FN Thomson Reuters Web of Science™ VR 1.0 PT J AU Rigby, JR Bayliss, MB Gladders, MD Sharon, K Wuyts, E Dahle, H Johnson, T Pena-Guerrero, M AF Rigby, J. R. Bayliss, M. B. Gladders, M. D. Sharon, K. Wuyts, E. Dahle, H. Johnson, T. Pena-Guerrero, M. TI C III] EMISSION IN STAR-FORMING GALAXIES NEAR AND FAR SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE galaxies: star formation; gravitational lensing: strong; techniques: spectroscopic ID LYMAN BREAK GALAXIES; SIMILAR-TO 7; WOLF-RAYET GALAXIES; LY-ALPHA EMISSION; LENSED GALAXIES; HIGH-REDSHIFT; REIONIZATION; Z=1.7; YOUNG; METALLICITY AB We measure [C III] 1907, C III] 1909 angstrom emission lines in 11 gravitationally lensed star-forming galaxies at z similar to 1.6-3, finding much lower equivalent widths than previously reported for fainter lensed galaxies. While it is not yet clear what causes some galaxies to be strong C III] emitters, C III] emission is not a universal property of distant star-forming galaxies. We also examine C III] emission in 46 star-forming galaxies in the local universe, using archival spectra from GHRS, FOS, and STIS on HST and IUE. Twenty percent of these local galaxies show strong C III] emission, with equivalent widths < -5 angstrom. Three nearby galaxies show C III] emission equivalent widths as large as the most extreme emitters yet observed in the distant universe; all three are Wolf-Rayet galaxies. At all redshifts, strong C III] emission may pick out low-metallicity galaxies experiencing intense bursts of star formation. Such local C III] emitters may shed light on the conditions of star formation in certain extreme high-redshift galaxies. C1 [Rigby, J. R.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA. [Bayliss, M. B.] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. [Bayliss, M. B.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Gladders, M. D.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. [Gladders, M. D.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Sharon, K.; Johnson, T.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Wuyts, E.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Dahle, H.] Univ Oslo, Inst Theoret Astrophys, NO-0315 Oslo, Norway. [Pena-Guerrero, M.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. RP Rigby, JR (reprint author), NASA, Goddard Space Flight Ctr, Astrophys Sci Div, 8800 Greenbelt Rd, Greenbelt, MD 20771 USA. OI Johnson, Traci/0000-0002-8829-5303 FU NASA [NAS 5-26555]; Research Council of Norway FX This Letter includes data gathered with the 6.5 m Magellan Telescopes located at Las Campanas Observatory, Chile. This research has made use of the NASA/IPAC Extragalactic Database (NED), which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. This Letter includes observations made with the NASA/ESA Hubble Space Telescope and with the International Ultraviolet Explorer, obtained from the Data Archive at the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-26555. J.R. thanks the "First Carnegie Symposium in honor of Leonard Searle." We thank G. Sonneborn and S. Heap for advice regarding IUE spectra. H.D. acknowledges support from the Research Council of Norway. NR 35 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 NOV 20 PY 2015 VL 814 IS 1 AR L6 DI 10.1088/2041-8205/814/1/L6 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CW5KX UT WOS:000365035400006 ER PT J AU Yee, JC AF Yee, Jennifer C. TI LENS MASSES AND DISTANCES FROM MICROLENS PARALLAX AND FLUX SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE gravitational lensing: micro ID SPITZER OBSERVATIONS; SATELLITE MASS; EVENTS; STAR AB I present a novel method for measuring lens masses for microlensing events. By combining a measured lens flux with the microlens parallax pi(E), it is possible to derive the mass of the lens system without knowing the angular size of the Einstein ring, theta(E). This enables mass and distance measurements for single, luminous lenses, as well as binary and planetary lenses without caustic crossings. I discuss applications of this method in the contexts of the Spitzer, Kepler, and WFIRST microlensing missions. C1 [Yee, Jennifer C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Yee, JC (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. FU NASA through the Sagan Fellowship Program FX The author would like to thank Andy Gould for helpful comments and discussion. The author would also like to thank the anonymous referee, Wei Zhu, and Subo Dong for additional input. Work by J.C.Y. was performed under contract with the California Institute of Technology (Caltech)/Jet Propulsion Laboratory (JPL) funded by NASA through the Sagan Fellowship Program executed by the NASA Exoplanet Science Institute. NR 15 TC 4 Z9 4 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 NOV 20 PY 2015 VL 814 IS 1 AR L11 DI 10.1088/2041-8205/814/1/L11 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CW5KX UT WOS:000365035400011 ER PT J AU Zhou, G Bayliss, D Hartman, JD Fulton, BJ Bakos, GA Howard, AW Isaacson, H Marcy, GW Schmidt, BP Brahm, R Jordan, A AF Zhou, G. Bayliss, D. Hartman, J. D. Fulton, B. J. Bakos, G. A. Howard, A. W. Isaacson, H. Marcy, G. W. Schmidt, B. P. Brahm, R. Jordan, A. TI A HIGH OBLIQUITY ORBIT FOR THE HOT-JUPITER HATS-14b TRANSITING A 5400 K STAR SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE planetary systems; planets and satellites: individual (HATS-14b) ID EXOPLANETARY SYSTEM; STELLAR OBLIQUITY; GIANT PLANETS; ECLIPSING BINARIES; TIDAL DISSIPATION; RADIAL-VELOCITIES; SUPER-NEPTUNE; HOST STARS; METALLICITY; MASS AB We report a spin-orbit misalignment for the hot-Jupiter HATS-14b, measuring a projected orbital obliquity of vertical bar lambda vertical bar = 76(-5)(+4) degrees. HATS-14b orbits a high metallicity, 5400 K G dwarf in a relatively short period orbit of 2.8 days. This obliquity was measured via the Rossiter-McLaughlin effect, obtained with observations from Keck-HIRES. The velocities were extracted using a novel technique, optimized for low signal-to-noise spectra, achieving a high precision of 4 m s(-1) point-to-point scatter. However, we caution that our uncertainties may be underestimated. Due to the low rotational velocity of the star, the detection significance is dependent on the v sin i prior that is imposed in our modeling. Based on trends observed in the sample of hot Jupiters with obliquity measurements, it has been suggested that these planets modify the spin axes of their host stars, with an efficiency that depends on the stellar type and orbital period of the system. In this framework, short-period planets around stars with surface convective envelopes, like HATS-14b, are expected to have orbits that are aligned with the spin axes of their host stars. HATS-14b, however, is a significant outlier from this trend, challenging the effectiveness of the tidal realignment mechanism. C1 [Zhou, G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Zhou, G.; Schmidt, B. P.] Australian Natl Univ, Res Sch Astron & Astrophys, Weston, ACT 2611, Australia. [Bayliss, D.] Univ Geneva, Astron Observ, CH-1290 Versoix, Switzerland. [Hartman, J. D.; Bakos, G. A.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. [Fulton, B. J.; Howard, A. W.] Univ Hawaii Manoa, Inst Astron, Honolulu, HI 96822 USA. [Isaacson, H.; Marcy, G. W.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Brahm, R.; Jordan, A.] Pontificia Univ Catolica Chile, Fac Fis, Inst Astrofis, Santiago 7820436, Chile. [Brahm, R.; Jordan, A.] Millennium Inst Astrophys, Santiago, Chile. RP Zhou, G (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM george.zhou@cfa.harvard.edu OI Jordan, Andres/0000-0002-5389-3944; Schmidt, Brian/0000-0001-6589-1287; Bakos, Gaspar/0000-0001-7204-6727; Isaacson, Howard/0000-0002-0531-1073; Hartman, Joel/0000-0001-8732-6166; Fulton, Benjamin/0000-0003-3504-5316 FU ARC Laureate Fellowship Grant [FL0992131] FX Work at the Australian National University is supported by ARC Laureate Fellowship Grant FL0992131. 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. G.Z. thanks helpful discussions with Simon Albrecht. NR 47 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 NOV 20 PY 2015 VL 814 IS 1 AR L16 DI 10.1088/2041-8205/814/1/L16 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CW5KX UT WOS:000365035400016 ER PT J AU Dziki, A Binford, GJ Coddington, JA Agnarsson, I AF Dziki, Austin Binford, Greta J. Coddington, Jonathan A. Agnarsson, Ingi TI Spintharus flavidus in the Caribbean-a 30 million year biogeographical history and radiation of a 'widespread species' SO PEERJ LA English DT Article DE Spintharus; GAARLandia; Theridiidae; Evolution; Caribbean; Adaptive radiation; Dispersal; Zoology; Arachnology ID GAARLANDIA LAND-BRIDGE; MOLECULAR PHYLOGENY; SPIDERS ARANEAE; ENDEMIC RADIATION; DIVERSIFICATION; ISLANDS; MITOCHONDRIAL; COLONIZATION; PALEOGEOGRAPHY; THERIDIIDAE AB The Caribbean island biota is characterized by high levels of endemism, the result of an interplay between colonization opportunities on islands and effective oceanic barriers among them. A relatively small percentage of the biota is represented by 'widespread species,' presumably taxa for which oceanic barriers are ineffective. Few studies have explored in detail the genetic structure of widespread Caribbean taxa. The cobweb spider Spintharus flavidus Hentz, 1850 (Theridiidae) is one of two described Spintharus species and is unique in being widely distributed from northern N. America to Brazil and throughout the Caribbean. As a taxonomic hypothesis, Spintharus "flavidus" predicts maintenance of gene flow among Caribbean islands, a prediction that seems contradicted by known S. flavidus biology, which suggests limited dispersal ability. As part of an extensive survey of Caribbean arachnids (project Car Bio), we conducted the first molecular phylogenetic analysis of S. flavidus with the primary goal of testing the 'widespread species' hypothesis. Our results, while limited to three molecular loci, reject the hypothesis of a single widespread species. Instead this lineage seems to represent a radiation with at least 16 species in the Caribbean region. Nearly all are short range endemics with several distinct mainland groups and others are single island endemics. While limited taxon sampling, with a single specimen from S. America, constrains what we can infer about the biogeographical history of the lineage, clear patterns still emerge. Consistent with limited overwater dispersal, we find evidence for a single colonization of the Caribbean about 30 million years ago, coinciding with the timing of the GAARLandia landbridge hypothesis. In sum, S. "flavidus" is not a single species capable of frequent overwater dispersal, but rather a 30 my old radiation of single island endemics that provides preliminary support for a complex and contested geological hypothesis. C1 [Dziki, Austin; Agnarsson, Ingi] Univ Vermont, Dept Biol, Burlington, VT 05405 USA. [Binford, Greta J.] Lewis & Clark Coll, Dept Biol, Portland, OR 97219 USA. [Coddington, Jonathan A.; Agnarsson, Ingi] Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol, Washington, DC 20560 USA. RP Agnarsson, I (reprint author), Univ Vermont, Dept Biol, Burlington, VT 05405 USA. EM iagnarsson@gmail.com FU National Science Foundation [DEB-1314749, DEB-1050187-1050253]; NSF [DBI-1349205]; Smithsonian Institution SI Barcode Network; UVM APLE grant FX Funding for this work comes from National Science Foundation (DEB-1314749 and DEB-1050187-1050253) to I Agnarsson and G Binford and NSF (DBI-1349205) to D Barrington, I Agnarsson and CW Kilpatrick. Additional funds came from the Smithsonian Institution 2013 SI Barcode Network to JA Coddington and I Agnarsson. Development of this project was further supported by a UVM APLE grant to A Dziki. The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 79 TC 2 Z9 2 U1 1 U2 9 PU PEERJ INC PI LONDON PA 341-345 OLD ST, THIRD FLR, LONDON, EC1V 9LL, ENGLAND SN 2167-8359 J9 PEERJ JI PeerJ PD NOV 19 PY 2015 VL 3 AR e1422 DI 10.7717/peerj.1422 PG 21 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA CX6IC UT WOS:000365803400010 PM 26618089 ER PT J AU Kayal, E Bentlage, B Cartwright, P Yanagihara, AA Lindsay, DJ Hopcroft, RR Collins, AG AF Kayal, Ehsan Bentlage, Bastian Cartwright, Paulyn Yanagihara, Angel A. Lindsay, Dhugal J. Hopcroft, Russell R. Collins, Allen G. TI Phylogenetic analysis of higher-level relationships within Hydroidolina (Cnidaria: Hydrozoa) using mitochondrial genome data and insight into their mitochondrial transcription SO PEERJ LA English DT Article DE Phylomitogenomics; Low-cost multiplexing library preparation; Filifera; Siphonophora; Capitata; Aplanulata; Leptothecata; Mitochondrial gene expression ID PROTEIN-SEQUENCE ALIGNMENTS; TRANSFER-RNA GENES; MOLECULAR PHYLOGENETICS; CHARACTER EVOLUTION; PHYLUM CNIDARIA; RDNA DATA; PROGRAM; MODELS; HYDRA; PERFORMANCE AB Hydrozoans display the most morphological diversity within the phylum Cnidaria. While recent molecular studies have provided some insights into their evolutionary history, sister group relationships remain mostly unresolved, particularly at mid-taxonomic levels. Specifically, within Hydroidolina, the most speciose hydrozoan subclass, the relationships and sometimes integrity of orders are highly unsettled. Here we obtained the near complete mitochondrial sequence of twenty-six hydroidolinan hydrozoan species from a range of sources (DNA and RNA-seq data, long-range PCR). Our analyses confirm previous inference of the evolution of mtDNA in Hydrozoa while introducing a novel genome organization. Using RNA-seq data, we propose a mechanism for the expression of mitochondrial mRNA in Hydroidolina that can be extrapolated to the other medusozoan taxa. Phylogenetic analyses using the full set of mitochondrial gene sequences provide some insights into the order-level relationships within Hydroidolina, including siphonophores as the first diverging clade, a well-supported clade comprised of Leptothecata-Filifera III-IV, and a second clade comprised of Aplanulata-Capitata s.s.-Filifera I-II. Finally, we describe our relatively inexpensive and accessible multiplexing strategy to sequence long-range PCR amplicons that can be adapted to most high-throughput sequencing platforms. C1 [Kayal, Ehsan; Bentlage, Bastian; Collins, Allen G.] Smithsonian Inst, Dept Invertebrate Zool, Washington, DC 20560 USA. [Cartwright, Paulyn] Univ Kansas, Dept Ecol & Evolutionary Biol, Lawrence, KS 66045 USA. [Yanagihara, Angel A.] Univ Hawaii Manoa, John A Burns Sch Med, Dept Trop Med Med Microbiol & Pharmacol, Honolulu, HI 96822 USA. [Lindsay, Dhugal J.] Japan Agcy Marine Earth Sci & Technol JAMSTEC, Yokosuka, Kanagawa, Japan. [Hopcroft, Russell R.] Univ Alaska Fairbanks, Inst Marine Sci, Fairbanks, AK USA. [Collins, Allen G.] Natl Museum Nat Hist, Natl Systemat Lab NOAAs Fisheries Serv, Washington, DC 20560 USA. RP Kayal, E (reprint author), Smithsonian Inst, Dept Invertebrate Zool, Washington, DC 20560 USA. EM kayale@si.edu RI Yanagihara, Angel/O-5664-2016 OI Yanagihara, Angel/0000-0001-6908-8176 FU Smithsonian Institution Peter Buck Predoctoral Grant; National Science Foundation's Assembling the Tree of Life program (DEB) [0829986]; NSF Doctoral Dissertation Improvement Grant [DEB 0910237]; National Oceanic and Atmospheric Administration under UAF [NA13OAR4320056, NA08OAR4320870]; project BOFYGO (from the board of the Danish Centre for Marine Research, DCH); Greenland Climate Research Centre via TGN [6505]; NIH/NIAMS [R01 AR059388] FX This project was mainly funded by a Smithsonian Institution Peter Buck Predoctoral Grant to EK. This work was also supported by the National Science Foundation's Assembling the Tree of Life program (DEB No. 0829986 to R.W. Thacker and A.G.C.). BB wishes to acknowledge an NSF Doctoral Dissertation Improvement Grant (DEB 0910237) that funded the sequencing of Liriope tetraphylla. RRH was funded in part by the National Oceanic and Atmospheric Administration under UAF cooperative agreements NA13OAR4320056 and NA08OAR4320870, and by the project BOFYGO (from the board of the Danish Centre for Marine Research, DCH) and the Greenland Climate Research Centre (project 6505) via TGN. Physalia physalis sequencing was supported by NIH/NIAMS, R01 AR059388 to AY. The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 56 TC 6 Z9 6 U1 3 U2 12 PU PEERJ INC PI LONDON PA 341-345 OLD ST, THIRD FLR, LONDON, EC1V 9LL, ENGLAND SN 2167-8359 J9 PEERJ JI PeerJ PD NOV 19 PY 2015 VL 3 AR e1403 DI 10.7717/peerj.1403 PG 24 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA CX6IC UT WOS:000365803400002 PM 26618080 ER PT J AU McKeon, CS O'Donnell, JL AF McKeon, C. Seabird O'Donnell, James L. TI Variation in partner benefits in a shrimp-sea anemone symbiosis SO PEERJ LA English DT Article DE Symbiosis; Evolutionary ecology; Fitness; Coral reef; Partner benefits; Speciation ID HOST SELECTION; BROOD PARASITE; SPECIALIZATION; PALAEMONIDAE; PEDERSONI; CARIDEA AB Symbiotic interactions, where two species occur in close physical proximity for the majority of the participants' lifespans, may constrain the fitness of one or both of the participants. Host choice could result in lineage divergence in symbionts if fitness benefits vary across the interaction with hosts. Symbiotic interactions are common in the marine environment, particularly in the most diverse marine ecosystems: coral reefs. However, the variation in symbiotic interactions that may drive diversification is poorly understood in marine systems. We measured the fecundity of the symbiotic shrimp Periclimenes yucatanicus on two anemone hosts on coral reefs in Panama, and found that while fecundity varies among host species, this variation is explained largely by host size, not species. This suggests that shrimp on larger hosts may have higher fitness regardless of host species, which in turn could drive selection for host choice, a proposed driver of diversification in this group. C1 [McKeon, C. Seabird] Smithsonian Inst, Natl Museum Nat Hist, Smithsonian Marine Stn, Ft Pierce, FL 34949 USA. [O'Donnell, James L.] Univ Washington, Sch Marine & Environm Affairs, Seattle, WA 98195 USA. RP McKeon, CS (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Smithsonian Marine Stn, Ft Pierce, FL 34949 USA. EM mckeons@si.edu FU Smithsonian Tropical Research Institute; Organization for Tropical Studies through the STRI/OTS; East Carolina University; Rivers Foundation FX We received support from the Smithsonian Tropical Research Institute and the Organization for Tropical Studies through the STRI/OTS scholarships and fellowships. Travel funding was received from East Carolina University and The Rivers Foundation. 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 5 PU PEERJ INC PI LONDON PA 341-345 OLD ST, THIRD FLR, LONDON, EC1V 9LL, ENGLAND SN 2167-8359 J9 PEERJ JI PeerJ PD NOV 19 PY 2015 VL 3 AR e1409 DI 10.7717/peerj.1409 PG 8 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA CX6IC UT WOS:000365803400003 PM 26618082 ER PT J AU Bartel, N Bietenholz, MF Lebach, DE Ransom, RR Ratner, MI Shapiro, II AF Bartel, N. Bietenholz, M. F. Lebach, D. E. Ransom, R. R. Ratner, M. I. Shapiro, I. I. TI VLBI for Gravity Probe B: the guide star, IM Pegasi SO CLASSICAL AND QUANTUM GRAVITY LA English DT Article DE VLBI; astrometry; radio star; IM Pegasi; proper motion; parallax; active galactic nuclei ID ASTROMETRY; HIPPARCOS; POSITION; MISSION AB We review the radio very long baseline interferometry (VLBI) observations of the guide star, IM Peg, and three compact extragalactic reference sources, made in support of the NASA/Stanford gyroscope relativity mission, Gravity Probe B (GP-B). The main goal of the observations was the determination of the proper motion of IM Peg relative to the distant Universe. VLBI observations made between 1997 and 2005 yield a proper motion of IM Peg of -20.83 +/- 0.09 mas yr(-1) in alpha and -27.27 +/- 0.09 mas yr(-1) in delta in a celestial reference frame of extragalactic radio galaxies and quasars virtually identical to the International Celestial Reference Frame 2 (ICRF2). They also yield a parallax for IM Peg of 10.37 +/- 0.07 mas, corresponding to a distance of 96.4 +/- 0.7 pc. The uncertainties are standard errors with statistical and estimated systematic contributions added in quadrature. These results met the pre-launch requirements of the GP-B mission to not discernibly degrade the estimates of the geodetic and frame-dragging effects. C1 [Bartel, N.; Bietenholz, M. F.] York Univ, Dept Phys & Astron, Toronto, ON M3J 1P3, Canada. [Bietenholz, M. F.] Hartebeesthoek Radio Astron Observ, ZA-1740 Krugersdorp, South Africa. [Lebach, D. E.; Ratner, M. I.; Shapiro, I. I.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Ransom, R. R.] Okanagan Coll, Penticton, BC V2A 8E1, Canada. [Ransom, R. R.] Natl Res Council Canada, Herzberg Inst Astrophys, Dominion Radio Astrophys Observ, Penticton, BC V2A 6K3, Canada. RP Bartel, N (reprint author), York Univ, Dept Phys & Astron, 4700 Keele St, Toronto, ON M3J 1P3, Canada. EM bartel@yorku.ca FU NASA from Stanford University; SAO; NASA [NAS 5-26555] FX We thank each of the following people, listed alphabetically, for their contributions of observations and data reductions to our investigations of IM Peg and its sky neighborhood, for providing us with unpublished updated catalog data, and/or for enlightening discussions on various aspects of this research program: S Berdyugina, A Buffington, D Buzasi, N Caldwell, R Campbell, J Chandler, T Dame R Donahue, G Fazio, D Fischer, O Franz, G Gatewood, D Gordon, E Guinan, P Hemenway, A Henden, M Holman, the late J Huchra, P Kalas, G Keiser, J Kolodziejczak, R Kurucz, B Lange, D Latham, J Lederman, J.-F Lestrade, J Lipa, P Luca, S Marsden, H McAlister, D Monet, N Nunes, L Petrov, R Schild, G Torres, WTraub, D Trilling, N Turner, the late H Wendker, and the late C Worley. This research was primarily supported by NASA, through a contract from Stanford University to SAO, with a major subcontract from SAO to York University. We obtained observations made with the 100 m telescope of the Max-Planck-Institut fur Radioastronomie at Effelsberg, with antennas of the National Radio Astronomy Observatory (NRAO), which is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, with antennas of the DSN, operated by JPL/Caltech, under contract with NASA, and with the NASA/ESA Hubble Space Telescope, which is operated by the Association of Universities for Research in Astronomy, under NASA contract NAS 5-26555. We made use of the SAO/NASA Astrophysics Data System Abstract Service, initiated, developed, and maintained at SAO. NR 24 TC 2 Z9 2 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0264-9381 EI 1361-6382 J9 CLASSICAL QUANT GRAV JI Class. Quantum Gravity PD NOV 19 PY 2015 VL 32 IS 22 AR 224021 DI 10.1088/0264-9381/32/22/224021 PG 21 WC Astronomy & Astrophysics; Physics, Multidisciplinary; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA CW9TG UT WOS:000365340500022 ER PT J AU Xu, QQ Qiu, J Jin, JH Zhou, ZK AF Xu, Qingqing Qiu, Jue Jin, Jianhua Zhou, Zhekun TI Eocene Podocarpium (Leguminosae) from South China and its biogeographic implications (vol 6, 938, 2015) SO FRONTIERS IN PLANT SCIENCE LA English DT Correction DE Eocene; Leguminosae; Podocarpium; phytogeography; South China C1 [Xu, Qingqing; Qiu, Jue; Jin, Jianhua] Sun Yat Sen Univ, Sch Life Sci, State Key Lab Biocontrol, Guangzhou 510275, Guangdong, Peoples R China. [Xu, Qingqing; Qiu, Jue; Jin, Jianhua] Sun Yat Sen Univ, Sch Life Sci, Guangdong Prov Key Lab Plant Resources, Guangzhou 510275, Guangdong, Peoples R China. [Xu, Qingqing] Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20560 USA. [Zhou, Zhekun] Chinese Acad Sci, Xishuangbanna Trop Bot Garden, Menglun, Peoples R China. RP Jin, JH (reprint author), Sun Yat Sen Univ, Sch Life Sci, State Key Lab Biocontrol, Guangzhou 510275, Guangdong, Peoples R China. EM lssjjh@mail.sysu.edu.cn; zhouzk@xtbg.ac.cn NR 1 TC 0 Z9 0 U1 2 U2 4 PU FRONTIERS MEDIA SA PI LAUSANNE PA PO BOX 110, EPFL INNOVATION PARK, BUILDING I, LAUSANNE, 1015, SWITZERLAND SN 1664-462X J9 FRONT PLANT SCI JI Front. Plant Sci. PD NOV 17 PY 2015 VL 6 AR 1036 DI 10.3389/fpls.2015.01036 PG 1 WC Plant Sciences SC Plant Sciences GA CY2WD UT WOS:000366268000001 PM 26635854 ER PT J AU Hastings, AK Bloch, JI Jaramillo, CA AF Hastings, Alexander K. Bloch, Jonathan I. Jaramillo, Carlos A. TI A new blunt-snouted dyrosaurid, Anthracosuchus balrogus gen. et sp nov (Crocodylomorpha, Mesoeucrocodylia), from the Palaeocene of Colombia SO HISTORICAL BIOLOGY LA English DT Article DE Dyrosauridae; Crocodylomorpha; Palaeocene; Colombia; Cerrejon; biogeography ID CERREJON FORMATION; AMERICAN ALLIGATOR; CROCODYLIFORM; MOROCCO; AFRICA; OSTEODERMS; REVISION; PHYLOGENY; BOUNDARY; BEHAVIOR AB A new exceptionally brevirostrine dyrosaurid is described from the middle Palaeocene (58-60 million years ago) Cerrejon Formation, northeastern Colombia, based on four partial skulls and associated postcrania. This taxon is unique among dyrosaurids not only in skull shape, but also in having orbital tuberosities, and osteoderms that are dorsoventrally thick and unpitted, a trait otherwise unknown in Crocodylomorpha. Results from a cladistic analysis of Dyrosauridae suggest that the new taxon, together with Cretaceous-Palaeocene Chenanisuchus lateroculi from Africa and Cerrejonisuchus improcerus also from the Cerrejon Formation, are the most basal members of the family. Results from a biogeographic analysis indicate at least three independent dispersals of dyrosaurids from Africa to the New World occurred in the Late Cretaceous or early Palaeocene. Widely set orbits in the new taxon indicate a deviation from surface-based predation, characteristic of other dyrosaurids, to sub-surface predation, as in modern Gavialis. Tooth impressions found on turtle shells recovered from the same locality match well with teeth of the new taxon indicating possible predation.http://www.zoobank.org/urn:lsid:zoobank.org:pub:AB2B24A5-27CC-4D3F-B580-F11F17851CE6 C1 [Hastings, Alexander K.; Bloch, Jonathan I.] Univ Florida, Florida Museum Nat Hist, Gainesville, FL 32611 USA. [Hastings, Alexander K.] Univ Halle Wittenberg, Zent Magazin Nat Wissensch Sammlungen, Geiseltalmuseum, Halle, Saale, Germany. [Jaramillo, Carlos A.] Smithsonian Trop Res Inst, Balboa, Panama. RP Hastings, AK (reprint author), Univ Florida, Florida Museum Nat Hist, Gainesville, FL 32611 USA. EM alexander.hastings@zns.uni-halle.de OI Bloch, Jonathan/0000-0003-1484-6931 FU National Science Foundation [DEB-0733725, DSGC 640179]; Florida Museum of Natural History; Smithsonian Tropical Research Institute; Geological Society of America; Gary S. Morgan Student Research Award; Cerrejon Coal mine FX Funding for research and fieldwork was made possible by the National Science Foundation [grant numbers DEB-0733725 and DSGC 640179], funds from the Florida Museum of Natural History, the Smithsonian Tropical Research Institute Paleobiology Fund, the Geological Society of America Graduate Student Research Grant, the R. Jerry Britt, Jr Paleobiology Award (Florida Museum of Natural History), Gary S. Morgan Student Research Award and the Cerrejon Coal mine. NR 70 TC 4 Z9 4 U1 1 U2 16 PU TAYLOR & FRANCIS LTD PI ABINGDON PA 4 PARK SQUARE, MILTON PARK, ABINGDON OX14 4RN, OXON, ENGLAND SN 0891-2963 EI 1029-2381 J9 HIST BIOL JI Hist. Biol. PD NOV 17 PY 2015 VL 27 IS 8 BP 998 EP 1020 DI 10.1080/08912963.2014.918968 PG 23 WC Biology; Paleontology SC Life Sciences & Biomedicine - Other Topics; Paleontology GA CL8GI UT WOS:000357211600005 ER PT J AU Norrbom, AL Rodriguez, EJ Steck, GJ Sutton, BA Nolazco, N AF Norrbom, Allen L. Rodriguez, Erick J. Steck, Gary J. Sutton, Bruce A. Nolazco, Norma TI New species and host plants of Anastrepha (Diptera: Tephritidae) primarily from Peru and Bolivia SO ZOOTAXA LA English DT Article DE fruit flies; taxonomy; host plants; Neotropical Region AB Twenty-eight new species of Anastrepha are described and illustrated: A. acca (Bolivia, Peru), A. adami (Peru), A. amplidentata (Bolivia, Peru), A. annonae (Peru), A. breviapex (Peru), A. caballeroi (Peru), A. camba (Bolivia, Peru), A. cicra( Bolivia, Peru), A. disjuncta (Peru), A. durantae (Peru), A. echaratiensis (Peru), A. eminens (Peru), A. ericki (Peru), A. gonzalezi (Bolivia, Peru), A. guevarai (Peru), A. gusi (Peru), A. kimi (Colombia, Peru), A. korytkowskii (Bolivia, Peru), A. latilanceola (Bolivia, Peru), A. melanoptera (Peru), A. mollyae (Bolivia, Peru), A. perezi (Peru), A. psidivora (Peru), A. robynae (Peru), A. rondoniensis (Brazil, Peru), A. tunariensis (Bolivia, Peru), A. villosa (Bolivia), and A. zacharyi (Peru). The following host plant records are reported: A. amplidentata from Spondias mombin L. (Anacardiaceae); A. caballeroi from Quararibea malacocalyx A. Robyns & S. Nilsson (Malvaceae); A. annonae from Annona mucosa Jacq. and Annonasp. (Annonaceae); A. durantae from Duranta peruviana Moldenke (Verbenaceae); and A. psidivora from Psidium guajavaL. (Myrtaceae). C1 [Norrbom, Allen L.] ARS, USDA, Smithsonian Inst, Systemat Entomol Lab, Washington, DC 20013 USA. [Rodriguez, Erick J.; Steck, Gary J.; Sutton, Bruce A.] Florida Dept Agr & Consumer Serv, Div Plant Ind Entomol, Gainesville, FL USA. [Nolazco, Norma] Ctr Diagnost Sanidad Vegetal, Serv Nacl Sanidad Agr, La Molina, Peru. RP Norrbom, AL (reprint author), ARS, USDA, Smithsonian Inst, Systemat Entomol Lab, POB 37012,MRC 168, Washington, DC 20013 USA. EM allen.norrbom@ars.usda.gov FU USDA; APHIS; CPHST; IS; [3.0342]; [13-8131-0291-CA] FX The majority of specimens examined in this study were collected through the USDA Farm Bill project "Enhancement of Fruit Fly Larvae Identification and Taxonomy" (Project Coordinator G.J. Steck, ADODR Norman Barr; project numbers 3.0342 (2012) and 13-8131-0291-CA (2013)). All of the authors contributed to the planning of the project and the collection, rearing, and sorting of the samples; the senior author was responsible for the taxonomic decisions and descriptions. We are grateful to Megan MacDowell, Valerie Peterson and Eileen Rosin of ACA, Laura Samaniego, Patrick Campbell, Adrian Tejedor, Yngrid Espinoza, Fernando Araoz, Norma Fernandez and Oswaldo Coycosi of ACCA, Erick Yabar of UNSAAC, and Erika Paliza and Frank Azorsa of CEBIO, whose collaboration was essential to the success of the project. We also sincerely thank the volunteers, students, and contractors who serviced our traps, particularly Tim Perez, Jorge Caballero, Tito Guevara, Marlene "Charito" Choque, Timo Forster, Jeniffer Alvarez Baca, Jonathan Leon Flores, Hugo Roger Ninantay Rivera, Wendy Coaquira, and Nicolas Castro. The following curators and institutions also kindly loaned or provided specimens for study: Jere Schweikert and Paul H. Arnaud, Jr. (CAS), Juan Jose Lagrava Sanchez and Elizabeth Quisberth (DSASC), Emilio Arevalo Penaranda (ICAB), Manuel Zumbado (INBio), Luis Joly (IZAM), Gerardo Lamas (MHNJP), Julieta Ledesma (MNKM), Freddy Colque (SENASAG), Uwe Kallweit (SMT), and J. Ziegler (ZMHU). William Farfan (Wake Forest University) and Pedro Acevedo and Mark Strong (Smithsonian Institution) kindly identified the host plants. Lucrecia Rodriguez, Taina Litwak, Elizabeth Roberts, George Venable, and Jerrett McCormick helped to produce many of the illustrations, and Terrence Walters (USDA, APHIS, CPHST) secured funding for some of the illustration work. Annabella Reszczynski (USDA, APHIS, IS) helped obtain funding for ALN to travel to Peru which facilitated collaboration with SENASA, and George "Andy" Ball and Cesar Orozco (USDA, APHIS, IS) assisted in multiple ways with travel and sampling efforts in Peru and Bolivia. We also thank Roberto Zucchi and Norman Woodley for their comments on previous drafts of the manuscript. USDA is an equal opportunity provider and employer. NR 16 TC 2 Z9 2 U1 1 U2 8 PU MAGNOLIA PRESS PI AUCKLAND PA PO BOX 41383, AUCKLAND, ST LUKES 1030, NEW ZEALAND SN 1175-5326 EI 1175-5334 J9 ZOOTAXA JI Zootaxa PD NOV 16 PY 2015 VL 4041 IS 1 BP 1 EP + PG 93 WC Zoology SC Zoology GA CW6WT UT WOS:000365139800001 PM 26624697 ER PT J AU Woodman, N AF Woodman, Neal TI MORPHOLOGICAL VARIATION AMONG BROAD-CLAWED SHREWS (MAMMALIA: EULIPOTYPHLA: SORICIDAE: CRYPTOTIS POMEL, 1848) FROM HIGHLANDS OF WESTERN HONDURAS, WITH DESCRIPTIONS OF THREE NEW CRYPTIC SPECIES SO ANNALS OF CARNEGIE MUSEUM LA English DT Article DE Blarinini; Central America; humerus; Insectivora; locomotion; manus; postcranial anatomy; Soricinae; Soricomorpha ID SMALL-EARED SHREWS; GENUS CRYPTOTIS; EVOLUTIONARY MORPHOLOGY; FUNCTIONAL-MORPHOLOGY; LOCOMOTORY BEHAVIOR; SKELETAL MORPHOLOGY; CENTRAL-AMERICA; FORELIMB; SORICOMORPHA; PROPORTIONS AB Broad-clawed shrews of the Cryptotis goldmani group (Mammalia: Eulipotyphla: Soricidae) are discontinuously distributed in temperate highlands from southern Tamaulipas, Mexico, to Honduras. The group represents a clade within the small-eared shrews (genus Cryptotis Pomel, 1848) that is characterized by modifications of the forelimb, including broadened fore-feet, elongated and broadened fore-claws, and a massive humerus with enlarged processes. Two species of C. goldmani group shrews have been recorded previously from Honduras: C. magnimanus Woodman and Timm, 1999, is endemic to the Cordillera de Montecillos, and C. goodwini Jackson, 1933, which also occurs in the Sierra Madre of southern Guatemala, has been recorded from three isolated highland regions with remnant forest in western Honduras. Morphological and morphometrical analyses of variation in the skull and postcranial skeleton within and among the three Honduran populations of C. goodwini reveal that each represents a distinct species of broad-clawed shrew. These are described herein as three new species of the C. goldmani group: Cryptotis celaque, Cryptotis mccarthyi, and Cryptotis cavatorculus, and their locomotory ability and substrate use are characterized relative to other small-eared shrews. C1 [Woodman, Neal] Smithsonian Inst, Natl Museum Nat Hist, USGS Patuxent Wildlife Res Ctr, Sect Mammals,Carnegie Museum Nat Hist, Washington, DC 20013 USA. RP Woodman, N (reprint author), Smithsonian Inst, Natl Museum Nat Hist, USGS Patuxent Wildlife Res Ctr, Sect Mammals,Carnegie Museum Nat Hist, Washington, DC 20013 USA. EM woodmanN@si.edu OI Woodman, Neal/0000-0003-2689-7373 NR 27 TC 3 Z9 3 U1 1 U2 4 PU CARNEGIE MUSEUM NATURAL HISTORY PI PITTSBURGH PA 4400 FORBES AVE, PITTSBURGH, PA 15213 USA SN 0097-4463 EI 1943-6300 J9 ANN CARNEGIE MUS JI Ann. Carnegie Mus. PD NOV 15 PY 2015 VL 83 IS 2 BP 95 EP 119 PG 25 WC Paleontology; Zoology SC Paleontology; Zoology GA CZ4MA UT WOS:000367076100002 ER PT J AU Bemporad, A Giordano, S Raymond, JC Knight, MM AF Bemporad, A. Giordano, S. Raymond, J. C. Knight, M. M. TI Study of sungrazing comets with space-based coronagraphs: New possibilities offered by METIS on board Solar Orbiter SO ADVANCES IN SPACE RESEARCH LA English DT Article DE Comets; General; Coronography; Future instrumentation ID SUN-GRAZING COMET; LYMAN-ALPHA OBSERVATIONS; LOVEJOY C/2011 W3; EXTREME-ULTRAVIOLET; SUNSKIRTING COMETS; UVCS OBSERVATION; WATER PRODUCTION; DUST PARTICLES; PERIHELION; SOHO AB Thanks to the launch of SOHO in the end of 1995 and to the continuous monitoring of the white light (WL) corona offered by the LASCO coronagraphs, it was discovered that sungrazing comets are much more common than previously thought. More than 2800 comets have been discovered so far over nearly 20 years, hence slightly less than a comet every 2 days is observed by coronagraphs. The WL emission seen by SOHO/LASCO and more recently also by the STEREO/SECCHI instruments provides information not only on the comet orbits (hence on their origin), but also on the dust-tail formation, dust-tail disconnection, occurrence of nucleus fragmentation and nucleus disintegration processes. Very interestingly, a few sungrazing comets have also been observed spectroscopically in the UV by the SOHO UV Coronagraph Spectrometer (UVCS), and the strong emission observed in the HI Lyman-alpha 1216 angstrom line provides direct information also on the water outgassing rate, tail chemical composition, nucleus size, and occurrence of nucleus fragmentation. Moreover, the UV cometary emission provides a new method to estimate physical parameters of the coronal plasma met by the comet (like electron density, proton temperature and solar wind velocity), so that these comets can be considered as "local probes" for the solar corona. Unique observations of comets will be provided in the near future by the METIS coronagraph on board the Solar Orbiter mission: METIS will simultaneously observe the corona in WL and in UV (HI Lyman-alpha), hence it will be a unique instrument capable of studying at the same time the transiting comets and the solar corona. Previous results and new possibilities offered by METIS on these topics are summarized and discussed here. (C) 2015 COSPAR. Published by Elsevier Ltd. All rights reserved. C1 [Bemporad, A.; Giordano, S.] INAF Turin Astrophys Observ, Turin, Italy. [Raymond, J. C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Knight, M. M.] Lowell Observ, Flagstaff, AZ 86001 USA. RP Bemporad, A (reprint author), INAF Turin Astrophys Observ, Turin, Italy. EM bemporad@oato.inaf.it; giordano@oato.inaf.it; jraymond@cfa.harvard.edu; knight@lowell.edu OI Bemporad, Alessandro/0000-0001-5796-5653; Giordano, Silvio/0000-0002-3468-8566 NR 44 TC 1 Z9 1 U1 0 U2 2 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 0273-1177 EI 1879-1948 J9 ADV SPACE RES JI Adv. Space Res. PD NOV 15 PY 2015 VL 56 IS 10 BP 2288 EP 2297 DI 10.1016/j.asr.2015.08.037 PG 10 WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA CV4QP UT WOS:000364251900022 ER PT J AU Liu, ZYC Zimbelman, JR AF Liu, Zac Yung-Chun Zimbelman, James R. TI Recent near-surface wind directions inferred from mapping sand ripples on Martian dunes SO ICARUS LA English DT Article DE Aeolian processes; Mars, surface; Geological processes ID GENERAL-CIRCULATION MODEL; TRANSVERSE AEOLIAN RIDGES; EOLIAN FEATURES; VARYING FLOWS; POLAR-REGIONS; GUSEV CRATER; MARS; HIRISE; TRANSPORT; ALIGNMENT AB The High Resolution Imaging Science Experiment (HiRISE) provides the capability to obtain orbital images of Mars that are of sufficient resolution to record wind ripple patterns on the surfaces of sand dunes. Ripple patterns provide valuable insights into aeolian erosion and deposition on Earth and Mars. In this study, we develop a systematic mapping procedure to examine sand ripple orientations and create surface process maps to evaluate the recent wind flow over the dunes, as well as the interplay of wind and dune shape. By carefully examining the morphology of the dunes and the location of grainflow and grainfall on dune slipfaces, the recent near-surface wind direction (short-term wind) can be identified. Results from the analysis of three dune fields on the floors of craters west of Hellas Basin show regional N, NW, SE, and ESE wind directions. In the three adjacent dune fields, surface process and flow maps suggest a complex wind pattern. The comparison of short-term wind with dune-constructing wind (long-term wind) shows NE and ESE winds may be persistent at least for the past thousands of years. The results also show that the orientation of inferred wind direction on linear dunes is correlated with the crestlines, which suggest that form-flow interaction may take place. The results of local wind flow documentation should improve Martian surface wind modeling and advance our understanding of sand transport, as well as the rates of sand mobility on both Mars and Earth. (C) 2015 Elsevier Inc. All rights reserved. C1 [Liu, Zac Yung-Chun] Brigham Young Univ, Dept Geol Sci, Provo, UT 84602 USA. [Zimbelman, James R.] Smithsonian Inst, Natl Air & Space Museum, Ctr Earth & Planetary Studies, Washington, DC 20013 USA. RP Liu, ZYC (reprint author), Arizona State Univ, Sch Earth & Space Explorat, ISTB4 745, Tempe, AZ 85287 USA. EM zacycliu@asu.edu; zimbelmanj@si.edu FU NASA MDAP [NNX12AJ38G] FX This project was carried out while Z.Y.-C.L. visited the National Air and Space Museum during the summers of 2013 and 2014, supported by funds from NASA MDAP Grant NNX12AJ38G. We would like to thank Jani Radebaugh and Eric Christiansen for their discussion and encouragement, and Molly Johnson for her technical support during the use of HiRISE images and ArcGIS. Nathan Bridges and Lori Fenton provided valuable suggestions and constructive reviews, which significantly improved the final manuscript. NR 65 TC 1 Z9 1 U1 6 U2 19 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 NOV 15 PY 2015 VL 261 BP 169 EP 181 DI 10.1016/j.icarus.2015.08.022 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CS9BZ UT WOS:000362385400015 ER PT J AU Laity, T Laffan, SW Gonzalez-Orozco, CE Faith, DP Rosauer, DF Byrne, M Miller, JT Crayn, D Costion, C Moritz, CC Newport, K AF Laity, Tania Laffan, Shawn W. Gonzalez-Orozco, Carlos E. Faith, Daniel P. Rosauer, Dan F. Byrne, Margaret Miller, Joseph T. Crayn, Darren Costion, Craig Moritz, Craig C. Newport, Karl TI Phylodiversity to inform conservation policy: An Australian example SO SCIENCE OF THE TOTAL ENVIRONMENT LA English DT Article DE Phylogeny; Species; Conservation planning; Policy; Diversity; Phylogenetic diversity; Phylogenetic endemism ID INTEGRATING PHYLOGENETIC DIVERSITY; EVOLUTIONARY HISTORY; BIODIVERSITY HOTSPOTS; SPECIES RICHNESS; ENDEMISM; CLIMATE; MAMMALS; AREAS; FLORA; EXTINCTION AB Phylodiversity measures summarise the phylogenetic diversity patterns of groups of organisms. By using branches of the tree of life, rather than its tips (e.g., species), phylodiversity measures provide important additional information about biodiversity that can improve conservation policy and outcomes. As a biodiverse nation with a strong legislative and policy framework, Australia provides an opportunity to use phylogenetic information to inform conservation decision-making. We explored the application of phylodiversity measures across Australia with a focus on two highly biodiverse regions, the south west of Western Australia (SWWA) and the South East Queensland bioregion (SEQ). We analysed seven diverse groups of organisms spanning five separate phyla on the evolutionary tree of life, the plant genera Acacia and Daviesia, mammals, hylid frogs, myobatrachid frogs, passerine birds, and camaenid land snails. We measured species richness, weighted species endemism (WE) and two phylodiversity measures, phylogenetic diversity (PD) and phylogenetic endemism(PE), as well as their respective complementarity scores (a measure of gains and losses) at 20 km resolution. Higher PD was identified within SEQ for all fauna groups, whereas more PD was found in SWWA for both plant groups. PD and PD complementarity were strongly correlated with species richness and species complementarity for most groups but less so for plants. PD and PE were found to complement traditional species-based measures for all groups studied: PD and PE follow similar spatial patterns to richness and WE, but highlighted different areas that would not be identified by conventional species-based biodiversity analyses alone. The application of phylodiversity measures, particularly the novel weighted complementary measures considered here, in conservation can enhance protection of the evolutionary history that contributes to present day biodiversity values of areas. Phylogenetic measures in conservation can include important elements of biodiversity in conservation planning, such as evolutionary potential and feature diversity that will improve decision-making and lead to better biodiversity conservation outcomes. Crown Copyright (C) 2015 Published by Elsevier B. V. All rights reserved. C1 [Laity, Tania; Newport, Karl] Dept Environm, Div Sci, Canberra, ACT 2601, Australia. [Laffan, Shawn W.] Univ New S Wales, Sch Biol Earth & Environm Sci, Ctr Ecosyst Sci, Sydney, NSW 2052, Australia. [Gonzalez-Orozco, Carlos E.] Univ Canberra, Inst Appl Ecol, Canberra, ACT 2601, Australia. [Gonzalez-Orozco, Carlos E.] Univ Canberra, Collaborat Res Murray Darling Basin Futures, Canberra, ACT 2601, Australia. [Faith, Daniel P.] Australian Museum, Res Inst, Sydney, NSW 2000, Australia. [Rosauer, Dan F.; Moritz, Craig C.] Australian Natl Univ, Res Sch Biol, Div Evolut Ecol & Genet, Canberra, ACT 2601, Australia. [Rosauer, Dan F.; Moritz, Craig C.] Australian Natl Univ, Ctr Biodivers Anal, Canberra, ACT 2601, Australia. [Byrne, Margaret] Bentley Delivery Ctr, Dept Pk & Wildlife, Sci & Conservat Div, Bentley, WA 6983, Australia. [Miller, Joseph T.] CSIRO, Ctr Australian Natl Biodivers Res, Canberra, ACT, Australia. [Crayn, Darren] James Cook Univ, Australian Trop Herbarium, Smithfield, Qld 4878, Australia. [Crayn, Darren; Costion, Craig] James Cook Univ, Ctr Trop Environm Sustainabil Sci, Smithfield, Qld 4878, Australia. [Costion, Craig] Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, MRC 166, Washington, DC 20013 USA. RP Laity, T (reprint author), Dept Environm, Div Sci, GPO Box 787, Canberra, ACT 2601, Australia. RI Research ID, CTBCC /O-3564-2014; James Cook University, TESS/B-8171-2012; Moritz, Craig/A-7755-2012; Crayn, Darren/A-7386-2011; Miller, Joe/M-2693-2016; OI Crayn, Darren/0000-0001-6614-4216; Miller, Joe/0000-0002-5788-9010; Laffan, Shawn/0000-0002-5996-0570 FU Australian Centre for Ecological Analysis and Synthesis (ACEAS); Australian Government National Collaborative Research Infrastructure Strategy (NCRIS); Australian Government Department of Environment FX This work was initiated at a workshop (Integrating Measures of Phylogenetic and Taxonomic Diversity and Endemism into National Conservation Assessment) supported by the Australian Centre for Ecological Analysis and Synthesis (ACEAS). ACEAS is a facility of the Terrestrial Ecosystem Research Network (TERN) funded by the Australian Government National Collaborative Research Infrastructure Strategy (NCRIS). Further support was provided by John Stanisic, Andrew Hugall, Simon Ferrier, Jane Ambrose, Jonathan Face, Brian Prince, and the Australian Government Department of Environment. NR 78 TC 11 Z9 11 U1 4 U2 61 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0048-9697 EI 1879-1026 J9 SCI TOTAL ENVIRON JI Sci. Total Environ. PD NOV 15 PY 2015 VL 534 BP 131 EP 143 DI 10.1016/j.scitotenv.2015.04.113 PG 13 WC Environmental Sciences SC Environmental Sciences & Ecology GA CQ0MK UT WOS:000360290100013 PM 25976346 ER PT J AU Wagner, PJ AF Wagner, Peter J. TI One era you are in-the next you are out SO SCIENCE LA English DT Editorial Material ID FOSSIL RECORD; BODY-SIZE; EVOLUTION; TRENDS; EXTINCTIONS; CARNIVORA; MAMMALIA C1 Smithsonian Inst, Dept Paleobiol, Natl Museum Nat Hist, Washington, DC 20560 USA. RP Wagner, PJ (reprint author), Smithsonian Inst, Dept Paleobiol, Natl Museum Nat Hist, Washington, DC 20560 USA. EM wagnerpj@si.edu NR 13 TC 0 Z9 0 U1 2 U2 3 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 NOV 13 PY 2015 VL 350 IS 6262 BP 736 EP 737 PG 2 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA CW3MS UT WOS:000364897000017 PM 26564831 ER PT J AU McKeon, CS Tunberg, BG Johnston, CA Barshis, DJ AF McKeon, C. Seabird Tunberg, Bjorn G. Johnston, Cora A. Barshis, Daniel J. TI Ecological drivers and habitat associations of estuarine bivalves SO PEERJ LA English DT Article DE Bivalve; Estuary; Biodiversity; Water flow; Salinity; Sediment ID INDIAN-RIVER-LAGOON; ST-LUCIE-ESTUARY; FEEDING BIVALVES; RANGIA-CUNEATA; CLAM; MOLLUSKS; FLORIDA; ECOSYSTEMS; DIVERSITY; SEDIMENTS AB Community composition of the infaunal bivalve fauna of the St. Lucie Estuary and southern Indian River Lagoon, eastern Florida was sampled quarterly for 10 years as part of a long-term benthic monitoring program. A total of 38,514 bivalves of 137 taxa were collected and identified. We utilized this data, along with sediment samples and environmental measurements gathered concurrently, to assess the community composition, distribution, and ecological drivers of the infaunal bivalves of this estuary system. Salinity had the strongest influence on bivalve assemblage across the 15 sites, superseding the influences of sediment type, water turbidity, temperature and other environmental parameters. The greatest diversity was found in higher salinity euhaline sites, while the greatest abundance of individual bivalves was found in medium salinity mixohaline sites, the lowest diversity and abundances were found in the low salinity oligohaline sites, demonstrating a strong positive association between salinity and diversity/abundance. Water management decisions for the estuary should incorporate understanding of the role of salinity on bivalve diversity, abundance, and ecosystem function. C1 [McKeon, C. Seabird] Smithsonian Inst, Natl Museum Nat Hist SMS, Ft Pierce, FL 34949 USA. [Tunberg, Bjorn G.] Gothenburg Univ, Dept Biol & Environm Sci, Kristineberg, Sweden. [Johnston, Cora A.] Univ Maryland, Dept Entomol, College Pk, MD 20742 USA. [Barshis, Daniel J.] Old Dominion Univ, Dept Biol Sci, Norfolk, VA 23529 USA. RP McKeon, CS (reprint author), Smithsonian Inst, Natl Museum Nat Hist SMS, Ft Pierce, FL 34949 USA. EM mckeons@si.edu FU South Florida Water Management District [CP040613]; Army Corps of Engineers [W32CS500361333, W32CS503069184, W32CS523215303, W32CS533500200, W32CS543214978, 190003, 190004] FX Funding for this project was provided by the South Florida Water Management District under contract #CP040613, and the Army Corps of Engineers Award Numbers: W32CS500361333, W32CS503069184, W32CS523215303, W32CS533500200, W32CS543214978 Designated Code: 190003,190004. The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 46 TC 0 Z9 0 U1 5 U2 14 PU PEERJ INC PI LONDON PA 341-345 OLD ST, THIRD FLR, LONDON, EC1V 9LL, ENGLAND SN 2167-8359 J9 PEERJ JI PeerJ PD NOV 12 PY 2015 VL 3 AR e1348 DI 10.7717/peerj.1348 PG 16 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA CX6IA UT WOS:000365803200002 PM 26587338 ER PT J AU Berta-Thompson, ZK Irwin, J Charbonneau, D Newton, ER Dittmann, JA Astudillo-Defru, N Bonfils, X Gillon, M Jehin, E Stark, AA Stalder, B Bouchy, F Delfosse, X Forveille, T Lovis, C Mayor, M Neves, V Pepe, F Santos, NC Udry, S Wunsche, A AF Berta-Thompson, Zachory K. Irwin, Jonathan Charbonneau, David Newton, Elisabeth R. Dittmann, Jason A. Astudillo-Defru, Nicola Bonfils, Xavier Gillon, Michael Jehin, Emmanuel Stark, Antony A. Stalder, Brian Bouchy, Francois Delfosse, Xavier Forveille, Thierry Lovis, Christophe Mayor, Michel Neves, Vasco Pepe, Francesco Santos, Nuno C. Udry, Stephane Wuensche, Anael TI A rocky planet transiting a nearby low-mass star SO NATURE LA English DT Article ID LATE-M-DWARFS; THERMAL PHASE CURVES; MAIN-SEQUENCE STARS; TERRESTRIAL PLANETS; RADIAL-VELOCITIES; STELLAR ACTIVITY; PROPER-MOTION; COOL STARS; METALLICITIES; EXOPLANET AB M-dwarf stars-hydrogen-burning stars that are smaller than 60 per cent of the size of the Sun-are the most common class of star in our Galaxy and outnumber Sun-like stars by a ratio of 12:1. Recent results have shown that M dwarfs host Earth-sized planets in great numbers(1,2): the average number of M-dwarf planets that are between 0.5 to 1.5 times the size of Earth is at least 1.4 per star(3). The nearest such planets known to transit their star are 39 parsecs away(4), too distant for detailed follow-up observations to measure the planetary masses or to study their atmospheres. Here we report observations of GJ 1132b, a planet with a size of 1.2 Earth radii that is transiting a small star 12 parsecs away. Our Doppler mass measurement of GJ 1132b yields a density consistent with an Earth-like bulk composition, similar to the compositions of the six known exoplanets with masses less than six times that of the Earth and precisely measured densities(5-11). Receiving 19 times more stellar radiation than the Earth, the planet is too hot to be habitable but is cool enough to support a substantial atmosphere, one that has probably been considerably depleted of hydrogen. Because the host star is nearby and only 21 per cent the radius of the Sun, existing and upcoming telescopes will be able to observe the composition and dynamics of the planetary atmosphere. C1 [Berta-Thompson, Zachory K.