia for operation as a National Facility managed by CSIRO. Herschel is an ESA space observatory with science instruments provided by European-led Principal Investigator consortia and with important participation from NASA. NRAO is a facility of the NSF operated under cooperative agreement by Associated Universities, Inc. The 45 m radio telescope and the Nobeyama Millimeter Array are operated by Nobeyama Radio Observatory, a branch of National Astronomical Observatory of Japan. The Submillimeter Array is a joint project between the Smithsonian Astrophysical Observatory and the Academia Sinica Institute of Astronomy and Astrophysics and is funded by the Smithsonian Institution and the Academia Sinica. The Spitzer Space Telescope is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. The Subaru Telescope is operated by National Astronomical Observatory of Japan. The United Kingdom Infrared Telescope is operated by the Joint Astronomy Centre on behalf of the Science and Technology Facilities Council of the U.K. This publication makes use of data products from the 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. NR 118 TC 0 Z9 0 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD AUG 1 PY 2015 VL 808 IS 2 AR 121 DI 10.1088/0004-637X/808/2/121 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DF0BA UT WOS:000371002400016 ER PT J AU Tripathi, A Kratter, KM Murray-Clay, RA Krumholz, MR AF Tripathi, Anjali Kratter, Kaitlin M. Murray-Clay, Ruth A. Krumholz, Mark R. TI SIMULATED PHOTOEVAPORATIVE MASS LOSS FROM HOT JUPITERS IN 3D (vol 808, 173, 2015) SO ASTROPHYSICAL JOURNAL LA English DT Correction C1 [Tripathi, Anjali; Murray-Clay, Ruth A.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Kratter, Kaitlin M.] Univ Arizona, Dept Astron, Tucson, AZ 85721 USA. [Kratter, Kaitlin M.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Murray-Clay, Ruth A.] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA. [Krumholz, Mark R.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. RP Tripathi, A (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM atripathi@cfa.harvard.edu NR 1 TC 0 Z9 0 U1 1 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD AUG 1 PY 2015 VL 808 IS 2 AR 159 DI 10.1088/0004-637X/811/2/159 PG 1 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DF0BA UT WOS:000371002400069 ER PT J AU Tripathi, A Kratter, KM Murray-Clay, RA Krumholz, MR AF Tripathi, Anjali Kratter, Kaitlin M. Murray-Clay, Ruth A. Krumholz, Mark R. TI SIMULATED PHOTOEVAPORATIVE MASS LOSS FROM HOT JUPITERS IN 3D SO ASTROPHYSICAL JOURNAL LA English DT Article DE hydrodynamics; planet-star interactions; planets and satellites: atmospheres; planets and satellites: gaseous planets ID EXTRASOLAR PLANET HD209458B; HD 189733B; X-RAY; TRANSIT OBSERVATIONS; ESCAPING ATMOSPHERE; GIANT PLANETS; HII-REGIONS; LYMAN-ALPHA; BOW SHOCKS; HYDROGEN AB Ionizing stellar photons heat the upper regions of planetary atmospheres, driving atmospheric mass loss. Gas escaping from several hot, hydrogen-rich planets has been detected using UV and X-ray transmission spectroscopy. Because these planets are tidally locked, and thus asymmetrically irradiated, escaping gas is unlikely to be spherically symmetric. In this paper, we focus on the effects of asymmetric heating on local outflow structure. We use the Athena code for hydrodynamics to produce 3D simulations of hot Jupiter mass loss that jointly model wind launching and stellar heating via photoionization. Our fiducial planet is an inflated, hot Jupiter with radius R-p = 2.14R(Jup) and mass M-p = 0.53M(Jup). We irradiate the initially neutral, atomic hydrogen atmosphere with 13.6 eV photons and compute the outflow's ionization structure. There are clear asymmetries in the atmospheric outflow, including a neutral shadow on the planet's nightside. Given an incident ionizing UV flux comparable to that of the Sun, we find a steady-state mass loss rate of similar to 2 x 10(10) g s(-1). The total mass loss rate and the outflow substructure along the substellar ray show good agreement with earlier 1D models, for two different fluxes. Our 3D data cube can be used to generate the outflow's extinction spectrum during transit. As a proof of concept, we find absorption of stellar Lya at Doppler-shifted velocities of up to +/- 50 km s(-1). Our work provides a starting point for further 3D models that can be used to predict observable signatures of hot Jupiter mass loss. C1 [Tripathi, Anjali; Murray-Clay, Ruth A.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Kratter, Kaitlin M.] Univ Arizona, Dept Astron, Tucson, AZ 85721 USA. [Kratter, Kaitlin M.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Murray-Clay, Ruth A.] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA. [Krumholz, Mark R.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. RP Tripathi, A (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM atripathi@cfa.harvard.edu OI Krumholz, Mark/0000-0003-3893-854X FU National Science Foundation [DGE-1144152]; NASA - Space Telescope Science Institute [HF-51306.01]; NASA [NAS 5-26555]; NSF [AST-1411536, AST-0955300] FX We thank Xuening Bai, Jim Stone, and James Owen for helpful discussions. We are grateful to the referee for helpful comments that improved the paper. A.T. was supported by the National Science Foundation Graduate Research Fellowship under grant No. DGE-1144152. K.M.K. was supported in part by NASA through Hubble Fellowship grant no. HF-51306.01 awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., for NASA, under contract NAS 5-26555. R.A.M. acknowledges support from NSF grant AST-1411536. M.R.K. acknowledges support from NSF grant AST-0955300. The computations in this paper were run on the Smithsonian Institution High Performance Cluster (SI/HPC) and the Odyssey cluster supported by the FAS Science Division Research Computing Group at Harvard University. NR 61 TC 9 Z9 9 U1 2 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 AUG 1 PY 2015 VL 808 IS 2 AR 173 DI 10.1088/0004-637X/808/2/173 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DF0BA UT WOS:000371002400068 ER PT J AU Williams, PKG Berger, E AF Williams, P. K. G. Berger, E. TI THE ROTATION PERIOD AND MAGNETIC FIELD OF THE T DWARF 2MASSI J1047539+212423 MEASURED FROM PERIODIC RADIO BURSTS SO ASTROPHYSICAL JOURNAL LA English DT Article DE brown dwarfs; radio continuum: stars; stars: individual (2MASSI J1047539+212423) ID SIMULTANEOUS MULTIWAVELENGTH OBSERVATIONS; ANGULAR-MOMENTUM EVOLUTION; ELECTRON-CYCLOTRON MASER; MAIN-SEQUENCE STARS; ALL-SKY SURVEY; BROWN DWARFS; X-RAY; ULTRACOOL DWARFS; BRIGHTNESS VARIATIONS; EMISSION AB Periodic radio bursts from very low mass stars and brown dwarfs simultaneously probe their magnetic and rotational properties. The brown dwarf 2MASSI J1047539+212423 (2M 1047+21) is currently the only T dwarf (T6.5) detected at radio wavelengths. Previous observations of this source with the Arecibo observatory revealed intermittent, 100%-polarized radio pulses similar to those detected from other brown dwarfs, but were unable to constrain a pulse periodicity; previous Very Large Array (VLA) observations detected quiescent emission a factor of similar to 100 times fainter than the Arecibo pulses but no additional events. Here we present 14 hr of VLA observations of this object that reveal a series of pulses at similar to 6 GHz with highly variable profiles, showing that the pulsing behavior evolves on time scales that are both long and short compared to the rotation period. We measure a periodicity of similar to 1.77 hr and identify it with the rotation period. This is just the sixth rotation period measurement in a late T dwarf, and the first obtained in the radio. We detect a pulse at 10 GHz as well, suggesting that the magnetic field strength of 2M 1047+21 reaches at least 3.6 kG. Although this object is the coolest and most rapidly rotating radio-detected brown dwarf to date, its properties appear continuous with those of other such objects, suggesting that the generation of strong magnetic fields and radio emission may continue to even cooler objects. Further studies of this kind will help to clarify the relationships between mass, age, rotation, and magnetic activity at and beyond the end of the main sequence, where both theories and observational data are currently scarce. C1 [Williams, P. K. G.; Berger, E.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RP Williams, PKG (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM pwilliams@cfa.harvard.edu OI Williams, Peter/0000-0003-3734-3587 FU National Science Foundation [AST-1008361] FX We thank the referee, Alex Wolszczan, for an insightful report that improved the paper. We acknowledge support for this work from the National Science Foundation through Grant AST-1008361. The VLA is operated by the National Radio Astronomy Observatory, a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. This research has made use of the SIMBAD database, operated at CDS, Strasbourg, France; NASA's Astrophysics Data System; and Astropy, a community-developed core Python package for astronomy (Astropy Collaboration et al. 2013). NR 60 TC 10 Z9 10 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD AUG 1 PY 2015 VL 808 IS 2 AR 189 DI 10.1088/0004-637X/808/2/189 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DF0BA UT WOS:000371002400085 ER PT J AU Chase, JM Powell, KI Knight, TM AF Chase, Jonathan M. Powell, Kristin I. Knight, Tiffany M. TI 'Bigger data' on scale-dependent effects of invasive species on biodiversity cannot overcome confounded analyses: a comment on Stohlgren & Rejmanek (2014) SO BIOLOGY LETTERS LA English DT Letter ID AREA RELATIONSHIPS; DIVERSITY; PLANTS AB A recent study by Stohlgren & Rejmanek (SR: Stohlgren TJ, Rejmanek M. 2014 Biol. Lett. 10. (doi:10.1098/rsb1.2013.0939)) purported to test the generality of a recent finding of scale-dependent effects of invasive plants on native diversity; dominant invasive plants decreased the intercept and increased the slope of the species area relationship. SR (2014) find little correlation between invasive species cover and the slopes and intercepts of SARs across a diversity of sites. We show that the analyses of SR (2014) are inappropriate because of confounding causality. C1 [Chase, Jonathan M.; Knight, Tiffany M.] German Ctr Integrat Biodivers Res iDiv, D-04103 Leipzig, Germany. [Powell, Kristin I.] Smithsonian Trop Res Inst, Forest Global Earth Observ, Ctr Trop Forest Sci, Washington, DC 20560 USA. [Knight, Tiffany M.] Washington Univ, Dept Biol, St Louis, MO 63130 USA. RP Chase, JM (reprint author), German Ctr Integrat Biodivers Res iDiv, D-04103 Leipzig, Germany. EM jonathan.chase@idiv.de NR 10 TC 1 Z9 1 U1 4 U2 15 PU ROYAL SOC PI LONDON PA 6-9 CARLTON HOUSE TERRACE, LONDON SW1Y 5AG, ENGLAND SN 1744-9561 EI 1744-957X J9 BIOL LETTERS JI Biol. Lett. PD AUG 1 PY 2015 VL 11 IS 8 AR 20150103 DI 10.1098/rsbl.2015.0103 PG 3 WC Biology; Ecology; Evolutionary Biology SC Life Sciences & Biomedicine - Other Topics; Environmental Sciences & Ecology; Evolutionary Biology GA CT4SR UT WOS:000362798100005 ER PT J AU Marra, PP Cohen, EB Loss, SR Rutter, JE Tonra, CM AF Marra, Peter P. Cohen, Emily B. Loss, Scott R. Rutter, Jordan E. Tonra, Christopher M. TI A call for full annual cycle research in animal ecology SO BIOLOGY LETTERS LA English DT Article DE annual cycle; seasonal interaction; research bias ID CARRY-OVER; MIGRATORY BIRDS; CLIMATE-CHANGE; MORTALITY; TRACKING AB For vertebrates, annual cycles are organized into a series of breeding and non-breeding periods that vary in duration and location but are inextricably linked biologically. Here, we show that our understanding of the fundamental ecology of four vertebrate classes has been limited by a severe breeding season research bias and that studies of individual and population-level responses to natural and anthropogenic change would benefit from a full annual cycle perspective. Recent emergence of new analytical and technological tools for studying individual and population-level animal movement could help reverse this bias. To improve understanding of species biology and reverse the population declines of many vertebrate species, a concerted effort to move beyond single season research is vital. C1 [Marra, Peter P.; Cohen, Emily B.; Loss, Scott R.; Rutter, Jordan E.; Tonra, Christopher M.] Natl Zool Pk, Smithsonian Conservat Biol Inst, Migratory Bird Ctr, Washington, DC 20013 USA. RP Marra, PP (reprint author), Natl Zool Pk, Smithsonian Conservat Biol Inst, Migratory Bird Ctr, POB 37012 MRC 5503, Washington, DC 20013 USA. EM marrap@si.edu RI Tonra, Christopher/B-1620-2013 FU NSF; US Fish and Wildlife Service's Migratory Bird Program; Upper Midwest/Great Lakes LCC; Smithsonian's Didden Fellowship FX Funding was provided by NSF, US Fish and Wildlife Service's Migratory Bird Program, Upper Midwest/Great Lakes LCC and Smithsonian's Didden Fellowship. NR 25 TC 26 Z9 27 U1 9 U2 27 PU ROYAL SOC PI LONDON PA 6-9 CARLTON HOUSE TERRACE, LONDON SW1Y 5AG, ENGLAND SN 1744-9561 EI 1744-957X J9 BIOL LETTERS JI Biol. Lett. PD AUG 1 PY 2015 VL 11 IS 8 AR 20150552 DI 10.1098/rsbl.2015.0552 PG 4 WC Biology; Ecology; Evolutionary Biology SC Life Sciences & Biomedicine - Other Topics; Environmental Sciences & Ecology; Evolutionary Biology GA CT4SR UT WOS:000362798100007 ER PT J AU Girard, JN Garsden, H Starck, JL Corbel, S Woiselle, A Tasse, C McKean, JP Bobin, J AF Girard, J. N. Garsden, H. Starck, J. L. Corbel, S. Woiselle, A. Tasse, C. McKean, J. P. Bobin, J. TI Sparse representations and convex optimization as tools for LOFAR radio interferometric imaging SO JOURNAL OF INSTRUMENTATION LA English DT Article; Proceedings Paper CT 2nd International Summer School on Intelligent Signal Processing for Frontier Research and Industry CY JUL 14-25, 2014 CL Univ Paris Diderot Campus, Paris, FRANCE HO Univ Paris Diderot Campus DE Image processing; Interferometry; Antennas ID WIDE-FIELD; SPLITTING METHODS; ALGORITHM; RECONSTRUCTION; CALIBRATION; ASTRONOMY; DECONVOLUTION; POLARIMETRY; PROJECTION; ARRAYS AB Compressed sensing theory is slowly making its way to solve more and more astronomical inverse problems. We address here the application of sparse representations, convex optimization and proximal theory to radio interferometric imaging. First, we expose the theory behind interferometric imaging, sparse representations and convex optimization, and second, we illustrate their application with numerical tests with SASIR, an implementation of the FISTA, a Forward-Backward splitting algorithm hosted in a LOFAR imager. Various tests have been conducted in Garsden et al., 2015. The main results are: i) an improved angular resolution (super resolution of a factor approximate to 2) with point sources as compared to CLEAN on the same data, ii) correct photometry measurements on a field of point sources at high dynamic range and iii) the imaging of extended sources with improved fidelity. SASIR provides better reconstructions (five time less residuals) of the extended emission as compared to CLEAN. With the advent of large radiotelescopes, there is scope for improving classical imaging methods with convex optimization methods combined with sparse representations. C1 [Girard, J. N.; Starck, J. L.; Corbel, S.; Bobin, J.] CEA, Serv Astrophys, F-91190 Gif Sur Yvette, France. [Garsden, H.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Woiselle, A.] Sagem Safran, F-75512 Paris 15, France. [Tasse, C.] Univ Paris Diderot, CNRS, Observ Paris, GEPI, F-92190 Meudon, France. [McKean, J. P.] Netherlands Inst Radio Astron ASTRON, NL-7990 AA Dwingeloo, Netherlands. RP Girard, JN (reprint author), CEA, Serv Astrophys, Bat 709, F-91190 Gif Sur Yvette, France. EM julien.girard@cea.fr OI Starck, Jean-Luc/0000-0003-2177-7794 NR 58 TC 1 Z9 1 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 1748-0221 J9 J INSTRUM JI J. Instrum. PD AUG PY 2015 VL 10 AR C08013 DI 10.1088/1748-0221/10/08/C08013 PG 19 WC Instruments & Instrumentation SC Instruments & Instrumentation GA CS8ZP UT WOS:000362378700013 ER PT J AU Newman, R Kaplan, E Derrick, M AF Newman, Richard Kaplan, Emily Derrick, Michele TI MOPA MOPA: SCIENTIFIC ANALYSIS AND HISTORY OF AN UNUSUAL SOUTH AMERICAN RESIN USED BY THE INKA AND ARTISANS IN PASTO, COLOMBIA SO JOURNAL OF THE AMERICAN INSTITUTE FOR CONSERVATION LA English DT Article DE Mopa mopa; Inka; Qero; Pasto; Elaeagia; Pyrolysis gas chromatography-mass spectrometry; Liquid chromatography-mass spectrometry ID MASS-SPECTROMETRY AB A native South American phenolic resin commonly called mopa mopa was used for many centuries in two cultural contexts, by artisans in the region of Pasto, Colombia (where it is still used), and by the Inka in Peru, where it was used to decorate ceremonial drinking cups known as qeros. It was softened to a rubbery state by heating in water, mixed with colorants, stretched into thin layers and applied as inlay to decorate wooden surfaces of various kinds of objects. The resin comes from trees of the genus Elaeagia, which grows in mountainous regions of western South America from Colombia to Ecuador. Botanical specimens from the two species that are the most likely sources of mopa mopa, Elaeagia pastoensis and Elaeagia utilis, were analyzed along with samples from colonial period objects made in Pasto and samples from Inka qeros. Species-specific identification of the resin is often possible, with E. pastoensis being utilized in Pasto and (probably) E. utilis by the Inka. This conclusion has important implications for the possible connection between the use of mopa mopa in the two widely separated areas. C1 [Newman, Richard; Derrick, Michele] Museum Fine Arts, Sci Res Lab, Boston, MA 02115 USA. [Kaplan, Emily] Smithsonian Natl Museum Amer Indian, Cultural Resources Ctr, New York, NY USA. RP Newman, R (reprint author), Museum Fine Arts, Sci Res Lab, 465 Huntington Ave, Boston, MA 02115 USA. EM rnewman@mfa.org; kaplane@si.edu; mderrick@mfa.org NR 53 TC 0 Z9 0 U1 0 U2 0 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 AUG PY 2015 VL 54 IS 3 BP 123 EP 148 DI 10.1179/1945233015Y.0000000005 PG 26 WC Humanities, Multidisciplinary SC Arts & Humanities - Other Topics GA CT0NR UT WOS:000362493500002 ER PT J AU Babb, JF Sadeghpour, H Kirby, K AF Babb, James F. Sadeghpour, Hossein Kirby, Kate TI Alexander Dalgarno obituary SO PHYSICS TODAY LA English DT Biographical-Item C1 [Babb, James F.; Sadeghpour, Hossein] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Kirby, Kate] Amer Phys Soc, College Pk, MD USA. RP Babb, JF (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 1 TC 0 Z9 0 U1 1 U2 1 PU AMER INST PHYSICS PI MELVILLE PA 1305 WALT WHITMAN RD, STE 300, MELVILLE, NY 11747-4501 USA SN 0031-9228 EI 1945-0699 J9 PHYS TODAY JI Phys. Today PD AUG PY 2015 VL 68 IS 8 BP 63 EP 63 PG 1 WC Physics, Multidisciplinary SC Physics GA CS7SZ UT WOS:000362287300019 ER PT J AU Cohen, O AF Cohen, O. TI Quantifying the Difference Between the Flux-Tube Expansion Factor at the Source Surface and at the Alfv,n Surface Using a Global MHD Model for the Solar Wind SO SOLAR PHYSICS LA English DT Article DE Magnetic fields; Models - Solar wind; Theory - Velocity fields; Solar wind ID NONSPHERICAL SOURCE-SURFACE; MAGNETIC-FIELD; CORONA; HELIOSPHERE; MAGNETOHYDRODYNAMICS; PREDICTION; WAVES AB The potential-field approximation has been providing a fast and computationally inexpensive estimation for the solar corona's global magnetic-field geometry for several decades. In contrast, more physics-based global magnetohydrodynamic (MHD) models have been used for a similar purpose, while being much more computationally expensive. Here, we investigate the difference in the field geometry between a global MHD model and the potential-field source-surface model (PFSSM) by tracing individual magnetic field lines in the MHD model from the Alfv,n surface (AS), through the source surface (SS), all the way to the field-line footpoint, and then back to the source surface in the PFSSM. We also compare the flux-tube expansion at two points at the SS and the AS along the same radial line. We study the effect of solar cycle variations, the order of the potential-field harmonic expansion, and different magnetogram sources. We find that the flux-tube expansion factor is consistently smaller at the AS than at the SS for solar minimum and the fast solar wind, but it is consistently larger for solar maximum and the slow solar wind. We use the Wang-Sheeley-Arge model to calculate the associated wind speed for each field line and propagate these solar-wind speeds to 1 AU. We find a deviation of more than five hours in the arrival time between the two models for 20 % of the field lines in the solar minimum case and for 40 % of the field lines in the solar maximum case. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Cohen, O (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM ocohen@cfa.harvard.edu OI Cohen, Ofer/0000-0003-3721-0215 FU NASA ESS; NASA ESTO-CT; NSF KDI; DoD MURI FX Simulation results were obtained using the Space Weather Modeling Framework, developed by the Center for Space Environment Modeling, at the University of Michigan with funding support from NASA ESS, NASA ESTO-CT, NSF KDI, and DoD MURI. NR 33 TC 5 Z9 5 U1 1 U2 2 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0038-0938 EI 1573-093X J9 SOL PHYS JI Sol. Phys. PD AUG PY 2015 VL 290 IS 8 BP 2245 EP 2263 DI 10.1007/s11207-015-0739-3 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CS3WY UT WOS:000362007300006 ER PT J AU Jurcsik, J Smitola, P Hajdu, G Sodor, A Nuspl, J Kolenberg, K Furesz, G Moor, A Kun, E Pal, A Bakos, J Kelemen, J Kovacs, T Kriskovics, L Sarneczky, K Szalai, T Szing, A Vida, K AF Jurcsik, J. Smitola, P. Hajdu, G. Sodor, A. Nuspl, J. Kolenberg, K. Furesz, G. Moor, A. Kun, E. Pal, A. Bakos, J. Kelemen, J. Kovacs, T. Kriskovics, L. Sarneczky, K. Szalai, T. Szing, A. Vida, K. TI OVERTONE AND MULTI-MODE RR LYRAE STARS IN THE GLOBULAR CLUSTER M3 SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE globular clusters: individual (M3); stars: horizontal-branch; stars: oscillations; stars: variables: RR Lyrae ID GRAVITATIONAL LENSING EXPERIMENT.; OGLE-III CATALOG; HORIZONTAL-BRANCH STARS; LARGE-MAGELLANIC-CLOUD; VARIABLE-STARS; GALACTIC BULGE; CLASSICAL CEPHEIDS; CCD PHOTOMETRY; LIGHT CURVES; MODULATION AB The overtone and multi-mode RR Lyrae stars in the globular cluster M3 are studied using a 200 day long, B, V, and I-C time-series photometry obtained in 2012. 70% of the 52 overtone variables observed show some kind of multi-periodicity (with additional frequency at f(0.61) = f(1O)/0.61 frequency ratio, Blazhko effect, double/multi-mode pulsation, and period doubling). A signal at the 0.587 frequency ratio to the fundamental-mode frequency is detected in the double-mode star, V13, which may be identified as the second radial overtone mode. If this mode identification is correct, than V13 is the first RR Lyrae star showing triple-mode pulsation of the first three radial modes. Either the Blazhko effect or the f(0.61) frequency (or both of these phenomena) appears in seven double-mode stars. The P-1O/P-F period ratio of RRd stars showing the Blazhko effect are anomalous. A displacement of the main frequency component at the fundamental mode with the value of modulation frequency (or its half), is detected in three Blazhko RRd stars that are parallel with the appearance of the overtone-mode pulsation. The f(0.61) frequency appears in RRc stars that lie at the blue side of the double-mode region and in RRd stars, raising the suspicion that its occurrence may be connected to double-mode pulsation. The changes of the Blazhko and double-mode properties of the stars are also reviewed using the recent and archive photometric data. C1 [Jurcsik, J.; Smitola, P.; Sodor, A.; Nuspl, J.; Moor, A.; Pal, A.; Bakos, J.; Kelemen, J.; Kovacs, T.; Kriskovics, L.; Sarneczky, K.; Vida, K.] Hungarian Acad Sci, Konkoly Observ, H-1525 Budapest, Hungary. [Hajdu, G.] Pontificia Univ Catolica Chile, Inst Astrofis, Santiago 7820436, Chile. [Hajdu, G.] Inst Milenio Astrofis, Santiago, Chile. [Kolenberg, K.] Katholieke Univ Leuven, Inst Astron, B-3001 Heverlee, Belgium. [Kolenberg, K.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Furesz, G.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Kun, E.] Univ Szeged, Dept Theoret Phys, H-6720 Szeged, Hungary. [Kun, E.] Univ Szeged, Dept Expt Phys, H-6720 Szeged, Hungary. [Kun, E.] Univ Szeged, Astron Observ, H-6720 Szeged, Hungary. [Szalai, T.] Univ Szeged, Dept Opt & Quantum Elect, H-6720 Szeged, Hungary. [Szing, A.] Univ Szeged, Baja Observ, H-6500 Baja, Hungary. RP Jurcsik, J (reprint author), Hungarian Acad Sci, Konkoly Observ, POB 67, H-1525 Budapest, Hungary. EM jurcsik@konkoly.hu OI Hajdu, Gergely/0000-0003-0594-9138 FU Ministry for the Economy, Development, and Tourisms Programa Iniciativa Cientifica Milenio [IC210009]; Proyecto Basal [PFB-06/2007]; Fondecyt [1141141]; CONICYT [Anillo ACT1101]; Marie Curie International Outgoing Fellowship within the 7th European Community Framework Programme [PIOF 255267 SAS-RRL]; OTKA grant [K-83790]; MTA CSFK Lendulet Disk Research Group; Lendulet program of the HAS; Hungarian OTKA grant [K-104607]; ESA PECS [4000110889/14/NL/NDe]; [LP2012-31]; [K-109276] FX The authors would like to express their acknowledgment to the referee for the notes, questions, and comments, which helped us improve the clarity and quality of the paper. G.H. acknowledges support by the Ministry for the Economy, Development, and Tourisms Programa Iniciativa Cientifica Milenio through grant IC210009, awarded to the Millennium Institute of Astrophysics; by Proyecto Basal PFB-06/2007; by Fondecyt grant 1141141; and by grants CONICYT Anillo ACT1101 CONICYT-PCHA/Doctorado Nacional/2014-63140099. K.K. is supported by a Marie Curie International Outgoing Fellowship within the 7th European Community Framework Programme (PIOF 255267 SAS-RRL). N.J. acknowledges the OTKA K-83790 grant; M.A. the grant of the MTA CSFK Lendulet Disk Research Group; and A.P. the LP2012-31, K-109276, and K-104607 grants. K.S. has been supported by the Lendulet-2009 program of the HAS, the Hungarian OTKA grant K-104607, and the ESA PECS Contract No. 4000110889/14/NL/NDe. NR 58 TC 6 Z9 6 U1 0 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0067-0049 EI 1538-4365 J9 ASTROPHYS J SUPPL S JI Astrophys. J. Suppl. Ser. PD AUG PY 2015 VL 219 IS 2 AR 25 DI 10.1088/0067-0049/219/2/25 PG 26 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CS2CY UT WOS:000361876600011 ER PT J AU Thongkittidilok, C Tharasanit, T Songsasen, N Sananmuang, T Buarpung, S Techakumphu, M AF Thongkittidilok, Chommanart Tharasanit, Theerawat Songsasen, Nucharin Sananmuang, Thanida Buarpung, Sirirak Techakumphu, Mongkol TI Epidermal growth factor improves developmental competence and embryonic quality of singly cultured domestic cat embryos SO JOURNAL OF REPRODUCTION AND DEVELOPMENT LA English DT Article DE Blastocyst; Cat; Epidermal growth factor (EGF); Epidermal growth factor receptor (EGFR); Single-embryo culture ID IN-VITRO CULTURE; CELL-CYCLE PROGRESSION; BOVINE EMBRYOS; GENE-EXPRESSION; PREIMPLANTATION EMBRYOS; OOCYTE MATURATION; EGF; RECEPTOR; DENSITY; COCULTURE AB This study examined the influence of EGF on the expression of EGF receptors (EGFR) and developmental competence of embryos cultured individually versus those cultured in groups. Cat oocytes were in vitro matured and fertilized (IVM/IVF), and cleaved embryos were randomly assigned to one of seven culture conditions: one group each in which embryos were subjected to group culture supplemented with or without 5 ng/ml EGF and five groups in which embryos were subjected to single-embryo culture supplemented with EGF (0, 5, 25, 50 or 100 ng/ml). Morulae, blastocysts and hatching blastocysts were assessed at days 5 and 7; post IVF, respectively, and total blastocyst cell numbers were assessed at day 7. Relative mRNA expressions of EGFR of 2-4-cell embryos, 8-16-cell embryos, morulae and blastocysts cultured in groups or singly with or without EGF supplementation were examined. OCT3/4 and Ki67 in blastocysts derived from the group or single-embryo culture systems with or without EGF supplementation were localized. A higher rate of embryos cultured in groups developed to blastocysts than individually incubated cohorts. Although EGF increased blastocyst formation in the single-embryo culture system, EGF did not affect embryo development in group culture. Expression levels of EGFR decreased in morulae and blastocysts cultured with EGF. An increased ratio of Ki67-positive cells to the total number of cells in the blastocyst was observed in singly cultured embryos in the presence of EGF. However, EGF did not affect the expression of OCT3/4. These findings indicate that EGF enhanced developmental competence of cat embryos cultured singly by stimulating cell proliferation and modulating the EGFR expression at various developmental stages. C1 [Thongkittidilok, Chommanart; Tharasanit, Theerawat; Buarpung, Sirirak; Techakumphu, Mongkol] Chulalongkorn Univ, Fac Vet Sci, Dept Obstet Gynaecol & Reprod, Bangkok 10330, Thailand. [Songsasen, Nucharin] Natl Zool Pk, Smithsonian Conservat Biol Inst, Ft Belvoir, VA 22630 USA. [Sananmuang, Thanida] Rajamangala Univ Technol, Fac Vet Med, Chon Buri 20110, Thailand. RP Techakumphu, M (reprint author), Chulalongkorn Univ, Fac Vet Sci, Dept Obstet Gynaecol & Reprod, Bangkok 10330, Thailand. EM tmongkol@chula.ac.th FU Royal Golden Jubilee Ph.D. Program, Thailand Research Fund (TRF) [PHD0032/2553]; 90th Anniversary of Chulalongkorn University Fund; [TRF-RSA5680028] FX C Thongkittidilok is the recipient of a grant from the Royal Golden Jubilee Ph.D. Program (PHD0032/2553), Thailand Research Fund (TRF). This research was financially supported by the 90th Anniversary of Chulalongkorn University Fund and TRF-RSA5680028. Finally, the authors would like to thank the Veterinary Public Health Division of the Bangkok Metropolitan Administration, Thailand, for sample collection. NR 69 TC 3 Z9 3 U1 0 U2 4 PU SOCIETY REPRODUCTION & DEVELOPMENT-SRD PI TSUKUBA PA C/O KAZUHIRO KIKUCHI, PHD DVM, NATL INST AGROBIOLOGICAL SCIENCES KANNONDAI 2-1-2, TSUKUBA, IBARAKI 305-8602, JAPAN SN 0916-8818 J9 J REPROD DEVELOP JI J. Reprod. Dev. PD AUG PY 2015 VL 61 IS 4 BP 269 EP 276 PG 8 WC Agriculture, Dairy & Animal Science; Reproductive Biology SC Agriculture; Reproductive Biology GA CR3YR UT WOS:000361269500004 PM 25985792 ER PT J AU Frye, JA Robbins, RK AF Frye, Jennifer A. Robbins, Robert K. TI Is the globally rare frosted elfin butterfly (Lycaenidae) two genetically distinct host plant races in Maryland? DNA evidence from cast larval skins provides an answer SO JOURNAL OF INSECT CONSERVATION LA English DT Article DE Callophrys irus; Wild indigo; Lupine; Host plant races; Mitochondrial CO1 DNA barcodes; Deer ID CALLOPHRYS-IRUS; LEPIDOPTERA; SPECIATION; CATERPILLARS; LUPINE AB Frosted elfin butterfly caterpillars (Callophrys irus) eat either lupine (Lupinus perennis) or wild indigo (Baptisia tinctoria) legumes. Data from larval behavior, adult morphology, demographics, and phenology have led to the suggestion that lupine-feeding populations are genetically distinct from wild indigo-feeding populations. Frosted elfins are of conservation concern throughout their range in the eastern half of North America, and the possibility of host plant races-in which females pass genetically determined oviposition preferences to their daughters-complicates assessments of this vulnerable species. The maternal inheritance of mitochondrial DNA sequences makes CO1 an excellent gene to determine if genetically distinct host plant races have evolved in frosted elfins. In this paper, we extracted DNA using cast larval skins, a non-lethal, minimal-disturbance method appropriate for insects of conservation concern. Fifty eggs and caterpillars were taken from the field, reared in the lab until molting, and then returned to the plant on which they were found. Over 80 % of individuals had DNA successfully sequenced from their cast larval skins. The sequences allowed unequivocal identification. Neither the lupine-feeding nor wild indigo-feeding populations formed monophyletic clusters because many lupine-feeding and wild-indigo feeding individuals shared the same CO1 658 base pair sequence. An isolated population from the mountains of western Maryland was also not genetically distinct from a coastal population 345 km to the east. These results show the usefulness of using cast larval skins as a non-lethal source of DNA in listed species and suggest that frosted elfins are generalist feeders of lupine and wild indigo and are not comprised of two genetically distinct host plant races. C1 [Frye, Jennifer A.] Maryland Dept Nat Resources, Nat Heritage Program, Wye Mills, MD 21601 USA. [Robbins, Robert K.] Smithsonian Inst, Dept Entomol, Washington, DC 20013 USA. RP Frye, JA (reprint author), Maryland Dept Nat Resources, Nat Heritage Program, 909 Wye Mills Rd, Wye Mills, MD 21601 USA. EM Jennifer.frye@maryland.gov; RobbinsR@SI.edu FU State Wildlife Grant from the US Fish and Wildlife Service; Department of Entomology, NMNH, Smithsonian Institution FX We thank the following individuals for their assistance in all aspects of field work: Paula Becker, Danny Thomas, Chris Frye, John Moulis, Kyle Rambo, Wes Knapp, Joe Fehrer Sara Tangren, and numerous volunteers from the Maryland DNR and the Nature Conservancy, most notably Jeff Bacon, Gordon and Mary Burton, David Hindle, Gary Marine, Tom Ogden, Margaret Schultz, Robert Turk and Tom Ogden. We thank Brian Harris and Margaret Rosati at Smithsonian for technical support, and Scott Miller (who urged us to use cast larval skins as a source for mitochondrial DNA), Paul Goldstein, and Karie Darrow for helpful advice. Dana Limpert at Maryland DNR provided mapmaking expertise, and Jeremy deWaard at Guelph greatly facilitated the sequencing of our samples. For reviewing and commenting on the manuscript, we are grateful to Robert Busby, Paul Goldstein, Scott Miller, Richard Smith, and David Wagner. Two anonymous reviewers and the Editor made many helpful suggestions, for which we are grateful. This project was funded in part through a State Wildlife Grant from the US Fish and Wildlife Service, and through the Department of Entomology, NMNH, Smithsonian Institution. NR 33 TC 2 Z9 2 U1 3 U2 9 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 1366-638X EI 1572-9753 J9 J INSECT CONSERV JI J. Insect Conserv. PD AUG PY 2015 VL 19 IS 4 BP 607 EP 615 DI 10.1007/s10841-015-9783-4 PG 9 WC Biodiversity Conservation; Entomology SC Biodiversity & Conservation; Entomology GA CQ8IF UT WOS:000360850000001 ER PT J AU Betremieux, Y Kaltenegger, L AF Betremieux, Yan Kaltenegger, Lisa TI Refraction in planetary atmospheres: improved analytical expressions and comparison with a new ray-tracing algorithm SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE radiative transfer; atmospheric effects; methods: analytical; methods: numerical; planets and satellites: atmospheres ID EARTH GJ 1214B; LUNAR ECLIPSE OBSERVATIONS; TRANSMISSION SPECTROSCOPY; RAYLEIGH-SCATTERING; SUPER-EARTHS; WATER-VAPOR; TRANSIT; EXOPLANET; SPECTRUM; SEARCH AB Atmospheric refraction affects to various degrees exoplanet transit, lunar eclipse, as well as stellar occultation observations. Exoplanet retrieval algorithms often use analytical expressions for the column abundance along a ray traversing the atmosphere as well as for the deflection of that ray, which are first-order approximations valid for low densities in a spherically symmetric homogeneous isothermal atmosphere. We derive new analytical formulae for both of these quantities, which are valid for higher densities, and use them to refine and validate a new ray-tracing algorithm which can be used for arbitrary atmospheric temperature-pressure profiles. We illustrate with simple isothermal atmospheric profiles the consequences of our model for different planets: temperate Earth-like and Jovian-like planets, as well as HD 189733b, and GJ1214b. We find that, for both hot exoplanets, our treatment of refraction does not make much of a difference to pressures as high as 10 atm, but that it is important to consider the variation of gravity with altitude for GJ1214b. However, we find that the temperate atmospheres have an apparent scaleheight significantly smaller than their actual density scaleheight at densities larger than 1 amagat, thus increasing the difficulty of detecting spectral features originating in these regions. These denser atmospheric regions form a refractive boundary layer where column abundances and ray deflection increases dramatically with decreasing impact parameter. This refractive boundary layer mimics a surface, and none of the techniques mentioned above can probe atmospheric regions denser than about 4 amagat on these temperate planets. C1 [Betremieux, Yan; Kaltenegger, Lisa] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Kaltenegger, Lisa] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Betremieux, Y (reprint author), Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany. EM betremieux@mpia.de FU DFG [ENP Ka 3142/1-1]; National Aeronautics and Space Administration FX The authors acknowledge support from DFG funding ENP Ka 3142/1-1. This research has made use of the NASA Exoplanet Archive, which is operated by the California Institute of Technology, under contract with the National Aeronautics and Space Administration under the Exoplanet Exploration Program. NR 43 TC 2 Z9 2 U1 1 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 AUG 1 PY 2015 VL 451 IS 2 BP 1268 EP 1283 DI 10.1093/mnras/stv1078 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CQ8BB UT WOS:000360830000009 ER PT J AU Li, GJ Naoz, S Kocsis, B Loeb, A AF Li, Gongjie Naoz, Smadar Kocsis, Bence Loeb, Abraham TI Implications of the eccentric Kozai-Lidov mechanism for stars surrounding supermassive black hole binaries SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE black hole physics; galaxies: kinematics and dynamics; galaxies: nuclei ID HIERARCHICAL 3-BODY SYSTEMS; TIDAL DISRUPTION EVENTS; GALACTIC-CENTER; STELLAR-SYSTEMS; RESONANT RELAXATION; SECULAR EVOLUTION; TEST PARTICLE; HOT JUPITERS; AGN DISCS; MASS AB An enhanced rate of stellar tidal disruption events (TDEs) may be an important characteristic of supermassive black hole (SMBH) binaries at close separations. Here, we study the evolution of the distribution of stars around an SMBH binary due to the eccentric Kozai-Lidov (EKL) mechanism, including octupole effects and apsidal precession caused by the stellar mass distribution and general relativity. We identify a region around one of the SMBHs in the binary where the EKL mechanism drives stars to high eccentricities, which ultimately causes the stars to either scatter off the second SMBH or get disrupted. For SMBH masses 10(7) and 10(8) M-circle dot, the TDE rate can reach similar to 10(-2) yr(-1) and deplete a region of the stellar cusp around the secondary SMBH in similar to 0.5 Myr. As a result, the final geometry of the stellar distribution between 0.01 and 0.1 pc around the secondary SMBH is a torus. These effects may be even more prominent in nuclear stellar clusters hosting a supermassive and an intermediate mass black hole. C1 [Li, Gongjie; Loeb, Abraham] Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, Cambridge, MA 02138 USA. [Naoz, Smadar] Univ Calif Los Angeles, Div Astron & Astrophys, Dept Phys & Astron, Los Angeles, CA 90095 USA. [Kocsis, Bence] Inst Adv Study, Princeton, NJ 08540 USA. RP Li, GJ (reprint author), Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, 60 Garden St, Cambridge, MA 02138 USA. EM gli@cfa.harvard.edu RI Kocsis, Bence/C-3061-2013 OI Kocsis, Bence/0000-0002-4865-7517 FU NSF [AST-1312034]; W. M. Keck Foundation Fund of the Institute for Advanced Study; NASA [NNX11AF29G, NNX14AM24G] FX This work was supported in part by NSF grant AST-1312034. BK was supported in part by the W. M. Keck Foundation Fund of the Institute for Advanced Study and NASA grants NNX11AF29G and NNX14AM24G. The numerical calculations were performed at the Harvard-Smithsonian Center for Astrophysics, the Institute for Theory and Computation, on Harvard Odyssey cluster. NR 95 TC 11 Z9 11 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 AUG 1 PY 2015 VL 451 IS 2 BP 1341 EP 1349 DI 10.1093/mnras/stv1031 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CQ8BB UT WOS:000360830000016 ER PT J AU Zhu, YC Narayan, R Sadowski, A Psaltis, D AF Zhu, Yucong Narayan, Ramesh Sadowski, Aleksander Psaltis, Dimitrios TI HERO - A 3D general relativistic radiative post-processor for accretion discs around black holes SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE accretion, accretion discs; black hole physics; radiative transfer; methods: numerical ID FLUX-LIMITED DIFFUSION; MONTE-CARLO METHOD; PROTOPLANETARY DISKS; NEUTRINO TRANSPORT; TRANSFER EQUATION; HYDRODYNAMICS; CODE; SIMULATIONS; ALGORITHM; DIMENSIONS AB HERO (Hybrid Evaluator for Radiative Objects) is a 3D general relativistic radiative transfer code which has been tailored to the problem of analysing radiation from simulations of relativistic accretion discs around black holes. HERO is designed to be used as a post-processor. Given some fixed fluid structure for the disc (i.e. density and velocity as a function of position from a hydrodynamic or magnetohydrodynamic simulation), the code obtains a self-consistent solution for the radiation field and for the gas temperatures using the condition of radiative equilibrium. The novel aspect of HERO is that it combines two techniques: (1) a short-characteristics (SC) solver that quickly converges to a self-consistent disc temperature and radiation field, with (2) a long-characteristics (LC) solver that provides a more accurate solution for the radiation near the photosphere and in the optically thin regions. By combining these two techniques, we gain both the computational speed of SC and the high accuracy of LC. We present tests of HERO on a range of 1D, 2D, and 3D problems in flat space and show that the results agree well with both analytical and benchmark solutions. We also test the ability of the code to handle relativistic problems in curved space. Finally, we discuss the important topic of ray defects, a major limitation of the SC method, and describe our strategy for minimizing the induced error. C1 [Zhu, Yucong; Narayan, Ramesh] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Sadowski, Aleksander] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Psaltis, Dimitrios] Univ Arizona, Tucson, AZ 85721 USA. RP Zhu, YC (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM yzhu@cfa.harvard.edu OI Narayan, Ramesh/0000-0002-1919-2730 FU NSF [AST1312651]; NASA [NNX 14AB47G, NAS8-03060]; NASA - Chandra X-ray Center [PF4-150126]; NSF XSEDE [TG-AST080026N] FX We would like to thank Nathan Roth, Jack Steiner, Jonathan McKinney, James Guillonchon, Jeff McClintock, Yan-Fei Jiang, Javier Garcia, Eric Keto, and Jiachen Jiang for their excellent insights on radiative transfer and comments/suggestions regarding HERO. We also thank our anonymous referee for their many suggestions that have greatly improved the cohesiveness of this paper (especially their recommendations of several relativistic benchmark tests). RN and YZ acknowledge support from NSF grant AST1312651 and NASA grant NNX 14AB47G. AS acknowledges support for this work by NASA through Einstein Post-doctoral Fellowships PF4-150126, awarded by the Chandra X-ray Center, which is operated by the Smithsonian Astrophysical Observatory for NASA under contract NAS8-03060. Finally, we are grateful for support from NSF XSEDE grant TG-AST080026N, the NASA HEC Programme, and the Harvard Odyssey cluster for providing computing resources used in developing this code. NR 87 TC 8 Z9 8 U1 0 U2 1 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD AUG 1 PY 2015 VL 451 IS 2 BP 1661 EP 1681 DI 10.1093/mnras/stv1046 PG 21 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CQ8BB UT WOS:000360830000041 ER PT J AU Dey, A Torrey, P Rubin, KHR Ben Zhu, G Suresh, J AF Dey, Arjun Torrey, Paul Rubin, Kate H. R. Ben Zhu, Guangtun Suresh, Joshua TI On the cosmic evolution of Fe/Mg in QSO absorption line systems SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies: abundances; galaxies: evolution; galaxies: haloes; intergalactic medium; quasars: absorption lines ID MG II ABSORBERS; DIGITAL SKY SURVEY; MASS-METALLICITY RELATION; DELAY-TIME DISTRIBUTION; HUBBLE-SPACE-TELESCOPE; HIGH-REDSHIFT GALAXIES; STAR-FORMING GALAXIES; SIMILAR-TO 0.5; GALACTIC OUTFLOWS; COSMOLOGICAL SIMULATIONS AB We investigate the variation of the ratio of the equivalent widths of the Fe II lambda 2600 line to the Mg II lambda lambda 2796, 2803 doublet as a function of redshift in a large sample of absorption lines drawn from the Johns Hopkins University - Sloan Digital Sky Survey Absorption Line Catalog. We find that despite large scatter, the observed ratio shows a trend where the equivalent width ratio R = W-Fe II/W-Mg II decreases monotonically with increasing redshift z over the range 0.55 <= z <= 1.90. Selecting the subset of absorbers where the signal-to-noise ratio of the MgII equivalent width W-Mg II is >= 3 and modelling the equivalent width ratio distribution as a Gaussian, we find that the mean of the Gaussian distribution varies as R proportional to (-0.045 +/- 0.005)z. We discuss various possible reasons for the trend. A monotonic trend in the Fe/Mg abundance ratio is predicted by a simple model where the abundances of Mg and Fe in the absorbing clouds are assumed to be the result of supernova (SN) ejecta and where the cosmic evolution in the SNIa and core-collapse SN rates is related to the cosmic star formation rate. If the trend in R reflects the evolution in the abundances, then it is consistent with the predictions of the simple model. C1 [Dey, Arjun] Natl Opt Astron Observ, Tucson, AZ 85726 USA. [Torrey, Paul] CALTECH, Pasadena, CA 91125 USA. [Torrey, Paul] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Rubin, Kate H. R.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Ben Zhu, Guangtun; Suresh, Joshua] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. RP Dey, A (reprint author), Harvard Univ, Radcliffe Inst Adv Study, Byerly Hall,8 Garden St, Cambridge, MA 02138 USA. EM dey@noao.edu OI Zhu, Guangtun/0000-0002-7574-8078; Torrey, Paul/0000-0002-5653-0786 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; NASA through Hubble Fellowship - Space Telescope Science Institute [HST-HF2-51351, NAS 5-26555]; National Optical Astronomy Observatory (NOAO) FX This research made use of the JHU-SDSS Metal Absorption Line Catalog (ZM13), which is based on the SDSS DR7 (Abazajian et al. 2009), and the NIST Atomic Spectra Database (Kramida et al. 2013). We thank Dr Brice Menard for useful advice and for putting together such a scientifically useful resource. AD thanks Joan Najita for assistance with the ASURV package and Tom Matheson for useful comments on the manuscript. We are grateful to the referee for a constructive report that resulted in improving this paper. Funding for the SDSS and SDSS-II was 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/. GBZ acknowledges partial support provided by NASA through Hubble Fellowship grant #HST-HF2-51351 awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under contract NAS 5-26555. AD's research activities are supported by the National Optical Astronomy Observatory (NOAO). AD thanks the Radcliffe Institute for Advanced Study and the Institute for Theory and Computation at Harvard University for their generous support during the period when this paper was written. NOAO is operated by the Association of Universities for Research in Astronomy (AURA) under cooperative agreement with the National Science Foundation. NR 62 TC 1 Z9 1 U1 0 U2 0 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD AUG 1 PY 2015 VL 451 IS 2 BP 1806 EP 1814 DI 10.1093/mnras/stv604 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CQ8BB UT WOS:000360830000052 ER PT J AU Silverman, JM Vinko, J Marion, GH Wheeler, JC Barna, B Szalai, T Mulligan, BW Filippenko, AV AF Silverman, Jeffrey M. Vinko, Jozsef Marion, G. H. Wheeler, J. Craig Barna, Barnabas Szalai, Tamas Mulligan, Brian W. Filippenko, Alexei V. TI High-velocity features of calcium and silicon in the spectra of Type Ia supernovae SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE methods: data analysis; techniques: spectroscopic; supernovae: general ID HUBBLE-SPACE-TELESCOPE; TIME OPTICAL-SPECTRA; LOW-LUMINOSITY HOST; WHITE-DWARF STAR; SN 2011FE; LIGHT CURVES; SPECTROSCOPIC OBSERVATIONS; COSMOLOGICAL CONSTRAINTS; CIRCUMSTELLAR MATERIAL; DIVERSITY AB 'High-velocity features' (HVFs) are spectral features in Type Ia supernovae (SNe Ia) that have minima indicating significantly higher (by greater than about 6000 km s-1) velocities than typical 'photospheric-velocity features' (PVFs). The PVFs are absorption features with minima indicating typical photospheric (i.e. bulk ejecta) velocities (usually similar to 9000-15 000 km s(-1) near B-band maximum brightness). In this work, we undertake the most in-depth study of HVFs ever performed. The data set used herein consists of 445 low-resolution optical and near-infrared (NIR) spectra (at epochs up to 5 d past maximum brightness) of 210 low-redshift SNe Ia that follow the 'Phillips relation'. A series of Gaussian functions is fit to the data in order to characterize possible HVFs of Ca II H&K, Si II lambda 6355, and the Ca II NIR triplet. The temporal evolution of the velocities and strengths of the PVFs and HVFs of these three spectral features is investigated, as are possible correlations with other SN Ia observables. We find that while HVFs of Ca II are regularly observed (except in underluminous SNe Ia, where they are never found), HVFs of Si II lambda 6355 are significantly rarer, and they tend to exist at the earliest epochs and mostly in objects with large photospheric velocities. It is also shown that stronger HVFs of Si II lambda 6355 are found in objects that lack C II absorption at early times and that have red ultraviolet/optical colours near maximum brightness. These results lead to a self-consistent connection between the presence and strength of HVFs of Si II lambda 6355 and many other mutually correlated SN Ia observables, including photospheric velocity. C1 [Silverman, Jeffrey M.; Vinko, Jozsef; Marion, G. H.; Wheeler, J. Craig; Mulligan, Brian W.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA. [Vinko, Jozsef; Barna, Barnabas; Szalai, Tamas] Univ Szeged, Dept Opt & Quantum Elect, H-6720 Szeged, Hungary. [Marion, G. H.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Filippenko, Alexei V.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. RP Silverman, JM (reprint author), Univ Texas Austin, Dept Astron, RLM 15308, Austin, TX 78712 USA. EM jsilverman@astro.as.utexas.edu FU W. M. Keck Foundation; NASA; NSF [AST-1302771, AST 11-09801, AST-1211916, PHY-1066293]; Hungarian OTKA [NN 107637, PD 112325]; Christopher R. Redlich Fund; TABASGO Foundation FX We thank the referee, M. J. Childress, for useful comments and stimulating discussion that helped improve this paper, R. J. Foley, K. Maguire, A. A. Miller, and L. Wang for useful discussions, and the staffs at the Lick, Keck, and McDonald Observatories for their assistance with the observations. The HET is a joint project of the University of Texas at Austin, the Pennsylvania State University, Stanford University, Ludwig-Maximilians-Universitat Munchen, and Georg-August-Universitat Gottingen. The HET is named in honor of its principal benefactors, William P. Hobby and Robert E. Eberly. The Marcario LRS is named for Mike Marcario of High Lonesome Optics who fabricated several optics for the instrument but died before its completion. The LRS is a joint project of the HET partnership and the Instituto de Astronomia de la Universidad Nacional Autonoma de Mexico. 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 NASA; 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 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. JMS is supported by an NSF Astronomy and Astrophysics Postdoctoral Fellowship under award AST-1302771. JV and TS are supported by Hungarian OTKA Grants NN 107637 and PD 112325, respectively. JCW's supernova group at UT Austin is supported by NSF Grant AST 11-09801. AVF is grateful for support from the Christopher R. Redlich Fund, the TABASGO Foundation, and NSF grant AST-1211916. Some work on this paper was done in the hospitable climate of the Aspen Center for Physics that is supported by NSF Grant PHY-1066293. NR 121 TC 17 Z9 17 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 AUG 1 PY 2015 VL 451 IS 2 BP 1973 EP 2014 DI 10.1093/mnras/stv1011 PG 42 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CQ8BB UT WOS:000360830000065 ER PT J AU Castelli, F Kurucz, RL Cowley, CR AF Castelli, F. Kurucz, R. L. Cowley, C. R. TI New Mn II energy levels from the STIS-HST spectrum of the HgMn star HD175640 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE line: identification; atomic data; stars: atmospheres; stars: chemically peculiar; stars: individual: HD 175640 ID OSCILLATOR-STRENGTHS; TRANSITION-PROBABILITIES; CHI-LUPI; GA-II; ULTRAVIOLET TRANSITIONS; LIFETIME MEASUREMENTS; IONIZED GOLD; ATOMIC DATA; PD II; LINES AB Aims. The NIST database lists several Mn II lines that were observed in the laboratory but not classified. They cannot be used in spectrum synthesis because their atomic line data are unknown. These lines are concentrated in the 2380-2700 angstrom interval. We aimed to assign energy levels and log gf values to these lines. Methods. Semi-empirical line data for Mn II computed by Kurucz were used to synthesize the ultraviolet spectrum of the slow-rotating, HgMn star HD175640. The spectrum was compared with the high-resolution spectrum observed with the HST-STIS equipment. A UVES spectrum covering the 3050-10 000 angstrom region was also examined. Results. We determined a total of 73 new energy levels, 58 from the STIS spectrum of HD175640 and another 15 from the UVES spectrum. The new energy levels give rise to numerous new computed lines. We have identified more than 50% of the unclassified lines listed in the NIST database and have changed the assignment of another 24 lines. An abundance analysis of the star HD175640, based on the comparison of observed and computed ultraviolet spectra in the 1250-3040 angstrom interval, is the by-product of this study on Mn II. C1 [Castelli, F.] Osserv Astron Trieste, Ist Nazl Astrofis, I-34143 Trieste, Italy. [Kurucz, R. L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Cowley, C. R.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. RP Castelli, F (reprint author), Osserv Astron Trieste, Ist Nazl Astrofis, Via Tiepolo 11, I-34143 Trieste, Italy. EM castelli@oats.inaf.it; rkurucz@cfa.harvard.edu; cowley@umich.edu NR 47 TC 2 Z9 2 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 EI 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD AUG PY 2015 VL 580 AR A10 DI 10.1051/0004-6361/201525903 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CP6TD UT WOS:000360020200010 ER PT J AU Falstad, N Gonzalez-Alfonso, E Aalto, S van der Werf, PP Fischer, J Veilleux, S Melendez, M Farrah, D Smith, HA AF Falstad, N. Gonzalez-Alfonso, E. Aalto, S. van der Werf, P. P. Fischer, J. Veilleux, S. Melendez, M. Farrah, D. Smith, H. A. TI Herschel spectroscopic observations of the compact obscured nucleus in Zw 049.057 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE ISM: molecules; galaxies: ISM; galaxies: individual: Zw 049.057; line: formation; infrared: galaxies; submillimeter: galaxies ID LUMINOUS INFRARED GALAXIES; ACTIVE GALACTIC NUCLEI; STAR-FORMING GALAXIES; WATER-VAPOR; NGC 4418; MOLECULAR OUTFLOWS; RADIATION PRESSURE; MARKARIAN 231; DISSOCIATIVE RECOMBINATION; ROTATIONAL-EXCITATION AB Context. The luminous infrared galaxy Zw 049.057 contains a compact obscured nucleus where a considerable amount of the galaxy's luminosity is generated. This nucleus contains a dusty environment that is rich in molecular gas. One approach to probing this kind of environment and to revealing what is hidden behind the dust is to study the rotational lines of molecules that couple well with the infrared radiation emitted by the dust. Aims. We probe the physical conditions in the core of Zw 049.057 and establish the nature of its nuclear power source (starburst or active galactic nucleus). Methods. We observed Zw 049.057 with the Photodetector Array Camera and Spectrometer (PACS) and the Spectral and Photometric Imaging Receiver (SPIRE) onboard the Herschel Space Observatory in rotational lines of H2O, (H2O)-O-18, OH, (OH)-O-18, and [O I]. We modeled the unresolved core of the galaxy using a spherically symmetric radiative transfer code. To account for the different excitation requirements of the various molecular transitions, we use multiple components and different physical conditions. Results. We present the full high-resolution SPIRE FTS spectrum of Zw 049.057, along with relevant spectral scans in the PACS range. We find that a minimum of two different components (nuclear and extended) are required in order to account for the rich molecular line spectrum of Zw 049.057. The nuclear component has a radius of 10-30 pc, a very high infrared surface brightness (similar to 10(14) L-circle dot kpc(-2)), warm dust (T-d > 100 K), and a very large H-2 column density (N-H2 = 10(24) - 10(25) cm(-2)). The modeling also indicates high nuclear H2O (similar to 5 x 10(-6)) and OH (similar to 4 x 10(-6)) abundances relative to H-2 as well as a low O-16/O-18-ratio of 50-100. We also find a prominent infall signature in the [O I] line. We tentatively detect a 500 km s(-1) outflow in the H2O 3(13) -> 2(02) line. Conclusions. The high surface brightness of the core indicates the presence of either a buried active galactic nucleus or a very dense nuclear starburst. The estimated column density towards the core of Zw 049.057 indicates that it is Compton-thick, making a buried X-ray source difficult to detect even in hard X-rays. We discuss the elevated H2O abundance in the nucleus in the context of warm grain and gas-phase chemistry. The H2O abundance is comparable to that of other compact (ultra-)luminous infrared galaxies such as NGC 4418 and Arp 220 - and also to hot cores in the Milky Way. The enhancement of O-18 is a possible indicator that the nucleus of Zw 049.057 is in a similar evolutionary stage as the nuclei of Arp 220 - and more advanced than NGC 4418. We discuss the origin of the extreme nuclear gas concentration and note that the infalling gas detected in [O I] implies that the gas reservoir in the central region of Zw 049.057 is being replenished. If confirmed, the H2O outflow suggests that the nucleus is in a stage of rapid evolution. C1 [Falstad, N.; Aalto, S.] Chalmers, Dept Earth & Space Sci, Onsala Space Observ, S-43992 Onsala, Sweden. [Gonzalez-Alfonso, E.] Univ Alcala de Henares, Dept Fis, Madrid 28871, Spain. [van der Werf, P. P.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [Fischer, J.] US Navy, Res Lab, Remote Sensing Div, Washington, DC 20375 USA. [Veilleux, S.; Melendez, M.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Farrah, D.] Virginia Tech, Dept Phys, Blacksburg, VA 24061 USA. [Smith, H. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Falstad, N (reprint author), Chalmers, Dept Earth & Space Sci, Onsala Space Observ, S-43992 Onsala, Sweden. EM niklas.falstad@chalmers.se FU Swedish National Space Board [145/11:1B, 285/12, 145/11:1-3]; US-ONR; NHSC/ JPL [1456609] FX We thank the anonymous referee for a thorough and constructive report that helped improve the paper. N.F. and S.A. thank the Swedish National Space Board for generous grant support (grant numbers 145/11:1B, 285/12 and 145/11:1-3). Basic research in IR astronomy at NRL is funded by the US-ONR; J.F. acknowledges support from NHSC/ JPL subcontract 1456609. NR 102 TC 7 Z9 7 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 EI 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD AUG PY 2015 VL 580 AR A52 DI 10.1051/0004-6361/201526114 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CP6TD UT WOS:000360020200052 ER PT J AU Forbrich, J Lada, CJ Lombardi, M Roman-Zuniga, C Alves, J AF Forbrich, Jan Lada, Charles J. Lombardi, Marco Roman-Zuniga, Carlos Alves, Joao TI Smoke in the Pipe Nebula: dust emission and grain growth in the starless core FeSt 1-457 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE dust, extinction; stars: formation; submillimeter: ISM; infrared: ISM; radio lines: ISM ID NEAR-INFRARED SURVEY; SPECTRAL INDEX; EXTINCTION MAPS; TEMPERATURE; NOISE; SUBMILLIMETER; POPULATION; HERSCHEL; DENSITY; APEX AB Context. The availability of submillimeter dust emission data in an unprecedented number of bands provides us with new opportunities to investigate the properties of interstellar dust in nearby clouds. Aims. The nearby Pipe Nebula is an ideal laboratory to study starless cores. We here aim to characterize the dust properties of the FeSt 1-457 core, as well as the relation between the dust and the dense gas, using Herschel, Planck, 2MASS, ESO Very Large Telescope, APEX-Laboca, and IRAM 30 m data. Methods. We derive maps of submillimeter dust optical depth and effective dust temperature from Herschel data that were calibrated against Planck. After calibration, we then fit a modified blackbody to the long-wavelength Herschel data, using the Planck-derived dust opacity spectral index beta, derived on scales of 30' (or similar to 1 pc). We use this model to make predictions of the submillimeter flux density at 850 mu m, and we compare these in turn with APEX-Laboca observations. Our method takes into account any additive zeropoint offsets between the Herschel/Planck and Laboca datasets. Additionally, we compare the dust emission with near-infrared extinction data, and we study the correlation of high-density-tracing N2H+ emission with the coldest and densest dust in FeSt 1-457. Results. A comparison of the submillimeter dust optical depth and near-infrared extinction data reveals evidence for an increased submillimeter dust opacity at high column densities, interpreted as an indication of grain growth in the inner parts of the core. Additionally, a comparison of the Herschel dust model and the Laboca data reveals that the frequency dependence of the submillimeter opacity, described by the spectral index beta, does not change. A single beta that is only slightly different from the Planck-derived value is sufficient to describe the data, beta = 1.53 +/- 0.07. We apply a similar analysis to Barnard 68, a core with significantly lower column densities than FeSt 1-457, and we do not find evidence for grain growth but also a single beta. Finally, our previously reported finding of a correlation of N2H+ emission with lower effective dust temperatures is confirmed for FeSt 1-457 in mapping observations. Conclusions. While we find evidence for grain growth from the dust opacity in FeSt 1-457, we find no evidence for significant variations in the dust opacity spectral index beta on scales 0.02 < x < 1 pc (or 36 '' < x < 30'). The correction to the Planck-derived dust beta that we find in both cases is on the order of the measurement error, not including any systematic errors, and it would thus be reasonable to directly apply the dust beta from the Planck all-sky dust model. As a corollary, reliable effective temperature maps can be derived which would be otherwise affected by beta variations. Finally, we note that the angular resolution of extinction maps for the study of nearby starless cores remains unsurpassed. C1 [Forbrich, Jan; Alves, Joao] Univ Vienna, Dept Astrophys, A-1180 Vienna, Austria. [Forbrich, Jan; Lada, Charles J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Lombardi, Marco] Univ Milan, Dept Phys, I-20133 Milan, Italy. [Roman-Zuniga, Carlos] Univ Nacl Autonoma Mexico, Inst Astron, Ensenada 22860, Baja California, Mexico. RP Forbrich, J (reprint author), Univ Vienna, Dept Astrophys, Turkenschanzstr 17, A-1180 Vienna, Austria. EM jan.forbrich@univie.ac.at RI Roman-Zuniga, Carlos/F-6602-2016; OI Roman-Zuniga, Carlos/0000-0001-8600-4798; LOMBARDI, MARCO/0000-0002-3336-4965 FU Austrian Science Fund (FWF) FX We thank an anonymous referee for comments that helped us to clarify and significantly improve the paper, Ralf Launhardt for insightful discussions, Arnaud Belloche, Giorgio Siringo, and Axel Weiss for help with the Laboca data analysis, and Ted Bergin for providing us with the TRAM data from the Aguti et al. (2007) paper. Herschel is an ESA space observatory with science instruments provided by European-led Principal Investigator consortia and with important participation from NASA. APEX is a collaboration between Max Planck Institut fur Radioastronomie (MPIfR), Onsala Space Observatory (OSO), and the European Southern Observatory (ESO). This publication in A&A is supported by the Austrian Science Fund (FWF). NR 40 TC 3 Z9 3 U1 0 U2 0 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD AUG PY 2015 VL 580 AR A114 DI 10.1051/0004-6361/201425375 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CP6TD UT WOS:000360020200114 ER PT J AU La Palombara, N Esposito, P Mereghetti, S Novara, G Tiengo, A AF La Palombara, N. Esposito, P. Mereghetti, S. Novara, G. Tiengo, A. TI Follow-up observations of X-ray emitting hot subdwarf stars: the He-rich sdO BD+37 degrees 1977 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE stars: early-type; stars: individual: BD+37 degrees 1977; subdwarfs; X-rays: stars ID PHOTON IMAGING CAMERA; EXTREME HELIUM STARS; SUBLUMINOUS O-STARS; WHITE-DWARF; STELLAR WINDS; MASS-LOSS; COMPACT COMPANION; XMM-NEWTON; HD 49798; EVOLUTION AB We report on the results of the first XMM-Newton satellite observation of the luminous and helium-rich O-type subdwarf BD+37 degrees 1977 carried out in April 2014. X-ray emission is detected with a flux of about 4 x 10(-14) erg cm(-2) s(-1) (0.2-1.5 keV), corresponding to a f(X)/f(bol) ratio similar to 10(-7); the source spectrum is very soft, and is well fit by the sum of two plasma components at different temperatures. Both characteristics are in agreement with what is observed in the main-sequence early-type stars, where the observed X-ray emission is due to turbulence and shocks in the stellar wind. A smaller but still significant stellar wind has also been observed in BD+37 degrees 1977; therefore, we suggest that in this case the detected X-ray flux has the same origin. C1 [La Palombara, N.; Esposito, P.; Mereghetti, S.; Novara, G.; Tiengo, A.] Ist Astrofis Spaziale & Fis Cosm Milano, INAF, I-20133 Milan, Italy. [Esposito, P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Novara, G.; Tiengo, A.] IUSS, I-27100 Pavia, Italy. [Tiengo, A.] Ist Nazl Fis Nucl, Sez Pavia, I-27100 Pavia, Italy. RP La Palombara, N (reprint author), Ist Astrofis Spaziale & Fis Cosm Milano, INAF, Via Bassini 15, I-20133 Milan, Italy. EM nicola@iasf-milano.inaf.it OI La Palombara, Nicola/0000-0001-7015-6359 FU ESA Member States; NASA FX This work is based on observations obtained with XMM-Newton, an ESA science mission with instruments and contributions directly funded by ESA Member States and NASA. P.E. acknowledges a Fulbright Research Scholar grant administered by the US-Italy Fulbright Commission and is grateful to the Harvard-Smithsonian Center for Astrophysics for hosting him during his Fulbright exchange. NR 40 TC 3 Z9 3 U1 0 U2 2 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD AUG PY 2015 VL 580 AR A56 DI 10.1051/0004-6361/201526141 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CP6TD UT WOS:000360020200056 ER PT J AU Mancini, L Hartman, JD Penev, K Bakos, GA Brahm, R Ciceri, S Henning, T Csubry, Z Bayliss, D Zhou, G Rabus, M de Val-Borro, M Espinoza, N Jordan, A Suc, V Bhatti, W Schmidt, B Sato, B Tan, TG Wright, DJ Tinney, CG Addison, BC Noyes, RW Lazar, J Papp, I Sari, P AF Mancini, L. Hartman, J. D. Penev, K. Bakos, G. A. Brahm, R. Ciceri, S. Henning, Th. Csubry, Z. Bayliss, D. Zhou, G. Rabus, M. de Val-Borro, M. Espinoza, N. Jordan, A. Suc, V. Bhatti, W. Schmidt, B. Sato, B. Tan, T. G. Wright, D. J. Tinney, C. G. Addison, B. C. Noyes, R. W. Lazar, J. Papp, I. Sari, P. TI HATS-13b and HATS-14b: two transiting hot Jupiters from the HATSouth survey SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE planetary systems; stars: fundamental parameters; techniques: radial velocities; techniques: photometric; stars: individual: HATS-13 (aka GSC6928-00497); stars: individual: HATS-14 (aka GSC6926-00259) ID PLANETARY PARAMETERS; EXTRASOLAR PLANETS; SURFACE GRAVITIES; KEPLER FIELD; LIGHT CURVES; G STAR; STELLAR; TELESCOPE; MASS; SPECTROGRAPH AB We report the discovery of HATS-13b and HATS-14b, which are two hot-Jupiter transiting planets discovered by the HATSouth survey. The host stars are quite similar to each other (HATS-13: V = 13.9 mag, M-star = 0.96 M-circle dot, R-star = 0.89 R-circle dot, T-eff approximate to 5500 K, [Fe/H] = 0.05; HATS-14: V = 13.8 mag, M-star = 0.97 M-circle dot, R-star = 0.93 R-circle dot, T-eff approximate to 5350 K, [Fe/H] = 0.33) and both the planets orbit around them with a period of similar to 3 days and a separation of similar to 0.04 au. However, even though they are irradiated in a similar way, the physical characteristics of the two planets are very different. HATS-13b, with a mass of M-p = 0.543 +/- 0.072 M-J and a radius of R-p = 1.212 +/- 0.035 R-J, appears as an inflated planet, while HATS-14b, having a mass of M-p = 1.071 +/- 0.070 M-J and a radius of R-p = 1.039 +/- 0.032 R-J, is only slightly larger in radius than Jupiter. C1 [Mancini, L.; Ciceri, S.; Henning, Th.; Rabus, M.] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Hartman, J. D.; Penev, K.; Bakos, G. A.; Csubry, Z.; de Val-Borro, M.; Bhatti, W.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. [Brahm, R.; Rabus, M.; Espinoza, N.; Jordan, A.; Suc, V.] Pontificia Univ Catolica Chile, Inst Astrofis, Santiago 7820436, Chile. [Brahm, R.; Espinoza, N.; Jordan, A.] Millennium Inst Astrophys, Santiago 7820436, Chile. [Bayliss, D.] Univ Geneva, Astron Observ, CH-1290 Versoix, Switzerland. [Zhou, G.; Schmidt, B.] Australian Natl Univ, Canberra, ACT 0200, Australia. [Sato, B.] Tokyo Inst Technol, Dept Earth & Planetary Sci, Meguro Ku, Tokyo 1528551, Japan. [Tan, T. G.] Perth Exoplanet Survey Telescope, Perth, WA, Australia. [Wright, D. J.; Tinney, C. G.; Addison, B. C.] Univ New S Wales, Sch Phys, Exoplanetary Sci Grp, Sydney, NSW 2052, Australia. [Tinney, C. G.] UNSW, Sch Phys, Australian Ctr Astrobiol, Exoplanetary Sci UNSW, Sydney, NSW, Australia. [Noyes, R. W.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Lazar, J.; Papp, I.; Sari, P.] Hungarian Astron Assoc, H-1121 Budapest, Hungary. RP Mancini, L (reprint author), Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany. EM mancini@mpia.de OI Jordan, Andres/0000-0002-5389-3944; Penev, Kaloyan/0000-0003-4464-1371; Schmidt, Brian/0000-0001-6589-1287; Tinney, Christopher/0000-0002-7595-0970; Tan, Thiam-Guan/0000-0001-5603-6895 FU NSF MRI grant [NSF/AST-0723074]; NASA [NNX09AB29G, NNX12AH91H, NNX13AQ62G]; FONDECYT [1130857]; BASAL CATA [PFB-06]; Millenium Science Initiative, Chilean Ministry of Economy [IC120009]; CONICYT-PCHA/Doctorado Nacional; "Millenium Institute of Astrophysics (MAS)" of the Millennium Science Initiative, Chilean Ministry of Economy [IC120009]; ARC Laureate Fellowship [FL0992131]; Robert Martin Ayers Sciences Fund; [NSF/AST-1108686] FX Development of the HATSouth project was funded by NSF MRI grant NSF/AST-0723074, operations have been supported by NASA grants NNX09AB29G and NNX12AH91H, and follow-up observations receive partial support from grant NSF/AST-1108686. A.J. acknowledges support from FONDECYT project 1130857, BASAL CATA PFB-06, and project IC120009 "Millennium Institute of Astrophysics (MAS)" of the Millenium Science Initiative, Chilean Ministry of Economy. R.B. and N.E. are supported by CONICYT-PCHA/Doctorado Nacional. R.B. and N.E. acknowledge additional support from project IC120009 "Millenium Institute of Astrophysics (MAS)" of the Millennium Science Initiative, Chilean Ministry of Economy. V.S. acknowledges support form BASAL CATA PFB-06. K.P. acknowledges support from NASA grant NNX13AQ62G. This work is based on observations made with telescopes at the ESO Observatory of La Silla. This paper also uses observations obtained with facilities of the Las Cumbres Observatory Global Telescope. Work at the Australian National University is supported by ARC Laureate Fellowship Grant FL0992131. We acknowledge the use of the AAVSO Photometric All-Sky Survey (APASS), funded by the Robert Martin Ayers Sciences Fund, and the SIMBAD database, operated at CDS, Strasbourg, France. Operations at the MPG 2.2m Telescope are jointly performed by the Max Planck Gesellschaft and the European Southern Observatory. The imaging system GROND has been built by the high-energy group of MPE in collaboration with the LSW Tautenburg and ESO. We thank Regis Lachaume for his technical assistance during the observations at the MPG 2.2m Telescope. We are grateful to P. Sackett for her help in the early phase of the HATSouth project. The reduced light curves presented in this work will be made available at the CDS (http://cdsweb.u-strasbg.fr/). We acknowledge the use of the following internet-based resources: the ESO Digitized Sky Survey; the TEPCat catalog; the SIMBAD data base operated at CDS, Strasbourg, France; and the arXiv scientific paper preprint service operated by Cornell University. NR 56 TC 6 Z9 6 U1 1 U2 7 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 AUG PY 2015 VL 580 AR A63 DI 10.1051/0004-6361/201526069 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CP6TD UT WOS:000360020200063 ER PT J AU Morosan, DE Gallagher, PT Zucca, P O'Flannagain, A Fallows, R Reid, H Magdalenic, J Mann, G Bisi, MM Kerdraon, A Konovalenko, AA MacKinnon, AL Rucker, HO Thide, B Vocks, C Alexov, A Anderson, J Asgekar, A Avruch, IM Bentum, MJ Bernardi, G Bonafede, A Breitling, F Broderick, JW Brouw, WN Butcher, HR Ciardi, B de Geus, E Eisloffel, J Falcke, H Frieswijk, W Garrett, MA Griessmeier, J Gunst, AW Hessels, JWT Hoeft, M Karastergiou, A Kondratiev, VI Kuper, G van Leeuwen, J McKay-Bukowski, D McKean, JP Munk, H Orru, E Paas, H Pizzo, R Polatidis, AG Scaife, AMM Sluman, J Tasse, C Toribio, MC Vermeulen, R Zarka, P AF Morosan, D. E. Gallagher, P. T. Zucca, P. O'Flannagain, A. Fallows, R. Reid, H. Magdalenic, J. Mann, G. Bisi, M. M. Kerdraon, A. Konovalenko, A. A. MacKinnon, A. L. Rucker, H. O. Thide, B. Vocks, C. Alexov, A. Anderson, J. Asgekar, A. Avruch, I. M. Bentum, M. J. Bernardi, G. Bonafede, A. Breitling, F. Broderick, J. W. Brouw, W. N. Butcher, H. R. Ciardi, B. de Geus, E. Eisloeffel, J. Falcke, H. Frieswijk, W. Garrett, M. A. Griessmeier, J. Gunst, A. W. Hessels, J. W. T. Hoeft, M. Karastergiou, A. Kondratiev, V. I. Kuper, G. van Leeuwen, J. McKay-Bukowski, D. McKean, J. P. Munk, H. Orru, E. Paas, H. Pizzo, R. Polatidis, A. G. Scaife, A. M. M. Sluman, J. Tasse, C. Toribio, M. C. Vermeulen, R. Zarka, P. TI LOFAR tied-array imaging and spectroscopy of solar S bursts SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE Sun: corona; Sun: radio radiation; Sun: particle emission; Sun: magnetic fields ID III RADIO-BURSTS; FINE-STRUCTURE; CORONA; POLARIZATION; FREQUENCY; RADIATION; DENSITY; SPIKES AB Context. The Sun is an active source of radio emission that is often associated with energetic phenomena ranging from nanoflares to coronal mass ejections (CMEs). At low radio frequencies (<100 MHz), numerous millisecond duration radio bursts have been reported, such as radio spikes or solar S bursts (where S stands for short). To date, these have neither been studied extensively nor imaged because of the instrumental limitations of previous radio telescopes. Aims. Here, LOw Frequency ARray (LOFAR) observations were used to study the spectral and spatial characteristics of a multitude of S bursts, as well as their origin and possible emission mechanisms. Methods. We used 170 simultaneous tied-array beams for spectroscopy and imaging of S bursts. Since S bursts have short timescales and fine frequency structures, high cadence (similar to 50 ms) tied-array images were used instead of standard interferometric imaging, that is currently limited to one image per second. Results. On 9 July 2013, over 3000 S bursts were observed over a time period of similar to 8 h. S bursts were found to appear as groups of short-lived (<1 s) and narrow-bandwidth (similar to 2.5 MHz) features, the majority drifting at similar to 3.5 MHz s(-1) and a wide range of circular polarisation degrees (2-8 times more polarised than the accompanying Type III bursts). Extrapolation of the photospheric magnetic field using the potential field source surface (PFSS) model suggests that S bursts are associated with a trans-equatorial loop system that connects an active region in the southern hemisphere to a bipolar region of plage in the northern hemisphere. Conclusions. We have identified polarised, short-lived solar radio bursts that have never been imaged before. They are observed at a height and frequency range where plasma emission is the dominant emission mechanism, however, they possess some of the characteristics of electron-cyclotron maser emission. C1 [Morosan, D. E.; Gallagher, P. T.; Zucca, P.; O'Flannagain, A.] Trinity Coll Dublin, Sch Phys, Dublin 2, Ireland. [Fallows, R.; Asgekar, A.; Bentum, M. J.; Brouw, W. N.; de Geus, E.; Falcke, H.; Frieswijk, W.; Garrett, M. A.; Gunst, A. W.; Hessels, J. W. T.; Kondratiev, V. I.; Kuper, G.; van Leeuwen, J.; McKean, J. P.; Munk, H.; Orru, E.; Pizzo, R.; Polatidis, A. G.; Sluman, J.; Toribio, M. C.; Vermeulen, R.] Netherlands Inst Radio Astron, ASTRON, NL-7990 AA Dwingeloo, Netherlands. [Reid, H.; MacKinnon, A. L.] Univ Glasgow, SUPA, Sch Phys & Astron, Glasgow G12 8QQ, Lanark, Scotland. [Magdalenic, J.] Royal Observ Belgium, SIDC, Solar Terr Ctr Excellence, B-1180 Brussels, Belgium. [Mann, G.; Vocks, C.; Breitling, F.] Leibniz Inst Astrophys Potsdam AIR, D-14482 Potsdam, Germany. [Bisi, M. M.] Harwell Oxford, RAE Space Sci & Technol Facil Council, Rutherford Appleton Lab, Oxford OX11 OQX, Oxon, England. [Kerdraon, A.; Tasse, C.; Zarka, P.] Observ Paris, LESIA, UMR 8109, CNRS, F-92195 Meudon, France. [Konovalenko, A. A.] Inst Radio Astron, UA-61002 Kharkov, Ukraine. [Rucker, H. O.] Austrian Acad Sci, Commiss Astron, A-8042 Graz, Austria. [Thide, B.] Swedish Inst Space Phys, S-75121 Uppsala, Sweden. [Alexov, A.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Anderson, J.] Hehnholtz Zentrum Potsdam, DeutschesGeoForschunesZentrum GFZ, Dept Geodesy & Remote Sensing 1, D-14473 Potsdam, Germany. [Asgekar, A.] Shell Technol Ctr, Bangalore 560099, Karnataka, India. [Avruch, I. M.] SRON Netherlands Inst Space Res, NL-9700 AV Groningen, Netherlands. [Avruch, I. M.; Brouw, W. N.; McKean, J. P.] Univ Groningen, Kapteyn Astron Inst, NL-9700 AV Groningen, Netherlands. [Bentum, M. J.] Univ Twente, NL-7522 NB Enxhede, Netherlands. [Bernardi, G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Bonafede, A.] Univ Hamburg, D-21029 Hamburg, Germany. [Broderick, J. W.; Karastergiou, A.] Univ Oxford, Astrophys, Oxford OX1 3RH, England. [Broderick, J. W.; Scaife, A. M. M.] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England. [Butcher, H. R.] Australian Natl Univ, Res Sch Astron & Astrophys, Mt Stromlo Obs, Weston, ACT 2611, Australia. [Ciardi, B.] Max Planck Inst Astrophys, D-85741 Garching, Germany. [de Geus, E.] SmarterVision BV, NL-9401 JX Assen, Netherlands. [Eisloeffel, J.; Hoeft, M.] Thnringer Landessternwarte, D-07778 Tautenburg, Germany. [Falcke, H.] Radboud Univ Nijmegen, Dept Astrophys IMAPP, NL-6500 GL Nijmegen, Netherlands. [Garrett, M. A.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [Griessmeier, J.] Univ Orleans, CNRS, LPC2E, F-45071 Orleans 2, France. [Griessmeier, J.] Univ Orleans, Stn Radioastron Nancay, Observ Paris, CNRS,INSU,USR 704,OSUC, F-18330 Nancay, France. [Hessels, J. W. T.; van Leeuwen, J.] Univ Amsterdam, Anton Pannekoek Inst, NL-1090 GE Amsterdam, Netherlands. [Kondratiev, V. I.] PN Lebedev Phys Inst, Ctr Astro Space, Moscow 117997, Russia. [McKay-Bukowski, D.] Univ Oulu, Sodankyla Geophys Observ, Sodankyla 99600, Finland. [McKay-Bukowski, D.] STFC Rutherford Appleton Lab, Didcot OX11 0QX, Oxon, England. [Paas, H.] Univ Groningen, CIT, NL-9700 CA Groningen, Netherlands. RP Morosan, DE (reprint author), Trinity Coll Dublin, Sch Phys, Dublin 2, Ireland. EM morosand@tcd.ie RI Ciardi, Benedetta/N-7625-2015; Gallagher, Peter/C-7717-2011; Kondratiev, Vladislav/N-1105-2015 OI Gallagher, Peter/0000-0001-9745-0400; Kondratiev, Vladislav/0000-0001-8864-7471 FU Government of Ireland studentship from the Irish Research Council (IRC); Non-Foundation Scholarship; Trinity College Dublin; Innovation Academy; IRC New Foundations; SUPA Advanced Fellowship; STFC [ST/L000741/1] FX This work has been supported by a Government of Ireland studentship from the Irish Research Council (IRC), the Non-Foundation Scholarship awarded by Trinity College Dublin, the Innovation Academy and the IRC New Foundations. Hamish Reid is supported by a SUPA Advanced Fellowship and an STFC grant ST/L000741/1. We would finally like to acknowledge the LOFAR telescope. LOFAR, the LOw Frequency ARray designed and constructed by ASTRON, has facilities in several countries, that are owned by various parties (each with their own funding sources), and that are collectively operated by the International LOFAR Telescope (ILT) foundation under a joint scientific policy. NR 29 TC 3 Z9 3 U1 1 U2 7 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 AUG PY 2015 VL 580 AR A65 DI 10.1051/0004-6361/201526064 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CP6TD UT WOS:000360020200065 ER PT J AU Pinilla, P Birnstiel, T Walsh, C AF Pinilla, P. Birnstiel, T. Walsh, C. TI Sequential planet formation in the HD 100546 protoplanetary disk? SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE protoplanetary disks; circumstellar matter; planet-disk interactions ID TRANSITIONAL DISKS; DUST GRAINS; CIRCUMSTELLAR DISK; EMBEDDED PLANETS; GIANT PLANETS; SOLAR NEBULA; HERBIG AE/BE; SAO 206462; GAP EDGES; COMPANION AB Context. The disk around the Herbig Ae star, HD 100546, shows structures that suggest the presence of two companions in the disk at similar to 10 and similar to 70 AU. The outer companion seems to be in the act of formation. Aims. Our aims are to provide constraints on the age of the planets in HD 100546 and to explore the potential evidence for sequential planet formation in transition disks such as HD 100546. Methods. We compare the recent resolved continuum observations of the disk around HD 100546 with the results of dust evolution simulations using an analytical prescription for the shapes of gaps carved by massive planets. Results. An inner pressure bump must have been present since early in the disk lifetime to have good agreement between the dust evolution models and the continuum observations of HD 100546. This pressure bump may have resulted from the presence of a very massive planet (similar to 20 M-Jup), which formed early in the inner disk (r similar to 10 AU). If only this single planet exists, the disk is likely to be old, comparable to the stellar age (similar to 5-10 Myr). Another possible explanation is an additional massive planet in the outer disk (r similar to 70 AU): either a low- mass outer planet (less than or similar to 5 M-Jup) injected at early times, or a higher mass outer planet (greater than or similar to 15 M-Jup) formed very recently, traps the right amount of dust in pressure bumps to reproduce the observations. In the latter case, the disk could be much younger (similar to 3.0 Myr). Conclusions. In the case in which two massive companions are embedded in the disk around HD 100546, as suggested in the literature, the outer companion could be at least greater than or similar to 2.5 Myr younger than the inner companion. C1 [Pinilla, P.; Walsh, C.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [Birnstiel, T.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Pinilla, P (reprint author), Leiden Univ, Leiden Observ, POB 9513, NL-2300 RA Leiden, Netherlands. EM pinilla@strw.leidenuniv.nl OI Birnstiel, Tilman/0000-0002-1899-8783 FU Koninklijke Nederlandse Akademie van Wetenschappen (KNAW) professor prize; NASA Origins of Solar Systems grant [NNX12AJ04G]; Netherlands Organisation for Scientific Research (NWO) [639.041.335]; Netherlands Research School for Astronomy (NOVA); Royal Netherlands Academy of Arts and Sciences (KNAW) professor prize; European Union A-ERC grant [291141 CHEMPLAN] FX The authors are very grateful to E. F. van Dishoeck and D. Harsono for all their comments and fruitful discussions. We thank to S. Bruderer for providing his data for the disk temperature and C. Wright for the ATCA data. P. P. is supported by Koninklijke Nederlandse Akademie van Wetenschappen (KNAW) professor prize to Ewine van Dishoeck. T.B. acknowledges support from NASA Origins of Solar Systems grant NNX12AJ04G. C.W. acknowledges support from the Netherlands Organisation for Scientific Research (NWO, grant number 639.041.335). Astrochemistry in Leiden is supported by the Netherlands Research School for Astronomy (NOVA), by a Royal Netherlands Academy of Arts and Sciences (KNAW) professor prize, and by the European Union A-ERC grant 291141 CHEMPLAN. This paper makes use of the following ALMA data: ADS/JAO.ALMA#2011.0.00863.S. ALMA is a partnership of ESO (representing its member states), NSF (USA) and NINS (Japan), together with NRC (Canada) and NSC and ASIAA (Taiwan), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by ESO, AUI/NRAO and NAOJ. NR 75 TC 4 Z9 4 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 EI 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD AUG PY 2015 VL 580 AR A105 DI 10.1051/0004-6361/201425539 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CP6TD UT WOS:000360020200105 ER PT J AU Santos, NC Adibekyan, V Mordasini, C Benz, W Delgado-Mena, E Dorn, C Buchhave, L Figueira, P Mortier, A Pepe, F Santerne, A Sousa, SG Udry, S AF Santos, N. C. Adibekyan, V. Mordasini, C. Benz, W. Delgado-Mena, E. Dorn, C. Buchhave, L. Figueira, P. Mortier, A. Pepe, F. Santerne, A. Sousa, S. G. Udry, S. TI Constraining planet structure from stellar chemistry: the cases of CoRoT-7, Kepler-10, and Kepler-93 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE planetary systems; planets and satellites: detection; stars: abundances; techniques: spectroscopic ID MASS-RADIUS RELATIONSHIPS; 100 EARTH MASSES; COMPOSITIONAL DIVERSITY; CHEMICAL-COMPOSITION; TERRESTRIAL PLANETS; GIANT PLANETS; ROCKY PLANET; STARS; METALLICITY; ABUNDANCES AB Aims. We explore the possibility that the stellar relative abundances of different species can be used to constrain the bulk abundances of known transiting rocky planets. Methods. We use high resolution spectra to derive stellar parameters and chemical abundances for Fe, Si, Mg, O, and C in three stars hosting low mass, rocky planets: CoRoT-7, Kepler-10, and Kepler-93. These planets follow the same line along the mass-radius diagram, pointing toward a similar composition. The derived abundance ratios are compared with the solar values. With a simple stoichiometric model, we estimate the iron mass fraction in each planet, assuming stellar composition. Results. We show that in all cases, the iron mass fraction inferred from the mass-radius relationship seems to be in good agreement with the iron abundance derived from the host star's photospheric composition. Conclusions. The results suggest that stellar abundances can be used to add constraints on the composition of orbiting rocky planets. C1 [Santos, N. C.; Adibekyan, V.; Delgado-Mena, E.; Figueira, P.; Santerne, A.; Sousa, S. G.] Univ Porto, CAUP, Inst Astrofis & Ciencias Espaco, P-4150762 Oporto, Portugal. [Santos, N. C.] Univ Porto, Fac Ciencias, Dept Fis & Astron, P-4169007 Oporto, Portugal. [Mordasini, C.; Benz, W.; Dorn, C.] Univ Bern, Inst Phys, CH-3012 Bern, Switzerland. [Buchhave, L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Buchhave, L.] Univ Copenhagen, Nat Hist Museum Denmark, Ctr Star & Planet Format, DK-1350 Copenhagen, Denmark. [Mortier, A.] Univ St Andrews, Sch Phys & Astron, SUPA, St Andrews KY16 9SS, Fife, Scotland. [Pepe, F.; Udry, S.] Univ Geneva, Observ Geneva, CH-1290 Sauverny, Switzerland. RP Santos, NC (reprint author), Univ Porto, CAUP, Inst Astrofis & Ciencias Espaco, Rua Estrelas, P-4150762 Oporto, Portugal. EM nuno@astro.up.pt RI Delgado Mena, Elisa/M-9178-2013; dorn, caroline/R-1864-2016; Figueira, Pedro/J-4916-2013; Adibekyan, Vardan/I-5026-2013; OI Delgado Mena, Elisa/0000-0003-4434-2195; Figueira, Pedro/0000-0001-8504-283X; Adibekyan, Vardan/0000-0002-0601-6199; Santerne, Alexandre/0000-0002-3586-1316; Buchhave, Lars A./0000-0003-1605-5666 FU Fundacao para a Ciencia e a Tecnologia (FCT) [UID/FIS/04434/2013]; FCT through Investigador FCT by FEDER through the program "Programa Operacional de Factores de Competitividade - COMPETE" [IF/01037/201, IF/00169/2012, IF/00028/2014]; FCT through POPH/FSE (EC) by FEDER through the program "Programa Operacional de Factores de Competitividade - COMPETE"; FCT [IF/01037/2013CP1191/CT0001, SFRH/BPD/76606/2011, SFRH/BPD/70574/2010]; EU under a Marie Curie Intra-European Fellowship for Career Development [627202]; Swiss National Science Foundation [BSSGI0_155816]; European Union Seventh Framework Program (FP7) [313014] FX We would like to thank the anonymous referee for the useful comments and suggestions. This work was supported by Fundacao para a Ciencia e a Tecnologia (FCT) through the research grant UID/FIS/04434/2013. P.F., N.C.S., and S.G.S. also acknowledge support from FCT through Investigador FCT contracts of reference IF/01037/2013, IF/00169/2012, and IF/00028/2014, and POPH/FSE (EC) by FEDER funding through the program "Programa Operacional de Factores de Competitividade - COMPETE". P.F. acknowledges support from FCT in the form of project reference IF/01037/2013CP1191/CT0001. A.S. is supported by the EU under a Marie Curie Intra-European Fellowship for Career Development with reference FP7-PEOPLE-2013-IEF, number 627202. E.D.M. and V.A. acknowledge the support from FCT in form of the grants SFRH/BPD/76606/2011 and SFRH/BPD/70574/2010. This work results within the collaboration of the COST Action TD 1308. C.M. acknowledges the support from the Swiss National Science Foundation under grant BSSGI0_155816. A.M. received funding from the European Union Seventh Framework Program (FP7/2007-2013) under grant agreement number 313014 (ETAEARTH). NR 48 TC 14 Z9 14 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 EI 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD AUG PY 2015 VL 580 AR L13 DI 10.1051/0004-6361/201526850 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CP6TD UT WOS:000360020200158 ER PT J AU Heer, K Helbig-Bonitz, M Fernandes, RG Mello, MAR Kalko, EKV AF Heer, Katrin Helbig-Bonitz, Maria Fernandes, Renato G. Mello, Marco A. R. Kalko, Elisabeth K. V. TI Effects of land use on bat diversity in a complex plantation-forest landscape in northeastern Brazil SO JOURNAL OF MAMMALOGY LA English DT Article DE acoustic monitoring; Atlantic Forest; fragmentation; land use; matrix habitat; mist netting ID AERIAL INSECTIVOROUS BATS; TROPICAL RAIN-FOREST; ATLANTIC FOREST; PHYLLOSTOMID BATS; SPECIES-DIVERSITY; LEVEL RESPONSES; STURNIRA-LILIUM; BRIDGE ISLANDS; FRAGMENT SIZE; EATING BATS AB In fragmented areas, the persistence of different species depends on their ability to use the surrounding matrix either as a corridor or as a foraging habitat. We assessed how species richness and abundance of Neotropical bats differ among forest fragments and rubber plantations under different management regimes. Our study site was located in a heterogeneous agricultural area in the Atlantic Forest of Bahia, northeastern Brazil. By combining mist netting and acoustic monitoring as complementary techniques, we caught 28 phyllostomid species and recorded 21 aerial insectivorous species, which either forage in open space or close to forests. Open space species were equally abundant and diverse in all land use types. In contrast, assemblages of phyllostomid and aerial insectivorous forest species differed significantly among habitats, with the highest species richness recorded in forest fragments. We identified a number of forest specialists in forest fragments, which indicates a relatively intact bat fauna. In intensively used rubber-cacao plantation, we found surprisingly high bat abundance and diversity, despite the shortage of resources for bats. Our results also indicate that patches of secondary vegetation around rubber plantations are important landscape features for bats and might contribute to the persistence of highly diverse bat assemblages. We suggest that bats do not perceive plantations as a hostile matrix, but probably use them as corridors between forest fragments and patches of secondary vegetation. C1 [Heer, Katrin; Helbig-Bonitz, Maria; Mello, Marco A. R.; Kalko, Elisabeth K. V.] Univ Ulm, Inst Expt Ecol, D-89069 Ulm, Germany. [Heer, Katrin] Univ Marburg, Conservat Biol, D-35043 Marburg, Germany. [Heer, Katrin] Univ Marburg, Dept Ecol, D-35043 Marburg, Germany. [Fernandes, Renato G.] Univ Fed Mato Grosso, Ctr Ciencias Biol Saude, Dept Biol, BR-79070900 Campo Grande, MS, Brazil. [Mello, Marco A. R.] Univ Fed Minas Gerais, Inst Ciencias Biol, Dept Biol Geral, BR-31270901 Belo Horizonte, MG, Brazil. [Kalko, Elisabeth K. V.] Smithsonian Trop Res Inst, Balboa, Panama. RP Heer, K (reprint author), Univ Ulm, Inst Expt Ecol, Albert Einstein Allee 11, D-89069 Ulm, Germany. EM katrin.heer@uni-marburg.de; maria.helbig@uni-ulm.de RI Mello, Marco/B-1095-2008 OI Mello, Marco/0000-0002-9098-9427 FU German National Academic Foundation; Ulm University; Humboldt Foundation (AvH) [1134644]; Sao Paulo Research Foundation (FAPESP) [06/00265-0, 05/00587-5, 07/50633-9]; Federal University of Minas Gerais (UFMG) [PRPq 01/2013, 14/2013, 02/2014]; Minas Gerais Research Foundation (FAPEMIG) [APQ-01043-13]; Brazilian Research Council (CNPq) [472372/2013-0]; Research Program on Atlantic Forest Biodiversity (PPBio-MA/CNPq); Ecotone Inc. ("Do Science and Get Support Program"); Center for Biodiversity Studies of the Michelin Ecological Reserve FX We thank M. Tschapka, K. M. Flesher, K. Jung, J. Dolezil, S. C. Renner, M. Knornschild, L. Opgenoorth, and R. Brandl for their help with data analysis and for commenting on earlier versions of the manuscript. KH was financed by the German National Academic Foundation. MARM was sponsored by Ulm University, Humboldt Foundation (AvH, 1134644), Sao Paulo Research Foundation (FAPESP, 06/00265-0, 05/00587-5; 07/50633-9), Federal University of Minas Gerais (UFMG, PRPq 01/2013, 14/2013, 02/2014), Minas Gerais Research Foundation (FAPEMIG, APQ-01043-13), Brazilian Research Council (CNPq, 472372/2013-0), Research Program on Atlantic Forest Biodiversity (PPBio-MA/CNPq), and Ecotone Inc. ("Do Science and Get Support Program"). The research permit was given by the Chico Mendes Institute for Biodiversity (SISBIO 19053-1). Logistical and financial support in Brazil was provided by the Center for Biodiversity Studies of the Michelin Ecological Reserve. NR 73 TC 3 Z9 3 U1 3 U2 47 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 AUG PY 2015 VL 96 IS 4 BP 720 EP 731 DI 10.1093/jmammal/gyv068 PG 12 WC Zoology SC Zoology GA CQ4NW UT WOS:000360582700010 ER PT J AU Quiroga-Carmona, M Woodman, N AF Quiroga-Carmona, Marcial Woodman, Neal TI A new species of Cryptotis (Mammalia, Eulipotyphla, Soricidae) from the Sierra de Perija, Venezuelan-Colombian Andes SO JOURNAL OF MAMMALOGY LA English DT Article DE Blarinini; Cryptotis thomasi species group; neotropical shrews; Soricinae; Soricomorpha; South America ID SMALL-EARED SHREW; GENUS CRYPTOTIS; SORICOMORPHA SORICIDAE AB The Sierra de Perija is the northern extension of the Cordillera Oriental of the Andes and includes part of the border between Colombia and Venezuela. The population of small-eared shrews (Mammalia, Eulipotyphla, Soricidae, Cryptotis) inhabiting the Sierra de Perija previously was known from only a single skull from an individual collected in Colombia in 1989. This specimen had been referred to alternatively as C. thomasi and C. meridensis, but a more precise definition of the known Colombian and Venezuelan species of Cryptotis has since excluded the Sierra de Perija population from any named species. The recent collection of a specimen from the Venezuelan slope of Sierra de Perija prompted us to re-evaluate the taxonomic status of this population and determine its relationship with other Andean shrews. Our examination of the available specimens revealed that they possess a unique suite of morphological and morphometrical characters, and we describe the Sierra de Perija population as a new species in the predominantly South American C. thomasi species group. Recognition of this new species adds to our knowledge of this genus in South America and to the biodiversity of the Sierra de Perija. C1 [Quiroga-Carmona, Marcial] Univ Carabobo, Fac Expt Ciencias & Tecnol, Dept Biol, Valencia 2005, Venezuela. [Quiroga-Carmona, Marcial] Inst Venezolano Invest Cient, Ctr Ecol, Caracas 1020A, Venezuela. [Woodman, Neal] Smithsonian Inst, US Geol Survey, Patuxent Wildlife Res Ctr, Natl Museum Nat Hist, Washington, DC 20013 USA. RP Quiroga-Carmona, M (reprint author), Univ Carabobo, Fac Expt Ciencias & Tecnol, Dept Biol, Valencia 2005, Venezuela. EM marcialquiroga@gmail.com OI Woodman, Neal/0000-0003-2689-7373 FU Fundacion Provita through Iniciativa de Especies Amenazadas (IEA) FX We thank the Fundacion Provita for partial sponsorship of this work through Iniciativa de Especies Amenazadas (IEA). We thank the following curators and collections managers for loans or for permission to examine specimens under their care: R. Voss (AMNH); P. Jenkins, L. Tomsett, and R. Portela-Miguez (BMNH); P. Soriano and J. Murillo (CVULA); F. Bisbal and J. Sanchez (EBRG); L. R. Heaney, B. D. Patterson, J. Phelps, and W. T. Stanley (FMNH); A. Cadena and H. Lopez-Arevalo (ICN); R. M. Timm (KU); R. Calchi and D. Prieto (MBLUZ); C. Ferreira and M. Salazar (MBUCV); J. M. Chupasko and M. Omura (MCZ); A. Ferrer (MHNLS); G. Pothet, M. Tranier, and C. Denys, Museum National d'HistoireNaturelle, Paris (MNHN); C. Cuartas-Calles and C. Delgado-V. (MUA); J. Eger and B. Lim (ROM). Special thanks to F. Rojas-Runjaic (MHNLS) for providing the paratype specimen (and its photographs), and J. Molinari for allowing work in his laboratory during this research. G. D'Elia and R. D. Fischer provided valuable comments on previous versions of this manuscript. Any use of trade, product, or firm names is for descriptive purposes only and does not imply endorsement by the United States government. NR 37 TC 4 Z9 4 U1 1 U2 2 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 AUG PY 2015 VL 96 IS 4 BP 800 EP 809 DI 10.1093/jmammal/gyv085 PG 10 WC Zoology SC Zoology GA CQ4NW UT WOS:000360582700017 ER PT J AU Salvador-Reyes, LA Sneed, J Paul, VJ Luesch, H AF Salvador-Reyes, Lilibeth A. Sneed, Jennifer Paul, Valerie J. Luesch, Hendrik TI Amantelides A and B, Polyhydroxylated Macrolides with Differential Broad-Spectrum Cytotoxicity from a Guamanian Marine Cyanobacteriurn SO JOURNAL OF NATURAL PRODUCTS LA English DT Article ID STEREOCHEMISTRY; MACROLACTONE; AMPHIDINOLS; METABOLITE; TOLYTOXIN AB Cytotoxicity-guided fractionation of a Guamanian cyanobacterial collection yielded the new compounds amantelides A (1) and B (2). These polyketides are characterized by a 40-membered macrolactone ring consisting of a 1,3-diol and contiguous 1,5-diol units and a tert-butyl substituent. Amantelide A (1) displayed potent cytotoxicity with submicromolar IC50 against HT29 colorectal adenocarcinoma and He La cervical carcinoma cell lines. Acetylation of the hydroxy group at C-33 in 2 caused a close to 10-fold decrease in potency. Exhaustive acetylation of the hydroxy groups abrogated the antiproliferative activity of amantelide A (1) by 20-67-fold. Further bioactivity assessment of 1 against bacterial pathogens and marine fungi indicated a broad spectrum of bioactivity. C1 [Salvador-Reyes, Lilibeth A.; Luesch, Hendrik] Univ Florida, Dept Med Chem, Gainesville, FL 32610 USA. [Luesch, Hendrik] Univ Florida, Ctr Nat Prod, Drug Discovery & Dev CNPD3, Gainesville, FL 32610 USA. [Salvador-Reyes, Lilibeth A.] Univ Philippines, Inst Marine Sci, UP Diliman, Quezon City 1101, Philippines. [Sneed, Jennifer; Paul, Valerie J.] Smithsonian Marine Stn, Ft Pierce, FL 34949 USA. RP Luesch, H (reprint author), Univ Florida, Dept Med Chem, 1345 Ctr Dr, Gainesville, FL 32610 USA. EM luesch@cop.ufl.edu FU National Institutes of Health; NIGMS [P41GM086210]; NCI [R01CA172310]; University of the Philippines Office of the Vice Chancellor for Research and Development; UP Balik Ph.D. program FX This research was supported by the National Institutes of Health, NIGMS grant P41GM086210, and NCI grant R01CA172310. L.A.S.R acknowledges funding support from the University of the Philippines Office of the Vice Chancellor for Research and Development and the UP Balik Ph.D. program. We are grateful to N. Engene for taxonomic assessment of the cyanobacterium and R. Ratnayake for acquiring the NOE spectra. This is contribution #1000 from the Smithsonian Marine Station at Fort Pierce. NR 20 TC 5 Z9 5 U1 2 U2 14 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0163-3864 EI 1520-6025 J9 J NAT PROD JI J. Nat. Prod. PD AUG PY 2015 VL 78 IS 8 BP 1957 EP 1962 DI 10.1021/acs.jnatprod.5b00293 PG 6 WC Plant Sciences; Chemistry, Medicinal; Pharmacology & Pharmacy SC Plant Sciences; Pharmacology & Pharmacy GA CQ7HN UT WOS:000360773700019 PM 26204500 ER PT J AU Chang, AL Deck, AK Malm, PD Attoe, S Willits, K Sullivan, LJ Morgan, SG AF Chang, Andrew L. Deck, Anna K. Malm, Preston D. Attoe, Sarikka Willits, Karissa Sullivan, Lindsay J. Morgan, Steven G. TI CURRENT AND FUTURE FRESHWATER FLOW CONTROL OF OLYMPIA OYSTER POPULATION DEMOGRAPHY IN THE SAN FRANCISCO ESTUARY SO JOURNAL OF SHELLFISH RESEARCH LA English DT Meeting Abstract C1 [Chang, Andrew L.] Smithsonian Environm Res Ctr, Tiburon, CA 94920 USA. [Deck, Anna K.; Malm, Preston D.; Attoe, Sarikka; Willits, Karissa; Morgan, Steven G.] Univ Calif Davis, Bodega Marine Lab, Bodega Bay, CA 94923 USA. [Deck, Anna K.] San Francisco Bay Natl Estuarine Res Reserve, Tiburon, CA 94920 USA. [Sullivan, Lindsay J.] San Francisco State Univ, Romberg Tiburon Ctr, Tiburon, CA 94920 USA. RI Chang, Andrew/J-8058-2016 OI Chang, Andrew/0000-0002-7870-285X NR 0 TC 0 Z9 0 U1 0 U2 4 PU NATL SHELLFISHERIES ASSOC PI GROTON PA C/O DR. SANDRA E. SHUMWAY, UNIV CONNECTICUT, 1080 SHENNECOSSETT RD, GROTON, CT 06340 USA SN 0730-8000 EI 1943-6319 J9 J SHELLFISH RES JI J. Shellfish Res. PD AUG PY 2015 VL 34 IS 2 BP 618 EP 618 PG 1 WC Fisheries; Marine & Freshwater Biology SC Fisheries; Marine & Freshwater Biology GA CQ2DV UT WOS:000360410500089 ER PT J AU Grosholz, ED Bible, J Ceballos, E Chang, AL Cheng, BS Deck, A Ferner, M Latta, M Wasson, K Zabin, C AF Grosholz, E. D. Bible, J. Ceballos, E. Chang, A. L. Cheng, B. S. Deck, A. Ferner, M. Latta, M. Wasson, K. Zabin, C. TI UNDERSTANDING ENVIRONMENTAL CONDITIONS THAT SUPPORT SUSTAINABLE OLYMPIA OYSTER POPULATIONS: INFORMING RESTORATION AND CONSERVATION SO JOURNAL OF SHELLFISH RESEARCH LA English DT Meeting Abstract C1 [Grosholz, E. D.; Zabin, C.] Univ Calif Davis, Dept Environm Sci & Policy MORE, Davis, CA USA. [Bible, J.; Cheng, B. S.] Univ Calif Davis, Bodega Marine Lab, MORE, Davis, CA USA. [Ceballos, E.; Chang, A. L.; Zabin, C.] Smithsonian Environm Res Ctr, Tiburon, CA USA. [Deck, A.; Ferner, M.] San Francisco Bay Natl Estuarine Res Reserve, Tiburon, CA USA. [Latta, M.] Calif State Coastal Conservancy, Oakland, CA USA. [Wasson, K.] Elkhorn Slough Natl Estuarine Res Reserve, Watsonville, CA USA. RI Chang, Andrew/J-8058-2016 OI Chang, Andrew/0000-0002-7870-285X NR 0 TC 0 Z9 0 U1 1 U2 5 PU NATL SHELLFISHERIES ASSOC PI GROTON PA C/O DR. SANDRA E. SHUMWAY, UNIV CONNECTICUT, 1080 SHENNECOSSETT RD, GROTON, CT 06340 USA SN 0730-8000 EI 1943-6319 J9 J SHELLFISH RES JI J. Shellfish Res. PD AUG PY 2015 VL 34 IS 2 BP 637 EP 637 PG 1 WC Fisheries; Marine & Freshwater Biology SC Fisheries; Marine & Freshwater Biology GA CQ2DV UT WOS:000360410500144 ER PT J AU Kiriakopolos, SL Zabin, CJ Martin, L Obernolte, R Abbott, R Grosholz, ED AF Kiriakopolos, Stephanie L. Zabin, Chela J. Martin, Lara Obernolte, Rena Abbott, Robert Grosholz, Edwin D. TI VARIATION IN NATIVE OYSTER (OSTREA LURIDA) PERFORMANCE BETWEEN AND WITHIN TWO RESTORATION SITES IN SAN FRANCISCO BAY SO JOURNAL OF SHELLFISH RESEARCH LA English DT Meeting Abstract C1 [Kiriakopolos, Stephanie L.; Zabin, Chela J.; Martin, Lara; Grosholz, Edwin D.] Univ Calif Davis, Davis, CA 95616 USA. [Kiriakopolos, Stephanie L.] San Francisco State Univ, Romberg Tiburon Ctr, Tiburon, CA 94920 USA. [Zabin, Chela J.] Smithsonian Environm Res Ctr, Romberg Tiburon Ctr, Tiburon, CA 94920 USA. [Martin, Lara] San Francisco Bay Natl Estuarine Res Reserve, Romberg Tiburon Ctr, Tiburon, CA 94920 USA. [Obernolte, Rena] Isla Arena Consulting, Emeryville, CA USA. [Abbott, Robert] ENVIRON, San Francisco, CA 94111 USA. NR 0 TC 0 Z9 0 U1 2 U2 3 PU NATL SHELLFISHERIES ASSOC PI GROTON PA C/O DR. SANDRA E. SHUMWAY, UNIV CONNECTICUT, 1080 SHENNECOSSETT RD, GROTON, CT 06340 USA SN 0730-8000 EI 1943-6319 J9 J SHELLFISH RES JI J. Shellfish Res. PD AUG PY 2015 VL 34 IS 2 BP 648 EP 648 PG 1 WC Fisheries; Marine & Freshwater Biology SC Fisheries; Marine & Freshwater Biology GA CQ2DV UT WOS:000360410500177 ER PT J AU Wasson, K Chang, AL Deck, A Dinnel, P Dudas, S Ferner, M Grosholz, T Ruesink, J Trimble, A Schaaf, DV Zabin, C Zacherl, D AF Wasson, Kerstin Chang, Andrew L. Deck, Anna Dinnel, Paul Dudas, Sarah Ferner, Matthew Grosholz, Ted Ruesink, Jennifer Trimble, Alan Schaaf, Dick Vander Zabin, Chela Zacherl, Danielle TI VARIANCE IN RECRUITMENT OF OLYMPIA OYSTERS ACROSS WEST COAST ESTUARIES SO JOURNAL OF SHELLFISH RESEARCH LA English DT Meeting Abstract C1 [Wasson, Kerstin] Elkhorn Slough Natl Estuarine Res Reserve, Watsonville, CA 95076 USA. [Chang, Andrew L.; Zabin, Chela] Smithsonian Environm Res Ctr, Tiburon, CA 94920 USA. [Deck, Anna; Ferner, Matthew] San Francisco Bay Natl Estuarine Res Reserve, Tiburon, CA 94920 USA. [Dinnel, Paul] Skagit Cty Marine Resources Comm, Mt Vernon, WA 98273 USA. [Dudas, Sarah] Ctr Shellfish Res, Nanaimo, BC V9R 5S5, Canada. [Grosholz, Ted; Zabin, Chela] Univ Calif Davis, Dept Environm Sci & Policy, Davis, CA 95616 USA. [Ruesink, Jennifer; Trimble, Alan] Univ Washington, Seattle, WA 98195 USA. [Schaaf, Dick Vander] Nat Conservancy Oregon, Portland, OR 97214 USA. [Zacherl, Danielle] Calif State Univ Fullerton, Fullerton, CA 92831 USA. RI Chang, Andrew/J-8058-2016 OI Chang, Andrew/0000-0002-7870-285X NR 0 TC 0 Z9 0 U1 0 U2 3 PU NATL SHELLFISHERIES ASSOC PI GROTON PA C/O DR. SANDRA E. SHUMWAY, UNIV CONNECTICUT, 1080 SHENNECOSSETT RD, GROTON, CT 06340 USA SN 0730-8000 EI 1943-6319 J9 J SHELLFISH RES JI J. Shellfish Res. PD AUG PY 2015 VL 34 IS 2 BP 689 EP 689 PG 1 WC Fisheries; Marine & Freshwater Biology SC Fisheries; Marine & Freshwater Biology GA CQ2DV UT WOS:000360410500296 ER PT J AU Zabin, C Wasson, K Fork, S AF Zabin, Chela Wasson, Kerstin Fork, Susanne TI RESTORATION OF NATIVE OYSTERS IN A HIGHLY INVADED ESTUARY SO JOURNAL OF SHELLFISH RESEARCH LA English DT Meeting Abstract C1 [Zabin, Chela] Univ Calif Davis, Smithsonian Environm Res Ctr, Tiburon, CA 94920 USA. [Zabin, Chela] Univ Calif Davis, Environm Sci & Policy Dept, Tiburon, CA 94920 USA. [Wasson, Kerstin; Fork, Susanne] Elkhorn Slough Natl Estuarine Res Reserve, Watsonville, CA 95039 USA. NR 0 TC 0 Z9 0 U1 0 U2 2 PU NATL SHELLFISHERIES ASSOC PI GROTON PA C/O DR. SANDRA E. SHUMWAY, UNIV CONNECTICUT, 1080 SHENNECOSSETT RD, GROTON, CT 06340 USA SN 0730-8000 EI 1943-6319 J9 J SHELLFISH RES JI J. Shellfish Res. PD AUG PY 2015 VL 34 IS 2 BP 694 EP 694 PG 1 WC Fisheries; Marine & Freshwater Biology SC Fisheries; Marine & Freshwater Biology GA CQ2DV UT WOS:000360410500309 ER PT J AU Loh, TL Jaafar, Z AF Loh, Tse-Lynn Jaafar, Zeehan TI Turning the tide on bottom trawling SO AQUATIC CONSERVATION-MARINE AND FRESHWATER ECOSYSTEMS LA English DT Editorial Material C1 [Loh, Tse-Lynn] John G Shedd Aquarium, Daniel P Haerther Ctr Conservat & Res, Chicago, IL 60605 USA. [Jaafar, Zeehan] Smithsonian Inst, Natl Museum Nat Hist, Div Fishes, Washington, DC 20560 USA. [Jaafar, Zeehan] Natl Univ Singapore, Dept Biol Sci, Singapore 117548, Singapore. RP Loh, TL (reprint author), John G Shedd Aquarium, Daniel P Haerther Ctr Conservat & Res, 1200 South Lake Shore Dr, Chicago, IL 60605 USA. EM tloh@sheddaquarium.org OI Loh, Tse-Lynn/0000-0003-1360-1991 NR 4 TC 1 Z9 1 U1 1 U2 4 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1052-7613 EI 1099-0755 J9 AQUAT CONSERV JI Aquat. Conserv.-Mar. Freshw. Ecosyst. PD AUG PY 2015 VL 25 IS 4 BP 581 EP 583 DI 10.1002/aqc.2563 PG 3 WC Environmental Sciences; Marine & Freshwater Biology; Water Resources SC Environmental Sciences & Ecology; Marine & Freshwater Biology; Water Resources GA CQ2QC UT WOS:000360445100010 ER PT J AU Ceron-Souza, I Gonzalez, EG Schwarzbach, AE Salas-Leiva, DE Rivera-Ocasio, E Toro-Perea, N Bermingham, E McMillan, WO AF Ceron-Souza, Ivania Gonzalez, Elena G. Schwarzbach, Andrea E. Salas-Leiva, Dayana E. Rivera-Ocasio, Elsie Toro-Perea, Nelson Bermingham, Eldredge Owen McMillan, W. TI Contrasting demographic history and gene flow patterns of two mangrove species on either side of the Central American Isthmus SO ECOLOGY AND EVOLUTION LA English DT Article DE Avicennia germinans; bottleneck; climate change; comparative phylogeography; gene flow; last glacial maximum; mangroves; Neotropics; population genetic structure; Rhizophora mangle ID MULTILOCUS GENOTYPE DATA; SEA-LEVEL RISE; GULF-OF-MEXICO; MAXIMUM-LIKELIHOOD-ESTIMATION; RHIZOPHORA-MANGLE; TROPICAL ATLANTIC; CHILLING TEMPERATURES; POPULATION EXPANSION; COALESCENT APPROACH; COMPUTER-PROGRAM AB Comparative phylogeography offers a unique opportunity to understand the interplay between past environmental events and life-history traits on diversification of unrelated but co-distributed species. Here, we examined the effects of the quaternary climate fluctuations and palaeomarine currents and present-day marine currents on the extant patterns of genetic diversity in the two most conspicuous mangrove species of the Neotropics. The black (Avicennia germinans, Avicenniaceae) and the red (Rhizophora mangle, Rhizophoraceae) mangroves have similar geographic ranges but are very distantly related and show striking differences on their life-history traits. We sampled 18 Atlantic and 26 Pacific locations for A.germinans (N=292) and R.mangle (N=422). We performed coalescence simulations using microsatellite diversity to test for evidence of population change associated with quaternary climate fluctuations. In addition, we examined whether patterns of genetic variation were consistent with the directions of major marine (historical and present day) currents in the region. Our demographic analysis was grounded within a phylogeographic framework provided by the sequence analysis of two chloroplasts and one flanking microsatellite region in a subsample of individuals. The two mangrove species shared similar biogeographic histories including: (1) strong genetic breaks between Atlantic and Pacific ocean basins associated with the final closure of the Central American Isthmus (CAI), (2) evidence for simultaneous population declines between the mid-Pleistocene and early Holocene, (3) asymmetric historical migration with higher gene flow from the Atlantic to the Pacific oceans following the direction of the palaeomarine current, and (4) contemporary gene flow between West Africa and South America following the major Atlantic Ocean currents. Despite the remarkable differences in life-history traits of mangrove species, which should have had a strong influence on seed dispersal capability and, thus, population connectivity, we found that vicariant events, climate fluctuations and marine currents have shaped the distribution of genetic diversity in strikingly similar ways. C1 [Ceron-Souza, Ivania; Owen McMillan, W.] Smithsonian Trop Res Inst, Apartado 084303092, Panama. [Ceron-Souza, Ivania] Univ Puerto Rico, San Juan, PR 00931 USA. [Gonzalez, Elena G.] MNCN CSIC, Dept Biodiversidad & Biol Evolut, Madrid 28006, Spain. [Schwarzbach, Andrea E.] Univ Texas Brownsville, Dept Biomed, Brownsville, TX 78520 USA. [Salas-Leiva, Dayana E.] Florida Int Univ, Dept Biol Sci, Miami, FL 33199 USA. [Salas-Leiva, Dayana E.] USDA ARS, Natl Germplasm Repository, SHRS, Miami, FL 33158 USA. [Rivera-Ocasio, Elsie] Univ Puerto Rico Bayamon, Dept Biol, Bayamon, PR 00959 USA. [Toro-Perea, Nelson] Univ Valle, Genet Sect, Dept Biol, Cali 25360, Colombia. [Bermingham, Eldredge] Patricia & Phillip Frost Museum Sci, Miami, FL USA. RP Ceron-Souza, I (reprint author), Oregon State Univ, Dept Bot & Plant Pathol, 2082 Cordley Hall, Corvallis, OR 97331 USA. EM iviceron@gmail.com RI Gonzalez, Elena/E-4465-2013 OI Gonzalez, Elena/0000-0002-4614-3889 FU Smithsonian Tropical Research Institute (STRI); University of Puerto Rico - Rio Piedras Campus (CREST-CATEC); University of Puerto Rico - Rio Piedras Campus (NSF-EPSCor); NSF [DEB 640279]; U.S. EPA-Science to Achieve Results (STAR) program [U915985] FX This work had the financial support from the Smithsonian Tropical Research Institute (STRI), the University of Puerto Rico - Rio Piedras Campus (CREST-CATEC and NSF-EPSCor) to ICS, NSF grants (DEB 640279) to WOM, and the U.S. EPA-Science to Achieve Results (STAR) program (Grant # U915985) to ERO. NR 83 TC 2 Z9 2 U1 3 U2 29 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 2045-7758 J9 ECOL EVOL JI Ecol. Evol. PD AUG PY 2015 VL 5 IS 16 BP 3486 EP 3499 DI 10.1002/ece3.1569 PG 14 WC Ecology; Evolutionary Biology SC Environmental Sciences & Ecology; Evolutionary Biology GA CP8XD UT WOS:000360177400022 PM 26380680 ER PT J AU Mouttham, L Fortune, JE Comizzoli, P AF Mouttham, Lara Fortune, Joanne E. Comizzoli, Pierre TI Damage to fetal bovine ovarian tissue caused by cryoprotectant exposure and vitrification is mitigated during tissue culture SO JOURNAL OF ASSISTED REPRODUCTION AND GENETICS LA English DT Article; Proceedings Paper CT International Conference on Fertility Preservation - Freezing of oocytes, embryos and ovarian tissue: focus on fertility management and fertility preservation CY JAN 16-17, 2015 CL Brussels, BELGIUM SP ISFP DE Ovarian tissue; Vitrification; Primordial follicle activation; Gamete rescue; Cryopreservation ID IN-VITRO CULTURE; NEEDLE IMMERSED VITRIFICATION; SOLID-SURFACE VITRIFICATION; PRIMORDIAL FOLLICLES; PREANTRAL FOLLICLES; FOLLICULAR-GROWTH; CRYOPRESERVATION; INITIATION; TRANSPLANTATION; PRESERVATION AB The objective of this study is to characterize the impact of exposure to cryoprotectants followed by vitrification on primordial follicle survival and activation using a fetal bovine model. In the first study, fetal bovine cortical pieces were exposed to cryoprotectants with or without sucrose and cultured up to 7 days in the presence or absence of insulin. In the second study, cortical pieces were exposed to cryoprotectants with or without sucrose, vitrified, and cultured up to 7 days after warming in the presence or absence of insulin. Viability and morphology of follicles, as well as proliferation and/or DNA repair in ovarian tissue were analyzed. When compared to non-exposed controls, normal follicular morphology was affected in groups exposed to cryoprotectants only immediately post-exposure and after 1 day of culture, but improved by day 3 and did not significantly differ by day 7. Similarly, normal follicular morphology was compromised in vitrified groups after warming and on day 1 compared to controls, but improved by days 3 and 7. Proliferation and/or DNA repair in ovarian tissue was not affected by vitrification in this model. Cryoprotectant exposure and vitrification of ovarian tissue did not impair the activation of primordial follicles in response to insulin, although activation was delayed relative to non-exposed controls. Interestingly, sucrose had no noticeable protective effect. Vitrified fetal bovine ovarian tissue has the intrinsic capacity to mitigate the immediate damage to primordial follicles' morphology and retains the capacity to activate. These findings provide a basis for a successful cryopreservation protocol for ovarian cortical tissue in other species including humans. C1 [Mouttham, Lara; Comizzoli, Pierre] Natl Zool Pk, Smithsonian Conservat Biol Inst, Washington, DC 20008 USA. [Mouttham, Lara; Fortune, Joanne E.] Cornell Univ, Dept Biomed Sci, Ithaca, NY USA. RP Comizzoli, P (reprint author), Natl Zool Pk, Smithsonian Conservat Biol Inst, Washington, DC 20008 USA. EM moutthaml@si.edu; comizzolip@si.edu FU United States Department of Agriculture Multistate Project [NE-1227] FX This research was supported by the United States Department of Agriculture Multistate Project (NE-1227). NR 50 TC 1 Z9 1 U1 0 U2 6 PU SPRINGER/PLENUM PUBLISHERS PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 1058-0468 EI 1573-7330 J9 J ASSIST REPROD GEN JI J. Assist. Reprod. Genet. PD AUG PY 2015 VL 32 IS 8 BP 1239 EP 1250 DI 10.1007/s10815-015-0543-x PG 12 WC Genetics & Heredity; Obstetrics & Gynecology; Reproductive Biology SC Genetics & Heredity; Obstetrics & Gynecology; Reproductive Biology GA CQ4AV UT WOS:000360547300013 PM 26249553 ER PT J AU Ielpi, A Gibling, MR Bashforth, AR Dennar, CI AF Ielpi, Alessandro Gibling, Martin R. Bashforth, Arden R. Dennar, Chinemerem I. TI IMPACT OF VEGETATION ON EARLY PENNSYLVANIAN FLUVIAL CHANNELS: INSIGHT FROM THE JOGGINS FORMATION OF ATLANTIC CANADA SO JOURNAL OF SEDIMENTARY RESEARCH LA English DT Article ID BOSS POINT FORMATION; NOVA-SCOTIA; CORDAITALEAN TREES; OKAVANGO DELTA; FOSSIL CLIFFS; NEW-BRUNSWICK; WOODY DEBRIS; ALLUVIAL ARCHITECTURE; CENTRAL AUSTRALIA; MARINE INFLUENCE AB Riparian vegetation profoundly influences modern fluvial channels in a variety of ways, depending on the life-history strategies of different plant types, disturbance frequency, and drainage conditions of available habitats. Direct evidence for these dynamic relationships is usually cryptic in ancient deposits. We report evidence for interactions between rivers and in situ vegetation for selected sites in the lower Pennsylvanian Joggins Formation of Atlantic Canada, encompassing fixed, meandering, and distributary channels originally up to 6 m deep. Channel bodies are associated with a suite of fossilized plant remains, specifically lycopsids that preferred stable wetland settings, disturbance-tolerant calamitaleans, and slow-growing, long-lived cordaitaleans. Vegetation was effective in stabilizing banks and bars and promoting aggradation. Lycopsids and calamitalean groves colonized the channel bed during periods of reduced flow, drawing on the groundwater table, and mounds around upright trunks indicate that they formed bar nuclei after flow resumed. Bank-attached bars with lateral-accretion sets contain upright trees, which may have stabilized inclined sediment surfaces, and trees present between small distributary channels may have formed vegetated islands. Erect lycopsids rooted below the channel base project up into the channel fill, where they formed obstacles and nucleated sediment mounds in active channels. On channel cutbanks, upright lycopsids are tilted towards the channel, and early formed rhizoconcretions are associated with deep cordaitalean root systems in the tops of channel fills. These features imply that vegetation contributed to stabilization of sediment surfaces. The predominance of in situ over transported plant remains suggests that these low-flow-strength rivers had limited ability to erode and entrain large woody debris, especially for small channels with strengthened banks. We infer that patterns of interaction between vegetation and rivers with a range of fluvial style broadly resembled those of today. By the early Pennsylvanian, rivers had moved from a geomorphic and biogeomorphic mode of operation into a fully ecological mode with prominent feedback loops between vegetation and fluvial processes. Vegetation is commonly poorly preserved in fluvial systems but should be incorporated into facies models for Pennsylvanian and younger strata, possibly also for some Devonian and Mississippian formations. C1 [Ielpi, Alessandro; Gibling, Martin R.; Dennar, Chinemerem I.] Dalhousie Univ, Dept Earth Sci, Halifax, NS B3H 4R2, Canada. [Bashforth, Arden R.] Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20560 USA. RP Ielpi, A (reprint author), Geol Survey Canada, 601 Booth St, Ottawa, ON K1A 0E8, Canada. EM alessandro.ielpi@nrcan.gc.ca FU Natural Sciences and Engineering Research Council of Canada (NSERC); NSERC FX The authors are greatly indebted to Rhea Hurnik for field support and to the Joggins Fossil Centre for logistical assistance. We thank reviewer Christopher Fielding, an anonymous reviewer, and editors Gregory Nadon and James MacEachern for insightful comments. Research was supported by a Discovery Grant to MRG from the Natural Sciences and Engineering Research Council of Canada (NSERC). AI and ARB acknowledge the support of Postdoctoral Fellowships from NSERC. The research was carried out under a Heritage Research Permit from the Nova Scotia Department of Communities, Culture and Heritage. NR 130 TC 3 Z9 3 U1 4 U2 16 PU SEPM-SOC SEDIMENTARY GEOLOGY PI TULSA PA 6128 EAST 38TH ST, STE 308, TULSA, OK 74135-5814 USA SN 1527-1404 EI 1938-3681 J9 J SEDIMENT RES JI J. Sediment. Res. PD AUG PY 2015 VL 85 IS 8 BP 999 EP 1018 DI 10.2110/jsr.2015.50 PG 20 WC Geology SC Geology GA CP8QT UT WOS:000360159900005 ER PT J AU van der Sar, T Casola, F Walsworth, R Yacoby, A AF van der Sar, Toeno Casola, Francesco Walsworth, Ronald Yacoby, Amir TI Nanometre-scale probing of spin waves using single-electron spins SO NATURE COMMUNICATIONS LA English DT Article ID AMBIENT CONDITIONS; NANOSCALE RESOLUTION; MAGNETIC-RESONANCE; MAGNETOMETRY; SENSITIVITY; SKYRMIONS AB Pushing the frontiers of condensed-matter magnetism requires the development of tools that provide real-space, few-nanometre-scale probing of correlated-electron magnetic excitations under ambient conditions. Here we present a practical approach to meet this challenge, using magnetometry based on single nitrogen-vacancy centres in diamond. We focus on spin-wave excitations in a ferromagnetic microdisc, and demonstrate local, quantitative and phase-sensitive detection of the spin-wave magnetic field at similar to 50 nm from the disc. We map the magnetic-field dependence of spin-wave excitations by detecting the associated local reduction in the disc's longitudinal magnetization. In addition, we characterize the spin-noise spectrum by nitrogen-vacancy spin relaxometry, finding excellent agreement with a general analytical description of the stray fields produced by spin-spin correlations in a 2D magnetic system. These complementary measurement modalities pave the way towards imaging the local excitations of systems such as ferromagnets and antiferromagnets, skyrmions, atomically assembled quantum magnets, and spin ice. C1 [van der Sar, Toeno; Casola, Francesco; Walsworth, Ronald; Yacoby, Amir] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. [Casola, Francesco; Walsworth, Ronald] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Yacoby, A (reprint author), Harvard Univ, Dept Phys, 17 Oxford St, Cambridge, MA 02138 USA. EM yacoby@physics.harvard.edu FU DARPA QuASAR program; National Science Foundation; Swiss National Science Foundation FX We acknowledge support of the DARPA QuASAR program and the National Science Foundation. F.C. acknowledges support from the Swiss National Science Foundation. NR 38 TC 12 Z9 12 U1 4 U2 43 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 AUG PY 2015 VL 6 AR 7886 DI 10.1038/ncomms8886 PG 7 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA CQ1GE UT WOS:000360344500005 PM 26249673 ER PT J AU Engene, N Tronholm, A Salvador-Reyes, LA Luesch, H Paul, VJ AF Engene, Niclas Tronholm, Ana Salvador-Reyes, Lilibeth A. Luesch, Hendrik Paul, Valerie J. TI CALDORA PENICILLATA GEN. NOV., COMB. NOV (CYANOBACTERIA), A PANTROPICAL MARINE SPECIES WITH BIOMEDICAL RELEVANCE SO JOURNAL OF PHYCOLOGY LA English DT Article DE dolastatin 10; largazole; Lyngbya; natural products; Phormidium; phylogenetics; secondary metabolites; Symploca; symplostatin 1 ID STRAINS CYANOBACTERIA; POLYPHASIC APPROACH; MAXIMUM-LIKELIHOOD; GENETIC DIVERSITY; DOLASTATIN 10; RNA GENES; OSCILLATORIALES; PHORMIDIUM; SEQUENCES; LARGAZOLE AB Many tropical marine cyanobacteria are prolific producers of bioactive secondary metabolites with ecological relevance and promising pharmaceutical applications. One species of chemically rich, tropical marine cyanobacteria that was previously identified as Symploca hydnoides or Symploca sp. corresponds to the traditional taxonomic definition of Phormidium penicillatum. In this study, we clarified the taxonomy of this biomedically and ecologically important cyanobacterium by comparing recently collected specimens with the original type material and the taxonomic description of P. penicillatum. Molecular phylogenetic analyses of the 16S rRNA gene and the 16S-23S internal transcribed spacer regions showed that P. penicillatum formed an independent clade sister to the genus Symploca, and distantly related to Phormidium and Lyngbya. We propose the new genus Caldora for this clade, with Caldora penicillata comb. nov. as the type species and designate as the epitype the recently collected strain FK13-1. Furthermore, the production of bioactive secondary metabolites among various geographically dispersed collections of C. penicillata showed that this species consistently produced the metabolite dolastatin 10 and/or the related compound symplostatin 1, which appear to be robust autapomorphic characters and chemotaxonomic markers for this taxon. C1 [Engene, Niclas] Florida Int Univ, Dept Biol Sci, Miami, FL 33199 USA. [Tronholm, Ana; Paul, Valerie J.] Smithsonian Marine Stn Ft Pierce, Ft Pierce, FL 34949 USA. [Salvador-Reyes, Lilibeth A.] Univ Philippines Diliman, Inst Marine Sci, Quezon City 1101, Philippines. [Luesch, Hendrik] Univ Florida, Dept Med Chem, Gainesville, FL 32610 USA. [Luesch, Hendrik] Univ Florida, Ctr Nat Prod Drug Discovery & Dev, Gainesville, FL 32610 USA. RP Engene, N (reprint author), Florida Int Univ, Dept Biol Sci, Miami, FL 33199 USA. EM nengene@fiu.edu FU Smithsonian Marine Science Network; NIH [R01CA172310] FX This research project was funded by the Smithsonian Marine Science Network (NE) and in part by the NIH (R01CA172310). Field collections were supported by the Carmabi Research Station (Curacao), Carrie Bow Cay Field Station (Belize), Mote Marine Laboratory (Summerland Key, FL), Smithsonian Marine Station (Ft. Pierce, FL), and the Council on International Educational Exchange Research Station (Bonaire). We acknowledge the governments of Curacao, Belize, Honduras, and Bonaire for permits to collect cyanobacteria. Research activities in the Florida Keys National Marine Sanctuary occurred under permit FKNMS-2013-023 (VP) and FKNMS-2011-007 (B. Lapointe). Field collections were partly supported by a NMNH Small Grant (VP) for Bonaire and Curacao, Mote Protect our Reefs Grants for the Florida Keys (VP), and by the Summit Foundation through the Centre for Marine Studies for Honduras (S. Box). We thank R. Ritson-Williams, S. Reed, and B. Lapointe for help with sampling, as well as A. Wood, B. Lapointe and Z. Foltz for underwater photography. We thank K. A. Miller and the late P. C. Silva at the University and Jepson Herbaria of the University of California at Berkeley for lending isotypes, W. Gerwick and T. Byrum for sharing the Symploca reference strain, and K. McPhail for providing the Leptolyngbya sp. strain PAC-10-03. We are very grateful to L. Le Gall and L. Kervran at PC for the loan of specimens of P. penicillatum. We also thank B. Brooks for help with deposition of specimens at US. We are also grateful to A. Economou-Amilli for help with botanical nomenclature. We thank M. Zubia, O. De Clerck, and T. Sauvage for providing us with valuable information about samples from Reunion. We gratefully acknowledge H. Reichardt and the staff at the SMSFP for general lab assistance. All SEM imaging was performed at the USDA Horticultural research laboratory with the assistance of J. Piraino. All gene sequencing was performed at the Laboratories of Analytical Biology of the NMNH thanks to J. Hunt and L. Weight. We thank A. Wright and P. Winder at Harbor Branch Oceanographic Institute at Florida Atlantic University for usage of LCMS and NMR, and S. Gunasekera for analytical assistance. SMSFP contribution no. 994 and CCRE contribution no. 974. NR 57 TC 3 Z9 3 U1 0 U2 7 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0022-3646 EI 1529-8817 J9 J PHYCOL JI J. Phycol. PD AUG PY 2015 VL 51 IS 4 BP 670 EP 681 DI 10.1111/jpy.12309 PG 12 WC Plant Sciences; Marine & Freshwater Biology SC Plant Sciences; Marine & Freshwater Biology GA CP5JY UT WOS:000359918800008 PM 26327714 ER PT J AU Hernandez-Kantun, JJ Rindi, F Adey, WH Heesch, S Pena, V Le Gall, L Gabrielson, PW AF Hernandez-Kantun, Jazmin J. Rindi, Fabio Adey, Walter H. Heesch, Svenja Pena, Viviana Le Gall, Line Gabrielson, Paul W. TI SEQUENCING TYPE MATERIAL RESOLVES THE IDENTITY AND DISTRIBUTION OF THE GENERITYPE LITHOPHYLLUM INCRUSTANS, AND RELATED EUROPEAN SPECIES L. HIBERNICUM AND L. BATHYPORUM (CORALLINALES, RHODOPHYTA) SO JOURNAL OF PHYCOLOGY LA English DT Article DE anatomy; Lithophyllum bathyporum; Lithophyllum hibernicum; Lithophyllum incrustans; psbA; rbcL; rhodolith; taxonomy; type specimens ID PHILIPPI,R.A. ORIGINAL COLLECTIONS; TAXONOMIC REASSESSMENT; NORTHEAST PACIFIC; SP-NOV; DNA; DIVERSITY; ATLANTIC; NUCLEAR; NAMES; MELOBESIOIDEAE AB DNA sequences from type material in the nongeniculate coralline genus Lithophyllum were used to unambiguously link some European species names to field-collected specimens, thus providing a great advance over morpho-anatomical identification. In particular, sequence comparisons of rbcL, COI and psbA genes from field-collected specimens allowed the following conclusion: the generitype species, L. incrustans, occurs mostly as subtidal rhodoliths and crusts on both Atlantic and Mediterranean coasts, and not as the common, NE Atlantic, epilithic, intertidal crust reported in the literature. The heterotypic type material of L. hibernicum was narrowed to one rhodolith belonging in Lithophyllum. As well as occurring as a subtidal rhodolith, L. hibernicum is a common, epilithic and epizoic crust in the intertidal zone from Ireland south to Mediterranean France. A set of four features distinguished L. incrustans from L. hibernicum, including epithallial cell diameter, pore canal shape of sporangial conceptacles and sporangium height and diameter. An rbcL sequence of the lectotype of Lithophyllum bathyporum, which was recently proposed to accommodate Atlantic intertidal collections of L. incrustans, corresponded to a distinct taxon hitherto known only from Brittany as the subtidal, bisporangial, lectotype, but also occurs intertidally in Atlantic Spain. Specimens from Ireland and France morpho-anatomically identified as L. fasciculatum and a specimen from Cornwall likewise identified as L. duckerae were resolved as L. incrustans and L. hibernicum, respectively. C1 [Hernandez-Kantun, Jazmin J.; Adey, Walter H.] Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, Washington, DC 20560 USA. [Hernandez-Kantun, Jazmin J.; Heesch, Svenja] Natl Univ Ireland, Ryan Inst, Irish Seaweed Res Grp, Galway, Ireland. [Rindi, Fabio] Univ Politecn Marche, Dipartimento Sci Vita & Ambiente, I-60131 Ancona, Italy. [Pena, Viviana] Univ A Coruna, Fac Ciencias, BIOCOST Res Grp, Dept Biol Anim Biol Vexetal & Ecol, La Coruna 15071, Spain. [Pena, Viviana; Le Gall, Line] Univ Paris 04, Museum Natl Hist Nat, EPHE,UMR ISYEB CNRS 7205, UPMC,Equipe Explorat Especes & Evolut,Inst Systma, F-75005 Paris, France. [Pena, Viviana] Univ Ghent, Phycol Res Grp, B-9000 Ghent, Belgium. [Gabrielson, Paul W.] Univ N Carolina, Dept Biol, Chapel Hill, NC 27599 USA. [Gabrielson, Paul W.] Univ N Carolina, Herbarium, Chapel Hill, NC 27599 USA. RP Hernandez-Kantun, JJ (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, MRC 166 POB 37012, Washington, DC 20560 USA. EM jaz1083@gmail.com RI Le Gall, Line/E-1884-2014; OI Le Gall, Line/0000-0001-7807-4569; Heesch, Svenja/0000-0002-4531-0921; Pena, Viviana/0000-0001-7003-3850 FU National Council for Science and Technology, Mexico [CONACyT-211950]; SEP (Secretariat for Public Education, Mexico); Marine Institute (Ireland) as part of the National Marine Biodiscovery Program (Beaufort Award for Marine Biodiscovery); European Community through the FP6 [NMP3-CT-2003-505758]; National University of Ireland, Galway through the Thomas Crawford Award; M.I.U.R. (Italian Ministry for Education, Universities and Research) through a P.R.I.N.; postdoctoral program Axudas de apoio a etapa inicial de formacion posdoutoral do Plan I2C (Xunta de Galicia); British Phycological Society; Spain's Ministerio de Economia y Competitividad [CGL2009-09495/BOS]; Action Transversale du Museum National d'Histoire Naturelle; network "Bibliotheque du Vivant" - CNRS; Museum National d'Histoire Naturelle; INRA; CEA (Centre National de Sequencage) FX We are very grateful to the following curators for the loan of type material essential to this research: J. Wilbraham (BM), Dr. E. Smets (L), and Dr. K. Hassel (TRH). Jacques Grall, Christine Maggs, Jason Hall-Spencer, Line Le Gall, Conxi Rodriguez-Prieto, Ignacio Barbara, Pilar Diaz, Antonio Secilla, Meadhbh Moriarty, Ricardo Bermejo Lacida, Alex Wan, Benoit Queguineur, Julia Nunn, and Marie Pazoutova are gratefully acknowledged for the collection of samples and/or assistance in the field. We thank P. Lalor for assistance with SEM images, Prof. J. Brodie for revising early versions of the manuscript, and the reviewers for helpful comments and suggestions; JHK was supported by a PhD scholarship from CONACyT-211950 (National Council for Science and Technology, Mexico) and SEP (Secretariat for Public Education, Mexico). Financial support was received from the Marine Institute (Ireland) as part of the National Marine Biodiscovery Program (Beaufort Award for Marine Biodiscovery to the National University of Ireland, Galway), from the European Community through the FP6-funded project HIPPOCRATES (NMP3-CT-2003-505758), from the National University of Ireland, Galway through the Thomas Crawford Award, and from the M.I.U.R. (Italian Ministry for Education, Universities and Research) through a P.R.I.N. 2011 project (Coastal bioconstructions: structure, function and management). VP acknowledges support by the postdoctoral program Axudas de apoio a etapa inicial de formacion posdoutoral do Plan I2C (Xunta de Galicia), and projects funded by British Phycological Society (Small Grant Scheme-Project Award 2011-2012) and Spain's Ministerio de Economia y Competitividad (CGL2009-09495/BOS, partially founded by ERDF); molecular data provided by VP were produced at the Service de Systematique Moleculaire of the Museum National d'Histoire Naturelle (CNRS - UMS 2700) with funds provided by Action Transversale du Museum National d'Histoire Naturelle ("Taxonomie moleculaire: DNA Barcode et gestion durable des collections," "Biodiversite actuelle et fossile. Crises, stress, restaurations et panchronisme: le message systematique" and "Emergences") and network "Bibliotheque du Vivant" funded by CNRS, Museum National d'Histoire Naturelle, INRA and CEA (Centre National de Sequencage). PWG thanks Dr. T. Vision (University of North Carolina, Chapel Hill) for use of lab space and equipment and Dr. D.W. Freshwater (DNA Analysis Core Facility, Center for Marine Sciences, University of North Carolina, Wilmington) for DNA sequencing. NR 68 TC 7 Z9 7 U1 0 U2 8 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0022-3646 EI 1529-8817 J9 J PHYCOL JI J. Phycol. PD AUG PY 2015 VL 51 IS 4 BP 791 EP 807 DI 10.1111/jpy.12319 PG 17 WC Plant Sciences; Marine & Freshwater Biology SC Plant Sciences; Marine & Freshwater Biology GA CP5JY UT WOS:000359918800017 PM 26986797 ER PT J AU Mullins, P Pugh, R Vaught, J AF Mullins, Piper Pugh, Rebecca Vaught, Jim TI Following up on ISBER 2015: Call for Environmental Biobanking Papers SO BIOPRESERVATION AND BIOBANKING LA English DT Editorial Material C1 [Mullins, Piper] Smithsonian Inst, Pan Smithsonian Gyo Initiat, Washington, DC 20560 USA. [Pugh, Rebecca] NIST, Charleston, SC USA. RP Mullins, P (reprint author), Smithsonian Inst, Pan Smithsonian Gyo Initiat, Washington, DC 20560 USA. EM jvaught@liebertpub.com NR 0 TC 1 Z9 1 U1 1 U2 1 PU MARY ANN LIEBERT, INC PI NEW ROCHELLE PA 140 HUGUENOT STREET, 3RD FL, NEW ROCHELLE, NY 10801 USA SN 1947-5535 EI 1947-5543 J9 BIOPRESERV BIOBANK JI Biopreserv. Biobank. PD AUG 1 PY 2015 VL 13 IS 4 BP 229 EP 230 DI 10.1089/bio.2015.29013.pm PG 2 WC Cell Biology; Chemistry, Applied; Medical Laboratory Technology SC Cell Biology; Chemistry; Medical Laboratory Technology GA CP0TX UT WOS:000359589800001 PM 26280500 ER PT J AU Merrill, RM Dasmahapatra, KK Davey, JW Dell'Aglio, DD Hanly, JJ Huber, B Jiggins, CD Joron, M Kozak, KM Llaurens, V Martin, SH Montgomery, SH Morris, J Nadeau, NJ Pinharanda, AL Rosser, N Thompson, MJ Vanjari, S Wallbank, RWR Yu, Q AF Merrill, R. M. Dasmahapatra, K. K. Davey, J. W. Dell'Aglio, D. D. Hanly, J. J. Huber, B. Jiggins, C. D. Joron, M. Kozak, K. M. Llaurens, V. Martin, S. H. Montgomery, S. H. Morris, J. Nadeau, N. J. Pinharanda, A. L. Rosser, N. Thompson, M. J. Vanjari, S. Wallbank, R. W. R. Yu, Q. TI The diversification of Heliconius butterflies: what have we learned in 150 years? SO JOURNAL OF EVOLUTIONARY BIOLOGY LA English DT Review DE adaptation; ecological genomics; gene flow; magic traits; mimicry; Nymphalidae; porous species; reproductive isolation; sensory ecology; speciation ID PASSION-VINE BUTTERFLIES; INSECT MUSHROOM BODIES; WITH-GENE-FLOW; MULLERIAN MIMICRY; WARNING-COLOR; HYBRID ZONES; HOST-PLANT; ECOLOGICAL SPECIATION; LINKAGE MAP; LEPIDOPTERA NYMPHALIDAE AB Research into Heliconius butterflies has made a significant contribution to evolutionary biology. Here, we review our understanding of the diversification of these butterflies, covering recent advances and a vast foundation of earlier work. Whereas no single group of organisms can be sufficient for understanding life's diversity, after years of intensive study, research into Heliconiushas addressed a wide variety of evolutionary questions. We first discuss evidence for widespread gene flow betweenHeliconius species and what this reveals about the nature of species. We then address the evolution and diversity of warning patterns, both as the target of selection and with respect to their underlying genetic basis. The identification of major genes involved in mimetic shifts, and homology at these loci between distantly related taxa, has revealed a surprising predictability in the genetic basis of evolution. In the final sections, we consider the evolution of warning patterns, and Heliconius diversity more generally, within a broader context of ecological and sexual selection. We consider how different traits and modes of selection can interact and influence the evolution of reproductive isolation. C1 [Merrill, R. M.; Davey, J. W.; Dell'Aglio, D. D.; Hanly, J. J.; Jiggins, C. D.; Kozak, K. M.; Martin, S. H.; Nadeau, N. J.; Pinharanda, A. L.; Thompson, M. J.; Vanjari, S.; Wallbank, R. W. R.; Yu, Q.] Univ Cambridge, Dept Zool, Cambridge CB2 3EJ, England. [Merrill, R. M.; Jiggins, C. D.; Joron, M.] Smithsonian Trop Res Inst, Panama City, Panama. [Dasmahapatra, K. K.; Huber, B.; Morris, J.; Rosser, N.] Univ York, Dept Biol, York YO10 5DD, N Yorkshire, England. [Huber, B.; Joron, M.; Llaurens, V.] Univ Paris 04, ISYEB UMR CNRS 7205, Museum Natl Hist Nat, MNHN,UPMC,EPHE,Inst Systemat,Evolut,Biodiversite, Paris, France. [Joron, M.] Univ Montpellier 3, CEFE UMR 5175, Ctr Ecol Fonct & Evolut, EPHE,CNRS, Montpellier 5, France. [Montgomery, S. H.] UCL, Dept Genet Evolut & Environm, London, England. [Nadeau, N. J.] Univ Sheffield, Dept Anim & Plant Sci, Sheffield S10 2TN, S Yorkshire, England. [Thompson, M. J.] Nat Hist Museum, Dept Life Sci, London SW7 5BD, England. [Yu, Q.] Chongqing Univ, Sch Life Sci, Chongqing 630044, Peoples R China. RP Merrill, RM (reprint author), Univ Cambridge, Dept Zool, Downing St, Cambridge CB2 3EJ, England. EM r.merrill@zoo.cam.ac.uk RI Jiggins, Chris/B-9960-2008; Martin, Simon/D-1410-2011; Nadeau, Nicola/E-1149-2011; OI Jiggins, Chris/0000-0002-7809-062X; Martin, Simon/0000-0002-0747-7456; Nadeau, Nicola/0000-0002-9319-921X; Kozak, Krzysztof/0000-0001-8980-3173; Davey, John/0000-0002-1017-9775; Dasmahapatra, Kanchon Kumar/0000-0002-2840-7019 FU Junior Research Fellowship at King's College, Cambridge; Balfour Studentship, University of Cambridge; Research Fellowship at St John's College, Cambridge; Research Fellowship from the Royal Commission for the Exhibition of 1851; Agence Nationale de la Recherche (France); Biology and Biotechnology Research Council (UK); British Ecological Society; European Research Council; Natural Environment Research Council (UK); Smithsonian Tropical Research Institute FX RMM is funded by a Junior Research Fellowship at King's College, Cambridge. KMK is supported by the Balfour Studentship, University of Cambridge; SHMa by a Research Fellowship at St John's College, Cambridge; and SHMo by a Research Fellowship from the Royal Commission for the Exhibition of 1851. Our work on Heliconius has been additionally supported by the Agence Nationale de la Recherche (France), the Biology and Biotechnology Research Council (UK), the British Ecological Society, the European Research Council, the Natural Environment Research Council (UK), and the Smithsonian Tropical Research Institute. We are grateful to Steven van Belleghem, Markus Moest, Brett Seymoure and Timothy Thurman for comments on the manuscript, and the wider Heliconius community for years of stimulating discussion and collaboration. We also thank Hanna Kokko, David Pfennig and a further anonymous reviewer, whose comments greatly improved this manuscript. This review was conceived by RMM and CDJ, and the first draft was written during an enjoyable retreat to North Wales. We would like to thank the trustees of Pen-y-Clip, Fachwen, for accommodating us. NR 239 TC 17 Z9 17 U1 23 U2 130 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1010-061X EI 1420-9101 J9 J EVOLUTION BIOL JI J. Evol. Biol. PD AUG PY 2015 VL 28 IS 8 BP 1417 EP 1438 DI 10.1111/jeb.12672 PG 22 WC Ecology; Evolutionary Biology; Genetics & Heredity SC Environmental Sciences & Ecology; Evolutionary Biology; Genetics & Heredity GA CP0ZS UT WOS:000359606200001 PM 26079599 ER PT J AU Vaslet, A Phillips, DL France, CAM Feller, IC Baldwin, CC AF Vaslet, A. Phillips, D. L. France, C. A. M. Feller, I. C. Baldwin, C. C. TI Trophic behaviour of juvenile reef fishes inhabiting interlinked mangrove-seagrass habitats in offshore mangrove islets SO JOURNAL OF FISH BIOLOGY LA English DT Article DE fish foraging habitats; gut contents; marine ecosystems; SIAR; SIBER; stable isotopes ID ISOTOPE MIXING MODELS; INCORPORATING CONCENTRATION-DEPENDENCE; STABLE-ISOTOPE; RELATIVE IMPORTANCE; FEEDING HABITATS; BEDS; COMMUNITIES; ESTUARINE; DIETARY; CARBON AB Stable isotope (C-13 and N-15) and gut content analyses were used to investigate size-related feeding habits of four reef fishes (the beaugregory Stegastes leucostictus, the french grunt Haemulon flavolineatum, the schoolmaster snapper Lutjanus apodus and the yellowtail snapper Ocyurus chrysurus) inhabiting an offshore (non-estuarine) mangrove islet off Belize, Central America. Comparisons of isotopic niche space and Schoener diet similarity index suggested a low to moderate degree of niche overlap between fish size groups. The C-13 gradient between mangrove and seagrass prey as well as results of Bayesian mixing models revealed that sampled fishes relied mostly on seagrass prey items. Only small and large juveniles of the carnivorous species L. apodus derived a part of their diet from mangroves by targeting mangrove-associated Grapsidae crabs and fish prey, respectively. Isotopic niche shifts were particularly obvious for carnivorous fishes that ingested larger prey items (Xanthidae crabs and fishes) during their ontogeny. The utilization of mangrove food resources is less than expected and depends on the ecology and life history of the fish species considered. This research highlights that mangrove-derived carbon contributed relatively little to the diets of four fish taxa from an offshore mangrove islet. C1 [Vaslet, A.] Smithsonian Marine Stn Ft Pierce, Ft Pierce, FL 34949 USA. [Phillips, D. L.] US EPA, Natl Hlth & Environm Effects Res Lab, Western Ecol Div, Corvallis, OR 97333 USA. [France, C. A. M.] Smithsonian Museum Conservat Inst, Suitland, MD 20746 USA. [Feller, I. C.