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Berta-Thompson, Zachory K.; Irwin, Jonathan; Charbonneau, David; Newton, Elisabeth R.; Dittmann, Jason A.; Stark, Antony A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Astudillo-Defru, Nicola; Bouchy, Francois; Lovis, Christophe; Mayor, Michel; Pepe, Francesco; Udry, Stephane] Univ Geneva, Observ Geneve, CH-1290 Sauverny, Switzerland. [Bonfils, Xavier; Delfosse, Xavier; Forveille, Thierry; Wuensche, Anael] Univ Grenoble Alpes, IPAG, F-33000 Grenoble, France. [Bonfils, Xavier; Delfosse, Xavier; Forveille, Thierry; Wuensche, Anael] CNRS, IPAG, F-38000 Grenoble, France. [Gillon, Michael; Jehin, Emmanuel] Univ Liege, Inst Astrophys & Geophys, B-4000 Liege, Belgium. [Stalder, Brian] Univ Hawaii Manoa, Inst Astron, Honolulu, HI 96822 USA. [Bouchy, Francois] Univ Aix Marseille 1, CNRS, Lab Astrophys Marseille, UMR 6110, F-13388 Marseille 13, France. [Neves, Vasco] Univ Fed Rio Grande do Norte, Dept Fis, BR-59072970 Natal, RN, Brazil. [Santos, Nuno C.] Univ Porto, Inst Astrofis & Ciencias Espaco, CAUP, P-4150762 Oporto, Portugal. [Santos, Nuno C.] Univ Porto, Fac Ciencias, Dept Fis & Astron, P-4169007 Oporto, Portugal. RP Berta-Thompson, ZK (reprint author), MIT, Kavli Inst Astrophys & Space Res, 77 Massachusetts Ave, Cambridge, MA 02139 USA. EM zkbt@mit.edu OI Berta-Thompson, Zachory/0000-0002-3321-4924; Astudillo-Defru, Nicola/0000-0002-8462-515X; Bonfils, Xavier/0000-0001-9003-8894; Stark, Antony/0000-0002-2718-9996 FU David and Lucile Packard Fellowship for Science and Engineering; National Science Foundation; John Templeton Foundation; Belgian Fund for Scientific Research; MIT Torres Fellowship for Exoplanet Research; French Agence Nationale de la Recherche; European Research Council; CNPq/BJT Post Doctorate fellowship; INCT INEspaco; Portuguese National Science Foundation (FCT); COMPETE program FX We thank the staff at the Cerro Tololo Inter-American Observatory for assistance in the construction and operation of MEarth-South; J. Winn and J. Berta-Thompson for comments on the manuscript; S. Seager and A. Zsom for conversations that improved the work; L. Delrez for her independent analysis of the TRAPPIST data; and J. Eastman, D. Dragomir and R. Siverd for their efforts to observe additional transits. The MEarth Project acknowledges funding from the David and Lucile Packard Fellowship for Science and Engineering, and the National Science Foundation, and a grant from the John Templeton Foundation. The opinions expressed here are those of the authors and do not necessarily reflect the views of the John Templeton Foundation. The development of the PISCO imager was supported by the National Science Foundation. HARPS observations were made with European Southern Observatory (ESO) Telescopes at the La Silla Paranal Observatory. TRAPPIST is a project funded by the Belgian Fund for Scientific Research, with the participation of the Swiss National Science Foundation. Z.K.B.-T is funded by the MIT Torres Fellowship for Exoplanet Research. X.B., X.D., T.F. and A.W. acknowledge the support of the French Agence Nationale de la Recherche and the European Research Council. M.G. and E.J. are FNRS Research Associates. V.N. acknowledges a CNPq/BJT Post Doctorate fellowship and partial financial support from the INCT INEspaco. N.C.S. acknowledges the support from the Portuguese National Science Foundation (FCT) as well as the COMPETE program. NR 64 TC 27 Z9 28 U1 2 U2 11 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 NOV 12 PY 2015 VL 527 IS 7577 BP 204 EP + DI 10.1038/nature15762 PG 10 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA CV6RC UT WOS:000364396700038 PM 26560298 ER PT J AU de Gasperin, F Intema, HT van Weeren, RJ Dawson, WA Golovich, N Wittman, D Bonafede, A Bruggen, M AF de Gasperin, F. Intema, H. T. van Weeren, R. J. Dawson, W. A. Golovich, N. Wittman, D. Bonafede, A. Brueggen, M. TI A powerful double radio relic system discovered in PSZ1 G108.18-11.53: evidence for a shock with non-uniform Mach number? SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies: clusters: individual: PSZ1 G108.18-11.53; large-scale structure of Universe; radio continuum: general ID MERGING GALAXY CLUSTER; MAGNETIC-FIELD AMPLIFICATION; LARGE-SCALE STRUCTURE; X-RAY; PARTICLE-ACCELERATION; CIZA J2242.8+5301; LOW-FREQUENCY; SKY SURVEY; SAUSAGE CLUSTER; ENERGY-SPECTRA AB Diffuse radio emission in the form of radio haloes and relics has been found in a number of merging galaxy clusters. These structures indicate that shock and turbulence associated with the merger accelerate electrons to relativistic energies. We report the discovery of a radio relic + radio halo system in PSZ1 G108.18-11.53 (z = 0.335). This cluster hosts the second most powerful double radio relic system ever discovered. We observed PSZ1 G108.18-11.53 with the Giant Meterwave Radio Telescope and the Westerbork Synthesis Radio Telescope. We obtained radio maps at 147, 323, 607 and 1380 MHz. We also observed the cluster with the Keck telescope, obtaining the spectroscopic redshift for 42 cluster members. From the injection index, we obtained the Mach number of the shocks generating the two radio relics. For the southern shock, we found M = 2.33(-0.26)(+0.19), while the northern shock Mach number goes from M=2.20(-0.14)(+0.07) in the north part down to M = 2.00(-0.08)(+0.03) in the southern region. If the relation between the injection index and the Mach number predicted by diffusive shock acceleration theory holds, this is the first observational evidence for a gradient in the Mach number along a galaxy cluster merger shock. C1 [de Gasperin, F.; Bonafede, A.; Brueggen, M.] Univ Hamburg, Hamburger Sternwarte, D-21029 Hamburg, Germany. [Intema, H. T.] Natl Radio Astron Observ, Socorro, NM 87801 USA. [van Weeren, R. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Dawson, W. A.] Lawrence Livermore Natl Lab, Livermore, CA 94550 USA. [Golovich, N.; Wittman, D.] Univ Calif Davis, Davis, CA 95616 USA. RP de Gasperin, F (reprint author), Univ Hamburg, Hamburger Sternwarte, Gojenbergsweg 112, D-21029 Hamburg, Germany. EM fdg@hs.uni-hamburg.de OI Wittman, David/0000-0002-0813-5888; van Weeren, Reinout/0000-0002-0587-1660 FU Deutsche Forschungsgemeinschaft [FOR 1254]; NASA through the Einstein Postdoctoral grant - Chandra X-ray Center [PF2-130104]; NASA [NAS8-03060]; US DOE [DE-AC52-07NA27344 (LLNL-JRNL-671211)]; NSF [AST-0071048]; CARA (Keck Observatory); UCO/Lick Observatory; NSF Facilities and Infrastructure grant [ARI92-14621]; Center for Particle Astrophysics FX AB and MB acknowledge support by the research group FOR 1254 funded by the Deutsche Forschungsgemeinschaft.; RJW 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.; Part of this work performed under the auspices of the US DOE by LLNL under Contract DE-AC52-07NA27344 (LLNL-JRNL-671211).; Funding for the DEEP2/DEIMOS pipelines has been provided by NSF grant AST-0071048. The DEIMOS spectrograph was funded by grants from CARA (Keck Observatory) and UCO/Lick Observatory, an NSF Facilities and Infrastructure grant (ARI92-14621), the Center for Particle Astrophysics, and by gifts from Sun Microsystems and the Quantum Corporation. NR 67 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 NOV 11 PY 2015 VL 453 IS 4 BP 3483 EP 3498 DI 10.1093/mnras/stv1873 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CU6OJ UT WOS:000363651600011 ER PT J AU Heida, M Torres, MAP Jonker, PG Servillat, M Repetto, S Roberts, TP Walton, DJ Moon, DS Harrison, FA AF Heida, M. Torres, M. A. P. Jonker, P. G. Servillat, M. Repetto, S. Roberts, T. P. Walton, D. J. Moon, D. -S. Harrison, F. A. TI Discovery of a red supergiant counterpart to RX J004722.4-252051, a ULX in NGC 253 SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE supergiants; infrared: stars; X-rays: binaries; X-rays: individual: RX J004722.4-252051 ID X-RAY SOURCE; MASS BLACK-HOLE; MAGELLAN INFRARED SPECTROGRAPH; XMM-NEWTON; ULTRALUMINOUS STATE; SOLAR MASSES; COOL STARS; GALAXY; ACCRETION; EMISSION AB We present two epochs of near-infrared spectroscopy of the candidate red supergiant counterpart to RX J004722.4-252051, a ULX in NGC 253. We measure radial velocities of the object and its approximate spectral type by cross-correlating our spectra with those of known red supergiants. Our VLT/X-shooter spectrum is best matched by that of early M-type supergiants, confirming the red supergiant nature of the candidate counterpart. The radial velocity of the spectrum, taken on 2014 August 23, is 417 +/- 4 kms(-1). This is consistent with the radial velocity measured in our spectrum taken with Magellan/MMIRS on 2013 June 28, of 410 +/- 70 km s(-1), although the large error on the latter implies that a radial velocity shift expected for a black hole of tens of M-circle dot can easily be hidden. Using nebular emission lines we find that the radial velocity due to the rotation of NGC 253 is 351 +/- 4 kms(-1) at the position of the ULX. Thus the radial velocity of the counterpart confirms that the source is located in NGC 253, but also shows an offset with respect to the local bulk motion of the galaxy of 66 +/- 6 kms(-1). We argue that the most likely origin for this displacement lies either in a SN kick, requiring a system containing a greater than or similar to 50 M-circle dot black hole, and/or in orbital radial velocity variations in the ULX binary system, requiring a greater than or similar to 100 M-circle dot black hole. We therefore conclude that RX J004722.4-252051 is a strong candidate for a ULX containing a massive stellar black hole. C1 [Heida, M.; Torres, M. A. P.; Jonker, P. G.] SRON Netherlands Inst Space Res, NL-3584 CA Utrecht, Netherlands. [Heida, M.; Torres, M. A. P.; Jonker, P. G.; Repetto, S.] Radboud Univ Nijmegen, IMAPP, Dept Astrophys, NL-6500 GL Nijmegen, Netherlands. [Torres, M. A. P.] European So Observ, Santiago 19, Chile. [Servillat, M.] Univ Paris Diderot, CEA Saclay, CNRS INSU, Lab AIM,CEA Irfu SAp, F-91191 Gif Sur Yvette, France. [Servillat, M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Roberts, T. P.] Univ Durham, Dept Phys, Durham DH1 3LE, England. [Walton, D. J.; Harrison, F. A.] CALTECH, Space Radiat Lab, Pasadena, CA 91125 USA. [Moon, D. -S.] Univ Toronto, Dept Astron & Astrophys, Toronto, ON M5S 3H4, Canada. RP Heida, M (reprint author), SRON Netherlands Inst Space Res, Sorbonnelaan 2, NL-3584 CA Utrecht, Netherlands. EM m.heida@astro.ru.nl; p.jonker@sron.nl FU ESO [093.D-0256]; ESO Telescopes at the La Silla Paranal Observatory [093.D-0256]; STFC consolidated grant [ST/L00075X/1] FX Observations based on ESO programme 093.D-0256. We thank the anonymous referee for their comments that helped improve the paper. We want to thank Ben Davies for sharing his X-shooter RSG spectra and Tom Marsh for developing MOLLY. This paper uses data products produced by the OIR Telescope Data Center, supported by the Smithsonian Astrophysical Observatory. Based on observations made with ESO Telescopes at the La Silla Paranal Observatory under programme ID 093.D-0256. TPR's contributions were funded as part of the STFC consolidated grant award ST/L00075X/1. NR 58 TC 3 Z9 3 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 NOV 11 PY 2015 VL 453 IS 4 BP 3510 EP 3518 DI 10.1093/mnras/stv1853 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CU6OJ UT WOS:000363651600013 ER PT J AU Bauer, A Springel, V Vogelsberger, M Genel, S Torrey, P Sijacki, D Nelson, D Hernquist, L AF Bauer, Andreas Springel, Volker Vogelsberger, Mark Genel, Shy Torrey, Paul Sijacki, Debora Nelson, Dylan Hernquist, Lars TI Hydrogen reionization in the Illustris universe SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE radiative transfer; methods: numerical; H II regions; galaxies: high-redshift; intergalactic medium; dark ages, reionization, first stars ID COSMIC STAR-FORMATION; SIMILAR-TO 7; RADIATIVE-TRANSFER SIMULATIONS; FULLY COUPLED SIMULATION; GALAXY FORMATION PHYSICS; FLUX-LIMITED DIFFUSION; LYMAN-BREAK GALAXIES; LY-ALPHA EMITTERS; INTERGALACTIC MEDIUM; HII-REGIONS AB Hydrodynamical simulations of galaxy formation such as the Illustris simulations have progressed to a state where they approximately reproduce the observed stellar mass function from high to low redshift. This in principle allows self-consistent models of reionization that exploit the accurate representation of the diffuse gas distribution together with the realistic growth of galaxies provided by these simulations, within a representative cosmological volume. In this work, we apply and compare two radiative transfer algorithms implemented in a GPU-accelerated code to the 106.5-Mpc-wide volume of Illustris in post-processing in order to investigate the reionization transition predicted by this model. We find that the first generation of galaxies formed by Illustris is just about able to reionize the universe by redshift z similar to 7, provided quite optimistic assumptions about the escape fraction and the resolution limitations are made. Our most optimistic model finds an optical depth of tau similar or equal to 0.065, which is in very good agreement with recent Planck 2015 determinations. Furthermore, we show that moment-based approaches for radiative transfer with the M1 closure give broadly consistent results with our angular-resolved radiative transfer scheme. In our favoured fiducial model, 20 per cent of the hydrogen is reionized by redshift z = 9.20, and this rapidly climbs to 80 per cent by redshift z = 6.92. It then takes until z = 6.24 before 99 per cent of the hydrogen is ionized. On average, reionization proceeds 'inside-out' in our models, with a size distribution of reionized bubbles that progressively features regions of ever larger size while the abundance of small bubbles stays fairly constant. C1 [Bauer, Andreas; Springel, Volker] Heidelberger Inst Theoret Studien, D-69118 Heidelberg, Germany. [Springel, Volker] Heidelberg Univ, Zentrum Astron, Astron Rech Inst, D-69120 Heidelberg, Germany. [Vogelsberger, Mark; Torrey, Paul] MIT, Kavli Inst Astrophys & Space Res, Dept Phys, Cambridge, MA 02139 USA. [Genel, Shy] Columbia Univ, Dept Astron, New York, NY 10027 USA. [Sijacki, Debora] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Sijacki, Debora] Univ Cambridge, Kavli Inst Cosmol, Cambridge CB3 0HA, England. [Nelson, Dylan; Hernquist, Lars] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Bauer, A (reprint author), Heidelberger Inst Theoret Studien, Schloss Wolfsbrunnenweg 35, D-69118 Heidelberg, Germany. EM andreas.bauer@h-its.org OI Torrey, Paul/0000-0002-5653-0786 FU European Research Council [ERC-StG EXAGAL-308037]; IMPRS for Astronomy & Cosmic Physics at the University of Heidelberg; NASA [NNX12AC67G, NAS5-26555]; NSF [AST-1312095]; NASA through a Hubble Fellowship from the Space Telescope Science Institute [HST-HF2-51341.001-A] FX We thank the anonymous referee for constructive criticism and valuable suggestions that helped to improve the paper. We also thank Rudiger Pakmor and Ewald Puchwein for helpful discussions. AB and VS acknowledge support by the European Research Council under ERC-StG EXAGAL-308037. AB acknowledges support by the IMPRS for Astronomy & Cosmic Physics at the University of Heidelberg. LH acknowledges support from NASA grant NNX12AC67G and NSF grant AST-1312095. SG acknowledges support for programme number HST-HF2-51341.001-A that was 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. We gratefully thank for GPU-accelerated computer time on the 'Milky Way' GPU cluster of the DFG Research Centre SFB-881 'The Milky Way System' and on 'Hydra' at the Max-Planck Computing Centre RZG in Garching. NR 114 TC 11 Z9 11 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 NOV 11 PY 2015 VL 453 IS 4 BP 3593 EP 3610 DI 10.1093/mnras/stv1893 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CU6OJ UT WOS:000363651600019 ER PT J AU Pastorello, A Prieto, JL Elias-Rosa, N Bersier, D Hosseinzadeh, G Morales-Garoffolo, A Noebauer, UM Taubenberger, S Tomasella, L Kochanek, CS Falco, E Basu, U Beacom, JF Benetti, S Brimacombe, J Cappellaro, E Danilet, AB Dong, SB Fernandez, JM Goss, N Granata, V Harutyunyan, A Holoien, TWS Ishida, EEO Kiyota, S Krannich, G Nicholls, B Ochner, P Pojmanski, G Shappee, BJ Simonian, GV Stanek, KZ Starrfield, S Szczygiel, D Tartaglia, L Terreran, G Thompson, TA Turatto, M Wagner, RM Wiethoff, WS Wilber, A Wozniak, PR AF Pastorello, A. Prieto, J. L. Elias-Rosa, N. Bersier, D. Hosseinzadeh, G. Morales-Garoffolo, A. Noebauer, U. M. Taubenberger, S. Tomasella, L. Kochanek, C. S. Falco, E. Basu, U. Beacom, J. F. Benetti, S. Brimacombe, J. Cappellaro, E. Danilet, A. B. Dong, Subo Fernandez, J. M. Goss, N. Granata, V. Harutyunyan, A. Holoien, T. W. -S. Ishida, E. E. O. Kiyota, S. Krannich, G. Nicholls, B. Ochner, P. Pojmanski, G. Shappee, B. J. Simonian, G. V. Stanek, K. Z. Starrfield, S. Szczygiel, D. Tartaglia, L. Terreran, G. Thompson, T. A. Turatto, M. Wagner, R. M. Wiethoff, W. S. Wilber, A. Wozniak, P. R. TI Massive stars exploding in a He-rich circumstellar medium - VII. The metamorphosis of ASASSN-15ed from a narrow line Type Ibn to a normal Type Ib Supernova SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE supernovae: general; supernovae: individual: ASASSN-15ed; supernovae: individual: SN 1991D; supernovae: individual: SN 2006jc; supernovae: individual: SN 2010al ID WOLF-RAYET STARS; DIGITAL SKY SURVEY; CORE-COLLAPSE SUPERNOVAE; SN 2006JC; FUNDAMENTAL PARAMETERS; DUST FORMATION; WNL STARS; EXPLOSION; SPECTROSCOPY; EXTINCTION AB We present the results of the spectroscopic and photometric monitoring campaign of ASASSN-15ed. The transient was discovered quite young by the All Sky Automated Survey for Super-Novae (ASAS-SN) survey. Amateur astronomers allowed us to sample the photometric SN evolution around maximum light, which we estimate to have occurred on JD=2457087.4 +/- 0.6 in the r band. Its apparent r-band magnitude at maximum was r = 16.91 +/- 0.10, providing an absolute magnitude M-r approximate to -20.04 +/- 0.20, which is slightly more luminous than the typical magnitudes estimated for Type Ibn SNe. The post-peak evolution was well monitored, and the decline rate (being in most bands around 0.1 mag d(-1) during the first 25 d after maximum) is marginally slower than the average decline rates of SNe Ibn during the same time interval. The object was initially classified as a Type Ibn SN because early-time spectra were characterized by a blue continuum with superimposed narrow P-Cygni lines of He I, suggesting the presence of a slowly moving (1200-1500 km s(-1)), He-rich circumstellar medium. Later on, broad P-Cygni He I lines became prominent. The inferred velocities, as measured from the minimum of the broad absorption components, were between 6000 and 7000 km s(-1). As we attribute these broad features to the SN ejecta, this is the first time we have observed the transition of a Type Ibn SN to a Type Ib SN. C1 [Pastorello, A.; Elias-Rosa, N.; Tomasella, L.; Benetti, S.; Cappellaro, E.; Granata, V.; Ochner, P.; Tartaglia, L.; Terreran, G.; Turatto, M.] INAF Osservatorio Astron Padova, I-35122 Padua, Italy. [Prieto, J. L.] Univ Diego Portales, Fac Ingn, Nucleo Astron, Santiago, Chile. [Prieto, J. L.] Millennium Inst Astrophys, Santiago, Chile. [Bersier, D.] Liverpool John Moores Univ, Astrophys Res Inst, Liverpool L3 5RF, Merseyside, England. [Hosseinzadeh, G.] Las Cumbres Observ, Global Telescope Network, Goleta, CA 93117 USA. [Hosseinzadeh, G.] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA. [Morales-Garoffolo, A.] CSIC IEEC, Inst Ciencies Espai, E-08193 Cerdanyola Del Valles, Spain. [Noebauer, U. M.; Taubenberger, S.; Ishida, E. E. O.] Max Planck Inst Astrophys, D-85748 Garching, Germany. [Taubenberger, S.] European Org Astron Res Southern Hemisphere ESO, D-85748 Garching, Germany. [Kochanek, C. S.; Basu, U.; Beacom, J. F.; Goss, N.; Holoien, T. W. -S.; Simonian, G. V.; Stanek, K. Z.; Thompson, T. A.; Wagner, R. M.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. [Kochanek, C. S.; Beacom, J. F.; Stanek, K. Z.; Thompson, T. A.] Ohio State Univ, Ctr Cosmol & Astro Particle Phys, Columbus, OH 43210 USA. [Falco, E.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Basu, U.; Goss, N.] Grove City High Sch, Grove City, OH 43123 USA. [Beacom, J. F.; Danilet, A. B.] Ohio State Univ, Dept Phys, Columbus, OH 43210 USA. [Brimacombe, J.] Coral Towers Observ, Unit Coral Towers 38, Cairns CAIRNS, Australia. [Dong, Subo] Peking Univ, Kavli Inst Astron & Astrophys, Beijing 100871, Peoples R China. [Fernandez, J. M.] Observ Inmaculada Molino, E-41640 Osuna, Spain. [Granata, V.; Tartaglia, L.] Univ Padua, Dipartimento Fis & Astron, I-35122 Padua, Italy. [Harutyunyan, A.] Fdn Galileo Galilei INAF, Telescopio Nazl Galileo, E-38712 Brena Baja, TF, Spain. [Kiyota, S.] Variable Star Observers League Japan, Chiba 2730126, Japan. [Krannich, G.] Roof Observ Kaufering, D-86916 Kaufering, Germany. [Nicholls, B.] Mt Vernon Observ, Nelson 7010, New Zealand. [Pojmanski, G.; Szczygiel, D.] Warsaw Univ, Astron Observ, PL-00478 Warsaw, Poland. [Shappee, B. J.] Observ Carnegie Inst Sci, Pasadena, CA 91101 USA. [Starrfield, S.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA. [Terreran, G.; Wilber, A.] Queens Univ Belfast, Sch Math & Phys, Astrophys Res Ctr, Belfast BT7 1NN, Antrim, North Ireland. [Wagner, R. M.] Univ Arizona, Large Binocular Telescope Observ, Tucson, AZ 85721 USA. [Wiethoff, W. S.] SOLO Observ, Port Wing, WI 54865 USA. [Wiethoff, W. S.] Univ Minnesota, Dept Geol Sci, Duluth, MN 55812 USA. [Wozniak, P. R.] Los Alamos Natl Lab, Los Alamos, NM 87545 USA. RP Pastorello, A (reprint author), INAF Osservatorio Astron Padova, Vicolo Osservatorio 5, I-35122 Padua, Italy. EM andrea.pastorello@oapd.inaf.it RI Elias-Rosa, Nancy/D-3759-2014; OI Wozniak, Przemyslaw/0000-0002-9919-3310; Beacom, John/0000-0002-0005-2631; Elias-Rosa, Nancy/0000-0002-1381-9125; Ishida, Emille/0000-0002-0406-076X; Noebauer, Ulrich/0000-0002-2453-853X; GRANATA, Valentina/0000-0002-1425-4541; Cappellaro, Enrico/0000-0001-5008-8619; Benetti, Stefano/0000-0002-3256-0016; lina, tomasella/0000-0002-3697-2616; Hosseinzadeh, Griffin/0000-0002-0832-2974 FU PRIN-INAF; project 'Transient Universe: unveiling new types of stellar explosions with PESSTO'; FONDECYT [1151445]; Ministry of Economy, Development, and Tourisms Millennium Science Initiative [IC120009]; European Union Seventh Framework Programme (FP7), 'Astronomy Fellowships in Italy' (AstroFIt) [267251]; Spanish Ministerio de Economia y Competitividad (MINECO) [ESP2013-41268-R]; German Research Foundation (DFG) [TRR33]; NSF [PHY-1404311, AST-0908816]; 'Strategic Priority Research Program - The Emergence of Cosmological Structures' of the Chinese Academy of Sciences [XDB09000000]; DOE Computational Science Graduate Fellowship [DE-FG02-97ER25308]; Brazilian agency CAPES [9229-13-2]; NASA through Hubble Fellowship - Space Telescope Science Institute [HF-51348.001]; NASA [NAS 5-26555]; Laboratory Directed Research and Development program at LANL; UK Science and Technology Facilities Council FX AP, SB, NER, AH, LT, GT and MT are partially supported by the PRIN-INAF 2014 with the project 'Transient Universe: unveiling new types of stellar explosions with PESSTO'. Support for JLP is in part by FONDECYT through the grant 1151445 and by the Ministry of Economy, Development, and Tourisms Millennium Science Initiative through grant IC120009, awarded to The Millennium Institute of Astrophysics, MAS. NER acknowledges the support from the European Union Seventh Framework Programme (FP7/2007-2013) under grant agreement no. 267251 'Astronomy Fellowships in Italy' (AstroFIt). AMG acknowledges financial support by the Spanish Ministerio de Economia y Competitividad (MINECO) grant ESP2013-41268-R. ST and UMN acknowledge support by TRR33 'The Dark Universe' of the German Research Foundation (DFG). JFB is supported by NSF Grant PHY-1404311. SD is supported by the 'Strategic Priority Research Program - The Emergence of Cosmological Structures' of the Chinese Academy of Sciences (grant no. XDB09000000). TW-SH is supported by the DOE Computational Science Graduate Fellowship, grant number DE-FG02-97ER25308. EEOI is partially supported by the Brazilian agency CAPES (grant number 9229-13-2). BJS is supported by NASA through Hubble Fellowship grant HF-51348.001 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. SS and AW acknowledge support from NSF and NASA grants to ASU. This work was supported by the Laboratory Directed Research and Development program at LANL. We thank LCOGT and its staff for their continued support of ASAS-SN.; Development of ASAS-SN has been supported by NSF grant AST-0908816 and the Center for Cosmology and AstroParticle Physics at the Ohio State University.; This paper is based on observations made with the Italian Telescopio Nazionale Galileo (TNG) operated on the island of La Palma by the Fundacion Galileo Galilei of the INAF (Istituto Nazionale di Astrofisica) and the 1.82-m Copernico Telescope of INAF-Asiago Observatory. This work also makes use of observations from the LCOGT network; it is also based on observations made with the Gran Telescopio Canarias (GTC), installed in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias, in the Island of La Palma; on observations made with the Nordic Optical Telescope (NOT), operated on the island of La Palma jointly by Denmark, Finland, Iceland, Norway, and Sweden, in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias; on observations obtained at the MDM Observatory, operated by Dartmouth College, Columbia University, Ohio State University, Ohio University, and the University of Michigan. The LT is operated on the island of La Palma by Liverpool John Moores University in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias with financial support from the UK Science and Technology Facilities Council. Data presented in this paper are also based on observations with the Fred Lawrence Whipple Observatory 1.5-m Telescope of SAO. This paper uses data products produced by the OIR Telescope Data Center, supported by the Smithsonian Astrophysical Observatory. NR 45 TC 4 Z9 4 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 NOV 11 PY 2015 VL 453 IS 4 BP 3649 EP 3661 DI 10.1093/mnras/stv1812 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CU6OJ UT WOS:000363651600023 ER PT J AU Miller-Jones, JCA Strader, J Heinke, CO Maccarone, TJ van den Berg, M Knigge, C Chomiuk, L Noyola, E Russell, TD Seth, AC Sivakoff, GR AF Miller-Jones, J. C. A. Strader, J. Heinke, C. O. Maccarone, T. J. van den Berg, M. Knigge, C. Chomiuk, L. Noyola, E. Russell, T. D. Seth, A. C. Sivakoff, G. R. TI Deep radio imaging of 47 Tuc identifies the peculiar X-ray source X9 as a new black hole candidate SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE stars: black holes; globular clusters: individual: 47 Tuc; radio continuum: general; X-rays: binaries ID MAGNETIC CATACLYSMIC VARIABLES; SPECTRAL ENERGY-DISTRIBUTIONS; SPACE-TELESCOPE COUNTERPARTS; GALACTIC GLOBULAR-CLUSTERS; SUB-LUMINOUS ACCRETION; BINARY 4U 0614+091; NOVA V404 CYGNI; NEUTRON-STAR; AE-AQUARII; STELLAR-MASS AB We report the detection of steady radio emission from the known X-ray source X9 in the globular cluster 47 Tuc. With a double-peaked C IV emission line in its ultraviolet spectrum providing a clear signature of accretion, this source had been previously classified as a cataclysmic variable. In deep ATCA (Australia Telescope Compact Array) imaging from 2010 and 2013, we identified a steady radio source at both 5.5 and 9.0 GHz, with a radio spectral index (defined as S-v alpha v(alpha)) of a = -0.4 +/- 0.4. Our measured flux density of 42 +/- 4 mu Jy beam(-1) at 5.5 GHz implies a radio luminosity (vL(v)) of 5.8 x 10(27) erg s(-1), significantly higher than any previous radio detection of an accreting white dwarf. Transitional millisecond pulsars, which have the highest radio-to-X-ray flux ratios among accreting neutron stars (still a factor of a few below accreting black holes at the same L-X), show distinctly different patterns of X-ray and radio variability than X9. When combined with archival X-ray measurements, our radio detection places 47 Tuc X9 very close to the radio/X-ray correlation for accreting black holes, and we explore the possibility that this source is instead a quiescent stellar-mass black hole X-ray binary. The nature of the donor star is uncertain; although the luminosity of the optical counterpart is consistent with a low-mass main-sequence donor star, the mass transfer rate required to produce the high quiescent X-ray luminosity of 10(33) erg s(-1) suggests the system may instead be ultracompact, with an orbital period of order 25 min. This is the fourth quiescent black hole candidate discovered to date in a Galactic globular cluster, and the only one with a confirmed accretion signature from its optical/ultraviolet spectrum. C1 [Miller-Jones, J. C. A.; Russell, T. D.] Curtin Univ, Int Ctr Radio Astron Res, Perth, WA 6845, Australia. [Strader, J.; Chomiuk, L.] Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA. [Heinke, C. O.; Sivakoff, G. R.] Univ Alberta, Dept Phys, Edmonton, AB T6G 2G7, Canada. [Heinke, C. O.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Maccarone, T. J.] Texas Tech Univ, Dept Phys, Lubbock, TX 79409 USA. [van den Berg, M.] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 XH Amsterdam, Netherlands. [van den Berg, M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Knigge, C.] Univ Southampton, Phys & Astron, Southampton SO17 1BJ, Hants, England. [Noyola, E.] Univ Texas Austin, McDonald Observ, Austin, TX 78712 USA. [Seth, A. C.] Univ Utah, Dept Phys & Astron, Salt Lake City, UT 84112 USA. RP Miller-Jones, JCA (reprint author), Curtin Univ, Int Ctr Radio Astron Res, GPO Box U1987, Perth, WA 6845, Australia. EM james.miller-jones@curtin.edu.au RI Miller-Jones, James/B-2411-2013; Sivakoff, Gregory/G-9602-2011; OI Miller-Jones, James/0000-0003-3124-2814; Sivakoff, Gregory/0000-0001-6682-916X; Seth, Anil/0000-0003-0248-5470 FU Commonwealth of Australia; NSF [AST-1308124]; Australian Research Council [FT140101082, DP120102393]; NSERC; Ingenuity New Faculty Award; Alexander von Humboldt Fellowship FX JCAMJ thanks Paul Hancock for assistance with the AEGEAN fitting package and Joe Callingham for useful discussions regarding CVs. We thank the anonymous referee for helpful and constructive comments. The ATCA is part of the Australia Telescope National Facility which is funded by the Commonwealth of Australia for operation as a National Facility managed by CSIRO. This work was supported by the NSF through grant AST-1308124. JCAMJ is the recipient of an Australian Research Council Future Fellowship (FT140101082), and also acknowledges support from an Australian Research Council Discovery Grant (DP120102393). COH and GRS acknowledge funding from NSERC Discovery Grants, and COH is also supported by an Ingenuity New Faculty Award and an Alexander von Humboldt Fellowship. This research has made use of NASA's Astrophysics Data System, and also of the PYTHON packages APLPY (an open-source plotting package for PYTHON hosted at http://aplpy.github.com) and ASTROPY (a community-developed core PYTHON package for Astronomy; Astropy Collaboration 2013). NR 152 TC 6 Z9 6 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 NOV 11 PY 2015 VL 453 IS 4 BP 3918 EP 3931 DI 10.1093/mnras/stv1869 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CU6OJ UT WOS:000363651600043 ER PT J AU Marinacci, F Vogelsberger, M Mocz, P Pakmor, R AF Marinacci, Federico Vogelsberger, Mark Mocz, Philip Pakmor, Ruediger TI The large-scale properties of simulated cosmological magnetic fields SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE magnetic fields; MHD; methods: numerical; cosmology: theory ID FARADAY-ROTATION MEASURE; ACTIVE GALACTIC NUCLEI; GALAXY CLUSTERS; RADIO-EMISSION; MAGNETOHYDRODYNAMIC SIMULATIONS; IDEAL MAGNETOHYDRODYNAMICS; PLASMA INSTABILITIES; ILLUSTRIS PROJECT; POWER SPECTRUM; DISC GALAXIES AB We perform uniformly sampled large-scale cosmological simulations including magnetic fields with the moving mesh code AREPO. We run two sets of MHD simulations: one including adiabatic gas physics only; the other featuring the fiducial feedback model of the Illustris simulation. In the adiabatic case, the magnetic field amplification follows the B alpha rho(2/3) scaling derived from 'flux-freezing' arguments, with the seed field strength providing an overall normalization factor. At high baryon overdensities the amplification is enhanced by shear flows and turbulence. Feedback physics and the inclusion of radiative cooling change this picture dramatically. In haloes, gas collapses to much larger densities and the magnetic field is amplified strongly and to the same maximum intensity irrespective of the initial seed field of which any memory is lost. At lower densities a dependence on the seed field strength and orientation, which in principle can be used to constrain models of cosmic magnetogenesis, is still present. Inside the most massive haloes magnetic fields reach values of similar to 10-100 mu G, in agreement with galaxy cluster observations. The topology of the field is tangled and gives rise to rotation measure signals in reasonable agreement with the observations. However, the rotation measure signal declines too rapidly towards larger radii as compared to observational data. C1 [Marinacci, Federico; Vogelsberger, Mark] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Mocz, Philip] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Pakmor, Ruediger] Heidelberger Inst Theoret Studien, D-69118 Heidelberg, Germany. RP Marinacci, F (reprint author), MIT, Kavli Inst Astrophys & Space Res, 77 Massachusetts Ave, Cambridge, MA 02139 USA. EM fmarinac@mit.edu OI Mocz, Philip/0000-0001-6631-2566 FU European Research Council [ERC-StG EXAGAL-308037]; DFG Research Centre [SFB-881]; Klaus Tschira Foundation; Magny cluster at the Heidelberg Institute for Theoretical Studies; Stampede supercomputer at the Texas Advanced Computing Center as part of XSEDE projects [TG-AST14007S8, TG-AST140082] FX We thank the referee Robi Banerjee for a constructive report and Dylan Nelson, Annalisa Pillepich, Lars Hernquist, Volker Springel, and Rainer Beck for their valuable suggestions. We further thank Volker Springel for giving us access to the AREPO code. RP acknowledges support by the European Research Council under ERC-StG EXAGAL-308037, by the DFG Research Centre SFB-881 'The Milky Way System', and by the Klaus Tschira Foundation. The simulations were performed on the joint MIT-Harvard computing cluster supported by MKI and FAS, the Magny cluster at the Heidelberg Institute for Theoretical Studies, and the Stampede supercomputer at the Texas Advanced Computing Center as part of XSEDE projects TG-AST14007S8 and TG-AST140082. All the figures in this work were produced by using the MATPLOTLIB graphics environment (Hunter 2007). NR 113 TC 6 Z9 6 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 NOV 11 PY 2015 VL 453 IS 4 BP 3999 EP 4019 DI 10.1093/mnras/stv1692 PG 21 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CU6OJ UT WOS:000363651600048 ER PT J AU See, V Jardine, M Vidotto, AA Donati, JF Folsom, CP Saikia, SB Bouvier, J Fares, R Gregory, SG Hussain, G Jeffers, SV Marsden, SC Morin, J Moutou, C do Nascimento, JD Petit, P Rosen, L Waite, IA AF See, V. Jardine, M. Vidotto, A. A. Donati, J. -F. Folsom, C. P. Saikia, S. Boro Bouvier, J. Fares, R. Gregory, S. G. Hussain, G. Jeffers, S. V. Marsden, S. C. Morin, J. Moutou, C. do Nascimento, J. D., Jr. Petit, P. Rosen, L. Waite, I. A. TI The energy budget of stellar magnetic fields SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE techniques: polarimetric; stars: activity; stars: magnetic field; stars: rotation ID PLANET-HOSTING STAR; PRE-MAIN-SEQUENCE; ACTIVITY-ROTATION RELATIONSHIP; SUN-LIKE STARS; DIFFERENTIAL ROTATION; M DWARFS; ACTIVE STARS; AB-DORADUS; RADIO-EMISSION; TAU-BOOTIS AB Spectropolarimetric observations have been used to map stellar magnetic fields, many of which display strong bands of azimuthal fields that are toroidal. A number of explanations have been proposed to explain how such fields might be generated though none are definitive. In this paper, we examine the toroidal fields of a sample of 55 stars with magnetic maps, with masses in the range 0.1-1.5M(circle dot). We find that the energy contained in toroidal fields has a power-law dependence on the energy contained in poloidal fields. However the power index is not constant across our sample, with stars less and more massive than 0.5M(circle dot) having power indices of 0.72 +/- 0.08 and 1.25 +/- 0.06, respectively. There is some evidence that these two power laws correspond to stars in the saturated and unsaturated regimes of the rotation-activity relation. Additionally, our sample shows that strong toroidal fields must be generated axisymmetrically. The latitudes at which these bands appear depend on the stellar rotation period with fast rotators displaying higher latitude bands than slow rotators. The results in this paper present new constraints for future dynamo studies. C1 [See, V.; Jardine, M.] Univ St Andrews, Sch Phys & Astron, SUPA, St Andrews KY16 9SS, Fife, Scotland. [Vidotto, A. A.] Univ Geneva, Observ Geneve, CH-1290 Sauverny, Switzerland. [Donati, J. -F.; Petit, P.] Univ Toulouse, Inst Rech Astrophys & Planetol, UPS OMP, F-31400 Toulouse, France. [Donati, J. -F.; Petit, P.] CNRS, Inst Rech Astrophys & Planetol, F-31400 Toulouse, France. [Folsom, C. P.; Bouvier, J.] Univ Grenoble Alpes, IPAG, F-38000 Grenoble, France. [Folsom, C. P.; Bouvier, J.] CNRS, IPAG, F-38000 Grenoble, France. [Saikia, S. Boro] Univ Gottingen, Inst Astrophys, D-37077 Gottingen, Germany. [Fares, R.] INAF Osservatorio Astrofis Catania, I-95123 Catania, Italy. [Hussain, G.] ESO, D-85748 Garching, Germany. [Marsden, S. C.; Waite, I. A.] Univ So Queensland, Computat Engn & Sci Res Ctr, Toowoomba, Qld 4350, Australia. [Morin, J.] CNRS, LUPM UMR5299, F-34095 Montpellier, France. [Morin, J.] Univ Montpellier 2, F-34095 Montpellier, France. [Moutou, C.] CNRS, Canada France Hawaii Telescope Corp, Kamuela, HI 96743 USA. [Moutou, C.] Aix Marseille Univ, CNRS, LAM, UMR 7326, F-13388 Marseille, France. [do Nascimento, J. D., Jr.] Univ Fed Rio Grande do Norte, Dept Fis Teor & Expt, BR-59072970 Natal, RN, Brazil. [do Nascimento, J. D., Jr.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Rosen, L.] Uppsala Univ, Dept Phys & Astron, SE-75120 Uppsala, SE, Sweden. RP See, V (reprint author), Univ St Andrews, Sch Phys & Astron, SUPA, St Andrews KY16 9SS, Fife, Scotland. EM wcvs@st-andrews.ac.uk OI Petit, Pascal/0000-0001-7624-9222; Boro Saikia, Sudeshna/0000-0002-3673-3746; Morin, Julien/0000-0002-4996-6901; Gregory, Scott/0000-0003-3674-5568; Vidotto, Aline/0000-0001-5371-2675 FU Science & Technology Facilities Council (STFC); Swiss National Science Foundation; Deutsche Forchungsgemeinschaft (DFG) under grant SFB; STFC [ST/J003255/1]; ANR [Blanc SIMI5-6 020 01] FX The authors thank the anonymous referee for their constructive comments. VS acknowledges the support of an Science & Technology Facilities Council (STFC) studentship. AAV acknowledges support from the Swiss National Science Foundation through an Ambizione Fellowship. SBS and SVJ acknowledge research funding by the Deutsche Forchungsgemeinschaft (DFG) under grant SFB, project A16. SGG acknowledges support from the STFC via an Ernest Rutherford Fellowship [ST/J003255/1]. This study was supported by the grant ANR 2011 Blanc SIMI5-6 020 01 'Toupies: Towards understanding the spin evolution of stars' (http://ipag.osug.fr/Anr_Toupies/). This work is based on observations obtained with ESPaDOnS at the CFHT and with NARVAL at the TBL. CFHT/ESPaDOnS are operated by the National Research Council of Canada, the Institut National des Sciences de l'Univers of the Centre National de la Recherche Scientifique (INSU/CNRS) of France and the University of Hawaii, while TBL/NARVAL are operated by INSU/CNRS. We thank the CFHT and TBL staff for their help during the observations. NR 50 TC 12 Z9 12 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 NOV 11 PY 2015 VL 453 IS 4 BP 4301 EP 4310 DI 10.1093/mnras/stv1925 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CU6OJ UT WOS:000363651600069 ER PT J AU Bakos, GA Penev, K Bayliss, D Hartman, JD Zhou, G Brahm, R Mancini, L de Val-Borro, M Bhatti, W Jordan, A Rabus, M Espinoza, N Csubry, Z Howard, AW Fulton, BJ Buchhave, LA Ciceri, S Henning, T Schmidt, B Isaacson, H Noyes, RW Marcy, GW Suc, V Howe, AR Burrows, AS Lazar, J Papp, I Sari, P AF Bakos, G. A. Penev, K. Bayliss, D. Hartman, J. D. Zhou, G. Brahm, R. Mancini, L. de Val-Borro, M. Bhatti, W. Jordan, A. Rabus, M. Espinoza, N. Csubry, Z. Howard, A. W. Fulton, B. J. Buchhave, L. A. Ciceri, S. Henning, T. Schmidt, B. Isaacson, H. Noyes, R. W. Marcy, G. W. Suc, V. Howe, A. R. Burrows, A. S. Lazar, J. Papp, I. Sari, P. TI HATS-7b: A HOT SUPER NEPTUNE TRANSITING A QUIET K DWARF STAR SO ASTROPHYSICAL JOURNAL LA English DT Article DE stars: individual (HATS-7); techniques: photometric; techniques: radial velocities; techniques: spectroscopic ID HATSOUTH SURVEY; PLANET SEARCH; LIGHT CURVES; MASS PLANET; TELESCOPE; FIELD; ATMOSPHERE; EXOPLANET; JUPITERS; MODELS AB We report the discovery by the HATSouth network of HATS-7b, a transiting Super-Neptune with a mass of 0.120 +/- 0.012 M-J, a radius of 0.563(-0.034)(+0.046) R-J, and an orbital period of 3.1853 days. The host star is a moderately bright (V = 13.340 +/- 0.010 mag, K-S = 10.976 +/- 0.026 mag) K dwarf star with a mass of 0.849 +/- 0.027 M-circle dot, a radius of 0.815(-0.035)(+0.049) R-circle dot, and a metallicity of [Fe/H]= +0.250 +/- 0.080. The star is photometrically quiet to within the precision of the HATSouth measurements, has low RV jitter, and shows no evidence for chromospheric activity in its spectrum. HATS-7b is the second smallest radius planet discovered by a wide-field ground-based transit survey, and one of only a handful of Neptune-size planets with mass and radius determined to 10% precision. Theoretical modeling of HATS-7b yields a hydrogen-helium fraction of 18 +/- 4% (rock-iron core and H-2-He envelope), or 9 +/- 4% (ice core and H-2-He envelope), i.e., it has a composition broadly similar to that of Uranus and Neptune, and very different from that of Saturn, which has 75% of its mass in H-2-He. Based on a sample of transiting exoplanets with accurately (<20%) determined parameters, we establish approximate power-law relations for the envelopes of the mass-density distribution of exoplanets. HATS-7b, which, together with the recently discovered HATS-8b, is one of the first two transiting super-Neptunes discovered in the Southern sky, is a prime target for additional follow-up observations with Southern hemisphere facilities to characterize the atmospheres of Super-Neptunes (which we define as objects with mass greater than that of Neptune, and smaller than halfway between that of Neptune and Saturn, i.e., 0.054M(J) < M-p < 0.18M(J)). C1 [Bakos, G. A.; Penev, K.; Hartman, J. D.; Zhou, G.; de Val-Borro, M.; Bhatti, W.; Csubry, Z.; Howe, A. R.; Burrows, A. S.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. [Bayliss, D.; Zhou, G.; Schmidt, B.] Australian Natl Univ, Res Sch Astron & Astrophys, Canberra, ACT 2611, Australia. [Bayliss, D.] Univ Geneva, Astron Observ, CH-1290 Versoix, Switzerland. [Brahm, R.; Jordan, A.; Rabus, M.; Espinoza, N.; Suc, V.] Pontificia Univ Catolica Chile, Fac Fis, Inst Astrofis, Santiago 7820436, Chile. [Brahm, R.; Jordan, A.; Espinoza, N.] Millennium Inst Astrophys, Santiago 7820436, Chile. [Mancini, L.; Rabus, M.; Ciceri, S.; Henning, T.] 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, Ctr Star & Planet Format, DK-1168 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 Bakos, GA (reprint author), Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. 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]; NSF/AST [1108686]; FONDECYT [1130857]; BASAL CATA [PFB-06]; "Millennium Institute of Astrophysics (MAS)" of the Millenium Science Initiative, Chilean Ministry of Economy [IC120009]; CONICYT-PCHA/Doctorado Nacional; ARC [FL0992131]; Robert Martin Ayers Sciences Fund 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 received 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. This work is based on observations made with ESO Telescopes at the La Silla Observatory. 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 2.2 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. 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. G. A. B. wishes to thank the warm hospitality of Adele and Joachim Cranz at the farm Isabis, supporting the operations and service missions of HATSouth. NR 54 TC 7 Z9 7 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 NOV 10 PY 2015 VL 813 IS 2 AR 111 DI 10.1088/0004-637X/813/2/111 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CW8ZU UT WOS:000365288900031 ER PT J AU Flaherty, KM Hughes, AM Rosenfeld, KA Andrews, SM Chiang, E Simon, JB Kerzner, S Wilner, DJ AF Flaherty, Kevin M. Hughes, A. Meredith Rosenfeld, Katherine A. Andrews, Sean M. Chiang, Eugene Simon, Jacob B. Kerzner, Skylar Wilner, David J. TI WEAK TURBULENCE IN THE HD 163296 PROTOPLANETARY DISK REVEALED BY ALMA CO OBSERVATIONS SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; protoplanetary disks; stars: individual (HD 163296); turbulence ID GLOBAL MHD SIMULATIONS; T-TAURI DISKS; ACCRETION DISKS; HERBIG AE/BE; MAGNETOROTATIONAL INSTABILITY; PLANETESIMAL FORMATION; MAGNETIZED ACCRETION; TEMPERATURE-GRADIENT; CIRCUMSTELLAR DISKS; NONLINEAR EVOLUTION AB Turbulence can transport angular momentum in protoplanetary disks and influence the growth and evolution of planets. With spatially and spectrally resolved molecular emission line measurements provided by (sub) millimeter interferometric observations, it is possible to directly measure non-thermal motions in the disk gas that can be attributed to this turbulence. We report a new constraint on the turbulence in the disk around HD 163296, a nearby young A star, determined from Atacama Large Millimeter/submillimeter Array Science Verification observations of four CO emission lines (the CO(3-2), CO(2-1), (CO)-C-13(2-1), and (CO)-O-18(2-1) transitions). The different optical depths for these lines permit probes of non-thermal line-widths at a range of physical conditions (temperature and density) and depths into the disk interior. We derive stringent limits on the non-thermal motions in the upper layers of the outer disk such that any contribution to the line-widths from turbulence is < 3% of the local sound speed. These limits are approximately an order of magnitude lower than theoretical predictions for full-blown magnetohydrodynamic turbulence driven by the magnetorotational instability, potentially suggesting that this mechanism is less efficient in the outer (R greater than or similar to 30 AU) disk than has been previously considered. C1 [Flaherty, Kevin M.; Hughes, A. Meredith] Wesleyan Univ, Dept Astron, Van Vleck Observ, Middletown, CT 06459 USA. [Rosenfeld, Katherine A.; Andrews, Sean M.; Wilner, David J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Chiang, Eugene; Kerzner, Skylar] Univ Calif Berkeley, Dept Earth & Planetary Sci, Berkeley, CA 94720 USA. [Chiang, Eugene] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Simon, Jacob B.] Southwest Res Inst, Dept Space Studies, Boulder, CO 80302 USA. [Simon, Jacob B.] Univ Colorado, JILA, Bouler, CO 80309 USA. [Simon, Jacob B.] NIST, Bouler, CO 80309 USA. RP Flaherty, KM (reprint author), Wesleyan Univ, Dept Astron, Van Vleck Observ, 96 Foss Hill Dr, Middletown, CT 06459 USA. OI Wilner, David/0000-0003-1526-7587 FU NASA Origins of Solar Systems [NNX13AI32G] FX We thank the referee for comments that helped improve the quality of the paper. We gratefully acknowledge support from NASA Origins of Solar Systems grant NNX13AI32G. We also thank Chunhua Qi and Karin Oberg for helpful discussions regarding the structure of CO. This paper makes use of the following ALMA data: ADS/JAO.ALMA#2011.0.00010. SV. ALMA is a partnership of ESO (representing its member states), NSF (USA), and NINS (Japan), together with NRC (Canada), NSC and ASIAA (Taiwan), and KASI (Republic of Korea), 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 cooperate agreement by Associate Universities, Inc. This research made use of Astropy, a community-developed core Python package for Astronomy (Astropy Collaboration et al. 2013). NR 91 TC 20 Z9 20 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 NOV 10 PY 2015 VL 813 IS 2 AR 99 DI 10.1088/0004-637X/813/2/99 PG 21 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CW8ZU UT WOS:000365288900019 ER PT J AU Garcia, JA Steiner, JF McClintock, JE Remillard, RA Grinberg, V Dauser, T AF Garcia, Javier A. Steiner, James F. McClintock, Jeffrey E. Remillard, Ronald A. Grinberg, Victoria Dauser, Thomas TI X-RAY REFLECTION SPECTROSCOPY OF THE BLACK HOLE GX 339-4: EXPLORING THE HARD STATE WITH UNPRECEDENTED SENSITIVITY SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; atomic processes; black hole physics; line: formation; X-rays: individual (GX 339-4) ID PROPORTIONAL COUNTER ARRAY; INNER ACCRETION DISK; LOW/HARD STATE; SWIFT J1753.5-0127; MASS-DISTRIBUTION; LOW-LUMINOSITY; JET POWER; IRON LINE; SPIN; SPECTRA AB We analyze simultaneously six composite RXTE spectra of GX 339-4 in the hard state comprising 77 million counts collected over 196 ks. The source spectra are ordered by luminosity and span the range 1.6%-17% of the Eddington luminosity. Crucially, using our new tool pcacorr, we re-calibrate the data to a precision of 0.1%, an order of magnitude improvement over all earlier work. Using our advanced reflection model relxill, we target the strong features in the component of emission reflected from the disk, namely, the relativistically broadened Fe K emission line, the Fe K edge, and the Compton hump. We report results for two joint fits to the six spectra: For the first fit, we fix the spin parameter to its maximal value (a(*) = 0.998) and allow the inner disk radius R-in to vary. Results include (i) precise measurements of R-in, with evidence that the disk becomes slightly truncated at a few percent of Eddington and (ii) an order-of-magnitude swing with luminosity in the high energy cutoff, which reaches > 890 keV at our lowest luminosity. For the second fit, we make the standard assumption in estimating spin that the inner edge of the accretion disk is located at the innermost stable circular orbit (R-in = RISCO) and find a(*) = 0.95(0.05)(+0.03)(90% confidence, statistical). For both fits, and at the same level of statistical confidence, we estimate that the disk inclination is i = 48 degrees +/- 1 degrees and that the Fe abundance is super-solar, A(Fe) = 5 +/- 1. C1 [Garcia, Javier A.; Steiner, James F.; McClintock, Jeffrey E.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Remillard, Ronald A.; Grinberg, Victoria] MIT, MIT Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Dauser, Thomas] Dr Karl Remeis Observ, D-96049 Bamberg, Germany. [Dauser, Thomas] Erlangen Ctr Astroparticle Phys, D-96049 Erlangen, Germany. RP Garcia, JA (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM javier@head.cfa.harvard.edu; jsteiner@head.cfa.harvard.edu; jem@cfa.harvard.edu; rr@space.mit.edu; grinberg@space.mit.edu; thomas.dauser@sternwarte.uni-erlangen.de OI Garcia, Javier/0000-0003-3828-2448; Remillard, Ronald/0000-0003-4815-0481 FU NASA [NNX11AD08G, NAS8-03060]; NASA Hubble Fellowship [HST-HF-51315.01]; NASA through the Smithsonian Astrophysical Observatory (SAO) [SV3-73016] FX We thank Felix Furst, Michael Nowak, Timothy Kallman, Rubens Reis, Francesco Tombesi, Andrzej Zdziarski, and Jon Miller for useful and valuable discussions. JG and JEM acknowledge the support of NASA grant NNX11AD08G. J. F. S. has been supported by NASA Hubble Fellowship grant HST-HF-51315.01. V. G. acknowledges support provided by NASA through the Smithsonian Astrophysical Observatory (SAO) contract SV3-73016 to MIT for support of the Chandra X-Ray Center (CXC) and Science Instruments; CXC is operated by SAO for and on behalf of NASA under contract NAS8-03060. NR 91 TC 14 Z9 14 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 NOV 10 PY 2015 VL 813 IS 2 AR 84 DI 10.1088/0004-637X/813/2/84 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CW8ZU UT WOS:000365288900004 ER PT J AU Gizis, JE Dettman, KG Burgasser, AJ Camnasio, S Alam, M Filippazzo, JC Cruz, KL Metchev, S Berger, E Williams, PKG AF Gizis, John E. Dettman, Kyle G. Burgasser, Adam J. Camnasio, Sara Alam, Munazza Filippazzo, Joseph C. Cruz, Kelle L. Metchev, Stanimir Berger, Edo Williams, Peter K. G. TI KEPLER MONITORING OF AN L DWARF. II. CLOUDS WITH MULTI-YEAR LIFETIMES SO ASTROPHYSICAL JOURNAL LA English DT Article DE brown dwarfs; stars: activity; stars: atmospheres; stars: individual (WISEP J190648.47+401106.8); starspots ID TIME-SERIES OBSERVATIONS; BRIGHT ULTRACOOL DWARFS; SPITZER-SPACE-TELESCOPE; BROWN DWARFS; T-DWARFS; PHOTOMETRIC VARIABILITY; OPTICAL VARIABILITY; GIANT PLANETS; SPECTROSCOPIC SURVEY; MODEL ATMOSPHERES AB We present Kepler, Spitzer Space Telescope, Gemini-North, MMT, and Kitt Peak observations of the L1 dwarf WISEP J190648.47+401106.8. We find that the Kepler optical light curve is consistent in phase and amplitude over nearly two years of monitoring, with a peak-to-peak amplitude of 1.4%. Spitzer Infrared Array Camera 3.6 mu m observations are in phase with Kepler, with similar light curve shapes and peak-to-peak amplitudes of 1.1%, but at 4.5 mu m, the variability has an amplitude of <0.1%. Chromospheric Ha emission is variable but not synced with the stable Kepler light curve. A single dark spot can reproduce the light curve but is not a unique solution. An inhomogeneous cloud deck, specifically a region of thick cloud cover, can explain the multi-wavelength data of this ultracool dwarf and need not be coupled with the asynchronous magnetic emission variations. The long life of the cloud is in contrast with weather changes seen in cooler brown dwarfs on the timescale of hours and days. C1 [Gizis, John E.; Dettman, Kyle G.] Univ Delaware, Dept Phys & Astron, Newark, DE 19716 USA. [Burgasser, Adam J.] Univ Calif San Diego, Ctr Astrophys & Space Sci, La Jolla, CA 92093 USA. [Camnasio, Sara; Alam, Munazza; Cruz, Kelle L.] CUNY, Dept Phys & Astron, Hunter Coll, New York, NY 10065 USA. [Filippazzo, Joseph C.; Cruz, Kelle L.] Amer Museum Nat Hist, Dept Astrophys, New York, NY 10034 USA. [Filippazzo, Joseph C.] CUNY Coll Staten Isl, Dept Engn Sci & Phys, Staten Isl, NY 10301 USA. [Metchev, Stanimir] Univ Western Ontario, Dept Phys & Astron, London, ON N6A 3K7, Canada. [Berger, Edo; Williams, Peter K. G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Gizis, JE (reprint author), Natl Opt Astron Observ, Kitt Peak Natl Observ, Tucson, AZ 85719 USA. OI Gizis, John/0000-0002-8916-1972; Metchev, Stanimir/0000-0003-3050-8203; Williams, Peter/0000-0003-3734-3587; Filippazzo, Joseph/0000-0002-0201-8306; Alam, Munazza/0000-0003-4157-832X FU NASA Science Mission directorate; NASA [NNX13AC18G]; NASA by JPL/Caltech; NSF FX This paper includes data collected by the Kepler mission. Funding for the Kepler mission is provided by the NASA Science Mission directorate. The material is based upon work supported by NASA under award No. NNX13AC18G. This work is based in part on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory of the California Institute of Technology, under a contract with NASA. Support for this work was provided by NASA through an award issued by JPL/Caltech. Some of the observations reported here were obtained at the MMT Observatory, a joint facility of the Smithsonian Institution and the University of Arizona. MMT telescope time was granted by NOAO, through the Telescope System Instrumentation Program (TSIP). TSIP is funded by NSF. This work is based in part on observations obtained at the Gemini Observatory, which is operated by the Association of Universities for Research in Astronomy (AURA) under a cooperative agreement with the NSF on behalf of the Gemini partnership: the National Science Foundation (United States), the Science and Technology Facilities Council (United Kingdom), the National Research Council (Canada), CONICYT (Chile), the Australian Research Council (Australia), CNPq (Brazil), and CONICET (Argentina). This research has made use of NASA's Astrophysics Data System, the VizieR catalog access tool, CDS, Strasbourg, France, and the NASA/IPAC Infrared Science Archive, which is operated by the Jet Propulsion Laboratory of the California Institute of Technology, under contract with NASA. This work made use of PyKE (Still & Barclay 2012), a software package for the reduction and analysis of Kepler data. This open source software project is developed and distributed by the NASA Kepler Guest Observer Office. This research has made use of IRAF, Astropy, a community-developed core Python package for Astronomy (Astropy Collaboration et al. 2013), and the triangle plotting code (Foreman-Mackey et al. 2014). IRAF is distributed by the National Optical Astronomy Observatory, which is operated by the Association of Universities for Research in Astronomy (AURA) under cooperative agreement with the National Science Foundation. NR 68 TC 6 Z9 6 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 NOV 10 PY 2015 VL 813 IS 2 AR 104 DI 10.1088/0004-637X/813/2/104 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CW8ZU UT WOS:000365288900024 ER PT J AU Johnson, MD Loeb, A Shiokawa, H Chael, AA Doeleman, SS AF Johnson, Michael D. Loeb, Abraham Shiokawa, Hotaka Chael, Andrew A. Doeleman, Sheperd S. TI MEASURING THE DIRECTION AND ANGULAR VELOCITY OF A BLACK HOLE ACCRETION DISK VIA LAGGED INTERFEROMETRIC COVARIANCE SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; black hole physics; Galaxy: center; techniques: high angular resolution; techniques: interferometric ID SAGITTARIUS-A-ASTERISK; GENERAL-RELATIVISTIC MAGNETOHYDRODYNAMICS; SCATTER-BROADENED IMAGE; SGR-A; GALACTIC-CENTER; EVENT-HORIZON; LINEAR-POLARIZATION; FLARING STRUCTURES; STELLAR ORBITS; INTRINSIC SIZE AB We show that interferometry can be applied to study irregular, rapidly rotating structures, as are expected in the turbulent accretion flow near a black hole. Specifically, we analyze the lagged covariance between interferometric baselines of similar lengths but slightly different orientations. For a flow viewed close to face-on, we demonstrate that the peak in the lagged covariance indicates the direction and angular velocity of the emission pattern from the flow. Even for moderately inclined flows, the covariance robustly estimates the flow direction, although the estimated angular velocity can be significantly biased. Importantly, measuring the direction of the flow as clockwise or counterclockwise on the sky breaks a degeneracy in accretion disk inclinations when analyzing time-averaged images alone. We explore the potential efficacy of our technique using three-dimensional, general relativistic magnetohydrodynamic simulations, and we highlight several baseline pairs for the Event Horizon Telescope (EHT) that are well-suited to this application. These results indicate that the EHT may be capable of estimating the direction and angular velocity of the emitting material near Sgr A*, and they suggest that a rotating flow may even be utilized to improve imaging capabilities. C1 [Johnson, Michael D.; Loeb, Abraham; Shiokawa, Hotaka; Chael, Andrew A.; Doeleman, Sheperd S.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Shiokawa, Hotaka] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Doeleman, Sheperd S.] MIT, Haystack Observ, Westford, MA 01886 USA. RP Johnson, MD (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM mjohnson@cfa.harvard.edu FU National Science Foundation [AST-1310896, AST-1312034, AST-1211539, AST-1440254]; Gordon and Betty Moore Foundation [GBMF-3561] FX We are pleased to acknowledge Charles Gammie for providing computation resources for the simulation, Scott Noble for originally developing HARM3D and the radiative transfer code we used, Olek Sadowski for discussions about orbital dynamics of thick accretion disks, and Laura Vertatschitsch for providing the Python code to generate Figure 4. We thank the National Science Foundation (AST-1310896, AST-1312034, AST-1211539, and AST-1440254) and the Gordon and Betty Moore Foundation (#GBMF-3561) for financial support of this work. NR 67 TC 5 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 NOV 10 PY 2015 VL 813 IS 2 AR 132 DI 10.1088/0004-637X/813/2/132 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CW8ZU UT WOS:000365288900052 ER PT J AU King, C Brown, WR Geller, MJ Kenyon, SJ AF King, Charles, III Brown, Warren R. Geller, Margaret J. Kenyon, Scott J. TI STELLAR VELOCITY DISPERSION AND ANISOTROPY OF THE MILKY WAY INNER HALO SO ASTROPHYSICAL JOURNAL LA English DT Article DE Galaxy: formation; Galaxy: fundamental parameters; Galaxy: halo; Galaxy: kinematics and dynamics; Galaxy: structure; stars: Population II ID HORIZONTAL-BRANCH STARS; SURVEY GALACTIC HALO; DIGITAL SKY SURVEY; SAGITTARIUS DWARF GALAXY; DARK-MATTER HALO; TRIGONOMETRIC PARALLAXES; MASS-DISTRIBUTION; KINEMATICS; SDSS; SUBSTRUCTURE AB We measure the three components of velocity dispersion, sigma(R), sigma(theta), sigma(phi), for stars within 6 < R < 30 kpc of the Milky Way using a new radial velocity sample from the MMT telescope. We combine our measurements with previously published data so that we can more finely sample the stellar halo. We use a maximum likelihood statistical method for estimating mean velocities, dispersions, and covariances assuming only that velocities are normally distributed. The alignment of the velocity ellipsoid is consistent with a spherically symmetric gravitational potential. From the spherical Jeans equation, the mass of the Milky Way is M( R <= 12 kpc) = 1.3 x 10(11) M-circle dot with an uncertainty of 40%. We also find a region of discontinuity, 15 less than or similar to R less than or similar to 25 kpc, where the estimated velocity dispersions and anisotropies diverge from their anticipated values, confirming the break observed by others. We argue that this break in anisotropy is physically explained by coherent stellar velocity structure in the halo, such as the Sgr stream. To significantly improve our understanding of halo kinematics will require combining radial velocities with future Gaia proper motions. C1 [King, Charles, III; Brown, Warren R.; Geller, Margaret J.; Kenyon, Scott J.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. [King, Charles, III] Pleiades Consulting Grp Inc, Lincoln, MA 01773 USA. RP King, C (reprint author), Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA. EM cking@cfa.harvard.edu; wbrown@cfa.harvard.edu; mgeller@cfa.harvard.edu; skenyon@cfa.harvard.edu OI Kenyon, Scott/0000-0003-0214-609X; Geller, Margaret/0000-0002-9146-4876 FU Smithsonian Astrophysical Observatory; Smithsonian Institution; Pleiades Consulting Group, Inc. FX We thank Mike Alegria, Perry Berlind, Mike Calkins, Nelson Caldwell, Scott Gotilla, John McAfee, Erin Martin, and Ale Milone for their assistance with observations obtained at the MMT Observatory, a joint facility of the Smithsonian Institution and the University of Arizona. We also thank William B. Simpson for helpful comments, Alis J. Deason for kindly providing data for Figure 12, and David R. Law for kindly providing the Sgr N-body model. C.K. dedicates this work to Carlos A. Berenstein. This paper uses data products created by the OIR Telescope Data Center, supported by the Smithsonian Astrophysical Observatory, and data products from the Sloan Digital Sky Survey, which is managed by the Astrophysical Research Consortium for the Participating Institutions. This research also makes use of NASA's Astrophysics Data System Bibliographic Services. This work was supported by the Smithsonian Institution. C.K. gratefully acknowledges additional support from the Pleiades Consulting Group, Inc. NR 74 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 NOV 10 PY 2015 VL 813 IS 2 AR 89 DI 10.1088/0004-637X/813/2/89 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CW8ZU UT WOS:000365288900009 ER PT J AU Pe'er, A Barlow, H O'Mahony, S Margutti, R Ryde, F Larsson, J Lazzati, D Livio, M AF Pe'er, Asaf Barlow, Hugh O'Mahony, Shane Margutti, Raffaella Ryde, Felix Larsson, Josefin Lazzati, Davide Livio, Mario TI HYDRODYNAMIC PROPERTIES OF GAMMA-RAY BURSTS OUTFLOWS DEDUCED FROM THE THERMAL COMPONENT SO ASTROPHYSICAL JOURNAL LA English DT Article DE gamma rays: stars; hydrodynamics; methods: data analysis; radiation mechanisms: thermal; radiative transfer ID SYNCHROTRON SHOCK MODEL; PROMPT EMISSION; PHOTOSPHERIC EMISSION; PEAK ENERGY; RELATIVISTIC JETS; SPECTRAL CATALOG; MAGNETIC-FIELDS; COLLAPSAR-JETS; LORENTZ FACTOR; GRB 100316D AB We study the properties of a significant thermal emission component that was identified in 47 gamma-ray bursts observed by different instruments. Within the framework of the "fireball" model, we deduce the values of the Lorentz factor Gamma, and the acceleration radius, r(0), for these bursts. We find that all the values of Gamma in our sample are in the range 10(2) <= Gamma <= 10(3), with = 370. We find a very weak dependence of Gamma on the acceleration radius r0, Gamma proportional to r(0)(alpha) with alpha - -0.10 +/- 0.09 at the sigma - 2.1 confidence level. The values of r(0) span a wide range, 10(6.5) <= r(0) <= 10(9.5) cm, with a mean value of < r(0)> similar to 10(8) cm. This is higher than the gravitational radius of a 10 M-circle dot black hole by a factor of approximate to 30. We argue that this result provides indirect evidence for jet propagation inside a massive star, and suggests the existence of recollimation shocks that take place close to this radius. C1 [Pe'er, Asaf; Barlow, Hugh; O'Mahony, Shane] Natl Univ Ireland Univ Coll Cork, Dept Phys, Cork, Ireland. [Margutti, Raffaella] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Ryde, Felix; Larsson, Josefin] Oskar Klein Ctr Cosmoparticle Phys, SE-10691 Stockholm, Sweden. [Ryde, Felix; Larsson, Josefin] KTH Royal Inst Technol, Dept Phys, AlbaNova, SE-10691 Stockholm, Sweden. [Lazzati, Davide] Oregon State Univ, Dept Phys, Corvallis, OR 97331 USA. RP Pe'er, A (reprint author), Natl Univ Ireland Univ Coll Cork, Dept Phys, Cork, Ireland. OI /0000-0003-0065-2933; Ryde, Felix/0000-0002-9769-8016; Margutti, Raffaella/0000-0003-4768-7586 FU European Union [618499]; National Science Foundation [PHYS-1066293] FX A.P. wishes to thank Miguel Aloy for useful discussions. We would like to thank Mohammed Basha, Kim Page, and Motoko Serino for providing us with direct access to their data. We would further like to thank the referee, Dr. Bing Zhang, for useful comments, that helped us improve this manuscript. This research was partially supported by the European Union Seventh Framework Programme (FP7/2007-2013) under grant agreement no 618499. This work was supported in part by National Science Foundation grant No. PHYS-1066293 and the hospitality of the Aspen Center for Physics. NR 98 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 NOV 10 PY 2015 VL 813 IS 2 AR 127 DI 10.1088/0004-637X/813/2/127 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CW8ZU UT WOS:000365288900047 ER PT J AU Qi, CH Oberg, KI Andrews, SM Wilner, DJ Bergin, EA Hughes, AM Hogherheijde, M D'Alessio, P AF Qi, Chunhua Oeberg, Karin I. Andrews, Sean M. Wilner, David J. Bergin, Edwin A. Hughes, A. Meredith Hogherheijde, Michiel D'Alessio, Paola TI CHEMICAL IMAGING OF THE CO SNOW LINE IN THE HD 163296 DISK SO ASTROPHYSICAL JOURNAL LA English DT Article DE astrochemistry; ISM: molecules; protoplanetary disks; radio lines: ISM; stars: formation; techniques: high angular resolution ID PROTOPLANETARY DISKS; MOLECULAR-EXCITATION; CIRCUMSTELLAR DISKS; DARK CLOUD; PROTOSTARS; CHEMISTRY; EVOLUTION; DEPLETION; SURFACE; SOLAR AB The condensation fronts (snow lines) of H2O, CO, and other abundant volatiles in the midplane of a protoplanetary disk affect several aspects of planet formation. Locating the CO snow line, where the CO gas column density is expected to drop substantially, based solely on CO emission profiles, is challenging. This has prompted an exploration of chemical signatures of CO freeze-out. We present ALMA Cycle 1 observations of the N2H+ J - 3 - 2 and DCO+ J = 4-3 emission lines toward the disk around the Herbig Ae star HD 163296 at similar to 0.'' 5 (60 AU) resolution, and evaluate their utility as tracers of the CO snow line location. The N2H+ emission is distributed in a ring with an inner radius at 90 AU, corresponding to a midplane temperature of 25 K. This result is consistent with a new analysis of optically thin (CO)-O-18 data, which implies a sharp drop in CO abundance at 90 AU. Thus N2H+ appears to be a robust tracer of the midplane CO snow line. The DCO+ emission also has a ring morphology, but neither the inner nor the outer radius coincide with the CO snow line location of 90 AU, indicative of a complex relationship between DCO+ emission and CO freeze-out in the disk midplane. Compared to TW Hya, CO freezes out at a higher temperature in the disk around HD 163296 (25 versus 17 K in the TW Hya disk), perhaps due to different ice compositions. This highlights the importance of actually measuring the CO snow line location, rather than assuming a constant CO freeze-out temperature for all disks. C1 [Qi, Chunhua; Oeberg, Karin I.; Andrews, Sean M.; Wilner, David J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Bergin, Edwin A.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Hughes, A. Meredith] Wesleyan Univ, Dept Astron, Van Vleck Observ, Middletown, CT 06459 USA. [Hogherheijde, Michiel] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [D'Alessio, Paola] Univ Nacl Autonoma Mexico, Ctr Radioastron & Astrofis, Morelia 58089, Michoacan, Mexico. RP Qi, CH (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. OI Wilner, David/0000-0003-1526-7587 FU NASA Origins of Solar Systems grant [NNX11AK63]; [2012.1.00681.S] FX This paper makes use of the following ALMA data: ADS/JAO. ALMA#2012.1.00681.S and ADS/JAO.ALMA#2011.0.00010. 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. We acknowledge NASA Origins of Solar Systems grant No. NNX11AK63. This paper is dedicated to the memory of Paola D'Alessio, who was one of the co-Is of project 2012.1.00681.S and passed away in 2013 November. NR 33 TC 0 Z9 0 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 NOV 10 PY 2015 VL 813 IS 2 AR 128 DI 10.1088/0004-637X/813/2/128 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CW8ZU UT WOS:000365288900048 ER PT J AU Ricci, L Maddison, ST Wilner, D MacGregor, MA Ubach, C Carpenter, JM Testi, L AF Ricci, L. Maddison, S. T. Wilner, D. MacGregor, M. A. Ubach, C. Carpenter, J. M. Testi, L. TI AN ATCA SURVEY OF DEBRIS DISKS AT 7 MILLIMETERS SO ASTROPHYSICAL JOURNAL LA English DT Article DE circumstellar matter; planets and satellites: formation; stars: individual (HD107146); submillimeter: stars ID BETA-PICTORIS; COLLISIONAL CASCADES; HD 107146; HR 8799; PLANETS; DISTRIBUTIONS; SPECTROSCOPY; EXOPLANETS; TELESCOPE; EVOLUTION AB We present Australia Telescope Compact Array continuum observations at a wavelength of 6.8 mm of five debris disks: beta Pictoris, q(1) Eridani, HD 107146, HD 181327, and HD 95086. These observations provide the detection at the longest wavelengths obtained to date for all these debris disks. By combining our 6.8 mm data with previous detections at shorter sub-millimeter/millimeter wavelengths we measure the long wavelength spectral index of these sources. We then use previous estimates for the temperature of the emitting dust to derive the spectral index of the dust emissivity. Under the assumption that all the detected flux comes from dust only, we constrain the slope of the solid size distribution, assumed to be a power-law. The values that we infer for the slope of the size distribution range between about 3.36 and 3.50. We compare our findings with the case of the Fomalhaut debris disk and use these results to test the predictions of collisional cascades of planetesimal belts. C1 [Ricci, L.; Wilner, D.; MacGregor, M. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Maddison, S. T.] Swinburne Univ Technol, Ctr Astrophys & Supercomp, Hawthorn, Vic 3122, Australia. [Ubach, C.] North Amer ALMA Sci Ctr, Natl Radio Astron Observ, Charlottesville, VA 22903 USA. [Carpenter, J. M.] CALTECH, Dept Astron, Pasadena, CA 91125 USA. [Testi, L.] European Southern Observ ESO Headquarters, D-85748 Garching, Germany. RP Ricci, L (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM luca.ricci@cfa.harvard.edu OI MacGregor, Meredith/0000-0001-7891-8143; Wilner, David/0000-0003-1526-7587 FU Commonwealth of Australia FX 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. NR 50 TC 4 Z9 4 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 NOV 10 PY 2015 VL 813 IS 2 AR 138 DI 10.1088/0004-637X/813/2/138 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CW8ZU UT WOS:000365288900058 ER PT J AU King, AL Miller, JM Raymond, J Reynolds, MT Morningstar, W AF King, Ashley L. Miller, Jon M. Raymond, John Reynolds, Mark T. Morningstar, Warren TI HIGH-RESOLUTION CHANDRA HETG SPECTROSCOPY OF V404 CYGNI IN OUTBURST SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE accretion, accretion disks; black hole physics; ISM: jets and outflows; X-rays: binaries ID X-RAY BINARIES; BLACK-HOLE; INFRARED-SPECTROSCOPY; GRS 1915+105; DISK WINDS; ACCRETION; MASS; CONTAMINATION; RADIATION; STELLAR AB As one of the best-characterized stellar-mass black holes, with good measurements of its mass, distance, and inclination, V404 Cyg is the ideal candidate to study Eddington-limited accretion episodes. After a long quiescent period, V404 Cyg underwent a new outburst in 2015 June. We obtained two Chandra HETG exposures of 20 and 25 ks. Many strong emission lines are observed; the ratio of Si He-like triplet lines gives an estimate for the formation region distance of 4 x 10(11) cm. A narrow Fe K alpha line is detected with an equivalent width greater than 1 keV in many epochs, signaling that we do not directly observe the central engine. Obscuration of the central engine and strong narrow emission lines signal that the outer disk may be illuminated, and its structure may help to drive the strong variability observed in V404 Cyg. In the highest flux phases, strong P-Cygni profiles consistent with a strong disk wind are observed, likely radiation or thermally driven as V404 Cyg approaches its Eddington limit. The kinetic power of this wind may be extremely high at >0.1 L-Bol. C1 [King, Ashley L.; Morningstar, Warren] Stanford Univ, Dept Phys, Stanford, CA 94305 USA. [Miller, Jon M.; Reynolds, Mark T.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Raymond, John] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP King, AL (reprint author), Stanford Univ, Dept Phys, 382 Via Pueblo Mall, Stanford, CA 94305 USA. EM ashking@stanford.edu FU NASA through Einstein Postdoctoral Fellowship [PF4-150125]; NASA [NAS8-03060] FX The authors thank the anonymous referee for their invaluable comments. The authors also thank Belinda Wilkes for this DDT, as well as Herman Marshall, David Huenemoerder, and the Chandra team for their invaluable help. A.L.K. would like to thank the support for this work, which was provided by NASA through Einstein Postdoctoral Fellowship grant number PF4-150125 awarded by the Chandra X-ray Center, operated by the Smithsonian Astrophysical Observatory for NASA under contract NAS8-03060. NR 39 TC 13 Z9 13 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 NOV 10 PY 2015 VL 813 IS 2 AR L37 DI 10.1088/2041-8205/813/2/L37 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CW5KT UT WOS:000365035000015 ER PT J AU Valenti, S Sand, DJ Barth, AJ Horne, K Treu, T Raganit, L Boroson, T Crawford, S Pancoast, A Pei, L Romero-Colmenero, E Villforth, C Winkler, H AF Valenti, S. Sand, D. J. Barth, A. J. Horne, K. Treu, T. Raganit, L. Boroson, T. Crawford, S. Pancoast, A. Pei, L. Romero-Colmenero, E. Villforth, C. Winkler, H. TI ROBOTIC REVERBERATION MAPPING OF ARP 151 SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE galaxies: active; galaxies: individual (Arp 151); galaxies: nuclei; galaxies: Seyfert; techniques: spectroscopic ID AGN MONITORING PROJECT; ACTIVE GALACTIC NUCLEI; BROAD-LINE REGION; SUPERMASSIVE BLACK-HOLES; VELOCITY-DELAY MAPS; DYNAMICAL MODELS; SEYFERT-GALAXIES; MASS; EMISSION; CALIBRATION AB We present the first results from the Las Cumbres Observatory Global Telescope (LCOGT) Network's Active Galactic Nuclei (AGNs) Key Project, a large program devoted to using the robotic resources of LCOGT to perform time domain studies of active galaxies. We monitored the Seyfert 1 galaxy Arp. 151 (Mrk. 40) for similar to 200 days with robotic imagers and with the FLOYDS robotic spectrograph at Faulkes Telescope North. Arp. 151 was highly variable during this campaign, with V-band light curve variations of similar to 0.3 mag and H beta flux changing by a factor of similar to 3. We measure robust time lags between the V-band continuum and the H alpha, H beta, and H gamma emission lines, with tau(cen) = 13.89(-1.41)(+1.39),7.52(-1.06)(+1.43), and 7.40(-1.32)(+1.50) days, respectively. The lag for the He II lambda 4686 emission line is unresolved. We measure a velocity-resolved lag for the H beta line, which is clearly asymmetric with higher lags on the blue wing of the line that decline to the red, possibly indicative of radial inflow, and is similar in morphology to past observations of the H beta transfer function shape. Assuming a virialization factor of f = 5.5, we estimate a black hole mass of M-BH = 6.2(-1.2)(+1.4) x 10(6)M(circle dot), also consistent with past measurements for this object. These results represent the first step to demonstrate the powerful robotic capabilities of LCOGT for long-term AGN time domain campaigns that human intensive programs cannot easily accomplish. Arp 151 is now one of just a few AGNs where the virial product is known to remain constant against substantial changes in H beta lag and luminosity. C1 [Valenti, S.; Boroson, T.] Las Cumbres Observ Global Telescope Network, Goleta, CA 93117 USA. [Valenti, S.; Treu, T.] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA. [Sand, D. J.; Raganit, L.] Texas Tech Univ, Dept Phys, Lubbock, TX 79409 USA. [Barth, A. J.; Pei, L.] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA. [Horne, K.; Villforth, C.] Univ St Andrews, SUPA Sch Phys & Astron, North Haugh KY16 9SS, Fife, Scotland. [Treu, T.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. [Crawford, S.] S African Astron Observ, ZA-7935 Cape Town, South Africa. [Pancoast, A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Romero-Colmenero, E.] Southern African Large Telescope Fdn, ZA-7935 Cape Town, South Africa. [Villforth, C.] Univ Bath, Dept Phys, Bath BA2 7AY, Avon, England. [Winkler, H.] Univ Johannesburg, Dept Phys, ZA-2006 Auckland Pk, South Africa. RP Valenti, S (reprint author), Las Cumbres Observ Global Telescope Network, 6740 Cortona Dr,Suite 102, Goleta, CA 93117 USA. RI Winkler, Hartmut/F-3367-2013; OI Winkler, Hartmut/0000-0003-2662-0526; Crawford, Steven/0000-0002-8969-5229; Sand, David/0000-0003-4102-380X; Barth, Aaron/0000-0002-3026-0562 FU NSF [AST-1412693, AST-1412504, AST-1517649, AST-1412315]; Packard Research Fellowship; National Research Foundation (NRF) of South Africa FX Research by A.J.B. and L.P. are supported by NSF grant AST-1412693. Research by D.J.S. is supported by NSF grant AST-1412504 and AST-1517649. Research by T.T. is supported by NSF grant AST-1412315 and a Packard Research Fellowship. E.R.C. and S.C. gratefully acknowledge the receipt of research grants from the National Research Foundation (NRF) of South Africa. NR 34 TC 1 Z9 1 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 NOV 10 PY 2015 VL 813 IS 2 AR L36 DI 10.1088/2041-8205/813/2/L36 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CW5KT UT WOS:000365035000014 ER PT J AU Yadav, RK Christensen, UR Morin, J Gastine, T Reiners, A Poppenhaeger, K Wolk, SJ AF Yadav, Rakesh K. Christensen, Ulrich R. Morin, Julien Gastine, Thomas Reiners, Ansgar Poppenhaeger, Katja Wolk, Scott J. TI EXPLAINING THE COEXISTENCE OF LARGE-SCALE AND SMALL-SCALE MAGNETIC FIELDS IN FULLY CONVECTIVE STARS SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE dynamo; methods: numerical; stars: interiors; stars: low-mass; stars: magnetic field ID MAIN-SEQUENCE STARS; M-DWARFS; DIFFERENTIAL ROTATION; DYNAMO ACTION; ACTIVE STARS; COOL STARS; GENERATION; TOPOLOGY; SIMULATIONS; KEPLER AB Despite the lack of a shear-rich tachocline region, low-mass fully convective (FC) stars are capable of generating strong magnetic fields, indicating that a dynamo mechanism fundamentally different from the solar dynamo is at work in these objects. We present a self-consistent three-dimensional model of magnetic field generation in low-mass FC stars. The model utilizes the anelastic magnetohydrodynamic equations to simulate compressible convection in a rotating sphere. A distributed dynamo working in the model spontaneously produces a dipole-dominated surface magnetic field of the observed strength. The interaction of this field with the turbulent convection in outer layers shreds it, producing small-scale fields that carry most of the magnetic flux. The Zeeman-Doppler-Imaging technique applied to synthetic spectropolarimetric data based on our model recovers most of the large-scale field. Our model simultaneously reproduces the morphology and magnitude of the large-scale field as well as the magnitude of the small-scale field observed on low-mass FC stars. C1 [Yadav, Rakesh K.; Poppenhaeger, Katja; Wolk, Scott J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Yadav, Rakesh K.; Christensen, Ulrich R.; Gastine, Thomas] Max Planck Inst Sonnensyst Forsch, D-37077 Gottingen, Germany. [Morin, Julien] Univ Montpellier, LUPM, CNRS, F-34095 Montpellier, France. [Reiners, Ansgar] Univ Gottingen, Inst Astrophys, D-37077 Gottingen, Germany. RP Yadav, RK (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM rakesh.yadav@cfa.harvard.edu RI Yadav, Rakesh/E-2169-2017; OI Yadav, Rakesh/0000-0002-9569-2438; Poppenhaeger, Katja/0000-0003-1231-2194; Morin, Julien/0000-0002-4996-6901; Wolk, Scott/0000-0002-0826-9261 FU DFG [SFB 963/A17, SPP 1488]; NASA [GO4-15011X] FX We thank the anonymous referee and J.-F. Donati for a careful reading and interesting suggestions. Funding from DFG (through SFB 963/A17 and SPP 1488) and NASA (through the Chandra grant GO4-15011X) is acknowledged. Simulations were performed at RZG and GWDG. NR 49 TC 9 Z9 9 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 NOV 10 PY 2015 VL 813 IS 2 AR L31 DI 10.1088/2041-8205/813/2/L31 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CW5KT UT WOS:000365035000009 ER PT J AU Carleton, MD Banasiak, RA Stanley, WT AF Carleton, Michael D. Banasiak, Rebecca A. Stanley, William T. TI A new species of the rodent genus Hylomyscus from Angola, with a distributional summary of the H. anselli species group (Muridae: Murinae: Praomyini) SO ZOOTAXA LA English DT Article DE Afromontane; biogeography; taxonomy; traditional morphometrics ID MORPHOLOGICAL EVOLUTION; AFRICAN GREENBULS; MITOCHONDRIAL-DNA; MUROID RODENTS; FOREST BIRDS; PATTERNS; BIODIVERSITY; BIOGEOGRAPHY; PHYLOGENY; CONSERVATION AB A new species of Hylomyscus, H. heinrichorum, is described from mountains in western Angola. Based on morphological traits and cranial morphometry, the new species is assigned to the H. anselli species group and is hypothesized to be most closely related to H. anselli Bishop proper, a species named from Zambia. Members of both the H. anselli and H. denniae species groups occupy the Afromontane Biotic Zone, found in various mountain systems to the south and east of the Congo Basin. Evidence is reviewed that supports the independent radiation of these two species groups within montane forest from different Guineo-Congolian ancestral stocks. C1 [Carleton, Michael D.] Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Washington, DC 20560 USA. [Banasiak, Rebecca A.; Stanley, William T.] Field Museum Nat Hist, Sci & Educ, Chicago, IL 60605 USA. RP Carleton, MD (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Washington, DC 20560 USA. EM carletonm@si.edu; rbanasiak@fieldmuseum.org; wstanley@fieldmuseum.org FU National Geographic Society [5053-93, 5244-94, 5711-96]; Critical Ecosystem Partnership Fund; Field Museum of Natural History FX This study would not have been possible without the indispensable field assistance of Philip M. Kihaule and Maiko J. Munissi. We acknowledge Steven M. Goodman for his collecting efforts in the East and West Usambara Mts and the South Pare Mts, Tanzania, and T. Davenport and K. M. Howell for their in-country logistical support. Partial financial support for Stanley's field surveys was provided by the National Geographic Society (Grants 5053-93, 5244-94, 5711-96), the Critical Ecosystem Partnership Fund, and the Field Museum of Natural History (Field Museum/IDP Foundation, Inc. African Training Fund, the Barbara Brown, Council on Africa, Ellen Thorne Smith, and Marshall Field Funds). Permits to conduct research in Tanzania were granted to Stanley by the Tanzania Commission for Science and Technology, the Tanzania Wildlife Research Institute, and the Ministry of Natural Resources and Tourism. Our manuscript benefited from the careful reviews of S.M. Goodman, R. Hutterer, and one anonymous referee. Lastly, the authors extend warm appreciation to Dr. Bernd Heinrich, who located old slides preserved from his parents' Angolan expeditions and permitted their reproduction (Figs. 8, 9). NR 76 TC 1 Z9 1 U1 1 U2 7 PU MAGNOLIA PRESS PI AUCKLAND PA PO BOX 41383, AUCKLAND, ST LUKES 1030, NEW ZEALAND SN 1175-5326 EI 1175-5334 J9 ZOOTAXA JI Zootaxa PD NOV 10 PY 2015 VL 4040 IS 2 BP 101 EP 128 PG 28 WC Zoology SC Zoology GA CV7AE UT WOS:000364423000001 PM 26624655 ER PT J AU Santos, LF Perez-Bernal, F AF Santos, Lea F. Perez-Bernal, Francisco TI Structure of eigenstates and quench dynamics at an excited-state quantum phase transition SO PHYSICAL REVIEW A LA English DT Article ID SYSTEMS; CHAOS; MODEL; PROPAGATION; SIGNATURES; SUPERFLUID; MONODROMY; SPECTRUM; GAS AB We study the structure of the eigenstates and the dynamics of a system that undergoes an excited-state quantum phase transition (ESQPT). The analysis is performed for two-level pairing models characterized by a U(n + 1) algebraic structure. They exhibit a second-order phase transition between two limiting dynamical symmetries represented by the U(n) and SO(n + 1) subalgebras. They are, or can be mapped onto, models of interacting bosons. We show that the eigenstates with energies very close to the ESQPT critical point, E-ESQPT, are highly localized in the U(n) basis. Consequently, the dynamics of a system initially prepared in a U(n)-basis vector with energy epsilon similar to E-ESQPT may be extremely slow. Signatures of an ESQPT can therefore be found in the structures of the eigenstates and in the speed of the system evolution after a sudden quench. Our findings can be tested experimentally with trapped ions. C1 [Santos, Lea F.] Yeshiva Univ, Dept Phys, New York, NY 10016 USA. [Santos, Lea F.] Harvard Smithsonian Ctr Astrophys, ITAMP, Cambridge, MA 02138 USA. [Perez-Bernal, Francisco] Univ Huelva, Fac Ciencias Expt, Dept Fis Aplicada, Huelva 21071, Spain. RP Santos, LF (reprint author), Yeshiva Univ, Dept Phys, New York, NY 10016 USA. RI Perez-Bernal, Francisco/K-4401-2014; Santos, Lea/D-5332-2012 OI Perez-Bernal, Francisco/0000-0002-3009-3696; Santos, Lea/0000-0001-9400-2709 FU NSF [DMR-1147430]; MINECO [FIS2011-28738-C02-02, FIS2014-53448-C2-2-P]; Spanish Consolider-Ingenio [CPANCSD2007-00042] FX L.F.S. thanks the ITAMP, where part of this work was done, for its hospitality. We thank Jose M. Arias, Jose E. Garcia-Ramos, Francesco Iachello, and Pedro Perez-Fernandez for useful discussions. L.F.S. was supported by the NSF Grant No. DMR-1147430. F.P.B. was funded by MINECO Grants No. FIS2011-28738-C02-02 and No. FIS2014-53448-C2-2-P and by the Spanish Consolider-Ingenio 2010 (CPANCSD2007-00042). NR 58 TC 11 Z9 11 U1 2 U2 12 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 1050-2947 EI 1094-1622 J9 PHYS REV A JI Phys. Rev. A PD NOV 9 PY 2015 VL 92 IS 5 AR 050101 DI 10.1103/PhysRevA.92.050101 PG 5 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA CV6QW UT WOS:000364396100001 ER PT J AU Xu, QQ Zhou, WJ Kodrul, TM Naugolnykh, SV Jin, JH AF Xu, Qingqing Zhou, Wenjun Kodrul, Tatiana M. Naugolnykh, Serge V. Jin, Jianhua TI Late Eocene white pines (Pinus subgenus Strobus) from southern China SO SCIENTIFIC REPORTS LA English DT Article ID GENUS PINUS; PINACEAE; EVOLUTION; LEAVES; PHYLOGENY; PATTERNS; HISTORY; CONES; WOODS AB Fossil records indicate that the genus Pinus L. split into two subgenera by the Late Cretaceous, although subgenus Strobus (D. Don) Lemmon is less well documented than subgenus Pinus L., especially in eastern Asia. In this paper, Pinus maomingensis sp. nov. is established based on a compressed seed cone from the upper Eocene of the Maoming Basin of southern China. This species is attributed to genus Pinus, subgenus Strobus, section Quinquefoliae Duhamel, subsection Strobus Loudon based on the combination of morphological characters obtained from the cone scales, specifically from the terminal umbo, rhombic apophysis, and cuticle structure. Associated fascicles of needle leaves with deciduous sheaths and bulbous bases are recognized as Pinus sp. and also represent Pinus subgenus Strobus. This new discovery from the Maoming Basin constitutes the first megafossil record of subgenus Strobus from southern China and implies that the members of this subgenus arrived in the southern region of China by the late Eocene. The extant species of subgenus Strobus are mainly distributed in northern temperate and tropical to subtropical mountainous regions. We propose that the Maoming Basin was adjacent to a mountainous region during the late Eocene. C1 [Xu, Qingqing; Zhou, Wenjun; Jin, Jianhua] Sun Yat Sen Univ, Sch Life Sci, State Key Lab Biocontrol, Guangzhou 510275, Guangdong, Peoples R China. [Xu, Qingqing; Zhou, Wenjun; Jin, Jianhua] Sun Yat Sen Univ, Sch Life Sci, Guangdong Prov Key Lab Plant Resources, Guangzhou 510275, Guangdong, Peoples R China. [Xu, Qingqing] Smithsonian Inst, Dept Paleobiol, Natl Museum Nat Hist, Washington, DC 20013 USA. [Kodrul, Tatiana M.; Naugolnykh, Serge V.] Russian Acad Sci, Inst Geol, Moscow 119017, Russia. RP Jin, JH (reprint author), Sun Yat Sen Univ, Sch Life Sci, State Key Lab Biocontrol, Guangzhou 510275, Guangdong, Peoples R China. EM lssjjh@mail.sysu.edu.cn FU National Natural Science Foundation of China [41210001, 41572011]; National Basic Research Program of China (973 Program) [2012CB822003]; joint Project of the National Natural Science Foundation of China; Russian Foundation for Basic Research [413111040, 14-05-91163]; State Key Laboratory of Palaeobiology and Stratigraphy (Nanjing Institute of Geology and Palaeontology, CAS) [123110]; Fundamental Research Funds for the Central Universities [12lgjc04]; Key Project of Sun Yat-sen University; Scientific Research Fund, Hongda Zhang; Sun Yat-sen University; State Project of the Geological Institute, Russian Academy of Sciences [01201459195]; State Scholarship Fund of China Scholarship Council (CSC) [201406380049] FX This study was supported by the National Natural Science Foundation of China (Grant Nos. 41210001, 41572011), the National Basic Research Program of China (973 Program) (Grant No. 2012CB822003), the joint Project of the National Natural Science Foundation of China and the Russian Foundation for Basic Research (Grant Nos. 413111040, 14-05-91163), State Key Laboratory of Palaeobiology and Stratigraphy (Nanjing Institute of Geology and Palaeontology, CAS) (Grant No. 123110), the Fundamental Research Funds for the Central Universities (Grant No. 12lgjc04), the Key Project of Sun Yat-sen University for inviting foreign teachers, and the Scientific Research Fund, Hongda Zhang, Sun Yat-sen University, the State Project of the Geological Institute, Russian Academy of Sciences (Grant No. 01201459195) and the State Scholarship Fund of China Scholarship Council (CSC) (No. 201406380049). The authors thank Botany graduate students at Sun Yat-sen University for their field work and fossil collecting. We greatly appreciate the National Museum of Natural History, Smithsonian Institution, especially for letting us use the library resources. We also offer our sincere gratitude to Ms. Margaret Joyner (U.S.A.) for editing and Prof. Conrad Labandeira and Mr. Thomas F. Jorstad (U.S.A.) for modification. NR 53 TC 0 Z9 0 U1 4 U2 26 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 NOV 9 PY 2015 VL 5 AR 16390 DI 10.1038/srep16390 PG 12 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA CV5JQ UT WOS:000364306500001 PM 26548658 ER PT J AU Kelbert, P Droege, G Barker, K Braak, K Cawsey, EM Coddington, J Robertson, T Whitacre, J Guntsch, A AF Kelbert, Patricia Droege, Gabriele Barker, Katharine Braak, Kyle Cawsey, E. Margaret Coddington, Jonathan Robertson, Tim Whitacre, Jamie Guentsch, Anton TI B-HIT - A Tool for Harvesting and Indexing Biodiversity Data SO PLoS One LA English DT Article AB With the rapidly growing number of data publishers, the process of harvesting and indexing information to offer advanced search and discovery becomes a critical bottleneck in globally distributed primary biodiversity data infrastructures. The Global Biodiversity Information Facility (GBIF) implemented a Harvesting and Indexing Toolkit (HIT), which largely automates data harvesting activities for hundreds of collection and observational data providers. The team of the Botanic Garden and Botanical Museum Berlin-Dahlem has extended this well-established system with a range of additional functions, including improved processing of multiple taxon identifications, the ability to represent associations between specimen and observation units, new data quality control and new reporting capabilities. The open source software B-HIT can be freely installed and used for setting up thematic networks serving the demands of particular user groups. C1 [Kelbert, Patricia; Droege, Gabriele; Guentsch, Anton] Free Univ Berlin, Bot Garden, Berlin, Germany. [Kelbert, Patricia; Droege, Gabriele; Guentsch, Anton] Free Univ Berlin, Bot Museum Berlin Dahlem, Berlin, Germany. [Barker, Katharine; Coddington, Jonathan; Whitacre, Jamie] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA. [Braak, Kyle; Robertson, Tim] Global Biodivers Informat Facil, Copenhagen, Denmark. [Cawsey, E. Margaret] CSIRO Natl Res Collect Australia, Australian Natl Wildlife Collect, Canberra, ACT, Australia. RP Kelbert, P (reprint author), Free Univ Berlin, Bot Garden, Berlin, Germany. EM p.kelbert@bgbm.org OI Braak, Kyle/0000-0002-3696-3496 FU German Research Foundation (DFG) [BE 2283/8-1]; DFG project GGBN [GU 1109/5-1]; National Science Foundation [NSF DEB 0956426] FX The design and implementation of the B-HIT was funded by the German Research Foundation (DFG, http://www.dfg.de) project BiNHum (BE 2283/8-1). The analysis of data for GGBN was funded by the DFG project GGBN (GU 1109/5-1) as well as the National Science Foundation (http://www.nsf.gov, NSF DEB 0956426). The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 15 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 NOV 6 PY 2015 VL 10 IS 11 AR e0142240 DI 10.1371/journal.pone.0142240 PG 9 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA CV6RT UT WOS:000364398700098 PM 26544980 ER PT J AU Reid, JP Schnitzer, SA Powers, JS AF Reid, Joseph Pignatello Schnitzer, Stefan A. Powers, Jennifer S. TI Short and Long-Term Soil Moisture Effects of Liana Removal in a Seasonally Moist Tropical Forest SO PLOS ONE LA English DT Article ID AMAZONIAN FORESTS; TREE REGENERATION; SECONDARY FOREST; EASTERN AMAZONIA; RAIN-FOREST; GROWTH; DYNAMICS; PATTERNS; ABUNDANCE; DROUGHT AB Lianas (woody vines) are particularly abundant in tropical forests, and their abundance is increasing in the neotropics. Lianas can compete intensely with trees for above-and below-ground resources, including water. As tropical forests experience longer and more intense dry seasons, competition for water is likely to intensify. However, we lack an understanding of how liana abundance affects soil moisture and hence competition with trees for water in tropical forests. To address this critical knowledge gap, we conducted a large-scale liana removal experiment in a seasonal tropical moist forest in central Panama. We monitored shallow and deep soil moisture over the course of three years to assess the effects of lianas in eight 0.64 ha removal plots and eight control plots. Liana removal caused short-term effects in surface soils. Surface soils (10 cm depth) in removal plots dried more slowly during dry periods and accumulated water more slowly after rainfall events. These effects disappeared within four months of the removal treatment. In deeper soils (40 cm depth), liana removal resulted in a multi-year trend towards 5-25% higher soil moisture during the dry seasons with the largest significant effects occurring in the dry season of the third year following treatment. Liana removal did not affect surface soil temperature. Multiple and mutually occurring mechanisms may be responsible for the effects of liana removal on soil moisture, including competition with trees, and altered microclimate, and soil structure. These results indicate that lianas influence hydrologic processes, which may affect tree community dynamics and forest carbon cycling. C1 [Reid, Joseph Pignatello; Powers, Jennifer S.] Univ Minnesota, Dept Ecol Evolut & Behav, St Paul, MN 55108 USA. [Schnitzer, Stefan A.] Marquette Univ, Dept Biol Sci, Milwaukee, WI 53201 USA. [Schnitzer, Stefan A.; Powers, Jennifer S.] Smithsonian Trop Res Inst, Balboa, Panama. [Powers, Jennifer S.] Univ Minnesota, Dept Plant Biol, St Paul, MN USA. RP Powers, JS (reprint author), Univ Minnesota, Dept Ecol Evolut & Behav, St Paul, MN 55108 USA. EM powers@umn.edu RI Reid, Joseph/I-3292-2012 OI Reid, Joseph/0000-0001-6905-5235 FU National Science Foundation [DEB 0845071]; NSF [DEB 1019436, DEB 1019441] FX This work was made possible by National Science Foundation Grants DEB 0845071 and NSF DEB 1019436 to S.A.S, and NSF DEB 1019441 to J.S.P. The website for the US National Science Foundation is: http://www.nsf.gov/. The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 48 TC 1 Z9 1 U1 4 U2 19 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 NOV 6 PY 2015 VL 10 IS 11 AR e0141891 DI 10.1371/journal.pone.0141891 PG 12 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA CV6RT UT WOS:000364398700060 PM 26545205 ER PT J AU Gawne, R AF Gawne, Richard TI The cultural evolution SO SCIENCE LA English DT Editorial Material RP Gawne, R (reprint author), Smithsonian Inst, Dept Entomol, Natl Museum Nat Hist, NHB 169, Washington, DC 20560 USA. EM gawner@si.edu NR 0 TC 0 Z9 0 U1 1 U2 4 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 NOV 6 PY 2015 VL 350 IS 6261 BP 639 EP 639 DI 10.1126/science.aad2745 PG 1 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA CV3MH UT WOS:000364162800032 ER PT J AU Easson, CG Matterson, KO Freeman, CJ Archer, SK Thacker, RW AF Easson, Cole G. Matterson, Kenan O. Freeman, Christopher J. Archer, Stephanie K. Thacker, Robert W. TI Variation in species diversity and functional traits of sponge communities near human populations in Bocas del Toro, Panama SO PEERJ LA English DT Article DE Community ecology; Microbial symbionts; Photosynthesis; Anthropogenic influences; Porifera ID CARIBBEAN CORAL-REEF; PHASE-SHIFTS; MARINE SPONGES; PHYLOGENETIC INFERENCE; MICROBIAL COMMUNITIES; ALTERNATIVE STATES; FLORIDA-KEYS; ABUNDANCE; ECOSYSTEMS; NITROGEN AB Recent studies have renewed interest in sponge ecology by emphasizing the functional importance of sponges in a broad array of ecosystem services. Many critically important habitats occupied by sponges face chronic stressors that might lead to alterations in their diversity, relatedness, and functional attributes. We addressed whether proximity to human activity might be a significant factor in structuring sponge community composition, as well as potential functional roles, by monitoring sponge diversity and abundance at two structurally similar sites that vary in distance to areas of high coastal development in Bocas Del Toro, Panama. We surveyed sponge communities at each site using belt transects and differences between two sites were compared using the following variables: (1) sponge species richness, Shannon diversity, and inverse Simpson's diversity; (2) phylogenetic diversity; (3) taxonomic and phylogenetic beta diversity; (4) trait diversity and dissimilarity; and (5) phylogenetic and trait patterns in community structure. We observed significantly higher sponge diversity at Punta Caracol, the site most distant from human development (similar to 5 km). Although phylogenetic diversity was lower at Saigon Bay, the site adjacent to a large village including many houses, businesses, and an airport, the sites did not exhibit significantly different patterns of phylogenetic relatedness in species composition. However, each site had a distinct taxonomic and phylogenetic composition (beta diversity). In addition, the sponge community at Saigon included a higher relative abundance of sponges with high microbial abundance and high chlorophyll a concentration, whereas the community at Punta Caracol had a more even distribution of these traits, yielding a significant difference in functional trait diversity between sites. These results suggest that lower diversity and potentially altered community function might be associated with proximity to human populations. This study highlights the importance of evaluating functional traits and phylogenetic diversity in addition to common diversity metrics when assessing potential environmental impacts on benthic communities. C1 [Easson, Cole G.; Matterson, Kenan O.] Univ Alabama Birmingham, Dept Biol, Birmingham, AL 35294 USA. [Freeman, Christopher J.] Smithsonian Marine Stn, Ft Pierce, FL USA. [Archer, Stephanie K.] N Carolina State Univ, Appl Ecol, Raleigh, NC 27695 USA. [Thacker, Robert W.] SUNY Stony Brook, Dept Ecol & Evolut, Stony Brook, NY 11794 USA. RP Easson, CG (reprint author), Univ Alabama Birmingham, Dept Biol, Birmingham, AL 35294 USA. EM cgeasson86@gmail.com FU US National Science Foundation Division of Environmental Biology [0829986, 1208310]; University of Alabama at Birmingham Office of Postdoctoral Education Career Enhancement Award; Sigma Xi; Smithsonian MarineGEO postdoctoral fellowship; National Science Foundation [OCE-1214303]; National Oceanic and Atmospheric Administration's National Institute for Undersea Science and the Technology [NA16RU1496] FX This work was supported by grants from the US National Science Foundation Division of Environmental Biology (grant numbers 0829986 and 1208310 awarded to Robert W. Thacker), the University of Alabama at Birmingham Office of Postdoctoral Education Career Enhancement Award (awarded to Cole G. Easson), Sigma Xi Grants-in-Aid (awarded to Kenan O. Matterson), and the Smithsonian MarineGEO postdoctoral fellowship (awarded to Christopher J. Freeman), the National Science Foundation award OCE-1214303 (awarded to Deborah J. Gochfeld), and the National Oceanic and Atmospheric Administration's National Institute for Undersea Science and the Technology award NA16RU1496 (awarded to Marc Slattery and Deborah J. Gochfeld). The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 84 TC 0 Z9 0 U1 9 U2 25 PU PEERJ INC PI LONDON PA 341-345 OLD ST, THIRD FLR, LONDON, EC1V 9LL, ENGLAND SN 2167-8359 J9 PEERJ JI PeerJ PD NOV 5 PY 2015 VL 3 AR e1385 DI 10.7717/peerj.1385 PG 19 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA CX6HX UT WOS:000365802900007 PM 26587347 ER PT J AU Plunkett, AL Arce, HG Mardones, D van Dokkum, P Dunham, MM Fernandez-Lopez, M Gallardo, J Corder, SA AF Plunkett, Adele L. Arce, Hector G. Mardones, Diego van Dokkum, Pieter Dunham, Michael M. Fernandez-Lopez, Manuel Gallardo, Jose Corder, Stuartt A. TI Episodic molecular outflow in the very young protostellar cluster Serpens South SO NATURE LA English DT Article ID STAR-FORMATION; JETS; CLOUDS; PROTOCLUSTER; SIMULATIONS; AQUILA AB The loss of mass from protostars, in the form of a jet or outflow, is a necessary counterpart to protostellar mass accretion(1,2). Outflow ejection events probably vary in their velocity and/or in the rate of mass loss. Such 'episodic' ejection events(3) have been observed during the class 0 protostellar phase (the early accretion stage)(4-10), and continue during the subsequent class I phase that marks the first one million years of star formation(11-14). Previously observed episodic-ejection sources were relatively isolated; however, the most common sites of star formation are clusters(15). Outflows link protostars with their environment and provide a viable source of the turbulence that is necessary for regulating star formation in clusters(3), but it is not known how an accretion-driven jet or outflow in a clustered environment manifests itself in its earliest stage. This early stage is important in establishing the initial conditions for momentum and energy transfer to the environment as the protostar and cluster evolve. Here we report that an outflow from a young, class 0 protostar, at the hub of the very active and filamentary Serpens South protostellar cluster(16-18), shows unambiguous episodic events. The (CO)-C-12-O-16 (J = 2-1) emission from the protostar reveals 22 distinct features of outflow ejecta, the most recent having the highest velocity. The outflow forms bipolar lobes one of the first detectable signs of star formation which originate from the peak of 1-mm continuum emission. Emission from the surrounding (CO)-O-18 envelope shows kinematics consistent with rotation and an infall of material onto the