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. [Baldwin, C. C.] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20013 USA. RP Vaslet, A (reprint author), Smithsonian Marine Stn Ft Pierce, 701 Seaway Dr, Ft Pierce, FL 34949 USA. EM amandine.vaslet@gmail.com OI Feller, Ilka/0000-0002-6391-1608 FU Marine Science Network Grant from the Smithsonian Institution FX The authors thank V. Paul, Z. Foltz, W. Lee and all the staff of Smithsonian Marine Station at Fort Pierce FL (SMSFP) for their assistance and access to laboratory facilities. We thank C. McIvor of the U.S. Geological Survey, St Petersburg, FL, and anonymous referees for their constructive review of the manuscript. This research was funded by a Marine Science Network Grant from the Smithsonian Institution through a Postdoctoral fellowship to A.V. D.L.P.'s time was provided by the U.S. Environmental Protection Agency. This document has been subjected to the Agency's peer and administrative review, and it has been approved for publication as an EPA document. This is contribution number #997 from the SMSFP and contribution number #975 from the Smithsonian's Caribbean Coral Reef Ecosystems Program. NR 57 TC 1 Z9 1 U1 6 U2 52 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0022-1112 EI 1095-8649 J9 J FISH BIOL JI J. Fish Biol. PD AUG PY 2015 VL 87 IS 2 BP 256 EP 273 DI 10.1111/jfb.12715 PG 18 WC Fisheries; Marine & Freshwater Biology SC Fisheries; Marine & Freshwater Biology GA CO8LS UT WOS:000359421400004 PM 26084450 ER PT J AU Hong, T AF Hong, Terry TI Wind/Pinball SO LIBRARY JOURNAL LA English DT Book Review C1 [Hong, Terry] Smithsonian BookDragon, Washington, DC 20024 USA. RP Hong, T (reprint author), Smithsonian BookDragon, Washington, DC 20024 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 AUG PY 2015 VL 140 IS 13 BP 87 EP 89 PG 3 WC Information Science & Library Science SC Information Science & Library Science GA CO7IS UT WOS:000359333400135 ER PT J AU Hong, T AF Hong, Terry TI The Investigation SO LIBRARY JOURNAL LA English DT Book Review C1 [Hong, Terry] Smithsonian BookDragon, Washington, DC 20024 USA. RP Hong, T (reprint author), Smithsonian BookDragon, Washington, DC 20024 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 AUG PY 2015 VL 140 IS 13 BP 87 EP 87 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA CO7IS UT WOS:000359333400131 ER PT J AU Kelley, AL de Rivera, CE Grosholz, ED Ruiz, GM Yamada, SB Gillespie, G AF Kelley, Amanda L. de Rivera, Catherine E. Grosholz, Edwin D. Ruiz, Gregory M. Yamada, Sylvia Behrens Gillespie, Graham TI Thermogeographic variation in body size of Carcinus maenas, the European green crab SO MARINE BIOLOGY LA English DT Article ID EASTERN BERING-SEA; DROSOPHILA-MELANOGASTER; CHIONOECETES-OPILIO; PHENOTYPIC PLASTICITY; SALINITY PREFERENCE; BRACHYURAN CRABS; FEMALE SIZE; COPES RULE; SHORE CRAB; TEMPERATURE AB Populations that span a large geographic range often experience a thermal gradient that can differentially affect the phenotypic response of individuals across the population. Variation in temperature has been shown to affect the final adult size of ectotherms, which is referred to as the temperature-size rule for ectotherms. Body size is a fundamentally important trait, as it can impact physiological performance, fecundity, longevity, and macroecological patterns. Hence, temperature may affect body size across a range, which can in turn influence maintenance of populations and ecological interactions. Here, we test whether biogeographic differences in size (carapace width) exist for a recent invasion of the non-native European green crab, Carcinus maenas, along the west coast of North America. We assembled trapping and temperature data collected from 10 sites along the western North American coast over a 5-year period. We also conducted a literature review of C. maenas size across their native range. Our results indicate that adult body size shows negative correlation with environmental temperature in both the native and invaded ranges, conforming to the temperature-size rule for ectotherms. Given the short time since colonization and lack of evident genetic structure across the invasive range, it may be that phenotypic plasticity in response to environmental temperature is driving this relationship. Forces that shape the phenotypic trajectory of species may play an important role in both invasion dynamics and subsequent ecological impacts. C1 [Kelley, Amanda L.] Univ Calif Santa Barbara, Dept Ecol Evolut & Marine Biol, Santa Barbara, CA 93106 USA. [de Rivera, Catherine E.; Ruiz, Gregory M.] Portland State Univ, Dept Environm Sci & Management, Portland, OR 97201 USA. [Grosholz, Edwin D.] Univ Calif Davis, Dept Environm Sci & Policy, Davis, CA 95616 USA. [Ruiz, Gregory M.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. [Yamada, Sylvia Behrens] Oregon State Univ, Integrat Biol, Corvallis, OR 97331 USA. [Gillespie, Graham] Fisheries & Oceans Canada, Sci Branch, Pacific Reg Pacific Biol Stn, Nanaimo, BC V9T 6N7, Canada. RP Kelley, AL (reprint author), Univ Calif Santa Barbara, Dept Ecol Evolut & Marine Biol, Santa Barbara, CA 93106 USA. EM amanda.kelley@lifesci.ucsb.edu OI Ruiz, Gregory/0000-0003-2499-441X FU UC Exotic Pest and Disease Program; Oceans and Fisheries, Canada; Pacific Marine Fisheries Commission; NSF Graduate Research Fellowship Grant [220005]; NOAA [NA06OAR4170261, NA06OAR4170159, NA07OAR4170501, NA08OAR4170927]; Alaska Department of Fish and Game [IHP-07-146] FX We would like to thank in no particular order: Brian Steves for the Bio-ORACLE temperature data extraction, Scott Groth of the Oregon Department of Fish and Wildlife, and the staff and faculty of the Oregon Institute of Marine Biology for their hospitality while sampling in Coos Bay, and W. McClees for creating Fig. 1. For their help in collecting data, we also thank: B. Kordas, A. Larson, C. Coleman-Hulbert, S. Attoe, I. Clarke, B. Turner, B. Cheng, D. Kimbro, A. Bakus, A. Deck. We also thank R. Preisler and K. Wasson for generously providing the data from Elkhorn Slough, and P. Coelho for CW data from Portugal. Financial support was provided (in part) by UC Exotic Pest and Disease Program, Oceans and Fisheries, Canada, the Pacific Marine Fisheries Commission, NSF Graduate Research Fellowship Grant to ALK, Grant Number 220005, NOAA (Grant #NA06OAR4170261, NA06OAR4170159, NA07OAR4170501, NA08OAR4170927), and Alaska Department of Fish and Game (#IHP-07-146). NR 63 TC 2 Z9 2 U1 5 U2 25 PU SPRINGER HEIDELBERG PI HEIDELBERG PA TIERGARTENSTRASSE 17, D-69121 HEIDELBERG, GERMANY SN 0025-3162 EI 1432-1793 J9 MAR BIOL JI Mar. Biol. PD AUG PY 2015 VL 162 IS 8 BP 1625 EP 1635 DI 10.1007/s00227-015-2698-5 PG 11 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA CO7ZV UT WOS:000359384600010 ER PT J AU Tepolt, CK Palumbi, SR AF Tepolt, C. K. Palumbi, S. R. TI Transcriptome sequencing reveals both neutral and adaptive genome dynamics in a marine invader SO MOLECULAR ECOLOGY LA English DT Article DE adaptation; invasive species; natural selection and contemporary evolution; neutral processes; population genetics - empirical; transcriptomics ID SNAIL LITTORINA-SAXATILIS; CRABS CARCINUS-MAENAS; POPULATION-STRUCTURE; LOCAL ADAPTATION; GENE FLOW; RANGE EXPANSION; GREEN CRAB; DROSOPHILA-SUBOBSCURA; ECOLOGICAL DIVERGENCE; BIOLOGICAL INVASIONS AB Species invasions cause significant ecological and economic damage, and genetic information is important to understanding and managing invasive species. In the ocean, many invasive species have high dispersal and gene flow, lowering the discriminatory power of traditional genetic approaches. High-throughput sequencing holds tremendous promise for increasing resolution and illuminating the relative contributions of selection and drift in marine invasion, but has not yet been used to compare the diversity and dynamics of a high-dispersal invader in its native and invaded ranges. We test a transcriptome-based approach in the European green crab (Carcinus maenas), a widespread invasive species with high gene flow and a well-known invasion history, in two native and five invasive populations. A panel of 10809 transcriptome-derived nuclear SNPs identified significant population structure among highly bottlenecked invasive populations that were previously undifferentiated with traditional markers. Comparing the full data set and a subset of 9246 putatively neutral SNPs strongly suggested that non-neutral processes are the primary driver of population structure within the species' native range, while neutral processes appear to dominate in the invaded range. Non-neutral native range structure coincides with significant differences in intraspecific thermal tolerance, suggesting temperature as a potential selective agent. These results underline the importance of adaptation in shaping intraspecific differences even in high geneflow marine invasive species. They also demonstrate that high-throughput approaches have broad utility in determining neutral structure in recent invasions of such species. Together, neutral and non-neutral data derived from high-throughput approaches may increase the understanding of invasion dynamics in high-dispersal species. C1 [Tepolt, C. K.; Palumbi, S. R.] Stanford Univ, Hopkins Marine Stn, Pacific Grove, CA 93950 USA. RP Tepolt, CK (reprint author), Smithsonian Environm Res Ctr, 647 Contees Wharf Rd, Edgewater, MD 21037 USA. EM carolyn.tepolt@gmail.com FU Partnership for the Interdisciplinary Study of Coastal Oceans; Myers Trust; Explorer's Club Exploration Fund; Lerner Gray Memorial Fund of the American Museum of Natural History; Vice Provost for Graduate Education at Stanford; Eugene C. and Aileen E. Haderlie Memorial Fund; National Science Foundation [1210057]; National Defense Science and Engineering Grant; Stanford Graduate Fellowship; Stanford Center for Computational, Evolutionary, and Human Genomics Fellowship; Smithsonian Institution Biodiversity Genomics Fellowship FX We sincerely thank John Lee; the Bamfield Marine Centre; Greg Ruiz and the Smithsonian Environmental Research Center; the Rutgers University Marine Field Station; the Darling Marine Center; Iain McGaw and the Ocean Sciences Centre; Joao Canning-Clode and the Laboratorio Maritimo da Guia; and Henrik Glenner and the Espegrend Marine Biological Station. We are grateful for support from the Partnership for the Interdisciplinary Study of Coastal Oceans, the Myers Trust, the Explorer's Club Exploration Fund, the Lerner Gray Memorial Fund of the American Museum of Natural History, the Vice Provost for Graduate Education at Stanford, the Eugene C. and Aileen E. Haderlie Memorial Fund, and a National Science Foundation Doctoral Dissertation Improvement Grant (1210057). CKT was supported on this project by a National Defense Science and Engineering Grant, a Stanford Graduate Fellowship, and a Stanford Center for Computational, Evolutionary, and Human Genomics Fellowship; she is currently supported by a Smithsonian Institution Biodiversity Genomics Fellowship. We also thank two anonymous reviewers for their thoughtful comments which significantly improved this manuscript. NR 83 TC 7 Z9 7 U1 7 U2 62 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 AUG PY 2015 VL 24 IS 16 BP 4145 EP 4158 DI 10.1111/mec.13294 PG 14 WC Biochemistry & Molecular Biology; Ecology; Evolutionary Biology SC Biochemistry & Molecular Biology; Environmental Sciences & Ecology; Evolutionary Biology GA CO7QM UT WOS:000359355900008 PM 26118396 ER PT J AU Christopher Monckton Brenchley Soon, WWH Legates, DR Briggs, WM AF Christopher Monckton Brenchley Soon, Willie W. -H. Legates, David R. Briggs, William M. TI Keeping it simple: the value of an irreducibly simple climate model SO SCIENCE BULLETIN LA English DT Article DE Climate change; Climate sensitivity; Climate models; Global warming; Temperature feedbacks ID PALEOCENE THERMAL MAXIMUM; SENSITIVITY; TRENDS; TEMPERATURES; VARIABILITY; PREDICTION AB Richardson et al. (Sci Bull, 2015. doi:10.1007/s11434-015-0806-z) suggest that the irreducibly simple climate model described in Monckton of Brenchley et al. (Sci Bull 60:122-135, 2015. doi:10.1007/s11434-014-0699-2) was not validated against observations, relying instead on synthetic test data based on underestimated global warming, illogical parameter choice and near-instantaneous response at odds with ocean warming and other observations. However, the simple model, informed by its authors' choice of parameters, usually hindcasts observed temperature change more closely than the general-circulation models, and finds high climate sensitivity implausible. With IPCC's choice of parameters, the model is further validated in that it duly replicates IPCC's sensitivity interval. Also, fast climate system response is consistent with near-zero or net-negative temperature feedback. Given the large uncertainties in the initial conditions and evolutionary processes determinative of climate sensitivity, subject to obvious caveats a simple sensitivity-focused model need not, and the present model does not, exhibit significantly less predictive skill than the general-circulation models. C1 [Christopher Monckton Brenchley] Sci & Publ Policy Inst, Haymarket, VA 20169 USA. [Soon, Willie W. -H.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Legates, David R.] Univ Delaware, Dept Geog, Newark, DE 19716 USA. RP Christopher Monckton Brenchley (reprint author), Sci & Publ Policy Inst, Haymarket, VA 20169 USA. EM monckton@mail.com NR 74 TC 0 Z9 0 U1 2 U2 10 PU SCIENCE PRESS PI BEIJING PA 16 DONGHUANGCHENGGEN NORTH ST, BEIJING 100717, PEOPLES R CHINA SN 2095-9273 EI 2095-9281 J9 SCI BULL JI Sci. Bull. PD AUG PY 2015 VL 60 IS 15 BP 1378 EP 1390 DI 10.1007/s11434-015-0856-2 PG 13 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA CP0HY UT WOS:000359557600010 ER PT J AU Bayliss, D Hartman, JD Bakos, GA Penev, K Zhou, G Brahm, R Rabus, M Jordan, A Mancini, L de Val-Borro, M Bhatti, W Espinoza, N Csubry, Z Howard, AW Fulton, BJ Buchhave, LA Henning, T Schmidt, B Ciceri, S Noyes, RW Isaacson, H Marcy, GW Suc, V Lazar, J Papp, I Sari, P AF Bayliss, D. Hartman, J. D. Bakos, G. A. Penev, K. Zhou, G. Brahm, R. Rabus, M. Jordan, A. Mancini, L. de Val-Borro, M. Bhatti, W. Espinoza, N. Csubry, Z. Howard, A. W. Fulton, B. J. Buchhave, L. A. Henning, T. Schmidt, B. Ciceri, S. Noyes, R. W. Isaacson, H. Marcy, G. W. Suc, V. Lazar, J. Papp, I. Sari, P. TI HATS-8b: A LOW-DENSITY TRANSITING SUPER-NEPTUNE SO ASTRONOMICAL JOURNAL LA English DT Article DE planetary systems; stars: individual (HATS-8); techniques: photometric; techniques: spectroscopic ID HOT JUPITERS; K STAR; MASS; STELLAR; EXOPLANETS; TELESCOPE; PLANETS; KEPLER; FIELD; POPULATION AB HATS-8b is a low density transiting super-Neptune discovered as part of the HATSouth project. The planet orbits its solar-like G-dwarf host (V = 14.03 +/- 0.10, T-eff = 5679 +/- 50 K) with a period of 3.5839 days. HATS-8b is the third lowest-mass transiting exoplanet to be discovered from a wide-field ground-based search, and with a mass of 0.138 +/- 0.019 M-J it is approximately halfway between the masses of Neptune and Saturn. However, HATS-8b has a radius of 0.873(-0.075)(+0.123) R-J, resulting in a bulk density of just 0.259 +/- 0.091 g cm(-3). The metallicity of the host star is super-solar ([Fe/H] = 0.210 +/- 0.080), providing evidence against the idea that low-density exoplanets form from metal-poor environments. The low density and large radius of HATS-8b results in an atmospheric scale height of almost 1000 km, and in addition to this there is an excellent reference star of nearly equal magnitude at just 19 '' separation in the sky. These factors make HATS-8b an exciting target for future atmospheric characterization studies, particularly for long-slit transmission spectroscopy. C1 [Bayliss, D.; Zhou, G.] Univ Geneva, Observ Astronom, CH-1290 Versoix, Switzerland. [Bayliss, D.; Schmidt, B.] Australian Natl Univ, Res Sch Astron & Astrophys, Canberra, ACT 2611, Australia. [Hartman, J. D.; Bakos, G. A.; Penev, K.; de Val-Borro, M.; Bhatti, W.; Csubry, Z.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. [Brahm, R.; Rabus, M.; Jordan, A.; Espinoza, N.; Suc, V.] Catholic Univ Chile, Fac Fis, Inst Astrofis, Santiago 7820436, Chile. [Brahm, R.; Jordan, A.; Espinoza, N.] Millennium Inst Astrophys, Santiago 7820436, Chile. [Rabus, M.; Henning, T.; Ciceri, S.] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Howard, A. W.; Fulton, B. J.] Univ Hawaii Manoa, Inst Astron, Honolulu, HI 96822 USA. [Buchhave, L. A.; Noyes, R. W.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Buchhave, L. A.] Univ Copenhagen, Nat Hist Museum Denmark, Ctr Star & Planet Format, DK-1350 Copenhagen, Denmark. [Isaacson, H.; Marcy, G. W.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Lazar, J.; Papp, I.; Sari, P.] Hungarian Astron Assoc, Budapest, Hungary. RP Bayliss, D (reprint author), Univ Geneva, Observ Astronom, 51 Ch Maillettes, CH-1290 Versoix, Switzerland. EM daniel.bayliss@unige.ch; rbrahm@astro.puc.cl OI Jordan, Andres/0000-0002-5389-3944; Penev, Kaloyan/0000-0003-4464-1371; Schmidt, Brian/0000-0001-6589-1287; Bakos, Gaspar/0000-0001-7204-6727; Buchhave, Lars A./0000-0003-1605-5666; Hartman, Joel/0000-0001-8732-6166 FU NSF MRI [NSF/AST-0723074]; NASA [NNX09AB29G/NNX12AH91H, NNX13AQ62G]; internal Princeton funds; FONDECYT [1130857]; BASAL CATA [PFB-06]; "Millennium Institute of Astrophysics (MAS)" of the Millennium Science Initiative, Chilean Ministry of Economy [IC120009]; CONICYT-PCHA/Doctorado Nacional; NSF Graduate Research Fellowship [2014184874]; Chilean Telescope Allocation Committee (CNTAC) [CN2012A-61, CN2013A-171, CN2014A-104]; W. M. Keck Foundation; ARC Laureate Fellowship [FL0992131]; National Aeronautics and Space Administration; [NSF/AST-1108686] FX Development of the HATSouth project was funded by NSF MRI grant NSF/AST-0723074; operations have been supported by NASA grants NNX09AB29G/NNX12AH91H and internal Princeton funds. Follow-up observations receive partial support from grant NSF/AST-1108686. A.J. acknowledges support from FONDECYT project 1130857, BASAL CATA PFB-06, and project IC120009 "Millennium Institute of Astrophysics (MAS)" of the Millennium Science Initiative, Chilean Ministry of Economy. R.B. and N.E. are supported by CONICYT-PCHA/Doctorado Nacional. R.B. and N.E. acknowledge additional support from project IC120009 "Millennium Institute of Astrophysics (MAS)" of the Millennium Science Initiative, Chilean Ministry of Economy. V.S. acknowledges support form BASAL CATA PFB-06. K.P. acknowledges support from NASA grant NNX13AQ62G. B.J.F. acknowledges support from the NSF Graduate Research Fellowship grant No. 2014184874. Any opinions, findings, and conclusions or recommendations expressed in this material are those of the authors and do not necessarily reflect the views of the National Science Foundation. Operations at the MPG 2.2m Telescope are jointly performed by the Max Planck Gesellschaft and the European Southern Observatory. This work is based on observations made with ESO Telescopes at the La Silla Observatory. Observations from the du Pont and Swope telescopes were taken as part of programs CN2012A-61, CN2013A-171, and CN2014A-104, awarded by the Chilean Telescope Allocation Committee (CNTAC). This paper also uses observations obtained using the facilities of the Las Cumbres Observatory Global Telescope. The radial velocity data presented herein were obtained at the W.M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California, and the National Aeronautics and Space Administration. The Observatory was made possible by the generous financial support of the W.M. Keck Foundation. The authors 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. Work at the Australian National University is supported by the ARC Laureate Fellowship grant FL0992131. This research has made use of the NASA Exoplanet Archive, which is operated by the California Institute of Technology under contract with the National Aeronautics and Space Administration under the Exoplanet Exploration Program. NR 38 TC 8 Z9 8 U1 1 U2 12 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 AUG PY 2015 VL 150 IS 2 AR 49 DI 10.1088/0004-6256/150/2/49 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CO0QL UT WOS:000358856900010 ER PT J AU Jenkins, JM Twicken, JD Batalha, NM Caldwell, DA Cochran, WD Endl, M Latham, DW Esquerdo, GA Seader, S Bieryla, A Petigura, E Ciardi, DR Marcy, GW Isaacson, H Huber, D Rowe, JF Torres, G Bryson, ST Buchhave, L Ramirez, I Wolfgang, A Li, J Campbell, JR Tenenbaum, P Sanderfer, D Henze, CE Catanzarite, JH Gilliland, RL Borucki, WJ AF Jenkins, Jon M. Twicken, Joseph D. Batalha, Natalie M. Caldwell, Douglas A. Cochran, William D. Endl, Michael Latham, David W. Esquerdo, Gilbert A. Seader, Shawn Bieryla, Allyson Petigura, Erik Ciardi, David R. Marcy, Geoffrey W. Isaacson, Howard Huber, Daniel Rowe, Jason F. Torres, Guillermo Bryson, Stephen T. Buchhave, Lars Ramirez, Ivan Wolfgang, Angie Li, Jie Campbell, Jennifer R. Tenenbaum, Peter Sanderfer, Dwight Henze, Christopher E. Catanzarite, Joseph H. Gilliland, Ronald L. Borucki, William J. TI DISCOVERY AND VALIDATION OF Kepler-452b: A 1.6 R phi SUPER EARTH EXOPLANET IN THE HABITABLE ZONE OF A G2 STAR SO ASTRONOMICAL JOURNAL LA English DT Article DE methods: statistical; planets and satellites: detection; stars: fundamental parameters; stars: individual (Kepler-452b, KIC 8311864, KOI7016.01) ID POTENTIAL TRANSIT SIGNALS; FALSE POSITIVES; MISSION DATA; SOPHIE VELOCIMETRY; EXTRASOLAR PLANETS; BLEND SCENARIOS; Y-2 ISOCHRONES; HARPS SEARCH; MILKY-WAY; SYSTEM AB We report on the discovery and validation of Kepler-452b, a transiting planet identified by a search through the 4 years of data collected by NASA's Kepler Mission. This possibly rocky 1.63(-0.20)(+0.23) R-circle plus every 384.843 (+0.007)(-0.012) days, the longest orbital period for a small (R-P < 2 R-circle plus) transiting exoplanet to date. The likelihood that this planet has a rocky composition lies between 49% and 62%. The star has an effective temperature of 5757 +/- 85 K and a log g of 4.32 +/- 0.09. At a mean orbital separation of 1.046 (-0.015) (+0.019) AU, this small planet is well within the optimistic habitable zone of its star (recent Venus/early Mars), experiencing only 10% more flux than Earth receives from the Sun today, and slightly outside the conservative habitable zone (runaway greenhouse/maximum greenhouse). The star is slightly larger and older than the Sun, with a present radius of 1.11 (-0.09) (+0.15) R-circle dot and an estimated age of similar to 6 Gyr. Thus, Kepler-452b has likely always been in the habitable zone and should remain there for another similar to 3 Gyr. C1 [Jenkins, Jon M.; Twicken, Joseph D.; Batalha, Natalie M.; Caldwell, Douglas A.; Seader, Shawn; Rowe, Jason F.; Bryson, Stephen T.; Li, Jie; Tenenbaum, Peter; Sanderfer, Dwight; Henze, Christopher E.; Catanzarite, Joseph H.; Borucki, William J.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Twicken, Joseph D.; Caldwell, Douglas A.; Seader, Shawn; Huber, Daniel; Rowe, Jason F.; Li, Jie; Tenenbaum, Peter; Catanzarite, Joseph H.] SETI Inst, Mountain View, CA 94043 USA. [Cochran, William D.; Endl, Michael; Ramirez, Ivan] Univ Texas Austin, McDonald Observ, Austin, TX 78712 USA. [Cochran, William D.; Endl, Michael; Ramirez, Ivan] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA. [Latham, David W.; Esquerdo, Gilbert A.; Bieryla, Allyson; Torres, Guillermo; Buchhave, Lars] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Petigura, Erik; Marcy, Geoffrey W.; Isaacson, Howard] Univ Calif Berkeley, Berkeley, CA 94720 USA. [Ciardi, David R.] CALTECH, NASA, Exoplanet Sci Inst, Pasadena, CA 91125 USA. [Huber, Daniel] Univ Sydney, Sch Phys, Sydney Inst Astron SIfA, Sydney, NSW 2006, Australia. [Huber, Daniel] Aarhus Univ, Dept Phys & Astron, Stellar Astrophys Ctr, DK-8000 Aarhus C, Denmark. [Buchhave, Lars] Univ Copenhagen, Nat Hist Museum Denmark, Ctr Star & Planet Format, DK-1350 Copenhagen, Denmark. [Wolfgang, Angie] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. [Campbell, Jennifer R.] NASA, Wyle Labs, Ames Res Ctr, Moffett Field, CA 94035 USA. [Gilliland, Ronald L.] Penn State Univ, Ctr Exoplanets & Habitable Worlds, University Pk, PA 16802 USA. RP Jenkins, JM (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. EM Jon.Jenkins@nasa.gov NR 89 TC 32 Z9 36 U1 18 U2 61 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 AUG PY 2015 VL 150 IS 2 AR 56 DI 10.1088/0004-6256/150/2/56 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CO0QL UT WOS:000358856900017 ER PT J AU Johnson, CI Rich, RM Pilachowski, CA Caldwell, N Mateo, M Bailey, JI Crane, JD AF Johnson, Christian I. Rich, R. Michael Pilachowski, Catherine A. Caldwell, Nelson Mateo, Mario Bailey, John I., III Crane, Jeffrey D. TI A SPECTROSCOPIC ANALYSIS OF THE GALACTIC GLOBULAR CLUSTER NGC 6273 (M19) SO ASTRONOMICAL JOURNAL LA English DT Article DE globular clusters: general; globular clusters: individual (NGC 6273, M19); stars: abundances ID MULTIPLE STELLAR POPULATIONS; METAL-POOR STARS; HUBBLE-SPACE-TELESCOPE; RED GIANT BRANCH; DWARF SPHEROIDAL GALAXY; MILKY-WAY BULGE; SODIUM-ABUNDANCE VARIATIONS; SELF-ENRICHMENT SCENARIO; NEUTRON-CAPTURE ELEMENTS; COLOR-MAGNITUDE DIAGRAMS AB A combined effort utilizing spectroscopy and photometry has revealed the existence of a new globular cluster class. These "anomalous" clusters, which we refer to as "iron-complex" clusters, are differentiated from normal clusters by exhibiting large (greater than or similar to 0.10 dex) intrinsic metallicity dispersions, complex sub-giant branches, and correlated [Fe/H] and s-process enhancements. In order to further investigate this phenomenon, we have measured radial velocities and chemical abundances for red giant branch stars in the massive, but scarcely studied, globular cluster NGC 6273. The velocities and abundances were determined using high resolution (R similar to 27,000) spectra obtained with the Michigan/Magellan Fiber System (M2FS) and MSpec spectrograph on the Magellan-Clay 6.5 m telescope at Las Campanas Observatory. We find that NGC 6273 has an average heliocentric radial velocity of +144.49 km s(-1) (sigma = 9.64 km s(-1)) and an extended metallicity distribution ([Fe/H] = -1.80 to -1.30) composed of at least two distinct stellar populations. Although the two dominant populations have similar [Na/Fe], [Al/Fe], and [alpha/Fe] abundance patterns, the more metal-rich stars exhibit significant [La/Fe] enhancements. The [La/Eu] data indicate that the increase in [La/Fe] is due to almost pure s-process enrichment. A third more metal-rich population with low [X/Fe] ratios may also be present. Therefore, NGC 6273 joins clusters such as omega Centauri, M2, M22, and NGC 5286 as a new class of iron-complex clusters exhibiting complicated star formation histories. C1 [Johnson, Christian I.; Caldwell, Nelson] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Rich, R. Michael] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. [Pilachowski, Catherine A.] Indiana Univ, Dept Astron, Bloomington, IN 47405 USA. [Mateo, Mario; Bailey, John I., III] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Crane, Jeffrey D.] Observ Carnegie Inst Sci, Pasadena, CA 91101 USA. RP Johnson, CI (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS-15, Cambridge, MA 02138 USA. EM cjohnson@cfa.harvard.edu; rmr@astro.ucla.edu; catyp@astro.indiana.edu; ncaldwell@cfa.harvard.edu; mmateo@umich.edu; baileyji@umich.edu; crane@obs.carnegiescience.edu OI Pilachowski, Catherine/0000-0002-3007-206X FU National Aeronautics and Space Administration; National Science Foundation [AST-1413755, AST-1412673, AST-0923160]; Clay Fellowship; Daniel Kirkwood Research Fund at Indiana University FX This research has made use of NASA's Astrophysics Data System Bibliographic Services. This publication has made use of data products from the 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. C.I.J. gratefully acknowledges support from the Clay Fellowship, administered by the Smithsonian Astrophysical Observatory. R.M.R. acknowledges support from the National Science Foundation (AST-1413755 and AST-1412673). C.A.P. gratefully acknowledges support from the Daniel Kirkwood Research Fund at Indiana University and from the National Science Foundation (AST-1412673). M.M. is grateful for support from the National Science Foundation to develop M2FS (AST-0923160) and carry out the observations reported here (AST-1312997), and to the University of Michigan for its direct support of M2FS construction and operation. NR 176 TC 11 Z9 11 U1 2 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 EI 1538-3881 J9 ASTRON J JI Astron. J. PD AUG PY 2015 VL 150 IS 2 AR 63 DI 10.1088/0004-6256/150/2/63 PG 21 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CO0QL UT WOS:000358856900024 ER PT J AU Young, KE Young, CH Lai, SP Dunham, MM Evans, NJ AF Young, Kaisa E. Young, Chadwick H. Lai, Shih-Ping Dunham, Michael M. Evans, Neal J., II TI THE SPITZER c2d SURVEY OF LARGE, NEARBY, INTERSTELLAR CLOUDS. XII. THE PERSEUS YSO POPULATION AS OBSERVED WITH IRAC AND MIPS SO ASTRONOMICAL JOURNAL LA English DT Article DE dust, extinction; infrared: stars; ISM: individual objects (IC 348, NGC 1333 Perseus); stars: formation ID STAR-FORMING REGIONS; 1ST HYDROSTATIC CORE; YOUNG STELLAR POPULATION; MOLECULAR CLOUD; LEGACY CLOUDS; SPACE-TELESCOPE; DISK POPULATION; FORMATION RATES; COLUMN DENSITY; H2O MASERS AB The Spitzer Space Telescope mapped the Perseus molecular cloud complex with the Infrared Array Camera (IRAC) and the Multi-Band Imaging Photometer for Spitzer (MIPS) as part of the c2d Spitzer Legacy project. This paper combines the observations from both instruments giving an overview of low-mass star formation across Perseus from 3.6 to 70 mu m. We provide an updated list of young stellar objects (YSOs) with new classifications and source fluxes from previous works, identifying 369 YSOs in Perseus with the Spitzer data set. By synthesizing the IRAC and MIPS maps of Perseus and building on the work of previous papers in this series, we present a current census of star formation across the cloud and within smaller regions. Sixty-seven percent of the YSOs are associated with the young clusters NGC 1333 and IC 348. The majority of the star formation activity in Perseus occurs in the regions around the clusters to the eastern and western ends of the cloud complex. The middle of the cloud is nearly empty of YSOs despite containing regions of high visual extinction. The western half of Perseus contains three-quarters of the total number of embedded YSOs (Class 0+I and Flat spectral energy distribution sources) in the cloud and nearly as many embedded YSOs as Class II and III sources. Class II and III objects greatly outnumber Class 0+I objects in eastern Perseus and IC 348. These results are consistent with previous age estimates for the clusters. Across the cloud, 56% of YSOs and 91% of the Class 0+I and Flat sources are in areas where A(v) >= 5 mag, indicating a possible extinction threshold for star formation. C1 [Young, Kaisa E.; Young, Chadwick H.] Nicholls State Univ, Dept Phys Sci, Thibodaux, LA 70310 USA. [Lai, Shih-Ping] Natl Tsing Hua Univ, Inst Astron, Hsinchu 30013, Taiwan. [Lai, Shih-Ping] Natl Tsing Hua Univ, Dept Phys, Hsinchu 30013, Taiwan. [Dunham, Michael M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Evans, Neal J., II] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA. RP Young, KE (reprint author), Nicholls State Univ, Dept Phys Sci, POB 2022, Thibodaux, LA 70310 USA. EM kaisa.young@nicholls.edu; chad.young@nicholls.edu; slai@phys.nthu.edu.tw; mdunham@cfa.harvard.edu; nje@astro.as.utexas.edu FU Spitzer Legacy Science Program; NASA [1224608, 1230782, 1230779, 1407]; Louisiana Space Consortium Research Enhancement Award through NASA EPSCoR [NNX10AI40H]; Submillimeter Array through an SMA postdoctoral fellowship; National Science Foundation [AST-1109116] FX Support for this work, part of the Spitzer Legacy Science Program, was provided by NASA through contracts 1224608, 1230782, and 1230779 issued by the Jet Propulsion Laboratory, California Institute of Technology, under NASA contract 1407. K.E.Y. and C.H.Y. acknowledge support from a Louisiana Space Consortium Research Enhancement Award through NASA EPSCoR grant number NNX10AI40H. M.M. D. acknowledges support from the Submillimeter Array through an SMA postdoctoral fellowship. N.J.E. acknowledges support from a grant from the National Science Foundation, AST-1109116. We would like to thank the anonymous referee for comments that improved the focus and clarity of this work. NR 68 TC 8 Z9 8 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 EI 1538-3881 J9 ASTRON J JI Astron. J. PD AUG PY 2015 VL 150 IS 2 AR 40 DI 10.1088/0004-6256/150/2/40 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CO0QL UT WOS:000358856900001 ER PT J AU Garcia, JA Dauser, T Steiner, JF McClintock, JE Keck, ML Wilms, J AF Garcia, Javier A. Dauser, Thomas Steiner, James F. McClintock, Jeffrey E. Keck, Mason L. Wilms, Joern TI ON ESTIMATING THE HIGH-ENERGY CUTOFF IN THE X-RAY SPECTRA OF BLACK HOLES VIA REFLECTION SPECTROSCOPY SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE accretion, accretion disks; atomic processes; black hole physics ID ACCRETION DISK; COMPTONIZATION MODELS; NUSTAR; LINE; GALAXIES; SPIN; OSSE AB The fundamental parameters describing the coronal spectrum of an accreting black hole are the slope Gamma of the power-law continuum and the energy E-cut at which it rolls over. Remarkably, this latter parameter can be accurately measured for values as high as 1 MeV by modeling the spectrum of X-rays reflected from a black hole accretion disk at energies below 100 keV. This is possible because the details in the reflection spectrum, rich in fluorescent lines and other atomic features, are very sensitive to the spectral shape of the hardest coronal radiation illuminating the disk. We show that by fitting simultaneous NuSTAR (3-79 keV) and low-energy (e.g., Suzaku) data with the most recent version of our reflection model relxill one can obtain reasonable constraints on E-cut at energies from tens of keV up to 1 MeV, for a source as faint as 1 mCrab in a 100 ks observation. C1 [Garcia, Javier A.; Steiner, James F.; McClintock, Jeffrey E.; Keck, Mason L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Dauser, Thomas; Wilms, Joern] Dr Karl Remeis Observ, D-96049 Bamberg, Germany. [Dauser, Thomas; Wilms, Joern] Erlangen Ctr Astroparticle Phys, D-96049 Bamberg, Germany. [Keck, Mason L.] Boston Univ, Inst Astrophys Res, Boston, MA 02215 USA. RP Garcia, JA (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; jsteiner@head.cfa.harvard.edu; keckm@bu.edu RI Wilms, Joern/C-8116-2013; XRAY, SUZAKU/A-1808-2009; OI Wilms, Joern/0000-0003-2065-5410; Garcia, Javier/0000-0003-3828-2448 FU NASA [NNX11AD08G, HST-HF-51315.01] FX J.G. and J.E.M. acknowledge the support of NASA grant NNX11AD08G. J.F.S. has been supported by NASA Hubble Fellowship HST-HF-51315.01. NR 32 TC 7 Z9 7 U1 0 U2 1 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 AUG 1 PY 2015 VL 808 IS 2 AR L37 DI 10.1088/2041-8205/808/2/L37 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CO1TS UT WOS:000358938800005 ER PT J AU Lee, PC Wildt, DE Comizzoli, P AF Lee, Pei-Chih Wildt, David E. Comizzoli, Pierre TI Nucleolar Translocation of Histone Deacetylase 2 Is Involved in Regulation of Transcriptional Silencing in the Cat Germinal Vesicle SO BIOLOGY OF REPRODUCTION LA English DT Article DE domestic cat; gamete biology; germinal vesicle; oocyte; transcription ID IN-VITRO MATURATION; DEVELOPMENTAL COMPETENCE; OOCYTE GROWTH; CHROMATIN CONFIGURATIONS; MEIOTIC COMPETENCE; BOVINE OOCYTES; MOUSE OOCYTES; DOMESTIC CAT; FERTILITY PRESERVATION; RIBOSOME BIOGENESIS AB Histone deacetylase 2 (HDAC2) is a key transcriptional coregulator that is suspected to play a role during oogenesis. It is known that RNA transcription in the cat germinal vesicle (GV) stops during folliculogenesis at the late antral follicle stage and is unrelated to histone deacetylation or chromatin condensation. The objective of the present study was to determine if and how HDAC2 participates in transcription regulation in the cat GV. Spatiotemporal HDAC2 protein expression was examined by immunostaining oocytes from primary to large antral follicles. HDAC2 was detected in the majority of GVs within oocytes from early, small, and large antral follicles. At early and small antral stages, HDAC2 was found primarily in the GV's nucleoplasm. There then was a significant shift in HDAC2 localization into the nucleolus, mostly in oocytes from large antral follicles. Assessments revealed that transcription was active in oocytes that contained nucleoplasm-localized HDAC2, whereas nucleolar-bound HDAC2 was associated with loss of both global transcription and ribosomal RNA presence at all antral stages. When oocytes were exposed to the HDAC inhibitor valproic acid, results indicated that HDAC regulated transcriptional activity in the nucleoplasm, but not in the nucleolus. Collective results suggest that nucleolar translocation of HDAC2 is associated with transcriptional silencing in the GV, thereby likely contributing to an oocyte's acquisition of competence. C1 Smithsonian Conservat Biol Inst, Ctr Species Survival, Washington, DC 20013 USA. Smithsonian Conservat Biol Inst, Ctr Species Survival, 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, a component of the National Institutes of Health (NIH) [R01 RR026064]; Office of Research Infrastructure Programs/Office of the Director [R01 OD010948] FX Supported by the National Center for Research Resources (R01 RR026064), a component of the National Institutes of Health (NIH), and currently by the Office of Research Infrastructure Programs/Office of the Director (R01 OD010948). NR 61 TC 3 Z9 3 U1 2 U2 5 PU SOC STUDY REPRODUCTION PI MADISON PA 1691 MONROE ST,SUITE # 3, MADISON, WI 53711-2021 USA SN 0006-3363 EI 1529-7268 J9 BIOL REPROD JI Biol. Reprod. PD AUG 1 PY 2015 VL 93 IS 2 AR 33 DI 10.1095/biolreprod.115.129106 PG 9 WC Reproductive Biology SC Reproductive Biology GA CO8UT UT WOS:000359448300008 PM 26108793 ER PT J AU Jacquet, J Estes, J Jackson, J Johnson, AE Knowlton, N Mcclenachan, L Pauly, D Sala, E AF Jacquet, Jennifer Estes, James Jackson, Jeremy Johnson, Ayana E. Knowlton, Nancy Mcclenachan, Loren Pauly, Daniel Sala, Enric TI Ocean Calamities: Hyped Litany or Legitimate Concern? SO BIOSCIENCE LA English DT Letter ID EUTROPHICATION; FISHERIES C1 [Jacquet, Jennifer] NYU, Dept Environm Studies, New York, NY 10003 USA. [Estes, James] Univ Calif Santa Cruz, Dept Ecol & Evolutionary Biol, Santa Cruz, CA 95064 USA. [Jackson, Jeremy] Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20560 USA. [Jackson, Jeremy] Univ Calif San Diego, Scripps Inst Oceanog, San Diego, CA 92103 USA. [Johnson, Ayana E.] Waitt Inst, Washington, DC USA. [Knowlton, Nancy] Natl Museum Nat Hist, Washington, DC 20560 USA. [Mcclenachan, Loren] Colby Coll, Dept Environm Studies, Waterville, ME 04901 USA. [Pauly, Daniel] Univ British Columbia, Sea Us, Vancouver, BC V5Z 1M9, Canada. [Sala, Enric] Natl Geog Soc, Washington, DC USA. RP Jacquet, J (reprint author), NYU, Dept Environm Studies, New York, NY 10003 USA. EM jacquet@nyu.edu NR 8 TC 2 Z9 2 U1 4 U2 29 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0006-3568 EI 1525-3244 J9 BIOSCIENCE JI Bioscience PD AUG PY 2015 VL 65 IS 8 BP 745 EP 746 DI 10.1093/biosci/biv087 PG 2 WC Biology SC Life Sciences & Biomedicine - Other Topics GA CO5FA UT WOS:000359183800002 ER PT J AU Pistone, M Arzilli, F Dobson, KJ Cordonnier, B Reusser, E Ulmer, P Marone, F Whittington, AG Mancini, L Fife, JL Blundy, JD AF Pistone, Mattia Arzilli, Fabio Dobson, Katherine J. Cordonnier, Benoit Reusser, Eric Ulmer, Peter Marone, Federica Whittington, Alan G. Mancini, Lucia Fife, Julie L. Blundy, Jonathan D. TI Gas-driven filter pressing in magmas: Insights into in-situ melt segregation from crystal mushes SO GEOLOGY LA English DT Article ID GENERATION; RHEOLOGY; SYSTEM AB Gas-driven filter pressing is the process of melt expulsion from a volatile-saturated crystal mush, induced by the buildup and subsequent release of gas pressure. Filter pressing is inferred to play a major role in magma fractionation at shallow depths (<10 km) by moving melt and gas relative to the solid, crystalline framework. However, the magmatic conditions at which this process operates remain poorly constrained. We present novel experimental data that illustrate how the crystal content of the mush affects the ability of gas-driven filter pressing to segregate melt. Hydrous haplogranite (2.1 wt% water in the melt) and dacite (4.2 wt% water in the melt) crystal mushes, with a wide range of crystallinities (34-80 vol% crystals), were investigated using in-situ, high-temperature (500-800 degrees C) synchrotron X-ray tomographic microscopy with high spatial (3 mm/pixel) and temporal resolution (similar to 8 s per three-dimensional data set). Our experimental results show that gas-driven filter pressing operates only below the maximum packing of bubbles and crystals (similar to 74 vol%). Above this threshold, the mush tends to fracture and gas escapes via fractures. Therefore, the efficiency of gas-driven filter pressing is promoted close to the percolation threshold and in situations where a mush inflates slowly relative to build-up of pressure and expulsion of melt. Such observations offer a likely explanation for the production of eruptible, crystal-poor magmas within Earth's crust. C1 [Pistone, Mattia] Smithsonian Inst, Natl Museum Nat Hist, Dept Mineral Sci, Washington, DC 20560 USA. [Pistone, Mattia; Blundy, Jonathan D.] Univ Bristol, Sch Earth Sci, Bristol BS8 1RJ, Avon, England. [Arzilli, Fabio; Mancini, Lucia] Elettra Sincrotrone Trieste SCpA, I-34149 Basovizza, Italy. [Arzilli, Fabio] Ist Nazl Geofis & Vulcanol, Sez Pisa, I-56126 Pisa, Italy. [Dobson, Katherine J.] Univ Munich, Dept Earth & Environm Sci, D-80333 Munich, Germany. [Reusser, Eric; Ulmer, Peter] ETH, Dept Earth Sci, CH-8092 Zurich, Switzerland. [Marone, Federica; Fife, Julie L.] Paul Scherrer Inst, Swiss Light Source, CH-5232 Villigen, Switzerland. [Whittington, Alan G.] Univ Missouri, Dept Geol Sci, Geol Sci 101, Columbia, MO 65211 USA. RP Pistone, M (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Mineral Sci, 10th St & Constitut Ave NW, Washington, DC 20560 USA. RI Marone, Federica/J-4420-2013; Dobson, Katherine/I-1223-2016; OI Dobson, Katherine/0000-0003-2272-626X; Mancini, Lucia/0000-0003-2416-3464; Pistone, Mattia/0000-0001-7560-3146 FU EU Transnational Access Programme (CALIPSO) [312284]; European Research Council Advanced Grant CRITMAG; EXTREMA European Cooperation in Science and Technology (COST) Action [MP1207] FX The EU Transnational Access Programme (CALIPSO; number 312284; FP7/2007-2013), the European Research Council Advanced Grant CRITMAG, and EXTREMA European Cooperation in Science and Technology (COST) Action MP1207 supported the work. We acknowledge C. Clapham, D. Hawley, U. Graber, G. Mikuljan, and G. Robert for technical support; D. Baker, M. Polacci, L. Caricchi, and D. Giordano for discussions; and R. Holdsworth, D. Floess, and two anonymous reviewers for their helpful comments. NR 18 TC 16 Z9 16 U1 1 U2 12 PU GEOLOGICAL SOC AMER, INC PI BOULDER PA PO BOX 9140, BOULDER, CO 80301-9140 USA SN 0091-7613 EI 1943-2682 J9 GEOLOGY JI Geology PD AUG PY 2015 VL 43 IS 8 BP 699 EP 702 DI 10.1130/G36766.1 PG 4 WC Geology SC Geology GA CO2VK UT WOS:000359014600011 ER PT J AU Bayer, FM Cairns, SD Cordeiro, RTS Perez, CD AF Bayer, Frederick M. Cairns, Stephen D. Cordeiro, Ralf T. S. Perez, Carlos D. TI New records of the genus Callogorgia (Anthozoa: Octocorallia) in the western Atlantic, including the description of a new species SO JOURNAL OF THE MARINE BIOLOGICAL ASSOCIATION OF THE UNITED KINGDOM LA English DT Article DE Deep-water corals; octocorals; Primnoidae; south Atlantic; Cnidaria; continental slope ID GULF-OF-MEXICO; DEEP; SEA AB Based on material collected during oceanographic campaigns in the western Atlantic from 1958 to 2011, two species of primnoid octocorals belonging to the genus Callogorgia were identified: Callogorgia americana and Callogorgia arawak sp. nov. These species are described and illustrated herein and their geographic and bathymetric are given. This is the first record of the genus in the south-western Atlantic. Additionally, the elevation of C. americana americana and C. a. delta to species level is proposed, keeping Callogorgia gilberti, C. delta and C. americana as separate species. C1 [Bayer, Frederick M.; Cairns, Stephen D.] Natl Museum Nat Hist, Smithsonian, Dept Invertebrate Zool, Washington, DC 20560 USA. [Cordeiro, Ralf T. S.] Univ Fed Pernambuco, Posgrad Biol Anim, BR-50670901 Recife, PE, Brazil. [Perez, Carlos D.] Univ Fed Pernambuco, Ctr Acad Vitoria, BR-55608680 Bela Vista, Vitoria de Sant, Brazil. RP Cordeiro, RTS (reprint author), Univ Fed Pernambuco, Posgrad Biol Anim, BR-50670901 Recife, PE, Brazil. EM ralfts@gmail.com FU CNPq - Conselho Nacional de Desenvolvimento Cientifico e Tecnologico [Edital PROTAX 2010 - 562320/2010-5]; FACEPE - Fundacao de Amparo a Ciencia e Tecnologia do Estado de Pernambuco [APQ-0828-2.04/12] FX The work was supported by CNPq - Conselho Nacional de Desenvolvimento Cientifico e Tecnologico (Grant - Edital PROTAX 2010 - 562320/2010-5) and FACEPE - Fundacao de Amparo a Ciencia e Tecnologia do Estado de Pernambuco (Grant - APQ-0828-2.04/12). NR 16 TC 3 Z9 3 U1 1 U2 6 PU CAMBRIDGE UNIV PRESS PI NEW YORK PA 32 AVENUE OF THE AMERICAS, NEW YORK, NY 10013-2473 USA SN 0025-3154 EI 1469-7769 J9 J MAR BIOL ASSOC UK JI J. Mar. Biol. Assoc. U.K. PD AUG PY 2015 VL 95 IS 5 BP 905 EP 911 DI 10.1017/S0025315414001957 PG 7 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA CO0NJ UT WOS:000358848400005 ER PT J AU Beck, AW Lawrence, DJ Peplowski, PN Prettyman, TH McCoy, TJ McSween, HY Toplis, MJ Yamashita, N AF Beck, Andrew W. Lawrence, David J. Peplowski, Patrick N. Prettyman, Thomas H. McCoy, Timothy J. McSween, Harry Y., Jr. Toplis, Michael J. Yamashita, Naoyuki TI Using HED meteorites to interpret neutron and gamma-ray data from asteroid4 Vesta SO METEORITICS & PLANETARY SCIENCE LA English DT Article ID DAWN MISSION; COLLISIONAL HISTORY; POLYMICT BRECCIAS; LUNAR-SURFACE; PARENT BODY; CONSTRAINTS; HOWARDITE; EUCRITE; CRYSTALLIZATION; SPECTROMETER AB Here, we construct a comprehensive howardite, eucrite, and diogenite (HED) bulk chemistry data set to compare with Dawn data. Using the bulk chemistry data set, we determine four gamma-ray/neutron parameters in the HEDs (1) relative fast neutron counts (fast counts), (2) macroscopic thermal neutron absorption cross section (absorption), (3) a high-energy gamma-ray compositional parameter (C-p), and (4) Fe abundance. These correspond to the four measurements of Vesta made by Dawn's Gamma Ray and Neutron Detector (GRaND) that can be used to discern HED lithologic variability on the Vestan surface. We investigate covariance between fast counts and average atomic mass (< A >) in the meteorite data set, where a strong correlation (r(2)=0.99) is observed, and we demonstrate that systematic offsets from the fast count/< A > trend are linked to changes in Fe and Ni concentrations. To compare the meteorite and GRaND data, we investigate and report covariance among fast counts, absorption, C-p, and Fe abundance in the HED meteorite data set. We identify several GRaND measurement spaces where the Yamato type B diogenites are distinct from all other HED lithologies, including polymict mixtures. The type B's are diogenites that are enriched in Fe+pigeonite+diopside +/- plagioclase, relative to typical, orthopyroxenitic diogenites. We then compare these results to GRaND data and demonstrate that regions north of similar to 70 degrees N latitude on Vesta (including the north pole) are consistent with type B diogenites. We propose two models to explain type B diogenite compositions in the north (1) deposition as Rheasilvia ejecta, or (2) type B plutons that were emplaced at shallow depths in the north polar region and sampled by local impacts. Lastly, using principal component (PC) analysis, we identify unique PC spaces for all HED lithologies, indicating that the corresponding GRaND measurables may be used to produce comprehensive lithologic maps for Vesta. C1 [Beck, Andrew W.; Lawrence, David J.; Peplowski, Patrick N.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. [Prettyman, Thomas H.; Yamashita, Naoyuki] Planetary Sci Inst, Tucson, AZ 85719 USA. [McCoy, Timothy J.] Smithsonian Inst, Dept Mineral Sci, Washington, DC 20560 USA. [McSween, Harry Y., Jr.] Univ Tennessee, Dept Earth & Planetary Sci, Knoxville, TN 37996 USA. [Toplis, Michael J.] Univ Toulouse, UPS OMP, Inst Rech Astrophys & Planetol, F-31400 Toulouse, France. [Toplis, Michael J.] IRAP, CNRS, F-31400 Toulouse, France. RP Beck, AW (reprint author), Johns Hopkins Univ, Appl Phys Lab, Johns Hopkins Rd, Laurel, MD 20723 USA. EM andrew.beck@jhuapl.edu RI Beck, Andrew/J-7215-2015; Peplowski, Patrick/I-7254-2012; Lawrence, David/E-7463-2015; OI Beck, Andrew/0000-0003-4455-2299; Peplowski, Patrick/0000-0001-7154-8143; Lawrence, David/0000-0002-7696-6667; Prettyman, Thomas/0000-0003-0072-2831 FU NASA Discovery Program Office; Dawn at Vesta participating scientist grants FX The Dawn mission is led by the University of California, Los Angeles, and managed by the Jet Propulsion Laboratory (JPL), Pasadena, California under the auspices of the NASA Discovery Program Office. Support for this work was provided by Dawn at Vesta participating scientist grants to DJL and TJM, work by HYM and THP was carried out under contract with the NASA JPL. We thank Christina Viviano-Beck for her help with IDL programming. We also thank Andy Tindle for the use of his element to oxide software, and Nicole Lunning and Sheri Singerling for their assistance in compiling HED data. This manuscript was significantly improved by comments from the reviewer, Tomohiro Usui. NR 59 TC 8 Z9 8 U1 3 U2 7 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1086-9379 EI 1945-5100 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD AUG PY 2015 VL 50 IS 8 BP 1311 EP 1337 DI 10.1111/maps.12467 PG 27 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA CO7QW UT WOS:000359356900001 ER PT J AU Corrigan, CM Lunning, NG Friedrich, JM McCoy, TJ AF Corrigan, C. M. Lunning, N. G. Friedrich, J. M. McCoy, T. J. TI AN H CHONDRITE CLAST IN AN LL CHONDRITE: IMPACT MELT OR INCIPIENT PARTIAL MELT? SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 78th Annual Meeting of the Meteoritical-Society CY JUL 27-31, 2015 CL Berkeley, CA SP Meteorit Soc, Barringer Crater Co, Natl Aeronaut & Space Adm, Inst Space & Astronaut Sci, Japan Aerosp Explorat Agcy, Japan Polar Res Assoc, Natl Inst Polar Res, NASA Mars Program Off, Agilent Technologies, CAMECA, Lockheed Martin Space Syst Co, Natl Electrostat Corp, TESCAN, Int Meteorite Collectors Assoc, Planetary Studies Fdn, Lunar & Planetary Inst, Univ Calif, Space Sci Lab C1 [Corrigan, C. M.; McCoy, T. J.] NMNH, Smithsonian Inst, Washington, DC 20560 USA. [Lunning, N. G.] Univ Tennessee, Knoxville, TN 37996 USA. [Friedrich, J. M.] Fordham Univ, New York, NY 10023 USA. EM corriganc@si.edu NR 18 TC 0 Z9 0 U1 1 U2 1 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1086-9379 EI 1945-5100 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD AUG PY 2015 VL 50 SU 1 SI SI MA 5283.pdf PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA CN7CR UT WOS:000358591900067 ER PT J AU Kita, NT Tenner, TJ Ushikubo, T Bouvier, A Wadhwa, M Bullock, ES MacPherson, GJ AF Kita, N. T. Tenner, T. J. Ushikubo, T. Bouvier, A. Wadhwa, M. Bullock, E. S. MacPherson, G. J. TI WHY DO U-PB AGES OF CHONDRULES AND CAIs HAVE MORE SPREAD THAN THEIR (26)AL AGES? SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 78th Annual Meeting of the Meteoritical-Society CY JUL 27-31, 2015 CL Berkeley, CA SP Meteorit Soc, Barringer Crater Co, Natl Aeronaut & Space Adm, Inst Space & Astronaut Sci, Japan Aerosp Explorat Agcy, Japan Polar Res Assoc, Natl Inst Polar Res, NASA Mars Program Off, Agilent Technologies, CAMECA, Lockheed Martin Space Syst Co, Natl Electrostat Corp, TESCAN, Int Meteorite Collectors Assoc, Planetary Studies Fdn, Lunar & Planetary Inst, Univ Calif, Space Sci Lab ID SOLAR PROTOPLANETARY DISK C1 [Kita, N. T.; Tenner, T. J.] Univ Wisconsin, Madison, WI 53706 USA. [Ushikubo, T.] JAMSTEC, Kochi 7838502, Japan. [Bouvier, A.] Univ Western Ontario, London, ON N6A 3K7, Canada. [Wadhwa, M.] Arizona State Univ, Ctr Meteorite Studies, Tempe, AZ 85287 USA. [Bullock, E. S.; MacPherson, G. J.] Smithsonian Inst, Washington, DC 20560 USA. EM noriko@geology.wisc.edu NR 10 TC 0 Z9 0 U1 1 U2 2 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1086-9379 EI 1945-5100 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD AUG PY 2015 VL 50 SU 1 SI SI MA 5360.pdf PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA CN7CR UT WOS:000358591900166 ER PT J AU Mayne, RG Mccoy, TJ AF Mayne, R. G. McCoy, T. J. TI PALLASITES: DOES DENSITY MATTER AFTER ALL? SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 78th Annual Meeting of the Meteoritical-Society CY JUL 27-31, 2015 CL Berkeley, CA SP Meteorit Soc, Barringer Crater Co, Natl Aeronaut & Space Adm, Inst Space & Astronaut Sci, Japan Aerosp Explorat Agcy, Japan Polar Res Assoc, Natl Inst Polar Res, NASA Mars Program Off, Agilent Technologies, CAMECA, Lockheed Martin Space Syst Co, Natl Electrostat Corp, TESCAN, Int Meteorite Collectors Assoc, Planetary Studies Fdn, Lunar & Planetary Inst, Univ Calif, Space Sci Lab C1 [Mayne, R. G.] Texas Christian Univ, Monnig Meteorite Collect, Ft Worth, TX 76109 USA. [McCoy, T. J.] Natl Museum Nat Hist, Smithsonian Inst, Washington, DC 20560 USA. EM r.g.mayne@tcu.edu NR 6 TC 0 Z9 0 U1 2 U2 2 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1086-9379 EI 1945-5100 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD AUG PY 2015 VL 50 SU 1 SI SI MA 5222.pdf PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA CN7CR UT WOS:000358591900214 ER PT J AU McCoy, TJ Bullock, ES AF McCoy, T. J. Bullock, E. S. TI VOLATILE-RICH PHASES IN AUBRITES: CLUES TO UNDERSTANDING THE MINERALOGY OF MERCURY? SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 78th Annual Meeting of the Meteoritical-Society CY JUL 27-31, 2015 CL Berkeley, CA SP Meteorit Soc, Barringer Crater Co, Natl Aeronaut & Space Adm, Inst Space & Astronaut Sci, Japan Aerosp Explorat Agcy, Japan Polar Res Assoc, Natl Inst Polar Res, NASA Mars Program Off, Agilent Technologies, CAMECA, Lockheed Martin Space Syst Co, Natl Electrostat Corp, TESCAN, Int Meteorite Collectors Assoc, Planetary Studies Fdn, Lunar & Planetary Inst, Univ Calif, Space Sci Lab C1 [McCoy, T. J.; Bullock, E. S.] Natl Museum Nat Hist, Smithsonian Inst, Dept Mineral Sci, Washington, DC 20560 USA. [Bullock, E. S.] Carnegie Inst Sci, Geophys Lab, Washington, DC 20015 USA. NR 9 TC 0 Z9 0 U1 0 U2 0 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1086-9379 EI 1945-5100 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD AUG PY 2015 VL 50 SU 1 SI SI MA 5280.pdf PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA CN7CR UT WOS:000358591900215 ER PT J AU Sanborn, ME Yin, QZ Schrader, DL AF Sanborn, M. E. Yin, Q-Z Schrader, D. L. TI AQUEOUS ALTERATION AND ITS EFFECT ON epsilon Cr-54: AN INVESTIGATION OF CR1 AND CR2 CHONDRITES. SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 78th Annual Meeting of the Meteoritical-Society CY JUL 27-31, 2015 CL Berkeley, CA SP Meteorit Soc, Barringer Crater Co, Natl Aeronaut & Space Adm, Inst Space & Astronaut Sci, Japan Aerosp Explorat Agcy, Japan Polar Res Assoc, Natl Inst Polar Res, NASA Mars Program Off, Agilent Technologies, CAMECA, Lockheed Martin Space Syst Co, Natl Electrostat Corp, TESCAN, Int Meteorite Collectors Assoc, Planetary Studies Fdn, Lunar & Planetary Inst, Univ Calif, Space Sci Lab C1 [Sanborn, M. E.; Yin, Q-Z] Univ Calif Davis, Dept Earth & Planetary Sci, Davis, CA 95616 USA. [Schrader, D. L.] Smithsonian Inst, Natl Museum Amer Hist, Washington, DC 20560 USA. [Schrader, D. L.] Arizona State Univ, SESE, Tempe, AZ 85281 USA. EM mesanborn@ucdavis.edu NR 8 TC 0 Z9 0 U1 1 U2 2 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1086-9379 EI 1945-5100 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD AUG PY 2015 VL 50 SU 1 SI SI MA 5157.pdf PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA CN7CR UT WOS:000358591900286 ER PT J AU Pikovski, I Zych, M Costa, F Brukner, C AF Pikovski, Igor Zych, Magdalena Costa, Fabio Brukner, Caslav TI Universal decoherence due to gravitational time dilation SO NATURE PHYSICS LA English DT Article ID SPIN BATH; QUANTUM; PARTICLES; GRAVITY; INTERFERENCE; REDUCTION; DYNAMICS; CLOCKS; OPTICS; MODELS AB The physics of low-energy quantum systems is usually studied without explicit consideration of the background spacetime. Phenomena inherent to quantum theory in curved spacetime, such as Hawking radiation, are typically assumed to be relevant only for extreme physical conditions: at high energies and in strong gravitational fields. Here we consider low-energy quantum mechanics in the presence of gravitational time dilation and show that the latter leads to the decoherence of quantum superpositions. Time dilation induces a universal coupling between the internal degrees of freedom and the centre of mass of a composite particle. The resulting correlations lead to decoherence in the particle position, even without any external environment. We also show that the weak time dilation on Earth is already sufficient to affect micrometre-scale objects. Gravity can therefore account for the emergence of classicality and this effect could in principle be tested in future matter-wave experiments. C1 [Pikovski, Igor; Zych, Magdalena; Costa, Fabio; Brukner, Caslav] Univ Vienna, Fac Phys, Vienna Ctr Quantum Sci & Technol VCQ, A-1090 Vienna, Austria. [Pikovski, Igor; Zych, Magdalena; Costa, Fabio; Brukner, Caslav] Austrian Acad Sci, IQOQI, A-1090 Vienna, Austria. [Pikovski, Igor] Harvard Smithsonian Ctr Astrophys, ITAMP, Cambridge, MA 02138 USA. [Pikovski, Igor] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. [Zych, Magdalena; Costa, Fabio] Univ Queensland, Sch Math & Phys, Ctr Engn Quantum Syst, St Lucia, Qld 4072, Australia. RP Pikovski, I (reprint author), Univ Vienna, Fac Phys, Vienna Ctr Quantum Sci & Technol VCQ, Boltzmanngasse 5, A-1090 Vienna, Austria. EM igor.pikovski@cfa.harvard.edu RI Zych, Magdalena/G-4007-2014; Costa, Fabio/G-3746-2014; OI Zych, Magdalena/0000-0002-8356-7613; Costa, Fabio/0000-0002-6547-6005; Pikovski, Igor/0000-0002-9441-2553 FU Austrian Science Fund (FWF) through the doctoral program Complex Quantum Systems (CoQuS); Vienna Center for Quantum Science and Technology (VCQ); SFB FoQuS; Foundational Questions Institute (FQXi); John Templeton Foundation; Australian Research Council Centre of Excellence for Engineered Quantum Systems [CE110001013]; European Commission through RAQUEL [323970]; COST Action [MP1209]; [24621] FX We thank M. Arndt, M. Aspelmeyer, L. Diosi and M. Vanner for discussions and S. Eibenberger for providing us with the illustration of the TPPF20 molecule. This work was supported by the Austrian Science Fund (FWF) through the doctoral program Complex Quantum Systems (CoQuS), the Vienna Center for Quantum Science and Technology (VCQ), the SFB FoQuS and the Individual Project 24621, by the Foundational Questions Institute (FQXi), the John Templeton Foundation, the Australian Research Council Centre of Excellence for Engineered Quantum Systems (grant number CE110001013), the European Commission through RAQUEL (No. 323970) and the COST Action MP1209. NR 32 TC 25 Z9 25 U1 5 U2 23 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 1745-2473 EI 1745-2481 J9 NAT PHYS JI Nat. Phys. PD AUG PY 2015 VL 11 IS 8 BP 668 EP + DI 10.1038/NPHYS3366 PG 7 WC Physics, Multidisciplinary SC Physics GA CO0OQ UT WOS:000358851900021 ER PT J AU Marques, AC Garcia, J Ames, CL AF Marques, Antonio Carlos Garcia, Jimena Ames, Cheryl Lewis TI Internal fertilization and sperm storage in cnidarians: a response to Orr and Brennan SO TRENDS IN ECOLOGY & EVOLUTION LA English DT Letter DE copulation; box jellyfish; Cubozoa; plankton ID CARYBDEA-SIVICKISI; REPRODUCTION; EVOLUTION; BEHAVIOR; CUBOZOA C1 [Marques, Antonio Carlos; Garcia, Jimena] Univ Sao Paulo, Inst Biosci, BR-05508090 Sao Paulo, Brazil. [Marques, Antonio Carlos; Garcia, Jimena] Univ Sao Paulo, Ctr Marine Biol, BR-05508090 Sao Paulo, Brazil. [Marques, Antonio Carlos] Univ Sao Paulo, Ctr Marine Biol, BR-11600000 Sao Paulo, Brazil. [Ames, Cheryl Lewis] Smithsonian Inst, Dept Invertebrate Zool, Natl Museum Nat Hist, Washington, DC 20013 USA. [Ames, Cheryl Lewis] Univ Maryland, Biol Sci Grad Program, BEES Concentrat, College Pk, MD 20742 USA. RP Marques, AC (reprint author), Univ Sao Paulo, Inst Biosci, R Matao Tr 14, BR-05508090 Sao Paulo, Brazil. EM marques@ib.usp.br RI Marques, Antonio/E-8049-2011 OI Marques, Antonio/0000-0002-2884-0541 NR 11 TC 2 Z9 2 U1 1 U2 25 PU ELSEVIER SCIENCE LONDON PI LONDON PA 84 THEOBALDS RD, LONDON WC1X 8RR, ENGLAND SN 0169-5347 J9 TRENDS ECOL EVOL JI Trends Ecol. Evol. PD AUG PY 2015 VL 30 IS 8 BP 435 EP 436 DI 10.1016/j.tree.2015.06.002 PG 2 WC Ecology; Evolutionary Biology; Genetics & Heredity SC Environmental Sciences & Ecology; Evolutionary Biology; Genetics & Heredity GA CO7GX UT WOS:000359328700001 PM 26115932 ER PT J AU Fugere, V O'Mara, MT Page, RA AF Fugere, Vincent Teague O'Mara, M. Page, Rachel A. TI Perceptual bias does not explain preference for prey call adornment in the frog-eating bat SO BEHAVIORAL ECOLOGY AND SOCIOBIOLOGY LA English DT Article DE Eavesdropping; Perceptual bias; Receiver bias; Prey detection; Predator-prey interaction; Fringe-lipped bat; Tungara frog ID FEMALE MATE CHOICE; TRACHOPS-CIRRHOSUS; SEXUAL SELECTION; MATING SIGNALS; TUNGARA FROGS; LOCALIZATION PERFORMANCE; PHYSALAEMUS-PUSTULOSUS; EAVESDROPPING BAT; FORAGING BEHAVIOR; SENSORY ECOLOGY AB Eavesdropping predators sometimes show preferences for certain prey signal variants, yet the ultimate and proximate reasons for such preferences are often unclear. The fringe-lipped bat, Trachops cirrhosus, eavesdrops on the advertisement calls of male tA(0)ngara frogs, Physalaemus pustulosus, and shows a marked preference for complex (adorned) calls over simple (non-adorned) calls. We hypothesized that this preference stems from perceptual biases in the sensory and/or cognitive systems of T. cirrhosus. To test this hypothesis, we conducted a series of preference experiments in which we presented bats with various modified simple calls, each altered to possess one of the acoustic properties that distinguish complex calls from simple calls. We reasoned that if perceptual bias accounts for the bat's preference for complex calls, then a novel stimulus with