protostar. The data suggest that episodic, accretion-driven outflow begins in the earliest phase of protostellar evolution, and that the outflow remains intact in a very clustered environment, probably providing efficient momentum transfer for driving turbulence. C1 [Plunkett, Adele L.; Arce, Hector G.; van Dokkum, Pieter] Yale Univ, Dept Astron, New Haven, CT 06511 USA. [Mardones, Diego] Univ Chile, Dept Astron, Santiago, Chile. [Dunham, Michael M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Fernandez-Lopez, Manuel] CCT La Plata CONICET, Inst Argentino Radioastron, RA-1894 Villa Elisa, Argentina. [Gallardo, Jose; Corder, Stuartt A.] Joint ALMA Observ, Santiago, Chile. RP Plunkett, AL (reprint author), Yale Univ, Dept Astron, New Haven, CT 06511 USA. EM adele.plunkett@yale.edu; hectorarce@yale.edu RI Mardones, Diego/I-5719-2016; OI Plunkett, Adele/0000-0002-9912-5705 FU National Science Foundation (NSF) [DGE-1122492]; NSF [AST-0845619]; CONICYT [PFB-06]; Submillimeter Array FX A.L.P. is supported by a National Science Foundation (NSF) Graduate Research Fellowship under grant DGE-1122492; this research was made possible by the US Student Program of Fulbright Chile. H.G.A. receives funding from the NSF under grant AST-0845619. D.M. acknowledges support from CONICYT project PFB-06. M.M.D. acknowledges support from the Submillimeter Array through a postdoctoral fellowship. ALMA is a partnership of the European Space Organization (ESO, representing its member states), NSF (USA) and National Institutes of Natural Sciences (Japan), together with the National Research Council (Canada) and National Security Council and Academia Sinica Institute of Astronomy and Astrophysics (Taiwan), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by ESO, Associated Universities Inc. (AUI)/National Radio Astronomy Observatory (NRAO) and National Astronomical Observatory of Japan. The NRAO is a facility of the NSF, operated under cooperative agreement by AUI. This paper makes use of the following ALMA data: ADS/JAO.ALMA 2012.1.00769.S. NR 29 TC 4 Z9 4 U1 2 U2 10 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 NOV 5 PY 2015 VL 527 IS 7576 BP 70 EP 73 DI 10.1038/nature15702 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA CV4XV UT WOS:000364270700044 PM 26536957 ER PT J AU Sholts, SB Korkalainen, M Simanainen, U Miettinen, HM Hakansson, H Viluksela, M AF Sholts, Sabrina B. Korkalainen, Merja Simanainen, Ulla Miettinen, Hanna M. Hakansson, Helen Viluksela, Matti TI In utero/lactational and adult exposures to 2,3,7,8-tetrachlorodibenzo-p-dioxin (TCDD) show differential effects on craniofacial development and growth in rats SO TOXICOLOGY LA English DT Article DE TCDD; Bone toxicity; in utero/lactational exposure; Craniofacial morphology; Geometric morphometrics ID EMBRYONIC PALATAL SHELVES; LONG-EVANS RATS; POLYCHLORINATED-BIPHENYLS; ORGAN-CULTURE; CLEFT-PALATE; MICE; ASYMMETRY; BONE; EXPRESSION; TOXICITY AB In a previous study of female Han/Wistar (H/W) and Long-Evans (L-E) rats, we found that adult exposure to 2,3,7,8-tetrachlorodibenzo-p-dioxin (TCDD) was associated with size decreases in the cranium and especially the face. In this study we compared these crania to those from male and female Sprague-Dawley (S-D) rats with in utero/lactational exposure to TCDD, using morphometric variables of size, shape, and fluctuating asymmetry to quantify the effects of dose on craniofacial development and growth. At the highest levels of exposure, in utero/lactational and adult TCDD exposures both resulted in small but significant reductions in facial size parameters (i.e., 3-5%) in only females and minor effects on facial shape in both sexes. The shape effects of in utero/lactational exposure were most significant at the sutural intersections, whereas adult exposure to TCDD corresponded to dose-dependent changes of decreasing facial length and vault breadth. Fluctuating asymmetry in general explained a relatively small amount of shape variation compared with other effects, and only increased significantly in female L-E rats with high levels of adult exposure to TCDD. These results indicate that TCDD-related changes in cranial development and growth in rats can vary with the timing and duration of exposure, and with sex. Further investigations of other dioxin-like compounds and animal species will broaden our understanding of how chemicals exposure can influence the development and growth of the mammalian skeleton. Published by Elsevier Ireland Ltd. C1 [Sholts, Sabrina B.] Smithsonian Inst, Dept Anthropol, Natl Museum Nat Hist, Washington, DC 20560 USA. [Korkalainen, Merja; Miettinen, Hanna M.; Viluksela, Matti] Natl Inst Hlth & Welf, Chem & Hlth Unit, FI-70701 Kuopio, Finland. [Simanainen, Ulla] Univ Sydney, ANZAC Res Inst, Androl Lab, Sydney, NSW 2139, Australia. [Hakansson, Helen] Karolinska Inst, Inst Environm Med, SE-17177 Stockholm, Sweden. [Viluksela, Matti] Univ Eastern Finland, Dept Environm Sci, Kuopio, Finland. RP Sholts, SB (reprint author), Smithsonian Inst, Dept Anthropol, Natl Museum Nat Hist, 10th & Constitut Ave NW, Washington, DC 20560 USA. EM sholtss@si.edu; merja.korkalainen@thl.fi; usimanainen@anzac.edu.au; hanna@nettiposti.net; Helen.Hakansson@ki.se; matti.viluksela@thl.fi FU European Commission, DG XII, Contract [ENV4-CT96-0336]; European Commission [QLK4-CT-2002-02528]; Academy of Finland, the Finnish Research Programme on Environmental Health [42551] FX The authors wish to thank Nico Stauffer-Mason for his help with sample preparations for this study, James DiLoreto and Marcia Bakry for help with the figures, and two anonymous reviewers whose comments helped improve the manuscript. This study was supported by the funding sources: European Commission, DG XII, Contract No. ENV4-CT96-0336; European Commission, Contract No. QLK4-CT-2002-02528 (BONETOX); the Academy of Finland, the Finnish Research Programme on Environmental Health (Project 42551). NR 51 TC 0 Z9 0 U1 3 U2 8 PU ELSEVIER IRELAND LTD PI CLARE PA ELSEVIER HOUSE, BROOKVALE PLAZA, EAST PARK SHANNON, CO, CLARE, 00000, IRELAND SN 0300-483X J9 TOXICOLOGY JI Toxicology PD NOV 4 PY 2015 VL 337 BP 30 EP 38 DI 10.1016/j.tox.2015.08.010 PG 9 WC Pharmacology & Pharmacy; Toxicology SC Pharmacology & Pharmacy; Toxicology GA CU8VF UT WOS:000363821500004 PM 26320568 ER PT J AU Xu, QQQ Qiu, J Zhou, ZKK Jin, JHH AF Xu, Qingqing Q. Qiu, Jue Zhou, Zhekun K. Jin, Jianhua H. TI Eocene Podocarpium (Leguminosae) from South China and its biogeographic implications SO FRONTIERS IN PLANT SCIENCE LA English DT Article DE Eocene; Leguminosae; Podocarpium; phytogeography; South China ID MIOCENE-SHANWANG FLORA; LEAF MARGIN ANALYSIS; MIDDLE-MIOCENE; COEXISTENCE APPROACH; EASTERN CHINA; FOSSIL POLLEN; RECONSTRUCTION; EVOLUTION; PALEOCLIMATE; PERSPECTIVE AB Podocarpium A. Braun ex Stizenberger is one of the most common legumes in the Neogene of Eurasia, including fossil fruits, seeds, leaves, and possible flower and pollen grains. This genus is not completely consistent with any extant genera according to gross morphological characters and poorly preserved cuticular structures reported in previous studies. The fossil pods collected from the coal bearing series of the Changchang Basin of Hainan Island and Maoming Basin of Guangdong, South China, are examined by morphologically comparative work, with special reference to venation patterns and placental position. These distinctive features, as well as the ovule development of pods from different developmental stages and the epidermal structure of the pods, as distinguished from previous records lead to the conclusion that these fossils can be recognized as a new species of Podocarpium, P. eocenicum sp. nov. This new discovery indicates that Podocarplum had arrived in South China by the Eocene. Investigation on the fossil records of this extinct genus shows that P eocenicum is the earliest and lowest latitude fossil data. The possible occurrence pattern of this genus is revealed as follows: Podocarpium had distributed in the South China at least in the middle Eocene, and then migrated to Europe during the Oligocene; in the Miocene this genus reached its peak in Eurasia, spreading extensively across subtropical areas to warm temperate areas; finally, Podocarpium shrank rapidly and became extinct in Eurasia during the Pliocene. C1 [Xu, Qingqing Q.; Qiu, Jue; Jin, Jianhua H.] Sun Yat Sen Univ, Sch Life Sci, State Key Lab Biocontrol, Guangzhou 510275, Guangdong, Peoples R China. [Xu, Qingqing Q.; Qiu, Jue; Jin, Jianhua H.] Sun Yat Sen Univ, Sch Life Sci, Guangdong Prov Key Lab Plant Resources, Guangzhou 510275, Guangdong, Peoples R China. [Xu, Qingqing Q.] Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20560 USA. [Zhou, Zhekun K.] Chinese Acad Sci, Xishuangbanna Trop Bot Garden, Menglun, Peoples R China. RP Zhou, ZKK (reprint author), Chinese Acad Sci, Xishuangbanna Trop Bot Garden, Menglun, Peoples R China. EM zhouzk@xtbg.ac.cn; lssjjh@mail.sysu.edu.cn FU National Natural Science Foundation of China [41210001]; joint Project of the National Natural Science Foundation of China; Russian Foundation for Basic Research [413111040, 14-05-91163]; State Key Laboratory of Palaeobiologry and Stratigraphy (Nanjing Institute of Geology and Palaeontology, CAS) [123110]; Scientific Research Fund, Hongda Zhang, Sun Yat-sen University; State Scholarship Fund of China Scholarship Council (CSC) [201406380049] FX This study was supported by the National Natural Science Foundation of China (Grant No. 41210001), the joint Project of the National Natural Science Foundation of China and the Russian Foundation for Basic Research (Grant Nos. 413111040, 14-05-91163), State Key Laboratory of Palaeobiologry and Stratigraphy (Nanjing Institute of Geology and Palaeontology, CAS) (Grant No. 123110), the Scientific Research Fund, Hongda Zhang, Sun Yat-sen University, and the State Scholarship Fund of China Scholarship Council (CSC) (No. 201406380049). NR 76 TC 1 Z9 1 U1 1 U2 5 PU FRONTIERS MEDIA SA PI LAUSANNE PA PO BOX 110, EPFL INNOVATION PARK, BUILDING I, LAUSANNE, 1015, SWITZERLAND SN 1664-462X J9 FRONT PLANT SCI JI Front. Plant Sci. PD NOV 3 PY 2015 VL 6 AR 938 DI 10.3389/fpls.2015.00938 PG 14 WC Plant Sciences SC Plant Sciences GA CV9AP UT WOS:000364580000001 PM 26579179 ER PT J AU Korth, WW Emry, RJ Musso, MR AF Korth, William W. Emry, Robert J. Musso, Marissa R. TI SYSTEMATICS, CRANIAL MORPHOLOGY, AND TAPHONOMY OF THE EOMYID RODENT ADJIDAUMO MINIMUS (MATTHEW, 1903) FROM THE CHADRONIAN (LATE EOCENE), FLAGSTAFF RIM AREA, WYOMING SO JOURNAL OF VERTEBRATE PALEONTOLOGY LA English DT Article ID MAMMALIA; MONTANA AB A collection of Adjidaumo minimus (Matthew, 1903) from the middle Chadronian (late Eocene) of Natrona County, Wyoming, consists of approximately 150 specimens, the largest sample of Adjidaumo from anywhere. The sample includes several partial to nearly complete crania, the most complete cranial material known for the genus. This large sample of a single species allows an examination of the variability in dental and cranial morphology of the species and a more complete description of the skull. The general morphology of the cranium is similar to that of other eomyids and differs most markedly in having a relatively shorter rostrum, an opening for the sphenopalatine vacuity, and a distinct groove on the alisphenoid. Additional topotypic specimens of A. burkei (Russell, 1954) show that it is a distinct species, rather than a synonym of A. minimus as some authors have suggested. Based on age profiles, the population of Adjidaumo from Jenny's Pocket appears to have been attritionally accumulated, whereas that from Al's Pocket was more likely catastrophic. Although the specimens from Jenny's Pocket were preserved in the filling of a burrow along with bones of a mammalian carnivore, examination of the bones and teeth preserved along with modification of the Adjidaumo skulls and jaws from that site indicate that they were more likely the result of predatory activity of a small owl. C1 [Korth, William W.] Rochester Inst Vertebrate Paleontol, Rochester, NY 14610 USA. [Emry, Robert J.] Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20013 USA. [Musso, Marissa R.] Nazareth Coll, Dept Biol, Rochester, NY 14618 USA. RP Korth, WW (reprint author), Rochester Inst Vertebrate Paleontol, 265 Carling Rd, Rochester, NY 14610 USA. EM wwkorth@frontiernet.net; emryr@si.edu; mmusso4@naz.edu NR 34 TC 1 Z9 1 U1 0 U2 1 PU TAYLOR & FRANCIS INC PI PHILADELPHIA PA 530 WALNUT STREET, STE 850, PHILADELPHIA, PA 19106 USA SN 0272-4634 EI 1937-2809 J9 J VERTEBR PALEONTOL JI J. Vertebr. Paleontol. PD NOV 2 PY 2015 VL 35 IS 6 AR UNSP e1001854 DI 10.1080/02724634.2014.1001854 PG 11 WC Paleontology SC Paleontology GA CW4UA UT WOS:000364987100002 ER PT J AU Nelson, D Pillepich, A Genel, S Vogelsberger, M Springel, V Torrey, P Rodriguez-Gomez, V Sijackif, D Snyder, GF Griffen, B Marinacci, F Blecha, L Sales, L Xu, D Hernquist, L AF Nelson, D. Pillepich, A. Genel, S. Vogelsberger, M. Springel, V. Torrey, P. Rodriguez-Gomez, V. Sijackif, D. Snyder, G. F. Griffen, B. Marinacci, F. Blecha, L. Sales, L. Xu, D. Hernquist, L. TI The illustris simulation: Public data release SO ASTRONOMY AND COMPUTING LA English DT Article DE Methods: data analysis; Methods: numerical; Galaxies: formation; Galaxies: evolution; Data management systems; Data access methods ID MOVING-MESH COSMOLOGY; MASSIVE BLACK-HOLES; DIGITAL SKY SURVEY; COSMIC STRUCTURE FORMATION; GALAXY FORMATION PHYSICS; COLD DARK MATTER; HYDRODYNAMICAL SIMULATIONS; RADIATIVE FEEDBACK; SATELLITE GALAXIES; NEUTRAL HYDROGEN AB We present the full public release of all data from the Illustris simulation project. Illustris is a suite of large volume, cosmological hydrodynamical simulations run with the moving-mesh code AREPO and including a comprehensive set of physical models critical for following the formation and evolution of galaxies across cosmic time. Each simulates a volume of (106.5 Mpc)(3) and self-consistently evolves five different types of resolution elements from a starting redshift of z = 127 to the present day, z = 0. These components are: dark matter particles, gas cells, passive gas tracers, stars and stellar wind particles, and supermassive black holes. This data release includes the snapshots at all 136 available redshifts, halo and subhalo catalogs at each snapshot, and two distinct merger trees. Six primary realizations of the Illustris volume are released, including the flagship Illustris-1 run. These include three resolution levels with the fiducial "full" baryonic physics model, and a dark matter only analog for each. In addition, we provide four distinct, high time resolution, smaller volume "subboxes". The total data volume is 265 TB, including 800 full volume snapshots and similar to 30,000 subbox snapshots. We describe the released data products as well as tools we have developed for their analysis. All data may be directly downloaded in its native HDF5 format. Additionally, we release a comprehensive, web-based API which allows programmatic access to search and data processing tasks. In both cases we provide example scripts and a getting-started guide in several languages: currently, IDL, Python, and Matlab. This paper addresses scientific issues relevant for the interpretation of the simulations, serves as a pointer to published and on-line documentation of the project, describes planned future additional data releases, and discusses technical aspects of the release. (C) 2015 Elsevier B.V. All rights reserved. C1 [Nelson, D.; Pillepich, A.; Genel, S.; Rodriguez-Gomez, V.; Hernquist, L.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Genel, S.] Columbia Univ, Dept Astron, New York, NY 10027 USA. [Vogelsberger, M.; Torrey, P.; Griffen, B.; Marinacci, F.] MIT, Dept Phys, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Springel, V.] Heidelberg Inst Theoret Studies, D-69118 Heidelberg, Germany. [Springel, V.] Heidelberg Univ, Zentrum Astron, ARI, D-69120 Heidelberg, Germany. [Sijackif, D.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Sijackif, D.] Univ Cambridge, Kavli Inst Cosmol, Cambridge CB3 0HA, England. [Torrey, P.] CALTECH, TAPIR, Pasadena, CA 91125 USA. [Snyder, G. F.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Sales, L.] Univ Calif Riverside, Dept Phys & Astron, Riverside, CA 92521 USA. [Blecha, L.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Blecha, L.] Univ Maryland, Joint Space Sci Inst, College Pk, MD 20742 USA. RP Nelson, D (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM dnelson@cfa.harvard.edu OI Torrey, Paul/0000-0002-5653-0786; /0000-0003-3816-7028; Rodriguez-Gomez, Vicente/0000-0002-9495-0079; Genel, Shy/0000-0002-3185-1540; Pillepich, Annalisa/0000-0003-1065-9274 FU HST [HST-AR-13897, HST-AR-12856.01-A, HST-AR-13887.004-A, 12856, 13887]; NASA through Hubble Fellowship [HST-HF2-51341 001-A]; STScI; NASA [NAS5-26555]; European Research Council under ERC-StG grant [EXAGAL-308037]; DFG Priority Program SPPEXA through project EXAMAG; NASA ATP Grant [NNX14AH35G]; NASA through Einstein Fellowship [PF2-130093]; NASA grant [NNX12AC67G]; NSF [AST-1312095] FX DN would like to thank Research Computing and the Odyssey cluster at Harvard University for significant computational resources. AP acknowledges support from the HST grant HST-AR-13897. SG acknowledges support provided by NASA through Hubble Fellowship grant HST-HF2-51341 001-A awarded by the STScI, which is operated by the Association of Universities for Research in Astronomy, Inc., for NASA, under contract NAS5-26555. VS acknowledges support by the European Research Council under ERC-StG grant EXAGAL-308037, and by the DFG Priority Program SPPEXA through project EXAMAG. PT acknowledges support from NASA ATP Grant NNX14AH35G. GS acknowledges support from HST grants HST-AR-12856.01-A and HST-AR-13887.004-A. Funding for HST programs #12856 and #13887 is provided by NASA through grants from STScI. LB acknowledges support provided by NASA through Einstein Fellowship grant PF2-130093. LH acknowledges support from NASA grant NNX12AC67G and NSF grant AST-1312095. The authors would like to thank many people for contributing to analysis and understanding of the Illustris simulations and their results: Andreas Bauer, Simeon Bird, Akos Bogdan, Aaron Bray, Eddie Chua, Benjamin Cook, Chris Hayward, Rahul Kannan, Luke Kelley, Cristina Popa, Kevin Schaal, Martin Sparre, Joshua Suresh, Sarah Wellons. NR 119 TC 41 Z9 41 U1 0 U2 1 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 2213-1337 EI 2213-1345 J9 ASTRON COMPUT JI Astron. Comput. PD NOV PY 2015 VL 13 BP 12 EP 37 DI 10.1016/j.ascom.2015.09.003 PG 26 WC Astronomy & Astrophysics; Computer Science, Interdisciplinary Applications SC Astronomy & Astrophysics; Computer Science GA DE2MA UT WOS:000370460200002 ER PT J AU Errickson, EL AF Errickson, Eve L. TI The Culture in Cultural Property: Expanding Legal Advocacy SO HERITAGE AND SOCIETY LA English DT Article DE cultural property law; cultural heritage law; cultural property advocacy; cultural heritage advocacy; historic architecture; architectural remnants AB The stream of cultural property wrongfully taken from developing countries continues in part as a result of the exclusive use of property-based legal strategies in efforts for its return. Advocates for cultural heritage protection have done much to reveal the shadow market of cultural property - elucidating the illicit traffic of items of cultural property from source countries to museums, collectors and auction houses. Because of its strict, transactional focus, property-based remedies may not be the exclusive mechanism for assessing the social, economic and civic harms associated with cultural property dispossession. This paper will: (1) provide general commentary on the history and practice of property law in the United States, and (2) propose tort theory as a possible solution for advocates seeking strategies for the repatriation of cultural property. C1 [Errickson, Eve L.] Smithsonian Inst, Washington, DC 20560 USA. RP Errickson, EL (reprint author), Smithsonian Inst, Washington, DC 20560 USA. EM eerrickson@hotmail.com NR 15 TC 0 Z9 0 U1 3 U2 4 PU MANEY PUBLISHING PI LEEDS PA STE 1C, JOSEPHS WELL, HANOVER WALK, LEEDS LS3 1AB, W YORKS, ENGLAND SN 2159-032X EI 2159-0338 J9 HERIT SOC JI Herit. Soc. PD NOV PY 2015 VL 8 IS 2 BP 97 EP 110 DI 10.1080/2159032X.2015.1126116 PG 14 WC Humanities, Multidisciplinary SC Arts & Humanities - Other Topics GA DC4DJ UT WOS:000369170000002 ER PT J AU Ando, A Huber, BT MacLeod, KG Watkins, DK AF Ando, Atsushi Huber, Brian T. MacLeod, Kenneth G. Watkins, David K. TI Early Cenomanian "hot greenhouse" revealed by oxygen isotope record of exceptionally well-preserved foraminifera from Tanzania SO PALEOCEANOGRAPHY LA English DT Article ID SEA-SURFACE TEMPERATURES; OCEANIC ANOXIC EVENT; TROPICAL ATLANTIC-OCEAN; DRILLING-PROJECT LEG-79; CENTRAL PACIFIC-OCEAN; GULF-OF-MEXICO; NORTH-ATLANTIC; PLANKTONIC-FORAMINIFERA; CRETACEOUS GREENHOUSE; QUANTITATIVE-ANALYSIS AB The search into Earth's mid-Cretaceous greenhouse conditions has recently been stimulated by the Tanzania Drilling Project (TDP) which has recovered exceptionally well-preserved biogenic carbonates from subsurface pre-Neogene marine sediments in the eastern margin of central Africa. Published Tanzanian oxygen isotope records measured on exquisitely preserved foraminiferal tests, dating to as old as similar to 93 Ma, provided evidence for a Turonian "hot greenhouse" with very high and stable water-column temperatures. We have generated a comparable data set of exceptionally well-preserved foraminifera from a lower Cenomanian interval of TDP Site 24 spanning 99.9-95.9 Ma (planktonic foraminiferal Thalmanninella globotruncanoides Zone; nannofossil Corollithion kennedyi to Lithraphidites eccentricus Zones), thereby extending the age coverage of the Tanzanian foraminiferal delta O-18 record back by similar to 7 million years. Throughout the interval analyzed, the new foraminiferal delta O-18 data are consistently around similar to 4.3% for surface-dwelling planktonic taxa and similar to 1.9% for benthic Lenticulina spp., which translate to conservative paleotemperature estimates of >31 degrees C at the surface and >17 degrees C at the sea floor (upper bathyal depths). Considering the similar to 40 degrees S Cenomanian paleolatitude of TDP Site 24, these estimates are higher than computer simulation results for accepted "normal" greenhouse conditions (those with up to 4X preindustrial pCO(2) level) and suggest that the climate mode of the early Cenomanian was very similar to the Turonian hot greenhouse. Taking account of other comparable data sources from different regions, the hot greenhouse mode within the normal mid-Cretaceous greenhouse may have begun by the latest Albian, but the precise timing of the critical transition remains uncertain. C1 [Ando, Atsushi; Huber, Brian T.] Smithsonian Inst, Dept Paleobiol, Natl Museum Nat Hist, Washington, DC 20560 USA. [Ando, Atsushi] BugWare Inc, Tallahassee, FL USA. [MacLeod, Kenneth G.] Univ Missouri, Dept Geol Sci, Columbia, MO USA. [Watkins, David K.] Univ Nebraska, Dept Earth & Atmospher Sci, Lincoln, NE USA. RP Ando, A (reprint author), Smithsonian Inst, Dept Paleobiol, Natl Museum Nat Hist, Washington, DC 20560 USA. EM AndoA@si.edu RI MacLeod, Kenneth/C-4042-2017 OI MacLeod, Kenneth/0000-0002-6016-0837 FU National Science Foundation [NSF EAR 0641956]; Smithsonian Institution's Walcott Fund; National Museum of Natural History; Smithsonian Institution; Geological Society of America; Cushman Foundation FX Biostratigraphic and numerical data supporting Figures 2 and 5 are available as Tables S1 and S2 of the supporting information. Funding was provided by the National Science Foundation (NSF EAR 0641956 to MacLeod and Huber) and the Smithsonian Institution's Walcott Fund (to Huber). The senior author (Ando) gratefully acknowledges funding supports from a Visiting Scientist fellowship from the National Museum of Natural History, Smithsonian Institution, and partly from the W. Storrs Cole Award from the Geological Society of America and the Cushman Foundation. We are grateful for the generous assistance of staff from the Tanzanian Development Petroleum Corporation, including Joyce Singano, Michael Kereme, Ephrem Mchana, Amina Mweneinda, and Emma Msaki, and the Tanzania Commission for Science and Technology. We also thank Alvaro Jimenez Berrocoso for provision of the source graphic file for TDP Site 24 lithostratigraphy and Ines Wendler for suggestions for benthic for aminiferal identifications. Constructive reviews from R. Mark Leckie and Paul Pearson are highly appreciated. NR 103 TC 0 Z9 0 U1 2 U2 8 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0883-8305 EI 1944-9186 J9 PALEOCEANOGRAPHY JI Paleoceanography PD NOV PY 2015 VL 30 IS 11 BP 1556 EP 1572 DI 10.1002/2015PA002854 PG 17 WC Geosciences, Multidisciplinary; Oceanography; Paleontology SC Geology; Oceanography; Paleontology GA DC0LO UT WOS:000368908900010 ER PT J AU Vergara-Asenjo, G Sharma, D Potvin, C AF Vergara-Asenjo, Gerardo Sharma, Divya Potvin, Catherine TI Engaging Stakeholders: Assessing Accuracy of Participatory Mapping of Land Cover in Panama SO CONSERVATION LETTERS LA English DT Article DE Land cover; participatory mapping; accuracy; decision trees; indigenous peoples ID CLASSIFICATION; REDD AB Full and effective participation of indigenous peoples and local communities, and high accuracy estimates are two current requirements for the purposes of monitoring forests at international level. We produced two land cover maps, both of which were based on digital image processing (decision trees) using Rapideye imagery, and a land cover participatory map, for indigenous territories of eastern Panama. Accuracy of the three maps was evaluated using field data. Classification that was based on participatory mapping gave best overall accuracy of 83.7% (kappa = 0.783), followed by the decision tree that included textural variables (DT2: overall accuracy of 79.9%, kappa = 0.757). We have demonstrated for the first time that local knowledge can improve land cover classification and facilitate the identification of forest degradation. The plea of the UNFCC for the full and effective participation of local and indigenous people could, therefore, improve the accuracy of monitoring. C1 [Vergara-Asenjo, Gerardo; Sharma, Divya; Potvin, Catherine] McGill Univ, Dept Biol, 1205 Doctor Penfield Ave, Montreal, PQ H3A 1B1, Canada. [Vergara-Asenjo, Gerardo] Forest Res Inst INFOR, Valdivia, Chile. [Potvin, Catherine] Smithsonian Trop Res Inst, Panama City, Panama. RP Vergara-Asenjo, G (reprint author), McGill Univ, Dept Biol, 1205 Doctor Penfield Ave, Montreal, PQ H3A 1B1, Canada. EM gerardo.vergaraasenjo@mail.mcgill.ca FU David and Lucile Packard Foundation; NSERC (Natural Sciences and Engineering Research Council of Canada); Ford Foundation; Global Environmental and Climate Change Centre (GEC3, Quebec, Canada); Fonds de recherche du Quebec - Nature et technologies (FQRNT); NSERC FX We greatly appreciate the invaluable collaboration of all traditional indigenous authorities of the Collective Lands of Alto Bayano, who authorized and participated in this study. We are grateful to all indigenous technicians, who collected information and supported this research, namely, Messrs. Chicho Chamorro, Angel Ruiz, Abdiel Omi, Jaime Caisamo, and Cristian Pacheco; to W.F.J. Parsons, Centre d'etude de la foret (CEF) for reviewing this document; and P.K. Joshi for support on Weka software. This study was supported by the David and Lucile Packard Foundation and a Discovery grant from NSERC (Natural Sciences and Engineering Research Council of Canada) to CP. We also thank the Ford Foundation International Fellowship Program and the Global Environmental and Climate Change Centre (GEC3, Quebec, Canada) for fellowships that were awarded to GV, and the Fonds de recherche du Quebec - Nature et technologies (FQRNT) and NSERC for financial support to DS. NR 32 TC 8 Z9 8 U1 3 U2 6 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1755-263X J9 CONSERV LETT JI Conserv. Lett. PD NOV-DEC PY 2015 VL 8 IS 6 BP 432 EP 439 DI 10.1111/conl.12161 PG 8 WC Biodiversity Conservation SC Biodiversity & Conservation GA DB5DE UT WOS:000368533300007 ER PT J AU Aira, M Bybee, S Perez-Losada, M Dominguez, J AF Aira, Manuel Bybee, Seth Perez-Losada, Marcos Dominguez, Jorge TI Feeding on microbiomes: effects of detritivory on the taxonomic and phylogenetic bacterial composition of animal manures SO FEMS MICROBIOLOGY ECOLOGY LA English DT Article DE bacterial communities; bacterial diversity; Bar-coded pyrosequencing; Eisenia andrei; earthworm; core microbiome ID LUMBRICUS-TERRESTRIS L; GUT MICROBIOTA; APORRECTODEA-CALIGINOSA; EISENIA-FOETIDA; DIGESTIVE-TRACT; IMAGE-ANALYSIS; EARTHWORM GUT; SOIL; COMMUNITIES; DIVERSITY AB Earthworms play a key role in nutrient cycling by interacting with microorganisms thus accelerating organic matter turnover in soil systems. As detritivores, some earthworm types ingest and digest a mixture of dead organic matter and microorganisms, like animal manures (i.e. animal gut microbiomes). Here we described the earthworm cast microbiome and the role ingested bacteria play on its composition. We fed Eisenia andrei with cow, horse and pig manures and determined the taxonomic and phylogenetic composition of the these manures before and after passage through the earthworm gut. Earthworm cast microbiomes showed a smaller diversity than the manure they fed on. Manures strongly differed in their taxonomic and phylogenetic composition, but these differences were markedly reduced once transformed into earthworm cast microbiomes after passage through the earthworm gut. The core earthworm cast microbiome comprised 30 OTUs (2.6% of OTUs from cast samples), of which 10 are possibly native to the earthworm gut. Most of the core cast microbiome OTUs belonged to phyla Actinobacteria and Proteobacteria, as opposed to already described animal core gut microbiomes, which are composed mainly of Firmicutes and Bacteroidetes. Our results suggest that earthworms build up their cast microbiome by selecting from the pool of ingested bacteria. C1 [Aira, Manuel; Dominguez, Jorge] Univ Vigo, Dept Ecol & Biol Anim, E-36310 Vigo, Spain. [Bybee, Seth] Brigham Young Univ, 4102 LSB, Provo, UT 84602 USA. [Perez-Losada, Marcos] Univ Porto, CIBIO InBIO, Ctr Invest Biodiversidade & Recursos Genet, Campus Agr Vairao, P-4485661 Vairao, Portugal. [Perez-Losada, Marcos] George Washington Univ, Computat Biol Inst, Ashburn, VA 20147 USA. [Perez-Losada, Marcos] US Natl Museum Nat Hist, Smithsonian Inst, Dept Invertebrate Zool, Washington, DC 20013 USA. [Aira, Manuel] Fac Ciencias, Dept Ecol & Biol Anim, Campus Univ As Lagoas, E-32004 Orense, Spain. RP Aira, M (reprint author), Univ Vigo, Dept Ecol & Biol Anim, E-36310 Vigo, Spain. EM aira@uvigo.es RI Perez-Losada, Marcos/I-4407-2013 OI Perez-Losada, Marcos/0000-0002-2585-4657 FU Ministerio de Economia y Competitividad [CTM2013-42540-R]; Xunta de Galicia [CN2012/305]; FCT Investigator Program; Brigham Young University FX This study was supported by grants from the Ministerio de Economia y Competitividad (CTM2013-42540-R) and, the Xunta de Galicia (CN2012/305) to MA and JD, a 'Projeto de investigacao Exploratoria' from the FCT Investigator Program to MP-L, and funds from Brigham Young University. NR 67 TC 0 Z9 0 U1 10 U2 23 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0168-6496 EI 1574-6941 J9 FEMS MICROBIOL ECOL JI FEMS Microbiol. Ecol. PD NOV PY 2015 VL 91 IS 11 DI 10.1093/femsec/fiv117 PG 10 WC Microbiology SC Microbiology GA DB3RY UT WOS:000368430300002 ER PT J AU Humphries, AL Maxwell, AB Ross, AH Ubelaker, DH AF Humphries, A. L. Maxwell, A. B. Ross, A. H. Ubelaker, D. H. TI A Geometric Morphometric Study of Regional Craniofacial Variation in Mexico SO INTERNATIONAL JOURNAL OF OSTEOARCHAEOLOGY LA English DT Article DE geometric morphometrics; craniofacial variation; craniometrics ID CRANIOMETRIC VARIATION; POPULATIONS; AMERINDIANS; COORDINATE; MORPHOLOGY; LANDMARKS; DIVERSITY; ADMIXTURE; EVOLUTION; CRANIA AB Spanish speaking populations in the USA have long been categorised under the umbrella term 'Hispanic', which is a cultural construct. The term Hispanic ignores the unique ethnohistories and biological variation among Hispanic groups with various European, African and indigenousAmerican influences. Considerable heterogeneity has been identified in pre-contact America and has continued to influence the cultural and biological compositions of various regions today. The purpose of this research is to examine biological variation in Mexico, which was influenced by indigenous migration patterns and the Old World conquests of the Americans. Usingmultivariate statistics, this paper compares 16 three-dimensional craniometric landmarks of samples from northern Central Mexico, northern Yucatan and western Mexico to examine the regional biological variation present in Mexico in both prehistoric and historic groups and also compares Mexican, Spanish and African American groups to examine patterns ofOld World conquests. Multivariate statistics detected significant group differences for both size and shape (centroid size, p < 0.0001; shape, p < 0.0001) and showed that while significantly different, all the Mexican groups are more similar to one another except for one prehistoric inland-western Mexican group, which ismorphologically distinct from the other Mexican groups. Previous mtDNA research in these areas shows a low prevalence of African American admixture and a high indigenous component in the northern Mexican groups, which is consistent with the findings of this paper. The prehistoric and historic Mexican groups were themost similar indicating the retention of indigenous admixture after contact. The results from this analysis demonstrate that all groups are significantly different fromone another supporting other findings that have shown that the indigenous populations of the NewWorld are heterogeneous and that this variationmay also contribute to the heterogeneity of contemporary populations. Copyright (C) 2013 John Wiley & Sons, Ltd. C1 [Humphries, A. L.; Maxwell, A. B.] Univ S Florida, Dept Anthropol, Tampa, FL 33620 USA. [Ross, A. H.] N Carolina State Univ, Dept Sociol & Anthropol, Raleigh, NC 27695 USA. [Ubelaker, D. H.] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA. RP Humphries, AL (reprint author), Univ S Florida, Dept Anthropol, Tampa, FL 33620 USA. EM ahumphri@mail.usf.edu OI Ross, Ann/0000-0001-8780-1414 NR 42 TC 1 Z9 1 U1 1 U2 5 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1047-482X EI 1099-1212 J9 INT J OSTEOARCHAEOL JI Int. J. Osteoarchaeol. PD NOV-DEC PY 2015 VL 25 IS 6 BP 795 EP 804 DI 10.1002/oa.2345 PG 10 WC Anthropology; Archaeology SC Anthropology; Archaeology GA DB4AP UT WOS:000368455400001 ER PT J AU Banks, ME Xiao, ZY Watters, TR Strom, RG Braden, SE Chapman, CR Solomon, SC Klimczak, C Byrne, PK AF Banks, Maria E. Xiao, Zhiyong Watters, Thomas R. Strom, Robert G. Braden, Sarah E. Chapman, Clark R. Solomon, Sean C. Klimczak, Christian Byrne, Paul K. TI Duration of activity on lobate-scarp thrust faults on Mercury SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article ID INNER SOLAR-SYSTEM; GLOBAL CONTRACTION; IMPACT CRATERS; SMOOTH PLAINS; CALORIS BASIN; MOON; MESSENGER; LUNAR; EVOLUTION; VOLCANISM AB Lobate scarps, landforms interpreted as the surface manifestation of thrust faults, are widely distributed across Mercury and preserve a record of its history of crustal deformation. Their formation is primarily attributed to the accommodation of horizontal shortening of Mercury's lithosphere in response to cooling and contraction of the planet's interior. Analyses of images acquired by the Mariner 10 and MErcury Surface, Space ENvironment, GEochemistry, and Ranging (MESSENGER) spacecraft during flybys of Mercury showed that thrust faults were active at least as far back in time as near the end of emplacement of the largest expanses of smooth plains. However, the full temporal extent of thrust fault activity on Mercury, particularly the duration of this activity following smooth plains emplacement, remained poorly constrained. Orbital images from the MESSENGER spacecraft reveal previously unrecognized stratigraphic relations between lobate scarps and impact craters of differing ages and degradation states. Analysis of these stratigraphic relations indicates that contraction has been a widespread and long-lived process on the surface of Mercury. Thrust fault activity had initiated by a time near the end of the late heavy bombardment of the inner solar system and continued through much or all of Mercury's subsequent history. Such deformation likely resulted from the continuing secular cooling of Mercury's interior. C1 [Banks, Maria E.; Watters, Thomas R.] Smithsonian Inst, Natl Air & Space Museum, Ctr Earth & Planetary Studies, Washington, DC 20560 USA. [Banks, Maria E.] Planetary Sci Inst, Tucson, AZ USA. [Xiao, Zhiyong; Strom, Robert G.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA. [Xiao, Zhiyong] China Univ Geosci, Sch Earth Sci, Wuhan 430074, Hubei, Peoples R China. [Xiao, Zhiyong] Univ Oslo, Ctr Earth Evolut & Dynam, Oslo, Norway. [Braden, Sarah E.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ USA. [Chapman, Clark R.] SW Res Inst, Dept Space Studies, Boulder, CO USA. [Solomon, Sean C.] Columbia Univ, Lamont Doherty Earth Observ, Palisades, NY USA. [Solomon, Sean C.; Klimczak, Christian; Byrne, Paul K.] Carnegie Inst Sci, Dept Terr Magnetism, Washington, DC USA. [Klimczak, Christian] Univ Georgia, Dept Geol, Athens, GA 30602 USA. [Byrne, Paul K.] Univ Space Res Assoc, Lunar & Planetary Inst, Houston, TX USA. RP Banks, ME (reprint author), Smithsonian Inst, Natl Air & Space Museum, Ctr Earth & Planetary Studies, Washington, DC 20560 USA. EM banks@psi.edu FU NASA [NASW-00002, NAS5-97271, NNX07AR60G] FX We thank the entire MESSENGER team for their support of this investigation. We also thank Mark Robinson and two anonymous reviewers for helpful reviews of an earlier version of this manuscript. The MESSENGER project is supported by the NASA Discovery Program under contracts NASW-00002 to the Carnegie Institution of Washington and NAS5-97271 to The Johns Hopkins University Applied Physics Laboratory. This work was also supported by NASA grant NNX07AR60G. Data are available from the NASA Planetary Data System (https://pds.jpl.nasa.gov/). NR 61 TC 4 Z9 4 U1 0 U2 1 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9097 EI 2169-9100 J9 J GEOPHYS RES-PLANET JI J. Geophys. Res.-Planets PD NOV PY 2015 VL 120 IS 11 BP 1751 EP 1762 DI 10.1002/2015JE004828 PG 12 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA DB3TU UT WOS:000368435500001 ER PT J AU Falcon-Lang, HJ Pufahl, PK Bashforth, AR Gibling, MR Miller, RF Minter, NJ AF Falcon-Lang, Howard J. Pufahl, Peir K. Bashforth, Arden R. Gibling, Martin R. Miller, Randall F. Minter, Nicholas J. TI A MARINE INCURSION IN THE LOWER PENNSYLVANIAN TYNEMOUTH CREEK FORMATION, CANADA: IMPLICATIONS FOR PALEOGEOGRAPHY, STRATIGRAPHY AND PALEOECOLOGY SO PALAIOS LA English DT Article ID SOUTHERN NEW-BRUNSWICK; JOGGINS FOSSIL CLIFFS; WORLD HERITAGE SITE; DISTRIBUTIVE FLUVIAL SYSTEMS; SEA-LEVEL CHANGES; NOVA-SCOTIA; ATLANTIC CANADA; BASIN; COAL; LIMESTONES AB We document the occurrence of a marine bed, and its associated biota, in the Lower Pennsylvanian (Langsettian) Tynemouth Creek Formation of New Brunswick, and discuss its implications for paleogeography, stratigraphy, and paleoecology. This is only the second marine interval found in the entire Pennsylvanian fill of the Maritimes Basin of Canada, the other being recently found in the broadly same-age Joggins Formation of Nova Scotia. Evidence for the new marine transgression comprises an echinoderm-rich limestone that infills irregularities on a vertic paleosol surface within the distal facies of a syntectonic fluvial megafan formed under a seasonally dry tropical climate. Gray, platy ostracod-rich shales and wave-rippled sandstone beds that directly overlie the marine limestone contain trace fossils characteristic of the Mermia Ichnofacies, upright woody trees, and adpressed megafloras. This association represents bay-fills fringed by freshwater coastal forests dominated by pteridosperms, cordaites, and other enigmatic plants traditionally attributed to dryland/upland habitats. The fossil site demonstrates that marine transgressions extended farther into the interior of Pangea than has previously been documented, and may allow correlation of the Tynemouth Creek and Joggins Formations with broadly coeval European successions near the level of the Gastrioceras subcrenatum and G. listeri marine bands. It also helps explain the close similarity of faunas between the Maritimes Basin and other paleotropical basins, if transgressions facilitated migration of marine taxa into the continental interior. C1 [Falcon-Lang, Howard J.] Univ London, Dept Earth Sci, Egham TW20 0EX, Surrey, England. [Pufahl, Peir K.] Acad Univ, Dept Earth & Environm Sci, Wolfville, NS B4P 2R6, Canada. [Bashforth, Arden R.] Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20560 USA. [Gibling, Martin R.] Dalhousie Univ, Dept Earth Sci, Halifax, NS B3H 4R2, Canada. [Miller, Randall F.] New Brunswick Museum, Dept Nat Sci, St John, NB E2K 1E5, Canada. [Minter, Nicholas J.] Univ Portsmouth, Sch Earth & Environm Sci, Portsmouth PO1 3QL, Hants, England. RP Falcon-Lang, HJ (reprint author), Univ London, Dept Earth Sci, Egham TW20 0EX, Surrey, England. EM h.falcon-lang@es.rhul.ac.uk FU Natural Environment Research Council (NERC) [NE/F014120/2]; Matthew Fellowship of the New Brunswick Museum; Tyrell Fund of the Geological Society of London; Winston Churchill Memorial Trust; Government of Canada Postdoctoral Research Fellowship under the Commonwealth Scholarship Programme; Social Sciences and Humanities Research Council of Canada-CURA project [833-2003-1015]; Canada Graduate Scholarship; Natural Sciences and Engineering Research Council of Canada (NSERC); Dalhousie University; NSERC Discovery Grants FX HFL gratefully acknowledges receipt of a Natural Environment Research Council (NERC) Advanced Fellowship (NE/F014120/2), the G.F. Matthew Fellowship (2005) of the New Brunswick Museum, the J.B. Tyrell Fund (2009) of the Geological Society of London, and a Winston Churchill Memorial Trust Travelling Fellowship (2011). NJM acknowledges funding through the Government of Canada Postdoctoral Research Fellowship under the Commonwealth Scholarship Programme, and the G.F. Matthew Fellowship (2013) of the New Brunswick Museum. RFM acknowledges the support of the Social Sciences and Humanities Research Council of Canada-CURA project (833-2003-1015) to study the history of geology in the Saint John, New Brunswick region. ARB acknowledges receipt of the G.F. Matthew Fellowship (2008) of the New Brunswick Museum, a Canada Graduate Scholarship and a Postdoctoral Fellowship from the Natural Sciences and Engineering Research Council of Canada (NSERC), and an Izaak Walton Killam Predoctoral Scholarship from Dalhousie University. MRG and PKP acknowledge funding from their respective NSERC Discovery Grants. We thank the two anonymous reviewers. NR 83 TC 2 Z9 2 U1 0 U2 2 PU SEPM-SOC SEDIMENTARY GEOLOGY PI TULSA PA 6128 EAST 38TH ST, STE 308, TULSA, OK 74135-5814 USA SN 0883-1351 EI 1938-5323 J9 PALAIOS JI Palaios PD NOV PY 2015 VL 30 IS 11 BP 779 EP 791 DI 10.2110/palo.2015.031 PG 13 WC Geology; Paleontology SC Geology; Paleontology GA DB4OV UT WOS:000368493600001 ER PT J AU Ubelaker, DH AF Ubelaker, Douglas H. TI Craniofacial Superimposition: Historical Review and Current Issues SO JOURNAL OF FORENSIC SCIENCES LA English DT Article DE forensic science; craniofacial identification; skulls; photographs ID FACIAL TISSUE THICKNESSES; FACE OVERLAY UNCERTAINTY; FORENSIC IDENTIFICATION; VIDEO SUPERIMPOSITION; PHOTOGRAPHIC SUPERIMPOSITION; SKULL IDENTIFICATION; PLASTIC RECONSTRUCTION; PHOTO SUPERIMPOSITION; RESEMBLANCE RATINGS; EXTERNAL NOSE AB Methodology of craniofacial superimposition has evolved dramatically since its inception in the early 20th century. Contemporary approaches involve advanced procedures of digitization, use of video cameras, warping algorithms, skull positioning devices and data derived from computed tomography, radiography, and ultrasound technology. Applications have proven most useful in exclusion and casework frequency has declined in some regions in recent years as molecular approaches to identification have become more widely available. Additional research is needed to clarify the probabilities involved and to facilitate comparisons when the technique is employed. C1 [Ubelaker, Douglas H.] Smithsonian Inst, Natl Museum Nat Hist, Dept Anthropol, Washington, DC 20013 USA. RP Ubelaker, DH (reprint author), Smithsonian Inst, Dept Anthropol, NMNH, POB 37012,MRC 112, Washington, DC 20013 USA. EM UBELAKED@si.edu NR 136 TC 1 Z9 1 U1 2 U2 7 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0022-1198 EI 1556-4029 J9 J FORENSIC SCI JI J. Forensic Sci. PD NOV PY 2015 VL 60 IS 6 BP 1412 EP 1419 DI 10.1111/1556-4029.12842 PG 8 WC Medicine, Legal SC Legal Medicine GA DA3CA UT WOS:000367672300003 PM 26212578 ER PT J AU Nelles, A Horandel, JR Karskens, T Krause, M Buitink, S Corstanje, A Enriquez, JE Erdmann, M Falcke, H Haungs, A Hiller, R Huege, T Krause, R Link, K Norden, MJ Rachen, JP Rossetto, L Schellart, P Scholten, O Schroder, FG ter Veen, S Thoudam, S Trinh, TNG Weidenhaupt, K Wijnholds, SJ Anderson, J Baehren, L Bell, ME Bentum, MJ Best, P Bonafede, A Bregman, J Brouw, WN Bruggen, M Butcher, HR Carbone, D Ciardi, B de Gasperin, F Duscha, S Eisloffel, J Fallows, RA Frieswijk, W Garrett, MA van Haarlem, MP Heald, G Hoeft, M Horneffer, A Iacobelli, M Juette, E Karastergiou, A Kohler, J Kondratiev, VI Kuniyoshi, M Kuper, G van Leeuwen, J Maat, P McFadden, R McKay-Bukowski, D Orru, E Paas, H Pandey-Pommier, M Pandey, VN Pizzo, R Polatidis, AG Reich, W Rottgering, H Schwarz, D Serylak, M Sluman, J Smirnov, O Tasse, C Toribio, MC Vermeulen, R van Weeren, RJ Wijers, RAMJ Wucknitz, O Zarka, P AF Nelles, A. Horandel, J. R. Karskens, T. Krause, M. Buitink, S. Corstanje, A. Enriquez, J. E. Erdmann, M. Falcke, H. Haungs, A. Hiller, R. Huege, T. Krause, R. Link, K. Norden, M. J. Rachen, J. P. Rossetto, L. Schellart, P. Scholten, O. Schroeder, F. G. ter Veen, S. Thoudam, S. Trinh, T. N. G. Weidenhaupt, K. Wijnholds, S. J. Anderson, J. Baehren, L. Bell, M. E. Bentum, M. J. Best, P. Bonafede, A. Bregman, J. Brouw, W. N. Brueggen, M. Butcher, H. R. Carbone, D. Ciardi, B. de Gasperin, F. Duscha, S. Eisloeffel, J. Fallows, R. A. Frieswijk, W. Garrett, M. A. van Haarlem, M. P. Heald, G. Hoeft, M. Horneffer, A. Iacobelli, M. Juette, E. Karastergiou, A. Kohler, J. Kondratiev, V. I. Kuniyoshi, M. Kuper, G. van Leeuwen, J. Maat, P. McFadden, R. McKay-Bukowski, D. Orru, E. Paas, H. Pandey-Pommier, M. Pandey, V. N. Pizzo, R. Polatidis, A. G. Reich, W. Roettgering, H. Schwarz, D. Serylak, M. Sluman, J. Smirnov, O. Tasse, C. Toribio, M. C. Vermeulen, R. van Weeren, R. J. Wijers, R. A. M. J. Wucknitz, O. Zarka, P. TI Calibrating the absolute amplitude scale for air showers measured at LOFAR SO JOURNAL OF INSTRUMENTATION LA English DT Article DE Antennas; Large detector systems for particle and astroparticle physics; Spectral responses ID RADIO-EMISSION; TUNKA-REX; ARRAY; RADIATION; SPECTRUM AB Air showers induced by cosmic rays create nanosecond pulses detectable at radio frequencies. These pulses have been measured successfully in the past few years at the LOw-Frequency ARray (LOFAR) and are used to study the properties of cosmic rays. For a complete understanding of this phenomenon and the underlying physical processes, an absolute calibration of the detecting antenna system is needed. We present three approaches that were used to check and improve the antenna model of LOFAR and to provide an absolute calibration of the whole system for air shower measurements. Two methods are based on calibrated reference sources and one on a calibration approach using the diffuse radio emission of the Galaxy, optimized for short data-sets. An accuracy of 19% in amplitude is reached. The absolute calibration is also compared to predictions from air shower simulations. These results are used to set an absolute energy scale for air shower measurements and can be used as a basis for an absolute scale for the measurement of astronomical transients with LOFAR. C1 [Nelles, A.; Horandel, J. R.; Karskens, T.; Krause, M.; Corstanje, A.; Enriquez, J. E.; Falcke, H.; Rachen, J. P.; Rossetto, L.; Schellart, P.; ter Veen, S.; Thoudam, S.] Radboud Univ Nijmegen, IMAPP, Dept Astrophys, NL-6500 GL Nijmegen, Netherlands. [Horandel, J. R.; Falcke, H.] Nikhef, NL-1098 XG Amsterdam, Netherlands. [Buitink, S.] Vrije Univ Brussel, Astrophys Inst, B-1050 Brussels, Belgium. [Erdmann, M.; Krause, R.; Weidenhaupt, K.] Rhein Westfal TH Aachen, Phys Inst A 3, D-52056 Aachen, Germany. [Falcke, H.; Norden, M. J.; ter Veen, S.; Wijnholds, S. J.; Bentum, M. J.; Bregman, J.; Brouw, W. N.; Duscha, S.; Fallows, R. A.; Frieswijk, W.; Garrett, M. A.; van Haarlem, M. P.; Heald, G.; Iacobelli, M.; Kondratiev, V. I.; Kuper, G.; van Leeuwen, J.; Maat, P.; McFadden, R.; Orru, E.; Pandey, V. N.; Pizzo, R.; Polatidis, A. G.; Sluman, J.; Toribio, M. C.; Vermeulen, R.] Netherlands Inst Radio Astron, ASTRON, NL-7990 AA Dwingeloo, Netherlands. [Falcke, H.; Horneffer, A.; Kohler, J.; Reich, W.; Wucknitz, O.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Haungs, A.; Hiller, R.; Huege, T.; Link, K.; Schroeder, F. G.] Karlsruhe Inst Technol, Inst Kernphys, D-76344 Eggenstein Leopoldshafen, Germany. [Scholten, O.; Trinh, T. N. G.] Univ Groningen, KVI CART, NL-9700 AB Groningen, Netherlands. [Anderson, J.] Deutsch GeoForschungsZentrum GFZ, Helmholtz Zentrum Potsdam, Dept Geodesy & Remote Sensing 1, D-14473 Potsdam, Germany. [Baehren, L.; Carbone, D.; van Leeuwen, J.; Wijers, R. A. M. J.] Univ Amsterdam, Anton Pannekoek Inst, NL-1090 GE Amsterdam, Netherlands. [Bell, M. E.] CSIRO Australia Telescope Natl Facil, Epping, NSW 1710, Australia. [Bentum, M. J.] Univ Twente, NL-7500 AE Enschede, Netherlands. [Best, P.] Univ Edinburgh, Inst Astron, Royal Observ Edinburgh, Edinburgh EH9 3HJ, Midlothian, Scotland. [Bonafede, A.; Brueggen, M.; de Gasperin, F.] Univ Hamburg, D-21029 Hamburg, Germany. [Brouw, W. N.; Heald, G.] Univ Groningen, Kapteyn Astron Inst, NL-9700 AV Groningen, Netherlands. [Butcher, H. R.; Eisloeffel, J.] Australian Natl Univ, Res Sch Astron & Astrophys, Weston, ACT 2611, Australia. [Ciardi, B.] Max Planck Inst Astrophys, D-85741 Garching, Germany. [Hoeft, M.] Thuringer Landessternwarte, D-07778 Tautenburg, Germany. [Garrett, M. A.; Roettgering, H.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [Juette, E.] Ruhr Univ Bochum, Astron Inst, D-44780 Bochum, Germany. [Karastergiou, A.; Serylak, M.] Univ Oxford, Astrophys, Oxford OX1 3RH, England. [Kondratiev, V. I.] PN Lebedev Phys Inst, Astro Space Ctr, Moscow 117997, Russia. [Kuniyoshi, M.] Natl Astron Observ Japan, Tokyo, Japan. [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 AB 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 & Elelctron, ZA-6140 Grahamstown, South Africa. [Smirnov, O.] SKA South Africa, ZA-7405 Pinelands, South Africa. [Tasse, C.; Zarka, P.] Observ Paris, CNRS, UMR 8109, LESIA, F-92195 Meudon, France. [van Weeren, R. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Nelles, A (reprint author), Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA. EM a.nelles@astro.ru.nl RI Kondratiev, Vladislav/N-1105-2015; OI Kondratiev, Vladislav/0000-0001-8864-7471; Wijers, Ralph/0000-0002-3101-1808; Krause, Maria/0000-0001-7595-0914; de Gasperin, Francesco/0000-0003-4439-2627; van Weeren, Reinout/0000-0002-0587-1660 FU European Research Council (FP) / ERC [227610]; European Research Council (ERC) under the European Union [640130]; FOM [12PR304]; NWO (VENI grant ) [639-041-130]; DFG [NE 2031/1-1]; Helmholtz Alliance for Astroparticle Physics HAP; Networking Fund of the Helmholtz Association, Germany FX The LOFAR cosmic ray key science project acknowledges funding from an Advanced Grant of the European Research Council (FP/2007-2013) / ERC Grant Agreement n. 227610. The project has also received funding from the European Research Council (ERC) under the European Union's Horizon 2020 research and innovation programme (grant agreement No 640130). We furthermore acknowledge financial support from FOM, (FOM-project 12PR304) and NWO (VENI grant 639-041-130). AN is supported by the DFG (research fellowship NE 2031/1-1).r The calibration methods used were developed under partial support by the 'Helmholtz Alliance for Astroparticle Physics HAP' and the Networking Fund of the Helmholtz Association, Germany. NR 45 TC 6 Z9 6 U1 1 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 NOV PY 2015 VL 10 AR P11005 DI 10.1088/1748-0221/10/11/P11005 PG 33 WC Instruments & Instrumentation SC Instruments & Instrumentation GA DA3DH UT WOS:000367676000015 ER PT J AU Temperli, C Veblen, TT Hart, SJ Kulakowski, D Tepley, AJ AF Temperli, Christian Veblen, Thomas T. Hart, Sarah J. Kulakowski, Dominik Tepley, Alan J. TI Interactions among spruce beetle disturbance, climate change and forest dynamics captured by a forest landscape model SO ECOSPHERE LA English DT Article DE climate change; Dendroctonus rufipennis; forest dynamics; landscape model LandClim; northwestern Colorado; Picea engelmannii ID MOUNTAIN PINE-BEETLE; SUB-ALPINE FOREST; WESTERN UNITED-STATES; COLORADO FRONT RANGE; SPATIOTEMPORAL PATTERNS; BARK BEETLES; FIRE REGIMES; CONIFEROUS FORESTS; ROCKY-MOUNTAINS; IPS-TYPOGRAPHUS AB The risk of bark beetle outbreaks is widely predicted to increase because of a warming climate that accelerates temperature-driven beetle population growth and drought stress that impairs host tree defenses. However, few if any studies have explicitly evaluated climatically enhanced beetle population dynamics in relation to climate-driven changes in forest composition and structure that may alter forest suitability for beetle infestation. We synthesized current understanding of the interactions among climate, spruce beetles (Dendroctonus rufipennis) and forest dynamics to parameterize and further advance the bark beetle module of a dynamic forest landscape model (LandClim) that also integrates fire and wind disturbance and climate-driven forest succession. We applied the model to a subalpine watershed in northwestern Colorado to examine the mechanisms and feedbacks that may lead to shifts in forest composition and spruce beetle disturbance under three climate change scenarios. Simulation results suggest increased drought-and beetle-induced reduction of large Engelmann spruce (Picea engelmannii) trees while Douglas-fir (Pseudotsuga menziesii) and ponderosa pine (Pinus ponderosa) increased in dominance throughout the study area under all climate change scenarios. This shift in forest composition and structure counterbalances the enhancing effects of accelerated beetle population development and increased drought-induced susceptibility of spruce to beetles. As a result, we projected a long-term decrease in beetle-induced spruce mortality to below historical values under all climate scenarios at low elevations (<2800 m asl). Beetle-induced spruce mortality above 2800 m asl and under moderate climate change was slightly higher and more variable than under historical conditions but decreased to 36% and 6% of historical values under intermediate and extreme climate change, respectively. Because mechanisms driving beetle disturbance dynamics are similar across different bark beetle species, we argue that the depletion of host trees due to drought and beetle disturbance may also be important in other climate-sensitive beetle-host systems. We advocate for the consideration of climate-driven shifts in forest and disturbance dynamics in devising adaptive management strategies. C1 [Temperli, Christian; Veblen, Thomas T.; Hart, Sarah J.] Univ Colorado, Dept Geog, Boulder, CO 80309 USA. [Kulakowski, Dominik] Clark Univ, Grad Sch Geog, Worcester, MA 01610 USA. [Tepley, Alan J.] Smithsonian Conservat Biol Inst, Front Royal, VA 22630 USA. RP Temperli, C (reprint author), Swiss Fed Inst Forest Snow & Landscape Res WSL, Resource Anal, zurcherstr 111, CH-8903 Birmensdorf, Switzerland. EM christian.temperli@wsl.ch RI Temperli, Christian/A-5853-2015; OI Temperli, Christian/0000-0003-1161-9864; Tepley, Alan/0000-0002-5701-9613 FU Swiss National Science Foundation [145714]; National Science Foundation [1262687, 1262691] FX We thank Matt Hanson for providing an unpublished description of the spruce beetle phenology model implemented in BioSim and two anonymous reviewers for their valuable suggestions for improvement of the manuscript. Christian Temperli was funded through a Swiss National Science Foundation Fellowship for prospective researchers (Grant number: 145714). Additional support came from National Science Foundation awards 1262687 and 1262691. NR 74 TC 7 Z9 7 U1 21 U2 51 PU ECOLOGICAL SOC AMER PI WASHINGTON PA 1990 M STREET NW, STE 700, WASHINGTON, DC 20036 USA SN 2150-8925 J9 ECOSPHERE JI Ecosphere PD NOV PY 2015 VL 6 IS 11 AR 231 DI 10.1890/ES15-00394.1 PG 20 WC Ecology SC Environmental Sciences & Ecology GA CZ7WH UT WOS:000367310600022 ER PT J AU Caplan, JS Hager, RN Megonigal, JP Mozdzer, TJ AF Caplan, Joshua S. Hager, Rachel N. Megonigal, J. Patrick Mozdzer, Thomas J. TI Global change accelerates carbon assimilation by a wetland ecosystem engineer SO ENVIRONMENTAL RESEARCH LETTERS LA English DT Article DE coastal wetland; elevated CO2; eutrophication; global change; Phragmites australis (common reed); tidal saltmarsh; primary productivity ID SEA-LEVEL RISE; GROSS PRIMARY PRODUCTION; NONNATIVE PHRAGMITES-AUSTRALIS; CO2 ENRICHMENT FACE; ELEVATED CO2; CHESAPEAKE BAY; COMMON REED; SALT-MARSH; PRIMARY PRODUCTIVITY; PLANT-COMMUNITIES AB The primary productivity of coastal wetlands is changing dramatically in response to rising atmospheric carbon dioxide (CO2) concentrations, nitrogen (N) enrichment, and invasions by novel species, potentially altering their ecosystem services and resilience to sea level rise. In order to determine how these interacting global change factors will affect coastal wetland productivity, we quantified growing-season carbon assimilation (approximate to gross primary productivity, or GPP) and carbon retained in living plant biomass (approximate to net primary productivity, or NPP) of North American mid-Atlantic saltmarshes invaded by Phragmites australis (common reed) under four treatment conditions: two levels of CO2 (ambient and + 300 ppm) crossed with two levels of N(0 and 25 gN added m(-2) yr(-1)). For GPP, we combined descriptions of canopy structure and leaf-level photosynthesis in a simulation model, using empirical data from an open-top chamber field study. Under ambient CO2 and low N loading (i.e., the Control), we determined GPP to be 1.66 +/- 0.05 kg Cm-2 yr(-1) at a typical Phragmites stand density. Individually, elevated CO2 and N enrichment increased GPP by 44 and 60%, respectively. Changes under N enrichment came largely from stimulation to carbon assimilation early and late in the growing season, while changes from CO2 came from stimulation during the early and mid-growing season. In combination, elevated CO2 and N enrichment increased GPP by 95% over the Control, yielding 3.24 +/- 0.08 kg Cm-2 yr(-1). We used biomass data to calculate NPP, and determined that it represented 44%-60% of GPP, with global change conditions decreasing carbon retention compared to the Control. Our results indicate that Phragmites invasions in eutrophied saltmarshes are driven, in part, by extended phenology yielding 3.1 x greater NPP than native marsh. Further, we can expect elevated CO2 to amplify Phragmites productivity throughout the growing season, with potential implications including accelerated spread and greater carbon storage belowground. C1 [Caplan, Joshua S.; Hager, Rachel N.; Mozdzer, Thomas J.] Bryn Mawr Coll, Dept Biol, Bryn Mawr, PA 19010 USA. [Caplan, Joshua S.; Hager, Rachel N.; Megonigal, J. Patrick; Mozdzer, Thomas J.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. [Hager, Rachel N.] Utah State Univ, Ctr Ecol, Logan, UT 84322 USA. [Hager, Rachel N.] Utah State Univ, Dept Watershed Sci, Logan, UT 84322 USA. RP Caplan, JS (reprint author), Bryn Mawr Coll, Dept Biol, 101 North Merion Ave, Bryn Mawr, PA 19010 USA. EM jcaplan@mail.com OI Mozdzer, Thomas/0000-0002-1053-0967 FU NSF LTREB [DEB-0950080]; Maryland Sea Grant [SA7528114-WW]; Bucher-Jackson Postdoctoral Fellowship; Smithsonian Environmental Research Center; Bryn Mawr College FX We thank Adam Langley, Franzisca Eller, Eric Hazelton, Blanca Bernal, Joshua Shapiro, Sydne Record, several anonymous reviewers, and students in the Global Change Ecology lab at Bryn Mawr College for their valuable input on this research. We are also grateful to Gary Peresta, Andrew Peresta, and Jim Duls for maintaining the field experiment and to the SERC Phytoplankton Lab for essential data on PPFD. We thank Daniel Potts, Kay Stefanik, and Adam Langley for contributing data as well. The field experiment was funded by grants from NSF LTREB (award DEB-0950080) and Maryland Sea Grant (award SA7528114-WW). JSC was funded by a Bucher-Jackson Postdoctoral Fellowship. Additional support was provided by the Smithsonian Environmental Research Center and by Bryn Mawr College. The authors have no conflicts of interest with respect to this research. NR 84 TC 6 Z9 6 U1 13 U2 53 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 1748-9326 J9 ENVIRON RES LETT JI Environ. Res. Lett. PD NOV PY 2015 VL 10 IS 11 AR 115006 DI 10.1088/1748-9326/10/11/115006 PG 12 WC Environmental Sciences; Meteorology & Atmospheric Sciences SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences GA CZ6ZO UT WOS:000367249900034 ER PT J AU Wang, SW Zhang, Q Martin, RV Philip, S Liu, F Li, M Jiang, XJ He, KB AF Wang, Siwen Zhang, Qiang Martin, Randall V. Philip, Sajeev Liu, Fei Li, Meng Jiang, Xujia He, Kebin TI Satellite measurements oversee China's sulfur dioxide emission reductions from coal-fired power plants SO ENVIRONMENTAL RESEARCH LETTERS LA English DT Article DE OMI; SO2 emissions; power plants ID OZONE MONITORING INSTRUMENT; NOX EMISSIONS; ACID-RAIN; SO2; RETRIEVAL; LIFETIMES; MODEL; AIR; ALGORITHM; OMI AB To evaluate the real reductions in sulfur dioxide (SO2) emissions from coal-fired power plants in China, Ozone Monitoring Instrument (OMI) remote sensing SO2 columns were used to inversely model the SO2 emission burdens surrounding 26 isolated power plants before and after the effective operation of their flue gas desulfurization (FGD) facilities. An improved two-dimensional Gaussian fitting method was developed to estimate SO2 burdens under complex background conditions, by using the accurate local background columns and the customized fitting domains for each target source. The OMI-derived SO2 burdens before effective FGD operation were correlated well with the bottom-up emission estimates (R = 0.92), showing the reliability of the OMI-derived SO2 burdens as a linear indicator of the associated source strength. OMI observations indicated that the average lag time period between installation and effective operation of FGD facilities at these 26 power plants was around 2 years, and no FGD facilities have actually operated before the year 2008. The OMI estimated average SO2 removal equivalence (56.0%) was substantially lower than the official report (74.6%) for these 26 power plants. Therefore, it has been concluded that the real reductions of SO2 emissions in China associated with the FGD facilities at coal-fired power plants were considerably diminished in the context of the current weak supervision measures. C1 [Wang, Siwen; Liu, Fei; Li, Meng; Jiang, Xujia; He, Kebin] Tsinghua Univ, Sch Environm, State Key Joint Lab Environm Simulat & Pollut Con, Beijing 100084, Peoples R China. [Zhang, Qiang; Li, Meng; Jiang, Xujia] Tsinghua Univ, Ctr Earth Syst Sci, Key Lab Earth Syst Modeling, Minist Educ, Beijing 100084, Peoples R China. [Wang, Siwen; Martin, Randall V.; Philip, Sajeev] Dalhousie Univ, Dept Phys & Atmospher Sci, Halifax, NS, Canada. [Martin, Randall V.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Wang, Siwen] Max Planck Inst Chem, D-55128 Mainz, Germany. RP Wang, SW (reprint author), Tsinghua Univ, Sch Environm, State Key Joint Lab Environm Simulat & Pollut Con, Beijing 100084, Peoples R China. EM qiangzhang@tsinghua.edu.cn RI Zhang, Qiang/D-9034-2012; Martin, Randall/C-1205-2014 OI Martin, Randall/0000-0003-2632-8402 FU National Natural Science Foundation of China [41222036, 41275026]; China's National Basic Research Program [2014CB441301] FX This work was funded by the National Natural Science Foundation of China (41222036 and 41275026) and the China's National Basic Research Program (2014CB441301). The work at Tsinghua University is a contribution to the EU FP-7 program MarcoPolo and PANDA. We acknowledge the free use of the PBL OMI SO2 Level 2 products and Tropospheric OMI NO2 Level 2 products from NASA GES Data and Information Service Center (http://disc.sci.gsfc.nasa.gov/Aura/). NR 42 TC 4 Z9 4 U1 13 U2 45 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 1748-9326 J9 ENVIRON RES LETT JI Environ. Res. Lett. PD NOV PY 2015 VL 10 IS 11 AR 114015 DI 10.1088/1748-9326/10/11/114015 PG 9 WC Environmental Sciences; Meteorology & Atmospheric Sciences SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences GA CZ6ZO UT WOS:000367249900019 ER PT J AU Fitzhugh, WW AF Fitzhugh, William W. TI Steaming to the North: The First Summer Cruise of the U.S. Revenue Cutter Bear, Alaska and Siberia, 1886 SO INTERNATIONAL JOURNAL OF MARITIME HISTORY LA English DT Book Review C1 [Fitzhugh, William W.] Smithsonian Inst, Washington, DC 20560 USA. RP Fitzhugh, WW (reprint author), Smithsonian Inst, Washington, DC 20560 USA. NR 1 TC 0 Z9 0 U1 2 U2 2 PU SAGE PUBLICATIONS LTD PI LONDON PA 1 OLIVERS YARD, 55 CITY ROAD, LONDON EC1Y 1SP, ENGLAND SN 0843-8714 EI 2052-7756 J9 INT J MARIT HIST JI Int. J. Marit. Hist. PD NOV PY 2015 VL 27 IS 4 SI SI BP 834 EP 835 DI 10.1177/0843871415608330g PG 2 WC History SC History GA CZ7BK UT WOS:000367254700025 ER PT J AU MacFadden, BJ Symister, C Cannarozzi, N Pimiento, C De Gracia, C AF MacFadden, Bruce J. Symister, Chanika Cannarozzi, Nicole Pimiento, Catalina De Gracia, Carlos TI Comparative Diagenesis and Rare Earth Element Variation in Miocene Invertebrate and Vertebrate Fossils from Panama SO JOURNAL OF GEOLOGY LA English DT Article ID TRACE-ELEMENTS; NORTH-AMERICA; BIOGENIC APATITES; GATUN FORMATION; MAMMALS; BONES; BIOMINERALIZATION; EVOLUTION; ARAGONITE; TAPHONOMY AB The incorporation of rare earth elements (REEs) into the mineral lattices of skeletonized fossils has been used, particularly in vertebrates, to understand diagenesis and other postmortem paleoenvironmental parameters. Little is known about similar processes in invertebrates. Invertebrate and vertebrate fossils were analyzed for REE concentrations and patterns from five Miocene formations in central Panama (similar to 20-6 m.yr. ago). These formations (Culebra, Cucaracha, Gatun, Chucunaque, and Chagres) contain sediments interpreted to range from freshwater to shallow marine environments (depth of <300 m). We also compared different compositional types of fossils, including hydroxylapatite (bone) and aragonite (otoliths) in vertebrates and calcite and aragonite in invertebrates. REEs from modern invertebrates indicate that, as previously reported for vertebrates, invertebrates do not incorporate significant amounts of REEs into their mineral lattices during life; therefore, uptake must primarily occur during diagenesis. Comparisons of REEN concentrations (REE concentrations normalized to Post-Archean Australian Shale) of the fossils from Panama indicate differences in diagenesis. Within our largest sample from the Gatun Formation, there are significance differences in REEN concentrations and patterns within different compositional types. For example, shark teeth have the highest REEN concentrations and otoliths the lowest, with these differences likely a result of physical, chemical, and mineralogical factors. Calcitic and aragonitic fossils from the Gatun Formation show REEN patterns indicating differential uptake of individual elements during diagenesis. The cerium anomaly, previously used to indicate relative paleobathymetry, did not discriminate water depth in the marine formations. Comparative analysis of REEs in vertebrates and invertebrates provides a powerful tool to understand diagenetic processes, as demonstrated in the five formations and different compositional types studied from the Miocene of Panama. C1 [MacFadden, Bruce J.; Symister, Chanika; Cannarozzi, Nicole; Pimiento, Catalina] Univ Florida, Florida Museum Nat Hist, Gainesville, FL 32611 USA. [Pimiento, Catalina; De Gracia, Carlos] Smithsonian Trop Res Inst, Ctr Trop Paleoecol & Archaeol, Ancon, Panama. [Pimiento, Catalina] Univ Zurich, Paleontol Inst & Museum, CH-8006 Zurich, Switzerland. RP MacFadden, BJ (reprint author), Univ Florida, Florida Museum Nat Hist, Gainesville, FL 32611 USA. EM bmacfadd@flmnh.ufl.edu OI De Gracia, Carlos/0000-0003-0637-3302 FU National Science Foundation [0966884] FX We thank the curators of fossil collections from the Smithsonian Institution (Paleobiology) and the Florida Museum of Natural History (Invertebrate Paleontology, Malacology, Mammalogy, and Vertebrate Paleontology) who allowed us access to the specimens analyzed here. A. Hendy helped with the selection of modern and fossil invertebrates. We thank G. Kamenov and J. Jaeger of the University of Florida Department of Geological Sciences for help with, respectively, the inductively coupled plasma mass spectrometer (for rare earth element analysis) and the X-ray diffraction laboratory. K. Rohlwing helped with specimen analysis and data reduction. This study benefitted from input provided by and/or discussions with A. Dutton, D. Jones, D. Herwartz, E. Martin, and M. Nash. This research was funded by National Science Foundation grant 0966884 (Office of International Science and Engineering [OISE], Division of Earth Sciences [EAR], Research on Learning in Formal and Informal Settings [DRL]). This is University of Florida Contribution to Paleobiology 685. NR 66 TC 1 Z9 1 U1 3 U2 14 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0022-1376 EI 1537-5269 J9 J GEOL JI J. Geol. PD NOV PY 2015 VL 123 IS 6 BP 491 EP 507 DI 10.1086/684006 PG 17 WC Geology SC Geology GA CY9VT UT WOS:000366755100001 ER PT J AU Moon, E Nam, SW Shin, W Park, MG Coats, DW AF Moon, Eunyoung Nam, Seung Won Shin, Woongghi Park, Myung Gil Coats, D. Wayne TI Do All Dinoflagellates have an Extranuclear Spindle? SO PROTIST LA English DT Article DE Amoebophrya; dinoflagellate; Syndinea; mitosis; parasite; ultrastructure ID ELECTRON-MICROSCOPIC OBSERVATIONS; PARASITIC DINOFLAGELLATE; FLAGELLAR APPARATUS; CELL-CYCLE; FINE-STRUCTURE; LIFE-CYCLE; CRYPTHECODINIUM-COHNII; MARINE DINOFLAGELLATE; EVOLUTIONARY HISTORY; BLASTODINIUM CHATTON AB The syndinean dinoflagellates are a diverse assemblage of alveolate endoparasites that branch basal to the core dinoflagellates. Because of their phylogenetic position, the syndineans are considered key model microorganisms in understanding early evolution in the dinoflagellates. Closed mitosis with an extranuclear spindle that traverses the nucleus in cytoplasmic grooves or tunnels is viewed as one of the morphological features shared by syndinean and core dinoflagellates. Here we describe nuclear morphology and mitosis in the syndinean dinoflagellate Amoebophrya sp. from Akashiwo sanguinea, a member of the A. ceratii complex, as revealed by protargol silver impregnation, DNA specific fluorochromes, and transmission electron microscopy. Our observations show that not all species classified as dinoflagellates have an extranuclear spindle. In Amoebophrya sp. from A. sanguinea, an extranuclear microtubule cylinder located in a depression in the nuclear surface during interphase moves into the nucleoplasm via sequential membrane fusion events and develops into an entirely intranuclear spindle. Results suggest that the intranuclear spindle of Amoebophrya spp. may have evolved from an ancestral extranuclear spindle and indicate the need for taxonomic revision of the Amoebophryidae. (C) 2015 Elsevier GmbH. All rights reserved. C1 [Moon, Eunyoung; Park, Myung Gil] Chonnam Natl Univ, Dept Oceanog, LOHABE, Kwangju 500757, South Korea. [Nam, Seung Won; Shin, Woongghi] Chungnam Natl Univ, Dept Biol Sci, Taejong 306764, South Korea. [Coats, D. Wayne] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. RP Park, MG (reprint author), Chonnam Natl Univ, Dept Oceanog, LOHABE, Kwangju 500757, South Korea. EM mpark@chonnam.ac.kr FU National Research Foundation of Korea (NRFK) Grant - Korean Government [NRF-2014R1A2A2A01004586] FX This work was supported by the National Research Foundation of Korea (NRFK) Grant funded by the Korean Government (NRF-2014R1A2A2A01004586). We thank Dr. Chuck Delwiche, University of Maryland, Department of Cell Biology and Molecular Genetics for providing access to photomicroscopes and Dr. Tsvetan Bachvaroff, University of Maryland, Institute of Marine and Environmental Technology for furnishing a subculture of Amoebophrya sp. from Akashiwo sanguinea. NR 72 TC 0 Z9 0 U1 3 U2 7 PU ELSEVIER GMBH, URBAN & FISCHER VERLAG PI JENA PA OFFICE JENA, P O BOX 100537, 07705 JENA, GERMANY SN 1434-4610 J9 PROTIST JI Protist PD NOV PY 2015 VL 166 IS 5 BP 569 EP 584 DI 10.1016/j.protis.2015.08.005 PG 16 WC Microbiology SC Microbiology GA CZ0OT UT WOS:000366806200006 PM 26491972 ER PT J AU Holtzman, JA Shetrone, M Johnson, JA Prieto, CA Anders, F Andrews, B Beers, TC Bizyaev, D Blanton, MR Bovy, J Carrera, R Chojnowski, SD Cunha, K Eisenstein, DJ Feuillet, D Frinchaboy, PM Galbraith-Frew, J Perez, AEG Garcia-Hernandez, DA Hasselquist, S Hayden, MR Hearty, FR Ivans, I Majewski, SR Martell, S Meszaros, S Muna, D Nidever, D Nguyen, DC O'Connell, RW Pan, K Pinsonneault, M Robin, AC Schiavon, RP Shane, N Sobeck, J Smith, VV Troup, N Weinberg, DH Wilson, JC Wood-Vasey, WM Zamora, O Zasowski, G AF Holtzman, Jon A. Shetrone, Matthew Johnson, Jennifer A. Allende Prieto, Carlos Anders, Friedrich Andrews, Brett Beers, Timothy C. Bizyaev, Dmitry Blanton, Michael R. Bovy, Jo Carrera, Ricardo Chojnowski, S. Drew Cunha, Katia Eisenstein, Daniel J. Feuillet, Diane Frinchaboy, Peter M. Galbraith-Frew, Jessica Garcia Perez, Ana E. Garcia-Hernandez, D. A. Hasselquist, Sten Hayden, Michael R. Hearty, Fred R. Ivans, Inese Majewski, Steven R. Martell, Sarah Meszaros, Szabolcs Muna, Demitri Nidever, David Duy Cuong Nguyen O'Connell, Robert W. Pan, Kaike Pinsonneault, Marc Robin, Annie C. Schiavon, Ricardo P. Shane, Neville Sobeck, Jennifer Smith, Verne V. Troup, Nicholas Weinberg, David H. Wilson, John C. Wood-Vasey, W. M. Zamora, Olga Zasowski, Gail TI ABUNDANCES, STELLAR PARAMETERS, AND SPECTRA FROM THE SDSS-III/APOGEE SURVEY SO ASTRONOMICAL JOURNAL LA English DT Article DE astronomical databases: miscellaneous; Galaxy: abundances; stars: abundances; surveys ID GALACTIC EVOLUTION EXPERIMENT; DIGITAL SKY SURVEY; OPEN CLUSTERS; CHEMICAL-COMPOSITION; RED GIANTS; MILKY-WAY; ELEMENTAL ABUNDANCE; MODEL ATMOSPHERES; EXPERIMENT APOGEE; METAL ABUNDANCES AB The SDSS-III/Apache Point Observatory Galactic Evolution Experiment (APOGEE) survey operated from 2011-2014 using the APOGEE spectrograph, which collects high-resolution (R similar to 22,500), near-IR (1.51-1.70 mu m) spectra with a multiplexing (300 fiber-fed objects) capability. We describe the survey data products that are publicly available, which include catalogs with radial velocity, stellar parameters, and 15 elemental abundances for over 150,000 stars, as well as the more than 500,000 spectra from which these quantities are derived. Calibration relations for the stellar parameters (T-eff, log g, [M/H], [alpha/M]) and abundances (C, N, O, Na, Mg, Al, Si, S, K, Ca, Ti, V, Mn, Fe, Ni) are presented and discussed. The internal scatter of the abundances within clusters indicates that abundance precision is generally between 0.05 and 0.09 dex across a broad temperature range; it is smaller for some elemental abundances within more limited ranges and at high signal-to-noise ratio. We assess the accuracy of the abundances using comparison of mean cluster metallicities with literature values, APOGEE observations of the solar spectrum and of Arcturus, comparison of individual star abundances with other measurements, and consideration of the locus of derived parameters and abundances of the entire sample, and find that it is challenging to determine the absolute abundance scale; external accuracy may be good to 0.1-0.2 dex. Uncertainties may be larger at cooler temperatures (T-eff < 4000 K). Access to the public data release and data products is described, and some guidance for using the data products is provided. C1 [Holtzman, Jon A.; Chojnowski, S. Drew; Feuillet, Diane; Hasselquist, Sten; Hayden, Michael R.] New Mexico State Univ, Las Cruces, NM 88003 USA. [Shetrone, Matthew] Univ Texas Austin, McDonald Observ, Ft Davis, TX 79734 USA. [Johnson, Jennifer A.; Muna, Demitri; Pinsonneault, Marc; Weinberg, David H.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. [Allende Prieto, Carlos; Carrera, Ricardo; Garcia Perez, Ana E.; Garcia-Hernandez, D. A.; Zamora, Olga] Inst Astrofis Canarias, E-38205 Tenerife, Spain. [Allende Prieto, Carlos; Carrera, Ricardo; Garcia Perez, Ana E.; Garcia-Hernandez, D. A.; Zamora, Olga] Univ La Laguna, Dept Astrofis, E-38206 Tenerife, Spain. [Anders, Friedrich] Leibniz Inst Astrophys Potsdam AIP, D-14482 Potsdam, Germany. [Anders, Friedrich] Lab Interinst & Astron LIneA, BR-20921400 Rio De Janeiro, RJ, Brazil. [Andrews, Brett; Wood-Vasey, W. M.] Univ Pittsburgh, Dept Phys & Astron, PITT PACC, Pittsburgh, PA 15260 USA. [Beers, Timothy C.] Univ Notre Dame, Dept Phys, Notre Dame, IN 46556 USA. [Beers, Timothy C.] Univ Notre Dame, JINA Ctr Evolut Elements, Notre Dame, IN 46556 USA. [Bizyaev, Dmitry; Pan, Kaike] Apache Point Observ, Sunspot, NM 88349 USA. [Blanton, Michael R.] NYU, Dept Phys, Ctr Cosmol & Particle Phys, New York, NY 10003 USA. [Bovy, Jo] Inst Adv Study, Princeton, NJ 08540 USA. [Cunha, Katia] Observ Nacl, Rio De Janeiro, Brazil. [Cunha, Katia] Univ Arizona, Tucson, AZ 85719 USA. [Eisenstein, Daniel J.; Frinchaboy, Peter M.] Texas Christian Univ, Ft Worth, TX 76129 USA. [Eisenstein, Daniel J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Galbraith-Frew, Jessica; Ivans, Inese] Univ Utah, Phys & Astron, Salt Lake City, UT 84112 USA. [Hearty, Fred R.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Hearty, Fred R.] Penn State Univ, Inst Gravitat & Cosmos, University Pk, PA 16802 USA. [Majewski, Steven R.; O'Connell, Robert W.; Shane, Neville; Sobeck, Jennifer; Troup, Nicholas; Wilson, John C.] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA. [Martell, Sarah] Univ New S Wales, Sch Phys, Sydney, NSW 2052, Australia. [Meszaros, Szabolcs] ELTE Gothard Astrophys Observ, H-9704 Szombathely, Hungary. [Nidever, David] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Duy Cuong Nguyen] Univ Toronto, Dunlap Inst Astron & Astrophys, Toronto, ON, Canada. [Robin, Annie C.] Univ Franche Comte, OSU THETA, Inst UTINAM, F-25030 Besancon, France. [Schiavon, Ricardo P.] Gemini Observ, Hilo, HI 96720 USA. [Schiavon, Ricardo P.] Liverpool John Moores Univ, Astrophys Res Inst, Liverpool L3 5RF, Merseyside, England. [Smith, Verne V.] Natl Opt Astron Observa, Tucson, AZ 85719 USA. [Zasowski, Gail] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. RP Holtzman, JA (reprint author), New Mexico State Univ, Las Cruces, NM 88003 USA. EM holtz@nmsu.edu; shetrone@astro.as.utexas.edu; jaj@astronomy.ohio-state.edu; callende@iac.es; dmbiz@apo.nmsu.edu; michael.blanton@gmail.com; cunha@email.noao.edu; deisenstein@cfa.harvard.edu; feuilldk@nmsu.edu; p.frinchaboy@tcu.edu; agp@iac.es; mrhayden@nmsu.edu; frh10@psu.edu; iii@physics.utah.edu; srm4n@virginia.edu; muna@astronomy.ohio-state.edu; dnidever@umich.edu; rwo@virginia.edu; annie@obs-besancon.fr; rpschiavon@gmail.com; vsmith@email.noao.edu; wmwv@pitt.edu; gail.zasowski@gmail.com RI Meszaros, Szabolcs/N-2287-2014; Carrera, Ricardo/K-8760-2014; OI Meszaros, Szabolcs/0000-0001-8237-5209; Carrera, Ricardo/0000-0001-6143-8151; Shane, Neville/0000-0003-1024-7739; Bovy, Jo/0000-0001-6855-442X; Bizyaev, Dmitry/0000-0002-3601-133X FU Alfred P. Sloan Foundation; National Science Foundation; U.S. Department of Energy Office of Science; National Science Foundation [AST-1109178, AST-1211673]; Spanish Ministry of Economy and Competitiveness (MINECO) [AYA2014-56359-P]; Spanish Ministry of Economy and Competitiveness [AYA-2011-27754]; Physics Frontier Center/Joint Institute or Nuclear Astrophysics (JINA) [PHY 08-22648]; Physics Frontier Center/JINA Center for the Evolution of the Elements (JINA-CEE) [PHY 14-30152]; Janos Bolyai Research Scholarship of the Hungarian Academy of Sciences; 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 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.; J. A. H., S. R. M., and V. V. S. acknowledge support for this research from the National Science Foundation (AST-1109178). J. A. J. and M. P. also acknowledge support from the National Science Foundation (AST-1211673).; C. A. P. is thankful for support from the Spanish Ministry of Economy and Competitiveness (MINECO) through grant AYA2014-56359-P.; D. A. G. H. and O. Z. acknowledge support provided by the Spanish Ministry of Economy and Competitiveness under grant AYA-2011-27754.; T. C. B. acknowledges partial support for this work from grants PHY 08-22648; Physics Frontier Center/Joint Institute or Nuclear Astrophysics (JINA), and PHY 14-30152; Physics Frontier Center/JINA Center for the Evolution of the Elements (JINA-CEE), awarded by the US National Science Foundation. S. M. has been supported by the Janos Bolyai Research Scholarship of the Hungarian Academy of Sciences. NR 45 TC 60 Z9 60 U1 1 U2 3 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 NOV PY 2015 VL 150 IS 5 AR 148 DI 10.1088/0004-6256/150/5/148 PG 27 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CY5PV UT WOS:000366460500010 ER PT J AU Torres, G Lacy, CHS Pavlovski, K Fekel, FC Muterspaugh, MW AF Torres, Guillermo Lacy, Claud H. Sandberg Pavlovski, Kresimir Fekel, Francis C. Muterspaugh, Matthew W. TI ABSOLUTE DIMENSIONS OF THE METALLIC-LINE ECLIPSING BINARY V501 MONOCEROTIS SO ASTRONOMICAL JOURNAL LA English DT Article DE binaries: eclipsing; stars: evolution; stars: fundamental parameters; stars: individual (V501 Mon); techniques: photometric; techniques: spectroscopic ID DISENTANGLED COMPONENT SPECTRA; CHEMICALLY PECULIAR STARS; PLEIADES OPEN CLUSTER; A-TYPE STARS; SPECTROSCOPIC BINARIES; ORBITAL ELEMENTS; MAIN-SEQUENCE; BOLOMETRIC CORRECTIONS; COMPOSITE SPECTRA; RADIAL-VELOCITIES AB We report extensive high-resolution spectroscopic observations and V-band differential photometry of the slightly eccentric 7.02 day detached eclipsing binary V501 Mon (A6m+ F0), which we use to determine its absolute dimensions to high precision (0.3% for the masses and 1.8% for the radii, or better). The absolute masses, radii, and temperatures are M-A = 1.6455 +/- 0.0043M(circle dot), R-A = 1.888 +/- 0.029 R-circle dot, and T-eff(A) = 7510 +/- 100 K for the primary and M-B = 1.4588 +/- 0.0025M(circle dot), R-B = 1.592 +/- 0.028 R-circle dot, and T-eff(B) = 7000 +/- 90 K for the secondary. Apsidal motion has been detected, to which General Relativity contributes approximately 70%. The primary star is found to be a metallic-line A star. A detailed chemical analysis of the disentangled spectra yields abundances for more than a dozen elements in each star. Based on the secondary, the system metallicity is near solar: [Fe/H] = + 0.01 +/- 0.06. Lithium is detected in the secondary but not in the primary. A comparison with current stellar evolution models shows a good match to the measured properties at an age of about 1.1 Gyr. C1 [Torres, Guillermo] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Lacy, Claud H. Sandberg] Univ Arkansas, Dept Phys, Fayetteville, AR 72701 USA. [Pavlovski, Kresimir] Univ Zagreb, Dept Phys, Fac Sci, Zagreb 10000, Croatia. [Fekel, Francis C.; Muterspaugh, Matthew W.] Tennessee State Univ, Ctr Excellence Informat Syst, Nashville, TN 37209 USA. [Muterspaugh, Matthew W.] Tennessee State Univ, Dept Math Sci, Coll Sci & Math, Nashville, TN 37209 USA. RP Torres, G (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM gtorres@cfa.harvard.edu OI Fekel, Francis/0000-0002-9413-3896 FU NSF grant [AST-1509375]; Croatian Science Foundation [2014-09-8656]; state of Tennessee through its Centers of Excellence program; NSF grant from the Major Research Instrumentation Program [1039522] FX We are grateful to P. Berlind, W. Brown, M. Calkins, G. Esquerdo, D. Latham, A. Milone, R. Stefanik, S. Tang, and S. Quinn for help in obtaining the CfA observations of V501 Mon with the DS and with TRES, and to R. J. Davis and J. Mink for maintaining the CfA echelle databases over the years. M. Wolf kindly provided his photometric measurements of a secondary eclipse of V501 Mon. The authors also wish to thank Bill Neely, who operates and maintains the NFO WebScope for the Consortium, and who handles preliminary processing of the images and their distribution. G. T. acknowledges partial support for this work from NSF grant AST-1509375. The work of KP has been supported in part by the Croatian Science Foundation under grant 2014-09-8656. NSF grant 1039522 from the Major Research Instrumentation Program, which was awarded to Tennessee State University, enabled the acquisition of the Fairborn observations. In addition, astronomy at Tennessee State is supported by the state of Tennessee through its Centers of Excellence program. This research has made use of the SIMBAD and VizieR databases, operated at CDS, Strasbourg, France, and of NASA's Astrophysics Data System Abstract Service. NR 84 TC 3 Z9 3 U1 0 U2 0 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 NOV PY 2015 VL 150 IS 5 AR 154 DI 10.1088/0004-6256/150/5/154 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CY5PV UT WOS:000366460500016 ER PT J AU Wolk, SJ Gunther, HM Poppenhaeger, K Cody, AM Rebull, LM Forbrich, J Gutermuth, RA Hillenbrand, LA Plavchan, P Stauffer, JR Covey, KR Song, I AF Wolk, Scott J. Guenther, H. Moritz Poppenhaeger, Katja Cody, A. M. Rebull, L. M. Forbrich, J. Gutermuth, R. A. Hillenbrand, L. A. Plavchan, P. Stauffer, J. R. Covey, K. R. Song, Inseok TI YSOVAR: MID-INFRARED VARIABILITY AMONG YSOs IN THE STAR FORMATION REGION GGD12-15 SO ASTRONOMICAL JOURNAL LA English DT Article DE infrared: stars; stars: evolution; stars: formation; stars: pre-main sequence; stars: protostars; stars: variables: T Tauri, Herbig Ae/Be ID YOUNG STELLAR OBJECTS; MAIN-SEQUENCE STARS; T-TAURI STARS; INFRARED PHOTOMETRIC VARIABILITY; POINT-SOURCE IDENTIFICATION; SPITZER-SPACE-TELESCOPE; HERBIG-HARO OBJECTS; ARRAY CAMERA IRAC; H-II REGIONS; X-RAY AB We present an IR-monitoring survey with the Spitzer Space Telescope of the star-forming region GGD 12-15. More than 1000 objects were monitored, including about 350 objects within the central 5', which is found to be especially dense in cluster members. The monitoring took place over 38 days and is part of the Young Stellar Object VARiability project. The region was also the subject of a contemporaneous 67 ks Chandra observation. The field includes 119 previously identified pre-main sequence star candidates. X-rays are detected from 164 objects, 90 of which are identified with cluster members. Overall, we find that about half the objects in the central 5' are young stellar objects (YSOs) based on a combination of their spectral energy distribution, IR variability, and X-ray emission. Most of the stars with IR excess relative to a photosphere show large amplitude (>0.1 mag) mid-infrared (mid-IR) variability. There are 39 periodic sources, and all but one is found to be a cluster member. Almost half of the periodic sources do not show IR excesses. Overall, more than 85% of the Class I, flat spectrum, and Class II sources are found to vary. The amplitude of the variability is larger in more embedded YSOs. Most of the Class I/II objects exhibit redder colors in a fainter state, which is compatible with time-variable extinction. A few become bluer when fainter, which can be explained with significant changes in the structure of the inner disk. A search for changes in the IR due to X-ray events is carried out, but the low number of flares prevented an analysis of the direct impact of X-ray flares on the IR light curves. However, we find that X-ray detected Class II sources have longer timescales for change in the MIR than a similar set of non-X-ray detected Class IIs. C1 [Wolk, Scott J.; Guenther, H. Moritz; Poppenhaeger, Katja] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Guenther, H. Moritz] MIT Kavli Inst, Cambridge, MA 02139 USA. [Cody, A. M.] NASA Ames Res Ctr, Moffett Field, CA 94035 USA. [Cody, A. M.] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. [Rebull, L. M.; Stauffer, J. R.] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. [Forbrich, J.] Univ Vienna, Dept Astrophys, A-1180 Vienna, Austria. [Gutermuth, R. A.] Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA. [Hillenbrand, L. A.] CALTECH, Dept Astron, Pasadena, CA 91125 USA. [Plavchan, P.] Missouri State Univ, Dept Phys Astron & Mat Sci, Springfield, MO 65897 USA. [Covey, K. R.] Western Washington Univ, Dept Phys & Astron, Bellingham, WA 98225 USA. [Song, Inseok] Univ Georgia, Dept Phys & Astron, Athens, GA 30602 USA. RP Wolk, SJ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM swolk@cfa.harvard.edu OI Gunther, Hans Moritz/0000-0003-4243-2840; Poppenhaeger, Katja/0000-0003-1231-2194; Wolk, Scott/0000-0002-0826-9261; Rebull, Luisa/0000-0001-6381-515X; Plavchan, Peter/0000-0002-8864-1667; Covey, Kevin/0000-0001-6914-7797 FU NASA; National Aeronautics and Space Administration; National Science Foundation; Spitzer [1490851]; NASA Exoplanet Science Institute; IPAC Visiting Graduate Fellowship program at Caltech/IPAC; NASA ADAP [NNX11AD14G, NNX13AF08G]; Caltech/JPL [1373081, 1424329, 1440160]; NASA [NAS8-03060] FX This work is based on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. Support for this work was provided by NASA through an award issued by JPL/Caltech. This research made use of Astropy, a community-developed core Python package for Astronomy (Astropy Collaboration et al. 2013). This research has made use of the SIMBAD database and the VizieR catalog access tool (Ochsenbein et al. 2000), both operated at CDS, Strasbourg, France, and of data products from the Two Micron All Sky Survey, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology, funded by the National Aeronautics and Space Administration and the National Science Foundation. H.M.G. acknowledges Spitzer grant 1490851. K.P. was funded through the Sagan Fellowship program executed by the NASA Exoplanet Science Institute. H.Y.A.M. and P.P. acknowledge support by the IPAC Visiting Graduate Fellowship program at Caltech/IPAC. P.P. also acknowledges the JPL Research and Technology Development and Exoplanet Exploration programs. R.A.G. gratefully acknowledges funding support from NASA ADAP grants NNX11AD14G and NNX13AF08G and Caltech/JPL awards 1373081, 1424329, and 1440160 in support of Spitzer Space Telescope observing programs. S.J.W. was supported by NASA contract NAS8-03060. We thank Fabio Favata and David James for critical readings of this paper. NR 81 TC 7 Z9 7 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 EI 1538-3881 J9 ASTRON J JI Astron. J. PD NOV PY 2015 VL 150 IS 5 AR 145 DI 10.1088/0004-6256/150/5/145 PG 23 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CY5PV UT WOS:000366460500007 ER PT J AU Kartaltepe, JS Mozena, M Kocevski, D McIntosh, DH Lotz, J Bell, EF Faber, S Ferguson, H Koo, D Bassett, R Bernyk, M Blancato, K Bournaud, F Cassata, P Castellano, M Cheung, E Conselice, CJ Croton, D Dahlen, T De Mello, DF DeGroot, L Donley, J Guedes, J Grogin, N Hathi, N Hilton, M Hollon, B Koekemoer, A Liu, N Lucas, RA Martig, M McGrath, E McPartland, C Mobasher, B Morlock, A O'Leary, E Peth, M Pforr, J Pillepich, A Rosario, D Soto, E Straughn, A Telford, O Sunnquist, B Trump, J Weiner, B Wuyts, S AF Kartaltepe, Jeyhan S. Mozena, Mark Kocevski, Dale McIntosh, Daniel H. Lotz, Jennifer Bell, Eric F. Faber, Sandy Ferguson, Harry Koo, David Bassett, Robert Bernyk, Maksym Blancato, Kirsten Bournaud, Frederic Cassata, Paolo Castellano, Marco Cheung, Edmond Conselice, Christopher J. Croton, Darren Dahlen, Tomas De Mello, Duilia F. DeGroot, Laura Donley, Jennifer Guedes, Javiera Grogin, Norman Hathi, Nimish Hilton, Matt Hollon, Brett Koekemoer, Anton Liu, Nick Lucas, Ray A. Martig, Marie McGrath, Elizabeth McPartland, Conor Mobasher, Bahram Morlock, Alice O'Leary, Erin Peth, Mike Pforr, Janine Pillepich, Annalisa Rosario, David Soto, Emmaris Straughn, Amber Telford, Olivia Sunnquist, Ben Trump, Jonathan Weiner, Benjamin Wuyts, Stijn TI CANDELS VISUAL CLASSIFICATIONS: SCHEME, DATA RELEASE, AND FIRST RESULTS SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE cosmology: observations; galaxies: evolution; galaxies: high-redshift ID SIMILAR-TO 2; DIGITAL-SKY-SURVEY; SPACE-TELESCOPE OBSERVATIONS; EXTRAGALACTIC LEGACY SURVEY; STAR-FORMING GALAXIES; LESS-THAN 3; MASSIVE GALAXIES; HUBBLE SEQUENCE; MORPHOLOGICAL CLASSIFICATIONS; QUIESCENT GALAXIES AB We have undertaken an ambitious program to visually classify all galaxies in the five CANDELS fields down to H < 24.5 involving the dedicated efforts of over 65 individual classifiers. Once completed, we expect to have detailed morphological classifications for over 50,000 galaxies spanning 0 < z < 4 over all the fields, with classifications from 3 to 5 independent classifiers for each galaxy. Here, we present our detailed visual classification scheme, which was designed to cover a wide range of CANDELS science goals. This scheme includes the basic Hubble sequence types, but also includes a detailed look at mergers and interactions, the clumpiness of galaxies, k-corrections, and a variety of other structural properties. In this paper, we focus on the first field to be completed-GOODS-S, which has been classified at various depths. The wide area coverage spanning the full field (wide+deep+ERS) includes 7634 galaxies that have been classified by at least three different people. In the deep area of the field, 2534 galaxies have been classified by at least five different people at three different depths. With this paper, we release to the public all of the visual classifications in GOODS-S along with the Perl/Tk GUI that we developed to classify galaxies. We present our initial results here, including an analysis of our internal consistency and comparisons among multiple classifiers as well as a comparison to the Sersic index. We find that the level of agreement among classifiers is quite good (>70% across the full magnitude range) and depends on both the galaxy magnitude and the galaxy type, with disks showing the highest level of agreement (>50%) and irregulars the lowest (<10%). A comparison of our classifications with the Sersic index and rest-frame colors shows a clear separation between disk and spheroid populations. Finally, we explore morphological k-corrections between the V-band and H-band observations and find that a small fraction (84 galaxies in total) are classified as being very different between these two bands. These galaxies typically have very clumpy and extended morphology or are very faint in the V-band. C1 [Kartaltepe, Jeyhan S.] Rochester Inst Technol, Sch Phys & Astron, Rochester, NY 14623 USA. [Kartaltepe, Jeyhan S.; Blancato, Kirsten; O'Leary, Erin; Pforr, Janine] Natl Opt Astron Observ, Tucson, AZ 85719 USA. [Mozena, Mark; Faber, Sandy; Koo, David; Cheung, Edmond] Univ Calif Santa Cruz, Univ Calif Observ Lick Observ, Santa Cruz, CA 95064 USA. [Kocevski, Dale] Univ Kentucky, Dept Phys & Astron, Lexington, KY 40506 USA. [McIntosh, Daniel H.; Hollon, Brett] Univ Missouri, Dept Phys, Kansas City, MO 64110 USA. [Lotz, Jennifer; Ferguson, Harry; Grogin, Norman; Koekemoer, Anton] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Bell, Eric F.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Bassett, Robert; Bernyk, Maksym; Croton, Darren; Martig, Marie] Swinburne Univ Technol, Ctr Astrophys & Supercomp, Hawthorn, Vic 3122, Australia. [Blancato, Kirsten] Wellesley Coll, Dept Astron, Wellesley, MA 02481 USA. [Bournaud, Frederic] Univ Paris Diderot, CE Saclay, CEA DSM Irfu CNRS, Lab AIM Paris Saclay, F-91191 Gif Sur Yvette, France. [Cassata, Paolo] Aix Marseille Univ, CNRS, LAM UMR 7326, F-13388 Marseille, France. [Castellano, Marco] IINAFOsserv Astron Roma, I-00040 Monte Porzio Catone, Italy. [Conselice, Christopher J.; Morlock, Alice] Univ Nottingham, Sch Phys & Astron, Nottingham NG7 2RD, England. [De Mello, Duilia F.; Soto, Emmaris] Catholic Univ Amer, Washington, DC 20064 USA. [DeGroot, Laura; Donley, Jennifer; Hathi, Nimish; Mobasher, Bahram] Univ Calif Riverside, Dept Phys & Astron, Riverside, CA 92521 USA. [Donley, Jennifer] Los Alamos Natl Lab, Los Alamos, NM USA. [Guedes, Javiera] ETH, Inst Astron, CH-8093 Zurich, Switzerland. [Hilton, Matt] Univ KwaZulu Natal, Sch Math Stat & Comp Sci, Astrophys & Cosmol Res Unit, ZA-4041 Durban, South Africa. [Liu, Nick] Pioneer High Sch, Ann Arbor, MI 48103 USA. [McGrath, Elizabeth] Colby Coll, Dept Phys & Astron, Waterville, ME 04901 USA. [McPartland, Conor] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [O'Leary, Erin] Macalester Coll, Dept Phys & Astron, St Paul, MN 55105 USA. [Peth, Mike] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Pillepich, Annalisa] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Rosario, David] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Straughn, Amber] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA. [Telford, Olivia] Univ Washington, Dept Astron, Seattle, WA 98195 USA. [Trump, Jonathan] Penn State, State Coll, PA USA. [Weiner, Benjamin] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Wuyts, Stijn] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. RP Kartaltepe, JS (reprint author), Rochester Inst Technol, Sch Phys & Astron, 84 Lomb Mem Dr, Rochester, NY 14623 USA. EM jeyhan@astro.rit.edu RI Hathi, Nimish/J-7092-2014; OI Hathi, Nimish/0000-0001-6145-5090; Cheung, Edmond/0000-0001-8546-1428; Martig, Marie/0000-0001-5454-1492; Koekemoer, Anton/0000-0002-6610-2048; Bell, Eric/0000-0002-5564-9873 FU NASA through Hubble Fellowship - Space Telescope Science Institute [HST-HF-51292.01A]; NASA [NAS 5-26555, NAS5-26555]; NASA through a grant from the Space Telescope Science Institute [HST-GO-12060]; NOAO/KPNO Research Experiences for Undergraduates (REU) Program from the National Science Foundation Research Experiences for Undergraduates Program [AST-0754223, AST-1262829] FX Support for this work was provided by NASA through Hubble Fellowship grant # HST-HF-51292.01A 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. Support for Program number HST-GO-12060 was provided by NASA through a grant from the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Incorporated, under NASA contract NAS5-26555. O'Leary and Blancato were supported by the NOAO/KPNO Research Experiences for Undergraduates (REU) Program with two grants from the National Science Foundation Research Experiences for Undergraduates Program (AST-0754223, AST-1262829). NR 72 TC 16 Z9 16 U1 0 U2 0 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 NOV PY 2015 VL 221 IS 1 AR 11 DI 10.1088/0067-0049/221/1/11 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CY7WS UT WOS:000366620600011 ER PT J AU Rauw, G Naze, Y Wright, NJ Drake, JJ Guarcello, MG Prinja, RK Peck, LW Colombo, JFA Herrero, A Kobulnicky, HA Sciortino, S Vink, JS AF Rauw, G. Naze, Y. Wright, N. J. Drake, J. J. Guarcello, M. G. Prinja, R. K. Peck, L. W. Albacete Colombo, J. F. Herrero, A. Kobulnicky, H. A. Sciortino, S. Vink, J. S. TI X-RAY EMISSION FROM MASSIVE STARS IN CYG OB2 SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE open clusters and associations: individual (Cyg OB2); stars: early-type; stars: Wolf-Rayet; X-rays: stars ID COLLIDING-WIND BINARY; O-TYPE STARS; RADIAL-VELOCITY SURVEY; STELLAR WINDS; XMM-NEWTON; WR 146; B-STARS; CLASSIFICATION-SYSTEM; ASSOCIATION; CLUSTERS AB We report on the analysis of the Chandra-ACIS data of O, B, and WR stars in the young association Cyg OB2. X-ray spectra of 49 O-stars, 54 B-stars, and 3 WR-stars are analyzed and for the brighter sources, the epoch dependence of the X-ray fluxes is investigated. The O-stars in Cyg OB2 follow a well-defined scaling relation between their X-ray and bolometric luminosities: log L-X/L-bol = -7.2 +/- 0.2. This relation is in excellent agreement with the one previously derived for the Carina OB1 association. Except for the brightest O-star binaries, there is no general X-ray overluminosity due to colliding winds in O-star binaries. Roughly half of the known B-stars in the surveyed field are detected, but they fail to display a clear relationship between L-X and L-bol. Out of the three WR stars in Cyg OB2, probably only WR 144 is itself responsible for the observed level of X-ray emission, at a very low log L-X/L-bol = -8.8 +/- 0.2. The X-ray emission of the other two WR-stars (WR 145 and 146) is most probably due to their O-type companion along with a moderate contribution from a wind-wind interaction zone. C1 [Rauw, G.; Naze, Y.] Univ Liege, Inst Astrophys & Geophys, B-4000 Liege, Belgium. [Wright, N. J.; Drake, J. J.; Guarcello, M. G.] Smithsonian Astrophys Observ, Cambridge, MA USA. [Prinja, R. K.; Peck, L. W.] UCL, Dept Phys & Astron, London WC1E 6BT, England. [Albacete Colombo, J. F.] Univ Nacl Comahue, Ctr Reg Zona Atlantica, Viedma, Argentina. [Herrero, A.] Univ La Laguna, Inst Astrofis Canarias, E-38207 San Cristobal la Laguna, Spain. [Kobulnicky, H. A.] Univ Wyoming, Dept Phys & Astron, Laramie, WY 82071 USA. [Sciortino, S.] Osserv Astron Palermo, INAF, Palermo, Italy. [Vink, J. S.] Armagh Observ, Armagh BT61 9DG, North Ireland. [Wright, N. J.] Univ Hertfordshire, Ctr Astrophys Res, Hatfield AL10 9AB, Herts, England. RP Rauw, G (reprint author), Univ Liege, Inst Astrophys & Geophys, B-4000 Liege, Belgium. EM rauw@astro.ulg.ac.be OI Naze, Yael/0000-0003-4071-9346 FU Belspo through an XMM PRODEX contract; FRS/FNRS; ARC grant for Concerted Research Actions - Federation Wallonia-Brussels; Royal Astronomical Society research fellowship FX The Liege team acknowledges support from Belspo through an XMM PRODEX contract, from the FRS/FNRS and from an ARC grant for Concerted Research Actions, financed by the Federation Wallonia-Brussels. N.J.W. was supported by a Royal Astronomical Society research fellowship. NR 73 TC 6 Z9 6 U1 0 U2 1 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 NOV PY 2015 VL 221 IS 1 AR 1 DI 10.1088/0067-0049/221/1/1 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CY7WS UT WOS:000366620600001 ER PT J AU Pena, V Pardo, C Lopez, L Carro, B Hernandez-Kantun, J Adey, WH Barbara, I Barreiro, R Le Gall, L AF Pena, Viviana Pardo, Cristina Lopez, Lua Carro, Belen Hernandez-Kantun, Jazmin Adey, Walter H. Barbara, Ignacio Barreiro, Rodolfo Le Gall, Line TI Phymatolithon lusitanicum sp nov (Hapalidiales, Rhodophyta): the third most abundant maerl-forming species in the Atlantic Iberian Peninsula SO CRYPTOGAMIE ALGOLOGIE LA English DT Article DE Biodiversity; DNA barcoding; Lithothamnion hamelii; Mediterranean; NE Atlantic; Phymatolithon laevigatum; Phymatolithon lamii; systematics ID CORALLINALES; DIVERSITY; MODELS AB Phymatolithon lusitanicum is a new maerl species described based on an integrative systematic approach including molecular (COI-5P, psbA) and morphological data obtained from recent collections, as well as comparison of type material from the morphologically and ecologically alike NE Atlantic species P. lamii and P. laevigatum. Molecular analyses including type material of P. lamii and P. laevigatum were congruent in delimiting P. lusitanicum as an independent lineage from these crustose species. The three species shared a common external morphology of multiporate asexual conceptacles, but P. lusitanicum has been detected only unattached as maerl while P. lamii and P. laevigatum are crustose. Phymatolithon lusitanicum is particularly abundant in subtidal maerl beds of the Atlantic Iberian Peninsula (Galicia and the Algarve); however it has also been detected northwards in Ireland intertidally and in Western Mediterranean Sea (Alboran Sea, Balearic Islands) down to 64 m. Phymatolithon lusitanicum differs from other Phymatolithon species reported for the European coasts mainly by the external shape of the multiporate asexual conceptacles (pore plate flush with surface or slightly sunken without a conspicuous thick raised rim) and its unattached habit as maerl/rhodolith. In addition, the lectotype of Lithothamnion hamelii turned out to be conspecific to Phymatolithon calcareum, therefore this taxon is proposed as a heterotypic synonym of P. calcareum. Finally, our molecular analyses detected cryptic diversity within the European collections of Phymatolithon, while collections identified as P. lenormandii from Canada or P. repandum from New Zealand were resolved as unrelated to the remaining Phymatolithon. In the light of these results, it is clear that further work is necessary to resolve species diversity within the genus Phymatolithon and its relationship with related genera. C1 [Pena, Viviana; Pardo, Cristina; Lopez, Lua; Carro, Belen; Barbara, Ignacio; Barreiro, Rodolfo] Univ A Coruna, Fac Ciencias, BIOCOST Res Grp, La Coruna 15071, Spain. [Pena, Viviana; Le Gall, Line] Univ Paris 04, UPMC, UMR ISYEB CNRS 7205,MNHN,EPHE, Equipe Explorat Especes & Evolut,Inst Systemat,Ev, F-75005 Paris, France. [Hernandez-Kantun, Jazmin; Adey, Walter H.] Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, Washington, DC 20560 USA. RP Pena, V (reprint author), Univ A Coruna, Fac Ciencias, BIOCOST Res Grp, Campus A Coruna, La Coruna 15071, Spain. EM vpena@udc.es RI Lopez, Lua/A-9710-2016; Le Gall, Line/E-1884-2014; Barreiro, Rodolfo/B-1005-2008; OI Lopez, Lua/0000-0002-3619-763X; Le Gall, Line/0000-0001-7807-4569; Barreiro, Rodolfo/0000-0002-6049-5215; Pena, Viviana/0000-0001-7003-3850 FU Action Transversale du Museum National d'Histoire Naturelle; British Phycological Society; Spain's Ministerio de Economia y Competitividad [CTM2010-18787]; ERDF; Xunta de Galicia [10MMA103003PR]; network 'Bibliotheque du Vivant' - CNRS; Museum National d'Histoire Naturelle; INRA; CEA (Centre National de Sequencage); postdoctoral programmes Axudas de apoio a etapa inicial de formacion posdoutoral do Plan I2C (Xunta de Galicia); Programa FPU (Spain's Ministerio de Educacion); Smithsonian Institution FX Financial support came from the following institutions and projects: Action Transversale du Museum National d'Histoire Naturelle ("Taxonomie moleculaire: DNA Barcode et gestion durable des collections" and "Biodiversite actuelle et fossile. Crises, stress, restaurations et panchronisme: le message systematique" and "Emergences"), British Phycological Society (Small Grant Scheme-Project Award 2011-2012), Spain's Ministerio de Economia y Competitividad (CTM2010-18787, partially founded by ERDF) and Xunta de Galicia (10MMA103003PR). Acquisition of molecular data was carried out at the CNRS-UMS 2700 in Service de Systematique Moleculaire, MNHN, Paris. This project was supported by the network 'Bibliotheque du Vivant' funded by CNRS, Museum National d'Histoire Naturelle, INRA and CEA (Centre National de Sequencage). VPF acknowledges support by the postdoctoral programmes Axudas de apoio a etapa inicial de formacion posdoutoral do Plan I2C (Xunta de Galicia). CP acknowledges support by Programa FPU-2010 (Spain's Ministerio de Educacion). JJHK acknowledges support by the Smithsonian Institution through a postdoctoral fellowship and Gabriel Johnson through technical assistance. We sincerely thank Jacques Grall, Antonio Secilla, Alberto Santolaria, Jan Rueness, Francis Bunker, Veronica Garcia, Pilar Diaz, Isabel Maneiro, Pedro Neves, Meadhbh Moriarty, Declan Hanniffy and Miguel Rodrigues for field collaboration and/or for providing samples. We also thank project INDEMARES for providing samples from Alboran Sea. We are also grateful to both reviewers for their helpful comments on the manuscript. NR 46 TC 6 Z9 6 U1 0 U2 1 PU ADAC-CRYPTOGAMIE PI PARIS PA 12 RUE DE BUFFON, 75005 PARIS, FRANCE SN 0181-1568 EI 1776-0984 J9 CRYPTOGAMIE ALGOL JI Cryptogam. Algol. PD NOV PY 2015 VL 36 IS 4 BP 429 EP 459 DI 10.7872/crya/v36.iss4.2015.429 PG 31 WC Plant Sciences; Marine & Freshwater Biology SC Plant Sciences; Marine & Freshwater Biology GA CY3AK UT WOS:000366280000004 ER PT J AU St Clair, JJH Burns, ZT Bettaney, EM Morrissey, MB Otis, B Ryder, TB Fleischer, RC James, R Rutz, C AF St Clair, James J. H. Burns, Zackory T. Bettaney, Elaine M. Morrissey, Michael B. Otis, Brian Ryder, Thomas B. Fleischer, Robert C. James, Richard Rutz, Christian TI Experimental resource pulses influence social-network dynamics and the potential for information flow in tool-using crows SO NATURE COMMUNICATIONS LA English DT Article ID CALEDONIAN CROWS; CORVUS-MONEDULOIDES; PROXIMITY LOGGERS; WILD BIRDS; GENETIC-MARKERS; EVOLUTION; CONSEQUENCES; MANUFACTURE; ELEPHANTS; PATTERNS AB Social-network dynamics have profound consequences for biological processes such as information flow, but are notoriously difficult to measure in the wild. We used novel transceiver technology to chart association patterns across 19 days in a wild population of the New Caledonian crow-a tool-using species that may socially learn, and culturally accumulate, tool-related information. To examine the causes and consequences of changing network topology, we manipulated the environmental availability of the crows' preferred tool-extracted prey, and simulated, in silico, the diffusion of information across field-recorded time-ordered networks. Here we show that network structure responds quickly to environmental change and that novel information can potentially spread rapidly within multi-family communities, especially when tool-use opportunities are plentiful. At the same time, we report surprisingly limited social contact between neighbouring crow communities. Such scale dependence in information-flow dynamics is likely to influence the evolution and maintenance of material cultures. C1 [St Clair, James J. H.; Burns, Zackory T.; Rutz, Christian] Univ Oxford, Dept Zool, Oxford OX1 3PS, England. [Bettaney, Elaine M.; James, Richard] Univ Bath, Dept Phys, Bath BA2 7AY, Avon, England. [Bettaney, Elaine M.; James, Richard] Univ Bath, Ctr Networks & Collect Behav, Bath BA2 7AY, Avon, England. [Morrissey, Michael B.] Univ St Andrews, Ctr Biol Divers, Sch Biol, St Andrews KY16 9TH, Fife, Scotland. [Otis, Brian] Univ Washington, Dept Elect Engn, Seattle, WA 98195 USA. [Ryder, Thomas B.; Fleischer, Robert C.] Smithsonian Conservat Biol Inst, Washington, DC 20013 USA. RP St Clair, JJH (reprint author), Univ Oxford, Dept Zool, Oxford OX1 3PS, England. EM jsc20@st-andrews.ac.uk; r.james@bath.ac.uk; christian.rutz@st-andrews.ac.uk RI James, Richard/E-5061-2013; Morrissey, Michael/F-3226-2010; OI Morrissey, Michael/0000-0001-6209-0177; St Clair, James/0000-0003-2902-4391 FU Biotechnology and Biological Sciences Research Council [BB/G023913/1, BB/G023913/2] FX We thank: T. Mennesson, J.-E. Lombardet and C. Lambert for facilitating fieldwork; the Province Sud and SEM Mwe Ara for invaluable logistical support in New Caledonia; J. Burt for help adapting the Encounternet hard and software for this project, and for assistance with fieldwork; Jayson Bowen for contributions to system development; C. Anagnostou and S.M.H. Ismar for field assistance; W. Loo and C.G.M. Paxton for help with R code; and J. Troscianko for permission to use his crow photograph. The project was approved by the University of Oxford's local ethical review committee, carried out with the permission of the DENV, Province Sud, New Caledonia (permits 1341-2010/ARR/DENV and 1886-2011/ARR/DENV), and funded by the Biotechnology and Biological Sciences Research Council (David Phillips Fellowship to C.R.: grant numbers BB/G023913/1 and /2), with contributions for genetic analyses by the Smithsonian Conservation Biology Institute's Center for Conservation and Evolutionary Genetics. NR 51 TC 9 Z9 9 U1 4 U2 23 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 NOV PY 2015 VL 6 AR 7197 DI 10.1038/ncomms8197 PG 8 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA CY3CI UT WOS:000366285400001 PM 26529116 ER PT J AU Hoyos-Santillan, J Lomax, BH Large, D Turner, BL Boom, A Lopez, OR Sjogersten, S AF Hoyos-Santillan, Jorge Lomax, Barry H. Large, David Turner, Benjamin L. Boom, Arnoud Lopez, Omar R. Sjoegersten, Sofie TI Getting to the root of the problem: litter decomposition and peat formation in lowland Neotropical peatlands SO BIOGEOCHEMISTRY LA English DT Article DE Carbon; Litter decomposition; Root; Tropical peat; Pyrolysis; Mass spectrometry ID SOIL ORGANIC-MATTER; PYROLYSIS-GC-MS; LEAF-LITTER; TERRESTRIAL ECOSYSTEMS; CARBON ACCUMULATION; CONIFEROUS FORESTS; OMBROTROPHIC PEAT; NITROGEN DYNAMICS; GLOBAL PATTERNS; PLANT CUTICLES AB Litter decomposition is an important control on carbon accumulation in tropical peatlands. We investigated the contribution of different litter tissues from two peatland tree species (Raphia taedigera and Campnosperma panamensis) to peat formation in four lowland tropical peatlands in the Republic of Panama. Leaves, stems, and roots decomposed at different rates; with roots being the slowest to decompose among tissues. The position of litter in the peat profile strongly influenced the decomposition rate of all tissue types. Roots decomposed up to five times faster at the surface than at 50 cm depth. Molecular characterization of litter and peat profiles by tetramethylammonium-pyrolysis-gas chromatography-mass spectrometry (TMAH-Py-GC/MS) revealed that the peat is formed predominantly of decomposed roots and stems, as indicated by the high lignin, low methylated fatty acids and carbohydrate concentrations in these litter types. Taken together, these data demonstrate that roots play a fundamental role in the formation of lowland Neotropical peatlands. C1 [Hoyos-Santillan, Jorge; Lomax, Barry H.; Sjoegersten, Sofie] Univ Nottingham, Sch Biosci, Div Agr & Environm Sci, Loughborough LE12 5RD, Leics, England. [Large, David] Univ Nottingham, Dept Chem & Environm Engn, Nottingham NG7 2RD, England. [Turner, Benjamin L.] Smithsonian Trop Res Inst, Balboa 084303092, Ancon, Panama. [Boom, Arnoud] Univ Leicester, Dept Geog, Leicester LE1 7RH, Leics, England. [Lopez, Omar R.] Inst Invest Cient & Serv Alta Tecnol INDICASAT AI, Ctr Biodiversidad & Descubrimiento Drogas, Clayton 084301103, Panama. RP Sjogersten, S (reprint author), Univ Nottingham, Sch Biosci, Div Agr & Environm Sci, Room C-36 Gateway Bldg,Sutton Bonington Campus, Loughborough LE12 5RD, Leics, England. EM Sofie.Sjogersten@nottingham.ac.uk RI Turner, Benjamin/E-5940-2011; Lomax, Barry/B-1136-2010; OI Turner, Benjamin/0000-0002-6585-0722; Lomax, Barry/0000-0003-0475-7839; Boom, Arnoud/0000-0003-1299-691X FU National Council on Science and Technology (CONACyT-Mexico) [211962]; Light Hawk program FX Data to support this article can be made available upon request. Jorge Hoyos-Santillan thanks The National Council on Science and Technology (CONACyT-Mexico) for his Ph.D. scholarship (211962). The authors also thank the Light Hawk program for its support in the aerial surveys. We thank Erick Brown for invaluable help as field assistant; as well as Gabriel Jacome, Plinio Gondola, Tania Romero and Dayana Agudo for logistical support and laboratory assistance at the STRI. In addition, we thank John Corrie and Darren Hepworth for their help in logistics and laboratory assistance at the University of Nottingham. NR 84 TC 4 Z9 4 U1 5 U2 21 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0168-2563 EI 1573-515X J9 BIOGEOCHEMISTRY JI Biogeochemistry PD NOV PY 2015 VL 126 IS 1-2 BP 115 EP 129 DI 10.1007/s10533-015-0147-7 PG 15 WC Environmental Sciences; Geosciences, Multidisciplinary SC Environmental Sciences & Ecology; Geology GA CX7FU UT WOS:000365868400008 ER PT J AU Feller, IC Dangremond, EM Devlin, DJ Lovelock, CE Proffitt, CE Rodriguez, W AF Feller, Ilka C. Dangremond, Emily M. Devlin, Donna J. Lovelock, Catherine E. Proffitt, C. Edward Rodriguez, Wilfrid TI Nutrient enrichment intensifies hurricane impact in scrub mangrove ecosystems in the Indian River Lagoon, Florida, USA SO ECOLOGY LA English DT Article DE coarse woody debris; delayed mortality; disturbance; Florida; growth rate; hurricane; Indian River Lagoon; leaf area index; mangrove forest; nutrient enrichment; resilience; resistance ID RHIZOPHORA-MANGLE; FOREST STRUCTURE; TROPICAL CYCLONES; SOUTH FLORIDA; WATER-QUALITY; COASTAL EUTROPHICATION; PRIMARY PRODUCTIVITY; MULTIPLE HURRICANES; CHARLOTTE HARBOR; TREE MORTALITY AB Mangroves are an ecological assemblage of trees and shrubs adapted to grow in intertidal environments along tropical, subtropical, and warm temperate coasts. Despite repeated demonstrations of their ecologic and economic value, multiple stressors including nutrient over-enrichment threaten these and other coastal wetlands globally. These ecosystems will be further stressed if tropical storm intensity and frequency increase in response to global climate changes. These stressors will likely interact, but the outcome of that interaction is uncertain. Here, we examined potential interaction between nutrient over-enrichment and the September 2004 hurricanes. Hurricanes Frances and Jeanne made landfall along Florida's Indian River Lagoon and caused extensive damage to a long-term fertilization experiment in a mangrove forest, which previously revealed that productivity was nitrogen (N) limited across the forest and, in particular, that N enrichment dramatically increased growth rates and aboveground biomass of stunted Avicennia germinans trees in the interior scrub zone. During the hurricanes, these trees experienced significant defoliation with three to four times greater reduction in leaf area index (LAI) than control trees. Over the long term, the +N scrub trees took four years to recover compared to two years for controls. In the adjacent fringe and transition zones, LAI was reduced by >70%, but with no differences based on zone or fertilization treatment. Despite continued delayed mortality for at least five years after the storms, LAI in the fringe and transition returned to pre-hurricane conditions in two years. Thus, nutrient over-enrichment of the coastal zone will increase the productivity of scrub mangroves, which dominate much of the mangrove landscape in Florida and the Caribbean; however, that benefit is offset by a decrease in their resistance and resilience to hurricane damage that has the potential to destabilize the system. C1 [Feller, Ilka C.; Dangremond, Emily M.; Rodriguez, Wilfrid] Smithsonian Inst, Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. [Devlin, Donna J.; Proffitt, C. Edward] Florida Atlantic Univ, Charles E Schmidt Coll Sci, Harbor Branch Oceanog Inst, Dept Biol Sci, Ft Pierce, FL 34946 USA. [Lovelock, Catherine E.] Univ Queensland, Sch Integrat Biol, Ctr Marine Studies, St Lucia, Qld 4072, Australia. RP Feller, IC (reprint author), Smithsonian Inst, Smithsonian Environm Res Ctr, 647 Contees Wharf Rd, Edgewater, MD 21037 USA. EM felleri@si.edu RI Lovelock, Catherine/G-7370-2012; OI Lovelock, Catherine/0000-0002-2219-6855; Feller, Ilka/0000-0002-6391-1608 FU NASA Climate and Biological Response program [NNX11AO94G]; NSF MacroSystems Biology program [EF1065821] FX We thank the Smithsonian Marine Station in Fort Pierce for logistical and field support and Anne Chamberlain and R. Feller for countless hours of fieldwork. This research was funded by the NASA Climate and Biological Response program (NNX11AO94G) and the NSF MacroSystems Biology program (EF1065821). This is SMSFP Contribution No. 995. We also thank Florida DEP Park Service and St. Lucie County Mosquito Control and Coastal Management Services for permission to work in Avalon SP. NR 99 TC 2 Z9 2 U1 17 U2 51 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 NOV PY 2015 VL 96 IS 11 BP 2960 EP 2972 DI 10.1890/14-1853.1 PG 13 WC Ecology SC Environmental Sciences & Ecology GA CX2IY UT WOS:000365521600011 PM 27070015 ER PT J AU Lefcheck, JS Duffy, JE AF Lefcheck, Jonathan S. Duffy, J. Emmett TI Multitrophic functional diversity predicts ecosystem functioning in experimental assemblages of estuarine consumers SO ECOLOGY LA English DT Article DE biodiversity; Chesapeake Bay; consumers; ecosystem functioning; estuaries; functional diversity; grazers; predators ID MARINE FOOD-WEB; PREDATOR DIVERSITY; PHYLOGENETIC DIVERSITY; COMMUNITY COMPOSITION; SPECIES RICHNESS; TROPHIC LEVELS; BIODIVERSITY; PLANT; BIOMASS; CONSEQUENCES AB The use of functional traits to explain how biodiversity affects ecosystem functioning has attracted intense interest, yet few studies have a priori altered functional diversity, especially in multitrophic communities. Here, we manipulated multivariate functional diversity of estuarine grazers and predators within multiple levels of species richness to test how species richness and functional diversity predicted ecosystem functioning in a multitrophic food web. Community functional diversity was a better predictor than species richness for the majority of ecosystem properties, based on generalized linear mixed-effects models. Combining inferences from eight traits into a single multivariate index increased prediction accuracy of these models relative to any individual trait. Structural equation modeling revealed that functional diversity of both grazers and predators was important in driving final biomass within trophic levels, with stronger effects observed for predators. We also show that different species drove different ecosystem responses, with evidence for both sampling effects and complementarity. Our study extends experimental investigations of functional trait diversity to a multilevel food web, and demonstrates that functional diversity can be more accurate and effective than species richness in predicting community biomass in a food web context. C1 [Lefcheck, Jonathan S.; Duffy, J. Emmett] Coll William & Mary, Virginia Inst Marine Sci, Dept Biol Sci, Gloucester Point, VA 23062 USA. [Duffy, J. Emmett] Smithsonian Inst, Tennenbaum Marine Observ Network, Washington, DC 20013 USA. RP Lefcheck, JS (reprint author), Coll William & Mary, Virginia Inst Marine Sci, Dept Biol Sci, Gloucester Point, VA 23062 USA. EM jslefche@vims.edu OI Lefcheck, Jonathan/0000-0002-8787-1786 FU VIMS Council; Maury Fellowships; NSF [OCE-1031061] FX We thank K. M. Laumann, S. Donadi, J. P. Richardson, K. Jenkins, and Berlioz for support during the experiment. We additionally thank J. N. Griffin, G. E. Edgar, J. J. Orth, and two anonymous reviewers for comments on previous versions of the manuscript. J. S. Lefcheck was supported by VIMS Council and Maury Fellowships. J. E. Duffy and J. S. Lefcheck were supported by NSF OCE-1031061 to J. E. Duffy. This is Contribution No. 3465 of the Virginia Institute of Marine Science, College of William and Mary. NR 61 TC 5 Z9 5 U1 18 U2 59 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0012-9658 EI 1939-9170 J9 ECOLOGY JI Ecology PD NOV PY 2015 VL 96 IS 11 BP 2973 EP 2983 DI 10.1890/14-1977.1 PG 11 WC Ecology SC Environmental Sciences & Ecology GA CX2IY UT WOS:000365521600012 PM 27070016 ER PT J AU Torchin, ME Miura, O Hechinger, RF AF Torchin, Mark E. Miura, Osamu Hechinger, Ryan F. TI Parasite species richness and intensity of interspecific interactions increase with latitude in two wide-ranging hosts SO ECOLOGY LA English DT Article DE biotic interactions; dispersal; diversity patterns; intraguild predation; latitudinal gradients; parasites; rarefaction; species richness; trematodes ID LARVAL TREMATODE PARASITES; SNAIL INTERMEDIATE HOSTS; COMMUNITY STRUCTURE; DIVERSITY GRADIENT; PATTERNS; TROPICS; BODY; DETERMINANTS; BIODIVERSITY; ECOLOGY AB Although the latitudinal diversity gradient is a well-known and general pattern, the mechanisms structuring it remain elusive. Two key issues limit differentiating these. First, habitat type usually varies with latitude, precluding a standardized evaluation of species richness. Second, broad-scale and local factors hypothesized to shape diversity patterns co-vary with one another, making it difficult to tease apart independent effects. Examining communities of parasites in widely distributed hosts can eliminate some of these confounding factors. We quantified diversity and interspecific interactions for trematode parasites infecting two similar snail species across 27 degrees of latitude from 43 locations in tropical and temperate oceans. Counter to typical patterns, we found that species richness, levels of parasitism, and intensity of intraguild predation increased with latitude. Because speciation rates are precluded from driving diversity gradients in this particular system, the reversed gradients are likely due to local ecological factors, specifically, increased productivity and stability. We highlight how this system may serve as a useful tool to provide insight into what processes drive diversity gradients in general. C1 [Torchin, Mark E.] Smithsonian Trop Res Inst, Balboa 084303092, Ancon, Panama. [Miura, Osamu] Kochi Univ, Ctr Sci Res, Oceanog Sect, Nankoku, Kochi 7838502, Japan. [Hechinger, Ryan F.] Univ Calif San Diego, Scripps Inst Oceanog, Div Marine Biol Res, La Jolla, CA 92093 USA. RP Torchin, ME (reprint author), Smithsonian Trop Res Inst, Balboa 084303092, Ancon, Panama. EM torchinm@si.edu FU Smithsonian Institution; STRI; Smithsonian Marine Science Network; Japan Society for the Promotion of Science; NSF-NIH Ecology of Infectious Diseases [OCE-1115965] FX C. Schloder, Y. Kam, S. Jagadeeshan, E. Ochoa, A. Jaramillo, V. Frankel, J. Johnston, A. Cornejo, J. Lorda, R. Bastida- Zavala, R. Guerrero-Arenas, I. Jimenez-Garcia, A. Armitage, A. Schulze, D. Aguirre, E. Mendoza, J. Violante-Gonzalez, E. Siu-Estrada, and N. Aleman provided field and lab assistance. A. Freestone, A. Kuris, K. Lafferty, C. Schloder, and two anonymous reviewers provided useful comments on the manuscript. The crew of the R. V. Urraca and the staff of the STRI's Naos Island Laboratories, Bocas del Toro Marine Station, Galeta Marine Station, Smithsonian Marine Station at Fort Pierce, and Carrie Bow Cay Marine Laboratory provided logistical assistance. We thank the University of California Natural Reserve System for access to Carpinteria Salt Marsh. Support was provided by the Smithsonian Institution, STRI, and the Smithsonian Marine Science Network, the Japan Society for the Promotion of Science (Grant-in-Aid for JSPS Fellows to O. Miura), and an NSF-NIH Ecology of Infectious Diseases grant (OCE-1115965). NR 64 TC 3 Z9 3 U1 9 U2 38 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 NOV PY 2015 VL 96 IS 11 BP 3033 EP 3042 DI 10.1890/15-0518.1 PG 10 WC Ecology SC Environmental Sciences & Ecology GA CX2IY UT WOS:000365521600018 PM 27070022 ER PT J AU Mashian, N Sternberg, A Loeb, A AF Mashian, Natalie Sternberg, Amiel Loeb, Abraham TI Predicting the intensity mapping signal for multi-J CO lines SO JOURNAL OF COSMOLOGY AND ASTROPARTICLE PHYSICS LA English DT Article DE high redshift galaxies; power spectrum ID STAR-FORMING GALAXIES; FUNDAMENTAL METALLICITY RELATION; MOLECULAR GAS; HIGH-REDSHIFT; FORMATION LAW; NEARBY GALAXIES; SPIRAL GALAXIES; MASS; REIONIZATION; EMISSION AB We present a novel approach to estimating the intensity mapping signal of any CO rotational line emitted during the Epoch of Reionization (EoR). Our approach is based on large velocity gradient (LVG) modeling, a radiative transfer modeling technique that generates the full CO spectral line energy distribution (SLED) for a speci fi ed gas kinetic temperature, volume density, velocity gradient, molecular abundance, and column density. These parameters, which drive the physics of CO transitions and ultimately dictate the shape and amplitude of the CO SLED, can be linked to the global properties of the host galaxy, mainly the star formation rate (SFR) and the SFR surface density. By further employing an empirically derived SFR - M relation for high redshift galaxies, we can express the LVG parameters, and thus the speci fi c intensity of any CO rotational transition, as functions of the host halo mass M and redshift z. Integrating over the range of halo masses expected to host CO-luminous galaxies, we predict a mean CO(1-0) brightness temperature ranging from similar to 0.6 mu K at z = 6 to similar to 0.03 mu K at z = 10 with brightness temperature fluctuations of Delta(2)(CO) similar to 0.1 and 0.005 mu K respectively, at k = 0.1 Mpc(-1). In this model, the CO emission signal remains strong for higher rotational levels at z = 6, with < T-CO > similar to 0.3 and 0.05 mu K for the CO J = 6 -> 5 and CO J = 10 -> 9 transitions respectively. Including the e ff ects of CO photodissociation in these molecular clouds, especially at low metallicities, results in the overall reduction in the amplitude of the CO signal, with the low-and high-J lines weakening by 2-20% and 10-45%, respectively, over the redshift range 4 < z < 10. C1 [Mashian, Natalie; Loeb, Abraham] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Mashian, Natalie; Sternberg, Amiel] Tel Aviv Univ, Raymond & Beverly Sackler Sch Phys & Astron, IL-69978 Tel Aviv, Israel. RP Mashian, N (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM nmashian@physics.harvard.edu; amiel@wise.tau.ac.il; aloeb@cfa.harvard.edu FU Raymond and Beverly Sackler Tel Aviv University-Harvard/ITC Astronomy Program; Sackler Professorship; PBC Israel Science Foundation I-CORE Program [1829/12]; NSF [AST-1312034]; National Science Foundation Graduate Research Fellowship [DGE1144152] FX We thank Reinhard Genzel for helpful discussions and suggestions. This work was supported by the Raymond and Beverly Sackler Tel Aviv University-Harvard/ITC Astronomy Program. A.L. acknowledges support from the Sackler Professorship by Special Appointment at Tel Aviv University. This work was also supported in part by a PBC Israel Science Foundation I-CORE Program grant 1829/12, and in part by NSF grant AST-1312034. This material is based upon work supported by the National Science Foundation Graduate Research Fellowship under Grant No. DGE1144152. Any opinion, 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. NR 56 TC 5 Z9 5 U1 1 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 1475-7516 J9 J COSMOL ASTROPART P JI J. Cosmol. Astropart. Phys. PD NOV PY 2015 IS 11 AR 028 DI 10.1088/1475-7516/2015/11/028 PG 25 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA CX6OU UT WOS:000365821200029 ER PT J AU Santos, S Bond-Buckup, G Buckup, L Bartholomei-Santos, ML Perez-Losada, M Jara, CG Crandall, KA AF Santos, Sandro Bond-Buckup, Georgina Buckup, Ludwig Bartholomei-Santos, Marlise Ladvocat Perez-Losada, Marcos Jara, Carlos G. Crandall, Keith A. TI THREE NEW SPECIES OF AEGLIDAE (AEGLA LEACH, 1820) FROM PARANA STATE, BRAZIL SO JOURNAL OF CRUSTACEAN BIOLOGY LA English DT Article DE Anomura; diversity; Iguacu River basin; IUCN Red List; Ivai River basin; Upper Ribeira River basin ID FRESH-WATER CRABS; MOLECULAR SYSTEMATICS; ANOMURA; BOOTSTRAP; DECAPODA; MODELS AB This study describes three new aeglid species, Aegla meloi, Aegla loyolai and Aegla lancinhas, all of them recorded from Parana. State, Brazil. Along with the description, we also present an analysis of their phylogenetic relationships to other species of Aegla. The conservation status using the IUCN Red List criteria was assessed for each new species. The new species have restricted distributions and can be found in altitudes higher than 700 m. The new species are phylogenetically close to other species present in Parana State and Ribeira do Iguape River basin, yet clearly differ morphologically and genetically from other known species of Aegla. C1 [Santos, Sandro; Bartholomei-Santos, Marlise Ladvocat] Univ Fed Santa Maria, Dept Ecol & Evolucao, BR-97105900 Santa Maria, RS, Brazil. [Bond-Buckup, Georgina; Buckup, Ludwig] Univ Fed Rio Grande do Sul, Inst Biociencias, Dept Zool, BR-90501970 Porto Alegre, RS, Brazil. [Jara, Carlos G.] Univ Austral Chile, Inst Zool, Valdivia, Chile. [Perez-Losada, Marcos; Crandall, Keith A.] George Washington Univ, Computat Biol Inst, Ashburn, VA 20147 USA. [Perez-Losada, Marcos; Crandall, Keith A.] Smithsonian Inst, US Natl Museum Nat Hist, Dept Invertebrate Zool, Washington, DC 20013 USA. [Perez-Losada, Marcos] Ctr Invest Biodiversidade & Recursos Genet, CIBIO InBIO, P-4485661 Vairao, Portugal. RP Santos, S (reprint author), Univ Fed Santa Maria, Dept Ecol & Evolucao, BR-97105900 Santa Maria, RS, Brazil. EM sandro.santos30@gmail.com RI Perez-Losada, Marcos/I-4407-2013; OI Perez-Losada, Marcos/0000-0002-2585-4657; Crandall, Keith/0000-0002-0836-3389 FU CNPq [311142/2014-1] FX We are especially thankful to the graduating students Adriana Zimmer and Raoni Goncalves by their help in field work, and Alberto Senra Goncalves, by his help with map preparation; to Ana Rossi, for her dedication in preparing illustrations of the new species; to Dr. Paula Araujo, Curator of the Crustacean Collection of Departamento de Zoologia of Universidade Federal do Rio Grande do Sul, for permission to examine specimens; and to CNPq, for productivity grant (Processo 311142/2014-1) to Sandro Santos. NR 29 TC 3 Z9 4 U1 1 U2 6 PU CRUSTACEAN SOC PI SAN ANTONIO PA 840 EAST MULBERRY, SAN ANTONIO, TX 78212 USA SN 0278-0372 EI 1937-240X J9 J CRUSTACEAN BIOL JI J. Crustac. Biol. PD NOV PY 2015 VL 35 IS 6 BP 839 EP 849 DI 10.1163/1937240X-00002376 PG 11 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA CX2XQ UT WOS:000365560500014 ER PT J AU Linares-Palomino, R Aybar, D Ruiz, EJM AF Linares-Palomino, Reynaldo Aybar, David Ruiz, Erika J. Morales TI Floristics of neotropical seasonally dry forests: a perspective from complete vascular plant inventories SO PHYTOCOENOLOGIA LA English DT Article DE endemism; Leguminosae; life form spectra; Poaceae; terrestrial herbs; trees ID TROPICAL FORESTS; SPECIES RICHNESS; CONSERVATION PRIORITIES; SOUTH-AMERICA; BOLIVIA; VEGETATION; DIVERSITY; PATTERNS; REGION; ENDEMISM AB Seasonally dry tropical forests (SDTF) most often are characterised through woody plant inventories. This approach is taken because these forests are subjected to strong seasonal droughts, during which most herbaceous plants dry out and are not amenable to collection and taxonomic identification. Several studies show that the non-woody component of tropical forests contains a considerable proportion of the species richness and endemism values of these forests. We investigated whether floristic patterns shown by SDTF woody plant inventories are paralleled by complete inventories of vascular plants. We collated data from nine SDTF sites from across the Neotropics where complete vascular plant inventories were implemented, and obtained information from 2259 species. We found partial agreement between the woody plant and the complete vascular plant approaches recognising the major neotropical SDTF groups proposed previously using woody plants only. Leguminosae dominated both approaches and additional important families in our data included Asteraceae, Malvaceae and Poaceae, with an overwhelming presence of herbs. Endemism values were much lower than suggested by woody plant approaches. We suggest strengthening the research focus during the rainy season and on non-woody plants as this will add valuable knowledge that can help understand these seasonal ecosystems, calling further attention to their conservation needs. C1 [Linares-Palomino, Reynaldo] Univ Nacl Agr La Molina, Fac Ciencias Forestales, Herbario Forestal MOL, Lima 12, Lima, Peru. [Linares-Palomino, Reynaldo] Natl Zool Pk, Smithsonian Conservat Biol Inst, Ctr Conservat & Sustainabil, Washington, DC 20013 USA. [Aybar, David] Ctr Ornitol & Biodiversidad CORBIDI, Div Mastozool, Lima 33, Lima, Peru. [Ruiz, Erika J. Morales] Univ Nacl Agr La Molina, Fac Ciencias Forestales, Lima 12, Lima, Peru. RP Linares-Palomino, R (reprint author), Univ Nacl Agr La Molina, Fac Ciencias Forestales, Herbario Forestal MOL, Lima 12, Lima, Peru. EM r.linaresp@yahoo.co.uk; david.aybar@gmail.com; erika.mru@gmail.com OI Linares-Palomino, Reynaldo/0000-0002-7631-5549 NR 63 TC 0 Z9 0 U1 3 U2 10 PU GEBRUDER BORNTRAEGER PI STUTTGART PA JOHANNESSTR 3A, D-70176 STUTTGART, GERMANY SN 0340-269X J9 PHYTOCOENOLOGIA JI Phytocoenologia PD NOV PY 2015 VL 45 IS 3 BP 251 EP 267 DI 10.1127/phyto/2015/0010 PG 17 WC Plant Sciences; Ecology SC Plant Sciences; Environmental Sciences & Ecology GA CX6SY UT WOS:000365833200002 ER PT J AU Lin, J Murphy, NA Shen, CC Raymond, JC Reeves, KK Zhong, JY Wu, N Li, Y AF Lin, Jun Murphy, Nicholas A. Shen, Chengcai Raymond, John C. Reeves, Katharine K. Zhong, Jiayong Wu, Ning Li, Yan TI Review on Current Sheets in CME Development: Theories and Observations SO SPACE SCIENCE REVIEWS LA English DT Review DE Sun: flares; Sun: coronal mass ejections (CMEs); Plasmas; Magnetic reconnection; Instabilities ID CORONAL MASS EJECTION; SUPRA-ARCADE DOWNFLOWS; RECONNECTING CURRENT SHEETS; CURRENT-LAYER FRAGMENTATION; FAST MAGNETIC RECONNECTION; FIELD LINE SHRINKAGE; FLUX-ROPE MODELS; HOT FLARE PLASMA; X-RAY TELESCOPE; 2010 NOVEMBER 3 AB We introduce how the catastrophe model for solar eruptions predicted the formation and development of the long current sheet (CS) and how the observations were used to recognize the CS at the place where the CS is presumably located. Then, we discuss the direct measurement of the CS region thickness by studying the brightness distribution of the CS region at different wavelengths. The thickness ranges from to about at heights between 0.27 and from the solar surface. But the traditional theory indicates that the CS is as thin as the proton Larmor radius, which is of order tens of meters in the corona. We look into the huge difference in the thickness between observations and theoretical expectations. The possible impacts that affect measurements and results are studied, and physical causes leading to a thick CS region in which reconnection can still occur at a reasonably fast rate are analyzed. Studies in both theories and observations suggest that the difference between the true value and the apparent value of the CS thickness is not significant as long as the CS could be recognised in observations. We review observations that show complex structures and flows inside the CS region and present recent numerical modelling results on some aspects of these structures. Both observations and numerical experiments indicate that the downward reconnection outflows are usually slower than the upward ones in the same eruptive event. Numerical simulations show that the complex structure inside CS and its temporal behavior as a result of turbulence and the Petschek-type slow-mode shock could probably account for the thick CS and fast reconnection. But whether the CS itself is that thick still remains unknown since, for the time being, we cannot measure the electric current directly in that region. We also review the most recent laboratory experiments of reconnection driven by energetic laser beams, and discuss some important topics for future works. C1 [Lin, Jun; Li, Yan] Chinese Acad Sci, Yunnan Observ, Kunming 650216, Yunnan, Peoples R China. [Murphy, Nicholas A.; Shen, Chengcai; Raymond, John C.; Reeves, Katharine K.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Zhong, Jiayong] Chinese Acad Sci, Key Lab Opt Astron, Natl Astron Observ China, Beijing 100012, Peoples R China. [Wu, Ning] Yunnan Normal Univ, Sch Tourism & Geog, Kunming 650092, Yunnan, Peoples R China. RP Lin, J (reprint author), Chinese Acad Sci, Yunnan Observ, POB 110, Kunming 650216, Yunnan, Peoples R China. EM jlin@ynao.ac.cn RI LIN, JUN/B-9890-2017; OI Murphy, Nicholas/0000-0001-6628-8033 FU Program 973 [2013CBA01503]; NSFC [11203069, 11273055, 11333007, 11403100]; CAS [XDB09040202]; Yunnan Province [2011FB113]; NSF SHINE [AGS-1156076, AGS-1358342] FX JL thanks the organizer of the Hinode-7 Science Meeting for invitation to give an overview on the related topic, and the main content of this paper was reported at the meeting. This work was supported by Program 973 grant 2013CBA01503, NSFC grants 11203069, 11273055, 11333007, and 11403100, CAS grant XDB09040202, Yunnan Province grant 2011FB113, as well as NSF SHINE grants AGS-1156076 and AGS-1358342. NR 262 TC 10 Z9 13 U1 6 U2 12 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0038-6308 EI 1572-9672 J9 SPACE SCI REV JI Space Sci. Rev. PD NOV PY 2015 VL 194 IS 1-4 BP 237 EP 302 DI 10.1007/s11214-015-0209-0 PG 66 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CX2FM UT WOS:000365511500004 ER PT J AU Lima, L Espinosa-Alvarez, O Ortiz, PA Trejo-Varon, JA Carranza, JC Pinto, CM Serrano, MG Buck, GA Camargo, EP Teixeira, MMG AF Lima, Luciana Espinosa-Alvarez, Oneida Ortiz, Paola A. Trejo-Varon, Javier A. Carranza, Julio C. Miguel Pinto, C. Serrano, Myrna G. Buck, Gregory A. Camargo, Erney P. Teixeira, Marta M. G. TI Genetic diversity of Trypanosoma cruzi in bats, and multilocus phylogenetic and phylogeographical analyses supporting Tcbat as an independent DTU (discrete typing unit) SO ACTA TROPICA LA English DT Article DE Trypanosoma cruzi; Chiroptera; Multilocus analysis; Phylogeny; Genotyping; Evolution ID CHAGAS-DISEASE; POPULATION-STRUCTURE; SEEDING HYPOTHESIS; NEOTROPICAL BATS; RIBOSOMAL-RNA; I GENOTYPES; SSU RDNA; EVOLUTIONARY; LINEAGES; SEQUENCE AB Trypanosoma cruzi is a complex of phenotypically and genetically diverse isolates distributed in six discrete typing units (DTUs) designated as TcI-TcVI. Five years ago, T. cruzi isolates from Brazilian bats showing unique patterns of traditional ribosomal and spliced leader PCRs not clustering into any of the six DTUs were designated as the Tcbat genotype. In the present study, phylogenies inferred using SSU rRNA (small subunit of ribosomal rRNA), gGAPDH (glycosomal glyceraldehyde 3-phosphate dehydrogenase) and Cytb (cytochrome b) genes strongly supported Tcbat as a monophyletic lineage prevalent in Brazil, Panama and Colombia. Providing strong support for Tcbat, sequences from 37 of 47 nuclear and 12 mitochondria! genes (retrieved from a draft genome of Tcbat) and reference strains of all DTUs available in databanks corroborated Tcbat as an independent DTU. Consistent with previous studies, multilocus analysis of most nuclear genes corroborated the evolution of T. cruzi from bat trypanosomes its divergence into two main phylogenetic lineages: the basal TcII; and the lineage clustering TcIV, the clade comprising TcIII and the sister groups TcI-Tcbat. Most likely, the common ancestor of Tcbat and TcI was a bat trypanosome. However, the results of the present analysis did not support Tcbat as the ancestor of all DTUs. Despite the insights provided by reports of TcIII, TcIV and TcII in bats, including Amazonian bats harbouring TcII, further studies are necessary to understand the roles played by bats in the diversification of all DTUs. We also demonstrated that in addition to value as molecular markers for DTU assignment, Cytb, ITS rDNA and the spliced leader (SL) polymorphic sequences suggest spatially structured populations of Tcbat. Phylogenetic and phylogeographical analyses, multiple molecular markers specific to Tcbat, and the degrees of sequence divergence between Tcbat and the accepted DTUs strongly support the definitive classification of Tcbat as a new DTU. (C) 2015 Elsevier B.V. All rights reserved. C1 [Lima, Luciana; Espinosa-Alvarez, Oneida; Ortiz, Paola A.; Camargo, Erney P.; Teixeira, Marta M. G.] Univ Sao Paulo, Inst Ciencias Biomed, Dept Parasitol, BR-05508900 Sao Paulo, SP, Brazil. [Trejo-Varon, Javier A.; Carranza, Julio C.] Univ Tolima, Fac Ciencias, Lab Invest Parasitol Trop, Ibague, Colombia. [Miguel Pinto, C.] Smithsonian Inst, Natl Museum Nat Hist, Div Mammals, Washington, DC 20560 USA. [Miguel Pinto, C.] Pontificia Univ Catalica Ecuador, Ctr Invest Enfermedades Infecciosas & Cronicas, Escuela Biol, Quito, Ecuador. [Serrano, Myrna G.; Buck, Gregory A.] Virginia Commonwealth Univ, Dept Microbiol & Immunol, Richmond, VA 23298 USA. RP Teixeira, MMG (reprint author), Univ Sao Paulo, Inst Ciencias Biomed, Dept Parasitol, BR-05508900 Sao Paulo, SP, Brazil. EM lulima@usp.br; oneidae07@usp.br; paolaortiz27@gmail.com; jatrejovaron@gmail.com; jcarranza@ut.edu.co; mpinto@amnh.org; gabuck@vcu.edu; erney@usp.br; mmgteix@icb.usp.br OI Camargo, Erney/0000-0003-0011-5871 FU Brazilian agency CNPq (CNPq-MCTI PROSUL); CAPES; FAPESP; Program ATOL (Assembling the tree of Life-Phylum Euglenozoa, National Science Foundation, USA) [DEB-0830056]; Kinetoplastid Genome Sequencing and Analysis Consortium NIH/NHGRI/NIAID [ID 59941]; Investissements d'Avenir; CAPES (PNPD); CNPq (PROTAX) FX This study was supported by the Brazilian agency CNPq (CNPq-MCTI PROSUL), CAPES and FAPESP. The draft genome of Tcbat was sponsored by the Program ATOL (Assembling the tree of Life-Phylum Euglenozoa, National Science Foundation, USA, DEB-0830056) and obtained with the collaboration of M.G. Serrano, F.M. Da Silva and J.M.P. Alves. We are grateful to The TriTrypDB and the Kinetoplastid Genome Sequencing and Analysis Consortium NIH/NHGRI/NIAID (project ID 59941) for making genomes of trypanosomes freely available. We would like to thank several students and collaborators for their inestimable help in the fieldworks and Prof Gustavo A. Vallejo for his support, hospitability and friendship during the work in Colombia. We thanks Ana C. Pavan (IB-USP) for some bat blood samples. The Suriname samples could be analyzed for the generosity of Burton K. Lim (Royal Ontario Museum) and grant support from an 'Investissements d'Avenir' managed by Agence Nationale de la Recherche (CEBA, ANR-10-LABX-25-01) to CMP. Luciana Lima and Paola A. Ortiz are postdoctoral fellows sponsored by FAPESP and CAPES (PNPD), respectively, and Oneida Espinosa-Alvarez is recipient of a PhD fellowship from CNPq (PROTAX). NR 58 TC 13 Z9 13 U1 2 U2 8 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0001-706X EI 1873-6254 J9 ACTA TROP JI Acta Trop. PD NOV PY 2015 VL 151 SI SI BP 166 EP 177 DI 10.1016/j.actatropica.2015.07.015 PG 12 WC Parasitology; Tropical Medicine SC Parasitology; Tropical Medicine GA CW2CE UT WOS:000364797900017 PM 26200788 ER PT J AU Grusz, AL Pryer, KM AF Grusz, Amanda L. Pryer, Kathleen M. TI DEVELOPMENT OF MICROSATELLITE MARKERS FOR THE APOMICTIC TRIPLOID FERN MYRIOPTERIS LINDHEIMERI (PTERIDACEAE) SO APPLICATIONS IN PLANT SCIENCES LA English DT Article DE asexual; cheilanthoid; Myriopteris lindheimeri; polyploidy; pteridophyte; simple sequence repeats (SSRs) ID CHEILANTHOID FERNS AB Premise of the study: Microsatellite markers were developed for investigating the population dynamics of Myriopteris lindheimeri (Pteridaceae), an apomictic triploid fern endemic to deserts of the southwestern United States and Mexico. Methods and Results: Using 454 sequencing, 21 microsatellite markers were developed. Of these, 14 were polymorphic with up to five alleles per locus and eight markers amplified in one or more congeneric close relatives (M. covillei, M. fendleri, M. aurea, and M. rufa). To demonstrate marker utility, M. lindheimeri samples from three Arizona populations were genotyped at nine loci. For each population, diversity measures including percent polymorphic loci, frequency of heterozygotes across all loci, and genotypic diversity were calculated. Across the three populations, on average, 63% of loci were polymorphic, the average frequency of heterozygotes (across all loci) was 0.32, and average genotypic diversity was 0.34. Conclusions: These markers provide a foundation for future studies exploring polyploidy and apomixis in myriopterid ferns. C1 [Grusz, Amanda L.] Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, Washington, DC 20013 USA. [Pryer, Kathleen M.] Duke Univ, Dept Biol, Durham, NC 27708 USA. RP Grusz, AL (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, Washington, DC 20013 USA. EM grusza@si.edu FU American Society of Plant Taxonomists Shirley and Alan Graham Graduate Student Research Award, a Duke University Department of Biology; National Science Foundation Doctoral Dissertation Improvement Grant [DEB-1110767] FX The authors thank M. H. Noor and M. D. Windham for initial encouragement of this project, and W. Booth and M. Rusham for contributing expertise. Funding was provided by the American Society of Plant Taxonomists Shirley and Alan Graham Graduate Student Research Award, a Duke University Department of Biology Grant-in-Aid, and a Sigma Xi Grant-in-Aid of Research awarded to A.L.G., as well as a National Science Foundation Doctoral Dissertation Improvement Grant awarded to K.M.P. and A.L.G. (DEB-1110767). NR 12 TC 1 Z9 1 U1 1 U2 4 PU BOTANICAL SOC AMER INC PI ST LOUIS PA PO BOX 299, ST LOUIS, MO 63166-0299 USA SN 2168-0450 J9 APPL PLANT SCI JI Appl. Plant Sci. PD NOV PY 2015 VL 3 IS 11 AR 1500061 DI 10.3732/apps.1500061 PG 5 WC Plant Sciences SC Plant Sciences GA CW9PP UT WOS:000365331000003 ER PT J AU Thitaram, C Dejchaisri, S Somgird, C Angkawanish, T Brown, J Phumphuay, R Chomdech, S Kangwanpong, D AF Thitaram, Chatchote Dejchaisri, Suthatip Somgird, Chaleamchat Angkawanish, Taweepoke Brown, Janine Phumphuay, Ratchadakorn Chomdech, Siriwadee Kangwanpong, Daoroong TI Social group formation and genetic relatedness in reintroduced Asian elephants (Elephas maximus) in Thailand SO APPLIED ANIMAL BEHAVIOUR SCIENCE LA English DT Article DE Asian elephant; Reintroduction; Microsatellite; Mitochondrial DNA; Group forming behavior ID LEMUR MICROCEBUS-MURINUS; AFRICAN ELEPHANT; MICROSATELLITE LOCI; MITOCHONDRIAL-DNA; NATIONAL-PARK; POPULATION-STRUCTURE; LOXODONTA-AFRICANA; COMPUTER-PROGRAM; SOUTHERN INDIA; DIVERSITY AB Captive-held elephants were recruited from several parts of Thailand and released as part of a reintroduction project. Wild elephants with a herd matriarch generally contain the same matrilineal line and are genetically related. However, reintroduced elephants are less likely to be related, but are known to establish social groups. The objective of this study was to investigate the genetic relatedness and behavioral relationships of elephants reintroduced into forested areas in central and northern Thailand. Blood samples were collected from 53 elephants before release into the Sublanka (SLK) and Doi Phamuang (DPM) Wildlife Sanctuaries, and DNA was extracted for microsatellite and mitochondrial analysis. Direct observations of social bonding behaviors were done weekly for 12 months after release, and an association index (AI) calculated for each individual. The results showed a low relatedness for both populations; the observed heterozygosity and number of mitochondrial haplotypes were 0.739 and 13 at SLK (n=26), and 0.808 and 11 at DPM (n = 27), respectively. Across both locations, 33 elephants formed into 11 groups (range 2-6 individuals/group). The average Al and pairwise genetic relatedness of elephant groups were 0.517 +/- 0.039 and 0.078 +/- 0.019, respectively, and were not correlated (r=-0.036; p = 0.78). Twenty elephants were not associated with specific groups and had average Al and pairwise genetic relatedness of 0.002 +/- 0.001 and 0.047 +/- 0.013, respectively, which were not correlated (r=-0.074; p = 0.491). Several mitochondrial haplotypes were found within the same group. Thus, social bonding of the reintroduced elephants was not influenced by genetic relatedness. Rather, groups formed in association with the presence of an elephant calf. Additionally, many elephants occasionally preferred isolation. Thus, reintroduction procedures should favor introducing elephant calves, or adults with calves to increase the chance of group formation and establishment of stable elephant herds. (C) 2015 Elsevier B.V. All rights reserved. C1 [Thitaram, Chatchote; Somgird, Chaleamchat; Phumphuay, Ratchadakorn] Chiang Mai Univ, Ctr Excellence Elephant Res & Educ, Chiang Mai 50200, Thailand. [Thitaram, Chatchote; Somgird, Chaleamchat] Chiang Mai Univ, Dept Compan Anim & Wildlife Clin, Fac Vet Med, Chiang Mai 50100, Thailand. [Thitaram, Chatchote; Somgird, Chaleamchat; Angkawanish, Taweepoke] Elephant Reintroduct Fdn, Bangkok 10100, Thailand. [Dejchaisri, Suthatip] Kasetsart Univ, Ctr Agr Biotechnol, Nakhon Pathom 73140, Thailand. [Angkawanish, Taweepoke] Forest Ind Org, Natl Elephant Inst, Lampang 52190, Thailand. [Brown, Janine] Smithsonian Conservat Biol Inst, Ctr Species Survival, Front Royal, VA 22630 USA. [Phumphuay, Ratchadakorn; Chomdech, Siriwadee; Kangwanpong, Daoroong] Chiang Mai Univ, Dept Biol, Fac Sci, Chiang Mai 50200, Thailand. RP Thitaram, C (reprint author), Chiang Mai Univ, Dept Compan Anim & Wildlife Clin, Fac Vet Med, Chiang Mai 50100, Thailand. EM cthitaram@gmail.com OI Thitaram, Chatchote/0000-0001-9319-5596 FU Thailand Research Fund [MRG5480260]; Elephant Reintroduction Foundation, Thailand FX The authors thank the Thailand Research Fund for the grant no. MRG5480260, and the Elephant Reintroduction Foundation, Thailand for funding this project. We also thank staff of the elephant reintroduction foundation, and Sublanka and Doi Phamuang wildlife sanctuaries for sample and behavior data collection. NR 52 TC 1 Z9 1 U1 18 U2 49 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0168-1591 EI 1872-9045 J9 APPL ANIM BEHAV SCI JI Appl. Anim. Behav. Sci. PD NOV PY 2015 VL 172 BP 52 EP 57 DI 10.1016/j.applanim.2015.09.002 PG 6 WC Agriculture, Dairy & Animal Science; Behavioral Sciences; Veterinary Sciences SC Agriculture; Behavioral Sciences; Veterinary Sciences GA CX0EY UT WOS:000365370900007 ER PT J AU Hansen, TT Andersen, J Nordstrom, B Beers, TC Yoon, J Buchhave, LA AF Hansen, T. T. Andersen, J. Nordstrom, B. Beers, T. C. Yoon, J. Buchhave, L. A. TI The role of binaries in the enrichment of the early Galactic halo I. r-process-enhanced metal-poor stars SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE stars: abundances; stars: chemically peculiar; binaries: spectroscopic; Galaxy: halo; ISM: structure ID HORIZONTAL-BRANCH STARS; RED GIANTS; SURVEY HERES; SPECTROSCOPIC BINARIES; CHEMICAL ABUNDANCES; CS 31082-001; EARLY GALAXY; 1ST STARS; KINEMATICS; DISCOVERY AB Context. The detailed chemical composition of most metal-poor halo stars has been found to be highly uniform, but a minority of stars exhibit dramatic enhancements in their abundances of heavy neutron-capture elements and/or of carbon. The key question for Galactic chemical evolution models is whether these peculiarities reflect the composition of the natal clouds, or if they are due to later (post-birth) mass transfer of chemically processed material from a binary companion. If the former case applies, the observed excess of certain elements was implanted within selected clouds in the early ISM from a production site at interstellar distances. Aims. Our aim is to determine the frequency and orbital properties of binaries among these chemically peculiar stars. This information provides the basis for deciding whether local mass transfer from a binary companion is necessary and sufficient to explain their unusual compositions. This paper discusses our study of a sample of 17 moderately (r-I) and highly (r-II) r-process-element enhanced VMP and EMP stars. Methods. High-resolution, low signal-to-noise spectra of the stars were obtained at roughly monthly intervals over eight years with the FIES spectrograph at the Nordic Optical Telescope. From these spectra, radial velocities with an accuracy of similar to 100 m s(-1) were determined by cross-correlation against an optimized template. Results. Fourteen of the programme stars exhibit no significant radial-velocity variation over this temporal window, while three are binaries with orbits of typical eccentricity for their periods, resulting in a normal binary frequency of similar to 18 +/- 6% for the sample. Conclusions. Our results confirm our preliminary conclusion from 2011, based on partial data, that the chemical peculiarity of the r-I and r-II stars is not caused by any putative binary companions. Instead, it was imprinted on the natal molecular clouds of these stars by an external, distant source. Models of the ISM in early galaxies should account for such mechanisms. C1 [Hansen, T. T.] Heidelberg Univ, ZAH, Landessternwarte, D-69117 Heidelberg, Germany. [Andersen, J.; Nordstrom, B.] Univ Copenhagen, Niels Bohr Inst, Dark Cosmol Ctr, DK-2100 Copenhagen, Denmark. [Andersen, J.; Nordstrom, B.] Aarhus Univ, Dept Phys & Astron, Stellar Astrophys Ctr, DK-8000 Aarhus C, Denmark. [Beers, T. C.; Yoon, J.] Univ Notre Dame, Dept Phys, Notre Dame, IN 46556 USA. [Beers, T. C.; Yoon, J.] Univ Notre Dame, JINA Ctr Evolut Elements, Notre Dame, IN 46556 USA. [Buchhave, L. A.] 