similar acoustic properties to the complex call should be attractive as well (i.e., the preference should be permissive). Except for weak evidence suggesting that the longer duration of complex calls could contribute to their greater attractiveness to T. cirrhosus, we did not find any indication that perceptual biases account for this eavesdropper preference. Instead, we suggest that T. cirrhosus developed their preference for call complexity because eavesdropping on complex calls provides greater fitness benefits than eavesdropping on simple calls, for example, because eavesdropping on complex calls may increase probability of prey capture and/or lead to more profitable food patches. C1 [Fugere, Vincent] McGill Univ, Dept Biol, Montreal, PQ H3A 1B1, Canada. [Fugere, Vincent; Teague O'Mara, M.; Page, Rachel A.] Smithsonian Trop Res Inst, Balboa Ancon 03092, Panama. [Teague O'Mara, M.] Max Planck Inst Ornithol, Dept Migrat & Immunoecol, Radolfzell am Bodensee, Germany. [Teague O'Mara, M.] Univ Konstanz, Dept Biol & Zukunftskolleg, Constance, Germany. RP Fugere, V (reprint author), McGill Univ, Dept Biol, 1205 Ave Docteur Penfield, Montreal, PQ H3A 1B1, Canada. EM vincent.fugere@mail.mcgill.ca OI O'Mara, M. Teague/0000-0002-6951-1648 FU Smithsonian Tropical Research Institute; Fonds de Recherche du Qurbec-Nature et Technologies; Natural Sciences and Engineering Research Council of Canada; Vanier Canada Graduate Fellowship Program FX The authors would like to thank the government of the Republic of Panama for their permission to work in Gamboa and Soberania National Park and the Smithsonian Tropical Research Institute for providing critical logistical support and infrastructure. Sara Troxell, Sean Griffin, Martha Moscoso, and Patricia Jones helped with capturing and caring for bats. The authors are also grateful to Michael J. Ryan for supplying the tungara frog recordings and to Ximena Bernal, Patricia Jones, Michael Caldwell, Michael J. Ryan, Christian Voigt, Gloriana Chaverri, and two anonymous reviewers for their constructive comments on previous versions of the manuscript. This study was supported by the Smithsonian Tropical Research Institute, the Fonds de Recherche du Qurbec-Nature et Technologies, the Natural Sciences and Engineering Research Council of Canada, and the Vanier Canada Graduate Fellowship Program. NR 62 TC 1 Z9 1 U1 2 U2 21 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0340-5443 EI 1432-0762 J9 BEHAV ECOL SOCIOBIOL JI Behav. Ecol. Sociobiol. PD AUG PY 2015 VL 69 IS 8 BP 1353 EP 1364 DI 10.1007/s00265-015-1949-2 PG 12 WC Behavioral Sciences; Ecology; Zoology SC Behavioral Sciences; Environmental Sciences & Ecology; Zoology GA CN8ZK UT WOS:000358734700012 ER PT J AU Wurzburger, N Wright, SJ AF Wurzburger, Nina Wright, S. Joseph TI Fine-root responses to fertilization reveal multiple nutrient limitation in a lowland tropical forest SO ECOLOGY LA English DT Article DE Barro Colorado Nature Monument, Panama; fine roots; mycorrhizal fungi; nitrogen; phosphorus; potassium; root functional traits; specific root length; tissue density; tropical forest ID ARBUSCULAR MYCORRHIZAL FUNGI; RAIN-FOREST; PHOSPHORUS LIMITATION; TREE GROWTH; POTASSIUM ADDITION; SOIL NUTRIENTS; NITROGEN; TRAITS; DYNAMICS; PATTERNS AB Questions remain as to which soil nutrients limit primary production in tropical forests. Phosphorus (P) has long been considered the primary limiting element in lowland forests, but recent evidence demonstrates substantial heterogeneity in response to nutrient addition, highlighting a need to understand and diagnose nutrient limitation across diverse forests. Fine-root characteristics including their abundance, functional traits, and mycorrhizal symbionts can be highly responsive to changes in soil nutrients and may help to diagnose nutrient limitation. Here, we document the response of fine roots to long-term nitrogen (N), P, and potassium (K) fertilization in a lowland forest in Panama. Because this experiment has demonstrated that N and K together limit tree growth and P limits fine litter production, we hypothesized that fine roots would also respond to nutrient addition. Specifically we hypothesized that N, P, and K addition would reduce the biomass, diameter, tissue density, and mycorrhizal colonization of fine roots, and increase nutrient concentration in root tissue. Most morphological root traits responded to the single addition of K and the paired addition of N and P, with the greatest response to all three nutrients combined. The addition of N, P, and K together reduced fine-root biomass, length, and tissue density, and increased specific root length, whereas root diameter remained unchanged. Nitrogen addition did not alter root N concentration, but P and K addition increased root P and K concentration, respectively. Mycorrhizal colonization of fine roots declined with N, increased with P, and was unresponsive to K addition. Although plant species composition remains unchanged after 14 years of fertilization, fine-root characteristics responded to N, P, and K addition, providing some of the strongest stand-level responses in this experiment. Multiple soil nutrients regulate fine-root abundance, morphological and chemical traits, and their association with mycorrhizal fungi in a species-rich lowland tropical forest. C1 [Wurzburger, Nina] Univ Georgia, Odum Sch Ecol, Athens, GA 30602 USA. [Wright, S. Joseph] Smithsonian Trop Res Inst, Balboa, Panama. RP Wurzburger, N (reprint author), Univ Georgia, Odum Sch Ecol, Athens, GA 30602 USA. EM ninawurz@uga.edu RI Wright, Stuart/M-3311-2013 OI Wright, Stuart/0000-0003-4260-5676 FU University of Georgia; Odum School of Ecology; Smithsonian Tropical Research Institute FX This study was funded by the University of Georgia, the Odum School of Ecology and the Smithsonian Tropical Research Institute. We gratefully acknowledge Courtney Collins, Kelly Andersen, and Rufino Gonzalez for their assistance in the field; Shialoh Wilson, Tierney O'Sullivan, and Brice Howell for assistance in the laboratory; and Sarah Batterman and Lars Hedin for their assistance and support during a pilot study that led to this work. We thank two anonymous reviewers for their constructive comments on the manuscript. NR 61 TC 9 Z9 9 U1 12 U2 87 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 AUG PY 2015 VL 96 IS 8 BP 2137 EP 2146 DI 10.1890/14-1362.1 PG 10 WC Ecology SC Environmental Sciences & Ecology GA CN5FF UT WOS:000358454500012 PM 26405739 ER PT J AU Touchon, JC McCoy, MW Landberg, T Vonesh, JR Warkentin, KM AF Touchon, Justin C. McCoy, Michael W. Landberg, Tobias Vonesh, James R. Warkentin, Karen M. TI Putting mu/g in a new light: plasticity in life history switch points reflects fine-scale adaptive responses SO ECOLOGY LA English DT Article DE Agalychnis callidryas; Anura; growth; life history switch point; mesocosm experiment; mortality; Neotropical treefrog; phenotypic plasticity; predator-induced variation; Smithsonian Tropical Research Institute, Gamboa, Panama; timing of metamorphosis ID RED-EYED TREEFROG; INDUCED PHENOTYPIC PLASTICITY; PREDATION RISK; TRADE-OFFS; DEVELOPMENTAL PLASTICITY; AMPHIBIAN METAMORPHOSIS; HATCHING AGE; REEF FISHES; GROWTH-RATE; PREY AB Life history theory predicts that organisms with complex life cycles should transition between life stages when the ratio of growth rate (g) to risk of mortality (mu) in the current stage falls below that in the subsequent stage. Empirical support for this idea has been mixed. Implicit in both theory and empirical work is that the risk of mortality in the subsequent stage is unknown. However, some embryos and larvae of both vertebrates and invertebrates assess cues of post-transition predation risk and alter the timing of hatching or metamorphosis accordingly. Furthermore, although life history switch points of prey have traditionally been treated as discrete shifts in morphology or habitat, for many organisms they are continuous transitional periods within which the timing of specific developmental and behavioral events can be plastic. We studied red-eyed treefrogs (Agalychnis callidryas), which detect predators of both larvae and metamorphs, to test if plastic changes during the process of metamorphosis could reconcile the mismatch between life history theory and empirical data and if plasticity in an earlier stage transition (hatching) would affect plasticity at a subsequent stage transition (metamorphosis). We reared tadpoles from hatching until metamorphosis in a full-factorial cross of two hatching ages (early-vs. late-hatched) and the presence or absence of free-roaming predators of larvae (giant water bugs) and metamorphs (fishing spiders). Hatching age affected the times from oviposition to tail resorption and from hatching to emergence onto land, but did not alter responses to predators or developmental stage at emergence. Tadpoles did not alter their age at emergence or tail resorption in response to larval or metamorph predators, despite the fact that predators reduced tadpole density by similar to 30%. However, developmental stage at emergence and time needed to complete metamorphosis in the terrestrial environment were plastic and consistent with predictions of the "minimize mu/g'' framework. Our results demonstrate that likely adaptive changes in life history transitions occur at previously unappreciated timescales. Consideration of plasticity in the developmental timing of ecologically important events within metamorphosis, rather than treating it as a discrete switch point, may help to reconcile inconsistencies between empirical studies of predator effects and expectations of long-standing ecological theory. C1 [Touchon, Justin C.] Vassar Coll, Dept Biol, Poughkeepsie, NY 12604 USA. [Touchon, Justin C.; McCoy, Michael W.] E Carolina Univ, Dept Biol, Greenville, NC 27858 USA. [Landberg, Tobias] Arcadia Univ, Dept Biol, Glenside, PA 19038 USA. [Landberg, Tobias; Warkentin, Karen M.] Boston Univ, Dept Biol, Boston, MA 02215 USA. [Vonesh, James R.] Virginia Commonwealth Univ, Dept Biol, Richmond, VA 23284 USA. [Warkentin, Karen M.] Smithsonian Trop Res Inst, Balboa, Panama. RP Touchon, JC (reprint author), Vassar Coll, Dept Biol, 124 Raymond Ave, Poughkeepsie, NY 12604 USA. EM jutouchon@vassar.edu RI Vonesh, James/I-1573-2013 OI Vonesh, James/0000-0003-2481-9988 FU National Science Foundation [DEB-0717220, DEB-0716923]; Boston University; Virginia Commonwealth University; East Carolina University; STRI FX We thank the Smithsonian Tropical Research Institute (STRI) for logistical support and the Autoridad Nacional del Ambiente de Panama for research permit SC/A-16-10. This research was conducted under Boston University IACUC protocol #08-011. We thank S. Bouchard, J. Charbonnier, Z. Costa, K. Cohen, R. Greene, C. Jenney, C. Noss, M. Palmer, S. Schleier, and B. Willink for assistance with the experiment and two anonymous reviewers for helpful comments on the manuscript. This research was funded by the National Science Foundation (DEB-0717220 to J. R. Vonesh and DEB-0716923 to K. M. Warkentin), Boston University, Virginia Commonwealth University, East Carolina University, and STRI. NR 54 TC 1 Z9 1 U1 5 U2 24 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 AUG PY 2015 VL 96 IS 8 BP 2192 EP 2202 DI 10.1890/14-1301.1 PG 11 WC Ecology SC Environmental Sciences & Ecology GA CN5FF UT WOS:000358454500017 PM 26405744 ER PT J AU Carmichael, SK Zorn, BT Santelli, CM Roble, LA Carmichael, MJ Brauer, SL AF Carmichael, Sarah K. Zorn, Bryan T. Santelli, Cara M. Roble, Leigh A. Carmichael, Mary J. Braeuer, Suzanna L. TI Nutrient input influences fungal community composition and size and can stimulate manganese (II) oxidation in caves SO ENVIRONMENTAL MICROBIOLOGY REPORTS LA English DT Article ID COAL-MINE DRAINAGE; SP STRAIN KR21-2; MICROBIAL DIVERSITY; LASCAUX CAVE; MN(II) OXIDATION; MOLECULAR-IDENTIFICATION; KARTCHNER CAVERNS; LECHUGUILLA CAVE; QUANTITATIVE PCR; DESERT VARNISH AB Little is known about the fungal role in biogeochemical cycling in oligotrophic ecosystems. This study compared fungal communities and assessed the role of exogenous carbon on microbial community structure and function in two southern Appalachian caves: an anthropogenically impacted cave and a near-pristine cave. Due to carbon input from shallow soils, the anthropogenically impacted cave had an order of magnitude greater fungal and bacterial quantitative-polymerase chain reaction (qPCR) gene copy numbers, had significantly greater community diversity, and was dominated by ascomycotal phylotypes common in early phase, labile organic matter decomposition. Fungal assemblages in the near-pristine cave samples were dominated by Basidiomycota typically found in deeper soils (and/or in late phase, recalcitrant organic matter decomposition), suggesting more oligotrophic conditions. In situ carbon and manganese (II) [Mn(II)] addition over 10 weeks resulted in growth of fungal mycelia followed by increased Mn(II) oxidation. A before/after comparison of the fungal communities indicated that this enrichment increased the quantity of fungal and bacterial cells, yet decreased overall fungal diversity. Anthropogenic carbon sources can therefore dramatically influence the diversity and quantity of fungi, impact microbial community function, and stimulate Mn(II) oxidation, resulting in a cascade of changes that can strongly influence nutrient and trace element biogeochemical cycles in karst aquifers. C1 [Carmichael, Sarah K.] Appalachian State Univ, Dept Geol, Boone, NC 28608 USA. [Zorn, Bryan T.; Braeuer, Suzanna L.] Appalachian State Univ, Dept Biol, Boone, NC 28608 USA. [Santelli, Cara M.] Natl Museum Nat Hist, Smithsonian Inst, Washington, DC 20560 USA. [Roble, Leigh A.] Univ Maryland, Dept Geol, College Pk, MD 20742 USA. [Carmichael, Mary J.] Wake Forest Univ, Dept Biol, Winston Salem, NC 27109 USA. RP Brauer, SL (reprint author), Appalachian State Univ, Dept Biol, Boone, NC 28608 USA. EM brauersl@appstate.edu OI Santelli, Cara/0000-0001-8617-0008 FU Appalachian State University, NC; Smithsonian Institution; NC Space Grant Graduate Research Fellowship FX The authors thank Dr. Charles Pepe-Ranney, Dr. Michael Madritch and Dr. Matt Estep for assistance with sequencing and data processing, and Dr. John Walker and Zack Anderson for assistance with fungal analyses. Dr. Jeffrey Post performed selected mu-XRD analyses and mineral phase identifications. Additionally, the authors are extremely grateful for assistance provided by Melanie Hoff, Milton Starnes and John Rossi for facilitating visits to the cave sites. Partial support was provided by Appalachian State University, NC Space Grant New Investigators Awards to SK Carmichael and SL Brauer, a small grant from the Smithsonian Institution awarded to CM Santelli and through a NC Space Grant Graduate Research Fellowship awarded to MJ Carmichael. NR 101 TC 0 Z9 0 U1 5 U2 29 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1758-2229 J9 ENV MICROBIOL REP JI Environ. Microbiol. Rep. PD AUG PY 2015 VL 7 IS 4 BP 592 EP 605 DI 10.1111/1758-2229.12291 PG 14 WC Environmental Sciences; Microbiology SC Environmental Sciences & Ecology; Microbiology GA CN5XM UT WOS:000358506800001 PM 25865809 ER PT J AU Glenn, DR Lee, K Park, H Weissleder, R Yacoby, A Lukin, MD Lee, H Walsworth, RL Connolly, CB AF Glenn, David R. Lee, Kyungheon Park, Hongkun Weissleder, Ralph Yacoby, Amir Lukin, Mikhail D. Lee, Hakho Walsworth, Ronald L. Connolly, Colin B. TI Single-cell magnetic imaging using a quantum diamond microscope SO NATURE METHODS LA English DT Article ID PROTEIN AB We apply a quantum diamond microscope for detection and imaging of immunomagnetically labeled cells. This instrument uses nitrogen-vacancy (NV) centers in diamond for correlated magnetic and fluorescence imaging. Our device provides single-cell resolution and a field of view (similar to 1 mm(2)) two orders of magnitude larger than that of previous NV imaging technologies, enabling practical applications. To illustrate, we quantified cancer biomarkers expressed by rare tumor cells in a large population of healthy cells. C1 [Glenn, David R.; Walsworth, Ronald L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Lee, Kyungheon; Weissleder, Ralph; Lee, Hakho] Massachusetts Gen Hosp, Ctr Syst Biol, Boston, MA 02114 USA. [Park, Hongkun; Yacoby, Amir; Lukin, Mikhail D.; Walsworth, Ronald L.] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. [Park, Hongkun] Harvard Univ, Dept Chem & Chem Biol, Cambridge, MA 02138 USA. [Park, Hongkun; Walsworth, Ronald L.] Harvard Univ, Ctr Brain Sci, Cambridge, MA 02138 USA. [Weissleder, Ralph] Harvard Univ, Sch Med, Dept Syst Biol, Boston, MA 02115 USA. [Connolly, Colin B.] Quantum Diamond Technol Inc, Somerville, MA USA. RP Lee, H (reprint author), Massachusetts Gen Hosp, Ctr Syst Biol, Boston, MA 02114 USA. EM hlee@mgh.harvard.edu; rwalsworth@cfa.harvard.edu; cconnolly@quantumdiamondtech.com FU US National Institutes of Health [R01HL113156, U54-CA119349]; US Defense Advanced Research Projects Agency (DARPA) QuASAR program; DARPA SBIR [W31P4Q-13-C-0064] FX The authors thank M.L. McKee for help with electron microscopy, as well as M. Liong and H. Shao for advice on magnetic assay protocols. This work was supported in part by US National Institutes of Health grants R01HL113156 (H.L.) and U54-CA119349 (R.W.) as well as the US Defense Advanced Research Projects Agency (DARPA) QuASAR program and DARPA SBIR contract W31P4Q-13-C-0064. NR 17 TC 19 Z9 19 U1 4 U2 71 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 1548-7091 EI 1548-7105 J9 NAT METHODS JI Nat. Methods PD AUG PY 2015 VL 12 IS 8 BP 736 EP U161 DI 10.1038/NMETH.3449 PG 5 WC Biochemical Research Methods SC Biochemistry & Molecular Biology GA CN8ZW UT WOS:000358736100015 PM 26098019 ER PT J AU Zhang, L Rothfels, CJ Ebihara, A Schuettpelz, E Le Pechon, T Kamau, P He, H Zhou, XM Prado, J Field, A Yatskievych, G Gao, XF Zhang, LB AF Zhang, Liang Rothfels, Carl J. Ebihara, Atsushi Schuettpelz, Eric Le Pechon, Timothee Kamau, Peris He, Hai Zhou, Xin-Mao Prado, Jefferson Field, Ashley Yatskievych, George Gao, Xin-Fen Zhang, Li-Bing TI A global plastid phylogeny of the brake fern genus Pteris (Pteridaceae) and related genera in the Pteridoideae SO CLADISTICS LA English DT Review ID MAXIMUM-LIKELIHOOD; CHLOROPLAST DNA; DRYOPTERIS DRYOPTERIDACEAE; ERIOSORUS PTERIDACEAE; EVOLUTIONARY LINEAGES; MODEL SELECTION; SEQUENCES; PARSIMONY; TAENITIDOIDEAE; MONILOPHYTES AB The brake fern genus Pteris belongs to the Pteridaceae subfamily Pteridoideae. It contains 200-250 species distributed on all continents except Antarctica, with its highest species diversity in tropical and subtropical regions. The monophyly of Pteris has long been in question because of its great morphological diversity and because of the controversial relationships of the Australian endemic monospecific genus Platyzoma. The circumscription of the Pteridoideae has likewise been uncertain. Previous studies typically had sparse sampling of Pteris species and related genera and used limited DNA sequence data. In the present study, DNA sequences of six plastid loci of 146 accessions representing 119 species of Pteris (including the type of the genus) and 18 related genera were used to infer a phylogeny using maximum-likelihood, Bayesian-inference and maximum-parsimony methods. Our major results include: (i) the previous uncertain relationships of Platyzoma were due to long-branch attraction; (ii) Afropteris, Neurocallis, Ochropteris and Platyzoma are all embedded within a well-supported Pteris sensu lato; (iii) the traditionally circumscribed Jamesonia is paraphyletic in relation to a monophyletic Eriosorus; (iv) Pteridoideae contains 15 genera: Actiniopteris, Anogramma, Austrogramme, Cerosora, Cosentinia, Eriosorus, Jamesonia, Nephopteris (no molecular data), Onychium, Pityrogramma, Pteris, Pterozonium, Syngramma, Taenitis and Tryonia; and (v) 15 well-supported clades within Pteris are identified, which differ from one another on molecular, morphological and geographical grounds, and represent 15 major evolutionary lineages. (C) The Willi Hennig Society 2014. C1 [Zhang, Liang; Le Pechon, Timothee; Zhou, Xin-Mao; Gao, Xin-Fen] Chinese Acad Sci, Chengdu Inst Biol, Chengdu 610041, Sichuan, Peoples R China. [Rothfels, Carl J.] Univ British Columbia, Dept Zool, Vancouver, BC V6T 1Z4, Canada. [Ebihara, Atsushi] Natl Museum Nat & Sci, Dept Bot, Tsukuba, Ibaraki 3050005, Japan. [Schuettpelz, Eric] Smithsonian Inst, Dept Bot MRC 166, Natl Museum Nat Hist, Washington, DC 20013 USA. [Kamau, Peris] Natl Museums Kenya, Dept Bot, Nairobi, Kenya. [He, Hai] Chongqing Normal Univ, Dept Biol, Chongqing 400047, Peoples R China. [Prado, Jefferson] Inst Bot Herbario SP, BR-04301012 Sao Paulo, Brazil. [Field, Ashley] James Cook Univ, Australian Trop Herbarium, Smithfield, Qld 4878, Australia. [Field, Ashley] Queensland Herbarium, Dept Sci Informat Technol Innovat & Arts, Toowong, Qld 4066, Australia. [Yatskievych, George; Zhang, Li-Bing] Missouri Bot Garden, St Louis, MO 63166 USA. RP Gao, XF (reprint author), Chinese Acad Sci, Chengdu Inst Biol, POB 416, Chengdu 610041, Sichuan, Peoples R China. EM xfgao@cib.ac.cn; Libing.Zhang@mobot.org RI Le Pechon, Timothee/N-9247-2013; Prado, Jefferson/C-4766-2012; OI Le Pechon, Timothee/0000-0003-3668-753X; Prado, Jefferson/0000-0003-4783-3125; Schuettpelz, Eric/0000-0003-3891-9904 NR 105 TC 10 Z9 10 U1 2 U2 20 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0748-3007 EI 1096-0031 J9 CLADISTICS JI Cladistics PD AUG PY 2015 VL 31 IS 4 BP 406 EP 423 DI 10.1111/cla.12094 PG 18 WC Evolutionary Biology SC Evolutionary Biology GA CN1KS UT WOS:000358179500002 ER PT J AU Garzon-Lopez, CX Ballesteros-Mejia, L Ordonez, A Bohlman, SA Olff, H Jansen, PA AF Garzon-Lopez, Carol X. Ballesteros-Mejia, Liliana Ordonez, Alejandro Bohlman, Stephanie A. Olff, Han Jansen, Patrick A. TI Indirect interactions among tropical tree species through shared rodent seed predators: a novel mechanism of tree species coexistence SO ECOLOGY LETTERS LA English DT Article DE Apparent competition; apparent mutualism; Astrocaryum standleyanum; Attalea butyracea; Dipteryx oleifera; indirect effects; Janzen-Connell hypothesis; seed predation; shared enemies; tropical forest ID RAIN-FOREST TREE; APPARENT COMPETITION; DENSITY-DEPENDENCE; SPATIAL AUTOCORRELATION; PLANT RECRUITMENT; DISPERSAL; PALM; HERBIVORES; DIVERSITY; SURVIVAL AB The coexistence of numerous tree species in tropical forests is commonly explained by negative dependence of recruitment on the conspecific seed and tree density due to specialist natural enemies that attack seeds and seedlings (Janzen-Connell' effects). Less known is whether guilds of shared seed predators can induce a negative dependence of recruitment on the density of different species of the same plant functional group. We studied 54 plots in tropical forest on Barro Colorado Island, Panama, with contrasting mature tree densities of three coexisting large seeded tree species with shared seed predators. Levels of seed predation were far better explained by incorporating seed densities of all three focal species than by conspecific seed density alone. Both positive and negative density dependencies were observed for different species combinations. Thus, indirect interactions via shared seed predators can either promote or reduce the coexistence of different plant functional groups in tropical forest. C1 [Garzon-Lopez, Carol X.; Ballesteros-Mejia, Liliana; Olff, Han; Jansen, Patrick A.] Univ Groningen, Groningen Inst Evolutionary Life Sci, NL-9700 CC Groningen, Netherlands. [Garzon-Lopez, Carol X.] Fdn Edmund Mach, GIS & Remote Sensing Unit, Res & Innovat Ctr, Dept Biodivers & Mol Ecol, I-38010 San Michele All Adige, TN, Italy. [Ballesteros-Mejia, Liliana] Univ Fed Goias UFG, Lab Genet & Biodiversidade, ICB, BR-74001970 Goiania, Go, Brazil. [Ordonez, Alejandro] Aarhus Univ, Sect Ecoinformat & Biodivers, Dept Biosci, DK-8000 Aarhus C, Denmark. [Bohlman, Stephanie A.; Jansen, Patrick A.] Smithsonian Trop Res Inst, Balboa 084303092, Panama. [Bohlman, Stephanie A.] Univ Florida, Sch Forest Resources & Conservat, Gainesville, FL 32611 USA. [Jansen, Patrick A.] Wageningen Univ, Dept Environm Sci, NL-6700 AA Wageningen, Netherlands. RP Garzon-Lopez, CX (reprint author), Univ Groningen, Groningen Inst Evolutionary Life Sci, Box 11103, NL-9700 CC Groningen, Netherlands. EM c.x.garzon@gmail.com RI Olff, Han/A-8516-2008; Garzon-Lopez, Carol/G-6251-2014 OI Olff, Han/0000-0003-2154-3576; Garzon-Lopez, Carol/0000-0002-4099-2740 FU Smithsonian Tropical Research Institute; Ubbo Emmius Scholarship programme; University of Groningen; EU BON (Building the European Biodiversity Observation Network) project; European Union [308454]; European Research Council [ERC-2012-StG-310886-HISTFUNC] FX We thank Erik Vasquez, Helen Esser and Eduardo Medina for their help in the field and laboratory; and Egbert Leigh, Robert Holt and two anonymous reviewers for their very helpful comments. This work was supported by the Smithsonian Tropical Research Institute, the Ubbo Emmius Scholarship programme (CXG) and the Marco Polo funds (LBM) of the University of Groningen. CXG was partially funded by the EU BON (Building the European Biodiversity Observation Network) project, funded by the European Union under the 7th Framework programme, Contract No. 308454. AO was supported by the European Research Council grant ERC-2012-StG-310886-HISTFUNC. NR 51 TC 3 Z9 3 U1 7 U2 62 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 AUG PY 2015 VL 18 IS 8 BP 752 EP 760 DI 10.1111/ele.12452 PG 9 WC Ecology SC Environmental Sciences & Ecology GA CM8NO UT WOS:000357958900002 PM 25939379 ER PT J AU Peay, KG Russo, SE McGuire, KL Lim, ZY Chan, JP Tan, S Davies, SJ AF Peay, Kabir G. Russo, Sabrina E. McGuire, Krista L. Lim, Zhenyu Chan, Ju Ping Tan, Sylvester Davies, Stuart J. TI Lack of host specificity leads to independent assortment of dipterocarps and ectomycorrhizal fungi across a soil fertility gradient SO ECOLOGY LETTERS LA English DT Article DE Borneo; Lambir Hills; mutualism; mycorrhiza; plant-soil feedback; tropical rainforest ID BORNEAN RAIN-FOREST; COMMUNITY STRUCTURE; MYCORRHIZAL FUNGI; TROPICAL FOREST; CO-INVASION; PLANT; ASSOCIATIONS; FEEDBACK; DISTRIBUTIONS; LIMITATION AB Plants interact with a diversity of microorganisms, and there is often concordance in their community structures. Because most community-level studies are observational, it is unclear if such concordance arises because of host specificity, in which microorganisms or plants limit each other's occurrence. Using a reciprocal transplant experiment, we tested the hypothesis that host specificity between trees and ectomycorrhizal fungi determines patterns of tree and fungal soil specialisation. Seedlings of 13 dipterocarp species with contrasting soil specialisationswereseeded into plots crossing soil type and canopy openness. Ectomycorrhizalcolonists were identified by DNA sequencing. After 2.5years, we found no evidence of host specificity. Rather, soil environment was the primary determinant of ectomycorrhizal diversity and composition on seedlings. Despite their close symbiosis, our results show that ectomycorrhizal fungi and tree communities in this Bornean rain forest assembleindependently of host-specific interactions, raising questions about howmutualism shapes the realised niche. C1 [Peay, Kabir G.; Lim, Zhenyu] Stanford Univ, Dept Biol, Stanford, CA 94305 USA. [Russo, Sabrina E.; Chan, Ju Ping] Univ Nebraska, Sch Biol Sci, Lincoln, NE 68588 USA. [McGuire, Krista L.] Columbia Univ, Barnard Coll, Dept Biol, New York, NY 10027 USA. [McGuire, Krista L.] Columbia Univ, Dept Ecol Evolut & Environm Biol, New York, NY 10027 USA. [Tan, Sylvester; Davies, Stuart J.] Smithsonian Inst, Ctr Trop Forest Sci, Washington, DC 20013 USA. RP Peay, KG (reprint author), Stanford Univ, Dept Biol, Stanford, CA 94305 USA. EM kpeay@stanford.edu OI Peay, Kabir/0000-0002-7998-7412 FU National Science Foundation [1249342, 0919136, 1120011] FX This research was supported by National Science Foundation DEB grants 1249342 to KGP, 0919136 to SER and 1120011 to KLM. The authors thank Sarawak Forest Research Corporation and Forest Department Sarawak for permission to conduct research at Lambir and Ms. Januarie Kulis, Park Warden of Lambir Hills National Park, for her support. Tadashi Fukami, the Fukami Lab and Peay Lab gave helpful comments on an early draft. NR 52 TC 18 Z9 18 U1 9 U2 73 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 AUG PY 2015 VL 18 IS 8 BP 807 EP 816 DI 10.1111/ele.12459 PG 10 WC Ecology SC Environmental Sciences & Ecology GA CM8NO UT WOS:000357958900008 PM 26032408 ER PT J AU Allan, E Manning, P Alt, F Binkenstein, J Blaser, S Bluethgen, N Bohm, S Grassein, F Holzel, N Klaus, VH Kleinebecker, T Morris, EK Oelmann, Y Prati, D Renner, SC Rillig, MC Schaefer, M Schloter, M Schmitt, B Schoning, I Schrumpf, M Solly, E Sorkau, E Steckel, J Steffen-Dewenter, I Stempfhuber, B Tschapka, M Weiner, CN Weisser, WW Werner, M Westphal, C Wilcke, W Fischer, M AF Allan, Eric Manning, Pete Alt, Fabian Binkenstein, Julia Blaser, Stefan Bluethgen, Nico Boehm, Stefan Grassein, Fabrice Hoelzel, Norbert Klaus, Valentin H. Kleinebecker, Till Morris, E. Kathryn Oelmann, Yvonne Prati, Daniel Renner, Swen C. Rillig, Matthias C. Schaefer, Martin Schloter, Michael Schmitt, Barbara Schoening, Ingo Schrumpf, Marion Solly, Emily Sorkau, Elisabeth Steckel, Juliane Steffen-Dewenter, Ingolf Stempfhuber, Barbara Tschapka, Marco Weiner, Christiane N. Weisser, Wolfgang W. Werner, Michael Westphal, Catrin Wilcke, Wolfgang Fischer, Markus TI Land use intensification alters ecosystem multifunctionality via loss of biodiversity and changes to functional composition SO ECOLOGY LETTERS LA English DT Article DE Biodiversity-ecosystem functioning; ecosystem services; global change; land use; multifunctionality ID PLANT-SPECIES RICHNESS; GRASSLAND COMMUNITIES; USE INTENSITY; SERVICES; DIVERSITY; PRODUCTIVITY; MANAGEMENT; FERTILIZATION; TRADEOFFS; LANDSCAPE AB Global change, especially land-use intensification, affects human well-being by impacting the delivery of multiple ecosystem services (multifunctionality). However, whether biodiversity loss is a major component of global change effects on multifunctionality in real-world ecosystems, as in experimental ones, remains unclear. Therefore, we assessed biodiversity, functional composition and 14 ecosystem services on 150 agricultural grasslands differing in land-use intensity. We also introduce five multifunctionality measures in which ecosystem services were weighted according to realistic land-use objectives. We found that indirect land-use effects, i.e. those mediated by biodiversity loss and by changes to functional composition, were as strong as direct effects on average. Their strength varied with land-use objectives and regional context. Biodiversity loss explained indirect effects in a region of intermediate productivity and was most damaging when land-use objectives favoured supporting and cultural services. In contrast, functional composition shifts, towards fast-growing plant species, strongly increased provisioning services in more inherently unproductive grasslands. C1 [Allan, Eric; Manning, Pete; Blaser, Stefan; Grassein, Fabrice; Prati, Daniel; Schmitt, Barbara; Fischer, Markus] Univ Bern, Inst Plant Sci, CH-3013 Bern, Switzerland. [Allan, Eric] Univ Bern, Ctr Dev & Environm, CH-3012 Bern, Switzerland. [Alt, Fabian; Oelmann, Yvonne; Sorkau, Elisabeth] Univ Tubingen, Geocol, D-72070 Tubingen, Germany. [Binkenstein, Julia; Schaefer, Martin] Univ Freiburg, Dept Ecol & Evolutionary Biol, Fac Biol, D-79104 Freiburg, Germany. [Bluethgen, Nico] Tech Univ Darmstadt, Ecol Networks, Biol, D-64287 Darmstadt, Germany. [Boehm, Stefan; Renner, Swen C.; Tschapka, Marco] Univ Ulm, Inst Expt Ecol, D-89069 Ulm, Germany. [Hoelzel, Norbert; Klaus, Valentin H.; Kleinebecker, Till] Univ Munster, Inst Landscape Ecol, D-48149 Munster, Germany. [Morris, E. Kathryn] Xavier Univ, Cincinnati, OH 45207 USA. [Renner, Swen C.] Univ Freiburg, Inst Biol Zool 1, D-79106 Freiburg, Germany. [Renner, Swen C.] Natl Zool Pk, Smithsonian Conservat Biol Ctr, Front Royal, VA 22630 USA. [Rillig, Matthias C.] Free Univ Berlin, Plant Ecol, D-14195 Berlin, Germany. [Rillig, Matthias C.] Berlin Brandenburg Inst Adv Biodivers Res BBIB, D-14195 Berlin, Germany. [Schloter, Michael] Helmholtz Zentrum Munchen, Res Unit Environm Genom, D-85758 Oberschleissheim, Germany. [Schoening, Ingo; Schrumpf, Marion; Solly, Emily] Max Planck Inst Biogeochem, D-07745 Jena, Germany. [Steckel, Juliane; Steffen-Dewenter, Ingolf; Weiner, Christiane N.; Werner, Michael] Univ Wurzburg, Dept Anim Ecol & Trop Biol, Bioctr, D-97974 Wurzburg, Germany. [Stempfhuber, Barbara] German Res Ctr Environm Hlth, Helmholtz Zentrum Munchen, Environm Genom, D-85764 Neuherberg, Germany. [Tschapka, Marco] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. [Weisser, Wolfgang W.] Univ Jena, Inst Ecol, D-07743 Jena, Germany. [Weisser, Wolfgang W.] Tech Univ Munich, Terr Ecol Res Grp, Dept Ecol & Ecosyst Management, Ctr Food & Life Sci Weihenstephan, D-85354 Freising Weihenstephan, Germany. [Westphal, Catrin] Univ Gottingen, Dept Crop Sci, Agroecol, D-37077 Gottingen, Germany. [Wilcke, Wolfgang] Univ Bern, Inst Geog, CH-3012 Bern, Switzerland. [Wilcke, Wolfgang] Karlsruhe Inst Technol, Inst Geog & Geoecol, D-76131 Karlsruhe, Germany. [Fischer, Markus] Senckenberg Gesell Nat Forsch Biodivers & Climate, D-60325 Frankfurt, Germany. [Fischer, Markus] Univ Potsdam, Biodivers Res Systemat Bot, D-14469 Potsdam, Germany. RP Allan, E (reprint author), Univ Bern, Inst Plant Sci, Altenbergrain 21, CH-3013 Bern, Switzerland. EM eric.allan@ips.unibe.ch RI Schoning, Ingo/D-3341-2009; Manning, Peter/I-6523-2012; Bluthgen, Nico/F-5983-2010; Westphal, Catrin/F-9560-2015; Fischer, Markus/C-6411-2008; Weisser, Wolfgang/B-9718-2014; Schrumpf, Marion/C-1671-2013; Oelmann, Yvonne/J-8730-2016; Wilcke, Wolfgang/P-4620-2016; Holzel, Norbert/H-8753-2013; Rillig, Matthias/B-3675-2009; OI Solly, Emily/0000-0002-3157-1805; Renner, Swen/0000-0002-6893-4219; Schoning, Ingo/0000-0002-9830-5026; Manning, Peter/0000-0002-7940-2023; Westphal, Catrin/0000-0002-2615-1339; Fischer, Markus/0000-0002-5589-5900; Weisser, Wolfgang/0000-0002-2757-8959; Oelmann, Yvonne/0000-0003-3513-6568; Wilcke, Wolfgang/0000-0002-6031-4613; Rillig, Matthias/0000-0003-3541-7853; Weiner, Christiane/0000-0003-4013-4663 FU Deutsche Forschungsgemeinschaft Priority Program 1374 'Infrastructure-Biodiversity Exploratories' FX We thank Robert Bagchi, Santiago Soliveres, Owen Petchey and Teja Tscharntke for comments on the manuscript. We also thank the managers of the three exploratories, Sonja Gockel, Kerstin Wiesner and Martin Gorke for their work in maintaining the plot and project infrastructure; Simone Pfeiffer and Christiane Fischer giving support through the central office, Birgitta Konig-Ries and Michael Owonibi for managing the central database, and Eduard Linsenmair, Dominik Hessenmoller, Jens Nieschulze, Francois Buscot, Ernst-Detlef Schulze, and the late Elisabeth Kalko for their role in setting up the Biodiversity Exploratories project. This work was funded by the Deutsche Forschungsgemeinschaft Priority Program 1374 'Infrastructure-Biodiversity Exploratories.' Fieldwork permits were given by the responsible state environmental offices of Baden-Wurttemberg, Thuringen and Brandenburg (according to 72 Brandenburgisches Naturschutzgesetz). NR 47 TC 22 Z9 23 U1 32 U2 206 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 AUG PY 2015 VL 18 IS 8 BP 834 EP 843 DI 10.1111/ele.12469 PG 10 WC Ecology SC Environmental Sciences & Ecology GA CM8NO UT WOS:000357958900011 PM 26096863 ER PT J AU Yingst, RA Russell, P ten Kate, IL Noble, S Graff, T Graham, LD Eppler, D AF Yingst, R. A. Russell, P. ten Kate, I. L. Noble, S. Graff, T. Graham, L. D. Eppler, D. TI Designing remote operations strategies to optimize science mission goals: Lessons learned from the Moon Mars Analog Mission Activities Mauna Kea 2012 field test SO ACTA ASTRONAUTICA LA English DT Article DE Apollo Valley geologic map; Science operations; MER ID MIMOS-II; EXPLORATION; HAWAII; ROVER AB The Moon Mars Analog Mission Activities Mauna Kea 2012 (MMAMA 2012) field campaign aimed to assess how effectively an integrated science and engineering rover team operating on a 24-h planning cycle facilitates high-fidelity science products. The science driver of this field campaign was to determine the origin of a glacially-derived deposit: was the deposit the result of (1) glacial outwash from meltwater; or (2) the result of an ice dam breach at the head of the valley? Lessons learned from MMAMA 2012 science operations include: (1) current rover science operations scenarios tested in this environment provide adequate data to yield accurate derivative products such as geologic maps; (2) instrumentation should be selected based on both engineering and science goals; and chosen during, rather than after, mission definition; and (3) paralleling the tactical and strategic science processes provides significant efficiencies that impact science return. The MER-model concept of operations utilized, in which rover operators were sufficiently facile with science intent to alter traverse and sampling plans during plan execution, increased science efficiency, gave the Science Backroom time to develop mature hypotheses and science rationales, and partially alleviated the problem of data flow being greater than the processing speed of the scientists. (C) 2015 IAA. Published by Elsevier Ltd. on behalf of IAA. This is an open access article under the CC BY-NC-ND license (http://creativecommons.org/licensesiby-nc-nd/4.0/). C1 [Yingst, R. A.] Planetary Sci Inst, Tucson, AZ 85719 USA. [Russell, P.] Smithsonian Inst, Natl Air & Space Museum, Washington, DC 20013 USA. [ten Kate, I. L.] Univ Utrecht, Dept Earth Sci, Fac Geosci, Utrecht, Netherlands. [Noble, S.] NASA Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Graff, T.] NASA Johnson Space Ctr, Houston, TX 77058 USA. [Graham, L. D.; Eppler, D.] NASA Johnson Space Ctr, Houston, TX 77058 USA. RP Yingst, RA (reprint author), Planetary Sci Inst, 1700 E Ft Lowell St, Tucson, AZ 85719 USA. EM yingst@psi.edu; russellp@si.edu; i.l.tenkate@uu.nl; sarah.noble@nasa.gov; trevor.g.graff@nasa.gov; lee.d.graham@nasa.gov; dean.b.eppler@nasa.gov FU NASA MMAMA program [NNX12AM27G]; MMAMA program grant FX We gratefully acknowledge the work of the Rover Team and their JUNO II rover, which performed like a true wahine koa (warrior woman), making this field test possible. We also acknowledge the comments of Dr. John Moores and an anonymous reviewer that greatly improved this manuscript. This work was supported by NASA MMAMA program, Grant NNX12AM27G to RAY and an additional MMAMA program grant to ILtK. NR 31 TC 1 Z9 1 U1 1 U2 7 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0094-5765 EI 1879-2030 J9 ACTA ASTRONAUT JI Acta Astronaut. PD AUG-SEP PY 2015 VL 113 BP 120 EP 131 DI 10.1016/j.actaastro.2015.02.029 PG 12 WC Engineering, Aerospace SC Engineering GA CL8RA UT WOS:000357240600011 ER PT J AU Powell, LL Cordeiro, NJ Stratford, JA AF Powell, Luke L. Cordeiro, Norbert J. Stratford, Jeffrey A. TI Ecology and conservation of avian insectivores of the rainforest understory: A pantropical perspective SO BIOLOGICAL CONSERVATION LA English DT Article DE Understory insectivores; Rainforests; Pantropical; Fragmentation; Deforestation; Mixed species flocks ID ANT-FOLLOWING BIRDS; BARRO-COLORADO ISLAND; MIXED-SPECIES FLOCKS; TROPICAL FOREST; NEST PREDATION; NEOTROPICAL FOREST; HABITAT FRAGMENTATION; AMAZONIAN BIRDS; MULTISPECIES TERRITORIALITY; BIODIVERSITY CONSERVATION AB Avian insectivores of the tropical rainforest understory ("understory insectivores") are common, diverse, and often sensitive to disturbance of tropical forest, making them useful as sentinels of rainforest ecosystem change. At the 2013 joint American Ornithologists' Union and Cooper Ornithological Society meeting in Chicago, USA, researchers convened a symposium to address the ecology and conservation of understory insectivores. This Special Issue of Biological Conservation is the result of that symposium: a collection of articles that unites our efforts to further understand and conserve understory insectivores. In this introductory paper, we review the diversity and ecology of understory insectivores, identify threats to the guild, discuss hypotheses on drivers of population declines, and make suggestions for future research. Deforestation and forest degradation are the immediate threats to this guild, with agricultural expansion (particularly oil palm plantations), urbanization, road expansion and logging leading the list. Although vulnerabilities of this guild are most evident in the Neotropics, there are few studies from Asia and fewer still from Africa we recommend increased geographic coverage. If we are to understand the vulnerabilities of understory insectivores from a pantropical perspective, researchers should prioritize understanding the most serious threats (e.g., edge effects, deforestation, fragmentation, etc.) and standardize efforts to gauge understory insectivores' response to these threats (e.g., via species richness, abundance, demographic metrics). A coordinated approach by researchers working in tropical rainforests across the globe can help us understand the ecology of understory insectivores and meaningfully apply conservation and management actions. Published by Elsevier Ltd. C1 [Powell, Luke L.; Stratford, Jeffrey A.] Inst Nacl de Pesquisas da Amazonia, Biol Dynam Forest Fragments Project, BR-69011097 Manaus, Amazonas, Brazil. [Powell, Luke L.] Louisiana State Univ, RNR 227, Sch Renewable Nat Resources, Baton Rouge, LA 70803 USA. [Powell, Luke L.] Louisiana State Univ, Ctr Agr, Baton Rouge, LA 70803 USA. [Cordeiro, Norbert J.] Roosevelt Univ, Dept Biol Chem & Phys Sci, Chicago, IL 60605 USA. [Cordeiro, Norbert J.] Field Museum, Life Sci Sci & Educ, Chicago, IL 60605 USA. [Stratford, Jeffrey A.] Wilkes Univ, Dept Biol & Hlth Sci, Wilkes Barre, PA 18766 USA. RP Powell, LL (reprint author), Natl Zool Pk, Smithsonian Conservat Biol Inst, Migratory Bird Ctr, Washington, DC 20013 USA. EM Luke.L.Powell@gmail.com NR 150 TC 17 Z9 17 U1 14 U2 95 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 0006-3207 EI 1873-2917 J9 BIOL CONSERV JI Biol. Conserv. PD AUG PY 2015 VL 188 SI SI BP 1 EP 10 DI 10.1016/j.biocon.2015.03.025 PG 10 WC Biodiversity Conservation; Ecology; Environmental Sciences SC Biodiversity & Conservation; Environmental Sciences & Ecology GA CL8LG UT WOS:000357225600001 ER PT J AU Powell, LL Wolfe, JD Johnson, EI Hines, JE Nichols, JD Stouffer, PC AF Powell, Luke L. Wolfe, Jared D. Johnson, Erik I. Hines, James E. Nichols, James D. Stouffer, Philip C. TI Heterogeneous movement of insectivorous Amazonian birds through primary and secondary forest: A case study using multistate models with radiotelemetry data SO BIOLOGICAL CONSERVATION LA English DT Article DE Amazon; Fidelity fragmentation; Neotropical birds; Secondary forest; Multistate models; Movement probability ID ALTERNATIVE SUCCESSIONAL PATHWAYS; RAIN-FOREST; BRAZILIAN AMAZONIA; CAPTURE-RECAPTURE; SPECIES RESPONSES; NEOTROPICAL BIRDS; UNDERSTORY BIRDS; LANDSCAPE CHANGE; HABITAT QUALITY; MARKED ANIMALS AB Given rates of deforestation, disturbance, and secondary forest accumulation in tropical rainforests, there is a great need to quantify habitat use and movement among different habitats. This need is particularly pronounced for animals most sensitive to disturbance, such as insectivorous understory birds. Here we use multistate capture-recapture models with radiotelemetry data to determine the successional stage at which within-day movement probabilities of Amazonian birds in secondary forest are similar to those in primary forest. We radio-tracked three common understory insectivore species in primary and secondary forest at the Biological Dynamics of Forest Fragments project near Manaus, Brazil: two woodcreepers, Glyphorynchus spirurus (n = 19) and Xiphorhynchus pardalotus (n = 18), and the terrestrial antthrush Formicarius colma (n = 19). Forest age was a strong predictor of fidelity to a given habitat. All three species showed greater fidelity to primary forest than to 8-14-year-old secondary forest, indicating the latter's relatively poor quality. The two woodcreeper species used 12-18-year-old secondary forest in a manner comparable to continuous forest, but F. colma avoided moving even to 27-31-year-old secondary forest the oldest at our site. Our results suggest that managers concerned with less sensitive species can assume that forest reserves connected by 12-18-year-old secondary forest corridors are effectively connected. On the other hand, >30 years are required after land abandonment before secondary forest serves as a primary forest-like conduit for movement by F. colma; more sensitive terrestrial insectivores may take longer still. Published by Elsevier Ltd. C1 [Powell, Luke L.; Wolfe, Jared D.; Johnson, Erik I.; Stouffer, Philip C.] Inst Nacl de Pesquisas da Amazonia, Biol Dynam Forest Fragments Project, BR-69011097 Manaus, Amazonas, Brazil. [Powell, Luke L.; Wolfe, Jared D.; Johnson, Erik I.; Stouffer, Philip C.] Louisiana State Univ, RNR 227, Sch Renewable Nat Resources, Baton Rouge, LA 70803 USA. [Powell, Luke L.; Wolfe, Jared D.; Johnson, Erik I.; Stouffer, Philip C.] Louisiana State Univ, Ctr Agr, Baton Rouge, LA 70803 USA. [Hines, James E.; Nichols, James D.] Patuxent Wildlife Res Ctr, USGS Biol Resources Div, Laurel, MD 20708 USA. RP Powell, LL (reprint author), Natl Zool Pk, Smithsonian Conservat Biol Inst, Migratory Bird Ctr, Washington, DC 20013 USA. EM Luke.L.Powell@gmail.com FU U.S. National Science Foundation [LTREB 0545491]; American Union of Ornithologists' Research Award; American Union of Ornithologists' Frank M. Chapman Award; Wilson Ornithological Society's Paul A. Stewart Award; American Philosophical Society's Lewis Clark Fund FX We thank Paul Des Brisay, Marconi Cerqueira, Elizabeth Condon, Camila Duarte, Gilberto Fernandez Arellano, Jairo Lopes, Alercio Marajo de Reis, Rachelle McLaughlin, Karl Mokross, Osmaildo, Aida Rodrigues, and Tatiana Straatmann for their contributions in the field. The LSU "Bird Lunch" group, Kristina Cockle, Norbert Cordeiro, Kyle Harms, Michael Kaller, Curtis Marantz, Michael Lefsky, Michael Patten, Scott Saleska, Bret Sandercock, Jeff Stratford, Stefan Woltmann, J. Van Remsen and several anonymous reviewers had important contributions, including insightful reviews and advice on data analyses. We thank the following funding sources: U.S. National Science Foundation (LTREB 0545491), American Union of Ornithologists' Research Award, the American Union of Ornithologists' Frank M. Chapman Award, the Wilson Ornithological Society's Paul A. Stewart Award, and the American Philosophical Society's Lewis & Clark Fund. We conducted this research under ISU Institutional Animal Care and Use Committee approval and under applicable Brazilian permits. This is publication number 660 in the BDFFP technical series and number 37 in the Amazonian ornithology technical series. This manuscript was approved for publication by the Director of the Louisiana Agricultural Experimental Station as manuscript number 2015-241-20967. NR 76 TC 9 Z9 9 U1 6 U2 41 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 0006-3207 EI 1873-2917 J9 BIOL CONSERV JI Biol. Conserv. PD AUG PY 2015 VL 188 SI SI BP 100 EP 108 DI 10.1016/j.biocon.2015.01.028 PG 9 WC Biodiversity Conservation; Ecology; Environmental Sciences SC Biodiversity & Conservation; Environmental Sciences & Ecology GA CL8LG UT WOS:000357225600011 ER PT J AU Yang, XH Cushman, JC Borland, AM Edwards, EJ Wullschleger, SD Tuskan, GA Owen, NA Griffiths, H Smith, JAC De Paoli, HC Weston, DJ Cottingham, R Hartwell, J Davis, SC Silvera, K Ming, R Schlauch, K Abraham, P Stewart, JR Guo, HB Albion, R Ha, JM Lim, SD Wone, BWM Yim, WC Garcia, T Mayer, JA Petereit, J Nair, SS Casey, E Hettich, RL Ceusters, J Ranjan, P Palla, KJ Yin, HF Reyes-Garcia, C Andrade, JL Freschi, L Beltran, JD Dever, LV Boxall, SF Waller, J Davies, J Bupphada, P Kadu, N Winter, K Sage, RF Aguilar, CN Schmutz, J Jenkins, J Holtum, JAM AF Yang, Xiaohan Cushman, John C. Borland, Anne M. Edwards, Erika J. Wullschleger, Stan D. Tuskan, Gerald A. Owen, Nick A. Griffiths, Howard Smith, J. Andrew C. De Paoli, Henrique C. Weston, David J. Cottingham, Robert Hartwell, James Davis, Sarah C. Silvera, Katia Ming, Ray Schlauch, Karen Abraham, Paul Stewart, J. Ryan Guo, Hao-Bo Albion, Rebecca Ha, Jungmin Lim, Sung Don Wone, Bernard W. M. Yim, Won Cheol Garcia, Travis Mayer, Jesse A. Petereit, Juli Nair, Sujithkumar S. Casey, Erin Hettich, Robert L. Ceusters, Johan Ranjan, Priya Palla, Kaitlin J. Yin, Hengfu Reyes-Garcia, Casandra Luis Andrade, Jose Freschi, Luciano Beltran, Juan D. Dever, Louisa V. Boxall, Susanna F. Waller, Jade Davies, Jack Bupphada, Phaitun Kadu, Nirja Winter, Klaus Sage, Rowan F. Aguilar, Cristobal N. Schmutz, Jeremy Jenkins, Jerry Holtum, Joseph A. M. TI A roadmap for research on crassulacean acid metabolism (CAM) to enhance sustainable food and bioenergy production in a hotter, drier world SO NEW PHYTOLOGIST LA English DT Article DE bioenergy; crassulacean acid metabolism (CAM); drought; genomics; photosynthesis; roadmap; synthetic biology; water-use efficiency (WUE) ID COMMON ICE PLANT; CARBON-ISOTOPE RATIOS; PORTULACA-OLERACEA L; MESEMBRYANTHEMUM-CRYSTALLINUM; C-4 PHOTOSYNTHESIS; POPULATION PROJECTIONS; REGULATORY NETWORKS; ADAPTIVE RADIATION; SEDUM-TELEPHIUM; EXPRESSION AB Crassulacean acid metabolism (CAM) is a specialized mode of photosynthesis that features nocturnal CO2 uptake, facilitates increased water-use efficiency (WUE), and enables CAM plants to inhabit water-limited environments such as semi-arid deserts or seasonally dry forests. Human population growth and global climate change now present challenges for agricultural production systems to increase food, feed, forage, fiber, and fuel production. One approach to meet these challenges is to increase reliance on CAM crops, such as Agave and Opuntia, for biomass production on semi-arid, abandoned, marginal, or degraded agricultural lands. Major research efforts are now underway to assess the productivity of CAM crop species and to harness the WUE of CAM by engineering this pathway into existing food, feed, and bioenergy crops. An improved understanding of CAM has potential for high returns on research investment. To exploit the potential of CAM crops and CAM bioengineering, it will be necessary to elucidate the evolution, genomic features, and regulatory mechanisms of CAM. Field trials and predictive models will be required to assess the productivity of CAM crops, while new synthetic biology approaches need to be developed for CAM engineering. Infrastructure will be needed for CAM model systems, field trials, mutant collections, and data management. C1 [Yang, Xiaohan; Borland, Anne M.; De Paoli, Henrique C.; Weston, David J.; Cottingham, Robert; Ranjan, Priya; Palla, Kaitlin J.] Oak Ridge Natl Lab, Biosci Div, Oak Ridge, TN 37831 USA. [Cushman, John C.; Albion, Rebecca; Ha, Jungmin; Lim, Sung Don; Wone, Bernard W. M.; Yim, Won Cheol; Garcia, Travis; Mayer, Jesse A.] Univ Nevada, Dept Biochem & Mol Biol, Reno, NV 89557 USA. [Borland, Anne M.; Casey, Erin] Newcastle Univ, Sch Biol, Newcastle Upon Tyne NE1 7RU, Tyne & Wear, England. [Edwards, Erika J.] Brown Univ, Dept Ecol & Evolutionary Biol, Providence, RI 02912 USA. [Wullschleger, Stan D.; Nair, Sujithkumar S.] Oak Ridge Natl Lab, Div Environm Sci, Oak Ridge, TN 37831 USA. [Owen, Nick A.; Griffiths, Howard] Univ Cambridge, Dept Plant Sci, Cambridge CB2 3EA, England. [Smith, J. Andrew C.; Beltran, Juan D.] Univ Oxford, Dept Plant Sci, Oxford OX1 3RB, England. [Hartwell, James; Dever, Louisa V.; Boxall, Susanna F.; Waller, Jade; Davies, Jack; Bupphada, Phaitun; Kadu, Nirja] Univ Liverpool, Inst Integrat Biol, Dept Plant Sci, Liverpool L69 7ZB, Merseyside, England. [Davis, Sarah C.] Ohio Univ, Voinovich Sch Leadership & Publ Affairs, Athens, OH 45701 USA. [Davis, Sarah C.] Ohio Univ, Dept Environm & Plant Biol, Athens, OH 45701 USA. [Silvera, Katia; Winter, Klaus] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. [Ming, Ray] Univ Illinois, Dept Plant Biol, Urbana, IL 61801 USA. [Ming, Ray] Fujian Agr & Forestry Univ, FAFU & UIUC SIB Joint Ctr Genom & Biotechnol, Fuzhou 350002, Peoples R China. [Schlauch, Karen; Petereit, Juli] Univ Nevada, Nevada Ctr Bioinformat, Reno, NV 89557 USA. [Abraham, Paul; Hettich, Robert L.] Oak Ridge Natl Lab, Div Chem Sci, Oak Ridge, TN 37831 USA. [Stewart, J. Ryan] Brigham Young Univ, Dept Plant & Wildlife Sci, Provo, UT 84602 USA. [Guo, Hao-Bo] Univ Tennessee, Dept Biochem & Cellular & Mol Biol, Knoxville, TN 37996 USA. [Ceusters, Johan] Katholieke Univ Leuven, Fac Engn Technol, TC Bioengn Technol, Dept M2S, B-2440 Geel, Belgium. [Yin, Hengfu] Chinese Acad Forestry, Res Inst Subtrop Forestry, Key Lab Forest Genet & Breeding, Fuyang 311400, Peoples R China. [Reyes-Garcia, Casandra; Luis Andrade, Jose] Ctr Invest Cient Yucatan, Colonia Chuburna De Hida 97200, Merida, Mexico. [Freschi, Luciano] Univ Sao Paulo, Dept Bot, BR-05508090 Sao Paulo, Brazil. [Sage, Rowan F.] Univ Toronto, Dept Ecol & Evolutionary Biol, Toronto, ON M5S 3B2, Canada. [Aguilar, Cristobal N.] Univ Autonoma Coahuila, Sch Chem, Dept Food Res, Saltillo, Coahuila, Mexico. [Schmutz, Jeremy; Jenkins, Jerry] HudsonAlpha Inst Biotechnol, Huntsville, AL 35801 USA. [Schmutz, Jeremy] US DOE, Joint Genome Inst, Walnut Creek, CA 94598 USA. [Holtum, Joseph A. M.] James Cook Univ, Coll Marine & Environm Sci, Townsville, Qld 4811, Australia. RP Yang, XH (reprint author), Oak Ridge Natl Lab, Biosci Div, Oak Ridge, TN 37831 USA. EM yangx@ornl.gov RI Yin, Hengfu/H-1695-2012; Yang, Xiaohan/A-6975-2011; Abraham, Paul/K-5599-2015; Research ID, CTBCC /O-3564-2014; Hartwell, James/M-7249-2014; Guo, Hao-Bo/B-7486-2009; Yim, Won Cheol/K-9100-2016; Wullschleger, Stan/B-8297-2012; Hettich, Robert/N-1458-2016; Tuskan, Gerald/A-6225-2011; OI Yin, Hengfu/0000-0002-0720-5311; Yang, Xiaohan/0000-0001-5207-4210; De Paoli, Henrique/0000-0001-8494-0603; Hartwell, James/0000-0001-5000-223X; Guo, Hao-Bo/0000-0003-1321-1758; Yim, Won Cheol/0000-0002-7489-0435; Wullschleger, Stan/0000-0002-9869-0446; Hettich, Robert/0000-0001-7708-786X; Tuskan, Gerald/0000-0003-0106-1289; Mayer, Jesse/0000-0001-9839-5001 FU Biotechnology and Biological Sciences Research Council [BB/F009313/1] NR 95 TC 23 Z9 23 U1 11 U2 83 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0028-646X EI 1469-8137 J9 NEW PHYTOL JI New Phytol. PD AUG PY 2015 VL 207 IS 3 BP 491 EP 504 DI 10.1111/nph.13393 PG 14 WC Plant Sciences SC Plant Sciences GA CM6TZ UT WOS:000357824400005 PM 26153373 ER PT J AU Berger, MA Asgari-Targhi, M DeLuca, EE AF Berger, M. A. Asgari-Targhi, M. DeLuca, E. E. TI Self-organized braiding in solar coronal loops SO JOURNAL OF PLASMA PHYSICS LA English DT Article ID ALFVEN-WAVE TURBULENCE; FLUX TUBES; RECONNECTION; CRITICALITY AB In this paper, we investigate the evolution of braided solar coronal loops. We assume that coronal loops consist of several internal strands which twist and braid about each other. Reconnection between the strands leads to small flares and heating of the loop to x-ray temperatures. Using a method of generating and releasing braid structure similar to a forest fire model, we show that the reconnected field lines evolve to a self-organised critical state. In this state, the frequency distributions of coherent braid sequences as well as flare energies follow power law distributions. We demonstrate how the presence of net helicity in the loop alters the distribution laws. C1 [Berger, M. A.] Univ Exeter, CEMPS, Exeter EX4 4QF, Devon, England. [Asgari-Targhi, M.; DeLuca, E. E.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Berger, MA (reprint author), Univ Exeter, CEMPS, Exeter EX4 4QF, Devon, England. EM m.berger@exeter.ac.uk RI DeLuca, Edward/L-7534-2013 OI DeLuca, Edward/0000-0001-7416-2895 FU Leverhulme Trust [SH-04409]; AIA [SP02H1701R] FX M. Berger is happy to thank the Leverhulme Trust grant SH-04409 which helped support this research. M. Asgari-Targhi and E.E. DeLuca are supported by the AIA contract SP02H1701R. NR 20 TC 0 Z9 0 U1 0 U2 7 PU CAMBRIDGE UNIV PRESS PI NEW YORK PA 32 AVENUE OF THE AMERICAS, NEW YORK, NY 10013-2473 USA SN 0022-3778 EI 1469-7807 J9 J PLASMA PHYS JI J. Plasma Phys. PD AUG PY 2015 VL 81 AR 395810404 DI 10.1017/S0022377815000483 PN 4 PG 13 WC Physics, Fluids & Plasmas SC Physics GA CK7TO UT WOS:000356436400017 ER PT J AU Dieleman, J Van Bocxlaer, B Manntschke, C Nyingi, DW Adriaens, D Verschuren, D AF Dieleman, Jorunn Van Bocxlaer, Bert Manntschke, Claudia Nyingi, Dorothy Wanja Adriaens, Dominique Verschuren, Dirk TI Tracing functional adaptation in African cichlid fishes through morphometric analysis of fossil teeth: exploring the methods SO HYDROBIOLOGIA LA English DT Article DE Cichlidae; Geometric morphometrics; Fish fossils; Adaptive modification; Tooth morphology; Africa ID LAKE MALAWI; PHENOTYPIC PLASTICITY; ADAPTIVE RADIATION; EAST-AFRICA; BODY SHAPE; SPECIATION; TANGANYIKA; EVOLUTION; RECORD AB The sedimentary archive of Crater Lake Challa in East Africa contains abundant fossil teeth of cichlid fishes throughout at least the last 25,000 years. Here, we use morphometric analyses of oral teeth from the two extant Oreochromis species inhabiting Lake Challa to explore the feasibility of tracing adaptive modification of the cichlid trophic apparatus in the lake's fossil record. We compared the performance of semi-landmark analysis (SLM) and elliptic Fourier analysis in capturing morphological variation in oral tooth crowns, and found that SLM, supplemented with tooth shaft measurements, ensured consistency with whole-body landmark analyses. Whole-body and tooth morphology data both allowed to discern between the indigenous Oreochromis hunteri and the recently introduced Oreochromis korogwe. Both species have an oral jaw arrangement of outer-row bicuspid and inner-rows tricuspid teeth, but O. hunteri has generally more slender teeth with a proportionally taller major cusp than O. korogwe, suggesting fine-scaled resource partitioning. Exploratory analysis of three fossil samples showed that the major tooth types of modern-day Oreochromis are also represented in the fossil record. Their total morphological variation is largely restricted to the morphospace occupied by contemporary teeth, suggesting a close functional relationship between ancient populations and their likely descendant, O. hunteri. C1 [Dieleman, Jorunn; Van Bocxlaer, Bert; Manntschke, Claudia; Verschuren, Dirk] Univ Ghent, Dept Biol, Limnol Unit, B-9000 Ghent, Belgium. [Van Bocxlaer, Bert] Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20013 USA. [Van Bocxlaer, Bert] Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, Washington, DC 20013 USA. [Van Bocxlaer, Bert] Univ Giessen, Dept Anim Ecol & Systemat, D-35392 Giessen, Germany. [Nyingi, Dorothy Wanja] Natl Museums Kenya, Ichthyol Sect, Dept Zool, Nairobi, Kenya. [Adriaens, Dominique] Univ Ghent, Dept Biol, Evolutionary Morphol Vertebrates, B-9000 Ghent, Belgium. RP Dieleman, J (reprint author), Univ Ghent, Dept Biol, Limnol Unit, KL Ledeganckstr 35, B-9000 Ghent, Belgium. EM jorunn.dieleman@ugent.be RI Van Bocxlaer, Bert/N-1965-2016 OI Van Bocxlaer, Bert/0000-0003-2033-326X FU CRA program of the Ghent University Research Council; Smithsonian Institution; Alexander von Humboldt Foundation; Flanders Research Foundation FX We thank Caxton Oluseno and the fishermen of Lake Challa for field assistance, Jos Snoeks for taxonomic information and Tom Geerinckx and Philippe Munyandamutsa for help with jaw and teeth preparation protocols. Moritz Muschick and an anonymous referee provided many useful suggestions that substantially improved the paper. The lake-sediment cores used in this study were collected under permit 13/001/11C of the Kenyan Ministry of Education, Science and Technology, in the framework of the European Science Foundation's EuroCLIMATE project CHALLACEA. This work is financed by the CRA program of the Ghent University Research Council to D.V., and by postdoctoral fellowships of the Smithsonian Institution, the Alexander von Humboldt Foundation and the Flanders Research Foundation to B. V. B. NR 54 TC 4 Z9 4 U1 13 U2 30 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0018-8158 EI 1573-5117 J9 HYDROBIOLOGIA JI Hydrobiologia PD AUG PY 2015 VL 755 IS 1 BP 73 EP 88 DI 10.1007/s10750-015-2218-0 PG 16 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA CK2KM UT WOS:000356039300006 ER PT J AU Dangremond, EM AF Dangremond, Emily M. TI Propagule predation by crabs limits establishment of an endemic mangrove SO HYDROBIOLOGIA LA English DT Article DE Seed predation; Refugia; Mangrove; Recruitment; Crab; Pelliciera rhizophorae ID PLANT-POPULATION DYNAMICS; SEED PREDATION; LAND CRABS; INTERTIDAL DISTRIBUTION; RAIN-FOREST; RECRUITMENT; HYPOTHESIS; DOMINANCE; ECOLOGY; DISTRIBUTIONS AB Recruitment of seedlings is crucial to the establishment and maintenance of plant populations and species ranges. Seed predation by crabs is prevalent in mangroves globally, but the importance of predation on mangrove abundance and distribution relative to other factors remain unclear. The rare Neotropical mangrove Pelliciera rhizophorae occurs in freshwater-influenced sites, and may lose many of its propagules to crab predation in other locations. Propagules of P. rhizophorae were placed in either Rhizophora mangle or P. rhizophorae-dominated forests on the Caribbean and Pacific coasts of Panama. On the Caribbean coast, crabs consumed 86.7% of propagules in the R. mangle forest but only 3.3% of propagules in the P. rhizophorae zone. On the Pacific coast, crabs consumed 90% of propagules in the R. mangle zone and 66.7% in the P. rhizophorae zone. When crab exclosures were used, seedling survival did not vary between forest types, suggesting that predation, rather than seedling survival once established, limits P. rhizophorae populations. Rhizophora mangle produces an order of magnitude more propagules per capita than P. rhizophorae and may well satiate its crab predators. The low salinity forest stands may provide a refuge from crab predation for the rare mangrove P. rhizophorae. C1 [Dangremond, Emily M.] Univ Calif Berkeley, Dept Integrat Biol, Berkeley, CA 94720 USA. RP Dangremond, EM (reprint author), Smithsonian Environm Res Ctr, 647 Contees Wharf Rd, Edgewater, MD 21307 USA. EM dangremonde@si.edu FU National Science Foundation FX Wayne Sousa, Paul Fine, Perry de Valpine, and Ilka Feller and an anonymous reviewer provided helpful comments on early versions of this paper. Sierra Flynn and Jorge Morales helped complete fieldwork. Funding was provided by the National Science Foundation Graduate Research Fellowship Program. Thanks to the Smithsonian Tropical Research Institute for use of their facilities at Punta Galeta and Bocas del Toro. NR 42 TC 1 Z9 1 U1 5 U2 22 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0018-8158 EI 1573-5117 J9 HYDROBIOLOGIA JI Hydrobiologia PD AUG PY 2015 VL 755 IS 1 BP 257 EP 266 DI 10.1007/s10750-015-2238-9 PG 10 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA CK2KM UT WOS:000356039300018 ER PT J AU Quinones, AE Wcislo, WT AF Quinones, A. E. Wcislo, W. T. TI Cryptic extended brood care in the facultatively eusocial sweat bee Megalopta genalis SO INSECTES SOCIAUX LA English DT Article DE Extended maternal care; Hygienic behavior; Megalopta genalis; Subsociality; Undertaking behavior; Eusociality ID ASSURED FITNESS RETURNS; ECUADORIA HYMENOPTERA; HALICTIDAE; EVOLUTION; INSECTS; SOCIALITY; LIFE AB As a result of different brood cell provisioning strategies, nest-making insects may differ in the extent to which adults regularly provide extended parental care to their brood beyond nest defense. Mass-provisioning species cache the entire food supply needed for larval development prior to the oviposition and typically seal the brood cell. It is usually assumed that there is no regular contact between the adult(s) and brood. Here, we show that the bee, Megalopta genalis, expresses a form of cryptic brood care, which would not be observed during normal development. Following experimental injections of different provisioning materials into brood cells, foundresses reopened manipulated cells and the brood were aborted in some cases, implying that the foundresses assessed conditions within the cells. In aborted cells, foundresses sometimes laid a second egg after first removing dead larvae, previously stored pollen and contaminants. Our results show that hygienic brood care can be cryptic and hence may be more widespread than previously believed, lending support to the hypothesis that extended parental care is a preadaptation toward eusociality. C1 [Quinones, A. E.] Univ Groningen, Theoret Biol Grp, NL-9747 AG Groningen, Netherlands. [Wcislo, W. T.] Smithsonian Trop Res Inst, Balboa 084303092, Apartado, Panama. RP Quinones, AE (reprint author), Univ Groningen, Theoret Biol Grp, Nijenborgh 7, NL-9747 AG Groningen, Netherlands. EM a.e.quinones.paredes@rug.nl FU Groningen University Fund (GUF); Marco Polo fund; Top master scholarship of the University of Groningen; STRI FX We thank Kate Ihle, Quinn McFrederick and Lizzette Jimenez for their help in the field during the data collection, Esther Chang for her helpful comments on the manuscript and Ido Pen for statistical advice. Finally, we would like to thank Associate Editor Dr. Miriam Richards and three anonymous reviewers for considerable help in improving the manuscript. AEQ was funded by Groningen University Fund (GUF), the Marco Polo fund and the Top master scholarship of the University of Groningen, and additional support was provided by general research funds from STRI to WTW. NR 33 TC 3 Z9 3 U1 1 U2 8 PU SPRINGER BASEL AG PI BASEL PA PICASSOPLATZ 4, BASEL, 4052, SWITZERLAND SN 0020-1812 EI 1420-9098 J9 INSECT SOC JI Insect. Soc. PD AUG PY 2015 VL 62 IS 3 BP 307 EP 313 DI 10.1007/s00040-015-0409-3 PG 7 WC Entomology SC Entomology GA CK5NM UT WOS:000356271800008 ER PT J AU Rabeling, C Schultz, TR Bacci, M Bollazzi, M AF Rabeling, C. Schultz, T. R. Bacci, M., Jr. Bollazzi, M. TI Acromyrmex charruanus: a new inquiline social parasite species of leaf-cutting ants SO INSECTES SOCIAUX LA English DT Article DE Leaf-cutter ants; Fungus-growing ants; Attini; Social parasitism; Inquilinism; Acromyrmex; Pseudoatta ID FUNGUS-GROWING ANTS; HYMENOPTERA-FORMICIDAE; SYMPATRIC SPECIATION; LEAFCUTTER ANT; EVOLUTION; HOST; COLONIES; BEHAVIOR; ATTINI; ORGANIZATION AB Social parasites exploit the colony resources of social species to secure their own survival and reproduction. Social parasites are frequently studied as models for conflict and cooperation as well as for speciation. The eusocial Hymenoptera harbor a diverse array of socially parasitic species with idiosyncratic life history strategies, but it is probably in the ants where social parasites are most speciose and have evolved the highest degrees of morphological and behavioral specialization. In the fungus-growing ants, a total of five obligate social parasites are known: four species are parasites of leaf-cutting ants and one species parasitizes a primitive fungus-growing ant species in the genus Mycocepurus. Here we describe a new species of socially parasitic leaf-cutting ant, Acromyrmex charruanus sp. nov., from Uruguay, and we report initial observations on the parasite's life history as well as on the morphological and behavioral adaptations related to the inquiline syndrome. Our observations suggest that Acromyrmex charruanus is an obligate inquiline social parasite of the thatch-mound-building, leaf-cutting ant Acromyrmex heyeri. Acromyrmex charruanus appears to be tolerant of the host, producing sexual offspring in the presence of the A. heyeri host queen. Queens of A. charruanus appear to reproduce semelparously and sexual offspring are produced during the austral fall (February), which differs significantly from the mating biology of the host species, which reproduces during the southern-hemisphere spring (October-December). We suggest that the diametrically opposed mating seasons of parasite and host might be adaptive, allowing the parasite to avoid competition for resources with the host sexual brood. The morphological and behavioral adaptations of A. charruanus accord with characters observed to arise early during the evolution of other ant inquiline parasite species, and so far we have no evidence for the existence of a worker caste in A. charruanus. Further field studies and behavioral experiments need to confirm our first observations and explore A. charruanus's behavioral ecology, evolution, and life history in more detail. C1 [Rabeling, C.] Univ Rochester, Dept Biol, Rochester, NY 14627 USA. [Schultz, T. R.] Smithsonian Inst, Dept Entomol, Natl Museum Nat Hist, Washington, DC 20560 USA. [Bacci, M., Jr.] Sao Paulo State Univ, Ctr Study Social Insects, BR-13506900 Rio Claro, SP, Brazil. [Bollazzi, M.] Univ Republica, Fac Agron, Sect Entomol, Montevideo 12900, Uruguay. RP Rabeling, C (reprint author), Univ Rochester, Dept Biol, Rochester, NY 14627 USA. EM crabeling@gmail.com FU National Science Foundation [DEB-1456964, DEB-0949689]; Harvard Society of Fellows; William F. Milton Fund from the Harvard Medical School; Smithsonian Competitive Grants Program for Science; FAPSP [2011/50226-0]; CNPq [311562/2012-4, 487639/2012-0] FX We gratefully acknowledge the Direccion General de Recursos Naturales Renovables for permission to conduct fieldwork in Uruguay. We thank Naomi Pierce for permission to conduct parts of this study in her laboratory at Harvard University. Sarah Callan and Amelia Harvey kindly assisted in the laboratory. Christian Rabeling was supported by the National Science Foundation (DEB-1456964), the Harvard Society of Fellows, and by the William F. Milton Fund from the Harvard Medical School. Ted Schultz was supported by the National Science Foundation (DEB-0949689, DEB-1456964) and the Smithsonian Competitive Grants Program for Science. Mauricio Bacci Jr. acknowledges support from FAPSP (2011/50226-0) and CNPq (311562/2012-4 and 487639/2012-0). Martin Bollazzi is grateful to Daniel Ramirez from Cambium Forestal for facilitating access to field research sites. NR 95 TC 4 Z9 4 U1 5 U2 29 PU SPRINGER BASEL AG PI BASEL PA PICASSOPLATZ 4, BASEL, 4052, SWITZERLAND SN 0020-1812 EI 1420-9098 J9 INSECT SOC JI Insect. Soc. PD AUG PY 2015 VL 62 IS 3 BP 335 EP 349 DI 10.1007/s00040-015-0406-6 PG 15 WC Entomology SC Entomology GA CK5NM UT WOS:000356271800011 ER PT J AU Ingley, SJ Reina, RG Bermingham, E Johnson, JB AF Ingley, Spencer J. Reina, Ruth G. Bermingham, Eldredge Johnson, Jerald B. TI Phylogenetic analyses provide insights into the historical biogeography and evolution of Brachyrhaphis fishes SO MOLECULAR PHYLOGENETICS AND EVOLUTION LA English DT Article DE Brachyrhaphis; Phylogeny; Historical biogeography; Ecology; Poeciliidae; Lower Central America ID LIFE-HISTORY; LIVEBEARING FISH; PREDATOR REGIMES; CENTRAL-AMERICA; DNA-SEQUENCES; EPISCOPI POECILIIDAE; GENUS BRACHYRHAPHIS; COMPARATIVE ECOLOGY; UNIQUE FEATURES; MIDDLE MIOCENE AB The livebearing fish genus Brachyrhaphis (Poeciliidae) has become an increasingly important model in evolution and ecology research, yet the phylogeny of this group is not well understood, nor has it been examined thoroughly using modern phylogenetic methods. Here, we present the first comprehensive phylogenetic analysis of Brachyrhaphis by using four molecular markers (3 mtDNA, 1 nucDNA) to infer relationships among species in this genus. We tested the validity of this genus as a monophyletic group using extensive outgroup sampling based on recent phylogenetic hypotheses of Poeciliidae. We also tested the validity of recently described species of Brachyrhaphis that are part of the B. episcopi complex in Panama. Finally, we examined the impact of historical events on diversification of Brachyrhaphis, and made predictions regarding the role of different ecological environments on evolutionary diversification where known historical events apparently fail to explain speciation. Based on our results, we reject the monophyly of Brachyrhaphis, and question the validity of two recently described species (B. hessfeldi and B. roswithae). Historical biogeography of Brachyrhaphis generally agrees with patterns found in other freshwater taxa in Lower Central America, which show that geological barriers frequently predict speciation. Specifically, we find evidence in support of an 'island' mod el of Lower Central American formation, which posits that the nascent isthmus was partitioned by several marine connections before linking North and South America. In some cases where historic events (e.g., vicariance) fail to explain allopatric species breaks in Brachyrhaphis, ecological processes (e.g., divergent predation environments) offer additional insight into our understanding of phylogenetic diversification in this group. (C) 2015 Elsevier Inc. All rights reserved. C1 [Ingley, Spencer J.; Johnson, Jerald B.] Brigham Young Univ, Dept Biol, Evolutionary Ecol Labs, Provo, UT 84602 USA. [Reina, Ruth G.; Bermingham, Eldredge] Smithsonian Trop Res Inst, Balboa, Panama. [Johnson, Jerald B.] Brigham Young Univ, Monte L Bean Life Sci Museum, Provo, UT 84602 USA. RP Ingley, SJ (reprint author), Brigham Young Univ, Dept Biol, Evolutionary Ecol Labs, 401 WIDB, Provo, UT 84602 USA. EM sjingley@byu.edu OI Ingley, Spencer/0000-0002-2414-9892 FU National Science Foundation [OISE 0530267]; Smithsonian Tropical Research Institute; Brigham Young University FX We kindly thank those who helped with field and laboratory work needed to complete this study, especially Rigoberto Gonzalez. We are indebted to John Boylan, Ken Normandin and Adrianus Schonewille, for their great help in collecting. Funding for this research was provided by the National Science Foundation (Graduate Research Fellowship awarded to SJI and OISE 0530267 awarded to JBJ), the Smithsonian Tropical Research Institute, and by Brigham Young University. Our manuscript was improved considerably by feedback from two anonymous reviewers and Dr. Guillermo Orti. NR 72 TC 6 Z9 6 U1 6 U2 36 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 1055-7903 EI 1095-9513 J9 MOL PHYLOGENET EVOL JI Mol. Phylogenet. Evol. PD AUG PY 2015 VL 89 BP 104 EP 114 DI 10.1016/j.ympev.2015.04.013 PG 11 WC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity SC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity GA CJ6YI UT WOS:000355640700009 PM 25916190 ER PT J AU Heim, O Treitler, JT Tschapka, M Knornschild, M Jung, K AF Heim, Olga Treitler, Julia T. Tschapka, Marco Knoernschild, Mirjam Jung, Kirsten TI The Importance of Landscape Elements for Bat Activity and Species Richness in Agricultural Areas SO PLOS ONE LA English DT Article ID SCATTERED TREES; LAND-USE; FORAGING HABITAT; BIRD POPULATIONS; FARMLAND BIRDS; BIODIVERSITY; ECHOLOCATION; INTENSIFICATION; IDENTIFICATION; CONSEQUENCES AB Landscape heterogeneity is regarded as a key factor for maintaining biodiversity and ecosystem function in production landscapes. We investigated whether grassland sites at close vicinity to forested areas are more frequently used by bats. Considering that bats are important consumers of herbivorous insects, including agricultural pest, this is important for sustainable land management. Bat activity and species richness were assessed using repeated monitoring from May to September in 2010 with acoustic monitoring surveys on 50 grassland sites in the Biosphere Reserve Schorfheide-Chorin (North-East Germany). Using spatial analysis (GIS), we measured the closest distance of each grassland site to potentially connecting landscape elements (e.g., trees, linear vegetation, groves, running and standing water). In addition, we assessed the distance to and the percent land cover of forest remnants and urban areas in a 200 m buffer around the recording sites to address differences in the local landscape setting. Species richness and bat activity increased significantly with higher forest land cover in the 200 m buffer and at smaller distance to forested areas. Moreover, species richness increased in proximity to tree groves. Larger amount of forest land cover and smaller distance to forest also resulted in a higher activity of bats on grassland sites in the beginning of the year during May, June and July. Landscape elements near grassland sites also influenced species composition of bats and species richness of functional groups (open, edge and narrow space foragers). Our results highlight the importance of forested areas, and suggest that agricultural grasslands that are closer to forest remnants might be better buffered against outbreaks of agricultural pest insects due to higher species richness and higher bat activity. Furthermore, our data reveals that even for highly mobile species such as bats, a very dense network of connecting elements within the landscape is beneficial to promote activity in open areas and thus assure vital ecosystem function in agricultural landscapes. C1 [Heim, Olga; Treitler, Julia T.; Tschapka, Marco; Knoernschild, Mirjam; Jung, Kirsten] Univ Ulm, Inst Evolutionary Ecol & Conservat Genom, D-89069 Ulm, Germany. [Tschapka, Marco; Knoernschild, Mirjam] Smithsonian Trop Res Inst, Balboa, Panama. RP Jung, K (reprint author), Univ Ulm, Inst Evolutionary Ecol & Conservat Genom, D-89069 Ulm, Germany. EM kirsten.jung@uni-ulm.de FU German Science Foundation [KA 1241/19-1] FX This work has been funded by the German Science Foundation (http://www.dfg.de), Priority Program 1374 (KA 1241/19-1) to MT. The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 56 TC 3 Z9 3 U1 11 U2 101 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 JUL 31 PY 2015 VL 10 IS 7 AR e0134443 DI 10.1371/journal.pone.0134443 PG 13 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA CO0JY UT WOS:000358838400119 PM 26231029 ER PT J AU Byers, JE Smith, RS Pringle, JM Clark, GF Gribben, PE Hewitt, CL Inglis, GJ Johnston, EL Ruiz, GM Stachowicz, JJ Bishop, MJ AF Byers, James E. Smith, Rachel S. Pringle, James M. Clark, Graeme F. Gribben, Paul E. Hewitt, Chad L. Inglis, Graeme J. Johnston, Emma L. Ruiz, Gregory M. Stachowicz, John J. Bishop, Melanie J. TI Invasion Expansion: Time since introduction best predicts global ranges of marine invaders SO SCIENTIFIC REPORTS LA English DT Article ID CLIMATE-CHANGE; BIOLOGICAL INVASIONS; PLANT INVASIVENESS; GEOGRAPHIC RANGE; RESIDENCE TIME; NORTH-AMERICA; LIFE-HISTORY; BODY-SIZE; BIVALVES; SUCCESS AB Strategies for managing biological invasions are often based on the premise that characteristics of invading species and the invaded environment are key predictors of the invader's distribution. Yet, for either biological traits or environmental characteristics to explain distribution, adequate time must have elapsed for species to spread to all potential habitats. We compiled and analyzed a database of natural history and ecological traits of 138 coastal marine invertebrate species, the environmental conditions at sites to which they have been introduced, and their date of first introduction. We found that time since introduction explained the largest fraction (20%) of the variability in non-native range size, while traits of the species and environmental variables had significant, but minimal, influence on non-native range size. The positive relationship between time since introduction and range size indicates that non-native marine invertebrate species are not at equilibrium and are still spreading, posing a major challenge for management of coastal ecosystems. C1 [Byers, James E.; Smith, Rachel S.] Univ Georgia, Odum Sch Ecol, Athens, GA 30602 USA. [Pringle, James M.] UNH, Ocean Proc Anal Lab, Durham, NH 03857 USA. [Smith, Rachel S.; Clark, Graeme F.; Johnston, Emma L.] Univ New S Wales, Sch Biol Earth & Environm Sci, Evolut & Ecol Res Ctr, Sydney, NSW 2052, Australia. [Gribben, Paul E.] Univ New S Wales, Sch Biol Earth & Environm Sci, Ctr Marine Bioinnovat, Sydney, NSW 2052, Australia. [Hewitt, Chad L.] Univ Waikato, Sch Sci, Hamilton 3240, New Zealand. [Inglis, Graeme J.] Natl Inst Water & Atmospher Res, Christchurch 8011, New Zealand. [Ruiz, Gregory M.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. [Stachowicz, John J.] Univ Calif Davis, Dept Ecol & Evolut, Davis, CA 95616 USA. [Bishop, Melanie J.] Macquarie Univ, Dept Biol Sci, N Ryde, NSW 2109, Australia. RP Byers, JE (reprint author), Univ Georgia, Odum Sch Ecol, Athens, GA 30602 USA. EM jebyers@uga.edu OI Ruiz, Gregory/0000-0003-2499-441X FU Genes to Geosciences Research Centre Macquarie University; Ecology and Evolution Research Centre University of New South Wales (UNSW), UNSW Gold Star Grant; NSF [0961830]; NZ Ministry for Primary Industries; NIWA; National SeaGrant Program; Smithsonian Institution FX Funding provided by Genes to Geosciences Research Centre Macquarie University, Ecology and Evolution Research Centre University of New South Wales (UNSW), UNSW Gold Star Grant Awarded to ELJ, and NSF #0961830 to JEB and JMP. We thank Rick Lumpkin (NOAA Atlantic Oceanographic and Meteorological Laboratory) for sharing data from the Global Drifter Project and Paula Pappalardo for help with plots. Data on New Zealand non-native species were compiled from projects funded by the NZ Ministry for Primary Industries and NIWA. Data collection and synthesis for NEMESIS were supported by the National SeaGrant Program and Smithsonian Institution, and we thank Paul Fofonoff and James Carlton for contributions to this effort. NR 46 TC 5 Z9 5 U1 5 U2 31 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 JUL 31 PY 2015 VL 5 AR 12436 DI 10.1038/srep12436 PG 9 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA CN9LS UT WOS:000358770800001 PM 26227803 ER PT J AU Kjer, KM Ware, JL Rust, J Wappler, T Lanfear, R Jermiin, LS Zhou, X Aspock, H Aspock, U Beutel, RG Blanke, A Donath, A Flouri, T Frandsen, PB Kapli, P Kawahara, AY Letsch, H Mayer, C McKenna, DD Meusemann, K Niehuis, O Peters, RS Wiegmann, BM Yeates, DK von Reumont, BM Stamatakis, A Misof, B AF Kjer, K. M. Ware, J. L. Rust, J. Wappler, T. Lanfear, R. Jermiin, L. S. Zhou, X. Aspoeck, H. Aspoeck, U. Beutel, R. G. Blanke, A. Donath, A. Flouri, T. Frandsen, P. B. Kapli, P. Kawahara, A. Y. Letsch, H. Mayer, C. McKenna, D. D. Meusemann, K. Niehuis, O. Peters, R. S. Wiegmann, B. M. Yeates, D. K. von Reumont, B. M. Stamatakis, A. Misof, B. TI Response to Comment on "Phylogenomics resolves the timing and pattern of insect evolution" SO SCIENCE LA English DT Editorial Material ID FOSSIL AB Tong et al. comment on the accuracy of the dating analysis presented in our work on the phylogeny of insects and provide a reanalysis of our data. They replace log-normal priors with uniform priors and add a "roachoid" fossil as a calibration point. Although the reanalysis provides an interesting alternative viewpoint, we maintain that our choices were appropriate. C1 [Kjer, K. M.] Univ Calif Davis, Davis, CA 95616 USA. [Ware, J. L.; Frandsen, P. B.] Rutgers State Univ, New Brunswick, NJ 08903 USA. [Rust, J.; Wappler, T.; Donath, A.; Mayer, C.; Peters, R. S.] Univ Bonn, Bonn, Germany. [Lanfear, R.] Macquarie Univ, Sydney, NSW 2109, Australia. [Jermiin, L. S.; Meusemann, K.; Yeates, D. K.] CSIRO, Canberra, ACT, Australia. [Zhou, X.] BGI Shenzhen, China Natl GeneBank, Shenzhen, Peoples R China. [Zhou, X.] BGI Shenzhen, Shenzhen, Peoples R China. [Aspoeck, H.; Aspoeck, U.; Letsch, H.] Univ Vienna, Vienna, Austria. [Aspoeck, U.] Nat Hist Museum Wien, Vienna, Austria. [Beutel, R. G.] Univ Jena, Phyletischem Museum Jena, D-07745 Jena, Germany. [Blanke, A.] Univ Tsukuba, Tsukuba, Ibaraki 305, Japan. [Donath, A.; Mayer, C.; Meusemann, K.; Niehuis, O.; Peters, R. S.; von Reumont, B. M.; Misof, B.] Zool Forsch Museum Alexander Koenig ZFMK, Bonn, Germany. [Flouri, T.; Kapli, P.; Stamatakis, A.] HITS, Heidelberg, Germany. [Frandsen, P. B.] Smithsonian Inst, Washington, DC 20560 USA. [Kawahara, A. Y.] Univ Florida, Gainesville, FL USA. [McKenna, D. D.] Univ Memphis, Memphis, TN 38152 USA. [Niehuis, O.] Arizona State Univ, Tempe, AZ USA. [Wiegmann, B. M.] N Carolina State Univ, Raleigh, NC 27695 USA. [von Reumont, B. M.] Nat Hist Museum, London SW7 5BD, England. RP Misof, B (reprint author), Zool Forsch Museum Alexander Koenig ZFMK, Bonn, Germany. EM bmisof@uni-bonn.de RI Jermiin, Lars/C-2458-2009; Blanke, Alexander/H-9858-2013; Stamatakis, Alexandros/B-8740-2009; Yeates, David/A-9917-2008 OI Jermiin, Lars/0000-0002-9619-3809; Yeates, David/0000-0001-7729-6143 NR 6 TC 3 Z9 3 U1 11 U2 33 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 JUL 31 PY 2015 VL 349 IS 6247 PG 2 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA CN8SP UT WOS:000358713300043 ER PT J AU Heer, K Kalko, EKV Albrecht, L Garcia-Villacorta, R Staeps, FC Herre, EA Dick, CW AF Heer, Katrin Kalko, Elisabeth K. V. Albrecht, Larissa Garcia-Villacorta, Roosevelt Staeps, Felix C. Allen Herre, Edward Dick, Christopher W. TI Spatial Scales of Genetic Structure in Free-Standing and Strangler Figs (Ficus, Moraceae) Inhabiting Neotropical Forests SO PLOS ONE LA English DT Article ID TROPICAL RAIN-FORESTS; MULTILOCUS GENOTYPE DATA; POPULATION-STRUCTURE; FRUIT CHARACTERISTICS; ARTIBEUS-JAMAICENSIS; POLLINATING WASPS; TREE; SOFTWARE; BAT; PHYLOGEOGRAPHY AB Wind-borne pollinating wasps (Agaonidae) can transport fig (Ficus sp., Moraceae) pollen over enormous distances (> 100 km). Because of their extensive breeding areas, Neotropical figs are expected to exhibit weak patterns of genetic structure at local and regional scales. We evaluated genetic structure at the regional to continental scale (Panama, Costa Rica, and Peru) for the free-standing fig species Ficus insipida. Genetic differentiation was detected only at distances > 300 km (Jost's D-est = 0.68 +/- 0.07 & F-ST = 0.30 +/- 0.03 between Mesoamerican and Amazonian sites) and evidence for phylogeographic structure (R-ST>>permuted R-ST) was only significant in comparisons between Central and South America. Further, we assessed local scale spatial genetic structure (SGS, d <= 8 km) in Panama and developed an agent-based model parameterized with data from F. insipida to estimate minimum pollination distances, which determine the contribution of pollen dispersal on SGS. The local scale data for F. insipida was compared to SGS data collected for an additional free-standing fig, F. yoponensis (subgenus Pharmacosycea), and two species of strangler figs, F. citrifolia and F. obtusifolia (subgenus Urostigma) sampled in Panama. All four species displayed significant SGS (mean Sp = 0.014 +/- 0.012). Model simulations indicated that most pollination events likely occur at distances > > 1 km, largely ruling out spatially limited pollen dispersal as the determinant of SGS in F. insipida and, by extension, the other fig species. Our results are consistent with the view that Ficus develops fine-scale SGS primarily as a result of localized seed dispersal and/or clumped seedling establishment despite extensive long-distance pollen dispersal. We discuss several ecological and life history factors that could have species-or subgenus-specific impacts on the genetic structure of Neotropical figs. C1 [Heer, Katrin] Univ Marburg, Fac Biol, Conservat Biol, D-35043 Marburg, Germany. [Heer, Katrin] Univ Marburg, Fac Biol, Dept Ecol, D-35043 Marburg, Germany. [Heer, Katrin; Kalko, Elisabeth K. V.; Albrecht, Larissa] Univ Ulm, Inst Expt Ecol, D-89069 Ulm, Germany. [Kalko, Elisabeth K. V.; Allen Herre, Edward] Smithsonian Trop Res Inst, Balboa, Panama. [Garcia-Villacorta, Roosevelt] Univ Edinburgh, Inst Mol Plant Sci, Edinburgh EH9 3JH, Midlothian, Scotland. [Dick, Christopher W.] Univ Michigan, Dept Ecol & Evolutionary Biol, Ann Arbor, MI 48109 USA. RP Heer, K (reprint author), Univ Marburg, Fac Biol, Conservat Biol, Karl von Frisch Str 8, D-35043 Marburg, Germany. EM katrin.heer@uni-marburg.de FU German National Merit Foundation (Studienstiftung des Deutschen Volkes); NSF [DEB 0640379] FX The project was funded by a scholarship from the German National Merit Foundation (Studienstiftung des Deutschen Volkes) to KH and NSF funding (DEB 0640379) to CWD. The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 78 TC 2 Z9 2 U1 5 U2 24 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 JUL 30 PY 2015 VL 10 IS 7 AR e0133581 DI 10.1371/journal.pone.0133581 PG 18 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA CO0JT UT WOS:000358837700026 PM 26226482 ER PT J AU Wilkerson, RC Linton, YM Fonseca, DM Schultz, TR Price, DC Strickman, DA AF Wilkerson, Richard C. Linton, Yvonne-Marie Fonseca, Dina M. Schultz, Ted R. Price, Dana C. Strickman, Daniel A. TI Making Mosquito Taxonomy Useful: A Stable Classification of Tribe Aedini that Balances Utility with Current Knowledge of Evolutionary Relationships SO PLOS ONE LA English DT Article ID RIFT-VALLEY FEVER; EASTERN EQUINE ENCEPHALITIS; ALLIED TAXA DIPTERA; PHYLOGENETIC-RELATIONSHIPS; YELLOW-FEVER; LIFE STAGES; ARBOVIRUS SURVEILLANCE; WUCHERERIA-BANCROFTI; MORPHOLOGICAL DATA; CULICIDAE DIPTERA AB The tribe Aedini (Family Culicidae) contains approximately one-quarter of the known species of mosquitoes, including vectors of deadly or debilitating disease agents. This tribe contains the genus Aedes, which is one of the three most familiar genera of mosquitoes. During the past decade, Aedini has been the focus of a series of extensive morphology-based phylogenetic studies published by Reinert, Harbach, and Kitching (RH&K). Those authors created 74 new, elevated or resurrected genera from what had been the single genus Aedes, almost tripling the number of genera in the entire family Culicidae. The proposed classification is based on subjective assessments of the "number and nature of the characters that support the branches" subtending particular monophyletic groups in the results of cladistic analyses of a large set of morphological characters of representative species. To gauge the stability of RH&K's generic groupings we reanalyzed their data with unweighted parsimony jackknife and maximum-parsimony analyses, with and without ordering 14 of the characters as in RH&K. We found that their phylogeny was largely weakly supported and their taxonomic rankings failed priority and other useful taxon-naming criteria. Consequently, we propose simplified aedine generic designations that 1) restore a classification system that is useful for the operational community; 2) enhance the ability of taxonomists to accurately place new species into genera; 3) maintain the progress toward a natural classification based on monophyletic groups of species; and 4) correct the current classification system that is subject to instability as new species are described and existing species more thoroughly defined. We do not challenge the phylogenetic hypotheses generated by the above-mentioned series of morphological studies. However, we reduce the ranks of the genera and subgenera of RH&K to subgenera or informal species groups, respectively, to preserve stability as new data become available. C1 [Wilkerson, Richard C.; Linton, Yvonne-Marie; Schultz, Ted R.] Smithsonian Inst, Dept Entomol, Natl Museum Nat Hist, Washington, DC 20560 USA. [Linton, Yvonne-Marie] Smithsonian Inst, Museum Support Ctr, Walter Reed Biosystemat Unit, Suitland, MD USA. [Linton, Yvonne-Marie] Walter Reed Army Inst Res, Dept Entomol, Silver Spring, MD USA. [Linton, Yvonne-Marie] Uniformed Serv Univ Hlth Sci, Fac Preventat Med & Biometr, Bethesda, MD 20814 USA. [Fonseca, Dina M.; Price, Dana C.] Rutgers State Univ, Dept Entomol, Sch Environm & Biol Sci, New Brunswick, NJ 08903 USA. [Strickman, Daniel A.] Bill & Melinda Gates Fdn, Global Hlth Program, Seattle, WA USA. RP Wilkerson, RC (reprint author), Smithsonian Inst, Dept Entomol, Natl Museum Nat Hist, NHB 169, Washington, DC 20560 USA. EM wilkersonr@si.edu OI Fonseca, Dina/0000-0003-4726-7100 NR 104 TC 33 Z9 35 U1 4 U2 15 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 JUL 30 PY 2015 VL 10 IS 7 AR e0133602 DI 10.1371/journal.pone.0133602 PG 26 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA CO0JT UT WOS:000358837700027 PM 26226613 ER PT J AU Xu, XG Wang, J Zeng, J Spurr, R Liu, X Dubovik, O Li, L Li, ZQ Mishchenko, MI Siniuk, A Holben, BN AF Xu, Xiaoguang Wang, Jun Zeng, Jing Spurr, Robert Liu, Xiong Dubovik, Oleg Li, Li Li, Zhengqiang Mishchenko, Michael I. Siniuk, Aliaksandr Holben, Brent N. TI Retrieval of aerosol microphysical properties from AERONET photopolarimetric measurements: 2. A new research algorithm and case demonstration SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article DE AERONET; polarization; aerosol retrieval algorithm; single-scattering albedo; remote sensing; absorption ID SKY RADIANCE MEASUREMENTS; BOUND CONSTRAINED OPTIMIZATION; OPTICAL-PROPERTIES; IMAGING SPECTRORADIOMETER; BIDIRECTIONAL REFLECTANCE; SPACEBORNE MEASUREMENTS; SATELLITE RETRIEVALS; TROPOSPHERIC AEROSOL; INVERSION ALGORITHM; INTEGRAL EQUATIONS AB A new research algorithm is presented here as the second part of a two-part study to retrieve aerosol microphysical properties from the multispectral and multiangular photopolarimetric measurements taken by Aerosol Robotic Network's (AERONET's) new-generation Sun photometer. The algorithm uses an advanced UNified and Linearized Vector Radiative Transfer Model and incorporates a statistical optimization approach. While the new algorithm has heritage from AERONET operational inversion algorithm in constraining a priori and retrieval smoothness, it has two new features. First, the new algorithm retrieves the effective radius, effective variance, and total volume of aerosols associated with a continuous bimodal particle size distribution (PSD) function, while the AERONET operational algorithm retrieves aerosol volume over 22 size bins. Second, our algorithm retrieves complex refractive indices for both fine and coarse modes, while the AERONET operational algorithm assumes a size-independent aerosol refractive index. Mode-resolved refractive indices can improve the estimate of the single-scattering albedo (SSA) for each aerosol mode and thus facilitate the validation of satellite products and chemistry transport models. We applied the algorithm to a suite of real cases over Beijing_RADI site and found that our retrievals are overall consistent with AERONET operational inversions but can offer mode-resolved refractive index and SSA with acceptable accuracy for the aerosol composed by spherical particles. Along with the retrieval using both radiance and polarization, we also performed radiance-only retrieval to demonstrate the improvements by adding polarization in the inversion. Contrast analysis indicates that with polarization, retrieval error can be reduced by over 50% in PSD parameters, 10-30% in the refractive index, and 10-40% in SSA, which is consistent with theoretical analysis presented in the companion paper of this two-part study. C1 [Xu, Xiaoguang; Wang, Jun; Zeng, Jing] Univ Nebraska, Earth & Atmospher Sci, Lincoln, NE 68588 USA. [Spurr, Robert] RT Solut Inc, Cambridge, MA USA. [Liu, Xiong] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Dubovik, Oleg] Univ Lille 1, CNRS, Lab Opt Atmospher, F-59655 Villeneuve Dascq, France. [Li, Li; Li, Zhengqiang] Chinese Acad Sci, State Environm Protect Key Lab Satellites Remote, Inst Remote Sensing & Digital Earth, Beijing, Peoples R China. [Mishchenko, Michael I.] NASA Goddard Inst Space Studies, New York, NY USA. [Siniuk, Aliaksandr; Holben, Brent N.] NASA Goddard Space Flight Ctr, Greenbelt, MD USA. RP Wang, J (reprint author), Univ Nebraska, Earth & Atmospher Sci, Lincoln, NE 68588 USA. EM jwangjun@gmail.com RI Liu, Xiong/P-7186-2014; Xu, Xiaoguang/B-8203-2016; Wang, Jun/A-2977-2008; OI Liu, Xiong/0000-0003-2939-574X; Xu, Xiaoguang/0000-0001-9583-980X; Wang, Jun/0000-0002-7334-0490; Li, Zhengqiang/0000-0002-7795-3630 FU NASA Earth and Space Science Fellowship; NASA Radiation Sciences Program; NASA Glory Mission Program FX This research is supported by a NASA Earth and Space Science Fellowship managed by Mingying Wei, as well as the NASA Radiation Sciences Program and the Glory Mission Program managed by Hal Maring. We acknowledge the data services provided by the AERONET team at NASA GSFC, and the computational support from the Holland Computing Center at the University of Nebraska. The data presented in the manuscript can be available upon request through email to the corresponding author at jwangjun@gmail.com. J. Zeng and J. Wang also thank Qingyuang Han for inspiring them to conduct this work. NR 80 TC 10 Z9 10 U1 1 U2 14 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD JUL 27 PY 2015 VL 120 IS 14 BP 7079 EP 7098 DI 10.1002/2015JD023113 PG 20 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA CP3TL UT WOS:000359804900024 ER PT J AU McCormick, B Popp, C Andrews, B Cottrell, E AF McCormick, Brendan Popp, Christoph Andrews, Benjamin Cottrell, Elizabeth TI Ten years of satellite observations reveal highly variable sulphur dioxide emissions at Anatahan Volcano, Mariana Islands SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article DE volcanic gas; satellite remote sensing; Anatahan volcano ID OZONE MONITORING INSTRUMENT; GROUND-BASED MEASUREMENTS; SOUFRIERE-HILLS VOLCANO; 2003 ERUPTION; SO2 EMISSIONS; SPACE; PLUMES; CHRONOLOGY; FLUX; COMMONWEALTH AB Satellite remote sensing enables continuous multiyear observations of volcanic activity in remote settings. Anatahan (Mariana Islands) is a remote volcano in the western North Pacific. Available ground-based measurements of sulphur dioxide (SO2) gas emissions at Anatahan place it among thelargest volcanic SO2 sources worldwide. These ground-based measurements, however, are restricted to eruptive intervals. Anatahan's activity since 2003 has been dominated temporally by prolonged periods of quiescence. Using 10years of satellite observations from OMI, AIRS, SCIAMACHY, and GOME-2, we report highly variable SO2 emissions within and between eruptive and quiescent intervals at Anatahan. We find close correspondence between levels of activity reported at the volcano and levels of SO2 emissions detected from space. Eruptive SO2 emission rates have a mean value of approximate to 6400td(-1), but frequently are in excess of 20,000td(-1). Conversely, SO2 emissions during quiescent intervals are below the detection limit of space-based sensors and therefore are not likely to exceed approximate to 300td(-1). We show that while Anatahan occupies a quiescent state for 85% of the past 10years, only approximate to 15% of total SO2 emissions over this interval occur during quiescence, with the remaining approximate to 85% released in short duration but intense syn-eruptive degassing. We propose that the integration of multiyear satellite data sets and activity histories are a powerful complement to targeted ground-based campaign measurements in better describing the long-term degassing behavior of remote volcanoes. C1 [McCormick, Brendan; Popp, Christoph; Andrews, Benjamin; Cottrell, Elizabeth] Natl Museum Nat Hist, Dept Mineral Sci, Smithsonian Inst, Washington, DC 20560 USA. RP McCormick, B (reprint author), Natl Museum Nat Hist, Dept Mineral Sci, Smithsonian Inst, Washington, DC 20560 USA. EM brendanvolc@gmail.com FU Deep Carbon Observatory; Alfred P Sloan Foundation; Smithsonian Global Volcanism Program; Smithsonian Grand Challenges Award FX We acknowledge NASA for making OMI level 2 and AIRS level 1 data products freely available and BIRA/TEMIS for making SCIAMACHY level 2 data products freely available. We are grateful to Caroline Nowlan for providing access to SAO GOME-2 data and to Fred Prata and Simon Carn, respectively, for IDL routines which aided our analysis of AIRS and OMI data. The derived satellite data products presented herein (SO2 mass loadings, emission rates) are included in the supporting information, and more extensive supporting data can be provided by the authors upon request. B.M. and C.P. acknowledge the Deep Carbon Observatory, the Alfred P Sloan Foundation, and the Smithsonian Global Volcanism Program for supporting their postdoctoral fellowships. EC and BA each acknowledge a Smithsonian Grand Challenges Award, and the Global Volcanism Program; EC acknowledges a grant from the Deep Carbon Observatory. We thank Rob Wright and Eric Pilger for their assistance with the MODIS MODVOLC product; Jennifer Jay, Matt Pritchard, and Chuck Wicks for discussions of deformation in the Marianas; and Ed Venzke for discussions of eruption durations in the GVP-VOTW database. Finally, we warmly thank Taryn Lopez, Arlin Krueger, and one anonymous reviewer, for their detailed and constructive comments, which greatly improved the quality of this manuscript. NR 93 TC 3 Z9 3 U1 1 U2 10 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD JUL 27 PY 2015 VL 120 IS 14 BP 7258 EP 7282 DI 10.1002/2014JD022856 PG 25 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA CP3TL UT WOS:000359804900035 ER PT J AU Torres-Herrera, EJ Santos, LF AF Torres-Herrera, E. J. Santos, Lea F. TI Dynamics at the many-body localization transition SO PHYSICAL REVIEW B LA English DT Article ID INVERSE PARTICIPATION RATIO; METAL-INSULATOR-TRANSITION; MOBILITY EDGE; ANDERSON LOCALIZATION; WAVE-PACKET; SYSTEMS; STATES; FLUCTUATIONS; DIFFUSION; PHASE AB The isolated one-dimensional Heisenberg model with static random magnetic fields has become paradigmatic for the analysis of many-body localization. Here, we study the dynamics of this system initially prepared in a highly-excited nonstationary state. Our focus is on the probability for finding the initial state later in time, the so-called survival probability. Two distinct behaviors are identified before equilibration. At short times, the decay is very fast and equivalent to that of clean systems. It subsequently slows down and develops a power-law behavior with an exponent that coincides with the multifractal dimension of the eigenstates. C1 [Torres-Herrera, E. J.; Santos, Lea F.] Yeshiva Univ, Dept Phys, New York, NY 10016 USA. [Torres-Herrera, E. J.] Univ Autonoma Puebla, Inst Fis, Puebla 72570, Mexico. [Santos, Lea F.] Harvard Smithsonian Ctr Astrophys, ITAMP, Cambridge, MA 02138 USA. RP Torres-Herrera, EJ (reprint author), Yeshiva Univ, Dept Phys, New York, NY 10016 USA. RI Santos, Lea/D-5332-2012 OI Santos, Lea/0000-0001-9400-2709 FU NSF [DMR-1147430]; CONACyT, Mexico FX This work was supported by the NSF Grant No. DMR-1147430. E.J.T.H. acknowledges support from CONACyT, Mexico. L.F.S. thanks the ITAMP hospitality, where part of this work was done. We thank J.A. Mendez-Bermudez and Z. Papic for useful suggestions. NR 65 TC 31 Z9 31 U1 1 U2 8 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 1098-0121 EI 1550-235X J9 PHYS REV B JI Phys. Rev. B PD JUL 24 PY 2015 VL 92 IS 1 AR 014208 DI 10.1103/PhysRevB.92.014208 PG 7 WC Physics, Condensed Matter SC Physics GA CN4YI UT WOS:000358436100001 ER PT J AU Marra, PP Studds, CE Wilson, S Sillett, TS Sherry, TW Holmes, RT AF Marra, Peter P. Studds, Colin E. Wilson, Scott Sillett, T. Scott Sherry, Thomas W. Holmes, Richard T. TI Non-breeding season habitat quality mediates the strength of density-dependence for a migratory bird SO PROCEEDINGS OF THE ROYAL SOCIETY B-BIOLOGICAL SCIENCES LA English DT Article DE American redstart; crowding; Setophaga ruticilla; carry-over effects; annual survival ID POPULATION REGULATION; NONBREEDING SEASON; REINTRODUCED POPULATION; AMERICAN REDSTARTS; FOOD AVAILABILITY; LARGE-SCALE; SURVIVAL; CONSEQUENCES; SONGBIRD; SEGREGATION AB Our understanding of when natural populations are regulated during their annual cycle is limited, particularly for migratory species. This information is needed for parametrizing models that can inform management and conservation. Here, we use 14 years of data on colour-marked birds to investigate how conspecific density and habitat quality during the tropical non-breeding period interact to affect body condition and apparent annual survival of a long-distance migratory songbird, the American redstart (Setophaga ruticilla). Body condition and survival of birds in high-quality mangrove habitat declined as density increased. By contrast, body condition improved and survival did not vary as density increased in adjacent, lower quality scrub habitat, although mean condition and survival were almost always lower than in mangrove. High rainfall enhanced body condition in scrub but not in mangrove, suggesting factors such as food availability outweighed consequences of crowding in lower quality habitat. Thus, survival of overwintering redstarts in mangrove habitat, disproportionately males, appears to be regulated by a crowding mechanism based on density-dependent resource competition. Survival of individuals in scrub, mostly females, appears to be limited by density-independent environmental factors but not regulated by crowding. The contrasting effects of density and food limitation on individuals overwintering in adjacent habitats illustrate the complexity of processes operating during the non-breeding period for migratory animals, and emphasize the need for long-term studies of animals in multiple habitats and throughout their annual cycles. C1 [Marra, Peter P.; Studds, Colin E.; Sillett, T. Scott] Smithsonian Inst, Natl Zool Pk, Smithsonian Conservat Biol Inst, Migratory Bird Ctr, Washington, DC 20008 USA. [Studds, Colin E.] Univ Maryland Baltimore Cty, Dept Geog & Environm Syst, Baltimore, MD 21250 USA. [Wilson, Scott] Carleton Univ, Environm Canada, Natl Wildlife Res Ctr, Ottawa, ON K1A 5B6, Canada. [Sherry, Thomas W.] Tulane Univ, Dept Ecol & Evolutionary Biol, New Orleans, LA 70118 USA. [Holmes, Richard T.] Dartmouth Coll, Dept Biol Sci, Hanover, NH 03755 USA. RP Marra, PP (reprint author), Smithsonian Inst, Natl Zool Pk, Smithsonian Conservat Biol Inst, Migratory Bird Ctr, 3001 Connecticut Ave NW, Washington, DC 20008 USA. EM marrap@si.edu FU NSF [0717338, 1242584 0649679, 1242588, 9276520, 9625186] FX This study was supported by NSF grants to P.P.M., T.S.S., T.W.S. (0717338, 1242584 0649679, 1242588) and R.T.H. (9276520, 9625186). NR 61 TC 5 Z9 5 U1 6 U2 29 PU ROYAL SOC PI LONDON PA 6-9 CARLTON HOUSE TERRACE, LONDON SW1Y 5AG, ENGLAND SN 0962-8452 EI 1471-2954 J9 P ROY SOC B-BIOL SCI JI Proc. R. Soc. B-Biol. Sci. PD JUL 22 PY 2015 VL 282 IS 1811 AR 20150624 DI 10.1098/rspb.2015.0624 PG 8 WC Biology; Ecology; Evolutionary Biology SC Life Sciences & Biomedicine - Other Topics; Environmental Sciences & Ecology; Evolutionary Biology GA CN8ZS UT WOS:000358735700011 ER PT J AU Rose, M Elvis, M Crenshaw, M Glidden, A AF Rose, Marvin Elvis, Martin Crenshaw, Michael Glidden, Ana TI Intermediate inclinations of type 2 Coronal-Line Forest AGN SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies: active; quasars: emission lines; quasars: general; galaxies: Seyfert ID ACTIVE GALACTIC NUCLEI; DIGITAL SKY SURVEY; REGION; CLASSIFICATION; GALAXIES; SPECTRA; TORUS; VIEW AB Coronal-Line Forest Active Galactic Nuclei (CLiF AGN) are remarkable in the sense that they have a rich spectrum of dozens of coronal emission lines (e.g. [Fe VII], [Fe X] and [Ne V]) in their spectra. Rose, Elvis & Tadhunter suggest that the inner obscuring torus wall is the most likely location of the coronal line region in CLiF AGN, and the unusual strength of the forbidden high-ionization lines is due to a specific AGN-torus inclination angle. Here, we test this suggestion using mid-IR colours (4.6-22 mu m) from the Wide-Field Infrared Survey Explorer for the CLiF AGN. We use the Fischer et al. result that showed that as the AGN-torus inclination becomes more face on, the Spitzer 5.5-30 mu m colours become bluer. We show that the [W2-W4] colours for the CLiF AGN (<[W2-W4]> = 5.92 +/- 0.12) are intermediate between Sloan Digital Sky Survey (SDSS) type 1 (<[W2-W4]> = 5.22 +/- 0.01) and type 2 AGN (<[W2-W4]> = 6.35 +/- 0.03). This implies that the AGN-torus inclinations for the CLiF AGN are indeed intermediate, supporting the work of Rose, Elvis & Tadhunter. The confirmed relation between CLiF AGN and their viewing angle shows that CLiF AGN may be useful for our understanding of AGN unification. C1 [Rose, Marvin; Elvis, Martin] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Crenshaw, Michael] Georgia State Univ, Dept Phys & Astron, Atlanta, GA 30303 USA. [Glidden, Ana] MIT, Dept Phys, Cambridge, MA 02139 USA. RP Rose, M (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM mrose@cfa.harvard.edu FU NASA [NNX13AE88G]; Planetary Science Division of the National Aeronautics and Space Administration; Alfred P. Sloan Foundation; National Science Foundation; US Department of Energy Office of Science FX This work was supported in part by NASA grant NNX13AE88G. We thank the referee for useful comments and suggestions which improved this work substantially. The authors acknowledge the data analysis facilities provided by the Starlink Project, which is run by CCLRC on behalf of PPARC. This publication makes use of data products from NEOWISE, which is a project of the Jet Propulsion Laboratory/California Institute of Technology, funded by the Planetary Science Division of the National Aeronautics and Space Administration. 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. Funding for SDSS-III has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, and the US Department of Energy Office of Science. NR 15 TC 5 Z9 5 U1 0 U2 0 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD JUL 21 PY 2015 VL 451 IS 1 BP L11 EP L15 DI 10.1093/mnrasl/slv056 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CR4KX UT WOS:000361302000003 ER PT J AU Russell, HR Fabian, AC McNamara, BR Broderick, AE AF Russell, H. R. Fabian, A. C. McNamara, B. R. Broderick, A. E. TI Inside the Bondi radius of M87 SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies: clusters: individual: M87; intergalactic medium X-rays: galaxies: clusters ID RAY-EMITTING GAS; SUPERMASSIVE BLACK-HOLE; ACTIVE GALACTIC NUCLEI; NONRADIATIVE ACCRETION FLOWS; CENTRAL DOMINANT GALAXIES; SAGITTARIUS-A-ASTERISK; X-RAY; COOLING FLOWS; VIRGO CLUSTER; XMM-NEWTON AB Chandra X-ray observations of the nearby brightest cluster galaxy M87 resolve the hot gas structure across the Bondi accretion radius of the central supermassive black hole (SMBH), a measurement possible in only a handful of systems but complicated by the bright nucleus and jet emission. By stacking only short frame-time observations to limit pileup, and after subtracting the nuclear point spread function, we analysed the X-ray gas properties within the Bondi radius at 0.12-0.22 kpc (1.5-2.8 arcsec), depending on the black hole mass. Within 2 kpc radius, we detect two significant temperature components, which are consistent with constant values of 2 and 0.9 keV down to 0.15 kpc radius. No evidence was found for the expected temperature increase within similar to 0.25 kpc due to the influence of the SMBH. Within the Bondi radius, the density profile is consistent with rho proportional to r(-1). The lack of a temperature increase inside the Bondi radius suggests that the hot gas structure is not dictated by the SMBH's potential and, together with the shallow density profile, shows that the classical Bondi rate may not reflect the accretion rate on to the SMBH. If this density profile extends in towards the SMBH, the mass accretion rate on to the SMBH could be at least two orders of magnitude less than the Bondi rate, which agrees with Faraday rotation measurements for M87. We discuss the evidence for outflow from the hot gas and the cold gas disc and for cold feedback, where gas cooling rapidly from the hot atmosphere could feed the cirumnuclear disc and fuel the SMBH. At 0.2 kpc radius, the cooler X-ray temperature component represents 20 per cent of the total X-ray gas mass and, by losing angular momentum to the hot gas component, could provide a fuel source of cold clouds within the Bondi radius. C1 [Russell, H. R.; Fabian, A. C.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Russell, H. R.; McNamara, B. R.; Broderick, A. E.] Univ Waterloo, Dept Phys & Astron, Waterloo, ON N2L 3G1, Canada. [McNamara, B. R.; Broderick, A. E.] Perimeter Inst Theoret Phys, Waterloo, ON N2L 2Y5, Canada. [McNamara, B. R.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Russell, HR (reprint author), Univ Cambridge, Inst Astron, Madingley Rd, Cambridge CB3 0HA, England. EM hrr27@ast.cam.ac.uk FU ERC; Natural Sciences and Engineering Council of Canada; Canadian Space Agency Space Science Enhancement Program; Perimeter Institute for Theoretical Physics; Government of Canada through Industry Canada; Province of Ontario through the Ministry of Research and Innovation FX We thank the reviewer for helpful and constructive comments. HRR and ACF acknowledge support from ERC Advanced Grant Feedback. BRM acknowledges support from the Natural Sciences and Engineering Council of Canada and the Canadian Space Agency Space Science Enhancement Program. AEB receives financial support from the Perimeter Institute for Theoretical Physics and the Natural Sciences and Engineering Council of Canada through a Discovery Grant. 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. We also thank Alastair Edge for helpful discussions. The scientific results reported in this paper are based on data obtained from the Chandra Data Archive. NR 133 TC 14 Z9 14 U1 0 U2 0 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD JUL 21 PY 2015 VL 451 IS 1 BP 588 EP 600 DI 10.1093/mnras/stv954 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CQ8AH UT WOS:000360827800044 ER PT J AU Kauffmann, G Huang, ML Moran, S Heckman, TM AF Kauffmann, Guinevere Huang, Mei-Ling Moran, Sean Heckman, Timothy M. TI A systematic study of the inner rotation curves of galaxies observed as part of the GASS and COLD GASS surveys SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies: formation; galaxies: haloes; galaxies: stellar content; galaxies: structure ID DARK-MATTER HALOES; ARECIBO SDSS SURVEY; SPIRAL GALAXIES; MASSIVE GALAXIES; INTERMEDIATE-REDSHIFT; IRREGULAR GALAXIES; LOCAL UNIVERSE; STAR-FORMATION; DISK GALAXIES; STELLAR AB We present a systematic analysis of the rotation curves of 187 galaxies with stellar masses greater than 10(10) M circle dot, with atomic gas masses from the GALEX Arecibo Sloan Survey (GASS) and with follow-up long-slit spectroscopy from the MMT. Our analysis focuses on stellar rotation curves derived by fitting stellar template spectra to the galaxy spectra binned along the slit. In this way, we are able to obtain accurate rotation velocity measurements for a factor of 2 more galaxies than possible with the H alpha line. Galaxies with high atomic gas mass fractions are the most dark-matter-dominated galaxies in our sample and have dark matter halo density profiles that are to first order well described by Navarro Frenk White profiles with an average concentration parameter of 10. The inner slopes of the rotation curves correlate more strongly with stellar population age than with galaxy mass or structural parameters. At fixed stellar mass, the rotation curves of more actively star-forming galaxies have steeper inner slopes than less actively star-forming galaxies. The ratio between the galaxy specific angular momentum and the total specific angular momentum of its dark matter halo, R-j, correlates strongly with galaxy mass, structure and gas content. Low-mass, disc-dominated galaxies with atomic gas mass fractions greater than 20 per cent have median values of R-j of around 1, but massive, bulge-dominated galaxies have R-j = 0.2-0.3. We argue that these trends can be understood in a picture where gas inflows triggered by disc instabilities lead to the formation of passive, bulge-dominated galaxies with low specific angular momentum. C1 [Kauffmann, Guinevere; Huang, Mei-Ling] Max Planck Inst Astrophys, D-85741 Garching, Germany. [Moran, Sean] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Heckman, Timothy M.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. RP Kauffmann, G (reprint author), Max Planck Inst Astrophys, D-85741 Garching, Germany. EM gamk@mpa-garching.mpg.de NR 40 TC 0 Z9 0 U1 1 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 JUL 21 PY 2015 VL 451 IS 1 BP 878 EP 887 DI 10.1093/mnras/stv1014 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CQ8AH UT WOS:000360827800067 ER PT J AU Wirshing, HH Baker, AC AF Wirshing, Herman H. Baker, Andrew C. TI Molecular and Morphological Species Boundaries in the Gorgonian Octocoral Genus Pterogorgia (Octocorallia: Gorgoniidae) SO PLOS ONE LA English DT Article ID PHYLOGENETIC ANALYSIS; SECONDARY STRUCTURES; DNA-SEQUENCES; CNIDARIA; CORAL; MITOCHONDRIAL; ANTHOZOA; FAMILY; ALCYONACEA; EVOLUTION AB Most gorgonian octocoral species are described using diagnostic characteristics of their sclerites (microscopic skeletal components). Species in the genus Pterogorgia, however, are separated primarily by differences in their calyx and branch morphology. Specimens of a morphologically unusual Pterogorgia collected from Saba Bank in the NE Caribbean Sea were found with calyx morphology similar to P. citrina and branch morphology similar to P. guadalupensis. In order to test morphological species boundaries, and the validity of calyx and branch morphology as systematic characters, a phylogenetic analysis was undertaken utilizing partial gene fragments of three mitochondrial (mtMutS, cytochrome b, and igr4; 726bp total) and two nuclear (ITS2, 166bp; and SRP54 intron, 143bp) loci. The datasets for nuclear and mitochondrial loci contained few phylogenetically informative sites, and tree topologies did not resolve any of the morphological species as monophyletic groups. Instead, the mitochondrial loci and SRP54 each recovered two clades but were slightly incongruent, with a few individuals of P. guadalupensis represented in both clades with SRP54. A concatenated dataset of these loci grouped all P. anceps and P. guadalupensis in a clade, and P. citrina and the Pterogorgia sp. from Saba Bank in a sister clade, but with minimal variation/resolution within each clade. However, in common with other octocoral taxa, the limited genetic variation may not have been able to resolve whether branch variation represents intraspecific variation or separate species. Therefore, these results suggest that there are at least two phylogenetic lineages of Pterogorgia at the species level, and the atypical Pterogorgia sp. may represent an unusual morphotype of P. citrina, possibly endemic to Saba Bank. Branch morphology does not appear to be a reliable morphological character to differentiate Pterogorgia species (e.g., branches "flat" or "3-4 edges" in P. guadalupensis and P. anceps, respectively), and a re-evaluation of species-level characters (e.g., sclerites) is needed. C1 [Wirshing, Herman H.; Baker, Andrew C.] Univ Miami, Rosenstiel Sch Marine & Atmospher Sci, Dept Marine Biol & Ecol, Miami, FL 33149 USA. RP Wirshing, HH (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, Washington, DC 20560 USA. EM wirshingh@si.edu FU U.S. National Science Foundation [OCE-0527184]; Rowlands Graduate Fellowship, University of Miami; Knight Graduate Fellowship, University of Miami FX This work was supported by the U.S. National Science Foundation OCE-0527184 to ACB and Rowlands and Knight Graduate Fellowships, University of Miami to HHW. The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 57 TC 1 Z9 1 U1 1 U2 7 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 JUL 21 PY 2015 VL 10 IS 7 AR e0133517 DI 10.1371/journal.pone.0133517 PG 16 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA CN6LZ UT WOS:000358547600107 PM 26196389 ER PT J AU Thomaz, AT Arcila, D Orti, G Malabarba, LR AF Thomaz, Andrea T. Arcila, Dahiana Orti, Guillermo Malabarba, Luiz R. TI Molecular phylogeny of the subfamily Stevardiinae Gill, 1858 (Characiformes: Characidae): classification and the evolution of reproductive traits SO BMC EVOLUTIONARY BIOLOGY LA English DT Article DE Tetras; Neotropical region; "Clade A"; Stevardiinae; Glandulocaudinae; Insemination; Multi-locus phylogeny ID TELEOSTEI OSTARIOPHYSI CHARACIFORMES; GENUS MONOTOCHEIRODON CHARACIFORMES; UPPER RIO PARANA; FISHES TELEOSTEI; HEMIBRYCON CHARACIFORMES; SPECIES TREES; GLANDULOCAUDINAE; SPERM; SEQUENCES; COLOMBIA AB Background: The subfamily Stevardiinae is a diverse and widely distributed clade of freshwater fishes from South and Central America, commonly known as "tetras" (Characidae). The group was named "clade A" when first proposed as a monophyletic unit of Characidae and later designated as a subfamily. Stevardiinae includes 48 genera and around 310 valid species with many species presenting inseminating reproductive strategy. No global hypothesis of relationships is available for this group and currently many genera are listed as incertae sedis or are suspected to be non-monophyletic. Results: We present a molecular phylogeny with the largest number of stevardiine species analyzed so far, including 355 samples representing 153 putative species distributed in 32 genera, to test the group's monophyly and internal relationships. The phylogeny was inferred using DNA sequence data from seven gene fragments (mtDNA: 12S, 16S and COI; nuclear: RAG1, RAG2, MYH6 and PTR). The results support the Stevardiinae as a monophyletic group and a detailed hypothesis of the internal relationships for this subfamily. Conclusions: A revised classification based on the molecular phylogeny is proposed that includes seven tribes and also defines monophyletic genera, including a resurrected genus Eretmobrycon, and new definitions for Diapoma, Hemibrycon, Bryconamericus sensu stricto, and Knodus sensu stricto, placing some small genera as junior synonyms. Inseminating species are distributed in several clades suggesting that reproductive strategy is evolutionarily labile in this group of fishes. C1 [Thomaz, Andrea T.] Univ Michigan, Dept Ecol & Evolutionary Biol EEB, Ann Arbor, MI 48109 USA. [Thomaz, Andrea T.; Malabarba, Luiz R.] Univ Fed Rio Grande do Sul, Dept Zool, BR-90501970 Porto Alegre, RS, Brazil. [Arcila, Dahiana; Orti, Guillermo] George Washington Univ, Dept Biol Sci, Washington, DC 20052 USA. [Arcila, Dahiana] Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Washington, DC 20013 USA. RP Malabarba, LR (reprint author), Univ Fed Rio Grande do Sul, Dept Zool, Ave Bento Goncalves 9500, BR-90501970 Porto Alegre, RS, Brazil. EM malabarb@ufrgs.br FU DeepFin Student Exchange Program (NSF grant) [DEB-1004765]; NSF grant [DEB-1019308]; CNPQ, Brazilian Government [477318/2012-6, 300705/2010-7] FX Financial support for this study was provided by the DeepFin Student Exchange Program to DA and ATT (NSF grant DEB-1004765), by NSF grant DEB-1019308 (Euteleost Tree of Life) to GO and by CNPQ, Brazilian Government (process 300705/2010-7; 477318/2012-6) to LRM. We thank all collections and people who kindly assisted with the loan of tissues and/or specimens: M. Sabaj Perez (ANSP), N. Lujan and J. Armbruster (AUM), M. Mirande (FML), C. A. Lucena (MCP), R. Covain and S. Fisch-Muller (MHNG), P. A. Buckup and M. Britto (MNRJ), H. Ortega (MUSM), H. Lopez-Fernandez (ROM), R.G. Reina (STRI) and J. Albert (ULL). Thanks to the ichthyologists that helped in confirming the identification of vouchers: T. P. Carvalho, F. Carvalho, J. Anyelo and C. A. Lucena and to J. Burns for providing the unpublished data on the presence or absence of the insemination in some stevardiines. Finally, we are thankful to R. P. Vari and W. Fink for valuable comments on earlier versions of this manuscript. NR 76 TC 7 Z9 8 U1 1 U2 13 PU BIOMED CENTRAL LTD PI LONDON PA 236 GRAYS INN RD, FLOOR 6, LONDON WC1X 8HL, ENGLAND SN 1471-2148 J9 BMC EVOL BIOL JI BMC Evol. Biol. PD JUL 21 PY 2015 VL 15 AR 146 DI 10.1186/s12862-015-0403-4 PG 25 WC Evolutionary Biology; Genetics & Heredity SC Evolutionary Biology; Genetics & Heredity GA CN0OM UT WOS:000358113200002 PM 26195030 ER PT J AU Bally, J Mann, RK Eisner, J Andrews, SM Di Francesco, J Hughes, M Johnstone, D Matthews, B Ricci, L Williams, JP AF Bally, John Mann, Rita K. Eisner, Josh Andrews, Sean M. Di Francesco, James Hughes, Meredith Johnstone, Doug Matthews, Brenda Ricci, Luca Williams, Jonathan P. TI ALMA OBSERVATIONS OF THE LARGEST PROTO-PLANETARY DISK IN THE ORION NEBULA, 114-426: A CO SILHOUETTE SO ASTROPHYSICAL JOURNAL LA English DT Article DE circumstellar matter; protoplanetary disks; stars: pre-main sequence ID CIRCUMSTELLAR DISKS; MOLECULAR CLOUD; STAR-FORMATION; GRAIN-GROWTH; PROPLYDS; CLUSTER; PHOTOEVAPORATION; EMISSION; OBJECTS; MASSES AB We present ALMA observations of the largest protoplanetary disk in the Orion Nebula, 114-426. Detectable 345 GHz (856 mu m) dust continuum is produced only in the 350 AU central region of the similar to 1000 AU diameter silhouette seen against the bright Ha background in Hubble Space Telescope images. Assuming optically thin dust emission at 345 GHz, a gas-to-dust ratio of 100, and a grain temperature of 20 K, the disk gas-mass is estimated to be 3.1 +/- 0.6 Jupiter masses. If most solids and ices have been incorporated into large grains, however, this value is a lower limit. The disk is not detected in dense-gas tracers such as HCO+ J = 4-3, HCN J = 4-3, or CS = 7-6. These results may indicate that the 114-426 disk is evolved and depleted in some light organic compounds found in molecular clouds. The CO J = 3-2 line is seen in absorption against the bright 50-80 K background of the Orion A molecular cloud over the full spatial extent and a little beyond the dust continuum emission. The CO absorption reaches a depth of 27 K below the background CO emission at V-LSR approximate to 6.7 km s(-1) similar to 0 ''.52 (210 AU) northeast and 12 K below the background CO emission at V-LSR approximate to 9.7 km s(-1) similar to 0 ''.34 (140 AU) southwest of the suspected location of the central star, implying that the embedded star has a mass less than 1 M-circle dot. C1 [Bally, John] Univ Colorado, Dept Astrophys & Planetary Sci, Boulder, CO 80309 USA. [Mann, Rita K.; Di Francesco, James; Johnstone, Doug; Matthews, Brenda] Natl Res Council Canada, Victoria, BC V9E 2E7, Canada. [Eisner, Josh] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Andrews, Sean M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Di Francesco, James; Johnstone, Doug; Matthews, Brenda] Uivers Victoria, Dept Phys & Astron, Victoria, BC V8P 1A1, Canada. [Hughes, Meredith] Wesleyan Univ, Van Vleck Observ, Dept Astron, Middletown, CT 06459 USA. [Ricci, Luca] CALTECH, Dept Astron, Pasadena, CA 91125 USA. [Williams, Jonathan P.] Univ Hawaii, Inst Astron, Honolulu, HI 96816 USA. RP Bally, J (reprint author), Univ Colorado, Dept Astrophys & Planetary Sci, UCB 389, Boulder, CO 80309 USA. EM john.bally@colorado.edu OI Johnstone, Doug/0000-0002-6773-459X; Williams, Jonathan/0000-0001-5058-695X; Di Francesco, James/0000-0002-9289-2450 FU National Science Foundation (NSF) [AST-1009847]; Natural Sciences and Engineering Research Council (NSERC) Discovery Grant; Associated Universities, Inc. FX This research of J.B. was in part supported by National Science Foundation (NSF) grant AST-1009847. D.J. acknowledges support from a Natural Sciences and Engineering Research Council (NSERC) Discovery Grant. This paper uses ALMA data obtained with program ADS/JAO.ALMA#2011.0.00028.S. ALMA is a partnership of the European Southern Observatory (ESO) representing member states, Associated Universities Incorporated (AUI) and the National Radio Astronomy Observatories (NRAO) for the National Science Foundation (NSF) in the USA, NINS in Japan, NRC in Canada, and NSC and ASIAA in Taiwan, in cooperation with the Republic of Chile. The Joint ALMA Observatory (JAO) is operated by ESO (Europe), AUI/NRAO (USA), and NAOJ (Japan). The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. NR 30 TC 5 Z9 5 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 JUL 20 PY 2015 VL 808 IS 1 AR 69 DI 10.1088/0004-637X/808/1/69 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CO3MS UT WOS:000359062500069 ER PT J AU Burkhart, B Collins, DC Lazarian, A AF Burkhart, Blakesley Collins, David C. Lazarian, Alex TI OBSERVATIONAL DIAGNOSTICS OF SELF-GRAVITATING MHD TURBULENCE IN GIANT MOLECULAR CLOUDS SO ASTROPHYSICAL JOURNAL LA English DT Article DE dust, extinction; ISM: kinematics and dynamics; magnetic fields; magnetohydrodynamics (MHD); molecular data; stars: formation; turbulence ID ADAPTIVE MESH REFINEMENT; INITIAL MASS FUNCTION; SUPERSONIC MAGNETOHYDRODYNAMIC TURBULENCE; DENSITY PROBABILITY-DISTRIBUTION; FIELD STRENGTH FLUCTUATIONS; STAR-FORMATION RATE; ENTROPIC INDEX-Q; INTERSTELLAR TURBULENCE; MAGNETIC-FIELDS; DISTANT HELIOSPHERE AB We study the observable signatures of self-gravitating magnetohydrodynamics (MHD) turbulence by applying the probability density functions (PDFs) and the spatial density power spectrum to synthetic column density maps. We find that there exists three characterizable stages of the evolution of the collapsing cloud which we term "early," "intermediate," and "advanced." At early times, i.e., t < 0.15t(ff), the column density has a power spectral slope similar to nongravitating supersonic turbulence and a lognormal distribution. At an intermediate stage, i.e., 0.15t(ff) < t <= 0.35t(ff), there exist signatures of the first cores in the shallower PDF and power spectrum power-law slopes. The column density PDF power-law tails at these times have line of sight averaged slopes ranging from -2.5 to -1.5 with shallower values belonging to simulations with lower magnetic field strength. The density power spectrum slope becomes shallow and can be characterized by P(k) = A(1)k(beta 2)e(-k/kc), where A(1) describes the amplitude, k(beta 2) describes the classical power-law behavior, and the scale k(c) characterizes the turn over from turbulence dominated to self-gravity dominated. At advanced stages of collapse, i.e., approximate to t > 0.35t(ff), the power spectral slope is positive valued, and a dramatic increase is observed in the PDF moments and the Tsallis incremental PDF parameters, which gives rise to deviations between PDF-sonic Mach number relations. Finally, we show that the imprint of gravity on the density power spectrum can be replicated in non-gravitating turbulence by introducing a delta-function with amplitude equivalent to the maximum valued point in a given self-gravitating map. We find that the turbulence power spectrum restored through spatial filtering of the high density material. C1 [Burkhart, Blakesley] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Collins, David C.] Florida State Univ, Dept Phys, Tallahassee, FL 32306 USA. [Lazarian, Alex] Univ Wisconsin, Dept Astron, Madison, WI 53706 USA. RP Burkhart, B (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. FU NASA Einstein Fellowship; NSF grant [AST 1212096]; Center for Magnetic Self-organization in Laboratory and Astrophysical Plasmas (CMSO) FX The authors would like to thank the referee for constructive comments and suggestions which greatly improved this paper. B.B. is grateful for support from the NASA Einstein Fellowship. A.L. is supported by the NSF grant AST 1212096. B.B. and A.L. are grateful for support from the Center for Magnetic Self-organization in Laboratory and Astrophysical Plasmas (CMSO). Computer time was provided through NSF TRAC allocations TG-AST090110 and TG-MCA07S014 and the XSEDE allocation TG-AST140008. The computations were performed on Nautilus and Kraken at the National Institute for Computational Sciences (http://www.nics.tennessee.edu/) and on Stampede and Maverick at the Texas Advanced Computing Center (https://www.tacc.utexas.edu). NR 101 TC 11 Z9 11 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 JUL 20 PY 2015 VL 808 IS 1 AR 48 DI 10.1088/0004-637X/808/1/48 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CO3MS UT WOS:000359062500048 ER PT J AU Dunn, JP Wasik, B Holtzclaw, CL Yenerall, D Bautista, M Arav, N Hayes, D Moe, M Ho, LC Dutton, SH AF Dunn, Jay P. Wasik, Branden Holtzclaw, Christin L. Yenerall, David Bautista, Manuel Arav, Nahum Hayes, Daniel Moe, Max Ho, Luis C. Dutton, S. Harper TI DETERMINING THE LOCATIONS OF DUST SOURCES IN FeLoBAL QUASARS SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: evolution; quasars: absorption lines ID BROAD-ABSORPTION-LINE; DIGITAL SKY SURVEY; LARGE TELESCOPE OBSERVATIONS; GALACTIC NUCLEUS FEEDBACK; EMISSION-LINE; REDDENED QUASARS; STELLAR OBJECTS; OUTFLOW CONTRIBUTION; SEYFERT-GALAXIES; SDSS J0318-0600 AB We conduct a spectroscopic search of quasars observed by the Sloan Digital Sky Survey (SDSS) with broad absorption line (BAL) troughs due to Mg II and troughs due to Fe II that simultaneously exhibit strong Balmer narrow emission lines (NELs). We find that in a redshift range of 0.4 <= z <= 0.9, approximately 23 of the 70 Mg II BALs and 4 of a subset of 15 Fe II BALs exhibit strong Balmer emission. We also find significant fractions of Mg II BALs (approximately 23%) and those Mg II BALs with Fe II troughs (approximately 27%) have strong continuum reddening, E(B - V) >= 0.1. From measurements of the Balmer decrement in three objects, we find similarly significant reddening of the NEL region in three of the four objects; the NELs in the fourth object are not measurable. We also include one object in this study not taken from the SDSS sample that shows Fe II absorption and strong narrow emission, but due to measurement uncertainty and low continuum reddening the comparison is consistent but inconclusive. We find a trend in both the Mg II and Fe II BAL samples between the NEL reddening and continuum reddening. Because the narrow line reddening is consistent with the continuum reddening in every object in the two SDSS samples, it suggests that the reddening sources in these objects likely exist at larger radial distances than the narrow line regions from the central nucleus. C1 [Dunn, Jay P.; Wasik, Branden; Holtzclaw, Christin L.; Yenerall, David; Hayes, Daniel; Dutton, S. Harper] Georgia Perimeter Coll, Dept Phys Sci, Dunwoody, GA 30338 USA. [Bautista, Manuel] Western Michigan Univ, Dept Phys, Kalamazoo, MI 49008 USA. [Arav, Nahum] Virginia Tech, Dept Phys, Blacksburg, VA 24060 USA. [Moe, Max] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Ho, Luis C.] Peking Univ, Kavli Inst Astron & Astrophys, Beijing 100871, Peoples R China. [Ho, Luis C.] Observ Carnegie Inst Sci, Pasadena, CA 91101 USA. RP Dunn, JP (reprint author), Georgia Perimeter Coll, Dept Phys Sci, Dunwoody, GA 30338 USA. EM jdunn@gpc.edu FU Kavli Foundation, Peking University; Chinese Academy of Sciences; Carnegie Institution for Science FX L.C.H. acknowledges additional support from the Kavli Foundation, Peking University, the Chinese Academy of Sciences, and the Carnegie Institution for Science. NR 52 TC 1 Z9 1 U1 0 U2 0 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 JUL 20 PY 2015 VL 808 IS 1 AR 94 DI 10.1088/0004-637X/808/1/94 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CO3MS UT WOS:000359062500094 ER PT J AU Ferre-Mateu, A Mezcua, M Trujillo, I Balcells, M van den Bosch, RCE AF Ferre-Mateu, Anna Mezcua, Mar Trujillo, Ignacio Balcells, Marc van den Bosch, Remco C. E. TI MASSIVE RELIC GALAXIES CHALLENGE THE CO-EVOLUTION OF SUPER-MASSIVE BLACK HOLES AND THEIR HOST GALAXIES SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; black hole physics; galaxies: evolution; galaxies: formation; galaxies: nuclei; galaxies: stellar content ID DIGITAL SKY SURVEY; ACTIVE GALACTIC NUCLEI; VELOCITY DISPERSION EVOLUTION; STAR-FORMATION HISTORIES; MILES SPECTRAL COVERAGE; SIZE EVOLUTION; ELLIPTIC GALAXIES; MINOR MERGERS; NGC 1277; SCALING RELATIONS AB We study a sample of eight massive galaxies that are extreme outliers (3-5s) in the M-center dot-Mbulge local scaling relation. Two of these galaxies are confirmed to host extremely large super-massive black holes (SMBHs), whereas the virial mass estimates for the other six are also consistent with having abnormally large SMBHs. From the analysis of their star formation histories and their structural properties, we find that all of these extreme outliers can be considered to be relic galaxies from the early (z similar to 2) universe: i.e., they are compact (R-e < 2 kpc) and have purely old stellar populations (t greater than or similar to 10 Gyr). In order to explain the nature of such deviations from the local relations, we propose a scenario in which the hosts of these uber-massive SMBHs are galaxies that have followed a different evolutionary path than the two-phase growth channel assumed for massive galaxies. Once the SMBH and the core of the galaxy are formed at z similar to 2, the galaxy skips the second phase, remaining structurally untouched and without further mass and size increase. We show that if the outliers had followed the normal evolutionary path by growing in size via merger activity, the expected (mild) growth in mass would place them closer to the observed local relations. Our results suggest that the SMBH growth epoch for the most massive galaxies stopped similar to 10 Gyr ago. C1 [Ferre-Mateu, Anna] Natl Inst Nat Sci, Natl Astron Observ Japan, Subaru Telescope, Hilo, HI 96720 USA. [Mezcua, Mar] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Mezcua, Mar; Trujillo, Ignacio] Inst Astrofis Canarias, E-38205 Tenerife, Spain. [Mezcua, Mar; Trujillo, Ignacio] Univ La Laguna, Dept Astrofis, E-38205 Tenerife, Spain. [Balcells, Marc] Isaac Newton Grp Telescopes, E-38700 Tenerife, Spain. [van den Bosch, Remco C. E.] Max Planck Inst Astron, D-69117 Heidelberg, Germany. RP Ferre-Mateu, A (reprint author), Natl Inst Nat Sci, Natl Astron Observ Japan, Subaru Telescope, 650 N Aohoku Pl, Hilo, HI 96720 USA. EM aferre@naoj.org OI van den Bosch, Remco/0000-0002-0420-6159; Ferre-Mateu, Anna/0000-0002-6411-220X; Trujillo, Ignacio/0000-0001-8647-2874; Mezcua, Mar/0000-0003-4440-259X FU Japan Society for the Promotion of Science (JSPS) [23224005]; Spanish Ministerio de Economia y Competitividad (MINECO) [AYA2009-11137, AYA2011-25527, AYA2013-48226-C3-1-P] FX This work was supported by the Japan Society for the Promotion of Science (JSPS) Grant-in-Aid for Scientific Research (KAKENHI) Number 23224005 and by the Spanish Ministerio de Economia y Competitividad (MINECO; grants AYA2009-11137, AYA2011-25527, and AYA2013-48226-C3-1-P). NR 72 TC 14 Z9 14 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUL 20 PY 2015 VL 808 IS 1 AR 79 DI 10.1088/0004-637X/808/1/79 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CO3MS UT WOS:000359062500079 ER PT J AU Gentry, ES Marshall, HL Hardcastle, MJ Perlman, ES Birkinshaw, M Worrall, DM Lenc, E Siemiginowska, A Urry, CM AF Gentry, Eric S. Marshall, Herman L. Hardcastle, Martin J. Perlman, Eric S. Birkinshaw, Mark Worrall, Diana M. Lenc, Emil Siemiginowska, Aneta Urry, C. Megan TI OPTICAL DETECTION OF THE PICTOR A JET AND TIDAL TAIL: EVIDENCE AGAINST AN IC/CMB JET SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: active; galaxies: individual (Pictor A); galaxies: jets; X-rays: galaxies ID X-RAY-EMISSION; HUBBLE-SPACE-TELESCOPE; QUASAR JETS; RADIO JETS; 3C 273; CHANDRA; 3C-273; GALAXY; SPECTRA AB New images of the FR II radio galaxy Pictor A from the Hubble Space Telescope reveal a previously undiscovered tidal tail, as well as a number of jet knots coinciding with a known X-ray and radio jet. The tidal tail is approximately 5 '' wide (3 kpc projected), starting 18 '' (12 kpc) from the center of Pictor A, and extends more than 90 '' (60 kpc). The knots are part of a jet observed to be about 4' (160 kpc) long, extending to a bright hotspot. These images are the first optical detections of this jet, and by extracting knot flux densities through three filters, we set constraints on emission models. While the radio and optical flux densities are usually explained by synchrotron emission, there are several emission mechanisms that might be used to explain the X-ray flux densities. Our data rule out Doppler-boosted inverse Compton scattering as a source of the high-energy emission. Instead, we find that the observed emission can be well described by synchrotron emission from electrons with a low-energy index (p similar to 2) that dominates the radio band, while a high-energy index (p similar to 3) is needed for the X-ray band and the transition occurs in the optical/infrared band. This model is consistent with a continuous electron injection scenario. C1 [Gentry, Eric S.