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. RP Hansen, TT (reprint author), Heidelberg Univ, ZAH, Landessternwarte, Konigstuhl 12, D-69117 Heidelberg, Germany. EM thansen@lsw.uni-heidelberg.de OI Hansen, Terese/0000-0001-6154-8983; Buchhave, Lars A./0000-0003-1605-5666 FU German Research Foundation (DFG) [Sonderfurschungsbereich SFB 881]; Physics Frontier Center/Joint Institute or Nuclear Astrophysics (JINA) [PHY 08-22648]; Physics Frontier Center/JINA Center for the Evolution of the Elements (JINA-CEE) [PHY 14-30152]; Danish Natural Science Research Council; Carlsberg Foundation; National Science Foundation [NSF PHY11-25915]; US National Science Foundation FX This paper is based on observations made with the Nordic Optical Telescope, operated by the Nordic Optical Telescope Scientific Association at the Observatorio del Roque de los Muchachos, La Palma, Spain, of the Instituto de Astrofisica de Canarias. We thank several NOT staff members and students for obtaining most of the observations for us in service mode. The work of T.H. was supported by Sonderfurschungsbereich SFB 881 "The Milky Way System" (subproject A4) of the German Research Foundation (DFG). T.C.B. and J.Y. acknowledge partial support for this work from grants PHY 08-22648; Physics Frontier Center/Joint Institute or Nuclear Astrophysics (JINA), and PHY 14-30152; Physics Frontier Center/JINA Center for the Evolution of the Elements (JINA-CEE), awarded by the US National Science Foundation. J.A. and B.N. gratefully acknowledge financial support from the Danish Natural Science Research Council and the Carlsberg Foundation. B.N. gratefully acknowledges partial support from the National Science Foundation under Grant No. NSF PHY11-25915. Furthermore, we thank the referee for helpful comments. NR 56 TC 6 Z9 6 U1 0 U2 0 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD NOV PY 2015 VL 583 AR A49 DI 10.1051/0004-6361/201526812 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CW5YC UT WOS:000365072200124 ER PT J AU Shulevski, A Morganti, R Barthel, PD Harwood, JJ Brunetti, G van Weeren, RJ Rottgering, HJA White, GJ Horellou, C Kunert-Bajraszewska, M Jamrozy, M Chyzy, KT Mahony, E Miley, G Brienza, M Birzan, L Rafferty, DA Bruggen, M Wise, MW Conway, J de Gasperin, F Vilchez, N AF Shulevski, A. Morganti, R. Barthel, P. D. Harwood, J. J. Brunetti, G. van Weeren, R. J. Rottgering, H. J. A. White, G. J. Horellou, C. Kunert-Bajraszewska, M. Jamrozy, M. Chyzy, K. T. Mahony, E. Miley, G. Brienza, M. Birzan, L. Rafferty, D. A. Brueggen, M. Wise, M. W. Conway, J. de Gasperin, F. Vilchez, N. TI AGN duty cycle estimates for the ultra-steep spectrum radio relic VLSS J1431.8+1331 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE galaxies: active; radio continuum: galaxies; galaxies: individual: VLSS J1431.8+1331 ID ACTIVE GALACTIC NUCLEI; SKY SURVEY; MAGNETIC-FIELD; A-PROJECTION; BLACK-HOLES; WIDE-FIELD; GALAXIES; CLUSTERS; LOFAR; FEEDBACK AB Context. Steep spectrum radio sources associated with active galactic nuclei (AGN) may contain remnants of past AGN activity episodes. Studying these sources gives us insight into the AGN activity history. Novel instruments like the LOw Frequency ARray (LOFAR) are enabling studies of these fascinating structures to be made at tens to hundreds of MHz with sufficient resolution to analyse their complex morphology. Aims. Our goal is to characterize the integrated and resolved spectral properties of VESS J1431+1331 and estimate source ages based on synchrotron radio emission models, thus putting constraints on the AGN duty cycle. Methods. Using a broad spectral coverage, we have derived spectral and curvature maps, and used synchrotron ageing models to determine the time elapsed from the last time the source plasma was energized. We used LOFAR, Giant Metrewave Radio Telescope (GMRT) and Jansky Very Large Array (VLA) data. Results. We confirm the morphology and the spectral index values found in previous studies of this object. Based on our ageing analysis, we infer that the AGN that created this source currently has very low levels of activity or that it is switched off. The derived ages for the larger source component range from around 60 to 130 Myr, hinting that the AGN activity decreased or stopped around 60 Myr ago. We observe that the area around the faint radio core located in the larger source component is the youngest, while the overall age of the smaller source component shows it to be the oldest part of the source. Conclusions. Our analysis suggests that VLSS J1431.8+1331 is an intriguing, two-component source. The larger component seems to host a faint radio core, suggesting that the source may be an AGN radio relic. The spectral index we observe from the smaller component is distinctly flatter at lower frequencies than the spectral index of the larger component, suggesting the possibility that the smaller component may be a shocked plasma bubble. From. the integrated source spectrum, we deduce that its shape and slope can be used as tracers of the activity history of this type of steep spectrum radio source. We discuss the implications this conclusion has for future studies of radio sources having similar characteristics. C1 [Shulevski, A.; Morganti, R.; Barthel, P. D.; Brienza, M.] Univ Groningen, Kapteyn Astron Inst, NL-9747 AD Groningen, Netherlands. [Shulevski, A.; Morganti, R.; Harwood, J. J.; Mahony, E.; Brienza, M.; Wise, M. W.; Vilchez, N.] Netherlands Inst Radio Astron, ASTRON, NL-7990 AA Dwingeloo, Netherlands. [Brunetti, G.] IRA INAF, I-40129 Bologna, Italy. [van Weeren, R. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Rottgering, H. J. A.; Miley, G.] Leiden Univ, Leiden Observ, NL-2333 CA Leiden, Netherlands. [Birzan, L.; Rafferty, D. A.; Brueggen, M.; de Gasperin, F.] Univ Hamburg, Hamburger Sternwarte, D-21029 Hamburg, Germany. [Wise, M. W.] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1090 GE Amsterdam, Netherlands. [Horellou, C.; Conway, J.] Chalmers, Onsala Space Observ, Dept Earth & Space Sci, S-43992 Onsala, Sweden. [White, G. J.] Open Univ, Dept Phys & Astron, Milton Keynes MK7 6AA, Bucks, England. [White, G. J.] Rutherford Appleton Lab, RAL Space, Didcot OX11 0QX, Oxon, England. [Kunert-Bajraszewska, M.] Nicholas Copernicus Univ, Torun Ctr Astron, Fac Phys Astron & Informat, PL-87100 Torun, Poland. [Jamrozy, M.; Chyzy, K. T.] Uniwersytet Jagiellonski, Obserwatorium Astron, PL-30244 Krakow, Poland. RP Shulevski, A (reprint author), Univ Groningen, Kapteyn Astron Inst, Landleven 12, NL-9747 AD Groningen, Netherlands. EM shulevski@astron.nl; morganti@astron.nl; pdb@astro.rug.nl RI Kunert-Bajraszewska, Magdalena/F-9060-2014; Harwood, Jeremy/D-9032-2016; OI Harwood, Jeremy/0000-0003-0251-6126; Mahony, Elizabeth/0000-0002-5053-2828; de Gasperin, Francesco/0000-0003-4439-2627; van Weeren, Reinout/0000-0002-0587-1660; Shulevski, Aleksandar/0000-0002-1827-0469 FU European Research Council under the European Union's Seventh Framework Programme [RADIOLIFE-320745]; NASA through the Einstein Postdoctoral grant - Chandra X-ray Center [PF2-130104]; NASA [NAS8-03060] FX LOFAR, the Low Frequency Array designed and constructed by ASTRON, has facilities in several countries, which are owned by various parties (each with their own funding sources), and which are collectively operated by the International LOFAR Telescope (ILT) foundation under a joint scientific policy. R.M. gratefully acknowledges support from the European Research Council under the European Union's Seventh Framework Programme (FP/2007-2013)/ERC Advanced Grant RADIOLIFE-320745. This research made use of the NASA/IPAC Extragalactic Database (NEM, which is operated by the jet Propulsion Laboratory; California Institute of Technology, under contract with the National Aeronautics and Space Administration. This research made use of APLpy, an open-source plotting package for Python hosted at http ://aplpy.github corn R.J.v.W. acknowledges the support 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. We thank the anonymous referee for the constructive comments that have improved the manuscript. NR 50 TC 2 Z9 2 U1 0 U2 0 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD NOV PY 2015 VL 583 AR A89 DI 10.1051/0004-6361/201525632 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CW5YC UT WOS:000365072200020 ER PT J AU Borthakur, S Heckman, T Tumlinson, J Bordoloi, R Thom, C Catinella, B Schiminovich, D Dave, R Kauffmann, G Moran, SM Saintonge, A AF Borthakur, Sanchayeeta Heckman, Timothy Tumlinson, Jason Bordoloi, Rongmon Thom, Christopher Catinella, Barbara Schiminovich, David Dave, Romeel Kauffmann, Guinevere Moran, Sean M. Saintonge, Amelie TI CONNECTION BETWEEN THE CIRCUMGALACTIC MEDIUM AND THE INTERSTELLAR MEDIUM OF GALAXIES: RESULTS FROM THE COS-GASS SURVEY SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: halos; galaxies: ISM; quasars: absorption lines ID ARECIBO SDSS SURVEY; ALPHA ABSORPTION SYSTEMS; FRACTION SCALING RELATIONS; LY-ALPHA; MASSIVE GALAXIES; GASEOUS EXTENT; ABSORBING GALAXIES; NEARBY GALAXIES; STELLAR CONTENT; DATA RELEASE AB We present a study exploring the nature and properties of the circumgalactic medium (CGM) and its connection to the atomic gas content in the interstellar medium (ISM) of galaxies as traced by the H I 21 cm line. Our sample includes 45 low-z (0.026-0.049) galaxies from the GALEX Arecibo SDSS Survey (Galaxy Evolution Explorer/Arecibo/Sloan Digital Sky Survey). Their CGM was probed via absorption in the spectra of background quasi-stellar objects at impact parameters of 63-231 kpc. The spectra were obtained with the Cosmic Origins Spectrograph aboard the Hubble Space Telescope. We detected neutral hydrogen (Ly alpha absorption lines) in the CGM of 92% of the galaxies. We find that the radial profile of the CGM as traced by the Ly alpha equivalent width can be fit as an exponential with a scale length of roughly the virial radius of the dark matter halo. We found no correlation between the orientation of the sightline relative to the galaxy's major axis and the Ly alpha equivalent width. The velocity spread of the circumgalactic gas is consistent with that seen in the atomic gas in the ISM. We find a strong correlation (99.8% confidence) between the gas fraction (M(H I)/M-star) and the impact-parameter-corrected Ly alpha equivalent width. This is stronger than the analogous correlation between corrected Ly alpha equivalent width and specific star formation rate (SFR)/M-star (97.5% confidence). These results imply a physical connection between the H I disk and the CGM, which is on scales an order of magnitude larger. This is consistent with the picture in which the H I disk is nourished by accretion of gas from the CGM. C1 [Borthakur, Sanchayeeta; Heckman, Timothy] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Borthakur, Sanchayeeta] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Tumlinson, Jason; Bordoloi, Rongmon; Thom, Christopher] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Catinella, Barbara] Swinburne Univ Technol, Ctr Astrophys & Supercomp, Hawthorn, Vic 3122, Australia. [Schiminovich, David] Columbia Univ, Dept Astron, New York, NY 10027 USA. [Dave, Romeel] Univ Western Cape, ZA-7535 Cape Town, South Africa. [Dave, Romeel] S African Astron Observ, ZA-7925 Cape Town, South Africa. [Dave, Romeel] African Inst Math Sci, ZA-7945 Cape Town, South Africa. [Kauffmann, Guinevere] Max Planck Inst Astrophys, D-85741 Garching, Germany. [Moran, Sean M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Saintonge, Amelie] UCL, Dept Phys & Astron, London WC1E 6BT, England. RP Borthakur, S (reprint author), Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. EM sanch@pha.jhu.edu OI Catinella, Barbara/0000-0002-7625-562X FU NASA [NAS5-26555]; Australian Research Council [FT120100660]; Alfred P. Sloan Foundation; National Science Foundation; U.S. Department of Energy Office of Science; 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; [HST GO 12603] FX We thank the HST and GBT staff for support during the observations. We also thank Cameron Hummels, Jessica Werk, Xavier Prochaska, and Hsiao-Wen Chen for useful discussions. This work is based on observations with the NASA/ESA Hubble Space Telescope, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555. S.B. and T.H. were supported by grant HST GO 12603. B.C. is the recipient of an Australian Research Council Future Fellowship (FT120100660).; This project also made use of SDSS data. 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. NR 46 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 NOV 1 PY 2015 VL 813 IS 1 AR 46 DI 10.1088/0004-637X/813/1/46 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CW8XZ UT WOS:000365284100046 ER PT J AU Casadio, C Gomez, JL Jorstad, SG Marscher, AP Larionov, VM Smith, PS Gurwell, MA Lahteenmaki, A Agudo, I Molina, SN Bala, V Joshi, M Taylor, B Williamson, KE Arkharov, AA Blinov, DA Borman, GA Di Paola, A Grishina, TS Hagen-Thorn, VA Itoh, R Kopatskaya, EN Larionova, EG Larionova, LV Morozova, DA Rastorgueva-Foi, E Sergeev, SG Tornikoski, M Troitsky, IS Thum, C Wiesemeyer, H AF Casadio, Carolina Gomez, Jose L. Jorstad, Svetlana G. Marscher, Alan P. Larionov, Valeri M. Smith, Paul S. Gurwell, Mark A. Laehteenmaeki, Anne Agudo, Ivan Molina, Sol N. Bala, Vishal Joshi, Manasvita Taylor, Brian Williamson, Karen E. Arkharov, Arkady A. Blinov, Dmitry A. Borman, George A. Di Paola, Andrea Grishina, Tatiana S. Hagen-Thorn, Vladimir A. Itoh, Ryosuke Kopatskaya, Evgenia N. Larionova, Elena G. Larionova, Liudmila V. Morozova, Daria A. Rastorgueva-Foi, Elizaveta Sergeev, Sergey G. Tornikoski, Merja Troitsky, Ivan S. Thum, Clemens Wiesemeyer, Helmut TI A MULTI-WAVELENGTH POLARIMETRIC STUDY OF THE BLAZAR CTA 102 DURING A GAMMA-RAY FLARE IN 2012 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: active; galaxies: jets; quasars: individual (CTA 102); techniques: interferometric; techniques: photometric; techniques: polarimetric ID ACTIVE GALACTIC NUCLEI; LARGE-AREA TELESCOPE; SPECTRUM RADIO-SOURCES; BL LACERTAE OBJECTS; BASE-LINE ARRAY; QUASAR 3C 454.3; POLARIZATION VARIABILITY; SUPERLUMINAL MOTION; MAGNETIC-FIELDS; COMPLETE SAMPLE AB We perform a multi-wavelength polarimetric study of the quasar CTA 102 during an extraordinarily bright gamma-ray outburst detected by the Fermi Large Area Telescope in 2012 September-October when the source reached a flux of F->100 MeV = 5.2 +/- 0.4 x 10(-6) photons cm(-2) s(-1). At the same time, the source displayed an unprecedented optical and near-infrared (near-IR) outburst. We study the evolution of the parsec-scale jet with ultra-high angular resolution through a sequence of 80 total and polarized intensity Very Long Baseline Array images at 43 GHz, covering the observing period from 2007 June to 2014 June. We find that the gamma-ray outburst is coincident with flares at all the other frequencies and is related to the passage of a new superluminal knot through the radio core. The powerful gamma-ray emission is associated with a change in direction of the jet, which became oriented more closely to our line of sight (theta similar to 1 degrees.2) during the ejection of the knot and the gamma-ray outburst. During the flare, the optical polarized emission displays intra-day variability and a clear clockwise rotation of electric vector position angles (EVPAs), which we associate with the path followed by the knot as it moves along helical magnetic field lines, although a random walk of the EVPA caused by a turbulent magnetic field cannot be ruled out. We locate the gamma-ray outburst a short distance downstream of the radio core, parsecs from the black hole. This suggests that synchrotron self-Compton scattering of NIR to ultraviolet photons is the probable mechanism for the gamma-ray production. C1 [Casadio, Carolina; Gomez, Jose L.; Agudo, Ivan; Molina, Sol N.] CSIC, Inst Astrofis Andalucia, E-18080 Granada, Spain. [Jorstad, Svetlana G.; Marscher, Alan P.; Bala, Vishal; Joshi, Manasvita; Taylor, Brian; Williamson, Karen E.] Boston Univ, Inst Astrophys Res, Boston, MA 02215 USA. [Jorstad, Svetlana G.; Larionov, Valeri M.; Blinov, Dmitry A.; Grishina, Tatiana S.; Hagen-Thorn, Vladimir A.; Kopatskaya, Evgenia N.; Larionova, Elena G.; Larionova, Liudmila V.; Morozova, Daria A.; Troitsky, Ivan S.] St Petersburg State Univ, Astron Inst, St Petersburg 198504, Russia. [Larionov, Valeri M.; Laehteenmaeki, Anne; Rastorgueva-Foi, Elizaveta; Tornikoski, Merja] Aalto Univ, Metsahovi Radio Observ, FI-02540 Kylmala, Finland. [Smith, Paul S.] Univ Arizona, Steward Observ, Tucson, AZ 85716 USA. [Gurwell, Mark A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Laehteenmaeki, Anne] Aalto Univ, Dept Radio Sci & Engn, FI-00076 Aalto, Finland. [Arkharov, Arkady A.] Pulkovo Observ, St Petersburg, Russia. [Blinov, Dmitry A.] Univ Crete, Iraklion, Greece. [Borman, George A.; Sergeev, Sergey G.] Crimean Astrophys Observ, Nauchnij, Ukraine. [Di Paola, Andrea] Osserv Astron Roma, INAF, I-00136 Rome, Italy. [Itoh, Ryosuke] Hiroshima Univ, Dept Phys Sci, Higashihiroshima, Hiroshima 7398526, Japan. [Rastorgueva-Foi, Elizaveta] Univ Tasmania, Sch Maths Phys, Hobart, Tas 7001, Australia. [Thum, Clemens] Inst Radio Astron Milimetr, Granada, Spain. [Wiesemeyer, Helmut] Max Planck Inst Radioastron, D-53121 Bonn, Germany. RP Casadio, C (reprint author), CSIC, Inst Astrofis Andalucia, Apartado 3004, E-18080 Granada, Spain. RI Lahteenmaki, Anne/L-5987-2013; Agudo, Ivan/G-1701-2015; Morozova, Daria/H-1298-2013; Larionova, Elena/H-7287-2013; Troitskiy, Ivan/K-7979-2013; Jorstad, Svetlana/H-6913-2013; Grishina, Tatiana/H-6873-2013; Blinov, Dmitry/G-9925-2013 OI Larionov, Valeri/0000-0002-4640-4356; Agudo, Ivan/0000-0002-3777-6182; Morozova, Daria/0000-0002-9407-7804; Larionova, Elena/0000-0002-2471-6500; Troitskiy, Ivan/0000-0002-4218-0148; Jorstad, Svetlana/0000-0001-9522-5453; Grishina, Tatiana/0000-0002-3953-6676; Blinov, Dmitry/0000-0003-0611-5784 FU Spanish Ministry of Economy and Competitiveness (MINECO) [AYA2013-40825-P]; NASA Fermi Guest Investigator grants [NNX14AQ58G, NNX13AO99G]; NASA Swift Guest Investigator grant [NNX14AI96G]; Ramon y Cajal grant of the MINECO; NSF; BU; Lowell Observatory; Russian RFBR grant [15-02-00949]; St. Petersburg University [6.38.335.2015]; NASA; W.M. Keck Foundation; INSU/CNRS (France); MPG (Germany); IGN (Spain); Smithsonian Institution; Academia Sinica; Fermi Guest Investigator grants [NNX08AW56G, NNX09AU10G, NNX12AO93G]; Academy of Finland [212656, 210338, 121148] FX This research has been supported by the Spanish Ministry of Economy and Competitiveness (MINECO) grant AYA2013-40825-P. The research at Boston University (BU) was funded in part by NASA Fermi Guest Investigator grants NNX14AQ58G and NNX13AO99G, and Swift Guest Investigator grant NNX14AI96G. I. A. acknowledges support by a Ramon y Cajal grant of the MINECO. The VLBA is operated by the National Radio Astronomy Observatory. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. The PRISM camera at Lowell Observatory was developed by K. Janes et al. at BU and Lowell Observatory, with funding from the NSF, BU, and Lowell Observatory. St. Petersburg University team acknowledges support from Russian RFBR grant 15-02-00949 and St. Petersburg University research grant 6.38.335.2015. This research was conducted in part using the Mimir instrument, jointly developed at Boston University and Lowell Observatory and supported by NASA, NSF, and the W.M. Keck Foundation. The Mimir observations were performed by Lauren Cashman, Jordan Montgomery, and Dan Clemens, all from Boston University. This research is partly based on data taken at the IRAM 30 m Telescope. IRAM is supported by INSU/CNRS (France), MPG (Germany), and IGN (Spain). The Submillimeter Array is a joint project between the Smithsonian Astrophysical Observatory and the Academia Sinica Institute of Astronomy and Astrophysics and is funded by the Smithsonian Institution and the Academia Sinica. Data from the Steward Observatory spectropolarimetric monitoring project were used. This program is supported by Fermi Guest Investigator grants NNX08AW56G, NNX09AU10G, and NNX12AO93G. The Metsahovi team acknowledges the support from the Academy of Finland to our observing projects (numbers 212656, 210338, 121148, and others). NR 74 TC 6 Z9 6 U1 2 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 NOV 1 PY 2015 VL 813 IS 1 AR 51 DI 10.1088/0004-637X/813/1/51 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CW8XZ UT WOS:000365284100051 ER PT J AU Dahle, H Gladders, MD Sharon, K Bayliss, MB Rigby, JR AF Dahle, H. Gladders, M. D. Sharon, K. Bayliss, M. B. Rigby, J. R. TI TIME DELAY MEASUREMENTS FOR THE CLUSTER-LENSED SEXTUPLE QUASAR SDSS J2222+2745 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: clusters: general; gravitational lensing: strong; quasars: individual (SDSS J2222+2745) ID IMAGE SEPARATION; GALAXIES; J1004+4112; J1029+2623; MASSES AB We report first results from an ongoing monitoring campaign to measure time delays between the six images of the quasar SDSS J2222+2745, gravitationally lensed by a galaxy cluster. The time delay between A and B, the two most highly magnified images, is measured to be tau(AB) = 47.7 +/- 6.0 days (95% confidence interval), consistent with previous model predictions for this lens system. The strong intrinsic variability of the quasar also allows us to derive a time delay value of tau(CA) = 722 +/- 24 days between image C and A, in spite of modest overlap between their light curves in the current data set. Image C, which is predicted to lead all the other lensed quasar images, has undergone a sharp, monotonic flux increase of 60%-75% during 2014. A corresponding brightening is firmly predicted to occur in images A and B during 2016. The amplitude of this rise indicates that time delays involving all six known images in this system, including those of the demagnified central images D-F, will be obtainable from further ground-based monitoring of this system during the next few years. C1 [Dahle, H.] Univ Oslo, Inst Theoret Astrophys, NO-0315 Oslo, Norway. [Gladders, M. D.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. [Gladders, M. D.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Sharon, K.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Bayliss, M. B.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Bayliss, M. B.] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. [Rigby, J. R.] NASA, Goddard Space Flight Ctr, Observat Cosmol Lab, Greenbelt, MD 20771 USA. RP Dahle, H (reprint author), Univ Oslo, Inst Theoret Astrophys, POB 1029, NO-0315 Oslo, Norway. EM hdahle@astro.uio.no FU Research Council of Norway; NSF [AST-1009012] FX H.D. acknowledges support from the Research Council of Norway. M.B.B. acknowledges support from the NSF through grant AST-1009012. We acknowledge use of the new Gemini Fast Turnaround Program and the Fast-Track Service mode at NOT, which both provided important data for this paper. We thank the staffs of NOT and Gemini for their flexibility in supporting the execution of our monitoring campaign. 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 24 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 NOV 1 PY 2015 VL 813 IS 1 AR 67 DI 10.1088/0004-637X/813/1/67 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CW8XZ UT WOS:000365284100067 ER PT J AU Garraffo, C Drake, JJ Cohen, O AF Garraffo, Cecilia Drake, Jeremy J. Cohen, Ofer TI THE DEPENDENCE OF STELLAR MASS AND ANGULAR MOMENTUM LOSSES ON LATITUDE AND THE INTERACTION OF ACTIVE REGION AND DIPOLAR MAGNETIC FIELDS SO ASTROPHYSICAL JOURNAL LA English DT Article DE stars: coronae; stars: magnetic field; stars: rotation ID SUN-LIKE STARS; SOLAR-LIKE STARS; PRE-MAIN-SEQUENCE; ROTATIONAL EVOLUTION; TAU-BOOTIS; DIFFERENTIAL ROTATION; POLAR SPOTS; MERIDIONAL FLOW; LOSS RATES; YOUNG SUN AB Rotation evolution of late-type stars is dominated by magnetic braking and the underlying factors that control this angular momentum loss are important for the study of stellar spin-down. In this work, we study angular momentum loss as a function of two different aspects of magnetic activity using a calibrated Alfven wave-driven magnetohydrodynamic wind model: the strengths of magnetic spots and their distribution in latitude. By driving the model using solar and modified solar surface magnetograms, we show that the topology of the field arising from the net interaction of both small-scale and large-scale field is important for spin-down rates and that angular momentum loss is not a simple function of large scale magnetic field strength. We find that changing the latitude of magnetic spots can modify mass and angular momentum loss rates by a factor of two. The general effect that causes these differences is the closing down of large-scale open field at mid-and high-latitudes by the addition of the small-scale field. These effects might give rise to modulation of mass and angular momentum loss through stellar cycles, and present a problem for ab initio attempts to predict stellar spin-down based on wind models. For all the magnetogram cases considered here, from dipoles to various spotted distributions, we find that angular momentum loss is dominated by the mass loss at mid-latitudes. The spin-down torque applied by magnetized winds therefore acts at specific latitudes and is not evenly distributed over the stellar surface, though this aspect is unlikely to be important for understanding spin-down and surface flows on stars. C1 [Garraffo, Cecilia; Drake, Jeremy J.; Cohen, Ofer] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Garraffo, C (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. OI Cohen, Ofer/0000-0003-3721-0215 FU Smithsonian Institution Consortium for Unlocking the Mysteries of the universe; SI CGPS grant "Can Exoplanets Around Red Dwarfs Maintain Habitable Atmospheres?"; NASA [NAS8-03060]; NASA HEC Pleiades system [SMD-13-4526] FX We thank Leon Mestel, Jonathan Mestel, Lorenzo Sironi, Steven Cranmer, and Gaston Giribet for useful discussions. We also thank the anonymous referee for providing us with constructive comments and suggestions. We thank Jean-Rene Galarneau for providing Figure 6 C.G. and O.C. were supported by Smithsonian Institution Consortium for Unlocking the Mysteries of the universe grant "Lessons from Mars: Are Habitable Atmospheres on Planets around M Dwarfs Viable?" during the course of this research. O.C. was also supported by SI CGPS grant "Can Exoplanets Around Red Dwarfs Maintain Habitable Atmospheres?". J.J.D. was supported by NASA contract NAS8-03060 to the Chandra X-ray Center, and thanks the Director, B. Wilkes, and the CXC science team for advice and support. Numerical simulations were performed on the NASA HEC Pleiades system under award SMD-13-4526. NR 89 TC 5 Z9 5 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD NOV 1 PY 2015 VL 813 IS 1 AR 40 DI 10.1088/0004-637X/813/1/40 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CW8XZ UT WOS:000365284100040 ER PT J AU Jiang, YF Cantiello, M Bildsten, L Quataert, E Blaes, O AF Jiang, Yan-Fei Cantiello, Matteo Bildsten, Lars Quataert, Eliot Blaes, Omer TI LOCAL RADIATION HYDRODYNAMIC SIMULATIONS OF MASSIVE STAR ENVELOPES AT THE IRON OPACITY PEAK SO ASTROPHYSICAL JOURNAL LA English DT Article DE hydrodynamics; methods: numerical; radiative transfer; stars: massive ID DOMINATED ACCRETION DISKS; STELLAR ASTROPHYSICS MESA; WOLF-RAYET STARS; EDDINGTON LIMIT; ENERGY-TRANSPORT; EVOLUTION; INSTABILITY; STABILITY; MODULES; ATMOSPHERE AB We perform three-dimensional radiation hydrodynamic simulations of the structure and dynamics of the radiation-dominated envelopes of massive stars at the location of the iron opacity peak. One-dimensional hydrostatic calculations predict an unstable density inversion at this location, whereas our simulations reveal a complex interplay of convective and radiative transport whose behavior depends on the ratio of the photon diffusion time to the dynamical time. The latter is set by the ratio of the optical depth per pressure scale height, tau(0), to tau(c) = c/c(g), where c(g) approximate to 50 km s(-1) is the isothermal sound speed in the gas alone. When tau(0) >> tau(c), convection reduces the radiation acceleration and removes the density inversion. The turbulent energy transport in the simulations agrees with mixing length theory and provides its first numerical calibration in the radiation-dominated regime. When tau(0) << tau(c), convection becomes inefficient and the turbulent energy transport is negligible. The turbulent velocities exceed cg, driving shocks and large density fluctuations that allow photons to preferentially diffuse out through low-density regions. However, the effective radiation acceleration is still larger than the gravitational acceleration so that the time average density profile contains a modest density inversion. In addition, the simulated envelope undergoes large-scale oscillations with periods of a few hours. The turbulent velocity field may affect the broadening of spectral lines and therefore stellar rotation measurements in massive stars, while the time variable outer atmosphere could lead to variations in their mass loss and stellar radius. C1 [Jiang, Yan-Fei] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Cantiello, Matteo; Bildsten, Lars] Univ Calif Santa Barbara, Kavli Inst Theoret Phys, Santa Barbara, CA 93106 USA. [Bildsten, Lars; Blaes, Omer] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA. [Quataert, Eliot] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Quataert, Eliot] Univ Calif Berkeley, Theoret Astrophys Ctr, Berkeley, CA 94720 USA. RP Jiang, YF (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. OI Cantiello, Matteo/0000-0002-8171-8596 FU National Science Foundation [ACI-1053575]; Office of Science of the U.S. Department of Energy [DE-AC02-05CH11231]; NASA through Einstein Postdoctoral Fellowship - Chandra X-ray Center [PF-140109]; NASA [NAS8-03060]; Simons Investigator Award from the Simons Foundation; NASA under TCAN grant [NNX14AB53G]; NSF [PHY 11-25915, AST 11-09174] FX Y.F.J thanks Jeremy Goodman, Jim Stone, Shane Davis and all members of the SPIDER network for helpful discussions. E.Q. thanks Mark Krumholz and Todd Thompson for useful conversations. This work was supported by the computational resources provided by the NASA High-End Computing (HEC) Program through the NASA Advanced Supercomputing (NAS) Division at Ames Research Center; the Extreme Science and Engineering Discovery Environment (XSEDE), which is supported by National Science Foundation grant number ACI-1053575; and 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. Y.F.J. is supported by NASA through Einstein Postdoctoral Fellowship grant number PF-140109 awarded by the Chandra X-ray Center, which is operated by the Smithsonian Astrophysical Observatory for NASA under contract NAS8-03060. E.Q. is supported in part by a Simons Investigator Award from the Simons Foundation. This project was supported by NASA under TCAN grant number NNX14AB53G and the NSF under grants PHY 11-25915 and AST 11-09174. NR 63 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 NOV 1 PY 2015 VL 813 IS 1 AR 74 DI 10.1088/0004-637X/813/1/74 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CW8XZ UT WOS:000365284100074 ER PT J AU Kipping, DM Schmitt, AR Huang, X Torres, G Nesvorny, D Buchhave, LA Hartman, J Bakos, GA AF Kipping, D. M. Schmitt, A. R. Huang, X. Torres, G. Nesvorny, D. Buchhave, L. A. Hartman, J. Bakos, G. A. TI THE HUNT FOR EXOMOONS WITH KEPLER (HEK). V. A SURVEY OF 41 PLANETARY CANDIDATES FOR EXOMOONS SO ASTROPHYSICAL JOURNAL LA English DT Article DE planetary systems; techniques: photometric ID TRANSIT TIMING VARIATIONS; HABITABLE-ZONE; ERROR-CORRECTION; LIGHT CURVES; II. ANALYSIS; ARCHIVE DATA; SATELLITES; EFFICIENT; EXOPLANET; TIME AB We present a survey of 41 Kepler Objects of Interest (KOIs) for exomoons using Bayesian photodynamics, more than tripling the number of KOIs surveyed with this technique. We find no compelling evidence for exomoons although 13 KOIs yield spurious detections driven by instrumental artifacts, stellar activity, and/or perturbations from unseen bodies. Regarding the latter, we find seven KOIs exhibiting > 5 sigma evidence of transit timing variations, including the "mega-Earth" Kepler-10c, likely indicating an additional planet in that system. We exploit the moderately large sample of 57 unique KOIs surveyed to date to infer several useful statistics. For example, although there is a diverse range in sensitivities, we find that we are sensitive to Pluto-Charon mass-ratio systems for similar or equal to 40% of KOIs studied and Earth-Moon mass-ratios for 1 in 8 cases. In terms of absolute mass, our limits probe down to 1.7 Ganymede masses, with a sensitivity to Earth-mass moons for 1 in 3 cases studied and to the smallest moons capable of sustaining an Earth-like atmosphere (0.3M(circle plus)) for 1 in 4. Despite the lack of positive detections to date, we caution against drawing conclusions yet, since our most interesting objects remain under analysis. Finally, we point out that had we searched for the photometric transit signals of exomoons alone, rather than using photodynamics, we estimate that 1 in 4 KOIs would have erroneously been concluded to harbor exomoons due to residual time correlated noise in the Kepler data, posing a serious problem for alternative methods. C1 [Kipping, D. M.] Columbia Univ, Dept Astron, New York, NY 10027 USA. [Huang, X.; Hartman, J.; Bakos, G. A.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. [Torres, G.; Buchhave, L. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Nesvorny, D.] Southwest Res Inst, Dept Space Studies, Boulder, CO 80302 USA. [Buchhave, L. A.] Univ Copenhagen, Ctr Star & Planet Format, Nat Hist Museum Denmark, DK-1350 Copenhagen, Denmark. RP Kipping, DM (reprint author), Columbia Univ, Dept Astron, 550 W 120th St, New York, NY 10027 USA. EM dkipping@astro.columbia.edu OI Bakos, Gaspar/0000-0001-7204-6727; Schmitt, Allan/0000-0002-5034-0949; Buchhave, Lars A./0000-0003-1605-5666; Hartman, Joel/0000-0001-8732-6166 FU Menzel Fellowship; NASA [NNX15AF09G, NNX13AJ15G]; NSF [AST-1008890]; [NNX14AF87G] FX This work made use of the Michael Dodds Computing Facility, for which we are grateful to Michael Dodds, Carl Allegretti, David Van Buren, Anthony Grange, Cameron Lehman, Ivan Long land, Dell Lunceford, Gregor Rothfuss, Matt Salzberg, Richard Sundvall, Graham Symmonds, Kenneth Takigawa, Marion Adam, Dour High Arch, Mike Barrett, Greg Cole, Sheena Dean, Steven De long, Robert Goodman, Mark Greene, Stephen Kitt, Robert Leyland, Matthias Meier, Roy Mitsuoka, David Nicholson, Nicole Papas, Steven Purcell, Austen Redman, Michael Sheldon, Ronald Sonenthal, Nicholas Steinbrecher, Corbin Sydney, John Vajgrt, Louise Valmoria, Hunter Williams, Troy Winarski, and Nigel Wright. D.M.K. is funded by the Menzel Fellowship. D.M.K. and D.N. acknowledge partial support from NASA grant NNX15AF09G. J.H. and G.B. acknowledge partial support from NASA grant NNX13AJ15G. J.H. acknowledges support from NNX14AF87G. D.N. acknowledges support from NSF AST-1008890. This paper includes data collected by the Kepler mission. Funding for the Kepler mission is provided by the NASA Science Mission directorate. NR 57 TC 7 Z9 7 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 NOV 1 PY 2015 VL 813 IS 1 AR 14 DI 10.1088/0004-637X/813/1/14 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CW8XZ UT WOS:000365284100014 ER PT J AU Lonsdale, CJ Lacy, M Kimball, AE Blain, A Whittle, M Wilkes, B Stern, D Condon, J Kim, M Assef, RJ Tsai, CW Efstathiou, A Jones, S Eisenhardt, P Bridge, C Wu, J Lonsdale, CJ Jones, K Jarrett, T Smith, R AF Lonsdale, Carol J. Lacy, M. Kimball, A. E. Blain, A. Whittle, M. Wilkes, B. Stern, D. Condon, J. Kim, M. Assef, R. J. Tsai, C. -W. Efstathiou, A. Jones, S. Eisenhardt, P. Bridge, C. Wu, J. Lonsdale, Colin J. Jones, K. Jarrett, T. Smith, R. TI RADIO JET FEEDBACK AND STAR FORMATION IN HEAVILY OBSCURED, HYPERLUMINOUS QUASARS AT REDSHIFTS similar to 0.5-3. I. ALMA OBSERVATIONS SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: active; galaxies: evolution; galaxies: jets; quasars: general; radio continuum: galaxies; submillimeter: galaxies ID ACTIVE GALACTIC NUCLEI; SPECTRAL ENERGY-DISTRIBUTIONS; MOLECULAR-HYDROGEN EMISSION; INTEGRAL-FIELD SPECTROSCOPY; SUPERMASSIVE BLACK-HOLES; COMPACT STEEP-SPECTRUM; LINE REGION; HOST GALAXIES; FOLLOW-UP; X-RAY AB We present Atacama Large Millimeter/submillimeter Array (ALMA) 870 mu m (345 GHz) data for 49 high-redshift (0.47 < z < 2.85), luminous (11.7 < log(L-bol/L-circle dot) < 14.2) radio-powerful active galactic nuclei (AGNs), obtained to constrain cool dust emission from starbursts concurrent with highly obscured radiative-mode black hole (BH) accretion in massive galaxies that possess a small radio jet. The sample was selected from the Wide-field Infrared Survey Explorer with extremely steep (red) mid-infrared colors and with compact radio emission from NVSS/FIRST. Twenty-six sources are detected at 870 mu m, and we find that the sample has large mid- to far-infrared luminosity ratios, consistent with a dominant and highly obscured quasar. The rest-frame 3 GHz radio powers are 24.7 < log P-3.0 GHz/W Hz(-1)) < 27.3, and all sources are radio-intermediate or radio-loud. BH mass estimates are 7.7 < log(M-BH/M-circle dot) < 10.2. The rest-frame 1-5 mu m spectral energy distributions are very similar to the "Hot DOGs" (hot dust-obscured galaxies), and steeper (redder) than almost any other known extragalactic sources. ISM masses estimated for the ALMA-detected sources are 9.9 < log (M-ISM/M-circle dot) < 11.75 assuming a dust temperature of 30 K. The cool dust emission is consistent with star formation rates reaching several thousand M-circle dot yr(-1), depending on the assumed dust temperature, but we cannot rule out the alternative that the AGN powers all the emission in some cases. Our best constrained source has radiative transfer solutions with approximately equal contributions from an obscured AGN and a young (10-15 Myr) compact starburst. C1 [Lonsdale, Carol J.; Lacy, M.; Kimball, A. E.; Condon, J.] Natl Radio Astron Observ, Charlottesville, VA 22903 USA. [Kimball, A. E.] CSIRO Astron & Space Sci, Australia Telescope Natl Facil, Epping, NSW 1710, Australia. [Blain, A.; Jones, S.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. [Whittle, M.; Jones, K.] Univ Virginia, Dept Astron, Charlottesville, VA 22903 USA. [Wilkes, B.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Stern, D.; Tsai, C. -W.; Eisenhardt, P.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Kim, M.] Observ Carnegie Inst Sci, Pasadena, CA 91101 USA. [Kim, M.] Korea Astron & Space Sci Inst, Daejeon 305348, South Korea. [Assef, R. J.] Univ Diego Portales, Fac Ingn, Nucleo Astron, Santiago, Chile. [Assef, R. J.] NASA Postdoctoral Program NPP, San Jose, CA USA. [Efstathiou, A.] European Univ Cyprus, Sch Sci, CY-1516 Nicosia, Cyprus. [Bridge, C.] CALTECH, Pasadena, CA 91125 USA. [Wu, J.] Univ Calif Los Angeles, Div Astron & Astrophys, Los Angeles, CA 90095 USA. [Lonsdale, Colin J.] MIT, Haystack Observ, Westford, MA 01886 USA. [Jarrett, T.] Univ Cape Town, Dept Astron, ZA-7925 Cape Town, South Africa. [Smith, R.] Drexel Univ, Dept Phys, Philadelphia, PA 19104 USA. RP Lonsdale, CJ (reprint author), Natl Radio Astron Observ, Edgemont Rd, Charlottesville, VA 22903 USA. EM clonsdal@nrao.edu FU National Aeronautics and Space Administration; National Science Foundation [AST 90-15755]; Alfred P. Sloan Foundation; National Science Foundation; U.S. Department of Energy Office of Science; Gemini-CONICYT [32120009] FX This paper makes use of the following ALMA data: ADS/JAO.ALMA#2011.0.00397. S. ALMA is a partnership of ESO (representing its member states), NSF (USA), and NINS (Japan), together with NRC (Canada), NSC and ASIAA (Taiwan), and KASI (Republic of Korea), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by ESO, AUI/NRAO, and NAOJ. This publication makes use of data products from the Wide-field Infrared Survey Explorer, which is a joint project of the University of California, Los Angeles, and the Jet Propulsion Laboratory/California Institute of Technology, funded by the National Aeronautics and Space Administration. This work is based on observations made with the Caltech Submillimeter Observatory, which is operated by the California Institute of Technology under funding from the National Science Foundation, contract AST 90-15755. This paper uses data from SDSS (DR 8). 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/. RJA was supported by Gemini-CONICYT grant number 32120009. We thank the anonymous referee for comments that helped improve the paper. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. NR 128 TC 3 Z9 3 U1 1 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD NOV 1 PY 2015 VL 813 IS 1 AR 45 DI 10.1088/0004-637X/813/1/45 PG 26 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CW8XZ UT WOS:000365284100045 ER PT J AU Perez, LM Chandler, CJ Isella, A Carpenter, JM Andrews, SM Calvet, N Corder, SA Deller, AT Dullemond, CP Greaves, JS Harris, RJ Henning, T Kwon, W Lazio, J Linz, H Mundy, LG Ricci, L Sargent, AI Storm, S Tazzari, M Testi, L Wilner, DJ AF Perez, Laura M. Chandler, Claire J. Isella, Andrea Carpenter, John M. Andrews, Sean M. Calvet, Nuria Corder, Stuartt A. Deller, Adam T. Dullemond, Cornelis P. Greaves, Jane S. Harris, Robert J. Henning, Thomas Kwon, Woojin Lazio, Joseph Linz, Hendrik Mundy, Lee G. Ricci, Luca Sargent, Anneila I. Storm, Shaye Tazzari, Marco Testi, Leonardo Wilner, David J. TI GRAIN GROWTH IN THE CIRCUMSTELLAR DISKS OF THE YOUNG STARS CY Tau AND DoAr 25 SO ASTROPHYSICAL JOURNAL LA English DT Article DE protoplanetary disks; radio continuum: planetary systems; stars: formation; stars: individual (CY Tau, DoAr 25) ID ANGULAR RESOLUTION OBSERVATIONS; PROTOPLANETARY ACCRETION DISKS; SPECTRAL ENERGY-DISTRIBUTIONS; ROSSBY-WAVE INSTABILITY; MILLIMETER WAVELENGTHS; OPTICAL-CONSTANTS; SIZE DISTRIBUTION; PLANET FORMATION; FORMING REGION; DUST PARTICLES AB We present new results from the Disks@EVLA program for two young stars: CY Tau and DoAr 25. We trace continuum emission arising from their circusmtellar disks from spatially resolved observations, down to tens of AU scales, at lambda = 0.9, 2.8, 8.0, 9.8 mm for DoAr 25 and at lambda = 1.3, 2.8, 7.1 mm for CY Tau. Additionally, we constrain the amount of emission whose origin is different from thermal dust emission from 5 cm observations. Directly from interferometric data, we find that observations at 7 mm and 1 cm trace emission from a compact disk while millimeter-wave observations trace an extended disk structure. From a physical disk model, where we characterize the disk structure of CY Tau and DoAr 25 at wavelengths shorter than 5 cm, we find that (1) dust continuum emission is optically thin at the observed wavelengths and over the spatial scales studied, (2) a constant value of the dust opacity is not warranted by our observations, and (3) a high-significance radial gradient of the dust opacity spectral index, beta, is consistent with the observed dust emission in both disks, with low-beta in the inner disk and high-beta in the outer disk. Assuming that changes in dust properties arise solely due to changes in the maximum particle size (a(max)), we constrain radial variations of a(max) in both disks, from cm-sized particles in the inner disk (R < 40 AU) to millimeter sizes in the outer disk (R > 80 AU). These observational constraints agree with theoretical predictions of the radial-drift barrier, however, fragmentation of dust grains could explain our a(max)(R) constraints if these disks have lower turbulence and/or if dust can survive high-velocity collisions. C1 [Perez, Laura M.; Chandler, Claire J.] Natl Radio Astron Observ, Socorro, NM 87801 USA. [Isella, Andrea] Rice Univ, Houston, TX 77005 USA. [Carpenter, John M.; Sargent, Anneila I.] CALTECH, Pasadena, CA 91125 USA. [Andrews, Sean M.; Ricci, Luca; Wilner, David J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Calvet, Nuria] Univ Michigan, Ann Arbor, MI 48109 USA. [Corder, Stuartt A.] Joint ALMA Observ, Santiago, Chile. [Deller, Adam T.] Netherlands Inst Radio Astron ASTRON, NL-7990 AA Dwingeloo, Netherlands. [Dullemond, Cornelis P.] Heidelberg Univ, Ctr Astron, Heidelberg, Germany. [Greaves, Jane S.] Univ St Andrews, Phys & Astron, St Andrews KY16 9SS, Fife, Scotland. [Harris, Robert J.] Univ Illinois, Urbana, IL 61801 USA. [Henning, Thomas; Linz, Hendrik] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Kwon, Woojin] Korea Astron & Space Sci Inst, Daejeon 34055, South Korea. [Lazio, Joseph] CALTECH, Jet Prop Lab, Pasadena, CA 91106 USA. [Mundy, Lee G.; Storm, Shaye] Univ Maryland, College Pk, MD 20742 USA. [Tazzari, Marco; Testi, Leonardo] European So Observ, D-85748 Garching, Germany. [Testi, Leonardo] INAF Osservatorio Astrofis Arcetri, I-50125 Florence, Italy. RP Perez, LM (reprint author), Natl Radio Astron Observ, POB O, Socorro, NM 87801 USA. OI Tazzari, Marco/0000-0003-3590-5814; Dullemond, Cornelis/0000-0002-7078-5910; Deller, Adam/0000-0001-9434-3837 FU Smithsonian Institution; Academia Sinica; National Aeronautics and Space Administration FX We thank the referee for valuable comments. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. Ongoing CARMA development and operations are supported by the National Science Foundation under a cooperative agreement, and by the CARMA partner universities. The SMA is a joint project between the Smithsonian Astrophysical Observatory and the Academia Sinica Institute of Astronomy and Astrophysics, funded by the Smithsonian Institution and Academia Sinica. Part of this research was carried out at the Jet Propulsion Laboratory, Caltech, under a contract with the National Aeronautics and Space Administration. NR 82 TC 11 Z9 11 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 NOV 1 PY 2015 VL 813 IS 1 AR 41 DI 10.1088/0004-637X/813/1/41 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CW8XZ UT WOS:000365284100041 ER PT J AU Saral, G Hora, JL Willis, SE Koenig, XP Gutermuth, RA Saygac, AT AF Saral, G. Hora, J. L. Willis, S. E. Koenig, X. P. Gutermuth, R. A. Saygac, A. T. TI YOUNG STELLAR OBJECTS IN THE MASSIVE STAR-FORMING REGION W49 SO ASTROPHYSICAL JOURNAL LA English DT Article DE infrared: stars; stars: early-type; stars: formation; stars: pre-main sequence ID ARRAY-CAMERA IRAC; SPITZER-SPACE-TELESCOPE; SPECTRAL ENERGY-DISTRIBUTIONS; GIANT MOLECULAR CLOUD; IN-FLIGHT PERFORMANCE; GALACTIC HII-REGIONS; H-II REGIONS; WIDE-FIELD; EMBEDDED CLUSTERS; RING SURVEY AB We present the initial results of our investigation of the star-forming complex W49, one of the youngest and most luminous massive star-forming regions in our Galaxy. We used Spitzer/Infrared Array Camera (IRAC) data to investigate massive star formation with the primary objective of locating. a representative set of protostars and the clusters of young stars that are forming around them. We present our source catalog with the mosaics from the IRAC data. In this study we used a combination of IRAC, MIPS, Two Micron All Sky Survey, and UKIRT Deep Infrared Sky Survey (UKIDSS) data to identify and classify the young stellar objects (YSOs). We identified 232 Class 0/I YSOs, 907 Class II YSOs, and 74 transition disk candidate objects using color-color and color-magnitude diagrams. In addition, to understand the evolution of star formation in W49, we analyzed the distribution of YSOs in the region to identify clusters using a minimal spanning tree method. The fraction of YSOs that belong to clusters with >= 7 members is found to be 52% for a cutoff distance of 96 '', and the ratio of Class II/I objects is 2.1. We compared the W49 region to the G305 and G333 star-forming regions and concluded that W49 has the richest population, with seven subclusters of YSOs. C1 [Saral, G.; Hora, J. L.; Willis, S. E.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Saral, G.] Istanbul Univ, Grad Sch Sci & Engn, Istanbul, Turkey. [Koenig, X. P.] Yale Univ, Dept Astron, New Haven, CT 06520 USA. [Gutermuth, R. A.] Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA. [Saygac, A. T.] Istanbul Univ, Fac Sci, Astron & Space Sci Dept, Istanbul, Turkey. RP Saral, G (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM gsaral@cfa.harvard.edu OI Saral, Gozde/0000-0001-9420-3156 FU NASA [NNX12AI60G]; National Aeronautics and Space Administration; National Science Foundation; Istanbul University [BAP50195] FX This work is based in part on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA. Support for this work was provided by NASA. This publication makes use of data products from the Two Micron All Sky Survey, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology, funded by the National Aeronautics and Space Administration and the National Science Foundation. The authors gratefully acknowledge the referee for useful comments and additional discussion. G. S. acknowledges partial support from NASA Grant NNX12AI60G and Istanbul University grant BAP50195 since this work is part of her PhD thesis research. NR 71 TC 5 Z9 5 U1 1 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD NOV 1 PY 2015 VL 813 IS 1 AR 25 DI 10.1088/0004-637X/813/1/25 PG 21 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CW8XZ UT WOS:000365284100025 ER PT J AU Stein, NM van Dyk, DA Kashyap, VL Siemiginowska, A AF Stein, Nathan M. van Dyk, David A. Kashyap, Vinay L. Siemiginowska, Aneta TI DETECTING UNSPECIFIED STRUCTURE IN LOW-COUNT IMAGES SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: jets; methods: data analysis; methods: statistical; quasars: individual (0730+257); techniques: image processing; X-rays: general ID HIERARCHICAL-MODELS; RECONSTRUCTION; RESTORATION; STATISTICS; CHECKING AB Unexpected structure in images of astronomical sources often presents itself upon visual inspection of the image, but such apparent structure may either correspond to true features in the source or be due to noise in the data. This paper presents a method for testing whether inferred structure in an image with Poisson noise represents a significant departure from a baseline (null) model of the image. To infer image structure, we conduct a Bayesian analysis of a full model that uses a multiscale component to allow flexible departures from the posited null model. As a test statistic, we use a tail probability of the posterior distribution under the full model. This choice of test statistic allows us to estimate a computationally efficient upper bound on a p-value that enables us to draw strong conclusions even when there are limited computational resources that can be devoted to simulations under the null model. We demonstrate the statistical performance of our method on simulated images. Applying our method to an X-ray image of the quasar 0730+257, we find significant evidence against the null model of a single point source and uniform background, lending support to the claim of an X-ray jet. C1 [Stein, Nathan M.] Univ Penn, Dept Stat, Wharton Sch, Philadelphia, PA 19104 USA. [van Dyk, David A.] Univ London Imperial Coll Sci Technol & Med, Stat Sect, London SW7 2AZ, England. [Kashyap, Vinay L.; Siemiginowska, Aneta] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Stein, NM (reprint author), Univ Penn, Dept Stat, Wharton Sch, 400 Jon M Huntsman Hall,3730 Walnut St, Philadelphia, PA 19104 USA. EM natstein@wharton.upenn.edu; dvandyk@imperial.ac.uk; vkashyap@cfa.harvard.edu; asiemiginowska@cfa.harvard.edu FU CHASC International Astrostatistics Center; NSF [DMS 1208791, DMS 1209232, DMS 1513492, DMS 1513484, DMS 1513546]; SI's Competitive Grants Fund [40488100HH0043]; Wolfson Research Merit Award by the British Royal Society; Marie-Curie Career Integration Grant by European Commission; NASA [NAS8-03060] FX This work was conducted under the auspices of the CHASC International Astrostatistics Center. CHASC is supported by NSF grants DMS 1208791, DMS 1209232, DMS 1513492, DMS 1513484, DMS 1513546, and SI's Competitive Grants Fund 40488100HH0043. In addition, D.v.D. acknowledges support 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, and V.K. and A.S. from a NASA contract to the Chandra X-ray Center NAS8-03060. We used data obtained from the Chandra Data Archive and software provided by the Chandra X-ray Center (CXC) in the application packages CIAO and Sherpa. Finally, we thank CHASC members for many helpful discussions, especially Xiao-Li Meng and Kathryn McKeough. NR 39 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 NOV 1 PY 2015 VL 813 IS 1 AR 66 DI 10.1088/0004-637X/813/1/66 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CW8XZ UT WOS:000365284100066 ER PT J AU Soon, W Connolly, R Connolly, M AF Soon, Willie Connolly, Ronan Connolly, Michael TI Re-evaluating the role of solar variability on Northern Hemisphere temperature trends since the 19th century SO EARTH-SCIENCE REVIEWS LA English DT Article DE Solar variability; Climate change; Urbanization bias; Northern Hemisphere temperatures; Total Solar Irradiance ID SURFACE AIR-TEMPERATURE; HISTORICAL CLIMATOLOGY NETWORK; GALACTIC COSMIC-RAYS; SUN-LIKE STARS; MAUNDER MINIMUM; IRRADIANCE VARIATIONS; UNITED-STATES; EMPIRICAL-EVIDENCE; LAST MILLENNIUM; MAGNETIC-FIELD AB Debate over what influence (if any) solar variability has had on surface air temperature trends since the 19th century has been controversial. In this paper, we consider two factors which may have contributed to this controversy: 1. Several different solar variability datasets exist While each of these datasets is constructed on plausible grounds, they often imply contradictory estimates for the trends in solar activity since the 19th century. 