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. [Gentry, Eric S.; Marshall, Herman L.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Hardcastle, Martin J.] Univ Hertfordshire, Sch Phys Astron & Math, Hatfield AL10 9AB, Herts, England. [Perlman, Eric S.] Florida Inst Technol, Dept Phys & Space Sci, Melbourne, FL 32901 USA. [Birkinshaw, Mark; Worrall, Diana M.] Univ Bristol, Dept Phys, Bristol BS8 1TL, Avon, England. [Birkinshaw, Mark; Worrall, Diana M.; Siemiginowska, Aneta] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Lenc, Emil] Univ Sydney, Sch Phys, Sydney Inst Astron, Sydney, NSW 2006, Australia. [Lenc, Emil] ARC Ctr Excellence All sky Astrophys CAASTRO, Canberra, ACT, Australia. [Urry, C. Megan] Yale Univ, Dept Phys, New Haven, CT 06511 USA. RP Gentry, ES (reprint author), Univ Calif Santa Cruz, Dept Astron & Astrophys, 1156 High St, Santa Cruz, CA 95064 USA. EM egentry@ucsc.edu; hermanm@space.mit.edu; m.j.hardcastle@herts.ac.uk; eperlman@fit.edu; Mark.Birkinshaw@bristol.ac.uk; D.Worrall@bristol.ac.uk; e.lenc@physics.usyd.edu.au; aneta@head.cfa.harvard.edu; meg.urry@yale.edu OI Gentry, Eric/0000-0002-4906-3745; Birkinshaw, Mark/0000-0002-1858-277X; Lenc, Emil/0000-0002-9994-1593; Urry, Meg/0000-0002-0745-9792; Hardcastle, Martin/0000-0003-4223-1117 FU National Aeronautics and Space Administration through the Smithsonian Astrophysical Observatory [SV3-73016]; Chandra X-Ray Center; National Aeronautics Space Administration [NAS8-03060]; [CE110001020] FX We thank the referee for useful feedback that helped improve the quality of this work. Support for this work was provided by the National Aeronautics and Space Administration through the Smithsonian Astrophysical Observatory contract SV3-73016 to MIT for Support of the Chandra X-Ray Center, which is operated by the Smithsonian Astrophysical Observatory for and on behalf of the National Aeronautics Space Administration under contract NAS8-03060. The Centre for All-sky Astrophysics (CAASTRO) is an Australian Research Council Centre of Excellence, funded by grant CE110001020. NR 27 TC 5 Z9 5 U1 0 U2 0 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 JUL 20 PY 2015 VL 808 IS 1 AR 92 DI 10.1088/0004-637X/808/1/92 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CO3MS UT WOS:000359062500092 ER PT J AU Matthews, LD Reid, MJ Menten, KM AF Matthews, L. D. Reid, M. J. Menten, K. M. TI NEW MEASUREMENTS OF THE RADIO PHOTOSPHERE OF MIRA BASED ON DATA FROM THE JVLA AND ALMA SO ASTROPHYSICAL JOURNAL LA English DT Article DE stars: AGB and post-AGB; stars: atmospheres; stars: fundamental parameters; stars: imaging ID VY CANIS MAJORIS; SYMBIOTIC STARS; VARIABLE-STARS; O-CETI; BINARY; EMISSION; INTERFEROMETRY; CONVECTION; ATMOSPHERE; LUMINOSITY AB We present new measurements of the millimeter wavelength continuum emission from the long period variable Mira (o Ceti) at frequencies of 46, 96, and 229 GHz (lambda approximate to 7, 3, and 1 mm) based on observations obtained with the Jansky Very Large Array (JVLA) and the Atacama Large Millimeter/submillimeter Array (ALMA). The measured millimeter flux densities are consistent with a radio photosphere model derived from previous observations, where flux density S-nu alpha nu(1.86). The stellar disk is resolved, and the measurements indicate a decrease in the size of the radio photosphere at higher frequencies, as expected if the opacity decreases at shorter wavelengths. The shape of the radio photosphere is found to be slightly elongated, with a flattening of similar to 10%-20%. The data also reveal evidence for brightness non-uniformities on the surface of Mira at radio wavelengths. Mira's hot companion, Mira B was detected at all three observed wavelengths, and we measure a radius for its radio-emitting surface of approximate to 2.0 x 10(13) cm. The data presented here highlight the power of the JVLA and ALMA for the study of the atmospheres of evolved stars. C1 [Matthews, L. D.] MIT, Haystack Observ, Westford, MA 01886 USA. [Reid, M. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Menten, K. M.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. RP Matthews, LD (reprint author), MIT, Haystack Observ, Off Route 40, Westford, MA 01886 USA. EM lmatthew@haystack.mit.edu FU Associated Universities, Inc. FX The authors thank T. Kaminski for valuable discussions and E. Greisen for developments in AIPS that aided this work. The JVLA observations presented here were part of NRAO program 14A-026. This paper makes use of the following ALMA data: ADS/JAO.ALMA #2011.0.00014.SV. ALMA is a partnership of ESO (representing its member states), NSF (USA), and NINS (Japan), together with NRC (Canada) and NSC and ASIAA (Taiwan), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by ESO, AUI/NRAO and NAOJ. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. NR 51 TC 5 Z9 5 U1 0 U2 0 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 JUL 20 PY 2015 VL 808 IS 1 AR 36 DI 10.1088/0004-637X/808/1/36 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CO3MS UT WOS:000359062500036 ER PT J AU Minh, YC Liu, HB Su, YN Hsieh, PY Liu, SY Kim, SS Wright, M Ho, PTP AF Minh, Young Chol Liu, Hauyu Baobab Su, Yu-Nung Hsieh, Pei-Ying Liu, Sheng-Yuan Kim, Sungsoo S. Wright, Melvyn Ho, Paul T. P. TI EMISSION IN THE GALACTIC CENTER SO ASTROPHYSICAL JOURNAL LA English DT Article DE Galaxy: center; ISM: individual objects (Sgr A, Circumnuclear Disk); ISM: molecules; radio lines: ISM; submillimeter: galaxies ID APERTURE SYNTHESIS OBSERVATIONS; SUPERMASSIVE BLACK-HOLE; SGR A-ASTERISK; CIRCUMNUCLEAR DISK; MOLECULAR ENVIRONMENT; STELLAR ORBITS; STAR-FORMATION; INFALLING GAS; CENTER REGION; SIO EMISSION AB The gas traced by the SiO 1-0 emission appears to not have a direct connection or interaction with the circumnuclear disk (CND). In contrast, higher-resolution observations of the SiO 5-4 emission confirm the dissymmetric gas distribution of the CND, as well as a large concentration of gas in the CND's southwest region. In particular, the SiO 5-4 emission peaks toward what is likely the "convergent" position, where the west arc of Sgt A West overlaps with the CND. We think that this is the position where several incoming and outgoing gas flows interact with each other. The high angular resolution (approximate to 1 ''.5) observations of the SiO 5-4 emission show several emission clumps with sizes similar to 2 ''. These clumps have different velocities that may have resulted from a collision with incoming clouds. We confirm that the overall fractional abundance of SiO is about 10-9 relative to the total H-2, and it probably resulted from the large-scale shocks prevalent in the Galactic center region. A comparison of the SiO fractional abundance suggests that in addition to the dense ambient cloud component, which surrounds but does not interact much with the CND, there are separate gas components that have more interactions with the CND. C1 [Minh, Young Chol] Korea Astron & Space Sci Inst, Taejon 305348, South Korea. [Liu, Hauyu Baobab; Su, Yu-Nung; Hsieh, Pei-Ying; Liu, Sheng-Yuan; Ho, Paul T. P.] Acad Sinica, Inst Astron & Astrophys, Taipei 10617, Taiwan. [Kim, Sungsoo S.] Kyung Hee Univ, Dept Astron & Space Sci, Yongin 446701, Kyungki Do, South Korea. [Wright, Melvyn] Univ Calif Berkeley, Radio Astron Lab, Berkeley, CA 94720 USA. [Ho, Paul T. P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Minh, YC (reprint author), Korea Astron & Space Sci Inst, 776 Daeduk Daero, Taejon 305348, South Korea. NR 41 TC 0 Z9 0 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUL 20 PY 2015 VL 808 IS 1 AR 86 DI 10.1088/0004-637X/808/1/86 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CO3MS UT WOS:000359062500086 ER PT J AU Mobasher, B Dahlen, T Ferguson, HC Acquaviva, V Barro, G Finkelstein, SL Fontana, A Gruetzbauch, R Johnson, S Lu, Y Papovich, CJ Pforr, J Salvato, M Somerville, RS Wiklind, T Wuyts, S Ashby, MLN Bell, E Conselice, CJ Dickinson, ME Faber, SM Fazio, G Finlator, K Galametz, A Gawiser, E Giavalisco, M Grazian, A Grogin, NA Guo, YC Hathi, N Kocevski, D Koekemoer, AM Koo, DC Newman, JA Reddy, N Santini, P Wechsler, RH AF Mobasher, Bahram Dahlen, Tomas Ferguson, Henry C. Acquaviva, Viviana Barro, Guillermo Finkelstein, Steven L. Fontana, Adriano Gruetzbauch, Ruth Johnson, Seth Lu, Yu Papovich, Casey J. Pforr, Janine Salvato, Mara Somerville, Rachel S. Wiklind, Tommy Wuyts, Stijn Ashby, Matthew L. N. Bell, Eric Conselice, Christopher J. Dickinson, Mark E. Faber, Sandra M. Fazio, Giovanni Finlator, Kristian Galametz, Audrey Gawiser, Eric Giavalisco, Mauro Grazian, Andrea Grogin, Norman A. Guo, Yicheng Hathi, Nimish Kocevski, Dale Koekemoer, Anton M. Koo, David C. Newman, Jeffrey A. Reddy, Naveen Santini, Paola Wechsler, Risa H. TI A CRITICAL ASSESSMENT OF STELLAR MASS MEASUREMENT METHODS SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: distances and redshifts; galaxies: high-redshift; galaxies: photometry; surveys ID LYMAN-BREAK GALAXIES; ULTRA-DEEP FIELD; SPACE-TELESCOPE OBSERVATIONS; EXTRAGALACTIC LEGACY SURVEY; STAR-FORMATION HISTORIES; BROAD-BAND PHOTOMETRY; SIMILAR-TO 7; POPULATION SYNTHESIS; LUMINOSITY FUNCTION; NEBULAR EMISSION AB This is the second paper in a series aimed at investigating the main sources of uncertainty in measuring the observable parameters in galaxies from their spectral energy distributions (SEDs). In the first paper we presented a detailed account of the photometric redshift measurements and an error analysis of this process. In this paper we perform a comprehensive study of the main sources of random and systematic error in stellar mass estimates for galaxies, and their relative contributions to the associated error budget. Since there is no prior knowledge of the stellar mass of galaxies (unlike their photometric redshifts), we use mock galaxy catalogs with simulated multi-waveband photometry and known redshift, stellar mass, age and extinction for individual galaxies. The multi-waveband photometry for the simulated galaxies were generated in 13 filters spanning from U-band to mid- infrared wavelengths. Given different parameters affecting stellar mass measurement (photometric signal-to-noise ratios (S/N), SED fitting errors and systematic effects), the inherent degeneracies and correlated errors, we formulated different simulated galaxy catalogs to quantify these effects individually. For comparison, we also generated catalogs based on observed photometric data of real galaxies in the Great Observatories Origins Deep Survey-South field, spanning the same passbands. The simulated and observed catalogs were provided to a number of teams within the Cosmic Assembly Near-infrared Deep Extragalactic Legacy Survey collaboration to estimate the stellar masses for individual galaxies. A total of 11 teams participated, with different combinations of stellar mass measurement codes/methods, population synthesis models, star formation histories, extinction and age. For each simulated galaxy, the differences between the input stellar masses, M-input, and those estimated by each team, M-est, is defined as Delta log(M) equivalent to log(M-estimated) - log(M-input), and used to identify the most fundamental parameters affecting stellar mass estimate in galaxies, with the following results. (1) No significant bias in Delta log(M) was found among different codes, with all having comparable scatter (sigma(Dlog(M))= 0.136 dex). The estimated stellar mass values are seriously affected by low photometric S/N, with the rms scatter increasing for galaxies with H-AB > 26 mag; (2) A source of error contributing to the scatter in Delta log(M) is found to be due to photometric uncertainties (0.136 dex) and low resolution in age and extinction grids when generating the SED templates; (3) The median of stellar masses among different methods provides a stable measure of the mass associated with any given galaxy (sigma(Delta log(M)) = 0.142 dex); (4) The Delta log(M) values are strongly correlated with deviations in age (defined as the difference between the estimated and expected values), with a weaker correlation with extinction; (5) The rms scatter in the estimated stellar masses due to free parameters (after fixing redshifts and initial mass function) are quantified and found to be sigma(Delta log(M)) = 0.110 dex; (6) Using the observed data, we studied the sensitivity of stellar masses to both the population synthesis codes and inclusion of nebular emission lines and found them to affect the stellar mass by 0.2 and 0.3 dex respectively. C1 [Mobasher, Bahram; Reddy, Naveen] Univ Calif Riverside, Dept Phys & Astron, Riverside, CA 92521 USA. [Dahlen, Tomas; Ferguson, Henry C.; Grogin, Norman A.; Koekemoer, Anton M.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Acquaviva, Viviana] CUNY, NYC Coll Technol, Dept Phys, Brooklyn, NY 11201 USA. [Barro, Guillermo; Faber, Sandra M.; Guo, Yicheng; Koo, David C.] Univ Calif Santa Cruz, Dept Astron & Astrophys, UCO Lick Observ, Santa Cruz, CA 95064 USA. [Finkelstein, Steven L.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA. [Fontana, Adriano; Galametz, Audrey; Grazian, Andrea; Santini, Paola] Osserv Astron Roma, INAF, I-00040 Monte Porzio Catone, Italy. [Gruetzbauch, Ruth] Observ Astron Lisboa, Ctr Astron & Astrophys, P-1349018 Lisbon, Portugal. [Johnson, Seth; Giavalisco, Mauro] Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA. [Lu, Yu; Wechsler, Risa H.] Stanford Univ, Kavli Inst Particle Phys & Cosmol, Stanford, CA 94305 USA. [Papovich, Casey J.] Texas A&M Res Fdn, Dept Phys & Astron, College Stn, TX 77843 USA. [Pforr, Janine; Dickinson, Mark E.] Natl Opt Astron Observ, Tucson, AZ 85719 USA. [Salvato, Mara; Wuyts, Stijn] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Somerville, Rachel S.; Gawiser, Eric] Rutgers State Univ, Dept Phys & Astron, Piscataway, NJ 08854 USA. [Wiklind, Tommy] Joint ALMA Observ, Santiago, Chile. [Ashby, Matthew L. N.; Fazio, Giovanni] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Bell, Eric] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Conselice, Christopher J.] Univ Nottingham, Sch Phys & Astron, Nottingham NG7 2RD, England. [Finlator, Kristian] Univ Copenhagen, Niels Bohr Inst, Dark Cosmol Ctr, DK-1168 Copenhagen, Denmark. [Hathi, Nimish] LAM Lab Astrophys Marseille, F-13388 Marseille 13, France. [Kocevski, Dale] Univ Kentucky, Dept Phys & Astron, Lexington, KY 40506 USA. [Newman, Jeffrey A.] Univ Pittsburgh, Dept Phys & Astron, Pittsburgh, PA 15260 USA. RP Mobasher, B (reprint author), Univ Calif Riverside, Dept Phys & Astron, Riverside, CA 92521 USA. RI Hathi, Nimish/J-7092-2014; OI Koekemoer, Anton/0000-0002-6610-2048; Bell, Eric/0000-0002-5564-9873; Hathi, Nimish/0000-0001-6145-5090; Santini, Paola/0000-0002-9334-8705 NR 44 TC 18 Z9 18 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 JUL 20 PY 2015 VL 808 IS 1 AR 101 DI 10.1088/0004-637X/808/1/101 PG 28 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CO3MS UT WOS:000359062500101 ER PT J AU Pennucci, TT Possenti, A Esposito, P Rea, N Haggard, D Baganoff, FK Burgay, M Zelati, FC Israel, GL Minter, A AF Pennucci, T. T. Possenti, A. Esposito, P. Rea, N. Haggard, D. Baganoff, F. K. Burgay, M. Zelati, F. Coti Israel, G. L. Minter, A. TI SIMULTANEOUS MULTI-BAND RADIO AND X-RAY OBSERVATIONS OF THE GALACTIC CENTER MAGNETAR SGR 1745-2900 SO ASTROPHYSICAL JOURNAL LA English DT Article DE Galaxy: center; pulsars: individual (PSR J1745-2900, SGR 1745-2900); stars: magnetars ID GIGAHERTZ-PEAKED SPECTRA; SAGITTARIUS-A-ASTERISK; CENTER PULSAR POPULATION; SUPERMASSIVE BLACK-HOLE; SOFT GAMMA-REPEATERS; NEUTRON-STARS; FLUX-DENSITY; MAGNETOTHERMAL EVOLUTION; BROADENING MEASUREMENTS; DISPERSION MEASURE AB We report on multi-frequency, wideband radio observations of the Galactic Center magnetar (SGR 1745-2900) with the Green Bank Telescope for similar to 100 days immediately following its initial X-ray outburst in 2013 April. We made multiple simultaneous observations at 1.5, 2.0, and 8.9 GHz, allowing us to examine the magnetar's flux evolution, radio spectrum, and interstellar medium parameters (such as the dispersion measure (DM), the scattering timescale, and its index). During two epochs, we have simultaneous observations from the Chandra X-ray Observatory, which permitted the absolute alignment of the radio and X-ray profiles. As with the two other radio magnetars with published alignments, the radio profile lies within the broad peak of the X-ray profile, preceding the X-ray profile maximum by similar to 0.2 rotations. We also find that the radio spectral index gamma is significantly negative between similar to 2 and 9 GHz; during the final similar to 30 days of our observations gamma similar to -1.4, which is typical of canonical pulsars. The radio flux has not decreased during this outburst, whereas the long-term trends in the other radio magnetars show concomitant fading of the radio and X-ray fluxes. Finally, our wideband measurements of the DMs taken in adjacent frequency bands in tandem are stochastically inconsistent with one another. Based on recent theoretical predictions, we consider the possibility that the DM is frequency-dependent. Despite having several properties in common with the other radio magnetars, such as L-X,L-qui/L-rot less than or similar to 1, an increase in the radio flux during the X-ray flux decay has not been observed thus far in other systems. C1 [Pennucci, T. T.] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA. [Possenti, A.; Burgay, M.] Osservatorio Astron Cagliari, I-09047 Cagliari, Italy. [Esposito, P.] INAF, Ist Astrofis Spaziale & Fis Cosm Milano, I-20133 Milan, Italy. [Esposito, P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Rea, N.; Zelati, F. Coti] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1090 GE Amsterdam, Netherlands. [Rea, N.] CSIC, IEEC, Inst Space Sci ICE, E-08193 Barcelona, Spain. [Haggard, D.] Amherst Coll, Dept Phys & Astron, Amherst, MA 01002 USA. [Baganoff, F. K.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Zelati, F. Coti] Univ Insubria, I-22100 Como, Italy. [Zelati, F. Coti] INAF Osservatorio Astron Brera, I-23807 Merate, LC, Italy. [Israel, G. L.] INAF Osservatorio Astron Roma, I-00040 Rome, Italy. [Minter, A.] Natl Radio Astron Observ, Green Bank, WV 24944 USA. RP Pennucci, TT (reprint author), Univ Virginia, Dept Astron, POB 400325, Charlottesville, VA 22904 USA. EM pennucci@virginia.edu OI Burgay, Marta/0000-0002-8265-4344; Israel, GianLuca/0000-0001-5480-6438; Esposito, Paolo/0000-0003-4849-5092; Rea, Nanda/0000-0003-2177-6388 FU National Science Foundation [0968296]; US. Department of State; Chandra X-ray Observatory Award [GO3-14121X]; NASA [NAS8-03060, NNX14AC30G]; NWO; European COST Action [MP1304]; [AYA2012-39303]; [SGR2014-1073] FX The authors would like to thank S. Ransom and P. Demorest for useful discussions and comments, as well as A. Bilous for significant contributions and a review of the manuscript. T. T. P. would also like to acknowledge the hospitality of the astronomers at the Osservatorio Astronomico di Cagliari, where this paper began. T. T. P. is supported in part by a National Science Foundation PIRE Grant (0968296) through NANOGrav and is a graduate student at the National Radio Astronomy Observatory (NRAO). The NRAO is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. P. E. acknowledges a Fulbright Research Scholar grant administered by the US-Italy Fulbright Commission and is grateful to the Harvard-Smithsonian Center for Astrophysics for hosting him during his Fulbright exchange. The Fulbright Scholar Program is sponsored by the US. Department of State and administered by CIES, a division of IIE. D. H. acknowledges support from Chandra X-ray Observatory Award Number GO3-14121X, operated by the Smithsonian Astrophysical Observatory for and on behalf of NASA under contract NAS8-03060, and also by NASA Swift grant NNX14AC30G. N. R. and F. C. Z. are supported by an NWO Vidi Grant (PI: N. Rea) and by the European COST Action MP1304 (NewCOMPSTAR). N. R. acknowledges support by grants AYA2012-39303 and SGR2014-1073. NR 80 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 JUL 20 PY 2015 VL 808 IS 1 AR 81 DI 10.1088/0004-637X/808/1/81 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CO3MS UT WOS:000359062500081 ER PT J AU Rubin, KHR Hennawi, JF Prochaska, JX Simcoe, RA Myers, A Lau, MW AF Rubin, Kate H. R. Hennawi, Joseph F. Prochaska, J. Xavier Simcoe, Robert A. Myers, Adam Lau, Marie Wingyee TI DISSECTING THE GASEOUS HALOS OF z similar to 2 DAMPED Ly alpha SYSTEMS WITH CLOSE QUASAR PAIRS SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: halos; galaxies: ISM; quasars: absorption lines ID STAR-FORMING GALAXIES; MASS-METALLICITY RELATION; DIGITAL SKY SURVEY; MG II ABSORPTION; OSCILLATION SPECTROSCOPIC SURVEY; GRAVITATIONALLY LENSED QUASAR; OPTICALLY THICK ABSORBERS; BARYONIC STRUCTURE SURVEY; REST-FRAME ULTRAVIOLET; LYMAN BREAK GALAXIES AB We use spectroscopy of close pairs of quasars to study diffuse gas in the circumgalactic medium (CGM) surrounding a sample of 40 damped Ly alpha systems (DLAs). The primary sightline in each quasar pair probes an intervening DLA in the redshift range 1.6 < z(DLA) < 3.6, such that the second quasar sightline then probes Ly alpha, C II, Si II, and C IV absorption in the CGM transverse to the DLA to projected distances R-perpendicular to < 300 kpc. Analysis of the Ly alpha profiles in these CGM sightlines constrains the covering fraction (f(C)) of optically thick H I (having column density N-H (I) > 10(17.2) cm(-2)) to be greater than or similar to 30% within R-perpendicular to < 200 kpc. Strong Si II lambda 1526 absorption with equivalent width W-1526 > 0.2 angstrom occurs with an incidence f(C) (W-1526 > 0.2 angstrom) = 20(-8)(+12) within R-perpendicular to < 100 kpc, indicating that Si II absorption associated with DLAs probes material within a physical distance R-3D less than or similar to 30 kpc. However, we find that strong C IV lambda 1548 absorption is ubiquitous in these environments (f(C)(W-1548 > 0.2 angstrom) = 57(-13)(+12)% within R-perpendicular to < 100 kpc), and in addition exhibits a high degree of kinematic coherence on scales up to similar to 175 kpc. We infer that this high-ionization material arises predominantly in large, quiescent structures extending beyond the scale of the DLA host dark matter halos rather than in ongoing galactic winds. The Ly alpha equivalent width in the DLA-CGM is anticorrelated with R-perpendicular to at > 98% confidence, suggesting that DLAs arise close to the centers of their host halos rather than on their outskirts. Finally, the average Ly alpha, and C II and C IV equivalent widths measured as a function of R-perpendicular to are consistent with those measured around z similar to 2 Lyman break galaxies. Assuming that DLAs trace a galaxy population at lower masses and luminosities, this finding implies that the absorption strength of cool circumgalactic material has a weak dependence on dark matter halo mass at M-h less than or similar to 10(12) M-circle dot. C1 [Rubin, Kate H. R.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Rubin, Kate H. R.; Hennawi, Joseph F.; Prochaska, J. Xavier] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Prochaska, J. Xavier; Lau, Marie Wingyee] Univ Calif Santa Cruz, UCO Lick Observ, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. [Simcoe, Robert A.] MIT, MIT Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Myers, Adam] Univ Wyoming, Dept Phys & Astron, Laramie, WY 82072 USA. RP Rubin, KHR (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM krubin@cfa.harvard.edu FU Alexander von Humboldt foundation; German Federal Ministry for Education and Research; National Science Foundation (NSF) [AST-1010004, AST-1109452, AST-1109447, AST-1412981]; W.M. Keck Foundation; Clay Postdoctoral Fellowship FX The authors wish to thank Sara Ellison, Crystal Martin, and George Djorgovski for aiding in collection and reduction of the Keck/ESI spectroscopy used in this study. We also wish to thank the anonymous referee for useful comments which improved the manuscript. It is our pleasure to thank Neil Crighton, Simeon Bird, Jeff Cooke, Claude-Andre Faucher-Giguere, Michele Fumagalli, John O'Meara, Celine Peroux, Ali Rahmati, and Sijing Shen for valuable discussion of this work, and to acknowledge Sijing Shen for sharing the results of her analysis of the CGM properties of the Eris2 simulation. Finally, we are grateful to Art Wolfe for sharing his insight on these results and for his inspiring and pioneering work in this field. K.H.R.R. acknowledges the generous support of the Clay Postdoctoral Fellowship, and J.F.H. acknowledges support from the Alexander von Humboldt foundation in the context of the Sofja Kovalevskaja Award. The Humboldt foundation is funded by the German Federal Ministry for Education and Research. J.X.P. and M.L. acknowledge support from National Science Foundation (NSF) grants AST-1010004, AST-1109452, AST-1109447, and AST-1412981. This paper includes data gathered with the 6.5m Magellan Telescopes located at Las Campanas Observatory, Chile. Some of the data presented herein were obtained at the W.M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California, and the National Aeronautics and Space Administration. The Observatory was made possible by the generous financial support of the W.M. Keck Foundation. The authors 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. NR 108 TC 7 Z9 7 U1 0 U2 0 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 JUL 20 PY 2015 VL 808 IS 1 AR 38 DI 10.1088/0004-637X/808/1/38 PG 30 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CO3MS UT WOS:000359062500038 ER PT J AU Swartz, DA Pavlov, GG Clarke, T Castelletti, G Zavlin, VE Bucciantini, N Karovska, M van der Horst, AJ Yukita, M Weisskopf, MC AF Swartz, Douglas A. Pavlov, George G. Clarke, Tracy Castelletti, Gabriela Zavlin, Vyacheslav E. Bucciantini, Niccolo Karovska, Margarita van der Horst, Alexander J. Yukita, Mihoko Weisskopf, Martin C. TI HIGH SPATIAL RESOLUTION X-RAY SPECTROSCOPY OF THE IC 443 PULSAR WIND NEBULA AND ENVIRONS SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM: individual objects (G189.22+2.90, IC 443); ISM: supernova remnants; stars: neutron; X-rays: individual (CXOU J061705.3+222127); X-rays: ISM ID SUPERNOVA REMNANT IC-443; BOW-SHOCK NEBULAE; VELA PULSAR; EMISSION; ROTATION; SPECTRUM; JET AB Deep Chandra ACIS observations of the region around the putative pulsar, CXOU J061705.3+222127, in the supernova remnant (SNR) IC 443 reveal an similar to 5 '' radius ring-like structure surrounding the pulsar and a jet-like feature oriented roughly north-south across the ring and through the pulsar's location at 06(h)17(m)5(s).200 + 22 degrees 21' 27 ''.52 (J2000.0 coordinates). The observations further confirm that (1) the spectrum and flux of the central object are consistent with a rotation-powered pulsar, (2) the non-thermal spectrum and morphology of the surrounding nebula are consistent with a pulsar wind, and (3) the spectrum at greater distances is consistent with thermal emission from the SNR. The cometary shape of the nebula, suggesting motion toward the southwest, appears to be subsonic: There is no evidence either spectrally or morphologically for a bow shock or contact discontinuity; the nearly circular ring is not distorted by motion through the ambient medium; and the shape near the apex of the nebula is narrow. Comparing this observation with previous observations of the same target, we set a 99% confidence upper limit to the proper motion of CXOU J061705.3+222127 to be less than 44 mas yr(-1) (310 km s(-1) for a distance of 1.5 kpc), with the best-fit (but not statistically significant) projected direction toward the west. C1 [Swartz, Douglas A.; Zavlin, Vyacheslav E.] NASA, USRA, Astrophys Off, Marshall Space Flight Ctr, Huntsville, AL 35812 USA. [Pavlov, George G.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Clarke, Tracy] Naval Res Lab, Remote Sensing Div, Washington, DC USA. [Castelletti, Gabriela] UBA, CONICET, IAFE, Buenos Aires, DF, Argentina. [Bucciantini, Niccolo] INAF Osservatorio Astrofis Arcetri, I-50125 Florence, Italy. [Bucciantini, Niccolo] INFN Sez Firenze, I-50019 Florence, Italy. [Karovska, Margarita] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. [van der Horst, Alexander J.] George Washington Univ, Dept Phys, Washington, DC 20052 USA. [Yukita, Mihoko] Johns Hopkins Univ, Baltimore, MD 21218 USA. [Yukita, Mihoko] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Weisskopf, Martin C.] NASA, Astrophys Off, Marshall Space Flight Ctr, Huntsville, AL 35812 USA. RP Swartz, DA (reprint author), NASA, USRA, Astrophys Off, Marshall Space Flight Ctr, ZP12, Huntsville, AL 35812 USA. RI Yukita, Mihoko/E-4135-2017; OI Bucciantini, Niccolo'/0000-0002-8848-1392 FU National Aeronautics Space Administration [NAS8-03060]; 6.1 Base funding FX The Chandra observations were obtained in response to Chandra Proposal Number 13500093 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. Optical observations were obtained with the SARA Observatory 0.9 m telescope at Kitt Peak, which is owned and operated by the Southeastern Association for Research in Astronomy. Basic research in radio astronomy at the Naval Research Laboratory (TC) is supported by 6.1 Base funding. NR 36 TC 1 Z9 1 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 JUL 20 PY 2015 VL 808 IS 1 AR 84 DI 10.1088/0004-637X/808/1/84 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CO3MS UT WOS:000359062500084 ER PT J AU Temim, T Slane, P Kolb, C Blondin, J Hughes, JP Bucciantini, N AF Temim, Tea Slane, Patrick Kolb, Christopher Blondin, John Hughes, John P. Bucciantini, Niccolo TI LATE-TIME EVOLUTION OF COMPOSITE SUPERNOVA REMNANTS: DEEP CHANDRA OBSERVATIONS AND HYDRODYNAMICAL MODELING OF A CRUSHED PULSAR WIND NEBULA IN SNR G327.1-1.1 SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM: individual objects (G327.1-1.1); ISM: supernova remnants; pulsars: general; radiation mechanisms: non-thermal; stars: neutron ID AREA TELESCOPE OBSERVATIONS; X-RAY; EMISSION AB In an effort to better understand the evolution of composite supernova remnants (SNRs) and the eventual fate of relativistic particles injected by their pulsars, we present a multifaceted investigation of the interaction between a pulsar wind nebula (PWN) and its host SNR G327.1-1.1. Our 350 Chandra X-ray observations of SNR G327.1-1.1 reveal a highly complex morphology: a cometary structure resembling a bow shock, prong-like features extending into large arcs in the SNR interior, and thermal emission from the SNR shell. Spectral analysis of the non-thermal emission offers clues about the origin of the PWN structures, while enhanced abundances in the PWN region provide evidence for a mixing of supernova ejecta with PWN material. The overall morphology and spectral properties of the SNR suggest that the PWN has undergone an asymmetric interaction with the SNR reverse shock (RS), whichcan occur as a result of a density gradient in the ambient medium and/or a moving pulsar that displaces the PWN from the center of the remnant. We present hydrodynamical simulations of G327.1-1.1 that show that its morphology and evolution can be described by a similar to 17,000-year-old composite SNR that expanded into a density gradient with an orientation perpendicular to the pulsar's motion. We also show that the RS/PWN interaction scenario can reproduce the broadband spectrum of the PWN from radio to.-ray wavelengths. The analysis and modeling presented in this work have important implications for our general understanding of the structure and evolution of composite SNRs. C1 [Temim, Tea] NASA, Goddard Space Flight Ctr, Observat Cosmol Lab, Greenbelt, MD 20771 USA. [Temim, Tea] Univ Maryland, CRESST, College Pk, MD 20742 USA. [Slane, Patrick] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Kolb, Christopher; Blondin, John] N Carolina State Univ, Raleigh, NC 27695 USA. [Hughes, John P.] Rutgers State Univ, New Brunswick, NJ 08901 USA. [Bucciantini, Niccolo] INAF Osservatorio Astrofis Arcetri, I-50125 Florence, Italy. RP Temim, T (reprint author), NASA, Goddard Space Flight Ctr, Observat Cosmol Lab, Code 665, Greenbelt, MD 20771 USA. OI Bucciantini, Niccolo'/0000-0002-8848-1392; Blondin, John/0000-0001-9691-6803; Temim, Tea/0000-0001-7380-3144 FU NASA [GO2-13075A, NAS8-03060] FX This work was supported by NASA under the grant number GO2-13075A. P.S. acknowledge support from the NASA Contract NAS8-03060. NR 27 TC 2 Z9 2 U1 2 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 JUL 20 PY 2015 VL 808 IS 1 AR 100 DI 10.1088/0004-637X/808/1/100 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CO3MS UT WOS:000359062500100 ER PT J AU Cordero, MJ Hansen, CJ Johnson, CI Pilachowski, CA AF Cordero, M. J. Hansen, C. J. Johnson, C. I. Pilachowski, C. A. TI A COMPARATIVE STUDY OF TWO 47 Tuc GIANT STARS WITH DIFFERENT s-PROCESS ENRICHMENT SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE globular clusters: individual (47 Tuc); stars: abundances; stars: chemically peculiar ID NEUTRON-CAPTURE ELEMENTS; GLOBULAR-CLUSTERS; ABUNDANCE VARIATIONS; STELLAR POPULATIONS; CHEMICAL ABUNDANCE; HEAVY-ELEMENTS; BRANCH STARS; BARIUM STARS; LARGE-SAMPLE; EVOLUTION AB Here we aim to understand the origin of 47 Tuc's La-rich star Lee 4710. We report abundances for O, Na, Mg, Al, Si, Ca, Sc, Ti, V, Cr, Co, Ni, Zn, Y, Zr, Ba, La, Ce, Pr, Nd, and Eu and present a detailed abundance analysis of two 47 Tuc stars with similar stellar parameters but different slow neutron-capture (s-)process enrichment. Star Lee 4710 has the highest known La abundance ratio in this cluster ([La/Fe] = 1.14), and star Lee 4626 is known to have normal s-process abundances (e.g., [Ba/Eu] < 0). The nucleosynthetic pattern of elements with Z greater than or similar to 56 for star Lee 4710 agrees with the predicted yields of a 1.3 M-circle dot asymptotic giant branch (AGB) star. Therefore, Lee 4710 may have been enriched by mass transfer from a more massive AGB companion, which is compatible with its location far away from the center of this relatively metal-rich ([Fe/H] similar to -0.7) globular cluster. A further analysis comparing the abundance pattern of Lee 4710 with data available in the literature reveals that nine out of the similar to 200 47 Tuc stars previously studied show strong s-process enhancements that point toward later enrichment by more massive AGB stars. C1 [Cordero, M. J.] Heidelberg Univ, Zentrum Astron, Astron Rech Inst, D-69120 Heidelberg, Germany. [Cordero, M. J.; Hansen, C. J.] Heidelberg Univ, ZAH, D-69117 Heidelberg, Germany. [Hansen, C. J.] Niels Bohr Inst, Dark Cosmol Ctr, DK-2100 Copenhagen, Denmark. [Johnson, C. I.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Pilachowski, C. A.] Indiana Univ, Dept Astron, Bloomington, IN 47405 USA. RP Cordero, MJ (reprint author), Heidelberg Univ, Zentrum Astron, Astron Rech Inst, Monchhofstr 12-14, D-69120 Heidelberg, Germany. EM mjcorde@ari.uni-heidelberg.de; cjhansen@lsw.uni-heidelberg.de; cjohnson@cfa.harvard.edu; catyp@astro.indiana.edu OI Hansen, Camilla Juul/0000-0002-7277-7922; Pilachowski, Catherine/0000-0002-3007-206X FU German Research Foundation (DFG) [Sonderforschungsbereich SFB 881]; VILLUM FONDEN [VKR023371]; Clay Fellowship FX We thank the referee for useful comments. M.J.C. and C.J.H. were supported by Sonderforschungsbereich SFB 881 "The Milky Way System" (subproject A4, A5, and A8) of the German Research Foundation (DFG) and C.J.H. also by a research grant (VKR023371) from VILLUM FONDEN. C.I.J. acknowledges support from the Clay Fellowship, administered by the Smithsonian Astrophysical Observatory. C.J.H. thanks Thomas Masseron for a fruitful discussion. NR 33 TC 3 Z9 3 U1 1 U2 2 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 JUL 20 PY 2015 VL 808 IS 1 AR L10 DI 10.1088/2041-8205/808/1/L10 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CN9OO UT WOS:000358778900010 ER PT J AU Kunder, A Rich, RM Hawkins, K Poleski, R Storm, J Johnson, CI Shen, J Li, ZY Cordero, MJ Nataf, DM Bono, G Walker, AR Koch, A De Propris, R Udalski, A Szymanski, MK Soszynski, I Pietrzynski, G Ulaczyk, K Wyrzykowski, L Pietrukowicz, P Skowron, J Kozlowski, S Mroz, P AF Kunder, Andrea Rich, R. M. Hawkins, K. Poleski, R. Storm, J. Johnson, C. I. Shen, J. Li, Z. -Y. Cordero, M. J. Nataf, D. M. Bono, G. Walker, A. R. Koch, A. De Propris, R. Udalski, A. Szymanski, M. K. Soszynski, I. Pietrzynski, G. Ulaczyk, K. Wyrzykowski, L. Pietrukowicz, P. Skowron, J. Kozlowski, S. Mroz, P. TI A HIGH-VELOCITY BULGE RR LYRAE VARIABLE ON A HALO-LIKE ORBIT SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE Galaxy: bulge; Galaxy: formation; Galaxy: halo; Galaxy: kinematics and dynamics; stars: Population II; stars: variables: RR Lyrae ID RED CLUMP STARS; GALACTIC BULGE; LIGHT CURVES; BAADE WINDOW; OGLE-III; GALAXY; METALLICITY; EXTINCTION; MAGNITUDE; DISTANCE AB We report on the RR Lyrae variable star, MACHO 176.18833.411, located toward the Galactic bulge and observed within the data from the ongoing Bulge RR Lyrae Radial Velocity Assay, which has the unusual radial velocity of -372 +/- 8 km s(-1) and true space velocity of -482 +/- 22 km s(-1) relative to the Galactic rest frame. Located less than 1 kpc from the Galactic center and toward a field at (l, b) = (3, -2.5), this pulsating star has properties suggesting it belongs to the bulge RR Lyrae star population, yet a velocity indicating it is abnormal, at least with respect to bulge giants and red clump stars. We show that this star is most likely a halo interloper and therefore suggest that halo contamination is not insignificant when studying metal-poor stars found within the bulge area, even for stars within 1 kpc of the Galactic center. We discuss the possibility that MACHO 176.18833.411 is on the extreme edge of the bulge RR Lyrae radial velocity distribution, and also consider a more exotic scenario in which it is a runaway star moving through the Galaxy. C1 [Kunder, Andrea; Storm, J.] Leibniz Inst Astrophys Potsdam AIP, D-14482 Potsdam, Germany. [Rich, R. M.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. [Hawkins, K.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Poleski, R.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. [Poleski, R.; Udalski, A.; Szymanski, M. K.; Soszynski, I.; Pietrzynski, G.; Ulaczyk, K.; Wyrzykowski, L.; Pietrukowicz, P.; Skowron, J.; Kozlowski, S.; Mroz, P.] Univ Warsaw Observ, PL-00478 Warsaw, Poland. [Johnson, C. I.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Shen, J.; Li, Z. -Y.] Chinese Acad Sci, Shanghai Astron Observ, Key Lab Res Galaxies & Cosmol, Shanghai 200030, Peoples R China. [Cordero, M. J.] Zentrum Astron, Astron Rech Inst, D-69120 Heidelberg, Germany. [Nataf, D. M.] Australian Natl Univ, Res Sch Astron & Astrophys, Canberra, ACT 2611, Australia. [Bono, G.] Univ Roma Tor Vergata, Dipartimento Fis, I-00133 Rome, Italy. [Bono, G.] Rome Astron Observ, INAF, I-00040 Monte Porzio Catone, Italy. [Walker, A. R.] Natl Opt Astron Observ, Cerro Tololo Inter Amer Observ, La Serena, Chile. [Koch, A.] Heidelberg Univ, Zentrum Astron, Landessternwarte, D-69117 Heidelberg, Germany. [De Propris, R.] Univ Turku, Finnish Ctr Astron ESO FINCA, Turku, Finland. [Pietrzynski, G.] Univ Concepcion, Dept Astron, Concepcion, Chile. [Ulaczyk, K.] Univ Warwick, Dept Phys, Coventry CV4 7AL, W Midlands, England. RP Kunder, A (reprint author), Leibniz Inst Astrophys Potsdam AIP, An der Sternwarte 16, D-14482 Potsdam, Germany. RI Skowron, Jan/M-5186-2014; Kozlowski, Szymon/G-4799-2013; OI Skowron, Jan/0000-0002-2335-1730; Kozlowski, Szymon/0000-0003-4084-880X; Storm, Jesper/0000-0002-8627-6096; Hawkins, Keith /0000-0002-1423-2174; Kunder, Andrea/0000-0002-2808-1370; Koch, Andreas/0000-0002-9859-4956 FU National Science Foundation [NSF PHY11-25915, AST-1413755]; German Research Foundation (DFG) [Sonderforschungsbereich SFB 881]; Polish Ministry of Science and Higher Education through the program "Ideas Plus" [IdP2012 000162]; Clay Fellowship; 973 Program of China [2014CB845700]; National Natural Science Foundation of China [11333003, 11322326, 11403072]; Strategic Priority Research Program "The Emergence of Cosmological Structures" of the Chinese Academy of Sciences [XDB09000000]; Shanghai Sailing Program [14YF1407700] FX We thank the Australian Astronomical Observatory, which has made these observations possible. This research was supported in part by the National Science Foundation under grant No. NSF PHY11-25915. This work was supported by Sonderforschungsbereich SFB 881 "The Milky Way System" (subprojects A4, A5, A8) of the German Research Foundation (DFG). This work has been partially supported by the Polish Ministry of Science and Higher Education through the program "Ideas Plus" award No. IdP2012 000162 to I.S. R.M.R. acknowledges support from grant AST-1413755 from the National Science Foundation. C.I.J. gratefully acknowledges support from the Clay Fellowship, administered by the Smithsonian Astrophysical Observatory.; J.S. acknowledges support from the 973 Program of China under grant No. 2014CB845700, the National Natural Science Foundation of China under grant Nos. 11333003 and 11322326, and the Strategic Priority Research Program "The Emergence of Cosmological Structures" (No. XDB09000000) of the Chinese Academy of Sciences. Z.Y.L. acknowledges support from the National Natural Science Foundation of China under grant No. 11403072 and Shanghai Sailing Program (No. 14YF1407700). This work made use of the facilities of the Center for High performance Computing at Shanghai Astronomical Observatory. Hospitality at APCTP during the 7th Korean Astrophysics Workshop is kindly acknowledged. NR 41 TC 10 Z9 10 U1 2 U2 4 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 JUL 20 PY 2015 VL 808 IS 1 AR L12 DI 10.1088/2041-8205/808/1/L12 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CN9OO UT WOS:000358778900012 ER PT J AU Mroczkowski, T Kovacs, A Bulbul, E Staguhn, J Benford, DJ Clarke, TE van Weeren, RJ Intema, HT Randall, S AF Mroczkowski, T. Kovacs, A. Bulbul, E. Staguhn, J. Benford, D. J. Clarke, T. E. van Weeren, R. J. Intema, H. T. Randall, S. TI RESOLVING THE MERGING PLANCK CLUSTER PLCK G147.3-16.6 WITH GISMO SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE cosmology: observations; galaxies: clusters: general; galaxies: clusters: individual (PLCK G147.3-16.6); galaxies: clusters: intracluster medium; X-rays: galaxies: clusters ID SPT-SZ SURVEY; GALAXY CLUSTERS; RADIO HALO; ZELDOVICH; GHZ; TELESCOPE; EMISSION AB The Planck satellite has recently completed an all-sky galaxy cluster survey exploiting the thermal Sunyaev-Zel'dovich (SZ) effect to locate some of the most massive systems observable. With a median redshift of < z > = 0.22, the clusters found by Planck at z > 0.3 are proving to be exceptionally massive and/or disturbed systems. One notable Planck discovery at z = 0.645, PLCK G147.3-16.6, has an elongated core and hosts a radio halo, indicating it is likely in the process of merging. We present a 16 ''.5 resolution SZ observation of this high-z merger using the Goddard-IRAM Superconducting 2-Millimeter Observer, and compare it to X-ray follow-up observations with XMM-Newton. We find the SZ pressure substructure is offset from the core components seen in X-ray. We interpret this as possible line of sight temperature or density substructure due to the on-going merger. C1 [Mroczkowski, T.; Clarke, T. E.] US Navy, Res Lab, Washington, DC 20375 USA. [Kovacs, A.] CALTECH, Pasadena, CA 91125 USA. [Kovacs, A.] Univ Minnesota, Inst Astrophys, Minneapolis, MN 55455 USA. [Bulbul, E.; van Weeren, R. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Staguhn, J.; Benford, D. J.] NASA, Goddard Space Flight Ctr, Observat Cosmol Lab, Code 665, Greenbelt, MD 20771 USA. [Staguhn, J.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Intema, H. T.] Natl Radio Astron Observ, Socorro, NM 87801 USA. [Mroczkowski, T.] Natl Acad Sci, Natl Res Council, London, England. RP Mroczkowski, T (reprint author), US Navy, Res Lab, 4555 Overlook Ave SW, Washington, DC 20375 USA. EM anthony.mroczkowski.ctr@nrl.navy.mil RI Kovacs, Attila/C-1171-2010; Intema, Huib/D-1438-2012; Benford, Dominic/D-4760-2012; OI Kovacs, Attila/0000-0001-8991-9088; Intema, Huib/0000-0002-5880-2730; Benford, Dominic/0000-0002-9884-4206; Mroczkowski, Tony/0000-0003-3816-5372; van Weeren, Reinout/0000-0002-0587-1660 FU 6.1 Base funding; NASA ADP grant [NNX13AE83G]; NASA through the Einstein Postdoctoral grant by the Chandra X-ray Center [PF2-130104]; NASA [NAS8-03060]; National Radio Astronomy Observatory, a facility of the National Science Foundation (NSF); NSF [1020981, 1106284]; INSU/CNRS (France); MPG (Germany); IGN (Spain) FX This research was performed while TM held a National Research Council Research Associateship Award at the Naval Research Laboratory (NRL). Basic research in radio astronomy at NRL by TM and TEC is supported by 6.1 Base funding. EB is supported in part by NASA ADP grant NNX13AE83G. RJvW is supported 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. HTI is supported by the National Radio Astronomy Observatory, a facility of the National Science Foundation (NSF) operated under cooperative agreement by Associated Universities, Inc. The GISMO instrument and team are supported through NSF ATI grants 1020981 and 1106284. IRAM is supported by INSU/CNRS (France), MPG (Germany), and IGN (Spain). NR 31 TC 1 Z9 1 U1 0 U2 1 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 JUL 20 PY 2015 VL 808 IS 1 AR L6 DI 10.1088/2041-8205/808/1/L6 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CN9OO UT WOS:000358778900006 ER PT J AU Sandoval, MA Vo, RP Romanowsky, AJ Strader, J Choi, J Jennings, ZG Conroy, C Brodie, JP Foster, C Villaume, A Norris, MA Janz, J Forbes, DA AF Sandoval, Michael A. Vo, Richard P. Romanowsky, Aaron J. Strader, Jay Choi, Jieun Jennings, Zachary G. Conroy, Charlie Brodie, Jean P. Foster, Caroline Villaume, Alexa Norris, Mark A. Janz, Joachim Forbes, Duncan A. TI HIDING IN PLAIN SIGHT: RECORD-BREAKING COMPACT STELLAR SYSTEMS IN THE SLOAN DIGITAL SKY SURVEY SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE galaxies: fundamental parameters; galaxies: nuclei; galaxies: star clusters: general ID EARLY-TYPE GALAXIES; VIRGO CLUSTER SURVEY; SUSTAINED INATTENTIONAL BLINDNESS; ULTRACOMPACT DWARF GALAXIES; DATA REDUCTION PROCEDURES; MASSIVE STAR-CLUSTERS; GLOBULAR-CLUSTERS; ABUNDANCE RATIOS; AIMSS PROJECT; DATA RELEASE AB Motivated by the recent, serendipitous discovery of the densest known galaxy, M60-UCD1, we present two initial findings from a follow-up search, using the Sloan Digital Sky Survey, Subaru/Suprime-Cam, and Hubble Space Telescope imaging, and SOuthern Astrophysical Research (SOAR)/Goodman spectroscopy. The first object discovered, M59-UCD3, has a similar size to M60-UCD1 (half-light radius of r(h) similar to 20 pc) but is 40% more luminous (M-V similar to 14.6), making it the new densest-known galaxy. The second, M85-HCC1, has a size like a typical globular cluster (GC; r(h) similar to 1.8pc) but is much more luminous (M-V similar to -12.5). This hypercompact cluster is by far the densest confirmed free-floating stellar system, and is equivalent to the densest known nuclear star clusters. From spectroscopy, we find that both objects are relatively young (similar to 9 and similar to 3 Gyr, respectively), with metal-abundances that resemble those of galaxy centers. Their host galaxies show clear signs of large-scale disturbances, and we conclude that these dense objects are the remnant nuclei of recently accreted galaxies. M59-UCD3 is an ideal target for follow-up with high-resolution imaging and spectroscopy to search for an overweight central supermassive black hole as was discovered in M60-UCD1. These findings also emphasize the potential value of ultra-compact dwarfs and massive GCs as tracers of the assembly histories of galaxies. C1 [Sandoval, Michael A.; Vo, Richard P.; Romanowsky, Aaron J.] San Jose State Univ, Dept Phys & Astron, San Jose, CA 95192 USA. [Vo, Richard P.] San Francisco State Univ, Dept Phys & Astron, San Francisco, CA 94131 USA. [Romanowsky, Aaron J.; Brodie, Jean P.] Univ Calif Observ, Santa Cruz, CA 95064 USA. [Strader, Jay] Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA. [Choi, Jieun; Conroy, Charlie] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Choi, Jieun; Jennings, Zachary G.; Villaume, Alexa] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. [Foster, Caroline] Australian Astron Observ, N Ryde, NSW 1670, Australia. [Norris, Mark A.] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Janz, Joachim; Forbes, Duncan A.] Swinburne Univ Technol, Ctr Astrophys & Supercomp, Hawthorn, Vic 3122, Australia. RP Sandoval, MA (reprint author), San Jose State Univ, Dept Phys & Astron, One Washington Sq, San Jose, CA 95192 USA. OI Sandoval, Michael/0000-0002-5088-4487; Villaume, Alexa/0000-0003-1887-0621; Foster, Caroline/0000-0003-0247-1204 FU National Science Foundation (NSF) [AST-1109878]; SJSU Undergraduate Research Grants; ARC [DP130100388]; Alfred P. Sloan Foundation; NSF; U. S. Department of Energy; National Aeronautics and Space Administration; Japanese Monbu-kagakusho; Max Planck Society; Higher Education Funding Council for England; Participating Institutions FX We thank the SJSU ASTR-117B class for their endurance through UCD fever, Katy Murphy for helpful discussions, Cindy Tsui for artistic assistance, and the referee for a quick and helpful report. We are immensely grateful for the efforts of SDSS, SDSS-III, and the Hubble Legacy Archive in making their data easily accessible to anyone in the world with an internet connection. This work was supported by National Science Foundation (NSF) grant AST-1109878, by SJSU Undergraduate Research Grants, and by the ARC (DP130100388). It used data from the Subaru telescope (National Astronomical Observatory of Japan) and the Southern Astrophysical Research (SOAR) telescope (joint project of Brasil, NOAO, UNC, MSU). SDSS/SDSS-III was funded by the Alfred P. Sloan Foundation, the Participating Institutions, the NSF, the U. S. Department of Energy, the National Aeronautics and Space Administration, the Japanese Monbu-kagakusho, the Max Planck Society, and the Higher Education Funding Council for England. NR 49 TC 4 Z9 4 U1 1 U2 3 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 JUL 20 PY 2015 VL 808 IS 1 AR L32 DI 10.1088/2041-8205/808/1/L32 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CN9OO UT WOS:000358778900032 ER PT J AU Bohu, T Santelli, CM Akob, DM Neu, TR Ciobota, V Rosch, P Popp, J Nietzsche, S Kusel, K AF Bohu, Tsing Santelli, Cara M. Akob, Denise M. Neu, Thomas R. Ciobota, Valerian Roesch, Petra Popp, Juergen Nietzsche, Sandor Kuesel, Kirsten TI Characterization of pH dependent Mn(II) oxidation strategies and formation of a bixbyite-like phase by Mesorhizobium australicum T-G1 SO FRONTIERS IN MICROBIOLOGY LA English DT Article DE catalase; low pH; Mn(II) oxidation; multi-copper oxidase; reactive oxygen species ID SP STRAIN SG-1; COAL-MINE DRAINAGE; ENZYMATIC MANGANESE(II) OXIDATION; PUTATIVE MULTICOPPER OXIDASE; MARINE BACILLUS; MN(II)-OXIDIZING BACTERIA; LEPTOTHRIX-DISCOPHORA; MICROBIAL COMMUNITIES; TREATMENT SYSTEMS; ESCHERICHIA-COLI AB Despite the ubiquity of Mn oxides in natural environments, there are only a few observations of biological Mn(II) oxidation at pH <6. The lack of low pH Mn-oxidizing bacteria (MOB) isolates limits our understanding of how pH influences biological Mn(II) oxidation in extreme environments. Here, we report that a novel MOB isolate, Mesorhizobium australicum strain T-G1, isolated from an acidic and metalliferous uranium mining area, can oxidize Mn(II) at both acidic and neutral pH using different enzymatic pathways. X-ray diffraction, Raman spectroscopy, and scanning electron microscopy with energy dispersive X-ray spectroscopy revealed that T-G1 initiated bixbyite-like Mn oxide formation at pH 5.5 which coincided with multi-copper oxidase expression from early exponential phase to late stationary phase. In contrast, reactive oxygen species (ROS), particularly superoxide, appeared to be more important for T-G1 mediated Mn(II) oxidation at neutral pH. ROS was produced in parallel with the occurrence of Mn(II) oxidation at pH 7.2 from early stationary phase. Solid phase Mn oxides did not precipitate, which is consistent with the presence of a high amount of H2O2 and lower activity of catalase in the liquid culture at pH 7.2. Our results show that M. australicum T-G1, an acid tolerant MOB, can initiate Mn(II) oxidation by varying its oxidation mechanisms depending on the pH and may play an important role in low pH manganese biogeochemical cycling. C1 [Bohu, Tsing; Kuesel, Kirsten] Univ Jena, Dept Aquat Geomicrobiol, D-07743 Jena, Germany. [Santelli, Cara M.] Smithsonian Inst, Dept Mineral Sci, Washington, DC 20560 USA. [Akob, Denise M.] US Geol Survey, Natl Res Program, Reston, VA 22092 USA. [Neu, Thomas R.] UFZ Helmholtz Ctr Environm Res, Dept River Ecol, Magdeburg, Germany. [Ciobota, Valerian; Roesch, Petra; Popp, Juergen] Univ Jena, Inst Phys Chem, D-07743 Jena, Germany. [Ciobota, Valerian; Roesch, Petra; Popp, Juergen] Univ Jena, Abbe Sch Phonton, D-07743 Jena, Germany. [Popp, Juergen] Leibniz Inst Phonton Technol, Jena, Germany. [Nietzsche, Sandor] Univ Jena, Univ Hosp Jena, Ctr Electron Microscopy, D-07743 Jena, Germany. [Kuesel, Kirsten] German Ctr Integrat Biodivers Res iDiv, Leipzig, Germany. RP Kusel, K (reprint author), Univ Jena, Dept Aquat Geomicrobiol, Dornburger Str 159, D-07743 Jena, Germany. EM kirsten.kuesel@uni-jena.de RI iDiv, Deutsches Zentrum/B-5164-2016; OI Akob, Denise/0000-0003-1534-3025; Santelli, Cara/0000-0001-8617-0008 FU German Science Foundation (DFG) [GRK 1257] FX The authors thank Dr. Juanjuan Wang and Dr. Shipeng Lu (Aquatic Geomicrobiology, FSU Jena) for help with sampling. The Laboratories of Analytical Biology of the Smithsonian Institution, USA provided free access to and assistance with Synergy HT Multi-Mode Microplate Reader. We also thank the German Science Foundation (DFG GRK 1257) for funding. Any use of trade, product, or firm names is for descriptive purposes only and does not imply endorsement by the U.S. Government. The authors declare no competing financial interest. NR 89 TC 4 Z9 4 U1 5 U2 28 PU FRONTIERS MEDIA SA PI LAUSANNE PA PO BOX 110, EPFL INNOVATION PARK, BUILDING I, LAUSANNE, 1015, SWITZERLAND SN 1664-302X J9 FRONT MICROBIOL JI Front. Microbiol. PD JUL 17 PY 2015 VL 6 AR 734 DI 10.3389/fmicb.2015.00734 PG 15 WC Microbiology SC Microbiology GA CN7ZJ UT WOS:000358654900001 PM 26236307 ER PT J AU Nguyen, TL McCarthy, MC Stanton, JF AF Thanh Lam Nguyen McCarthy, Michael C. Stanton, John F. TI Relatively Selective Production of the Simplest Criegee Intermediate in a CH4/O-2 Electric Discharge: Kinetic Analysis of a Plausible Mechanism SO JOURNAL OF PHYSICAL CHEMISTRY A LA English DT Article ID ACTIVE THERMOCHEMICAL TABLES; ATOMIC NATURAL ORBITALS; TRANSITION-STATE THEORY; REACTION-RATE CONSTANTS; GAUSSIAN-BASIS SETS; GAS-PHASE; AB-INITIO; GENERAL CONTRACTION; O-2; CH2OO AB High -accuracy coupled cluster methods in combination with microcanonical semiclassical transition state theory are used to investigate a plausible formation mechanism of the simplest Criegee intermediate in a CH4/O-2 discharge experiment. Our results suggest that the Criegee intermediate is produced in a three-step process: (i) production of methyl radical by cleavage of a C-H bond of CH4; (ii) association of methyl radical with molecular oxygen to form a vibrationally excited methyl peroxy, which is in a rapid microequilibrium with the reactants; and finally, (iii) H-abstraction of CH3OO by O-2, which results in the formation of cool CH2OO, which has insufficient internal energy to rearrange to dioxirane. C1 [Thanh Lam Nguyen; Stanton, John F.] Univ Texas Austin, Dept Chem, Austin, TX 78712 USA. [McCarthy, Michael C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Stanton, JF (reprint author), Univ Texas Austin, Dept Chem, Mail Stop A5300, Austin, TX 78712 USA. EM jfstanton@mail.utexas.edu FU Robert A. Welch Foundation [F-1283]; U.S. Department of Energy, Office of Basic Energy Sciences [DE-FG02-07ER15884]; NSF [CHE-1058063] FX J.F.S. and T.L.N. are supported by the Robert A. Welch Foundation (Grant F-1283). This material is based on the work supported by the U.S. Department of Energy, Office of Basic Energy Sciences under Award Number DE-FG02-07ER15884. M.C.M. is supported by NSF Grant No. CHE-1058063. NR 51 TC 3 Z9 3 U1 9 U2 23 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 JUL 16 PY 2015 VL 119 IS 28 BP 7197 EP 7204 DI 10.1021/jp510554g PG 8 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA CN3PA UT WOS:000358337600014 PM 25405528 ER PT J AU Liu, H Xu, QY He, PC Santiago, LS Yang, KM Ye, Q AF Liu, Hui Xu, Qiuyuan He, Pengcheng Santiago, Louis S. Yang, Keming Ye, Qing TI Strong phylogenetic signals and phylogenetic niche conservatism in ecophysiological traits across divergent lineages of Magnoliaceae SO SCIENTIFIC REPORTS LA English DT Article ID HYDRAULIC ARCHITECTURE; WATER RELATIONS; FUNCTIONAL CONVERGENCE; CORRELATED EVOLUTION; CANOPY TREES; LEAF; ECOLOGY; PLANT; EFFICIENCY; BIOLOGY AB The early diverged Magnoliaceae shows a historical temperate-tropical distribution among lineages indicating divergent evolution, yet which ecophysiological traits are phylogenetically conserved, and whether these traits are involved in correlated evolution remain unclear. Integrating phylogeny and 20 ecophysiological traits of 27 species, from the four largest sections of Magnoliaceae, we tested the phylogenetic signals of these traits and the correlated evolution between trait pairs. Phylogenetic niche conservatism (PNC) in water-conducting and nutrient-use related traits was identified, and correlated evolution of several key functional traits was demonstrated. Among the three evergreen sections of tropical origin, Gwillimia had the lowest hydraulic-photosynthetic capacity and the highest drought tolerance compared with Manglietia and Michelia. Contrastingly, the temperate centred deciduous section, Yulania, showed high rates of hydraulic conductivity and photosynthesis at the cost of drought tolerance. This study elucidated the regulation of hydraulic and photosynthetic processes in the temperate-tropical adaptations for Magnoliaceae species, which led to strong phylogenetic signals and PNC in ecophysiological traits across divergent lineages of Magnoliaceae. C1 [Liu, Hui; Xu, Qiuyuan; He, Pengcheng; Ye, Qing] Chinese Acad Sci, South China Bot Garden, Key Lab Vegetat Restorat & Management Degraded Ec, Guangzhou 510650, Guangdong, Peoples R China. [Xu, Qiuyuan; He, Pengcheng] Univ Chinese Acad Sci, Beijing 100049, Peoples R China. [Santiago, Louis S.] Univ Calif Riverside, Bot & Plant Sci, Riverside, CA 92521 USA. [Santiago, Louis S.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. [Yang, Keming] Chinese Acad Sci, Hort Ctr, South China Bot Garden, Guangzhou 510520, Guangdong, Peoples R China. RP Xu, QY (reprint author), Chinese Acad Sci, South China Bot Garden, Key Lab Vegetat Restorat & Management Degraded Ec, Xingke Rd 723, Guangzhou 510650, Guangdong, Peoples R China. EM qye@scbg.ac.cn RI Santiago, Louis/E-3185-2016 OI Santiago, Louis/0000-0001-5994-6122 FU National Natural Science Foundation of China [31300334]; Natural Science Foundation of Guangdong Province [S2013040015044]; Chinese Academy of Sciences through its Hundred Talent Program and Knowledge Innovation Project [KSCX2-EW-J-28]; Scientific Research Foundation for the Returned Overseas Chinese Scholars, State Education Ministry of China FX We thank Ronghua Li and Shidan Zhu for their assistance in lab work and discussion. This work was funded by the National Natural Science Foundation of China (31300334), the Natural Science Foundation of Guangdong Province (S2013040015044) and the Chinese Academy of Sciences through its Hundred Talent Program and Knowledge Innovation Project (KSCX2-EW-J-28), and the Scientific Research Foundation for the Returned Overseas Chinese Scholars, State Education Ministry of China. NR 62 TC 5 Z9 5 U1 5 U2 46 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 JUL 16 PY 2015 VL 5 AR 12246 DI 10.1038/srep12246 PG 12 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA CM9GH UT WOS:000358014900001 PM 26179320 ER PT J AU Cramer, KL Leonard-Pingel, JS Rodriguez, F Jackson, JBC AF Cramer, Katie L. Leonard-Pingel, Jill S. Rodriguez, Felix Jackson, Jeremy B. C. TI Molluscan subfossil assemblages reveal the long-term deterioration of coral reef environments in Caribbean Panama SO MARINE POLLUTION BULLETIN LA English DT Article DE Barbatia cancellaria; Bocas del Toro; Dendostrea frons; Historical ecology; Water quality ID BOCAS-DEL-TORO; CENTRAL-AMERICA; THALASSIA COMMUNITIES; SPECIES RICHNESS; HUMAN IMPACTS; WEST-INDIES; ECOLOGY; GASTROPODS; CONVERGENCE; RADIOCARBON AB Caribbean reef corals have declined sharply since the 1980s, but the lack of prior baseline data has hindered identification of drivers of change. To assess anthropogenic change in reef environments over the past century, we tracked the composition of subfossil assemblages of bivalve and gastropod mollusks excavated from pits below lagoonal and offshore reefs in Bocas del Toro, Panama. The higher prevalence of (a) infaunal suspension-feeding bivalves and herbivorous and omnivorous gastropods in lagoons and (b) epifaunal and suspension-feeding bivalves and carnivorous and suspension-feeding gastropods offshore reflected the greater influence of land-based nutrients/sediments within lagoons. Temporal changes indicated deteriorating environmental conditions pre-1960 in lagoons and post-1960 offshore, with offshore communities becoming more similar to lagoonal ones since 1960. Relative abundances of dominant bivalve species tracked those of their coral hosts, revealing broader ecosystem effects of coral community change. The nature and timing of changes implicate land-based runoff in reef deterioration. (C) 2015 Elsevier Ltd. All rights reserved. C1 [Cramer, Katie L.; Rodriguez, Felix; Jackson, Jeremy B. C.] Smithsonian Trop Res Inst, Balboa, Panama. [Cramer, Katie L.; Jackson, Jeremy B. C.] Univ Calif San Diego, Scripps Inst Oceanog, La Jolla, CA 92093 USA. [Leonard-Pingel, Jill S.] Washington & Lee Univ, Lexington, VA 24450 USA. [Jackson, Jeremy B. C.] Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20013 USA. RP Cramer, KL (reprint author), Univ Calif San Diego, Scripps Inst Oceanog, 9500 Gilman Dr, La Jolla, CA 92093 USA. EM kcramer@ucsd.edu; j.leonardpingel@gmail.com; rodriguezf@si.edu; jeremybcjackson@gmail.com FU Smithsonian Institution; NSF Integrative Graduate Education and Research Traineeship; Center for Marine Biodiversity and Conservation at Scripps Institution of Oceanography; University of California Academic Senate; PADI Foundation's Project AWARE FX We thank C. Angioletti, E. Ochoa, G. Jacome, P. Gondola, J. Morales, and C. Degracia for help in the laboratory and field in Panama, T. Guilderson for conducting radiocarbon analyses and assisting with calibrations to calendar ages, H. Guzman for his help with interpretation of study results, and Minerals Resources Department and National Authority for the Environment of Panama and C. De Leon for providing collection permits. Study supported by Smithsonian Institution, NSF Integrative Graduate Education and Research Traineeship, Center for Marine Biodiversity and Conservation at Scripps Institution of Oceanography, University of California Academic Senate, and PADI Foundation's Project AWARE. NR 68 TC 3 Z9 3 U1 2 U2 12 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0025-326X EI 1879-3363 J9 MAR POLLUT BULL JI Mar. Pollut. Bull. PD JUL 15 PY 2015 VL 96 IS 1-2 BP 176 EP 187 DI 10.1016/j.marpolbul.2015.05.031 PG 12 WC Environmental Sciences; Marine & Freshwater Biology SC Environmental Sciences & Ecology; Marine & Freshwater Biology GA CM0DP UT WOS:000357348900031 PM 26031382 ER PT J AU Najita, JR Andrews, SM Muzerolle, J AF Najita, Joan R. Andrews, Sean M. Muzerolle, James TI Demographics of transition discs in Ophiuchus and Taurus SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE planets and satellites: formation; protoplanetary discs; circumstellar matter; stars: formation; stars: pre-main-sequence ID YOUNG STELLAR OBJECTS; MAIN-SEQUENCE STARS; SPECTRAL ENERGY-DISTRIBUTIONS; SUBMILLIMETER CONTINUUM FLUX; CIRCUMSTELLAR DUST DISKS; MASS ACCRETION RATES; RHO-OPHIUCHI; MOLECULAR CLOUD; PROTOPLANETARY DISKS; X-RAY AB Transition disc systems are young stars that appear to be on the verge of dispersing their protoplanetary discs. We explore the nature of these systems by comparing the stellar accretion rates (M) over dot(*) and disc masses M-d of transition discs and normal T Tauri stars in Taurus and Ophiuchus. After controlling for the known dependences of (M) over dot(*) and M-d on age, (M) over dot(*) on stellar mass and M-d on the presence of stellar or substellar companions, we find that the normal T Tauri stars show a trend of (M) over dot(*) increasing with M-d. The transition discs tend to have higher average disc masses than normal T Tauri stars as well as lower accretion rates than normal T Tauri stars of the same disc mass. These results are most consistent with the interpretation that the transition discs have formed objects massive enough to alter the accretion flow, i.e. single or multiple giant planets. Several Ophiuchus T Tauri stars that are not known transition disc systems also have very low accretion rates for their disc masses. We speculate on the possible nature of these sources. C1 [Najita, Joan R.] Natl Opt Astron Observ, 950 Cherry Ave, Tucson, AZ 85719 USA. [Najita, Joan R.; Andrews, Sean M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Muzerolle, James] Space Telescope Sci Inst, Baltimore, MD 21218 USA. RP Najita, JR (reprint author), Natl Opt Astron Observ, 950 Cherry Ave, Tucson, AZ 85719 USA. EM najita@noao.edu; sandrews@cfa.harvard.edu; muzerol@stsci.edu NR 108 TC 14 Z9 14 U1 0 U2 0 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD JUL 11 PY 2015 VL 450 IS 4 BP 3559 EP 3567 DI 10.1093/mnras/stv839 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CQ7YY UT WOS:000360824000014 ER PT J AU Glennie, A Jonker, PG Fender, RP Nagayama, T Pretorius, ML AF Glennie, A. Jonker, P. G. Fender, R. P. Nagayama, T. Pretorius, M. L. TI Two fast X-ray transients in archival Chandra data SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE stars: flare; stars: late-type; infrared: stars; X-rays: bursts ID POINT-SOURCE CATALOG; MASSIVE BLACK-HOLES; ALL-SKY SURVEY; TIDAL DISRUPTION; WHITE-DWARFS; GALAXY; FLARE; EMISSION; ROTATION; SAMPLE AB We present the discovery of two new X-ray transients in archival Chandra data. The first transient, XRT 110103, occurred in 2011 January and shows a sharp rise of at least three orders of magnitude in count rate in less than 10 s, a flat peak for about 20 s and decays by two orders of magnitude in the next 60 s. We find no optical or infrared counterpart to this event in pre-existing survey data or in an observation taken by the Simultaneous-3color InfraRed Imager for Unbiased Survey (SIRIUS) instrument at the Infrared Survey Facility similar to 2.1 yr after the transient, providing limiting magnitudes of J > 18.1, H > 17.6 and K-s > 16.3. This event shows similarities to the transient previously reported in Jonker et al. which was interpreted as the possible tidal disruption of a white dwarf by an intermediate-mass black hole. We discuss the possibility that these transients originate from the same type of event. If we assume these events are related a rough estimate of the rates gives 1.4 x 10(5) per year over the whole sky with a peak 0.3-7 keV X-ray flux greater than 2 x 10(-10) erg cm(-2) s(-1). The second transient, XRT 120830, occurred in 2012 August and shows a rise of at least three orders of magnitude in count rate and a subsequent decay of around one order of magnitude all within 10 s, followed by a slower quasi-exponential decay over the remaining 30 ks of the observation. We detect a likely infrared counterpart with magnitudes J = 16.70 +/- 0.06, H = 15.92 +/- 0.04 and K-s = 15.37 +/- 0.06 which shows an average proper motion of 74 +/- 19 mas yr(-1) compared to archival 2MASS observations. The JHK(s) magnitudes, proper motion and X-ray flux of XRT 120830 are consistent with a bright flare from a nearby late M or early L dwarf. C1 [Glennie, A.; Fender, R. P.; Pretorius, M. L.] Univ Oxford, Dept Phys, Oxford OX1 3RH, England. [Jonker, P. G.] SRON, Netherlands Inst Space Res, NL-3584 CA Utrecht, Netherlands. [Jonker, P. G.] Radboud Univ Nijmegen, Dept Astrophys IMAPP, NL-6500 GL Nijmegen, Netherlands. [Jonker, P. G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Nagayama, T.] Nagoya Univ, Dept Astrophys, Chikusa Ku, Nagoya, Aichi 4648602, Japan. [Nagayama, T.] Kagoshima Univ, Dept Sci & Engn, Korimoto, Kagoshima, Japan. RP Glennie, A (reprint author), Univ Oxford, Dept Phys, Oxford OX1 3RH, England. EM aidan.glennie@astro.ox.ac.uk FU European Research Council [267697]; National Aeronautics and Space Administration; National Science Foundation FX This project was funded in part by European Research Council Advanced Grant 267697 '4 pi sky: Extreme Astrophysics with Revolutionary Radio Telescopes.'; This publication makes use of data products from the 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. NR 33 TC 1 Z9 1 U1 0 U2 0 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD JUL 11 PY 2015 VL 450 IS 4 BP 3765 EP 3770 DI 10.1093/mnras/stv801 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CQ7YY UT WOS:000360824000028 ER PT J AU D'Ammando, F Orienti, M Tavecchio, F Ghisellini, G Torresi, E Giroletti, M Raiteri, CM Grandi, P Aller, M Aller, H Gurwell, MA Malaguti, G Pian, E Tosti, G AF D'Ammando, F. Orienti, M. Tavecchio, F. Ghisellini, G. Torresi, E. Giroletti, M. Raiteri, C. M. Grandi, P. Aller, M. Aller, H. Gurwell, M. A. Malaguti, G. Pian, E. Tosti, G. TI Unveiling the nature of the gamma-ray emitting active galactic nucleus PKS 0521-36 SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies: active; galaxies: individual: PKS0521-36; galaxies: nuclei; quasars: general; gamma-rays: galaxies; gamma-rays: general ID LARGE-AREA TELESCOPE; BL LACERTAE OBJECTS; SOURCE CATALOG; COMPLETE SAMPLE; RADIO GALAXIES; EGRET CATALOG; LAC OBJECTS; SKY SURVEY; FERMI-LAT; NGC 1275 AB PKS 0521-36 is an active galactic nucleus (AGN) with uncertain classification. We investigate the properties of this source from radio to gamma-rays. The broad emission lines in the optical and ultraviolet bands and steep radio spectrum indicate a possible classification as an intermediate object between broad-line radio galaxies (BLRG) and steep spectrum radio quasars (SSRQ). On pc-scales PKS 0521-36 shows a knotty structure similar to misaligned AGN. The core dominance and the gamma-ray properties are similar to those estimated for other SSRQ and BLRG detected in gamma-rays, suggesting an intermediate viewing angle with respect to the observer. In this context the flaring activity detected from this source by Fermi-Large Area Telescope between 2010 June and 2012 February is very intriguing. We discuss the gamma-ray emission of this source in the framework of the structured jet scenario, comparing the spectral energy distribution (SED) of the flaring state in 2010 June with that of a low state. We present three alternative models corresponding to three different choices of the viewing angles theta(v) = 6 degrees, 15 degrees, and 20 degrees. We obtain a good fit for the first two cases, but the SED obtained with theta(v) = 15 degrees if observed at a small angle does not resemble that of a typical blazar since the synchrotron emission should dominate by a large factor (similar to 100) the inverse Compton component. This suggests that a viewing angle between 6 degrees and 15 degrees is preferred, with the rapid variability observed during gamma-ray flares favouring a smaller angle. However, we cannot rule out that PKS 0521-36 is the misaligned counterpart of a synchrotron-dominated blazar. C1 [D'Ammando, F.] Univ Bologna, Dipartimento Fis Astron, I-40127 Bologna, Italy. [D'Ammando, F.; Orienti, M.; Giroletti, M.] INAF, Ist Radioastron, I-40129 Bologna, Italy. [Tavecchio, F.; Ghisellini, G.] INAF, Osservatorio Astron Brera, I-23807 Merate, Italy. [Torresi, E.; Grandi, P.; Malaguti, G.] INAF, Ist Astrofis Spaziale Fis Cosm, I-40129 Bologna, Italy. [Raiteri, C. M.] INAF, Osservatorio Astron Torino, I-10025 Pino Torinese, TO, Italy. [Aller, M.; Aller, H.] Univ Michigan, Ann Arbor, MI 48109 USA. [Gurwell, M. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Pian, E.] Scuola Normale Super Pisa, I-56126 Pisa, Italy. [Tosti, G.] Univ Perugia, Dipartimento Fis, I-06123 Perugia, Italy. [Tosti, G.] INFN Sezione Perugia, I-06123 Perugia, Italy. RP D'Ammando, F (reprint author), Univ Bologna, Dipartimento Fis Astron, Via Ranzani 1, I-40127 Bologna, Italy. EM dammando@ira.inaf.it OI Grandi, Paola/0000-0003-1848-6013; Malaguti, Giuseppe/0000-0001-9872-3378; Ghisellini, Gabriele/0000-0002-0037-1974 FU Smithsonian Institution; Academia Sinica; University of Michigan; National Science Foundation [AST-0607523]; NASA [NNX09AU16G, NNX10AP16G, NNX11AO13G, NNX13AP18G] FX We thank the Swift team for making these observations possible, the duty scientists, and science planners. The Submillimeter Array is a joint project between the Smithsonian Astrophysical Observatory and the Academia Sinica Institute of Astronomy and Astrophysics and is funded by the Smithsonian Institution and the Academia Sinica. This research has made use of data from the University of Michigan Radio Astronomy Observatory which has been supported by the University of Michigan and by a series of grants from the National Science Foundation, most recently AST-0607523. This research was supported in part by NASA Fermi Guest Investigator awards NNX09AU16G, NNX10AP16G, NNX11AO13G, and NNX13AP18G. Part of this work is based on archival data, software, or online service provided by ASI Science Data Center (ASDC). The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. We thank S. Digel, D. J. Thompson, J. Perkins, D. Gasparrini, and the anonymous referee for useful comments and suggestions. NR 82 TC 2 Z9 2 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 JUL 11 PY 2015 VL 450 IS 4 BP 3975 EP 3990 DI 10.1093/mnras/stv909 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CQ7YY UT WOS:000360824000046 ER PT J AU Zhuravleva, I Churazov, E Arevalo, P Schekochihin, AA Allen, SW Fabian, AC Forman, WR Sanders, JS Simionescu, A Sunyaev, R Vikhlinin, A Werner, N AF Zhuravleva, I. Churazov, E. Arevalo, P. Schekochihin, A. A. Allen, S. W. Fabian, A. C. Forman, W. R. Sanders, J. S. Simionescu, A. Sunyaev, R. Vikhlinin, A. Werner, N. TI Gas density fluctuations in the Perseus Cluster: clumping factor and velocity power spectrum SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE turbulence; methods: observational; methods: statistical; techniques: image processing; galaxies: clusters: intracluster medium; X-rays: galaxies: clusters ID DEEP CHANDRA OBSERVATION; RELAXED GALAXY CLUSTERS; XMM-NEWTON OBSERVATIONS; JET-INFLATED BUBBLES; X-RAY SPECTROSCOPY; INTRACLUSTER MEDIUM; ELLIPTIC GALAXIES; COSMOLOGICAL SIMULATIONS; COOLING FLOWS; NGC 1275 AB X-ray surface brightness fluctuations in the core of the Perseus Cluster are analysed, using deep observations with the Chandra observatory. The amplitude of gas density fluctuations on different scales is measured in a set of radial annuli. It varies from 7 to 12 per cent on scales of similar to 10-30 kpc within radii of 30-220 kpc from the cluster centre. Using a statistical linear relation between the observed amplitude of density fluctuations and predicted velocity, the characteristic velocity of gas motions on each scale is calculated. The typical amplitudes of the velocity outside the central 30 kpc region are 90-140 km s(-1) on similar to 20-30 kpc scales and 70-100 km s(-1) on smaller scales similar to 7-10 kpc. The velocity power spectrum ( PS) is consistent with cascade of turbulence and its slope is in a broad agreement with the slope for canonical Kolmogorov turbulence. The gas clumping factor estimated from the PS of the density fluctuations is lower than 7-8 per cent for radii similar to 30-220 kpc from the centre, leading to a density bias of less than 3-4 per cent in the cluster core. Uncertainties of the analysis are examined and discussed. Future measurements of the gas velocities with the Astro-H, Athena and Smart-X observatories will directly measure the gas density-velocity perturbation relation and further reduce systematic uncertainties in this analysis. C1 [Zhuravleva, I.; Allen, S. W.; Werner, N.] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94305 USA. [Zhuravleva, I.; Allen, S. W.; Werner, N.] Stanford Univ, Dept Phys, Stanford, CA 94305 USA. Max Planck Inst Astrophys, D-85741 Garching, Germany. [Churazov, E.] Space Res Inst IKI, Moscow 117997, Russia. [Arevalo, P.] Univ Valparaiso, Fac Ciencias, Inst Fis & Astron, Valparaiso, Chile. [Schekochihin, A. A.] Univ Oxford, Rudolf Peierls Ctr Theoret Phys, Oxford OX1 3NP, England. [Schekochihin, A. A.] Univ Oxford Merton Coll, Oxford OX1 4JD, England. [Allen, S. W.] SLAC Natl Accelerator Lab, Menlo Pk, CA 94025 USA. [Fabian, A. C.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Forman, W. R.; Vikhlinin, A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Sanders, J. S.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Simionescu, A.] Japan Aerosp Explorat Agcy, Sagamihara, Kanagawa 2525210, Japan. RP Zhuravleva, I (reprint author), Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, 452 Lomita Mall, Stanford, CA 94305 USA. EM zhur@stanford.edu; churazov@mpa-arching.mpg.de; arevalo.patricia@gmail.com RI Churazov, Eugene/A-7783-2013; OI Sanders, Jeremy/0000-0003-2189-4501; Forman, William/0000-0002-9478-1682 FU NASA, Chandra X-ray Observatory Center [AR4-15013X]; NASA [NAS8-03060]; US Department of Energy [DE-AC02-76SF00515]; Suzaku grants [NNX12AE05G, NNX13AI49G]; FONDECYT [1140304]; Russian Scientific Foundation [14-22-00271] FX Support for this work was provided by the NASA through Chandra award number AR4-15013X issued by the Chandra X-ray Observatory Center, which is operated by the Smithsonian Astrophysical Observatory for and on behalf of the NASA under contract NAS8-03060. SWA acknowledges support from the US Department of Energy under contract number DE-AC02-76SF00515. IZ and NW are partially supported from Suzaku grants NNX12AE05G and NNX13AI49G. PA acknowledges financial support from FONDECYT grant 1140304. EC and RS are partly supported by grant No. 14-22-00271 from the Russian Scientific Foundation. NR 79 TC 17 Z9 17 U1 1 U2 2 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD JUL 11 PY 2015 VL 450 IS 4 BP 4184 EP 4197 DI 10.1093/mnras/stv900 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CQ7YY UT WOS:000360824000062 ER PT J AU Torres, MAP Jonker, PG Miller-Jones, JCA Steeghs, D Repetto, S Wu, JF AF Torres, M. A. P. Jonker, P. G. Miller-Jones, J. C. A. Steeghs, D. Repetto, S. Wu, Jianfeng TI VLT spectroscopy of the black hole candidate Swift J1357.2-0933 in quiescence SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE accretion, accretion discs; black hole physics; binaries: close; stars: individual: Swift J1357.2-0933; X-rays: binaries ID X-RAY BINARY; ACCRETION DISKS; GRO J0422+32; XMM-NEWTON; ORBITAL PERIOD; MASS; SUPERHUMPS; EMISSION; XTE-J1118+480; COMPANION AB We present time-resolved optical spectroscopy of the counterpart to the high-inclination black hole low-mass X-ray binary Swift J1357.2-0933 in quiescence. Absorption features from the mass donor star were not detected. Instead the spectra display prominent broad double-peaked H alpha emission and weaker He I emission lines. From the H alpha peak-to-peak separation, we constrain the radial velocity semi-amplitude of the donor star to K-2 > 789 km s(-1). Further analysis through radial velocity and equivalent width measurements indicates that the H alpha line is free of variability due to S-wave components or disc eclipses. From our data and previous observations during outburst, we conclude that long-term radial velocity changes ascribed to a precessing disc were of low amplitude or not present. This implies that the centroid position of the line should closely represent the systemic radial velocity, gamma. Using the derived gamma = -150 km s(-1) and the best available limits on the source distance, we infer that the black hole is moving towards the plane in its current Galactic orbit unless the proper motion is substantial. Finally, the depth of the central absorption in the double-peaked profiles adds support for Swift J1357.2-0933 as a high-inclination system. On the other hand, we argue that the low hydrogen column density inferred from X-ray fitting suggests that the system is not seen edge-on. C1 [Torres, M. A. P.; Jonker, P. G.] SRON, Netherlands Inst Space Res, NL-3584 CA Utrecht, Netherlands. [Torres, M. A. P.; Jonker, P. G.; Repetto, S.] Radboud Univ Nijmegen, Dept Astrophys IMAPP, NL-6525 AJ Nijmegen, Netherlands. [Torres, M. A. P.] European So Observ, Santiago 19001, Chile. [Miller-Jones, J. C. A.] Curtin Univ, Internat Ctr Radio Astron Res, Perth, WA 6845, Australia. [Steeghs, D.] Univ Warwick, Dept Phys, Coventry CV4 7AL, W Midlands, England. [Wu, Jianfeng] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Torres, MAP (reprint author), SRON, Netherlands Inst Space Res, Sorbonnelaan 2, NL-3584 CA Utrecht, Netherlands. EM M.Torres@sron.nl RI Miller-Jones, James/B-2411-2013 OI Miller-Jones, James/0000-0003-3124-2814 FU Australian Research Council (ARC) [FT140101082, DP120102393]; STFC [PP/D005914/1, ST/I001719/1] FX We thank the anonymous referee for useful comments on the manuscript. We would like to thank Remco de Kok for an independent search for the cross-correlation signal from the donor star in J1357.2 and Jorge Casares for providing us with spectral templates used in these analysis. JCAMJ is the recipient of an Australian Research Council (ARC) Future Fellowship (FT140101082), and also acknowledges support from an ARC Discovery Grant (DP120102393). DS acknowledges support from STFC through an Advanced Fellowship (PP/D005914/1) as well as grant ST/I001719/1 NR 60 TC 4 Z9 4 U1 0 U2 1 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD JUL 11 PY 2015 VL 450 IS 4 BP 4292 EP 4300 DI 10.1093/mnras/stv720 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CQ7YY UT WOS:000360824000071 ER PT J AU Aikawa, Y Furuya, K Nomura, H Qi, CH AF Aikawa, Yuri Furuya, Kenji Nomura, Hideko Qi, Chunhua TI ANALYTICAL FORMULAE OF MOLECULAR ION ABUNDANCES AND THE N2H+ RING IN PROTOPLANETARY DISKS SO ASTROPHYSICAL JOURNAL LA English DT Article DE astrochemistry; protoplanetary disks ID RADIATION HYDRODYNAMIC MODEL; DENSE INTERSTELLAR CLOUDS; PROTOSTELLAR COLLAPSE; HYDROGEN EMISSION; IONIZATION RATE; RAY IONIZATION; GRAIN-GROWTH; COSMIC-RAYS; CHEMISTRY; CO AB We investigate the chemistry of ion molecules in protoplanetary disks, motivated by the detection of the N2H+ ring around TW Hya. While the ring inner radius coincides with the CO snow line, it is not apparent why N2H+ is abundant outside the CO snow line in spite of the similar sublimation temperatures of CO and N-2. Using the full gas-grain network model, we reproduced the N2H+ ring in a disk model with millimeter grains. The chemical conversion of CO and N-2 to less volatile species (sink effect hereinafter) is found to affect the N2H+ distribution. Since the efficiency of the sink depends on various parameters such as activation barriers of grain-surface reactions, which are not well constrained, we also constructed the no-sink model; the total (gas and ice) CO and N-2 abundances are set constant, and their gaseous abundances are given by the balance between adsorption and desorption. Abundances of molecular ions in the no-sink model are calculated by analytical formulae, which are derived by analyzing the full-network model. The N2H+ ring is reproduced by the no-sink model, as well. The 2D (R-Z) distribution of N2H+, however, is different among the full-network model and no-sink model. The column density of N2H+ in the no-sink model depends sensitively on the desorption rate of CO and N-2. and the cosmic-ray flux. We also found that N2H+ abundance can peak at the temperature slightly below the CO sublimation, even if the desorption energies of CO and N-2 are the same. C1 [Aikawa, Yuri] Univ Tsukuba, Ctr Computat Sci, Tsukuba, Ibaraki 3058577, Japan. [Furuya, Kenji] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [Nomura, Hideko] Tokyo Inst Technol, Dept Earth & Planetary Sci, Meguro Ku, Tokyo 1528551, Japan. [Qi, Chunhua] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Aikawa, Y (reprint author), Univ Tsukuba, Ctr Computat Sci, 1-1-1 Tennoudai, Tsukuba, Ibaraki 3058577, Japan. EM aikawa@ccs.tsukuba.ac.jp FU JSPS KAKENHI Grant [23103004, 23103005, 23540266, 25400229]; Japan Society for the Promotion of Science (JSPS) FX We thank Karin Oberg and Catherine Walsh for helpful discussions. We thank the anonymous referee for his/her constructive comments. This work was supported by JSPS KAKENHI Grant Numbers 23103004, 23103005, 23540266, and 25400229. Numerical calculation was partly conducted using SR16000 at YITP in Kyoto University for numerical calculations. K.F. is supported by the Research Fellowship from the Japan Society for the Promotion of Science (JSPS). NR 53 TC 5 Z9 5 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 JUL 10 PY 2015 VL 807 IS 2 AR 120 DI 10.1088/0004-637X/807/2/120 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CO2EB UT WOS:000358967000006 ER PT J AU Akiyama, K Lu, RS Fish, VL Doeleman, SS Broderick, AE Dexter, J Hada, K Kino, M Nagai, H Honma, M Johnson, MD Algaba, JC Asada, K Brinkerink, C Blundell, R Bower, GC Cappallo, R Crew, GB Dexter, M Dzib, SA Freund, R Friberg, P Gurwell, M Ho, PTP Inoue, M Krichbaum, TP Loinard, L MacMahon, D Marrone, DP Moran, JM Nakamura, M Nagar, NM Ortiz-Leon, G Plambeck, R Pradel, N Primiani, RA Rogers, AEE Roy, AL SooHoo, J Tavares, JL Tilanus, RPJ Titus, M Wagner, J Weintroub, J Yamaguchi, P Young, KH Zensus, A Ziurys, LM AF Akiyama, Kazunori Lu, Ru-Sen Fish, Vincent L. Doeleman, Sheperd S. Broderick, Avery E. Dexter, Jason Hada, Kazuhiro Kino, Motoki Nagai, Hiroshi Honma, Mareki Johnson, Michael D. Algaba, Juan C. Asada, Keiichi Brinkerink, Christiaan Blundell, Ray Bower, Geoffrey C. Cappallo, Roger Crew, Geoffrey B. Dexter, Matt Dzib, Sergio A. Freund, Robert Friberg, Per Gurwell, Mark Ho, Paul T. P. Inoue, Makoto Krichbaum, Thomas P. Loinard, Laurent MacMahon, David Marrone, Daniel P. Moran, James M. Nakamura, Masanori Nagar, Neil M. Ortiz-Leon, Gisela Plambeck, Richard Pradel, Nicolas Primiani, Rurik A. Rogers, Alan E. E. Roy, Alan L. SooHoo, Jason Tavares, Jonathan-Leon Tilanus, Remo P. J. Titus, Michael Wagner, Jan Weintroub, Jonathan Yamaguchi, Paul Young, Ken H. Zensus, Anton Ziurys, Lucy M. TI 230 GHz VLBI OBSERVATIONS OF M87: EVENT-HORIZON-SCALE STRUCTURE DURING AN ENHANCED VERY-HIGH-ENERGY gamma-RAY STATE IN 2012 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: active; galaxies: individual (M87); galaxies: jets; radio continuum: galaxies; techniques: high angular resolution; techniques: interferometric ID SUPERMASSIVE BLACK-HOLE; SAGITTARIUS-A-ASTERISK; ADVECTION-DOMINATED ACCRETION; ACTIVE GALACTIC NUCLEI; SIMILAR-TO-10 SCHWARZSCHILD RADII; HIGH-FREQUENCY VLBI; TEV EMISSION; JET BASE; UNIFIED SCHEMES; X-RAY AB We report on 230 GHz (1.3 mm) very long baseline interferometry (VLBI) observations of M87 with the Event Horizon Telescope using antennas on Mauna Kea in Hawaii, Mt. Graham in Arizona, and Cedar Flat in California. For the first time, we have acquired 230 GHz VLBI interferometric phase information on M87 through measurement of the closure phase on the triangle of long baselines. Most of the measured closure phases are consistent with 0 degrees as expected by physically motivated models for 230 GHz structure such as jet models and accretion disk models. The brightness temperature of the event-horizon-scale structure is similar to 1 x 10(10) K derived from the compact flux density of similar to 1 Jy and the angular size of similar to 40 mu as similar to 5.5 R-s, which is broadly consistent with the peak brightness of the radio cores at 1-86 GHz located within similar to 10(2) R-s. Our observations occurred in the middle of an enhancement in very-high-energy (VHE) gamma-ray flux, presumably originating in the vicinity of the central black hole. Our measurements, combined with results of multi-wavelength observations, favor a scenario in which the VHE region has an extended size of similar to 20-60 R-s. C1 [Akiyama, Kazunori] Univ Tokyo, Grad Sch Sci, Dept Astron, Bunkyo Ku, Tokyo 1130033, Japan. [Akiyama, Kazunori; Hada, Kazuhiro; Nagai, Hiroshi; Honma, Mareki] Natl Astron Observ Japan, Mitaka, Tokyo 1818588, Japan. [Lu, Ru-Sen; Fish, Vincent L.; Doeleman, Sheperd S.; Cappallo, Roger; Crew, Geoffrey B.; Rogers, Alan E. E.; SooHoo, Jason; Titus, Michael] MIT, Haystack Observ, Westford, MA 01886 USA. [Lu, Ru-Sen; Dzib, Sergio A.; Krichbaum, Thomas P.; Roy, Alan L.; Wagner, Jan; Zensus, Anton] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Doeleman, Sheperd S.; Johnson, Michael D.; Blundell, Ray; Gurwell, Mark; Moran, James M.; Primiani, Rurik A.; Weintroub, Jonathan; Yamaguchi, Paul; Young, Ken H.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Broderick, Avery E.] Perimeter Inst Theoret Phys, North Waterloo, ON N2L 2Y5, Canada. [Broderick, Avery E.] Univ Waterloo, Dept Phys & Astron, Waterloo, ON N21 3G1, Canada. [Dexter, Jason] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Hada, Kazuhiro] INAF Ist Radioastron, I-40129 Bologna, Italy. [Kino, Motoki; Algaba, Juan C.; Wagner, Jan] Korea Astron & Space Sci Inst KASI, Taejon 305348, South Korea. [Honma, Mareki] Grad Univ Adv Studies, Mitaka, Tokyo 1818588, Japan. [Algaba, Juan C.; Asada, Keiichi; Ho, Paul T. P.; Inoue, Makoto; Nakamura, Masanori; Pradel, Nicolas] Acad Sinica, Inst Astron & Astrophys, Taipei 10617, Taiwan. [Brinkerink, Christiaan; Tilanus, Remo P. J.] Radboud Univ Nijmegen, Dept Astrophys, IMAPP, NL-6500 GL Nijmegen, Netherlands. [Bower, Geoffrey C.] Acad Sinica, Inst Astron & Astrophys, Hilo, HI 96720 USA. [Dexter, Matt; MacMahon, David; Plambeck, Richard] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Dzib, Sergio A.; Loinard, Laurent; Ortiz-Leon, Gisela] Univ Nacl Autonoma Mexico, Ctr Radiostron & Astrofis, Morelia 58089, Michoacan, Mexico. [Freund, Robert; Marrone, Daniel P.; Ziurys, Lucy M.] Univ Arizona, Arizona Radio Observ, Steward Observ, Tucson, AZ 85721 USA. [Friberg, Per] Joint Astron Ctr, James Clerk Maxwell Telescope, Hilo, HI 96720 USA. [Nagar, Neil M.] Univ Concepcion, Dept Astron, Concepcion, Chile. [Tavares, Jonathan-Leon] Inst Nacl Astrofis Opt & Electr, Puebla 72000, Mexico. [Tilanus, Remo P. J.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. RP Akiyama, K (reprint author), Univ Tokyo, Grad Sch Sci, Dept Astron, Bunkyo Ku, 7-3-1 Hongo, Tokyo 1130033, Japan. EM kazunori.akiyama@nao.ac.jp FU Japan Society for the Promotion of Science (JSPS); Perimeter Institute for Theoretical Physics; Natural Sciences and Engineering Research Council of Canada; DGAPA; UNAM; CONACyT (Mexico); National Science Foundation (NSF); Gordon and Betty Moore Foundation [GMBF-3561]; NSF University Radio Observatories (URO) program [AST 1140030]; Smithsonian Institution; Academia Sinica; NSF; CARMA partner universities; MEXT/JSPS KAKENHI [24540242, 25120007, 25120008]; Government of Canada through Industry Canada; Province of Ontario through the Ministry of Research and Innovation FX We would like to thank an anonymous referee for many constructive suggestions to improve the paper. K. Akiyama thanks Dr. Akihiro Doi, Prof. Alan Marscher, Dr. Svetlana Jorstad, and Dr. Jose L. Gomez for fruitful discussions on scientific interpretations. K. Akiyama and K. H. are supported by a Grant-in-Aid for Research Fellows of the Japan Society for the Promotion of Science (JSPS). A. E. B. receives financial support from the Perimeter Institute for Theoretical Physics and the Natural Sciences and Engineering Research Council of Canada through a Discovery Grant. L. L. and G. O. L. acknowledge the support of DGAPA, UNAM, and CONACyT (Mexico). Event Horizon Telescope work at the MIT Haystack Observatory and the Harvard Smithsonian Center for Astrophysics is supported by grants from the National Science Foundation (NSF) and through an award from the Gordon and Betty Moore Foundation (GMBF-3561). The Arizona Radio Observatory (ARO) is partially supported through the NSF University Radio Observatories (URO) program under grant No. AST 1140030. The Submillimeter Array is a joint project between the Smithsonian Astrophysical Observatory and the Academia Sinica Institute of Astronomy and Astrophysics and is funded by the Smithsonian Institution and the Academia Sinica. Funding for ongoing CARMA development and operations is supported by the NSF and the CARMA partner universities. Event Horizon Telescope work at the Mizusawa VLBI Observatory is financially supported by the MEXT/JSPS KAKENHI Grant Numbers 24540242, 25120007, and 25120008. 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. This work has benefited from open source technology shared by the Collaboration for Astronomy Signal Processing and Electronics Research (CASPER) and from equipment donated by Xilinx Inc. NR 92 TC 17 Z9 16 U1 2 U2 8 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUL 10 PY 2015 VL 807 IS 2 AR 150 DI 10.1088/0004-637X/807/2/150 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CO2EB UT WOS:000358967000036 ER PT J AU Asgari-Targhi, M Schmelz, JT Imada, S Pathak, S Christian, GM AF Asgari-Targhi, M. Schmelz, J. T. Imada, S. Pathak, S. Christian, G. M. TI MODELING OF HOT PLASMA IN THE SOLAR ACTIVE REGION CORE SO ASTROPHYSICAL JOURNAL LA English DT Article DE magnetohydrodynamics (MHD); Sun: corona; Sun: UV radiation ID EUV IMAGING SPECTROMETER; ALFVEN-WAVE TURBULENCE; FIELD TEMPERATURE DISTRIBUTIONS; AN ATOMIC DATABASE; X-RAY TELESCOPE; CORONAL LOOPS; EMISSION MEASURE; HINODE; DYNAMICS; MOTIONS AB Magnetically confined plasma with temperatures >= 5 MK are a feature of hot coronal loops observed in the core of active regions. In this paper, using observations and MHD modeling of coronal loops, we investigate whether wave heating (Alternating Current) models can describe the high temperature loops observed in the active region of 2012 September 7. We construct three-dimensional MHD models for the Alfven wave turbulence within loops with high temperature. We find that for the Alfven waves to create enough turbulence to heat the corona, the rms velocity at the footpoints must be 5-6 km s(-1). We conclude that the Alfven wave turbulence model may be a candidate for explaining how the hot loops are heated, provided the loops have a high velocity at their photospheric footpoints. C1 [Asgari-Targhi, M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Schmelz, J. T.; Pathak, S.; Christian, G. M.] Univ Memphis, Dept Phys, Memphis, TN 38152 USA. [Imada, S.] Nagoya Univ, Solar Terr Environm Lab, Chikusa Ku, Nagoya, Aichi 4648601, Japan. RP Asgari-Targhi, M (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St MS 15, Cambridge, MA 02138 USA. FU UK's Engineering and Physical Sciences Research Council [EP/I034327/1] FX We thank the referee for comments which helped to improve the paper. We thank Adriaan A. van Ballegooijen for discussions and comments that helped improve the paper. We are most grateful to Alex Voss from the School of Computer Science at the University of St. Andrews for his support with the computational work, which was funded by the UK's Engineering and Physical Sciences Research Council (EP/I034327/1). NR 55 TC 2 Z9 2 U1 0 U2 0 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 JUL 10 PY 2015 VL 807 IS 2 AR 146 DI 10.1088/0004-637X/807/2/146 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CO2EB UT WOS:000358967000032 ER PT J AU Cheung, MCM Boerner, P Schrijver, CJ Testa, P Chen, F Peter, H Malanushenko, A AF Cheung, Mark C. M. Boerner, P. Schrijver, C. J. Testa, P. Chen, F. Peter, H. Malanushenko, A. TI THERMAL DIAGNOSTICS WITH THE ATMOSPHERIC IMAGING ASSEMBLY ON BOARD THE SOLAR DYNAMICS OBSERVATORY: A VALIDATED METHOD FOR DIFFERENTIAL EMISSION MEASURE INVERSIONS SO ASTROPHYSICAL JOURNAL LA English DT Article DE methods: observational; plasmas; radiation mechanisms: thermal; Sun: activity; Sun: atmosphere; Sun: corona ID ACTIVE-REGION; TEMPERATURE STRUCTURE; MAGNETIC-FIELD; FUNDAMENTAL LIMITATIONS; PLASMAS. APPLICATION; ATOMIC DATABASE; FLUX EMERGENCE; CORONAL LOOPS; SIMULATIONS; SPECTRA AB We present a new method for performing differential emission measure (DEM) inversions on narrow-band EUV images from the Atmospheric Imaging Assembly (AIA) on board the Solar Dynamics Observatory. The method yields positive definite DEM solutions by solving a linear program. This method has been validated against a diverse set of thermal models of varying complexity and realism. These include (1) idealized Gaussian DEM distributions, (2) 3D models of NOAA Active Region 11158 comprising quasi-steady loop atmospheres in a nonlinear force-free field, and (3) thermodynamic models from a fully compressible, 3D MHD simulation of active region (AR) corona formation following magnetic flux emergence. We then present results from the application of the method to AIA observations of Active Region 11158, comparing the region's thermal structure on two successive solar rotations. Additionally, we show how the DEM inversion method can be adapted to simultaneously invert AIA and Hinode X-ray Telescope data, and how supplementing AIA data with the latter improves the inversion result. The speed of the method allows for routine production of DEM maps, thus facilitating science studies that require tracking of the thermal structure of the solar corona in time and space. C1 [Cheung, Mark C. M.; Boerner, P.; Schrijver, C. J.; Malanushenko, A.] Lockheed Martin Solar & Astrophys Lab, Palo Alto, CA 94304 USA. [Testa, P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Chen, F.; Peter, H.] Max Planck Inst Solar Syst Res, D-37077 Gottingen, Germany. [Malanushenko, A.] Natl Ctr Atmospher Res, High Altitude Observ, Boulder, CO 80301 USA. RP Cheung, MCM (reprint author), Lockheed Martin Solar & Astrophys Lab, 3251 Hanover St Bldg 252, Palo Alto, CA 94304 USA. EM cheung@lmsal.com RI Chen, Feng/B-1968-2012 OI Chen, Feng/0000-0002-1963-5319 FU NASA's SDO/AIA contract [NNG04EA00C]; NASA [NNX14AI14G] FX The authors acknowledge support from NASA's SDO/AIA contract (NNG04EA00C) to LMSAL. AIA is an instrument on board the Solar Dynamics Observatory, a mission for NASA's Living With a Star program. Additionally, M.C.M.C., P.T. and A.M. acknowledge support from NASA's Heliophysics Grand Challenges Research grant (NNX14AI14G). The authors wish to thank members of the Hinode/XRT team (especially M. Weber and K. Reeves) for valuable discussions about joint AIA/XRT inversions. Furthermore, we wish to thank H. Warren, J. Plowman, S. White, and the anonymous referee for helpful comments that led to improvements in this work. NR 60 TC 8 Z9 9 U1 0 U2 0 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 JUL 10 PY 2015 VL 807 IS 2 AR 143 DI 10.1088/0004-637X/807/2/143 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CO2EB UT WOS:000358967000029 ER PT J AU Espaillat, C Andrews, S Powell, D Feldman, D Qi, C Wilner, D D'Alessio, P AF Espaillat, C. Andrews, S. Powell, D. Feldman, D. Qi, C. Wilner, D. D'Alessio, P. TI THE TRANSITIONAL DISK AROUND IRAS 04125+2902 SO ASTROPHYSICAL JOURNAL LA English DT Article DE infrared: planetary systems; planet-disk interactions; planets and satellites: formation; protoplanetary disks; stars: pre-main sequence; submillimeter: planetary systems ID T-TAURI STARS; MAIN-SEQUENCE STARS; AURIGA MOLECULAR CLOUD; MASS ACCRETION RATES; SPITZER IRS SPECTRA; ALL-SKY SURVEY; PROTOPLANETARY DISKS; PRETRANSITIONAL DISKS; YOUNG OBJECTS; GRAIN-GROWTH AB Resolved submillimeter imaging of transitional disks is increasingly revealing the complexity of disk structure. Here, we present the first high-resolution submillimeter image of a recently identified transitional disk around IRAS 04125+2902 in the Taurus star-forming region. We measure an inner disk hole of similar to 20 AU around IRAS 04125+2902 by simultaneously modeling new 880 mu m Submillimeter Array data along with an existing spectral energy distribution supplemented by new Discovery Channel Telescope photometry. We also constrain the outer radius of the dust disk in IRAS 04125+2902 to similar to 50-60 AU. Such a small dust disk could be attributed to initial formation conditions, outward truncation by an unseen companion, or dust evolution in the disk. Notably, the dust distribution of IRAS 04125+2902 resembles a narrow ring (Delta R similar to 35 AU) composed of large dust grains at the location of the disk wall. Such narrow dust rings are also seen in other transitional disks and may be evidence of dust trapping in pressure bumps, possibly produced by planetary companions. More sensitive submillimeter observations of the gas are necessary to further probe the physical mechanisms at work in shaping the spatial distribution of large dust in this disk. Interestingly, the IRAS 04125+2902 disk is significantly fainter than other transitional disks that have been resolved at submillimeter wavelengths, hinting that more objects with large disk holes may exist at the faint end of the submillimeter luminosity distribution that await detection with more sensitive imaging telescopes. C1 [Espaillat, C.; Feldman, D.] Boston Univ, Dept Astron, Boston, MA 02215 USA. [Andrews, S.; Powell, D.; Qi, C.; Wilner, D.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [D'Alessio, P.] Univ Nacl Autonoma Mexico, Ctr Radioastron & Astrofis, Morelia 58089, Michoacan, Mexico. RP Espaillat, C (reprint author), Boston Univ, Dept Astron, 725 Commonwealth Ave, Boston, MA 02215 USA. EM cce@bu.edu FU Smithsonian Institution; Academia Sinica; University of Maryland; University of Toledo; Northern Arizona University; Discovery Communications, Inc., Boston University FX We thank the referee for comments that helped to improve the paper. We thank Nuria Calvet, Ramiro Franco-Hernanndez, Elise Furlan, and Melissa McClure for discussions. We thank Adam Kraus for sharing results before publication. The SMA is a joint project between the Smithsonian Astrophysical Observatory and the Academia Sinica Institute of Astronomy and Astrophysics and is funded by the Smithsonian Institution and the Academia Sinica. The 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. These results made use of the Discovery Channel Telescope at Lowell Observatory, supported by Discovery Communications, Inc., Boston University, the University of Maryland, the University of Toledo and Northern Arizona University. Finally, a special recognition of the contribution of Paola D'Alessio, who passed away in November of 2013. She is greatly missed as a scientist, colleague, and friend. Paola would have been happy to see her research continue to have an important impact in the star formation community. NR 103 TC 3 Z9 3 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUL 10 PY 2015 VL 807 IS 2 AR 156 DI 10.1088/0004-637X/807/2/156 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CO2EB UT WOS:000358967000042 ER PT J AU Keisler, R Hoover, S Harrington, N Henning, JW Ade, PAR Aird, KA Austermann, JE Beall, JA Bender, AN Benson, BA Bleem, LE Carlstrom, JE Chang, CL Chiang, HC Cho, HM Citron, R Crawford, TM Crites, AT de Haan, T Dobbs, MA Everett, W Gallicchio, J Gao, J George, EM Gilbert, A Halverson, NW Hanson, D Hilton, GC Holder, GP Holzapfel, WL Hou, Z Hrubes, JD Huang, N Hubmayr, J Irwin, KD Knox, L Lee, AT Leitch, EM Li, D Luong-Van, D Marrone, DP McMahon, JJ Mehl, J Meyer, SS Mocanu, L Natoli, T Nibarger, JP Novosad, V Padin, S Pryke, C Reichardt, CL Ruhl, JE Saliwanchik, BR Sayre, JT Schaffer, KK Shirokoff, E Smecher, G Stark, AA Story, KT Tucker, C Vanderlinde, K Vieira, JD Wang, G Whitehorn, N Yefremenko, V Zahn, O AF Keisler, R. Hoover, S. Harrington, N. Henning, J. W. Ade, P. A. R. Aird, K. A. Austermann, J. E. Beall, J. A. Bender, A. N. Benson, B. A. Bleem, L. E. Carlstrom, J. E. Chang, C. L. Chiang, H. C. Cho, H-M. Citron, R. Crawford, T. M. Crites, A. T. de Haan, T. Dobbs, M. A. Everett, W. Gallicchio, J. Gao, J. George, E. M. Gilbert, A. Halverson, N. W. Hanson, D. Hilton, G. C. Holder, G. P. Holzapfel, W. L. Hou, Z. Hrubes, J. D. Huang, N. Hubmayr, J. Irwin, K. D. Knox, L. Lee, A. T. Leitch, E. M. Li, D. Luong-Van, D. Marrone, D. P. McMahon, J. J. Mehl, J. Meyer, S. S. Mocanu, L. Natoli, T. Nibarger, J. P. Novosad, V. Padin, S. Pryke, C. Reichardt, C. L. Ruhl, J. E. Saliwanchik, B. R. Sayre, J. T. Schaffer, K. K. Shirokoff, E. Smecher, G. Stark, A. A. Story, K. T. Tucker, C. Vanderlinde, K. Vieira, J. D. Wang, G. Whitehorn, N. Yefremenko, V. Zahn, O. TI MEASUREMENTS OF SUB-DEGREE B-MODE POLARIZATION IN THE COSMIC MICROWAVE BACKGROUND FROM 100 SQUARE DEGREES OF SPTPOL DATA SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmic background radiation; cosmology: observations ID SOUTH-POLE TELESCOPE; LARGE-SCALE STRUCTURE; CMB POLARIZATION; POWER SPECTRUM; ANISOTROPIES; TEMPERATURE; COMPUTATION; PARAMETERS; PHYSICS; RADIO AB We present a measurement of the B-mode polarization power spectrum (the BB spectrum) from 100 deg(2) of sky observed with SPTpol, a polarization-sensitive receiver currently installed on the South Pole Telescope. The observations used in this work were taken during 2012 and early 2013 and include data in spectral bands centered at 95 and 150 GHz. We report the BB spectrum in five bins in multipole space, spanning the range 300 <= l <= 2300, and for three spectral combinations: 95 GHz x 95 GHz, 95 GHz x 150 GHz, and 150 GHz x 150 GHz. We subtract small (<0.5 sigma in units of statistical uncertainty) biases from these spectra and account for the uncertainty in those biases. The resulting power spectra are inconsistent with zero power but consistent with predictions for the BB spectrum arising from the gravitational lensing of E-mode polarization. If we assume no other source of BB power besides lensed B modes, we determine a preference for lensed B modes of 4.9 sigma. After marginalizing over tensor power and foregrounds, namely, polarized emission from galactic dust and extragalactic sources, this significance is 4.3 sigma. Fitting for a single parameter, A(lens), that multiplies the predicted lensed B-mode spectrum, and marginalizing over tensor power and foregrounds, we find A(lens) = 1.08 +/- 0.26, indicating that our measured spectra are consistent with the signal expected from gravitational lensing. The data presented here provide the best measurement to date of the B-mode power spectrum on these angular scales. C1 [Keisler, R.; Irwin, K. D.] Stanford Univ, Dept Phys, Stanford, CA 94305 USA. [Keisler, R.] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94305 USA. [Hoover, S.; Henning, J. W.; Bender, A. N.; Benson, B. A.; Bleem, L. E.; Carlstrom, J. E.; Chang, C. L.; Citron, R.; Crawford, T. M.; Crites, A. T.; Gallicchio, J.; Hou, Z.; Leitch, E. M.; Mehl, J.; Meyer, S. S.; Mocanu, L.; Natoli, T.; Schaffer, K. K.; Shirokoff, E.; Story, K. T.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Hoover, S.; Bleem, L. E.; Carlstrom, J. E.; Natoli, T.; Story, K. T.] Univ Chicago, Dept Phys, Chicago, IL 60637 USA. [Harrington, N.; de Haan, T.; George, E. M.; Holzapfel, W. L.; Huang, N.; Lee, A. T.; Reichardt, C. L.; Whitehorn, N.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. [Henning, J. W.; Austermann, J. E.; Everett, W.; Halverson, N. W.] Univ Colorado, Dept Astrophys & Planetary Sci, Boulder, CO 80309 USA. [Ade, P. A. R.; Tucker, C.] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales. [Aird, K. A.; Hrubes, J. D.; Luong-Van, D.] Univ Chicago, Chicago, IL 60637 USA. [Austermann, J. E.; Beall, J. A.; Gao, J.; Hilton, G. C.; Hubmayr, J.; Li, D.; Nibarger, J. P.] NIST, Quantum Devices Grp, Boulder, CO 80305 USA. [Bender, A. N.; Dobbs, M. A.; Gilbert, A.; Hanson, D.; Holder, G. P.; Smecher, G.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada. [Bender, A. N.; Bleem, L. E.; Carlstrom, J. E.; Chang, C. L.; Mehl, J.; Wang, G.; Yefremenko, V.] Argonne Natl Lab, Div High Energy Phys, Argonne, IL 60439 USA. [Benson, B. A.; Carlstrom, J. E.; Chang, C. L.; Crawford, T. M.; Crites, A. T.; Leitch, E. M.; Meyer, S. S.; Mocanu, L.; Shirokoff, E.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. [Benson, B. A.] Fermilab Natl Accelerator Lab, Batavia, IL 60510 USA. [Carlstrom, J. E.; Meyer, S. S.; Schaffer, K. K.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA. [Chiang, H. C.] Univ KwaZulu Natal, Sch Math Stat & Comp Sci, Durban, South Africa. [Cho, H-M.; Li, D.] SLAC Natl Accelerator Lab, Menlo Pk, CA 94025 USA. [Crites, A. T.; Padin, S.] CALTECH, Pasadena, CA 91125 USA. [Dobbs, M. A.] Canadian Inst Adv Res, CIFAR Program Cosmol & Grav, Toronto, ON M5G 1Z8, Canada. [Halverson, N. W.] Univ Colorado, Dept Phys, Boulder, CO 80309 USA. [Knox, L.] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA. [Lee, A. T.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Div Phys, Berkeley, CA 94720 USA. [Marrone, D. P.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [McMahon, J. J.] Univ Michigan, Dept Phys, Ann Arbor, MI 48109 USA. [Ruhl, J. E.; Saliwanchik, B. R.; Sayre, J. T.] Case Western Reserve Univ, Ctr Educ & Res Cosmol & Astrophys, Dept Phys, Cleveland, OH 44106 USA. [Novosad, V.] Argonne Natl Lab, Div Mat Sci, Argonne, IL 60439 USA. [Pryke, C.] Univ Minnesota, Sch Phys & Astron, Minneapolis, MN 55455 USA. [Reichardt, C. L.] Univ Melbourne, Sch Phys, Parkville, Vic 3010, Australia. [Schaffer, K. K.] Sch Art Inst Chicago, Liberal Arts Dept, Chicago, IL 60603 USA. [Smecher, G.] Three Speed Log Inc, Vancouver, BC V6A 2J8, Canada. [Stark, A. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Vanderlinde, K.] Univ Toronto, Dunlap Inst Astron & Astrophys, Toronto, ON M5S 3H4, Canada. [Vanderlinde, K.] Univ Toronto, Dept Astron Astrophys, Toronto, ON M5S 3H4, Canada. [Vieira, J. D.] Univ Illinois, Dept Astron, Urbana, IL 61801 USA. [Vieira, J. D.] Univ Illinois, Dept Phys, Urbana, IL 61801 USA. [Zahn, O.] Univ Calif Berkeley, Berkeley Ctr Cosmol Phys, Dept Phys, Berkeley, CA 94720 USA. [Zahn, O.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA. RP Keisler, R (reprint author), Stanford Univ, Dept Phys, 382 Via Pueblo Mall, Stanford, CA 94305 USA. EM rkeisler@stanford.edu RI Novosad, V /J-4843-2015; OI CRAWFORD, THOMAS/0000-0001-9000-5013; Aird, Kenneth/0000-0003-1441-9518; Reichardt, Christian/0000-0003-2226-9169; Stark, Antony/0000-0002-2718-9996 FU National Science Foundation [PLR-1248097, AST-1402161]; NSF Physics Frontier Center [PHY-0114422]; Kavli Foundation; Gordon and Betty Moore Foundation through Grant GBMF [947]; Natural Sciences and Engineering Research Council of Canada; Canadian Institute for Advanced Research; Canada Research Chairs program; Fermi Research Alliance, LLC [De-AC02-07CH11359]; U.S. Department of Energy; NSF [AST-0956135]; UChicago Argonne, LLC, Operator of Argonne National Laboratory (Argonne); Argonne, a U.S. Department of Energy Office of Science Laboratory [DE-AC02-06CH11357]; Argonne Center for Nanoscale Materials; Office of Science of the U.S. Department of Energy [DE-AC02-05CH11231] FX The South Pole Telescope program is supported by the National Science Foundation through grant PLR-1248097. Partial support is also provided by the NSF Physics Frontier Center grant PHY-0114422 to the Kavli Institute of Cosmological Physics at the University of Chicago, the Kavli Foundation, and the Gordon and Betty Moore Foundation through Grant GBMF#947 to the University of Chicago. The McGill authors acknowledge funding from the Natural Sciences and Engineering Research Council of Canada, Canadian Institute for Advanced Research, and Canada Research Chairs program. J.W.H. is supported by the National Science Foundation under Award No. AST-1402161. B.B. is supported by the Fermi Research Alliance, LLC, under Contract No. De-AC02-07CH11359 with the U.S. Department of Energy. The CU Boulder group acknowledges support from NSF AST-0956135. This work is also supported by the U.S. Department of Energy. Work at Argonne National Lab is supported by UChicago Argonne, LLC, Operator of Argonne National Laboratory (Argonne). Argonne, a U.S. Department of Energy Office of Science Laboratory, is operated under Contract No. DE-AC02-06CH11357. We also acknowledge support from the Argonne Center for Nanoscale Materials. This research used resources of the National Energy Research Scientific Computing Center, a DOE Office of Science User Facility supported by the Office of Science of the U.S. Department of Energy under Contract No. DE-AC02-05CH11231. The data analysis pipeline uses the scientific python stack (Jones et al. 2001; Hunter 2007; van der Walt et al. 2011) and the HDF5 file format (The HDF Group 1997). NR 56 TC 33 Z9 33 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 JUL 10 PY 2015 VL 807 IS 2 AR 151 DI 10.1088/0004-637X/807/2/151 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CO2EB UT WOS:000358967000037 ER PT J AU Skibba, RA Coil, AL Mendez, AJ Blanton, MR Bray, AD Cool, RJ Eisenstein, DJ Guo, H Miyaji, T Moustakas, J Zhu, GT AF Skibba, Ramin A. Coil, Alison L. Mendez, Alexander J. Blanton, Michael R. Bray, Aaron D. Cool, Richard J. Eisenstein, Daniel J. Guo, Hong Miyaji, Takamitsu Moustakas, John Zhu, Guangtun TI DARK MATTER HALO MODELS OF STELLAR MASS-DEPENDENT GALAXY CLUSTERING IN PRIMUS+DEEP2 AT 0.2 < z < 1.2 SO ASTROPHYSICAL JOURNAL LA English DT Article DE dark matter; galaxies: evolution; galaxies: halos; large-scale structure of universe; methods: analytical; methods: statistical AB We utilize Lambda CDM halo occupation models of galaxy clustering to investigate the evolving stellar mass dependent clustering of galaxies in the PRIsm MUlti-object Survey (PRIMUS) and DEEP2 Redshift Survey over the past eight billion years of cosmic time, between 0.2 < z < 1.2. These clustering measurements provide new constraints on the connections between dark matter halo properties and galaxy properties in the context of the evolving large-scale structure of the universe. Using both an analytic model and a set of mock galaxy catalogs, we find a strong correlation between central galaxy stellar mass and dark matter halo mass over the range M-halo similar to 10(11)-10(13)h(-1) M-circle dot, approximately consistent with previous observations and theoretical predictions. However, the stellar-to-halo mass relation and the mass scale where star formation efficiency reaches a maximum appear to evolve more strongly than predicted by other models, including models based primarily on abundance-matching constraints. We find that the fraction of satellite galaxies in halos of a given mass decreases significantly from z similar to 0.5 to z similar to 0.9, partly due to the fact that halos at fixed mass are rarer at higher redshift and have lower abundances. We also find that the M-1/M-min ratio, a model parameter that quantifies the critical mass above which halos host at least one satellite, decreases from approximate to 20 at z similar to 0 to approximate to 13 at z similar to 0.9. Considering the evolution of the subhalo mass function vis-a-vis satellite abundances, this trend has implications for relations between satellite galaxies and halo substructures and for intracluster mass, which we argue has grown due to stripped and disrupted satellites between z similar to 0.9 and z similar to 0.5. C1 [Skibba, Ramin A.; Coil, Alison L.; Mendez, Alexander J.] Univ Calif San Diego, Dept Phys, Ctr Astrophys & Space Sci, La Jolla, CA 92093 USA. [Mendez, Alexander J.; Zhu, Guangtun] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Blanton, Michael R.] NYU, Dept Phys, Ctr Cosmol & Particle Phys, New York, NY 10003 USA. [Bray, Aaron D.; Eisenstein, Daniel J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Cool, Richard J.] Univ Arizona, MMT Observ, Tucson, AZ 85721 USA. [Guo, Hong] Chinese Acad Sci, Shanghai Astron Observ, Key Lab Res Galaxies & Cosmol, Shanghai 200030, Peoples R China. [Miyaji, Takamitsu] Univ Nacl Autonoma Mexico, Inst Astron, Ensenada, Baja California, Mexico. [Moustakas, John] Siena Coll, Dept Phys & Astron, Loudonville, NY 12211 USA. RP Skibba, RA (reprint author), Univ Calif San Diego, Dept Phys, Ctr Astrophys & Space Sci, 9500 Gilman Dr, La Jolla, CA 92093 USA. EM raminskibba@gmail.com RI Guo, Hong/J-5797-2015; OI Guo, Hong/0000-0003-4936-8247; Zhu, Guangtun/0000-0002-7574-8078; Miyaji, Takamitsu/0000-0002-7562-485X FU NSF CAREER award [AST-1055081]; UNAM-DGAPA PAPIIT [IN110209]; CONACyT [83564]; NSF [PHYS-1066293, AST-0607701, 0908246, 0908442, 0908354]; NASA [08-ADP08-0019] FX R.A.S. and A.L.C. acknowledge support from the NSF CAREER award AST-1055081. T.M. is supported by UNAM-DGAPA PAPIIT IN110209 and CONACyT Grant #83564. We thank the Aspen Center for Physics, which has been supported by NSF grant PHYS-1066293, for hospitality during the summer 2014 workshop on the "Galaxy-Halo Connection Across Cosmic Time," where some of this work was completed. We acknowledge Peter Behroozi, Andrew Hearin, Alexie Leauthaud, Ravi Sheth, and Doug Watson for valuable discussions about our models and results, and we thank Idit Zehavi and Zheng Zheng for helpful comments on a previous draft. We also thank the anonymous referee for valuable recommendations that improved the quality of the paper. We acknowledge Scott Burles and Kenneth Wong for their contributions to the PRIMUS project. Funding for PRIMUS has been provided by NSF grants AST-0607701, 0908246, 0908442, 0908354, and NASA grant 08-ADP08-0019. NR 0 TC 12 Z9 12 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUL 10 PY 2015 VL 807 IS 2 AR 152 DI 10.1088/0004-637X/807/2/152 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CO2EB UT WOS:000358967000038 ER PT J AU Su, YN van Ballegooijen, A McCauley, P Ji, HS Reeves, KK DeLuca, EE AF Su, Yingna van Ballegooijen, Adriaan McCauley, Patrick Ji, Haisheng Reeves, Katharine K. DeLuca, Edward E. TI MAGNETIC STRUCTURE AND DYNAMICS OF THE ERUPTING SOLAR POLAR CROWN PROMINENCE ON 2012 MARCH 12 SO ASTROPHYSICAL JOURNAL LA English DT Article DE Sun: activity; Sun: corona; Sun: coronal mass ejections (CMEs); Sun: filaments; prominences; Sun: magnetic fields ID CORONAL MASS EJECTIONS; FLUX ROPES; RECONNECTION OUTFLOWS; ACTIVE REGIONS; CURRENT SHEET; FILAMENT; FLARES; FIELD; MODEL; ONSET AB We present an investigation of the polar crown prominence that erupted on 2012 March 12. This prominence is observed at the southeast limb by the Solar Dynamics Observatory (SDO)/Atmospheric Imaging Assembly (AIA; end-on view) and displays a quasi-vertical thread structure. A bright U-shaped or horn-like structure is observed surrounding the upper portion of the prominence at 171 angstrom before the eruption and becomes more prominent during the eruption. The disk view of STEREOB shows that this long prominence is composed of a series of vertical threads and displays a half-loop-like structure during the eruption. We focus on the magnetic support of the prominence vertical threads by studying the structure and dynamics of the prominence before and during the eruption using observations from SDO and STEREO_B. We also construct a series of magnetic field models (sheared arcade model, twisted flux rope model, and unstable model with hyperbolic flux tube). Various observational characteristics appear to be in favor of the twisted flux rope model. We find that the flux rope supporting the prominence enters the regime of torus instability at the onset of the fast-rise phase, and signatures of reconnection (posteruption arcade, new U-shaped structure, rising blobs) appear about one hour later. During the eruption, AIA observes dark ribbons seen in absorption at 171 angstrom corresponding to the bright ribbons shown at 304 angstrom, which might be caused by the erupting filament material falling back along the newly reconfigured magnetic fields. Brightenings at the inner edge of the erupting prominence arcade are also observed in all AIA EUV channels, which might be caused by the heating due to energy released from reconnection below the rising prominence. C1 [Su, Yingna; Ji, Haisheng] Chinese Acad Sci, Purple Mt Observ, Key Lab Dark Matter & Space Sci, Nanjing 210008, Jiangsu, Peoples R China. [Su, Yingna; van Ballegooijen, Adriaan; McCauley, Patrick; Reeves, Katharine K.; DeLuca, Edward E.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Su, YN (reprint author), Chinese Acad Sci, Purple Mt Observ, Key Lab Dark Matter & Space Sci, Nanjing 210008, Jiangsu, Peoples R China. EM ynsu@pmo.ac.cn RI McCauley, Patrick/P-7747-2015; DeLuca, Edward/L-7534-2013; OI McCauley, Patrick/0000-0002-1450-7350; DeLuca, Edward/0000-0001-7416-2895; van Ballegooijen, Adriaan/0000-0002-5622-3540; Reeves, Katharine/0000-0002-6903-6832 FU LMSAL [SP02H1701R]; NASA [NNX12AI30G]; Natural Science Foundation of China (NSFC) [11333009, 11173062, 11473071]; Youth Fund of Jiangsu [BK20141043]; Chinese Academy of Sciences FX We thank the referee for helpful comments to improve the manuscript. Y.N.S. is grateful to Drs. Cheng Fang, Bernhard Kliem, Xin Cheng, Eric Priest, and Bin Chen for valuable discussions. We thank the teams of SDO/AIA, SDO/HMI, STEREO/EUVI for providing the valuable data. The STEREO and HMI data are downloaded via the Virtual Solar Observatory and the Joint Science Operations Center. This project is partially supported under contract SP02H1701R from LMSAL to SAO as well as NASA grant NNX12AI30G. This work is also supported by the Natural Science Foundation of China (NSFC) No. 11333009, 11173062, 11473071, and the Youth Fund of Jiangsu No. BK20141043. Y.N.S. is also supported by the "One hundred talent project" of the Chinese Academy of Sciences. NR 71 TC 9 Z9 9 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 JUL 10 PY 2015 VL 807 IS 2 AR 144 DI 10.1088/0004-637X/807/2/144 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CO2EB UT WOS:000358967000030 ER PT J AU Estrada, C Degner, EC Rojas, EI Wcislo, WT Van Bael, SA AF Estrada, Catalina Degner, Ethan C. Rojas, Enith I. Wcislo, William T. Van Bael, Sunshine A. TI The role of endophyte diversity in protecting plants from defoliation by leaf-cutting ants SO CURRENT SCIENCE LA English DT Article DE Atta colombica; Colletotrichum tropicale; fungal community; herbivory; symbiosis ID IN-VITRO INTERACTIONS; FUNGAL ENDOPHYTES; FUSARIUM-VERTICILLIOIDES; FOLIAR ENDOPHYTES; SYMBIOTIC FUNGI; USTILAGO-MAYDIS; SALICYLIC-ACID; PATHOGEN; RESISTANCE; TRAITS AB Plants host a vast diversity of fungal symbionts inside their tissues that live in close proximity with each other to form rich and dynamic communities. Although endophytes can affect plant-herbivore interactions in several ways, it is still not known to what extent such effects are influenced by the properties of endophyte communities or by particular species traits. Here we compared the effects of high versus low foliar fungal endophyte diversity on the preferences of laboratory and wild colonies of leaf-cutting ants. We found that when endophyte densities were high, the ants responded similarly to leaves hosting one endophyte species, Colletotrichum tropicale, or those hosting a species-rich endophyte community. Results were also consistent when comparing the laboratory versus wild ant colonies. We discuss the significance of these results with respect to the ecological effects of plant-endophyte interactions in natural and agricultural ecosystems. C1 [Estrada, Catalina; Degner, Ethan C.; Rojas, Enith I.; Wcislo, William T.; Van Bael, Sunshine A.] Smithsonian Trop Res Inst, Panama City, Panama. [Van Bael, Sunshine A.] Tulane Univ, Dept Ecol & Evolutionary Biol, New Orleans, LA 70118 USA. RP Estrada, C (reprint author), Smithsonian Trop Res Inst, Apartado 0843-03092, Panama City, Panama. EM estradac@si.edu FU Smithsonian Institute Scholarly Studies Program; STRI Internship; NSF [DEB-0949602]; SENACYT [FID10-091] FX We thank M. Caballero and F. Santos (STRI) for laboratory support. This work was funded by the Smithsonian Institute Scholarly Studies Program to W.T.W. and S.A.V.; Restricted Endowment Funds to C.E., S.A.V. and W.T.W.; postdoctoral Fellowship to C.E., STRI Internship to E.C.D., NSF DEB-0949602 to S.A.V. and W.T.W. and SENACYT FID10-091 to S.A.V. and W.T.W. We also thank Panama's Authority on the Environment (ANAM), for permission to undertake this research. NR 44 TC 2 Z9 3 U1 8 U2 45 PU INDIAN ACAD SCIENCES PI BANGALORE PA C V RAMAN AVENUE, SADASHIVANAGAR, P B #8005, BANGALORE 560 080, INDIA SN 0011-3891 J9 CURR SCI INDIA JI Curr. Sci. PD JUL 10 PY 2015 VL 109 IS 1 BP 55 EP 61 PG 7 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA CN2JR UT WOS:000358247500015 ER PT J AU Zhang, Y Cao, QS Rubenstein, DI Zang, S Songer, M Leimgruber, P Chu, HJ Cao, J Li, K Hu, DF AF Zhang, Yongjun Cao, Qing S. Rubenstein, Daniel I. Zang, Sen Songer, Melissa Leimgruber, Peter Chu, Hongjun Cao, Jie Li, Kai Hu, Defu TI Water Use Patterns of Sympatric Przewalski's Horse and Khulan: Interspecific Comparison Reveals Niche Differences SO PLOS ONE LA English DT Article ID SOCIAL-ORGANIZATION; ECOLOGY; POPULATION; MONGOLIA; BEHAVIOR; TAKHI AB Acquiring water is essential for all animals, but doing so is most challenging for desert-living animals. Recently Przewalski's horse has been reintroduced to the desert area in China where the last wild surviving member of the species was seen before it vanished from China in the 1960s. Its reintroduction placed it within the range of a close evolutionary relative, the con-generic Khulan. Determining whether or not these two species experience competition and whether or not such competition was responsible for the extinction of Przewalski's horses in the wild over 50 years ago, requires identifying the fundamental and realized niches of both species. We remotely monitored the presence of both species at a variety of water points during the dry season in Kalamaili Nature Reserve, Xinjiang, China. Przewalski's horses drank twice per day mostly during daylight hours at low salinity water sources while Khulans drank mostly at night usually at high salinity water points or those far from human residences. Spatial and temporal differences in water use enables coexistence, but suggest that Przewalski's horses also restrict the actions of Khulan. Such differences in both the fundamental and realized niches were associated with differences in physiological tolerances for saline water and human activity as well as differences in aggression and dominance. C1 [Zhang, Yongjun; Zang, Sen; Chu, Hongjun; Li, Kai; Hu, Defu] Beijing Forestry Univ, Coll Nat Conservat, Beijing, Peoples R China. [Cao, Qing S.; Rubenstein, Daniel I.] Princeton Univ, Dept Ecol & Evolutionary Biol, Princeton, NJ 08544 USA. [Cao, Qing S.; Songer, Melissa; Leimgruber, Peter] Natl Zool Pk, Smithsonian Conservat Biol Inst, Front Royal, VA USA. [Chu, Hongjun] Altai Forestry Bur, Altai, Xinjiang, Peoples R China. [Cao, Jie] Xinjiang Forestry Dept, Wild Horse Breeding Ctr, Urumqi, Xinjiang, Peoples R China. RP Hu, DF (reprint author), Beijing Forestry Univ, Coll Nat Conservat, Beijing, Peoples R China. EM hudf@bjfu.edu.cn RI Leimgruber, Peter/O-1304-2015 OI Leimgruber, Peter/0000-0002-3682-0153 FU National Natural Science Foundation of China [30970545]; National Science Foundation [NSF-IIS-0705311]; Association of Zoos and Aquarium's Conservation Endowment Fund [11-1059] FX National Natural Science Foundation of China (Grant No. 30970545); National Science Foundation (NSF-IIS-0705311); Association of Zoos and Aquarium's Conservation Endowment Fund (Grant No. 11-1059). The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 53 TC 2 Z9 2 U1 1 U2 17 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 JUL 10 PY 2015 VL 10 IS 7 AR e0132094 DI 10.1371/journal.pone.0132094 PG 17 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA CN1FD UT WOS:000358162300091 PM 26161909 ER PT J AU Kristensen, LE Bergin, EA AF Kristensen, Lars E. Bergin, Edwin A. TI TRACING EMBEDDED STELLAR POPULATIONS IN CLUSTERS AND GALAXIES USING MOLECULAR EMISSION: METHANOL AS A SIGNATURE OF THE LOW-MASS END OF THE IMF SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE astrochemistry; ISM: jets and outflows; line: profiles; stars: formation; stars: winds, outflows ID SPATIALLY-RESOLVED CHEMISTRY; STAR-FORMATION RATES; NEARBY GALAXIES; PROTOSTARS; EVOLUTION; OUTFLOWS; CLOUDS; CORE; II.; GAS AB Most low-mass protostars form in clusters, in particular high-mass clusters; however, how low-mass stars form in high-mass clusters and what the mass distribution is are still open questions both in our own Galaxy and elsewhere. To access the population of forming embedded low-mass protostars observationally, we propose using molecular outflows as tracers. Because the outflow emission scales with mass, the effective contrast between low-mass protostars and their high-mass cousins is greatly lowered. In particular, maps of methanol emission at 338.4 GHz (J = 7(0)-6(0) A(+)) in low-mass clusters illustrate that this transition is an excellent probe of the low-mass population. We present here a model of a forming cluster where methanol emission is assigned to every embedded low-mass protostar. The resulting model image of methanol emission is compared to recent ALMA observations toward a high-mass cluster and the similarity is striking: the toy model reproduces observations to better than a factor of two and suggests that approximately 50% of the total flux originates in low-mass outflows. Future fine-tuning of the model will eventually make it a tool for interpreting the embedded low-mass population of distant regions within our own Galaxy and ultimately higher-redshift starburst galaxies, not just for methanol emission but also water and high-J CO. C1 [Kristensen, Lars E.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Bergin, Edwin A.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. RP Kristensen, LE (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM lkristensen@cfa.harvard.edu RI Kristensen, Lars E/F-4774-2011 OI Kristensen, Lars E/0000-0003-1159-3721 NR 30 TC 0 Z9 0 U1 0 U2 2 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 JUL 10 PY 2015 VL 807 IS 2 AR L25 DI 10.1088/2041-8205/807/2/L25 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CM8HC UT WOS:000357938600005 ER PT J AU Thyagarajan, N Jacobs, DC Bowman, JD Barry, N Beardsley, AP Bernardi, G Briggs, F Cappallo, RJ Carroll, P Deshpande, AA de Oliveira-Costa, A Dillon, JS Ewall-Wice, A Feng, L Greenhill, LJ Hazelton, BJ Hernquist, L Hewitt, JN Hurley-Walker, N Johnston-Hollitt, M Kaplan, DL Kim, HS Kittiwisit, P Lenc, E Line, J Loeb, A Lonsdale, CJ McKinley, B McWhirter, SR Mitchell, DA Morales, MF Morgan, E Neben, AR Oberoi, D Offringa, AR Ord, SM Paul, S Pindor, B Pober, JC Prabu, T Procopio, P Riding, J Shankar, NU Sethi, SK Srivani, KS Subrahmanyan, R Sullivan, IS Tegmark, M Tingay, SJ Trott, CM Wayth, RB Webster, RL Williams, A Williams, CL Wyithe, JSB AF Thyagarajan, Nithyanandan Jacobs, Daniel C. Bowman, Judd D. Barry, N. Beardsley, A. P. Bernardi, G. Briggs, F. Cappallo, R. J. Carroll, P. Deshpande, A. A. de Oliveira-Costa, A. Dillon, Joshua S. Ewall-Wice, A. Feng, L. Greenhill, L. J. Hazelton, B. J. Hernquist, L. Hewitt, J. N. Hurley-Walker, N. Johnston-Hollitt, M. Kaplan, D. L. Kim, Han-Seek Kittiwisit, P. Lenc, E. Line, J. Loeb, A. Lonsdale, C. J. McKinley, B. McWhirter, S. R. Mitchell, D. A. Morales, M. F. Morgan, E. Neben, A. R. Oberoi, D. Offringa, A. R. Ord, S. M. Paul, Sourabh Pindor, B. Pober, J. C. Prabu, T. Procopio, P. Riding, J. Shankar, N. Udaya Sethi, Shiv K. Srivani, K. S. Subrahmanyan, R. Sullivan, I. S. Tegmark, M. Tingay, S. J. Trott, C. M. Wayth, R. B. Webster, R. L. Williams, A. Williams, C. L. Wyithe, J. S. B. TI CONFIRMATION OF WIDE-FIELD SIGNATURES IN REDSHIFTED 21 cm POWER SPECTRA SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE cosmology: observations; dark ages, reionization, first stars; large-scale structure of universe; methods: statistical; radio continuum: galaxies; techniques: interferometric ID MURCHISON WIDEFIELD ARRAY; CENTIMETER FLUCTUATIONS; INTERGALACTIC MEDIUM; DARK-AGES; 150 MHZ; REIONIZATION; EPOCH; FOREGROUNDS; EMISSION; 21-CM AB We confirm our recent prediction of the "pitchfork" foreground signature in power spectra of high-redshift 21 cm measurements where the interferometer is sensitive to large-scale structure on all baselines. This is due to the inherent response of a wide-field instrument and is characterized by enhanced power from foreground emission in Fourier modes adjacent to those considered to be the most sensitive to the cosmological H I signal. In our recent paper, many signatures from the simulation that predicted this feature were validated against Murchison Widefield Array (MWA) data, but this key pitchfork signature was close to the noise level. In this paper, we improve the data sensitivity through the coherent averaging of 12 independent snapshots with identical instrument settings and provide the first confirmation of the prediction with a signal-to-noise ratio > 10. This wide-field effect can be mitigated by careful antenna designs that suppress sensitivity near the horizon. Simple models for antenna apertures that have been proposed for future instruments such as the Hydrogen Epoch of Reionization Array and the Square Kilometre Array indicate they should suppress foreground leakage from the pitchfork by similar to 40 dB relative to the MWA and significantly increase the likelihood of cosmological signal detection in these critical Fourier modes in the three-dimensional power spectrum. C1 [Thyagarajan, Nithyanandan; Jacobs, Daniel C.; Bowman, Judd D.; Kittiwisit, P.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA. [Barry, N.; Beardsley, A. P.; Carroll, P.; Hazelton, B. J.; Morales, M. F.; Pober, J. C.; Sullivan, I. S.] Univ Washington, Dept Phys, Seattle, WA 98195 USA. [Bernardi, G.] SKA SA, ZA-7405 Pinelands, South Africa. [Bernardi, G.] Rhodes Univ, Dept Phys & Elect, ZA-6140 Grahamstown, South Africa. [Bernardi, G.; Greenhill, L. J.; Hernquist, L.; Loeb, A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Briggs, F.; Offringa, A. R.] Australian Natl Univ, Res Sch Astron & Astrophys, Canberra, ACT 2611, Australia. [Cappallo, R. J.; Lonsdale, C. J.; McWhirter, S. R.] MIT, Haystack Observ, Westford, MA 01886 USA. [Deshpande, A. A.; Paul, Sourabh; Prabu, T.; Shankar, N. Udaya; Sethi, Shiv K.; Srivani, K. S.; Subrahmanyan, R.] Raman Res Inst, Bangalore 560080, Karnataka, India. [de Oliveira-Costa, A.; Dillon, Joshua S.; Ewall-Wice, A.; Feng, L.; Hewitt, J. N.; Morgan, E.; Neben, A. R.; Tegmark, M.; Williams, C. L.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Hurley-Walker, N.; Ord, S. M.; Tingay, S. J.; Trott, C. M.; Wayth, R. B.; Williams, A.] Curtin Univ, Int Ctr Radio Astron Res, Perth, WA 6845, Australia. [Johnston-Hollitt, M.] Victoria Univ Wellington, Sch Chem & Phys Sci, Wellington 6140, New Zealand. [Kaplan, D. L.] Univ Wisconsin, Milwaukee, WI 53201 USA. [Kim, Han-Seek; Line, J.; McKinley, B.; Pindor, B.; Procopio, P.; Riding, J.; Webster, R. L.; Wyithe, J. S. B.] Univ Melbourne, Sch Phys, Parkville, Vic 3010, Australia. [Lenc, E.] Univ Sydney, Sydney Inst Astron, Sch Phys, Sydney, NSW 2006, Australia. [Mitchell, D. A.] CASS, Epping, NSW 1710, Australia. [Oberoi, D.] Tata Inst Fundamental Res, Natl Ctr Radio Astrophys, Pune 411007, Maharashtra, India. RP Thyagarajan, N (reprint author), Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA. EM t_nithyanandan@asu.edu RI Wayth, Randall/B-2444-2013; Trott, Cathryn/B-5325-2013; Udayashankar , N/D-4901-2012; Hurley-Walker, Natasha/B-9520-2013; Sethi, Shiv/D-4893-2012; Subrahmanyan, Ravi/D-4889-2012; M, Manjunath/N-4000-2014; Deshpande, Avinash/D-4868-2012; OI Jacobs, Daniel/0000-0002-0917-2269; Thyagarajan, Nithyanandan/0000-0003-1602-7868; Lenc, Emil/0000-0002-9994-1593; Wayth, Randall/0000-0002-6995-4131; Trott, Cathryn/0000-0001-6324-1766; Hurley-Walker, Natasha/0000-0002-5119-4808; M, Manjunath/0000-0001-8710-0730; Wyithe, Stuart/0000-0001-7956-9758; KIM, HANSIK/0000-0002-5507-5769; /0000-0002-0086-7363 FU U.S. National Science Foundation (NSF) [AST-1109257]; NSF Astronomy and Astrophysics Postdoctoral Fellowship [AST-1401708]; NSF Astronomy and Astrophysics Fellowship [AST-1302774]; NSF [AST-0457585, PHY-0835713, CAREER-0847753, AST-0908884]; Australian Research Council [LE0775621, LE0882938]; U.S. Air Force Office of Scientific Research [FA9550-0510247]; Centre for All-sky Astrophysics (an Australian Research Council Centre of Excellence) [CE110001020]; Smithsonian Astrophysical Observatory; MIT School of Science; Raman Research Institute; Australian National University; Victoria University of Wellington (via New Zealand Ministry of Economic Development and an IBM Shared University Research Grant) [MED-E1799]; Australian Federal government via the Commonwealth Scientific and Industrial Research Organisation (CSIRO); National Collaborative Research Infrastructure Strategy, Education Investment Fund; Australia India Strategic Research Fund; Astronomy Australia Limited; NVIDIA at Harvard University; International Centre for Radio Astronomy Research (ICRAR); Joint Venture of Curtin University; University of Western Australia - Western Australian State government FX This work was supported by the U.S. National Science Foundation (NSF) through award AST-1109257. D.C.J. is supported by an NSF Astronomy and Astrophysics Postdoctoral Fellowship under award AST-1401708. J.C.P. is supported by an NSF Astronomy and Astrophysics Fellowship under award AST-1302774. This work makes use of the Murchison Radio-astronomy Observatory, operated by CSIRO. We acknowledge the Wajarri Yamatji people as the traditional owners of the observatory site. Support for the MWA comes from the NSF (awards: AST-0457585, PHY-0835713, CAREER-0847753, and AST-0908884), the Australian Research Council (LIEF grants LE0775621 and LE0882938), the U.S. Air Force Office of Scientific Research (grant FA9550-0510247), and the Centre for All-sky Astrophysics (an Australian Research Council Centre of Excellence funded by grant CE110001020). Support is also provided by the Smithsonian Astrophysical Observatory, the MIT School of Science, the Raman Research Institute, the Australian National University, and the Victoria University of Wellington (via grant MED-E1799 from the New Zealand Ministry of Economic Development and an IBM Shared University Research Grant). The Australian Federal government provides additional support via the Commonwealth Scientific and Industrial Research Organisation (CSIRO), National Collaborative Research Infrastructure Strategy, Education Investment Fund, and the Australia India Strategic Research Fund, and Astronomy Australia Limited, under contract to Curtin University. We acknowledge the iVEC Petabyte Data Store, the Initiative in Innovative Computing and the CUDA Center for Excellence sponsored by NVIDIA at Harvard University, and the International Centre for Radio Astronomy Research (ICRAR), a Joint Venture of Curtin University and The University of Western Australia, funded by the Western Australian State government. NR 50 TC 19 Z9 19 U1 0 U2 5 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 JUL 10 PY 2015 VL 807 IS 2 AR L28 DI 10.1088/2041-8205/807/2/L28 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CM8HC UT WOS:000357938600008 ER PT J AU Trakhtenbrot, B Urry, CM Civano, F Rosario, DJ Elvis, M Schawinski, K Suh, H Bongiorno, A Simmons, BD AF Trakhtenbrot, Benny Urry, C. Megan Civano, Francesca Rosario, David J. Elvis, Martin Schawinski, Kevin Suh, Hyewon Bongiorno, Angela Simmons, Brooke D. TI An over-massive black hole in a typical star-forming galaxy, 2 billion years after the Big Bang SO SCIENCE LA English DT Article ID ACTIVE GALACTIC NUCLEI; HOST GALAXIES; HIGH-REDSHIFT; COSMIC EVOLUTION; STELLAR MASS; GROWTH-RATE; NGC 1277; COEVOLUTION; FIELD; M87 AB Supermassive black holes (SMBHs) and their host galaxies are generally thought to coevolve, so that the SMBH achieves up to about 0.2 to 0.5% of the host galaxy mass in the present day. The radiation emitted from the growing SMBH is expected to affect star formation throughout the host galaxy. The relevance of this scenario at early cosmic epochs is not yet established. We present spectroscopic observations of a galaxy at redshift z = 3.328, which hosts an actively accreting, extremely massive BH, in its final stages of growth. The SMBH mass is roughly one-tenth the mass of the entire host galaxy, suggesting that it has grown much more efficiently than the host, contrary to models of synchronized coevolution. The host galaxy is forming stars at an intense rate, despite the presence of a SMBH-driven gas outflow. C1 [Trakhtenbrot, Benny; Schawinski, Kevin] ETH, Inst Astron, Dept Phys, CH-8093 Zurich, Switzerland. [Urry, C. Megan] Yale Univ, Dept Phys, New Haven, CT 06520 USA. [Urry, C. Megan; Civano, Francesca] Yale Ctr Astron & Astrophys, New Haven, CT 06520 USA. [Urry, C. Megan] Yale Univ, Dept Astron, New Haven, CT 06520 USA. [Civano, Francesca; Elvis, Martin; Suh, Hyewon] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Rosario, David J.] Max Planck Inst Extraterr Phys MPE, D-85741 Garching, Germany. [Suh, Hyewon] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Bongiorno, Angela] INAF Osservatorio Astron Roma, I-00040 Rome, Italy. [Simmons, Brooke D.] Oxford Astrophys, Oxford OX1 3RH, England. RP Trakhtenbrot, B (reprint author), ETH, Inst Astron, Dept Phys, Wolfgang Pauli Str 27, CH-8093 Zurich, Switzerland. EM benny.trakhtenbrot@phys.ethz.ch OI Bongiorno, Angela/0000-0002-0101-6624; Schawinski, Kevin/0000-0001-5464-0888; Simmons, Brooke/0000-0001-5882-3323; Urry, Meg/0000-0002-0745-9792 FU W. M. Keck Foundation; European Southern Observatory (ESO) Telescopes at the La Silla Paranal Observatory under ESO program [179.A-2005]; Swiss National Science Foundation [PP00P2 138979/1]; NASA [GO3-14150C]; NASA Chandra [GO2-13127X] FX The new MOSFIRE 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. We thank M. Kassis and the rest of the staff at the W. M. Keck observatories at Waimea, HI, for their support during the observing run. We 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. Some of the analysis presented here is based on data products from observations made with European Southern Observatory (ESO) Telescopes at the La Silla Paranal Observatory under ESO program ID 179.A-2005 and on data products produced by TERAPIX and the Cambridge Astronomy Survey Unit on behalf of the UltraVISTA consortium. We are grateful to A. Faisst and M. Onodera for their assistance with the acquisition and reduction of the MOSFIRE data. We thank S. Tacchella, J. Woo, and W. Hartley for their assistance with some of the evolutionary calculations. K.S. gratefully acknowledges support from Swiss National Science Foundation Professorship grant PP00P2 138979/1. F.C. acknowledges financial support by the NASA grant GO3-14150C. M.E. acknowledges financial support by the NASA Chandra grant GO2-13127X. B.T. is a Zwicky Fellow at the ETH Zurich. NR 29 TC 16 Z9 16 U1 0 U2 7 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 JUL 10 PY 2015 VL 349 IS 6244 BP 168 EP 171 DI 10.1126/science.aaa4506 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA CM4OM UT WOS:000357664300038 PM 26160942 ER PT J AU Alles, A Buchert, T Al Roumi, F Wiegand, A AF Alles, Alexandre Buchert, Thomas Al Roumi, Fosca Wiegand, Alexander TI Lagrangian theory of structure formation in relativistic cosmology. III. Gravitoelectric perturbation and solution schemes at any order SO PHYSICAL REVIEW D LA English DT Article ID FRIEDMAN-LEMAITRE COSMOLOGIES; NON-LINEAR THEORY; GRAVITATIONAL-INSTABILITY; ZELDOVICH APPROXIMATION; EXPANDING UNIVERSE; NEWTONIAN COSMOLOGY; GENERAL-RELATIVITY; PANCAKE THEORY; WEYL TENSOR; DYNAMICS AB The relativistic generalization of the Newtonian Lagrangian perturbation theory is investigated. In previous works, the first-order trace solutions that are generated by the spatially projected gravitoelectric part of the Weyl tensor were given together with extensions and applications for accessing the nonperturbative regime. We furnish here construction rules to obtain from Newtonian solutions the gravitoelectric class of relativistic solutions, for which we give the complete perturbation and solution schemes at any order of the perturbations. By construction, these schemes generalize the complete hierarchy of solutions of the Newtonian Lagrangian perturbation theory. C1 [Alles, Alexandre; Buchert, Thomas; Al Roumi, Fosca] Univ Lyon 1, CNRS, Ctr Rech Astrophys Lyon, Observ Lyon,UMR 5574, F-69230 St Genis Laval, France. [Alles, Alexandre; Buchert, Thomas; Al Roumi, Fosca] Ecole Normale Super Lyon, F-69230 St Genis Laval, France. [Wiegand, Alexander] Max Planck Inst Gravitat Phys, Albert Einstein Inst, D-14476 Golm, Germany. [Wiegand, Alexander] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Alles, A (reprint author), Univ Lyon 1, CNRS, Ctr Rech Astrophys Lyon, Observ Lyon,UMR 5574, 9 Ave Charles Andre, F-69230 St Genis Laval, France. EM alexandre.alles@ens-lyon.fr; buchert@ens-lyon.fr; fosca.al_roumi@ens-lyon.fr; jwiegand@cfa.harvard.edu OI Buchert, Thomas/0000-0002-0828-3901 FU Lyon Institute of Origins [ANR-10-LABX-66]; Ecole Doctorale Lyon; French-Bavarian Cooperation Center; BFHZ Munich; DFG [WI 4501/1-1] FX The work of A. A., T. B., and F. R. was conducted within the "Lyon Institute of Origins" under Grant No. ANR-10-LABX-66. A. A. and F. R. acknowledge support by the Ecole Doctorale Lyon. T. B. and F. R. acknowledge student exchange support from the French-Bavarian Cooperation Center, BFHZ Munich http://www.bayern-france.org/. A. W. acknowledges the hospitality of the Harvard CfA where part of this work was done. Part of the work of A. W. was supported by the German research organization DFG, Grant No. WI 4501/1-1. Special thanks go to Leo Brunswic, Martin Kerscher, Mikolaj Korzynski, Pierre Mourier, Slava Mukhanov, Jan Ostrowski, Cornelius Rampf, Herbert Wagner, and the referee for fruitful discussions and valuable remarks. NR 46 TC 6 Z9 6 U1 0 U2 2 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 1550-7998 EI 1550-2368 J9 PHYS REV D JI Phys. Rev. D PD JUL 9 PY 2015 VL 92 IS 2 AR 023512 DI 10.1103/PhysRevD.92.023512 PG 18 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA CM4FF UT WOS:000357639100003 ER PT J AU Baldeck, CA Asner, GP Martin, RE Anderson, CB Knapp, DE Kellner, JR Wright, SJ AF Baldeck, Claire A. Asner, Gregory P. Martin, Robin E. Anderson, Christopher B. Knapp, David E. Kellner, James R. Wright, S. Joseph TI Operational Tree Species Mapping in a Diverse Tropical Forest with Airborne Imaging Spectroscopy SO PLOS ONE LA English DT Article ID VECTOR DOMAIN DESCRIPTION; REMOTE-SENSING IMAGES; HYPERSPECTRAL DATA; LIDAR DATA; AERIAL-PHOTOGRAPHY; CLASSIFICATION; DISCRIMINATION; IDENTIFICATION; LEAF; BIODIVERSITY AB Remote identification and mapping of canopy tree species can contribute valuable information towards our understanding of ecosystem biodiversity and function over large spatial scales. However, the extreme challenges posed by highly diverse, closed-canopy tropical forests have prevented automated remote species mapping of non-flowering tree crowns in these ecosystems. We set out to identify individuals of three focal canopy tree species amongst a diverse background of tree and liana species on Barro Colorado Island, Panama, using airborne imaging spectroscopy data. First, we compared two leading singleclass classification methods-binary support vector machine (SVM) and biased SVM-for their performance in identifying pixels of a single focal species. From this comparison we determined that biased SVM was more precise and created a multi-species classification model by combining the three biased SVM models. This model was applied to the imagery to identify pixels belonging to the three focal species and the prediction results were then processed to create a map of focal species crown objects. Crown-level cross-validation of the training data indicated that the multi-species classification model had pixel-level producer's accuracies of 94-97% for the three focal species, and field validation of the predicted crown objects indicated that these had user's accuracies of 94-100%. Our results demonstrate the ability of high spatial and spectral resolution remote sensing to accurately detect non-flowering crowns of focal species within a diverse tropical forest. We attribute the success of our model to recent classification and mapping techniques adapted to species detection in diverse closed-canopy forests, which can pave the way for remote species mapping in a wider variety of ecosystems. C1 [Baldeck, Claire A.; Asner, Gregory P.; Martin, Robin E.; Anderson, Christopher B.; Knapp, David E.] Carnegie Inst Sci, Dept Plant Biol, Dept Global Ecol, Stanford, CA 94305 USA. [Kellner, James R.] Brown Univ, Dept Ecol & Evolutionary Biol, Providence, RI 02912 USA. [Wright, S. Joseph] Smithsonian Trop Res Inst, Washington, DC USA. RP Baldeck, CA (reprint author), Carnegie Inst Sci, Dept Plant Biol, Dept Global Ecol, 290 Panama St, Stanford, CA 94305 USA. EM cbaldeck@carnegiescience.edu RI Wright, Stuart/M-3311-2013 OI Wright, Stuart/0000-0003-4260-5676 FU Avatar Alliance Foundation; Gordon and Betty Moore Foundation; John D. and Catherine R. MacArthur Foundation; Grantham Foundation for the Protection of the Environment; W. M. Keck Foundation; Margaret A. Cargill Foundation FX This study has been supported by the Avatar Alliance Foundation, Gordon and Betty Moore Foundation, John D. and Catherine R. MacArthur Foundation, Grantham Foundation for the Protection of the Environment, W. M. Keck Foundation, Margaret A. Cargill Foundation, Mary Anne Nyburg Baker and G. Leonard Baker Jr., and William R. Hearst III. There are no grant numbers or URLs. The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 58 TC 8 Z9 8 U1 10 U2 40 PU PUBLIC LIBRARY SCIENCE PI SAN FRANCISCO PA 1160 BATTERY STREET, STE 100, SAN FRANCISCO, CA 94111 USA SN 1932-6203 J9 PLOS ONE JI PLoS One PD JUL 8 PY 2015 VL 10 IS 7 AR e0118403 DI 10.1371/journal.pone.0118403 PG 21 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA CN1EJ UT WOS:000358159700001 PM 26153693 ER PT J AU Todaro, MA Dal Zotto, M Leasi, F AF Todaro, M. Antonio Dal Zotto, Matteo Leasi, Francesca TI An Integrated Morphological and Molecular Approach to the Description and Systematisation of a Novel Genus and Species of Macrodasyida (Gastrotricha) SO PLOS ONE LA English DT Article ID ITALIAN MARINE GASTROTRICHA; RIBOSOMAL-RNA GENES; NERVOUS-SYSTEM; PAUCITUBULATINA GASTROTRICHA; DACTYLOPODOLA-BALTICA; MEDITERRANEAN SEA; MUSCULAR SYSTEM; CHAETONOTIDA; PHYLOGENY; FRESH AB Background Gastrotricha systematics is in a state of flux mainly due to the conflicts between cladistic studies base on molecular markers and the classical systematisation based on morphological traits. In sandy samples from Thailand, we found numerous macrodasyidan gastrotrichs belonging to an undescribed species of difficult taxonomic affiliation. The abundance and original nature of the specimens prompted us to undertake a deep survey of both morphological and molecular traits aiming at a reliable systematisation of the new taxon. Methodology/Principal Findings Using several microscopical techniques we investigated the external and internal anatomy, including the muscular and nervous systems of the new species. Additional specimens were used to obtain the 18S rRNA gene sequence; molecular data was analysed cladistically in conjunction with data from additional species belonging to the near complete Macrodasyida taxonomic spectrum. Specimens are vermiform, up to 806 mu m in total length, and show a well-defined head equipped with peculiar leaf-like sensorial organs and a single-lobed posterior end. The adhesive apparatus includes anterior, ventrolateral, dorsal and posterior tubes. Pharynx is about 1/4 of the total length and shows pores at its posterior 3/4. Adult specimens exhibit maturing eggs and a bulky, muscular caudal organ, but do not show sperm nor the frontal organ. Musculature and nervous system organisation resemble the usual macrodasyidan plan; however, the somatic circular muscles of the intestinal region surround all other muscular components and a third FMRFamide-IR commissure ventral to the pharyngo-intestinal junction appear to be an autoapomorphic traits of the new species. Conclusions/Significance While the anatomical characteristics of the Asian specimens appear so unique to grant the establishment of a new taxon, for which the name Thaidasys tongiorgii gen. et sp. nov. is proposed, the result of phylogenetic analyses based on the 18S rRNA gene unites the new genus with the family Macrodasyidae. C1 [Todaro, M. Antonio; Dal Zotto, Matteo] Univ Modena & Reggio Emilia, Dept Life Sci, Modena, Italy. [Dal Zotto, Matteo] Consorzio Interuniv Ctr Biol Marina & Ecol Applic, Livorno, Italy. [Leasi, Francesca] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA. RP Todaro, MA (reprint author), Univ Modena & Reggio Emilia, Dept Life Sci, Modena, Italy. EM antonio.todaro@unimore.it RI LEASI, FRANCESCA/E-4361-2017 FU TIOME project (MAT, PI) FX Funding for this research was provided by the TIOME project (MAT, PI); the study falls within the framework of the strategic research line Environment, food and health (WP2) - of UNIMORE. The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 65 TC 4 Z9 5 U1 2 U2 5 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 JUL 8 PY 2015 VL 10 IS 7 AR e0130278 DI 10.1371/journal.pone.0130278 PG 32 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA CN1EJ UT WOS:000358159700027 PM 26153694 ER PT J AU Borregaard, J Komar, P Kessler, EM Lukin, MD Sorensen, AS AF Borregaard, J. Komar, P. Kessler, E. M. Lukin, M. D. Sorensen, A. S. TI Long-distance entanglement distribution using individual atoms in optical cavities SO PHYSICAL REVIEW A LA English DT Article ID QUANTUM COMMUNICATION; NOISY CHANNELS; LINEAR OPTICS; CRYPTOGRAPHY; PURIFICATION; ENSEMBLES; REPEATERS; SECURITY; NETWORK; STATES AB Individual atoms in optical cavities can provide an efficient interface between stationary qubits and flying qubits (photons), which is an essential building block for quantum communication. Furthermore, cavity-assisted controlled-not (CNOT) gates can be used for swapping entanglement to long distances in a quantum repeater setup. Nonetheless, dissipation introduced by the cavity during the CNOT may increase the experimental difficulty in obtaining long-distance entanglement distribution using these systems. We analyze and compare a number of cavity-based repeater schemes combining various entanglement generation schemes and cavity-assisted CNOT gates. We find that a scheme, where high-fidelity entanglement is first generated in a two-photon detection scheme and then swapped to long distances using a recently proposed heralded controlled-Z (CZ) gate, exhibits superior performance compared to the other schemes. The heralded gate moves the effect of dissipation from the fidelity to the success probability of the gate thereby enabling high-fidelity entanglement swapping. As a result, high-rate entanglement distribution can be achieved over long distances even for low cooperativities of the atom-cavity systems. This high-fidelity repeater is shown to outperform the other cavity-based schemes by up to two orders of magnitude in the rate for realistic parameters and large distances (1000 km). C1 [Borregaard, J.; Sorensen, A. S.] Univ Copenhagen, Niels Bohr Inst, DK-2100 Copenhagen O, Denmark. [Borregaard, J.; Komar, P.; Kessler, E. M.; Lukin, M. D.] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. [Kessler, E. M.] Harvard Smithsonian Ctr Astrophys, ITAMP, Cambridge, MA 02138 USA. RP Borregaard, J (reprint author), Univ Copenhagen, Niels Bohr Inst, Blegdamsvej 17, DK-2100 Copenhagen O, Denmark. RI Sorensen, Anders/L-1868-2013 OI Sorensen, Anders/0000-0003-1337-9163 FU Lundbeck Foundation; Carlsberg Foundation; NSF; CUA; DARPA; AFOSR MURI; ARL; European Research Council under the European Unions Seventh Framework Programme (FP) through SIQS [600645]; ERC Grant QIOS [306576] FX A.S. would like to thank Naomi H. Nickerson for helpful discussions. We gratefully acknowledge the support from the Lundbeck Foundation, the Carlsberg Foundation, NSF, CUA, DARPA, AFOSR MURI, and ARL. The research leading to these results has also received funding from the European Research Council under the European Unions Seventh Framework Programme (FP/2007-2003) through SIQS (Grant No. 600645) and ERC Grant QIOS (Grant No. 306576). NR 37 TC 3 Z9 3 U1 1 U2 19 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 1050-2947 EI 1094-1622 J9 PHYS REV A JI Phys. Rev. A PD JUL 8 PY 2015 VL 92 IS 1 AR 012307 DI 10.1103/PhysRevA.92.012307 PG 15 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA CM4DI UT WOS:000357634000003 ER PT J AU Aiello, BR Iriarte-Diaz, J Blob, RW Butcher, MT Carrano, MT Espinoza, NR Main, RP Ross, CF AF Aiello, B. R. Iriarte-Diaz, J. Blob, R. W. Butcher, M. T. Carrano, M. T. Espinoza, N. R. Main, R. P. Ross, C. F. TI Bone strain magnitude is correlated with bone strain rate in tetrapods: implications for models of mechanotransduction SO PROCEEDINGS OF THE ROYAL SOCIETY B-BIOLOGICAL SCIENCES LA English DT Article DE bone mechanotransduction; bone fluid flow; bone strain; strain rate ID FLOW-INDUCED MECHANOTRANSDUCTION; SKELETAL STRUCTURAL ADAPTATIONS; MECHANICAL USAGE SATMU; REDEFINING WOLFF LAW; IN-VIVO STRAINS; MOTOR UNITS; TERRESTRIAL LOCOMOTION; CORTICAL BONE; PERICELLULAR MATRIX; PSEUDEMYS-CONCINNA AB Hypotheses suggest that structural integrity of vertebrate bones is maintained by controlling bone strain magnitude via adaptive modelling in response to mechanical stimuli. Increased tissue-level strain magnitude and rate have both been identified as potent stimuli leading to increased bone formation. Mechanotransduction models hypothesize that osteocytes sense bone deformation by detecting fluid flow-induced drag in the bone's lacunar-canalicular porosity. This model suggests that the osteocyte's intracellular response depends on fluid-flow rate, a product of bone strain rate and gradient, but does not provide a mechanism for detection of strain magnitude. Such a mechanism is necessary for bone modelling to adapt to loads, because strain magnitude is an important determinant of skeletal fracture. Using strain gauge data from the limb bones of amphibians, reptiles, birds and mammals, we identified strong correlations between strain rate and magnitude across clades employing diverse locomotor styles and degrees of rhythmicity. The breadth of our sample suggests that this pattern is likely to be a common feature of tetrapod bone loading. Moreover, finding that bone strain magnitude is encoded in strain rate at the tissue level is consistent with the hypothesis that it might be encoded in fluid-flow rate at the cellular level, facilitating bone adaptation via mechanotransduction. C1 [Aiello, B. R.; Ross, C. F.] Univ Chicago, Dept Organismal Biol & Anat, Chicago, IL 60637 USA. [Iriarte-Diaz, J.] Univ Illinois, Dept Oral Biol, Chicago, IL 60612 USA. [Blob, R. W.; Espinoza, N. R.] Clemson Univ, Dept Biol Sci, Clemson, SC 29634 USA. [Butcher, M. T.] Youngstown State Univ, Dept Biol Sci, Youngstown, OH 44555 USA. [Carrano, M. T.] Smithsonian Inst, Dept Paleobiol, Washington, DC 20013 USA. [Main, R. P.] Purdue Univ, Coll Vet Med, Dept Basic Med Sci, W Lafayette, IN 47907 USA. [Main, R. P.] Purdue Univ, Weldon Sch Biomed Engn, W Lafayette, IN 47907 USA. RP Aiello, BR (reprint author), Univ Chicago, Dept Organismal Biol & Anat, 1025 E 57Th St, Chicago, IL 60637 USA. EM braiello@uchicago.edu; rossc@uchicago.edu RI Carrano, Matthew/C-7601-2011; Iriarte-Diaz, Jose/A-2486-2008 OI Carrano, Matthew/0000-0003-2129-1612; Iriarte-Diaz, Jose/0000-0003-3566-247X FU National Science Foundation [DGE-0903637, IOB-0517340, BCS-010913] FX This material is based on work supported by the National Science Foundation under grants DGE-0903637 (an Integrative Graduate Education and Research Traineeship supporting B.R.A), IOB-0517340 (to R.W.B.) and BCS-010913 (to C.F.R.). NR 76 TC 1 Z9 1 U1 2 U2 9 PU ROYAL SOC PI LONDON PA 6-9 CARLTON HOUSE TERRACE, LONDON SW1Y 5AG, ENGLAND SN 0962-8452 EI 1471-2954 J9 P ROY SOC B-BIOL SCI JI Proc. R. Soc. B-Biol. Sci. PD JUL 7 PY 2015 VL 282 IS 1810 AR 20150321 DI 10.1098/rspb.2015.0321 PG 8 WC Biology; Ecology; Evolutionary Biology SC Life Sciences & Biomedicine - Other Topics; Environmental Sciences & Ecology; Evolutionary Biology GA CM5HY UT WOS:000357719500009 ER PT J AU de Silva, P Miranda, R Bernal, XE AF de Silva, Priyanka Miranda, Roberto Bernal, Ximena E. TI First report of mite parasitization in frog-biting midges (Corethrella species) SO INTERNATIONAL JOURNAL OF ACAROLOGY LA English DT Article DE frog-biting midges; Corethrellidae; Hydrachnidae; mite parasitism ID LARVAL WATER MITES; MATING SUCCESS; ACARINE PARASITES; SEX BIASES; ARRENURUS; DIPTERA; MOSQUITOS; CULICIDAE; ODONATA; ECTOPARASITISM AB Water mites (Acari: Hydrachnidiae) were collected from males of frog-biting midges (Corethrellidae) in Gamboa, Panama. All Corethrella squamifemora males collected were parasitized with water mites. The mites were attached to the soft tissues of the thoracic region of the midges. No mites were found on female frog-biting midges of the same species. This study is the first report of mite parasitization in frog-biting midges. C1 [de Silva, Priyanka] Univ Peradeniya, Fac Sci, Dept Zool, Peradeniya, Sri Lanka. [Miranda, Roberto] Inst Conmemorat Gorgas Estudios Salud, Entomol Med, Calidonia Panama, Panama. [Bernal, Ximena E.] Purdue Univ, Dept Biol Sci, W Lafayette, IN 47907 USA. [Bernal, Ximena E.] Smithsonian Trop Res Inst, Balboa, Panama. RP de Silva, P (reprint author), Univ Peradeniya, Fac Sci, Dept Zool, Peradeniya, Sri Lanka. EM depriyanka@pdn.ac.lk; mirandarjc@gmail.com; xbernal@purdue.edu FU National Science Foundation, Directorate for Biological Sciences [1433990] FX This work was supported by the National Science Foundation, Directorate for Biological Sciences [IOS#1433990]. NR 36 TC 0 Z9 0 U1 1 U2 4 PU TAYLOR & FRANCIS INC PI PHILADELPHIA PA 530 WALNUT STREET, STE 850, PHILADELPHIA, PA 19106 USA SN 0164-7954 EI 1945-3892 J9 INT J ACAROL JI Int. J. Acarol. PD JUL 4 PY 2015 VL 41 IS 5 BP 389 EP 392 DI 10.1080/01647954.2015.1046922 PG 4 WC Entomology SC Entomology GA CP2KE UT WOS:000359705100003 ER PT J AU Wegner, G Onofrio, R AF Wegner, Gary A. Onofrio, Roberto TI Higgs shifts from electron-positron annihilations near neutron stars SO EUROPEAN PHYSICAL JOURNAL C LA English DT Article ID GAMMA-RAY BURSTS; KONUS EXPERIMENT DATA; HIGH-RESOLUTION SPECTROSCOPY; GALACTIC-CENTER REGION; RADIATION; CYCLOTRON; MODEL; MASS; SPECTRUM; FEATURES AB We discuss the potential for using neutron stars to determine bounds on the Higgs-Kretschmann coupling by looking at peculiar shifts in gamma-ray spectroscopic features. In particular, we reanalyze multiple lines observed in GRB781119 detected by two gamma-ray spectrometers, and derive an upper bound on the Higgs-Kretschmann coupling that is much more constraining than the one recently obtained from white dwarfs. This calls for targeted analyses of spectra of gamma-ray bursts from more recent observatories, dedicated searches for differential shifts on electron-positron and proton-antiproton annihilation spectra in proximity of compact sources, and signals of electron and proton cyclotron lines from the same neutron star. C1 [Wegner, Gary A.] Dartmouth Coll, Dept Phys & Astron, Hanover, NH 03755 USA. [Onofrio, Roberto] Univ Padua, Dipartimento Fis & Astron Galileo Galilei, I-35131 Padua, Italy. [Onofrio, Roberto] Harvard Smithsonian Ctr Astrophys, ITAMP, Cambridge, MA 02138 USA. RP Wegner, G (reprint author), Dartmouth Coll, Dept Phys & Astron, 6127 Wilder Lab, Hanover, NH 03755 USA. EM gary.a.wegner@dartmouth.edu; onofrior@gmail.com FU SCOAP3 FX Funded by SCOAP3. NR 74 TC 2 Z9 2 U1 0 U2 2 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 1434-6044 EI 1434-6052 J9 EUR PHYS J C JI Eur. Phys. J. C PD JUL 4 PY 2015 VL 75 IS 7 AR 307 DI 10.1140/epjc/s10052-015-3523-5 PG 7 WC Physics, Particles & Fields SC Physics GA CM1ZT UT WOS:000357479900001 ER PT J AU Opresko, DM AF Opresko, D. M. TI New species of black corals (Cnidaria: Anthozoa: Antipatharia) from New Zealand and adjacent regions SO NEW ZEALAND JOURNAL OF ZOOLOGY LA English DT Article DE Antipathidae; Aphanipathidae; black corals; new species; New Zealand; Schizopathidae; taxonomy ID SOUTHERN FJORDS; POPULATION-STRUCTURE; FIORDENSIS AB Seven new species of antipatharian corals are described from the territorial waters of New Zealand and adjacent regions. Differential diagnoses are given and comparisons are made to related nominal species. Described as new are: Antipathes leptocrada; Antipathes craticulata; Asteriopathes octocrada; Phanopathes zealandica; Tetrapathes latispina; Parantipathes dodecasticha; and Parantipathes robusta.http://zoobank.org/urn:lsid:zoobank.org:pub:DCF9A2BD-63DE-4240-AA4E-0B8BE7E095F1 C1 [Opresko, D. M.] Smithsonian Inst, Dept Invertebrate Zool, US Natl Museum Nat Hist, Washington, DC 20560 USA. RP Opresko, DM (reprint author), Smithsonian Inst, Dept Invertebrate Zool, US Natl Museum Nat Hist, Washington, DC 20560 USA. EM dmopresko@hotmail.com FU New Zealand Foundation for Research, Science and Technology; Ministry of Fisheries; NOAA Satellite Operations Facility; United States Department of Justice (DoJ); DoJ FX Samples from cruises KAH0011, TAN0205 and TAN0413 were supplied by the NIWA Invertebrate Collection and were collected as part of a research programme 'Seamounts: their importance to fisheries and marine ecosystems', undertaken by the NIWA and funded by the former New Zealand Foundation for Research, Science and Technology and with additional funding from the Ministry of Fisheries and NOAA Satellite Operations Facility.; The author also wishes to thank S Cairns, W Keel, C Bright, W Moser and P Greenhall for their assistance during visits to the USNMNH. The photomicrographs were prepared in the SEM Laboratory of the USNMNH; SD Whittaker of the USNMNH kindly assisted in the SEM operation. DM Opresko is a Research Associate of the USNMNH, and gratefully acknowledges that affiliation. Funding for this project was provided, in part, by a United States Department of Justice (DoJ) grant to the Smithsonian Institution. The author is very appreciative of the DoJ's support of black coral research at the Smithsonian. Sincere thanks also go to T Molodtsova and M Bo for reviewing the manuscript and providing many useful comments and suggestions, and to Jonathan Banks and Marie Hodgkinson for their editorial assistance. Permission to use the photo of Antipathes densa (see Fig. 3A) was kindly provided by Nikoletta Helidonis of Bayerischen Akademie der Wissenschaften. NR 31 TC 0 Z9 0 U1 2 U2 4 PU TAYLOR & FRANCIS LTD PI ABINGDON PA 4 PARK SQUARE, MILTON PARK, ABINGDON OX14 4RN, OXON, ENGLAND SN 0301-4223 EI 1175-8821 J9 NEW ZEAL J ZOOL JI N. Z. J. Zool. PD JUL 3 PY 2015 VL 42 IS 3 BP 145 EP 164 DI 10.1080/03014223.2015.1051550 PG 20 WC Zoology SC Zoology GA CX3OI UT WOS:000365608200002 ER PT J AU Deutsch, JI AF Deutsch, James I. TI Stanley Kubrick: new perspectives SO HISTORICAL JOURNAL OF FILM RADIO AND TELEVISION LA English DT Book Review C1 [Deutsch, James I.] Smithsonian Inst, Washington, DC 20560 USA. RP Deutsch, JI (reprint author), Smithsonian Inst, Washington, DC 20560 USA. EM deutschj@si.edu NR 1 TC 0 Z9 0 U1 1 U2 2 PU ROUTLEDGE JOURNALS, TAYLOR & FRANCIS LTD PI ABINGDON PA 4 PARK SQUARE, MILTON PARK, ABINGDON OX14 4RN, OXFORDSHIRE, ENGLAND SN 0143-9685 EI 1465-3451 J9 HIST J FILM RADIO TV JI Hist. J. Film Radio Telev. PD JUL 3 PY 2015 VL 35 IS 3 BP 518 EP 519 DI 10.1080/01439685.2015.1059611 PG 2 WC Film, Radio, Television SC Film, Radio & Television GA CP2IA UT WOS:000359699500009 ER PT J AU Egan, AN Pan, B AF Egan, Ashley N. Pan, Bo TI Resolution of polyphyly in Pueraria (Leguminosae, Papilionoideae): The creation of two new genera, Haymondia and Toxicopueraria, the resurrection of Neustanthus, and a new combination in Teyleria SO PHYTOTAXA LA English DT Article DE classification; Fabaceae; Glycininae; Phaseoleae; taxonomy AB Recent molecular phylogenetic studies (Egan et al., in prep.) have demonstrated widespread polyphyly within the genus Pueraria. A new classification is presented here that delineates monophyletic groups previously considered congeneric with Pueraria. This taxonomic treatment provides several new species combinations and a more natural circumscription of Pueraria by reinstating the genus Neustanthus, transferring one species to Teyleria and establishing two new genera: Haymondia and Toxicopueraria. C1 [Egan, Ashley N.] Smithsonian Inst NMNH, Dept Bot, US Natl Herbarium US, Washington, DC 20560 USA. [Pan, Bo] Chinese Acad Sci, Xishuangbanna Trop Bot Garden, Ctr Integrat Conservat, Mengla 666303, Yunnan, Peoples R China. RP Egan, AN (reprint author), Smithsonian Inst NMNH, Dept Bot, US Natl Herbarium US, MRC 166,10th & Constitut Ave, Washington, DC 20560 USA. EM egana@si.edu FU East Carolina University; Smithsonian Institution; National Science Foundation (NSF) [DEB 1120186/1352217]; Xishuangbanna Tropical Botanical Garden through the Recruitment Program of Foreign Experts [WQ20110491035] FX A.N. Egan thanks the staff and affiliates of the Forest Herbarium, the Royal Thai Forest Department, and the Flora of Thailand Project for help and support in field collection efforts and herbarium access and specimen loans, especially Kongkanda Chayamarit, Rachun Pooma, Sukontip Sirimongkol, Thaveechok Jumruschay, Voradol Chamchumroon, Nannapat Pattharahirantricin, and Rumrada Meeboonya, in no particular order, as well as Xin-Fen Gao and Bo Xu from Chengdu Institute of Biology for aid in field collections in China. Bo Pan thanks Jian-Tao Yin, Shi-Shun Zhou, Yun-Hong Tan, Qiang Liu, Hong Wang, Han Lai, Li Wang from Xishuangbanna Botanical Garden, Jing-Hua Wang from Herbarium of Kunming Institute of Botany, Si-Rong Yi from Chongqing Institute of Medicinal Plants, and Li He from Beijing Forestry University for their support in both herbarium and field work. Illustrations were beautifully provided by Alice Tangerini of the U.S. National Herbarium, Smithsonian Institution. Thanks to Christopher Puttock, a research associate at the Smithsonian Institution, Sue Sherman-Broyles of Cornell University, and Ruth P. Clark of Royal Botanic Gardens, Kew for helpful comments on the manuscript. A.N. Egan was supported in part by funding from East Carolina University, Smithsonian Institution, and the National Science Foundation (NSF DEB 1120186/1352217). Bo Pan was funded by Xishuangbanna Tropical Botanical Garden through the Recruitment Program of Foreign Experts (WQ20110491035). NR 0 TC 1 Z9 1 U1 0 U2 1 PU MAGNOLIA PRESS PI AUCKLAND PA PO BOX 41383, AUCKLAND, ST LUKES 1030, NEW ZEALAND SN 1179-3155 EI 1179-3163 J9 PHYTOTAXA JI Phytotaxa PD JUL 3 PY 2015 VL 218 IS 3 BP 201 EP 226 PG 26 WC Plant Sciences SC Plant Sciences GA CO2YA UT WOS:000359021900001 ER PT J AU Egan, AN Pan, B AF Egan, Ashley N. Pan, Bo TI Pueraria stracheyi, a new synonym to Apios carnea (Fabaceae) SO PHYTOTAXA LA English DT Article DE Leguminosae; taxonomy; India; Sir Richard Strachey; Shuteria AB Pueraria stracheyi has long been recognized as erroneously placed in the genus Pueraria. Here we examined the history behind this collection, past hypotheses concerning its taxonomic affinities, and morphological and ecological comparisons with Shuteria and Apios carnea, wherein we conclude that Pueraria stracheyi represents a synonym of the latter. C1 [Egan, Ashley N.] Smithsonian Inst NMNH, US Natl Herbarium, Dept Bot, Washington, DC 20560 USA. [Pan, Bo] Chinese Acad Sci, Xishuangbanna Trop Bot Garden, Ctr Integrat Conservat, Mengla 666303, Yunnan, Peoples R China. RP Egan, AN (reprint author), Smithsonian Inst NMNH, US Natl Herbarium, Dept Bot, MRC 166,10th & Constitut Ave, Washington, DC 20560 USA. EM egana@si.edu FU East Carolina University; Smithsonian Institution; National Science Foundation [NSF DEB 1120186/1352217]; Xishuangbanna Tropical Botanical Garden through the Recruitment Program of Foreign Experts [WQ20110491035] FX The authors thank the curators and staff of herbaria E, K, and US for access to facilities and collections. A.N. Egan was supported in part by funding from East Carolina University, Smithsonian Institution, and the National Science Foundation (NSF DEB 1120186/1352217). Bo Pan was funded by Xishuangbanna Tropical Botanical Garden through the Recruitment Program of Foreign Experts (WQ20110491035). NR 23 TC 1 Z9 1 U1 0 U2 1 PU MAGNOLIA PRESS PI AUCKLAND PA PO BOX 41383, AUCKLAND, ST LUKES 1030, NEW ZEALAND SN 1179-3155 EI 1179-3163 J9 PHYTOTAXA JI Phytotaxa PD JUL 2 PY 2015 VL 218 IS 2 BP 147 EP 155 DI 10.11646/phytotaxa.218.2.4 PG 9 WC Plant Sciences SC Plant Sciences GA CM7EI UT WOS:000357852800004 ER PT J AU Skog, LE Clark, JL AF Skog, Laurence E. Clark, John L. TI NOVAE GESNERIACEAE NEOTROPICARUM XIX: A third, new species of the elusive Anetanthus found in Guyana SO PHYTOTAXA LA English DT Article DE Biodiversity; Classification; Guyana; Taxonomy AB A new species of Anetanthus (Gesneriaceae) is described from Guyana as A. disjuncta. A discussion of the known species is provided as well as a key to the known taxa. C1 [Skog, Laurence E.] Smithsonian Inst, Dept Bot, Washington, DC 20013 USA. [Clark, John L.] Univ Alabama, Dept Biol Sci, Tuscaloosa, AL 35487 USA. RP Skog, LE (reprint author), Smithsonian Inst, Dept Bot, MRC 166, Washington, DC 20013 USA. EM skogl@si.edu; jlc@ua.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 are grateful to the Biological Diversity of the Guiana Shield Program (Smithsonian Institution's Department of Botany) and especially field collectors H. David Clarke and Terry Henkel for many years of exploratory collecting that resulted in discoveries such as the one published here. We also are grateful for the line drawings prepared by Alice Tangerini, staff illustrator in the Smithsonian Institution's Department of Botany. NR 14 TC 0 Z9 0 U1 0 U2 0 PU MAGNOLIA PRESS PI AUCKLAND PA PO BOX 41383, AUCKLAND, ST LUKES 1030, NEW ZEALAND SN 1179-3155 EI 1179-3163 J9 PHYTOTAXA JI Phytotaxa PD JUL 2 PY 2015 VL 218 IS 2 BP 177 EP 183 DI 10.11646/phytotaxa.218.2.8 PG 7 WC Plant Sciences SC Plant Sciences GA CM7EI UT WOS:000357852800008 ER PT J AU Zhang, WT Shih, CK Labandeira, CC Ren, D AF Zhang, Wei-Ting Shih, Chung-Kun Labandeira, Conrad C. Ren, Dong TI A new taxon of a primitive moth (Insecta: Lepidoptera: Eolepidopterigidae) from the latest Middle Jurassic of northeastern China SO JOURNAL OF PALEONTOLOGY LA English DT Article AB A new genus and species, Aclemus patulus n. gen. n. sp., is described based on a new specimen collected from the latest Middle Jurassic Jiulongshan Formation in Inner Mongolia, China. Based on a combination of characters from this fossil, including a homonomous fore-and hindwing, a 3-branched media vein, wings lacking long cilia on their margins; and a cross-vein absent between subcosta and radius, we establish a new genus assigned to the Eolepidopterigidae. In addition, the diagnosis of Longcapitalis excelsus Zhang, Shih, Labandeira and Ren 2013, is emended based on new fossil material. C1 [Zhang, Wei-Ting] Shijiazhuang Univ Econ, Geosci Museum, Shijiazhuang 050031, Peoples R China. [Zhang, Wei-Ting; Shih, Chung-Kun; Labandeira, Conrad C.; Ren, Dong] Capital Normal Univ, Key Lab Insect Evolut & Environm Changes, Beijing 100048, Peoples R China. [Labandeira, Conrad C.] Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20013 USA. [Labandeira, Conrad C.] Univ Maryland, Dept Entomol, College Pk, MD 20742 USA. RP Zhang, WT (reprint author), Shijiazhuang Univ Econ, Geosci Museum, Shijiazhuang 050031, Peoples R China. EM zhangweitinghao@163.com; chungkun.shih@gmail.com; labandec@si.edu; rendong@mail.cnu.edu.cn FU National Basic Research Program of China (973 Program) [2012CB821906]; National Natural Science Foundation of China [31172143, 31230065, 31272352, 41272006, 41402009]; Project of the Great Wall Scholar and KEY project of the Beijing Municipal Commission of Education [KZ201310028033]; Natural Science Foundation of Hebei Province [D2015403010]; China Geological Survey [1212011120115]; PhD Research Startup Foundation of Shijiazhuang University of Economics [BQ201319] FX This research was supported by the National Basic Research Program of China (973 Program) (grant 2012CB821906), National Natural Science Foundation of China (grants 31172143, 31230065, 31272352, 41272006 and 41402009), Project of the Great Wall Scholar and KEY project of the Beijing Municipal Commission of Education (grant KZ201310028033), Natural Science Foundation of Hebei Province (grant D2015403010), China Geological Survey (grant 1212011120115), and the PhD Research Startup Foundation of Shijiazhuang University of Economics (No. BQ201319). This is contribution 264 of the Evolution of Terrestrial Ecosystems Consortium of the National Museum of Natural History, in Washington, D.C., U.S.A. NR 21 TC 1 Z9 1 U1 1 U2 1 PU CAMBRIDGE UNIV PRESS PI NEW YORK PA 32 AVENUE OF THE AMERICAS, NEW YORK, NY 10013-2473 USA SN 0022-3360 EI 1937-2337 J9 J PALEONTOL JI J. Paleontol. PD JUL PY 2015 VL 89 IS 4 BP 617 EP 621 DI 10.1017/jpa.2015.39 PG 5 WC Paleontology SC Paleontology GA DF5LL UT WOS:000371393100007 ER PT J AU Amaya-Marquez, M Skog, LE Kvist, LP AF Amaya-Marquez, Marisol Skog, Laurence E. Kvist, Lars Peter TI TWO NEW SPECIES AND TWO NEW VARIETIES OF COLUMNEA (GESNERIACEAE) SO CALDASIA LA English DT Article DE Columnea chocoensis; Columnea stilesiana; Columnea ericae; Gesneriaceae; Choco Biogeographical Region ID CLASSIFICATION AB In this paper two new species of Gesneriaceae (genus Columnea) are described and illustrated. Columnea chocoensis is distributed in the Colombian departments of Choco and Valle del Cauca, while its variety, C. chocoensis var. altaquerensis is restricted to the Department of Narino, Colombia. Columnea stilesiana was found in La Serrania de Los Paraguas located in the Cordillera Occidental between the Choco and Valle del Cauca Departments in Colombia. Further, Columnea archidonae is here considered a variety of C. ericae; Columnea ericae var. archidonae is distributed in Colombia and Ecuador, in forests at elevations higher than those in which the typical variety is found. C1 [Amaya-Marquez, Marisol] Univ Nacl Colombia, Inst Ciencias Nat, Bogota, DC, Colombia. [Skog, Laurence E.] Smithsonian Inst, Dept Bot, Washington, DC 20013 USA. [Kvist, Lars Peter] Univ Aarhus, Inst Biol Sci, DK-8000 Aarhus C, Denmark. RP Amaya-Marquez, M (reprint author), Univ Nacl Colombia, Inst Ciencias Nat, Apartado 7495, Bogota, DC, Colombia. EM mamayam@unal.edu.co; skogl@si.edu; lp@hels-gym.dk NR 7 TC 0 Z9 0 U1 1 U2 1 PU INST CIENCIAS NATURALES, MUSEO HISTORIA NATURAL PI BOGOTA PA FAC CIENCIAS, UNIV NACIONAL COLOMBIA, APARTADO 7495, BOGOTA, 00000, COLOMBIA SN 0366-5232 J9 CALDASIA JI Caldasia PD JUL-DEC PY 2015 VL 37 IS 2 BP 233 EP 250 PG 18 WC Plant Sciences; Multidisciplinary Sciences; Zoology SC Plant Sciences; Science & Technology - Other Topics; Zoology GA DB3SC UT WOS:000368430800001 ER PT J AU Furth, DG Savini, V Chaboo, CS AF Furth, David G. Savini, Vilma Chaboo, Caroline S. TI Beetles (Coleoptera) of Peru: A Survey of the Families. Chrysomelidae: Alticinae (Flea Beetles) SO JOURNAL OF THE KANSAS ENTOMOLOGICAL SOCIETY LA English DT Article C1 [Furth, David G.] Smithsonian Inst, Dept Entomol, Natl Museum Nat Hist, Washington, DC 20560 USA. [Savini, Vilma] Cent Univ Venezuela, Muse Inst Zool Agr, Fac Agron, Maracay 2101A, Venezuela. [Chaboo, Caroline S.] Univ Kansas, Div Entomol, Biodivers Inst, Lawrence, KS 66045 USA. RP Chaboo, CS (reprint author), Univ Kansas, Div Entomol, Biodivers Inst, 1501 Crestline Dr,Suite 140, Lawrence, KS 66045 USA. EM cschaboo@ku.edu FU NSF-EPSCoR [66928]; University of Kansas Department of Ecology and Evolutionary Biology-General Research Fund FX We acknowledge NSF-EPSCoR #66928 (PI: CS Chaboo) for supporting the Peru beetle project and the University of Kansas Department of Ecology and Evolutionary Biology-General Research Fund (PI: CS Chaboo) for funding this publication. NR 24 TC 1 Z9 1 U1 0 U2 0 PU KANSAS ENTOMOLOGICAL SOC PI LAWRENCE PA PO BOX 368, LAWRENCE, KS 66044 USA SN 0022-8567 EI 1937-2353 J9 J KANSAS ENTOMOL SOC JI J. Kans. Entomol. Soc. PD JUL PY 2015 VL 88 IS 3 BP 368 EP 374 PG 7 WC Entomology SC Entomology GA DA0QB UT WOS:000367501100008 ER PT J AU Chaboo, CS Staines, CL AF Chaboo, C. S. Staines, C. L. TI Beetles (Coleoptera) of Peru: A Survey of the Families. Chrysomelidae: Cassidinae Gyllenhal sensu lato SO JOURNAL OF THE KANSAS ENTOMOLOGICAL SOCIETY LA English DT Article C1 [Chaboo, C. S.] Univ Kansas, Biodivers Inst, Div Entomol, Lawrence, KS 66045 USA. [Staines, C. L.] Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol, Washington, DC 20013 USA. RP Chaboo, CS (reprint author), Univ Kansas, Biodivers Inst, Div Entomol, 1501 Crestline Dr,Suite 140, Lawrence, KS 66045 USA. EM cschaboo@ku.edu FU NSF-EPSCoR [66928]; University of Kansas' Department of Ecology and Evolutionary Biology-General Research Fund FX We acknowledge NSF-EPSCoR #66928 (PI: CS Chaboo) for supporting the 'Beetles of Peru' project and the University of Kansas' Department of Ecology and Evolutionary Biology-General Research Fund (PI: CS Chaboo) for funding this publication. NR 17 TC 1 Z9 1 U1 0 U2 0 PU KANSAS ENTOMOLOGICAL SOC PI LAWRENCE PA PO BOX 368, LAWRENCE, KS 66044 USA SN 0022-8567 EI 1937-2353 J9 J KANSAS ENTOMOL SOC JI J. Kans. Entomol. Soc. PD JUL PY 2015 VL 88 IS 3 BP 387 EP 398 PG 12 WC Entomology SC Entomology GA DA0QB UT WOS:000367501100012 ER PT J AU Salazar-Porzio, M AF Salazar-Porzio, Margaret TI The ecology of arts and humanities education: Bridging the worlds of universities and museums SO ARTS AND HUMANITIES IN HIGHER EDUCATION LA English DT Article DE Arts and humanities; experiential learning; higher education; mentorship; museums; partnerships; public history AB In recent years, colleges and universities have been talking seriously about civic learning, but other stakeholders, particularly public arts, culture, and humanities institutions, must be part of the conversation in order to create a context for learning that develops the skills of graduates in robust ways that reflect the full promise of liberal education. This piece places museums within the ecology of higher education through the experiences of faculty, curators, and students in one of the most museum-rich regions in the nation, Washington, DC. Students bridge the worlds of higher education and museums as research fellows, interns, and young professionals. Their experiences provide a window into thinking about the roles of faculty and curator mentors and the importance of finding the intersections between higher education and museums in the ecology of arts and humanities learning and practice. C1 [Salazar-Porzio, Margaret] Smithsonian Inst, Natl Museum Amer Hist, Washington, DC 20013 USA. RP Salazar-Porzio, M (reprint author), Smithsonian Inst, 14th St,Constitution Ave,NW MRC 615,POB 37012, Washington, DC 20013 USA. EM salazar-porziom@si.edu NR 41 TC 0 Z9 0 U1 3 U2 3 PU SAGE PUBLICATIONS LTD PI LONDON PA 1 OLIVERS YARD, 55 CITY ROAD, LONDON EC1Y 1SP, ENGLAND SN 1474-0222 EI 1741-265X J9 ARTS HUM HIGH EDUC JI Arts Hum. High. Educ. PD JUL PY 2015 VL 14 IS 3 SI SI BP 274 EP 292 DI 10.1177/1474022215583949 PG 19 WC Education & Educational Research SC Education & Educational Research GA CV3NZ UT WOS:000364167200004 ER PT J AU Coquillon, N Staples, J AF Coquillon, Naomi Staples, James TI Webcasting for Secondary Students: Notes from the Field SO JOURNAL OF MUSEUM EDUCATION LA English DT Article AB This article argues that webcasting holds great potential to connect students to museum content and to their peers while building content knowledge and skills. The authors outline the opportunities and challenges of webcasts for secondary students by discussing their experience with the National Museum of American History's National Youth Summit webcast series. C1 [Coquillon, Naomi] Smithsonians Natl Museum Amer Hist NMAH, Youth & Teacher Programs, Washington, DC 20001 USA. [Staples, James] Cent Audiovisual Branch, Smithsonian, DC USA. RP Coquillon, N (reprint author), Smithsonians Natl Museum Amer Hist NMAH, Youth & Teacher Programs, Washington, DC 20001 USA. NR 7 TC 0 Z9 0 U1 1 U2 2 PU MANEY PUBLISHING PI LEEDS PA STE 1C, JOSEPHS WELL, HANOVER WALK, LEEDS LS3 1AB, W YORKS, ENGLAND SN 1059-8650 EI 2051-6169 J9 J MUS EDUC JI J. Museum Education PD JUL PY 2015 VL 40 IS 2 BP 110 EP 118 PG 9 WC Education & Educational Research SC Education & Educational Research GA CU9YH UT WOS:000363902500004 ER PT J AU Smith, LF Smith, JK Arcand, KK Smith, RK Bookbinder, JA AF Smith, Lisa F. Smith, Jeffrey K. Arcand, Kimberly K. Smith, Randall K. Bookbinder, Jay A. TI Aesthetics and Astronomy: How Museum Labels Affect the Understanding and Appreciation of Deep-Space Images SO CURATOR-THE MUSEUM JOURNAL LA English DT Article ID SCIENCE MUSEUM; PERCEPTION; PAINTINGS AB How can we best communicate to museum visitors the science that underlies the incredible images of space that are generated through the data collected from satellites and observatories? The Aesthetics and Astronomy Group, a collection of astrophysicists, space image developers, science communication experts, and research psychologists, has studied how individuals respond to space-image descriptions when viewing images on websites such as the Astronomy Picture of the Day and the Chandra telescope site. In this article, we turn our attention to the communication of scientific information in museum settings, in particular where the exhibit is comprised solely of images. We developed a traveling exhibition of space images expressly for this purpose, and interviewed 167 visitors to the exhibition at four major science museums. We asked the visitors what types of labels they preferred, what they would like to see in labels, and what impressed them about the images. The results of our efforts are presented here. C1 [Smith, Lisa F.] Univ Otago, Coll Educ, Dunedin, New Zealand. [Smith, Jeffrey K.] Univ Otago, Dunedin, New Zealand. [Smith, Randall K.] Smithsonian Astrophys Observ, Div High Energy Astrophys, Cambridge, MA USA. [Bookbinder, Jay A.] Smithsonian Astrophys Observ, Div High Energy Astrophys, Cambridge, MA USA. RP Smith, LF (reprint author), Univ Otago, Coll Educ, Dunedin, New Zealand. EM lisa.smith@otago.ac.nz; jeffrey.smith@otago.ac.nz; kkowal@cfa.harvard.edu; rsmith@cfa.harvard.edu; jbookbinder@cfa.harvard.edu NR 21 TC 0 Z9 0 U1 2 U2 5 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0011-3069 EI 2151-6952 J9 CURATOR JI Curator PD JUL PY 2015 VL 58 IS 3 BP 283 EP 297 DI 10.1111/cura.12114 PG 15 WC Humanities, Multidisciplinary SC Arts & Humanities - Other Topics GA CU6PV UT WOS:000363655600004 ER PT J AU Chan, S Cope, A AF Chan, Sebastian Cope, Aaron TI Strategies against Architecture: Interactive Media and Transformative Technology at the Cooper Hewitt, Smithsonian Design Museum SO CURATOR-THE MUSEUM JOURNAL LA English DT Article AB After being closed for three years, the Cooper Hewitt, Smithsonian Design Museum reopened at the end of 2014 a transformed museum in a renovated heritage building: Andrew Carnegie's former home on the Upper East Side of New York City. New galleries, a collection that was being rapidly digitized, a new brand, and a desire for new audiences drove the museum to rethink and reposition its role as a design museum. At the core of the new museum is a digital platform, built in-house, that connects collection-and patron-management systems to in-gallery and online experiences. These have allowed the museum to redesign everything from object labels and vitrines to the fundamentals of the "visitor experience." This paper explores in detail the process, the decisions made-and resulting tradeoffs-during each stage of the process. In so doing, it reveals the challenges of collaborating with internal and external capacities, operating internationally with online collaboration tools, and rapid prototyping. C1 [Chan, Sebastian] Smithsonian Design Museum, Cooper Hewitt, Digital & Emerging Media, New York, NY 10128 USA. [Cope, Aaron] Smithsonian Design Museum, Cooper Hewitt, New York, NY USA. RP Chan, S (reprint author), Smithsonian Design Museum, Cooper Hewitt, Digital & Emerging Media, New York, NY 10128 USA. EM seb@freshandnew.org; aaron@aaronland.net NR 33 TC 0 Z9 0 U1 1 U2 3 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0011-3069 EI 2151-6952 J9 CURATOR JI Curator PD JUL PY 2015 VL 58 IS 3 BP 353 EP 368 DI 10.1111/cura.12118 PG 16 WC Humanities, Multidisciplinary SC Arts & Humanities - Other Topics GA CU6PV UT WOS:000363655600008 ER PT J AU Woodman, N AF Woodman, Neal TI Shippingport, Kentucky, is the type locality for the white-footed mouse, Peromyscus leucopus (Rafinesque, 1818) (Mammalia: Rodentia: Cricetidae) SO PROCEEDINGS OF THE BIOLOGICAL SOCIETY OF WASHINGTON LA English DT Article DE Muroidea; Neotominae; systematics; taxonomy AB The white-footed mouse, Musculus leucopus Rafinesque, 1818 (= Peromyscus leucopus), is a common small mammal that is widespread in the eastern and central United States. Its abundance in many habitats renders it ecologically important, and its status as a reservoir for hantavirus and Lyme disease gives the species medical and economic significance. The recognition of two cytotypes and up to 17 morphological subspecies of P. leucopus indicates considerable variation in the species, and to understand this variation, it is important that the nominate subspecies be adequately defined so as to act as a standard for comparison. Relevant to this standard for the white-footed mouse is its type locality, which has generally been accepted to be either the vague "pine barrens of Kentucky'' or the mouth of the Ohio River. Newly assembled information regarding the life and travels of Constantine S. Rafinesque, the North American naturalist who described P. leucopus, establishes that Rafinesque observed this species in July 1818 while visiting Shippingport, Kentucky, which is now within the city limits of Louisville, Jefferson Co., Kentucky. Shippingport is therefore the actual type locality for this species. C1 Smithsonian Inst, Natl Museum Nat Hist, USGS Patuxent Wildlife Res Ctr, Washington, DC 20013 USA. RP Woodman, N (reprint author), Smithsonian Inst, Natl Museum Nat Hist, USGS Patuxent Wildlife Res Ctr, MRC 111,POB 37012, Washington, DC 20013 USA. EM woodmann@si.edu OI Woodman, Neal/0000-0003-2689-7373 NR 39 TC 1 Z9 1 U1 1 U2 7 PU BIOL SOC WASHINGTON PI WASHINGTON PA NAT MUSEUM NAT HIST SMITHSONIAN INST, WASHINGTON, DC 20560 USA SN 0006-324X EI 1943-6327 J9 P BIOL SOC WASH JI Proc. Biol. Soc. Wash. PD JUL PY 2015 VL 128 IS 2 BP 152 EP 163 DI 10.2988/0006-324X-128.2.152 PG 12 WC Biology SC Life Sciences & Biomedicine - Other Topics GA CS8VL UT WOS:000362367500003 ER PT J AU Shockley, FW Thomas, MC AF Shockley, Floyd W. Thomas, Michael C. TI Notes on the taxonomic identity of Trogosita pusillima Mannerheim, 1843, with transfer from Laemophloeidae and synonymy under Holoparamecus depressus Curtis, 1833 (Endomychidae: Merophysiinae) SO PAN-PACIFIC ENTOMOLOGIST LA English DT Editorial Material C1 [Shockley, Floyd W.] Smithsonian Inst, Dept Entomol, Natl Museum Nat Hist, Washington, DC 20013 USA. [Thomas, Michael C.] Florida Dept Agr & Consumer Serv, Florida State Collect Arthropods, Div Plant Ind Entomol, Gainesville, FL 32614 USA. RP Shockley, FW (reprint author), Smithsonian Inst, Dept Entomol, Natl Museum Nat Hist, POB 37012,MRC 165, Washington, DC 20013 USA. EM ShockleyF@si.edu; Michael.Thomas@FreshFromFlorida.com NR 10 TC 0 Z9 0 U1 0 U2 0 PU PACIFIC COAST ENTOMOL SOC PI SAN FRANCISCO PA C/O CALIFORNIA ACADEMY SCIENCES, 875 HOWARD STREET, SAN FRANCISCO, CA 94103-3009 USA SN 0031-0603 EI 2162-0237 J9 PAN-PAC ENTOMOL JI Pan-Pacific Entomol. PD JUL PY 2015 VL 91 IS 3 BP 278 EP 280 PG 3 WC Entomology SC Entomology GA CS8AE UT WOS:000362307300006 ER PT J AU Richardson, DJ Moser, WE Hammond, CI Lazo-Wasem, EA AF Richardson, Dennis J. Moser, William E. Hammond, Charlotte I. Lazo-Wasem, Eric A. TI New Host and Geographic Distribution Records for Glossiphoniid Leeches Associated with Turtles in Southern New England SO COMPARATIVE PARASITOLOGY LA English DT Article DE Placobdella ali; Placobdella hollensis; Helobdella papillata; Helobdella modesta; Helobdella lineata; Chelydra serpentina; Sternotherus odoratus; common snapping turtle; stinkpot turtle; common musk turtle; Massachusetts; Rhode Island; Hirudinida; Hirudinea; Leech; Glossiphoniidae ID MITOCHONDRIAL GENE-SEQUENCES; HIRUDINIDA GLOSSIPHONIIDAE; MOLECULAR CHARACTERIZATION; HELOBDELLA-MODESTA; MORPHOLOGICAL DATA; PHYLOGENY AB During the summer of 2013, collection of glossiphoniid leeches from turtles in southern New England U.S.A. revealed several new host associations and geographic distribution records. Placobdella ali is reported for the first time from Massachusetts and Rhode Island. Placobdella hollensis is reported for the first time from mainland Rhode Island and for the first time from the common snapping turtle (Chelydra serpentina) and the stinkpot turtle or common musk turtle (Sternotherus odoratus). Helobdella papillata and Helobdella modesta were collected from common snapping turtles, and Helobdella lineata was collected from a stinkpot turtle. Data on the frequency of association of Helobdella spp. with aquatic vertebrates suggest that although Helobdella spp. are not parasitic, a symbiotic relationship likely exists between Helobdella spp. and their hosts, the nature of which is yet to be elucidated. C1 [Richardson, Dennis J.; Hammond, Charlotte I.] Quinnipiac Univ, Dept Biol Sci, Hamden, CT 06518 USA. [Moser, William E.] Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, Museum Support Ctr MRC 534, Suitland, MD 20746 USA. [Lazo-Wasem, Eric A.] Yale Univ, Peabody Museum Nat Hist, Div Invertebrate Zool, New Haven, CT 06520 USA. RP Richardson, DJ (reprint author), Quinnipiac Univ, Dept Biol Sci, 275 Mt Carmel Ave, Hamden, CT 06518 USA. EM Dennis.Richardson@quinnipiac.edu; moserw@si.edu; Charlotte.Hammond@quinnipiac.edu; eric.lazo-wasem@yale.edu NR 19 TC 1 Z9 1 U1 1 U2 5 PU HELMINTHOLOGICAL SOC WASHINGTON PI LAWRENCE PA C/O ALLEN PRESS INC, 1041 NEW HAMPSHIRE ST, ACCT# 141866, LAWRENCE, KS 66044 USA SN 1525-2647 EI 1938-2952 J9 COMP PARASITOL JI Comp. Parasitol. PD JUL PY 2015 VL 82 IS 2 BP 240 EP 243 PG 4 WC Parasitology; Zoology SC Parasitology; Zoology GA CR7VT UT WOS:000361560600010 ER PT J AU Condit, R AF Condit, Richard TI Extracting Environmental Benefits from a New Canal in Nicaragua: Lessons from Panama SO PLOS BIOLOGY LA English DT Article ID 21ST-CENTURY AB Biologists have raised objections to a new canal in Nicaragua, but in this Essay I argue that dire predictions of environmental catastrophe are exaggerated. I present an alternative view based on my research experience in Panama, where Canal operations foster forest conservation. Currently in Nicaragua, the rate of forest loss is so rapid that the canal cannot make it worse. Rather, I contend, adoption of international standards in canal construction could lead to net environmental and social benefits for the country. C1 Smithsonian Trop Res Inst, Panama City, Panama. RP Condit, R (reprint author), Smithsonian Trop Res Inst, Panama City, Panama. EM conditr@gmail.com NR 20 TC 5 Z9 5 U1 6 U2 25 PU PUBLIC LIBRARY SCIENCE PI SAN FRANCISCO PA 1160 BATTERY STREET, STE 100, SAN FRANCISCO, CA 94111 USA SN 1545-7885 J9 PLOS BIOL JI PLoS. Biol. PD JUL PY 2015 VL 13 IS 7 AR e1002208 DI 10.1371/journal.pbio.1002208 PG 7 WC Biochemistry & Molecular Biology; Biology SC Biochemistry & Molecular Biology; Life Sciences & Biomedicine - Other Topics GA CQ5BA UT WOS:000360617100020 PM 26214182 ER PT J AU Wurst, C Wann, S Thompson, R Keller, A Maixner, F Allam, A Finch, C Frohlich, B Kaplan, H Lombardi, G Sutherland, L Sutherland, J Watson, L Cox, S Miyamoto, M Narula, J Stewart, A Thomas, G Zink, A AF Wurst, C. Wann, S. Thompson, R. Keller, A. Maixner, F. Allam, A. Finch, C. Frohlich, B. Kaplan, H. Lombardi, G. Sutherland, L. Sutherland, J. Watson, L. Cox, S. Miyamoto, M. Narula, J. Stewart, A. Thomas, G. Zink, A. TI ATHEROSCLEROSIS IN ANCIENT MUMMIFIED HUMAN REMAINS: LINKING GENETIC PREDISPOSITION WITH THE OCCURRENCE OF CALCIFIED PLAQUES SO ATHEROSCLEROSIS LA English DT Meeting Abstract CT 83rd Congress of the European-Atherosclerosis-Society (EAS) CY MAR 22-25, 2015 CL Glasgow, SCOTLAND SP European Atherosclerosis Soc C1 [Wurst, C.; Maixner, F.; Zink, A.] Inst Mummies & Iceman, European Acad Bozen Bolzano, Bolzano, Italy. [Wann, S.] Columbia St Marys Healthcare, Cardiovasc Grp, Milwaukee, WI USA. [Thompson, R.] St Lukes Mid Amer Heart Inst, Cardiol, Kansas City, MO USA. [Keller, A.] Clin Bioinformat, Dept Clin Bioinformat, Saarbrucken, Germany. [Allam, A.] Al Azahr Univ, Cairo, Egypt. [Finch, C.] Univ So Calif, Davis Sch Gerontol, Los Angeles, CA USA. [Frohlich, B.] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA. [Kaplan, H.] Univ New Mexico, Dept Anthropol, Albuquerque, NM 87131 USA. [Lombardi, G.] Univ Peruana Cayetano Heredia, Lima, Peru. [Sutherland, L.] Newport Q3 Diagnost Ctr, Newport Beach, CA USA. [Sutherland, J.] Saddleback Mem Med Ctr, Laguna Hills, CA USA. [Watson, L.] Univ Nacl Autonoma Mexico, Mexico City 04510, DF, Mexico. [Cox, S.] Univ Cambridge, Dept Archeol, Cambridge, England. [Miyamoto, M.] Mission Internal Med Grp, Mission Viejo, CA USA. [Narula, J.] Icahn Sch Med Mt Sinai, Zena & Michael A Wiener Cardiovasc Inst, New York, NY 10029 USA. [Stewart, A.] Univ Ottawa, Inst Heart, John & Jennifer Ruddy Canadian Cardiovasc Genet, Ottawa, ON, Canada. [Thomas, G.] Univ Calif Irvine, Mem Care Heart & Vasc Inst, Long Beach, CA USA. RI Zink, Albert/P-4024-2015 OI Zink, Albert/0000-0002-1461-747X NR 0 TC 0 Z9 0 U1 0 U2 3 PU ELSEVIER IRELAND LTD PI CLARE PA ELSEVIER HOUSE, BROOKVALE PLAZA, EAST PARK SHANNON, CO, CLARE, 00000, IRELAND SN 0021-9150 EI 1879-1484 J9 ATHEROSCLEROSIS JI Atherosclerosis PD JUL PY 2015 VL 241 IS 1 MA EAS-0863 BP E140 EP E140 PG 1 WC Cardiac & Cardiovascular Systems; Peripheral Vascular Disease SC Cardiovascular System & Cardiology GA CP7WS UT WOS:000360100600463 ER PT J AU Loi, ST Trott, CM Murphy, T Cairns, IH Bell, M Hurley-Walker, N Morgan, J Lenc, E Offringa, AR Feng, L Hancock, PJ Kaplan, DL Kudryavtseva, N Bernardi, G Bowman, JD Briggs, F Cappallo, RJ Corey, BE Deshpande, AA Emrich, D Gaensler, BM Goeke, R Greenhill, LJ Hazelton, BJ Johnston-Hollitt, M Kasper, JC Kratzenberg, E Lonsdale, CJ Lynch, MJ McWhirter, SR Mitchell, DA Morales, MF Morgan, E Oberoi, D Ord, SM Prabu, T Rogers, AEE Roshi, A Shankar, NU Srivani, KS Subrahmanyan, R Tingay, SJ Waterson, M Wayth, RB Webster, RL Whitney, AR Williams, A Williams, CL AF Loi, Shyeh Tjing Trott, Cathryn M. Murphy, Tara Cairns, Iver H. Bell, Martin Hurley-Walker, Natasha Morgan, John Lenc, Emil Offringa, A. R. Feng, L. Hancock, P. J. Kaplan, D. L. Kudryavtseva, N. Bernardi, G. Bowman, J. D. Briggs, F. Cappallo, R. J. Corey, B. E. Deshpande, A. A. Emrich, D. Gaensler, B. M. Goeke, R. Greenhill, L. J. Hazelton, B. J. Johnston-Hollitt, M. Kasper, J. C. Kratzenberg, E. Lonsdale, C. J. Lynch, M. J. McWhirter, S. R. Mitchell, D. A. Morales, M. F. Morgan, E. Oberoi, D. Ord, S. M. Prabu, T. Rogers, A. E. E. Roshi, A. Shankar, N. Udaya Srivani, K. S. Subrahmanyan, R. Tingay, S. J. Waterson, M. Wayth, R. B. Webster, R. L. Whitney, A. R. Williams, A. Williams, C. L. TI Power spectrum analysis of ionospheric fluctuations with the Murchison Widefield Array SO RADIO SCIENCE LA English DT Article DE Murchison Widefield Array; ionosphere; power spectrum ID ATMOSPHERIC GRAVITY-WAVES; RADIO-INTERFEROMETER ARRAY; WHISTLER DUCTS; STRONG SCINTILLATIONS; ELECTRIC-FIELDS; F-REGION; 74 MHZ; PLASMASPHERE; DISTURBANCES; CALIBRATION AB Low-frequency, wide field-of-view (FOV) radio telescopes such as the Murchison Widefield Array (MWA) enable the ionosphere to be sampled at high spatial completeness. We present the results of the first power spectrum analysis of ionospheric fluctuations in MWA data, where we examined the position offsets of radio sources appearing in two data sets. The refractive shifts in the positions of celestial sources are proportional to spatial gradients in the electron column density transverse to the line of sight. These can be used to probe plasma structures and waves in the ionosphere. The regional (10-100km) scales probed by the MWA, determined by the size of its FOV and the spatial density of radio sources (typically thousands in a single FOV), complement the global (100-1000km) scales of GPS studies and local (0.01-1km) scales of radar scattering measurements. Our data exhibit a range of complex structures and waves. Some fluctuations have the characteristics of traveling ionospheric disturbances, while others take the form of narrow, slowly drifting bands aligned along the Earth's magnetic field. C1 [Loi, Shyeh Tjing; Murphy, Tara; Cairns, Iver H.; Lenc, Emil; Bernardi, G.; Bowman, J. D.; Cappallo, R. J.; Corey, B. E.; Deshpande, A. A.; Gaensler, B. M.; Greenhill, L. J.; Hazelton, B. J.; Johnston-Hollitt, M.; Kasper, J. C.; Kratzenberg, E.; Lonsdale, C. J.; McWhirter, S. R.; Morales, M. F.; Oberoi, D.; Prabu, T.; Rogers, A. E. E.; Shankar, N. Udaya; Srivani, K. S.; Subrahmanyan, R.; Webster, R. L.; Whitney, A. R.] Univ Sydney, Sch Phys, Sydney Inst Astron, Sydney, NSW 2006, Australia. [Loi, Shyeh Tjing; Trott, Cathryn M.; Murphy, Tara; Bell, Martin; Lenc, Emil; Offringa, A. R.; Hancock, P. J.; Bowman, J. D.; Briggs, F.; Gaensler, B. M.; Mitchell, D. A.; Ord, S. M.; Roshi, A.; Subrahmanyan, R.; Tingay, S. J.; Wayth, R. B.; Webster, R. L.] ARC Ctr Excellence All Sky Astrophys, Sydney, NSW, Australia. [Trott, Cathryn M.; Hurley-Walker, Natasha; Morgan, John; Hancock, P. J.; Kudryavtseva, N.; Cappallo, R. J.; Corey, B. E.; Emrich, D.; Kratzenberg, E.; Lonsdale, C. J.; Lynch, M. J.; McWhirter, S. R.; Ord, S. M.; Rogers, A. E. E.; Tingay, S. J.; Waterson, M.; Wayth, R. B.; Whitney, A. R.; Williams, A.] Curtin Univ, Int Ctr Radio Astron Res, Bentley, WA, Australia. [Bell, Martin; Deshpande, A. A.; Mitchell, D. A.; Prabu, T.; Shankar, N. Udaya; Srivani, K. S.; Subrahmanyan, R.] CSIRO Astron & Space Sci, Epping, NSW, Australia. [Offringa, A. R.; Briggs, F.; Gaensler, B. M.; Waterson, M.] Australian Natl Univ, Res Sch Astron & Astrophys, Canberra, ACT, Australia. [Offringa, A. R.; Hazelton, B. J.; Morales, M. F.] ASTRON Netherlands Inst Radio Astron, Dwingeloo, Netherlands. [Feng, L.; Goeke, R.; Johnston-Hollitt, M.; Morgan, E.; Williams, C. L.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Kaplan, D. L.; Kasper, J. C.] Univ Wisconsin, Dept Phys, Milwaukee, WI USA. [Bernardi, G.; Oberoi, D.] Square Kilometre Array South Africa, Cape Town, South Africa. [Bernardi, G.; Greenhill, L. J.; Kasper, J. C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Bernardi, G.] Rhodes Univ, Dept Phys & Elect, ZA-6140 Grahamstown, South Africa. [Bowman, J. D.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ USA. [Cappallo, R. J.; Corey, B. E.; Kratzenberg, E.; Lonsdale, C. J.; McWhirter, S. R.; Rogers, A. E. E.; Whitney, A. R.] MIT, Haystack Observ, Westford, MA 01886 USA. [Deshpande, A. A.; Prabu, T.; Shankar, N. Udaya; Srivani, K. S.; Subrahmanyan, R.] Raman Res Inst, Bangalore 560080, Karnataka, India. [Gaensler, B. M.] Univ Toronto, Dunlap Inst Astron & Astrophys, Toronto, ON, Canada. [Hazelton, B. J.; Morales, M. F.] Univ Washington, Dept Phys, Seattle, WA 98195 USA. [Johnston-Hollitt, M.] Victoria Univ Wellington, Sch Chem & Phys Sci, Wellington, New Zealand. [Kasper, J. C.] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA. [Oberoi, D.] Tata Inst Fundamental Res, Natl Ctr Radio Astrophys, Pune, Maharashtra, India. [Roshi, A.] Natl Radio Astron Observ, Charlottesville, VA USA. [Webster, R. L.] Univ Melbourne, Sch Phys, Parkville, Vic 3052, Australia. RP Loi, ST (reprint author), Univ Sydney, Sch Phys, Sydney Inst Astron, Sydney, NSW 2006, Australia. EM sloi5113@uni.sydney.edu.au RI Wayth, Randall/B-2444-2013; Trott, Cathryn/B-5325-2013; Udayashankar , N/D-4901-2012; Hurley-Walker, Natasha/B-9520-2013; Emrich, David/B-7002-2013; Subrahmanyan, Ravi/D-4889-2012; M, Manjunath/N-4000-2014; Deshpande, Avinash/D-4868-2012; OI Cairns, Iver/0000-0001-6978-9765; Gaensler, Bryan/0000-0002-3382-9558; Lenc, Emil/0000-0002-9994-1593; Kudryavtseva, Nadia/0000-0002-1372-0942; Hancock, Paul/0000-0002-4203-2946; Wayth, Randall/0000-0002-6995-4131; Trott, Cathryn/0000-0001-6324-1766; Hurley-Walker, Natasha/0000-0002-5119-4808; Emrich, David/0000-0002-4058-1837; M, Manjunath/0000-0001-8710-0730; Loi, Shyeh Tjing/0000-0002-6528-4548; Murphy, Tara/0000-0002-2686-438X FU U.S. National Science Foundation [AST-0457585, PHY-0835713, CAREER-0847753, AST-0908884]; Australian Research Council (LIEF) [LE0775621, LE0882938]; U.S. Air Force Office of Scientic Research [FA9550-0510247]; Centre for All-sky Astrophysics (an Australian Research Council Centre of Excellence) [CE110001020]; Smithsonian Astrophysical Observatory; MIT School of Science; Raman Research Institute; Australian National University; Victoria University of Wellington (New Zealand Ministry of Economic Development) [MED-E1799]; Victoria University of Wellington (IBM Shared University Research grant) [MED-E1799]; Australian Federal government via the National Collaborative Research Infrastructure Strategy; Australian Federal government via the Education Investment Fund; Australian Federal government via the Australia India Strategic Research Fund; Australian Federal government via the Astronomy Australia Limited; NVIDIA at Harvard University; International Centre for Radio Astronomy Research (ICRAR), a Joint Venture of Curtin University; University of Western Australia - Western Australian State government; Australian Research Council D