2. Although attempts have been made to account for non-climatic biases in previous estimates of surface air temperature trends, recent research by two of the authors has shown that current estimates are likely still affected by non-climatic biases, particularly urbanization bias. With these points in mind, we first review the debate over solar variability. We summarise the points of general agreement between most groups and the aspects which still remain controversial. We discuss possible future research which may help resolve the controversy of these aspects. Then, in order to account for the problem of urbanization bias, we compile a new estimate of Northern Hemisphere surface air temperature trends since 1881, using records from predominantly rural stations in the monthly Global Historical Climatology Network dataset Like previous weather station-based estimates, our new estimate suggests that surface air temperatures warmed during the 1880s-1940s and 1980s-2000s. However, this new estimate suggests these two warming periods were separated by a pronounced cooling period during the 1950s-1970s and that the relative warmth of the mid-20th century warm period was comparable to the recent warm period. We then compare our weather station-based temperature trend estimate to several other independent estimates. This new record is found to be consistent with estimates of Northern Hemisphere Sea Surface Temperature (SST) trends, as well as temperature-proxy-based estimates derived from glacier length records and from tree ring widths. However, the multi-model means of the recent Coupled Model Intercomparison Project Phase 5 (CMIP5) climate model hindcasts were unable to adequately reproduce the new estimate although the modelling of certain volcanic eruptions did seem to be reasonably well reproduced. Finally, we compare our new composite to one of the solar variability datasets not considered by the CMIP5 climate models, i.e., Scafetta and Willson, 2014's update to the Hoyt and Schatten, 1993 dataset A strong correlation is found between these two datasets, implying that solar variability has been the dominant influence on Northern Hemisphere temperature trends since at least 1881. We discuss the significance of this apparent correlation, and its implications for previous studies which have instead suggested that increasing atmospheric carbon dioxide has been the dominant influence. Published by Elsevier B.V. C1 [Soon, Willie] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RP Soon, W (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. OI Connolly, Ronan/0000-0001-5843-3544 NR 268 TC 2 Z9 2 U1 4 U2 26 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0012-8252 EI 1872-6828 J9 EARTH-SCI REV JI Earth-Sci. Rev. PD NOV PY 2015 VL 150 BP 409 EP 452 DI 10.1016/j.earscirev.2015.08.010 PG 44 WC Geosciences, Multidisciplinary SC Geology GA CW2BN UT WOS:000364796200020 ER PT J AU Jensen-Clem, R Muirhead, PS Bottom, M Wallace, JK Vasisht, G Johnson, JA AF Jensen-Clem, Rebecca Muirhead, Philip S. Bottom, Michael Wallace, J. Kent Vasisht, Gautam Johnson, John Asher TI Attaining Doppler Precision of 10 cm s(-1) with a Lock-in Amplified Spectrometer SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC LA English DT Article ID EXTERNALLY DISPERSED INTERFEROMETER; STELLAR RADIAL-VELOCITIES; LASER FREQUENCY COMBS; ADAPTIVE OPTICS; SUPER-EARTHS; SPECTROGRAPH; MASS; PLANETS; TELESCOPE; STARS AB We explore the radial velocity performance benefits of coupling starlight to a fast-scanning interferometer and a fast-readout spectrometer with zero readout noise. By rapidly scanning an interferometer, we can decouple wavelength calibration errors from precise radial velocity measurements, exploiting the advantages of lock-in amplification. In a Bayesian framework, we investigate the correlation between wavelength calibration errors and resulting radial velocity errors. We construct an end-to-end simulation of this approach to address the feasibility of achieving 10 cm s(-1) radial velocity precision on a typical Sun-like star using existing, 5 m-class telescopes. We find that such a precision can be reached in a single night, opening up possibilities for ground-based detections of Earth-Sun analog systems. C1 [Jensen-Clem, Rebecca; Bottom, Michael] CALTECH, Pasadena, CA 91101 USA. [Muirhead, Philip S.] Boston Univ, Dept Astron, Boston, MA 02215 USA. [Wallace, J. Kent; Vasisht, Gautam] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Johnson, John Asher] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Jensen-Clem, R (reprint author), CALTECH, Pasadena, CA 91101 USA. RI Muirhead, Philip/H-2273-2014 OI Muirhead, Philip/0000-0002-0638-8822 FU National Science Foundation Graduate Research Fellowship [DGE-1144469]; Hubble Fellowship Program; NASA through Hubble Fellowship - STScI [HST-HF-51326.01-A, NAS 5-26555]; Directors Research and Development Fund; California Institute of Technology/Jet Propulsion Laboratory; National Space Technology Research Fellowship; David and Lucile Packard Foundation; Alfred P. Sloan Foundation; Caltech-JPL President and Director's fund FX This material is based upon work supported by the National Science Foundation Graduate Research Fellowship under Grant No. DGE-1144469. P. S. M. acknowledges support for his work from the Hubble Fellowship Program, provided by NASA through Hubble Fellowship grant HST-HF-51326.01-A, awarded by the STScI, which is operated by the AURA, Inc., for NASA, under contract NAS 5-26555. P. S. M, G. V., and J. K. W. were supported by the Directors Research and Development Fund and the California Institute of Technology/Jet Propulsion Laboratory. M. B. is supported by a National Space Technology Research Fellowship. J. A. J. is supported by generous grants from the David and Lucile Packard Foundation and the Alfred P. Sloan Foundation. We would like to thank Lynne Hillenbrand for useful discussions. J. K. W. and G. V. are supported by the Caltech-JPL President and Director's fund. NR 34 TC 2 Z9 2 U1 0 U2 2 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-6280 EI 1538-3873 J9 PUBL ASTRON SOC PAC JI Publ. Astron. Soc. Pac. PD NOV PY 2015 VL 127 IS 957 BP 1105 EP 1112 DI 10.1086/683796 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CW2IC UT WOS:000364814000002 ER PT J AU Tepley, AJ Veblen, TT AF Tepley, Alan J. Veblen, Thomas T. TI Spatiotemporal fire dynamics in mixed-conifer and aspen forests in the San Juan Mountains of southwestern Colorado, USA SO ECOLOGICAL MONOGRAPHS LA English DT Article DE dendro-ecology; fire history; fire reconstruction; fire severity; mixed-conifer forest; mixed-severity fire regime; quaking aspen; San Juan Mountains; tree recruitment ID PONDEROSA PINE FORESTS; UPPER MONTANE FORESTS; STAND-REPLACING FIRE; TREE RECRUITMENT; QUAKING ASPEN; KLAMATH MOUNTAINS; FRONT-RANGE; REGIMES; HISTORY; CLIMATE AB Mixed-severity fire regimes may be the most extensive yet poorly understood fire regimes of western North America. Understanding their long-term spatiotemporal dynamics is central to debates regarding altered fire regimes and the need for restoration in the context of changing climate and nearly a century of active fire suppression. However, the complexity of fire patterns and forest stand and landscape structures characteristic of mixed-severity regimes poses a substantial challenge to understanding their long-term dynamics. In this study, we develop analysis methods aimed at understanding the fire-driven forest dynamics of mixed-severity systems and apply them in the San Juan Mountains of southwestern Colorado. We sampled fire scars, stand structure, and >4300 tree ages across two 1340-ha landscapes (Williams Creek and Squaretop Mountain) that span the environmental gradient of montane mixed-conifer and aspen forests. New approaches were applied to identify pulses of tree recruitment, evaluate climate and fire as potential drivers of synchronous recruitment pulses, and combine fire scar and recruitment data to reconstruct fires. The reconstructions provided detailed fire history for each stand, which in turn was used to develop a fire-severity metric, compare fire frequency and severity by forest type, and develop a simulation procedure to evaluate the degree to which tree regeneration depended on fire by species within each forest type. Twenty fires were reconstructed since 1685 at Williams Creek and 13 fires since 1748 at Squaretop Mountain. Patterns of fire severity varied within each fire and over successive events, including high-severity patches of hundreds of hectares in both study areas. Dry mixed-conifer forests experienced relatively short fire intervals (mean 21 years) and low fire severity, and regeneration of the main conifer species was largely dependent on open conditions sustained over successive fires. Moist mixed-conifer forests experienced longer fire intervals (mean 32 years) and a broader range of severities, and fire-caused canopy openings were important for initiating pulses of tree recruitment. Most (83%) aspen stands included two or more post-fire cohorts. The methods presented here can be adapted to other mixed-severity systems to better understand their long-term spatial and temporal dynamics and develop restoration priorities. C1 [Tepley, Alan J.; Veblen, Thomas T.] Univ Colorado, Dept Geog, Boulder, CO 80309 USA. RP Tepley, AJ (reprint author), Smithsonian Conservat Biol Inst, 1500 Remount Rd, Front Royal, VA 22630 USA. EM TepleyA@si.edu OI Tepley, Alan/0000-0002-5701-9613 FU National Science Foundation Partnerships for International Research and Education (PIRE) grant [OISE-0966472] FX This work benefited from field and laboratory assistance by Nick Story, Anthony Culpepper, Alessandra Boterro, Claudio Alvarez, Julia Hicks, Keli Baker, Kate Borrasca, Ignacio Mundo, Dejan Firm, Ryan Lenberg, and Zach Husted. We thank Phil Higuera for advice on using CharAnalysis. Fred Swanson, Julia Jones, Cameron Naficy, and two anonymous reviewers provided helpful comments on drafts of the manuscript. This work was supported by a National Science Foundation Partnerships for International Research and Education (PIRE) grant (OISE-0966472). NR 56 TC 5 Z9 5 U1 8 U2 21 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0012-9615 EI 1557-7015 J9 ECOL MONOGR JI Ecol. Monogr. PD NOV PY 2015 VL 85 IS 4 BP 583 EP 603 DI 10.1890/14-1496.1 PG 21 WC Ecology SC Environmental Sciences & Ecology GA CW4LF UT WOS:000364962200005 ER PT J AU Sneed, JM Ritson-Williams, R Paul, VJ AF Sneed, Jennifer M. Ritson-Williams, Raphael Paul, Valerie J. TI Crustose coralline algal species host distinct bacterial assemblages on their surfaces SO ISME JOURNAL LA English DT Article ID MARINE-INVERTEBRATE LARVAE; BLACK BAND DISEASE; SETTLEMENT; RECRUITMENT; DIVERSITY; METAMORPHOSIS; CYANOBACTERIA; COMMUNITIES; REEFS; MACROALGAE AB Crustose coralline algae (CCA) are important components of many marine ecosystems. They aid in reef accretion and stabilization, create habitat for other organisms, contribute to carbon sequestration and are important settlement substrata for a number of marine invertebrates. Despite their ecological importance, little is known about the bacterial communities associated with CCA or whether differences in bacterial assemblages may have ecological implications. This study examined the bacterial communities on four different species of CCA collected in Belize using bacterial tag-encoded FLX amplicon pyrosequencing of the V1-V3 region of the 16S rDNA. CCA were dominated by Alphaproteobacteria, Gammaproteobacteria and Actinomycetes. At the operational taxonomic unit (OTU) level, each CCA species had a unique bacterial community that was significantly different from all other CCA species. Hydrolithon boergesenii and Titanoderma prototypum, CCA species that facilitate larval settlement in multiple corals, had higher abundances of OTUs related to bacteria that inhibit the growth and/or biofilm formation of coral pathogens. Fewer coral larvae settle on the surfaces of Paragoniolithon solubile and Porolithon pachydermum. These CCA species had higher abundances of OTUs related to known coral pathogens and cyanobacteria. Coral larvae may be able to use the observed differences in bacterial community composition on CCA species to assess the suitability of these substrata for settlement and selectively settle on CCA species that contain beneficial bacteria. C1 [Sneed, Jennifer M.; Ritson-Williams, Raphael; Paul, Valerie J.] Smithsonian Marine Stn Ft Pierce, Ft Pierce, FL USA. [Ritson-Williams, Raphael] Univ Hawaii Manoa, Dept Biol, Honolulu, HI 96822 USA. RP Sneed, JM (reprint author), Smithsonian Inst, Smithsonian Marine Stn Ft Pierce, 701 Seaway Dr, Ft Pierce, FL 34949 USA. EM SneedJ@si.edu FU Smithsonian Institution's Next Generation Sequencing Small Grant; Smithsonian Competitive Grants Program for Science; Smithsonian Marine Station at Fort Pierce FX Funding was provided by the Smithsonian Institution's Next Generation Sequencing Small Grant and the Smithsonian Competitive Grants Program for Science. Support for J Sneed's postdoctoral fellowship was provided by the Smithsonian Marine Station at Fort Pierce. We thank Dr Mary Rice for her helpful input on this project. We thank the Belize Fisheries Department for providing permits to conduct research at Carrie Bow Cay, Belize. This is contribution no. 992 from the Smithsonian Marine Station and 973 from the CCRE program. NR 48 TC 5 Z9 5 U1 10 U2 33 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 1751-7362 EI 1751-7370 J9 ISME J JI ISME J. PD NOV PY 2015 VL 9 IS 11 BP 2527 EP 2536 DI 10.1038/ismej.2015.67 PG 10 WC Ecology; Microbiology SC Environmental Sciences & Ecology; Microbiology GA CW6EZ UT WOS:000365091700018 PM 25918832 ER PT J AU Birnstiel, T Andrews, SM Pinilla, P Kama, M AF Birnstiel, Tilman Andrews, Sean M. Pinilla, Paola Kama, Mihkel TI DUST EVOLUTION CAN PRODUCE SCATTERED LIGHT GAPS IN PROTOPLANETARY DISKS SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE accretion, accretion disks; circumstellar matter; protoplanetary disks ID HD 100546 B; CIRCUMSTELLAR DISK; PLANET FORMATION; CANDIDATE; GAS; FRAGMENTATION; COAGULATION; DISCOVERY; GROWTH; AU AB Recent imaging of protoplanetary disks with high resolution and contrast have revealed a striking variety of substructure. Of particular interest are cases where near-infrared scattered light images show evidence for low-intensity annular "gaps." The origins of such structures are still uncertain, but the interaction of the gas disk with planets is a common interpretation. We study the impact that the evolution of the solid material can have on the observable properties of disks in a simple scenario without any gravitational or hydrodynamical disturbances to the gas disk structure. Even with a smooth and continuous gas density profile, we find that the scattered light emission produced by small dust grains can exhibit ring-like depressions similar to those presented in recent observations. The physical mechanisms responsible for these features rely on the inefficient fragmentation of dust particles. The occurrence and position of the proposed "gap" features depend most strongly on the dust-to-gas ratio, the fragmentation threshold velocity, the strength of the turbulence, and the age of the disk, and should be generic (at some radius) for typically adopted disk parameters. The same physical processes can affect the thermal emission at optically thin wavelengths (similar to 1 mm), although the behavior can be more complex; unlike for disk-planet interactions, a "gap" should not be present at these longer wavelengths. C1 [Birnstiel, Tilman; Andrews, Sean M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Pinilla, Paola; Kama, Mihkel] Leiden Observ, NL-2300 RA Leiden, Netherlands. RP Birnstiel, T (reprint author), Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany. EM tbirnstiel@cfa.harvard.edu; sandrews@cfa.harvard.edu; pinilla@strw.leidenuniv.nl; mkama@strw.leidenuniv.nl OI Kama, Mihkel/0000-0003-0065-7267; Birnstiel, Tilman/0000-0002-1899-8783 FU NASA Origins of Solar Systems grant [NNX12AJ04G]; Smithsonian Institution Pell Grant program; NOVA, KNAW professor prize; European Union A-ERC grant [291141] FX We thank M. Benisty and M. Flock for useful discussions. S.M.A. and T.B. are grateful for support from the NASA Origins of Solar Systems grant NNX12AJ04G, the Smithsonian Institution Pell Grant program, and for generous computing time on the Smithsonian Institution high performance cluster, hydra. Astrochemistry in Leiden is supported by NOVA, KNAW professor prize, and by the European Union A-ERC grant 291141. NR 42 TC 7 Z9 7 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 NOV 1 PY 2015 VL 813 IS 1 AR L14 DI 10.1088/2041-8205/813/1/L14 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CV7WG UT WOS:000364486200014 ER PT J AU Dai, F Winn, JN Arriagada, P Butler, RP Crane, JD Johnson, JA Shectman, SA Teske, JK Thompson, IB Vanderburg, A Wittenmyer, RA AF Dai, Fei Winn, Joshua N. Arriagada, Pamela Butler, R. Paul Crane, Jeffrey D. Johnson, John Asher Shectman, Stephen A. Teske, Johanna K. Thompson, Ian B. Vanderburg, Andrew Wittenmyer, Robert A. TI DOPPLER MONITORING OF THE WASP-47 MULTIPLANET SYSTEM SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE planetary systems; planets and satellites: composition; stars: individual (WASP-47); techniques: radial velocities ID 16 CYGNI B; TERRESTRIAL PLANETS; HIGH-ECCENTRICITY; SIZED EXOPLANET; HOT JUPITERS; MASS; TRANSIT; DENSITY; KEPLER; ORBITS AB We present precise Doppler observations of WASP-47, a transiting planetary system featuring a hot Jupiter with both inner and outer planetary companions. This system has an unusual architecture and also provides a rare opportunity to measure planet masses in two different ways: the Doppler method, and the analysis of transit-timing variations (TTV). Based on the new Doppler data, obtained with the Planet Finder Spectrograph on the Magellan/Clay 6.5 m telescope, the mass of the hot Jupiter is 370 +/- 29 M-circle plus. This is consistent with the previous Doppler determination as well as the TTV determination. For the inner planet WASP-47e, the Doppler data lead to a mass of 12.2 +/- 3.7 M-circle plus, in agreement with the TTV-based upper limit of < 22 M-circle plus (95% confidence). For the outer planet WASP-47d, the Doppler mass constraint of 10.4 +/- 8.4 M-circle plus is consistent with the TTV-based measurement of 15.2(-7.6)(+6.7) M-circle plus. C1 [Dai, Fei; Winn, Joshua N.] MIT, Dept Phys, Cambridge, MA 02139 USA. [Dai, Fei; Winn, Joshua N.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Arriagada, Pamela; Butler, R. Paul; Teske, Johanna K.] Carnegie Inst Sci, Dept Terr Magnetism, Washington, DC 20015 USA. [Crane, Jeffrey D.; Shectman, Stephen A.; Teske, Johanna K.; Thompson, Ian B.] Observ Carnegie Inst Washington, Pasadena, CA 91101 USA. [Johnson, John Asher; Vanderburg, Andrew] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Wittenmyer, Robert A.] UNSW Australia, Sch Phys, Exoplanetary Sci UNSW, Sydney, NSW 2052, Australia. [Wittenmyer, Robert A.] UNSW Australia, Australian Ctr Astrobiol, Sydney, NSW 2052, Australia. RP Dai, F (reprint author), MIT, Dept Phys, Cambridge, MA 02139 USA. EM fd284@mit.edu RI Butler, Robert/B-1125-2009; OI /0000-0002-4265-047X; /0000-0002-8958-0683; Butler, R. Paul/0000-0003-1305-3761; Vanderburg, Andrew/0000-0001-7246-5438 FU NASA Origins program [NNX11AG85G]; Transiting Exoplanet Survey Satellite mission; National Science Foundation [DGE 1144152] FX We thank the referee for a very stimulating review of the manuscript. Work by F.D. and J.N.W. was supported by the NASA Origins program (grant NNX11AG85G) as well as the Transiting Exoplanet Survey Satellite mission. A.V. is supported by the National Science Foundation Graduate Research Fellowship, grant No. DGE 1144152. Australian access to the Magellan Telescopes was supported by the Australian Federal Government through the Department of Industry and Science. NR 39 TC 10 Z9 10 U1 0 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 NOV 1 PY 2015 VL 813 IS 1 AR L9 DI 10.1088/2041-8205/813/1/L9 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CV7WG UT WOS:000364486200009 ER PT J AU Johnston, KG Robitaille, TP Beuther, H Linz, H Boley, P Kuiper, R Keto, E Hoare, MG van Boekel, R AF Johnston, Katharine G. Robitaille, Thomas P. Beuther, Henrik Linz, Hendrik Boley, Paul Kuiper, Rolf Keto, Eric Hoare, Melvin G. van Boekel, Roy TI A KEPLERIAN-LIKE DISK AROUND THE FORMING O-TYPE STAR AFGL 4176 SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE circumstellar matter; ISM: jets and outflows; radiative transfer; stars: formation; stars: massive; techniques: interferometric ID INTERSTELLAR DUST GRAINS; MASSIVE STARS; PROTOPLANETARY DISK; CHEMICAL EVOLUTION; METHANOL MASERS; ACCRETION; EMISSION; ALMA; CANDIDATE; PROTOSTAR AB We present Atacama Large Millimeter/submillimeter Array line and continuum observations at 1.2 mm with similar to 0.'' 3 resolution that uncover a Keplerian-like disk around the forming O-type star AFGL 4176. The continuum emission from the disk at 1.21 mm (source mm1) has a deconvolved size of 870 +/- 110 AU x 330 +/- 300 AU and arises from a structure similar to 8 M-circle dot in mass, calculated assuming a dust temperature of 190 K. The first-moment maps, pixel-to-pixel line modeling, assuming local thermodynamic equilibrium (LTE), and position-velocity diagrams of the CH3CN J = 13-12 K-line emission all show a velocity gradient along the major axis of the source, coupled with an increase in velocity at small radii, consistent with Keplerian-like rotation. The LTE line modeling shows that where CH3CN J = 13-12 is excited, the temperatures in the disk range from similar to 70 to at least 300 K and that the H-2 column density peaks at 2.8 x 10(24) cm(-2). In addition, we present Atacama Pathfinder Experiment (CO)-C-12 observations that show a large-scale outflow from AFGL 4176 perpendicular to the major axis of mm1, supporting the disk interpretation. Finally, we present a radiative transfer model of a Keplerian disk surrounding an O7 star, with a disk mass and radius of 12 M-circle dot and 2000 AU that reproduces the line and continuum data, further supporting our conclusion that our observations have uncovered a Keplerian-like disk around an O-type star. C1 [Johnston, Katharine G.; Hoare, Melvin G.] Univ Leeds, Sch Phys & Astron, Leeds LS2 9JT, W Yorkshire, England. [Johnston, Katharine G.; Robitaille, Thomas P.; Beuther, Henrik; Linz, Hendrik; Kuiper, Rolf; van Boekel, Roy] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Boley, Paul] Ural Fed Univ, Astron Observ, Ekaterinburg, Russia. [Kuiper, Rolf] Univ Tubingen, Inst Astron & Astrophys, D-72076 Tubingen, Germany. [Keto, Eric] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Johnston, KG (reprint author), Univ Leeds, Sch Phys & Astron, EC Stoner Bldg, Leeds LS2 9JT, W Yorkshire, England. EM k.g.johnston@leeds.ac.uk OI Beuther, Henrik/0000-0002-1700-090X; Robitaille, Thomas/0000-0002-8642-1329; Kuiper, Rolf/0000-0003-2309-8963 FU Russian Science Foundation [15-12-10017] FX We thank the referee for insightful comments that helped improve this Letter. We are grateful to have been able to observe with ALMA and APEX on Llano de Chajnantor, Chile. ALMA is a partnership of ESO (representing its member states), NSF (USA) and NINS (Japan), together with NRC (Canada), NSC and ASIAA (Taiwan), and KASI (Republic of Korea), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by ESO, AUI/NRAO and NAOJ. We thank Frank Wyrowski, Miguel Angel Requena Torres, and our ALMA contact scientist Edwige Chapillon. P.B. acknowledges support from the Russian Science Foundation, grant No. 15-12-10017. NR 44 TC 12 Z9 12 U1 6 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 NOV 1 PY 2015 VL 813 IS 1 AR L19 DI 10.1088/2041-8205/813/1/L19 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CV7WG UT WOS:000364486200019 ER PT J AU Montet, BT Bowler, BP Shkolnik, EL Deck, KM Wang, J Horch, EP Liu, MC Hillenbrand, LA Kraus, AL Charbonneau, D AF Montet, Benjamin T. Bowler, Brendan P. Shkolnik, Evgenya L. Deck, Katherine M. Wang, Ji Horch, Elliott P. Liu, Michael C. Hillenbrand, Lynne A. Kraus, Adam L. Charbonneau, David TI DYNAMICAL MASSES OF YOUNG M DWARFS: MASSES AND ORBITAL PARAMETERS OF GJ 3305 AB, THE WIDE BINARY COMPANION TO THE IMAGED EXOPLANET HOST 51 ERI SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE astrometry; binaries: close; stars: fundamental parameters; stars: individual (GJ 3305 AB) ID PRE-MAIN-SEQUENCE; PICTORIS MOVING GROUP; SOLAR NEIGHBORHOOD; RADIAL-VELOCITIES; GIANT PLANETS; STARS; SEARCH; AGE; KINEMATICS; ASTROMETRY AB We combine new high resolution imaging and spectroscopy from Keck/NIRC2, Discovery Channel Telescope/DSSI, and Keck/HIRES with published astrometry and radial velocities to measure individual masses and orbital elements of the GJ 3305 AB system, a young (similar to 20 Myr) M+M binary (unresolved spectral type M0) member of the beta Pictoris moving group comoving with the imaged exoplanet host 51 Eri. We measure a total system mass of 1.11 +/- 0.04 M-circle dot, a period of 29.03 +/- 0.50 year, a semimajor axis of 9.78 +/- 0.14 AU, and an eccentricity of 0.19 +/- 0.02. The primary component has a dynamical mass of 0.67 +/- 0.05 M-circle dot and the secondary has a mass of 0.44 +/- 0.05 M-circle dot. The recently updated BHAC15 models are consistent with the masses of both stars to within 1.5 sigma. Given the observed masses the models predict an age of the GJ 3305 AB system of 37 +/- 9 Myr. Based on the observed system architecture and our dynamical mass measurement, it is unlikely that the orbit of 51 Eri b has been significantly altered by the Kozai-Lidov mechanism. C1 [Montet, Benjamin T.; Bowler, Brendan P.; Deck, Katherine M.; Wang, Ji; Hillenbrand, Lynne A.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA. [Montet, Benjamin T.; Charbonneau, David] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Shkolnik, Evgenya L.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA. [Shkolnik, Evgenya L.] Lowell Observ, Flagstaff, AZ 86001 USA. [Wang, Ji] Yale Univ, Dept Astron, New Haven, CT 06511 USA. [Horch, Elliott P.] So Connecticut State Univ, Dept Phys, New Haven, CT 06515 USA. [Liu, Michael C.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Kraus, Adam L.] 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; Wang, Ji/0000-0002-4361-8885 FU National Science Foundation [DGE-1144469]; National Aeronautics and Space Administration; Discovery Communications; John Templeton Foundation FX B.T.M. is supported by the National Science Foundation Graduate Research Fellowship under grant No. DGE-1144469.; This research has made use of the Keck Observatory Archive (KOA), which is operated by the W. M. Keck Observatory and the NASA Exoplanet Science Institute (NExScI), under contract with the National Aeronautics and Space Administration.; These results made use of Lowell Observatory's Discovery Channel Telescope. Lowell operates the DCT in partnership with Boston University, Northern Arizona University, the University of Maryland, and the University of Toledo. Partial support of the DCT was provided by Discovery Communications.; This publication was made possible through the support of a grant from the John Templeton Foundation. The opinions expressed in this publication are those of the authors and do not necessarily reflect the views of the John Templeton Foundation. NR 43 TC 6 Z9 6 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 NOV 1 PY 2015 VL 813 IS 1 AR L11 DI 10.1088/2041-8205/813/1/L11 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CV7WG UT WOS:000364486200011 ER PT J AU Costion, CM Simpson, L Pert, PL Carlsen, MM Kress, WJ Crayn, D AF Costion, Craig M. Simpson, Lalita Pert, Petina L. Carlsen, Monica M. Kress, W. John Crayn, Darren TI Will tropical mountaintop plant species survive climate change? Identifying key knowledge gaps using species distribution modelling in Australia SO BIOLOGICAL CONSERVATION LA English DT Article DE Cloud forest; Endemics; Threatened species; Range shifts; Acclimation; Wet Tropics ID MONTANE CLOUD FORESTS; RAIN-FOREST; WET TROPICS; GEOGRAPHIC DISTRIBUTIONS; RANGE SHIFTS; IMPACTS; RESPONSES; VULNERABILITY; BIODIVERSITY; TEMPERATURES AB Species inhabiting tropical mountaintops may be most at risk from the detrimental effects of climate change. Yet few regional assessments have critically assessed the degree of threat to species in these habitats. Here we model under three climate scenarios the current and future suitable climate niche of 19 plant species endemic to tropical mountaintops in northeast Queensland, Australia. The suitable climate niche for each of the 19 species is predicted to decline by a minimum of 17% and maximum of 100% by 2040 (mean for all species of 81%) and minimum of 46% (mean for all species of 95%) by 2080. Seven species are predicted to have some suitable climate niche space reductions (ranging from 1 to 54% of their current suitable area) by 2080 under all three climate scenarios. Three additional species are projected to retain between 0.1 and 9% of their current distribution under one or two of the climate scenarios. In addition to these declines, which are predicted to occur over the next 30 years in northeast Queensland, we discuss and outline pressing research priorities that may be relevant for the conservation of biodiversity on tropical mountaintop environments across the globe. Specifically, further research is needed on thermal tolerances, acclimation potentials, and physiological constraints of tropical mountaintop taxa as current species distributions are primarily determined by climatic factors. (C) 2015 Elsevier Ltd. All rights reserved. C1 [Costion, Craig M.; Simpson, Lalita; Crayn, Darren] James Cook Univ, Australian Trop Herbarium, Cairns, Qld 4870, Australia. [Costion, Craig M.; Carlsen, Monica M.; Kress, W. John] Natl Museum Nat Hist, Dept Bot, Smithsonian Inst, Washington, DC 20013 USA. [Costion, Craig M.] James Cook Univ, Ctr Trop Biodivers & Climate Change, Cairns, Qld 4870, Australia. [Pert, Petina L.] CSIRO Ecosyst Sci, Cairns, Qld 4870, Australia. [Pert, Petina L.; Crayn, Darren] James Cook Univ, Coll Marine & Environm Sci, Cairns, Qld 4870, Australia. [Crayn, Darren] James Cook Univ, Ctr Trop Environm Sustainabil Sci, Cairns, Qld 4870, Australia. RP Costion, CM (reprint author), Natl Museum Nat Hist, Dept Bot, Smithsonian Inst, MRC 166,POB 37012, Washington, DC 20013 USA. EM costionc@si.edu RI Crayn, Darren/A-7386-2011; Pert, Petina/F-5211-2010 OI Crayn, Darren/0000-0001-6614-4216; Pert, Petina/0000-0002-7738-7691 FU National Environment Research Program of Australia FX We would like to thank the National Environment Research Program of Australia for funding this research and supporting climate change and threatened species research in general. We also wish to thank Andrew Ford and Jeremy VanDerWal for providing helpful comments and recommendations for improving the manuscript. NR 64 TC 6 Z9 6 U1 10 U2 33 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 NOV PY 2015 VL 191 BP 322 EP 330 DI 10.1016/j.biocon.2015.07.022 PG 9 WC Biodiversity Conservation; Ecology; Environmental Sciences SC Biodiversity & Conservation; Environmental Sciences & Ecology GA CV4SP UT WOS:000364257100037 ER PT J AU Castillo-Cardenas, MF Ramirez-Silva, JA Sanjur, O Toro-Perea, N AF Fernanda Castillo-Cardenas, Maria Alejandro Ramirez-Silva, Jose Sanjur, Oris Toro-Perea, Nelson TI Evidence of incipient speciation in the Neotropical mangrove Pelliciera rhizophorae (Tetrameristaceae) as revealed by molecular, morphological, physiological and climatic characteristics SO BOTANICAL JOURNAL OF THE LINNEAN SOCIETY LA English DT Article DE climate; molecular markers; morphology; speciation ID NICHE CONSERVATISM; STOMATAL DENSITY; EVOLUTION; DIVERSIFICATION; PLASTICITY AB Two variants of the Neotropical mangrove species Pelliciera rhizophorae distributed along both sides of the Isthmus of Panama were detected by different colouration of the floral bracts and the size of the floral and vegetative structures. These findings raised questions concerning a possible speciation event in P. rhizophorae, for which a series of macro-and microscopic morphological traits (reproductive and vegetative structures), molecular markers from plastid DNA and climatic profiles were analyzed. Samples of P. rhizophorae were collected in three localities from the Panamanian Caribbean and Pacific coasts. The data obtained from molecular markers and morphological traits showed significant differences between the variants. The climatic profiles showed contrasting characteristics of rainfall and temperature in their habitats: variant A is found in wetter zones and variant B occupies drier zones. Evidence suggesting that a process of incipient speciation has occurred in P. rhizophorae in response to ecogeographical isolation due to climatic factors is presented. The presence of two geographically separate genetic-morphological groups, adapted to contrasting climatic conditions, will be the basis for suggesting the existence of incipient lineages in Pelliciera. (C) 2015 The Linnean Society of London. C1 [Fernanda Castillo-Cardenas, Maria; Sanjur, Oris] Smithsonian Trop Res Inst, Balboa 084303092, Ancon, Panama. [Fernanda Castillo-Cardenas, Maria; Toro-Perea, Nelson] Univ Valle, Dept Biol, Cali 25360, Colombia. [Alejandro Ramirez-Silva, Jose] Univ Panama, Dept Bot, Fac Ciencias Exactas Nat & Tecnol, Panama City, Panama. RP Castillo-Cardenas, MF (reprint author), Smithsonian Trop Res Inst, Balboa 084303092, Ancon, Panama. EM mfcastillo@gmail.com FU International Foundation for Science [D/3832-3] FX We would like to express our gratitude to the International Foundation for Science for supporting the development of this research through funding this study (grant D/3832-3). We are also grateful to Biologist Jorge Ceballos (from the Smithsonian Tropical Research Institute) for his assistance with the microscopy work. We are grateful to MSc Alonso Santos and Biologist Daniel Buitrago, who collaborated in the field work and photography. NR 42 TC 0 Z9 0 U1 5 U2 5 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0024-4074 EI 1095-8339 J9 BOT J LINN SOC JI Bot. J. Linnean Soc. PD NOV PY 2015 VL 179 IS 3 BP 499 EP 510 DI 10.1111/boj.12337 PG 12 WC Plant Sciences SC Plant Sciences GA CV8JL UT WOS:000364530100011 ER PT J AU Reudink, MW Van Wilgenburg, SL Steele, LS Pillar, AG Marra, PP McKellar, AE AF Reudink, Matthew W. Van Wilgenburg, Steven L. Steele, Lauren S. Pillar, Andrew G. Marra, Peter P. McKellar, Ann E. TI Patterns of migratory connectivity in Vaux's Swifts at a northern migratory roost: A multi-isotope approach SO CONDOR LA English DT Article DE cluster analysis; conservation; migratory connectivity; roost; stable isotope; Vaux's Swift ID STABLE-ISOTOPES; REPRODUCTIVE SUCCESS; HABITAT SEGREGATION; NONBREEDING-SEASON; WINTERING GROUNDS; MIGRANT SONGBIRDS; HYDROGEN ISOTOPES; OXYGEN ISOTOPES; DATA SET; ORIGINS AB The strength of migratory connectivity between breeding, stopover, and wintering areas can have important implications for population dynamics, evolutionary processes, and conservation. For example, patterns of migratory connectivity may influence the vulnerability of species and populations to stochastic events. For many migratory songbirds, however, we are only beginning to understand patterns of migratory connectivity. We investigated the potential strength of migratory connectivity within a population of Vaux's Swifts (Chaetura vauxi). Like many aerial insectivores, this species is currently experiencing population declines. In 2012, a mass mortality event at a spring migratory roost on Vancouver Island, British Columbia, Canada, resulted in the deaths of >1,000 individuals (similar to 2% of the British Columbia population). In these individuals, we examined variation in 3 stable isotopes (delta H-2, delta C-13, and delta N-15) from claw samples to determine whether spring migrants showed inherent isotopic similarity in the habitats they used on their Mexican and Central American wintering grounds. Our results indicated the presence of 2 or 3 broad isotopic clusters, which suggests that Vaux's Swifts that migrated through Vancouver Island most likely originated from 2 or 3 overwintering locales or habitat types. We found no evidence of sex- or morphology-based segregation, which suggests that these groups likely share a similar overwintering ecology and, thus, may be equally vulnerable to stochastic events or habitat loss on the wintering grounds. Our results highlight the need for more studies on the nonbreeding-season ecology and migratory connectivity of this species. C1 [Reudink, Matthew W.; Steele, Lauren S.; Pillar, Andrew G.] Thompson Rivers Univ, Dept Biol Sci, Kamloops, BC, Canada. [Van Wilgenburg, Steven L.; McKellar, Ann E.] Environm Canada, Saskatoon, SK, Canada. [Marra, Peter P.] Smithsonian Conservat Biol Inst, Migratory Bird Ctr, Washington, DC USA. RP Reudink, MW (reprint author), Thompson Rivers Univ, Dept Biol Sci, Kamloops, BC, Canada. EM mreudink@tru.ca OI Reudink, Matthew/0000-0001-8956-5849 FU Natural Sciences and Engineering Research Council of Canada Discovery Grant; Thompson Rivers University Internal Research Fund Award; National Science Foundation grant FX Funding was provided by a Natural Sciences and Engineering Research Council of Canada Discovery Grant, a Thompson Rivers University Internal Research Fund Award to M.W.R., and a National Science Foundation grant to P.P.M. NR 93 TC 0 Z9 0 U1 6 U2 11 PU COOPER ORNITHOLOGICAL SOC PI LAWRENCE PA ORNITHOLOGICAL SOC NORTH AMER PO BOX 1897, LAWRENCE, KS 66044-8897 USA SN 0010-5422 EI 1938-5129 J9 CONDOR JI Condor PD NOV PY 2015 VL 117 IS 4 BP 670 EP 682 DI 10.1650/CONDOR-15-82.1 PG 13 WC Ornithology SC Zoology GA CV4HT UT WOS:000364228500017 ER PT J AU Sharpe, DMT Langerhans, RB Low-Decarie, E Chapman, LJ AF Sharpe, D. M. T. Langerhans, R. B. Low-Decarie, E. Chapman, L. J. TI Little evidence for morphological change in a resilient endemic species following the introduction of a novel predator SO JOURNAL OF EVOLUTIONARY BIOLOGY LA English DT Article DE contemporary evolution; dagaa; ecomorphology; geometric morphometrics; introduced species; Lake Victoria; mukene; predation; predator-prey interactions ID RESTRICTED MAXIMUM-LIKELIHOOD; GUPPIES POECILIA-RETICULATA; LIFE-HISTORY EVOLUTION; EAST-AFRICAN CYPRINID; LATES-NILOTICUS L; LAKE-VICTORIA; NILE PERCH; RASTRINEOBOLA-ARGENTEA; BODY SHAPE; GASTEROSTEUS-ACULEATUS AB Human activities, such as species introductions, are dramatically and rapidly altering natural ecological processes and often result in novel selection regimes. To date, we still have a limited understanding of the extent to which such anthropogenic selection may be driving contemporary phenotypic change in natural populations. Here, we test whether the introduction of the piscivorous Nile perch, Lates niloticus, into East Africa's Lake Victoria and nearby lakes coincided with morphological change in one resilient native prey species, the cyprinid fish Rastrineobola argentea. Drawing on prior ecomorphological research, we predicted that this novel predator would select for increased allocation to the caudal region in R.argentea to enhance burst-swimming performance and hence escape ability. To test this prediction, we compared body morphology of R.argentea across space (nine Ugandan lakes differing in Nile perch invasion history) and through time (before and after establishment of Nile perch in Lake Victoria). Spatial comparisons of contemporary populations only partially supported our predictions, with R.argentea from some invaded lakes having larger caudal regions and smaller heads compared to R.argentea from uninvaded lakes. There was no clear evidence of predator-associated change in body shape over time in Lake Victoria. We conclude that R.argentea have not responded to the presence of Nile perch with consistent morphological changes and that other factors are driving observed patterns of body shape variation in R.argentea. C1 [Sharpe, D. M. T.; Chapman, L. J.] McGill Univ, Dept Biol, Montreal, PQ H3A 1B1, Canada. [Sharpe, D. M. T.] Smithsonian Trop Res Inst, Panama City 084303092, Panama. [Langerhans, R. B.] N Carolina State Univ, Dept Biol Sci, Raleigh, NC 27695 USA. [Langerhans, R. B.] N Carolina State Univ, WM Keck Ctr Behav Biol, Raleigh, NC 27695 USA. [Low-Decarie, E.] Univ Essex, Sch Biol Sci, Colchester CO4 3SQ, Essex, England. RP Sharpe, DMT (reprint author), Smithsonian Trop Res Inst, Naos Labs, Panama City 084303092, Panama. EM sharped@si.edu OI Low-Decarie, Etienne/0000-0002-0413-567X FU NSERC Discovery Grant; Canada Research Chair funds; U.S. National Science Foundation [DEB 0842364]; NSERC USRA; NSERC Canada Graduate Scholarship; NSERC Michael Smith Foreign Study Supplement; FQRNT Bourse de Recherche Doctorale; National Geographic Society Young Explorer's Grant FX We thank our colleagues at NaFIRRI, especially Dr. John Balirwa (Director), Dr. Dismas Mbabazi, S.B. Wandera and A. Byekwaso, for their long-term support of our research programme and for kindly providing access to the museum collections at NaFIRRI. The Uganda National Council for Science and Technology (UNSCT), the Office of the President, the Uganda Wildlife Authority (UWA) and the Fisheries Commissioner of Uganda granted permission for us to conduct our research in Uganda and export samples. Funding was provided by a NSERC Discovery Grant and Canada Research Chair funds (L. Chapman), a U.S. National Science Foundation Grant (DEB 0842364, B. Langerhans), an NSERC USRA (E. Low-Decarie) and a NSERC Canada Graduate Scholarship, NSERC Michael Smith Foreign Study Supplement, FQRNT Bourse de Recherche Doctorale, and a National Geographic Society Young Explorer's Grant (to D. Sharpe). We gratefully acknowledge A. Byekwaso, C. Chapman, C. Freisen, S. Gray, M. Hillary, A. Jacob, S. Kehler, D. Mbabazi, C. Morgan, E. Nyboer, P. Omega, D. Twinomuguisha and the field assistants at Lake Nabugabo for assistance with field work and data collection. M. Turner helped to digitize and analyse R. argentea samples from earlier collections as part of a pilot study that helped to guide this work. We thank L.F. De Leon, C. Firmat, Editor Karin Pfennig and two other anonymous reviewers, whose comments greatly improved the manuscript. NR 105 TC 0 Z9 0 U1 6 U2 22 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 NOV PY 2015 VL 28 IS 11 BP 2054 EP 2067 DI 10.1111/jeb.12720 PG 14 WC Ecology; Evolutionary Biology; Genetics & Heredity SC Environmental Sciences & Ecology; Evolutionary Biology; Genetics & Heredity GA CV9XM UT WOS:000364641900012 PM 26278629 ER PT J AU Loeb, A AF Loeb, Abraham TI The infinity pool SO NATURE PHYSICS LA English DT Editorial Material C1 [Loeb, Abraham] Harvard Smithsonian Ctr Astrophys, Harvard Astron Dept, Cambridge, MA 02138 USA. [Loeb, Abraham] Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, Cambridge, MA 02138 USA. RP Loeb, A (reprint author), Harvard Smithsonian Ctr Astrophys, Harvard Astron Dept, 60 Garden St, Cambridge, MA 02138 USA. EM aloeb@cfa.harvard.edu NR 0 TC 0 Z9 0 U1 2 U2 2 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 NOV PY 2015 VL 11 IS 11 BP 884 EP 885 PG 2 WC Physics, Multidisciplinary SC Physics GA CW2DF UT WOS:000364800600003 ER PT J AU Bush, AM Bambach, RK AF Bush, Andrew M. Bambach, Richard K. TI Sustained Mesozoic-Cenozoic diversification of marine Metazoa: A consistent signal from the fossil record SO GEOLOGY LA English DT Article ID PHANEROZOIC TAXONOMIC DIVERSITY; LARGE-SCALE; CONTINENTAL SCALES; SPECIES-DIVERSITY; ALPHA-DIVERSITY; EXTINCTION; BIODIVERSITY; HISTORY; ORIGINATION; DYNAMICS AB Paleobiological data provide a key historical record of global biodiversity dynamics, but their interpretation is controversial due to geological and sampling biases. Raw data suggest that marine metazoans diversified dramatically during the late Mesozoic and Cenozoic, whereas bias-corrected analyses based on occurrence-level data in the Paleobiology Database (PBDB) have indicated much less Cenozoic diversification. These standardized analyses are cited as evidence that biases strongly conceal underlying patterns in the global fossil record. However, we show that marine diversity did increase substantially and continuously from the Jurassic to the Neogene, even after correcting for biases in PBDB data. Previous standardized analyses did not capture this diversification in full because they were based on incomplete data. In the Cenozoic, observed richness rose to twice the Paleozoic average, which is within the range of values seen in analyses of raw data, suggesting that even the raw global marine fossil record preserves first-order signals of diversity history. C1 [Bush, Andrew M.] Univ Connecticut, Dept Ecol & Evolutionary Biol, Storrs, CT 06269 USA. [Bush, Andrew M.] Univ Connecticut, Ctr Integrat Geosci, Storrs, CT 06269 USA. [Bambach, Richard K.] Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20013 USA. RP Bush, AM (reprint author), Univ Connecticut, Dept Ecol & Evolutionary Biol, 75 North Eagleville Rd, Storrs, CT 06269 USA. NR 43 TC 3 Z9 4 U1 1 U2 21 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 NOV PY 2015 VL 43 IS 11 BP 979 EP 982 DI 10.1130/G37162.1 PG 4 WC Geology SC Geology GA CV1ZW UT WOS:000364057700013 ER PT J AU Sanders, RW Cooke, SL Fischer, JM Fey, SB Heinze, AW Jeffrey, WH Macaluso, AL Moeller, RE Morris, DP Neale, PJ Olson, MH Pakulski, JD Porter, JA Schoener, DM Williamson, CE AF Sanders, Robert W. Cooke, Sandra L. Fischer, Janet M. Fey, Samuel B. Heinze, Adam W. Jeffrey, Wade H. Macaluso, Amy L. Moeller, Robert E. Morris, Donald P. Neale, Patrick J. Olson, Mark H. Pakulski, J. Dean Porter, Jason A. Schoener, Donald M. Williamson, Craig E. TI Shifts in microbial food web structure and productivity after additions of naturally occurring dissolved organic matter: Results from large-scale lacustrine mesocosms SO LIMNOLOGY AND OCEANOGRAPHY LA English DT Article ID FRESH-WATER; ULTRAVIOLET-RADIATION; BACTERIAL PRODUCTION; CLIMATE-CHANGE; COMPENSATORY DYNAMICS; COMMUNITY RESPONSES; LAKES; CARBON; PHYTOPLANKTON; ZOOPLANKTON AB Predicting the effects of dissolved organic matter (DOM) on pelagic food webs can be difficult because DOM modifies water column optics and can have contrasting effects on species across trophic levels. We combined large mesocosm, smaller-scale experiments and autoregressive modeling driven bu DOC concentration or DOM optical quality (colored DOM, or CDOM, measured as DOC-specific absorbance at 320 nm, SUVA(320)) to assess how heterotrophic and phototrophic microbial populations were altered in a temperate oligotrophic lake. DOM additions yielded DOC concentrations of 1.6 mg L-1 (control) 2.5 mg L-1, 3.0 mg L-1, and 4.3 mg L-1. Primary (PP) and bacterial (BP) production as well as heterotrophic and autotrophic protist abundances were stimulated in the higher DOM additions. BP responded rapidly to DOM additions, but unlike PP, returned to the level of controls within 2-7 d. A bioassay showed that the DOM was a nitrogen source for phytoplankton. The two models revealed that BP and edible phytoplankton were stimulated by CDOM (SUVA(320)), but only BP was stimulated by DOC concentration. Ultraviolet radiation (UV) inhibited protists in both models, but stimulated edible phytoplankton only in the SUVA(320) model runs. These results suggest that in transparent oligotrophic lakes large influxes of terrestrial (high SUVA(320)) DOM will stimulate the microbial food web by providing a nutrient subsidy to bacteria and reducing exposure of protists to damaging UV. Nutrients associated with moderate DOM input may also stimulate PP relative to BP, as was observed in these and other experiments, rather than causing an overall system shift toward heterotrophy. C1 [Sanders, Robert W.; Heinze, Adam W.; Macaluso, Amy L.; Schoener, Donald M.] Temple Univ, Dept Biol, Philadelphia, PA 19122 USA. [Cooke, Sandra L.; Morris, Donald P.; Porter, Jason A.] Lehigh Univ, Dept Earth & Environm Sci, Bethlehem, PA 18015 USA. [Cooke, Sandra L.] High Point Univ, Dept Biol, High Point, NC USA. [Fischer, Janet M.; Olson, Mark H.] Franklin & Marshall Coll, Dept Biol, Lancaster, PA 17604 USA. [Fey, Samuel B.] Yale Univ, Dept Ecol & Evolutionary Biol, New Haven, CT USA. [Heinze, Adam W.] Alvernia Univ, Dept Biol, Reading, PA USA. [Jeffrey, Wade H.; Pakulski, J. Dean] Univ W Florida, Ctr Environm Diagnost & Bioremediat, Pensacola, FL 32514 USA. [Moeller, Robert E.; Williamson, Craig E.] Miami Univ, Dept Zool, Oxford, OH 45056 USA. [Neale, Patrick J.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. [Porter, Jason A.] KIPP DuBois Collegiate Acad, Philadelphia, PA USA. [Schoener, Donald M.] Massasoit Community Coll, Dept Biol, Canton, MA USA. RP Sanders, RW (reprint author), Temple Univ, Dept Biol, Philadelphia, PA 19122 USA. EM robert.sanders@temple.edu RI Sanders, Robert/C-1116-2011 OI Sanders, Robert/0000-0001-7264-1059 FU NSF [DEB-0210972] FX This article is dedicated to the memory of our friend and colleague Robert E. Moeller. We thank the Blooming Grove Hunting and Fishing Club for access to Lake Giles and Lacawac Sanctuary for facilities use. We thank Timothy Guida, Ryan Lockwood and Jaclyn Nicolai who supplied help in the field. This work was supported by NSF Grant DEB-0210972. NR 53 TC 4 Z9 4 U1 11 U2 62 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0024-3590 EI 1939-5590 J9 LIMNOL OCEANOGR JI Limnol. Oceanogr. PD NOV PY 2015 VL 60 IS 6 BP 2130 EP 2144 DI 10.1002/lno.10159 PG 15 WC Limnology; Oceanography SC Marine & Freshwater Biology; Oceanography GA CU9TO UT WOS:000363888400020 ER PT J AU Ineson, J Croston, JH Hardcastle, MJ Kraft, RP Evans, DA Jarvis, M AF Ineson, J. Croston, J. H. Hardcastle, M. J. Kraft, R. P. Evans, D. A. Jarvis, M. TI The link between accretion mode and environment in radio-loud active galaxies SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies: active; galaxies: clusters: intracluster medium; galaxies: jets ID BRIGHTEST CLUSTER GALAXIES; SUPERMASSIVE BLACK-HOLES; X-RAY-PROPERTIES; 2 JY SAMPLE; GALACTIC NUCLEI; XMM-NEWTON; ASTRONOMICAL DATA; HERCULES-A; INTRACLUSTER MEDIUM; STAR-FORMATION AB The interactions between radio-loud AGN and their environments play an important role in galaxy and cluster evolution. Recent work has demonstrated fundamental differences between high-and low-excitation radio galaxies (HERGs and LERGs), and shown that they may have different relationships with their environments. In the Chandra Large Project ERA (Environments of Radio-loud AGN), we made the first systematic X-ray environmental study of the cluster environments of radio galaxies at a single epoch (z similar to 0.5), and found tentative evidence for a correlation between radio luminosity and cluster X-ray luminosity. We also found that this relationship appeared to be driven by the LERG subpopulation. We have now repeated the analysis with a low-redshift sample (z similar to 0.1), and found strong correlations between radio luminosity and environment richness and between radio luminosity and central density for the LERGs but not for the HERGs. These results are consistent with models in which the HERGs are fuelled from accretion discs maintained from local reservoirs of gas, while LERGs are fuelled more directly by gas ingested from the intracluster medium. Comparing the samples, we found that although the maximum environment richness of the HERG environments is similar in both samples, there are poorer HERG environments in the z similar to 0.1 sample than in the z similar to 0.5 sample. We have therefore tentative evidence of evolution of the HERG environments. We found no differences between the LERG subsamples for the two epochs, as would be expected if radio and cluster luminosities are related. C1 [Ineson, J.; Croston, J. H.] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England. [Croston, J. H.] Univ Cambridge, Inst Continuing Educ, Cambridge CB23 8AQ, England. [Hardcastle, M. J.; Jarvis, M.] Univ Hertfordshire, Sch Phys Astron & Math, Hatfield AL10 9AB, Herts, England. [Kraft, R. P.; Evans, D. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Jarvis, M.] Univ Oxford, Subdept Astrophys, Dept Phys, Oxford OX1 3RH, England. [Jarvis, M.] Univ Western Cape, Dept Phys, ZA-7535 Bellville, South Africa. RP Ineson, J (reprint author), Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England. EM ji1g10@soton.ac.uk; J.Croston@soton.ac.uk OI Hardcastle, Martin/0000-0003-4223-1117 FU South-East Physics Network (SEPnet); Science and Technology Facilities Council (STFC) [ST/J001600/1]; ESA Member States; NASA; National Aeronautics and Space Administration FX The authors would like to thank the referee for a useful report. JI acknowledges the support of the South-East Physics Network (SEPnet). JHC acknowledges support from the Science and Technology Facilities Council (STFC) under grant ST/J001600/1.; The scientific results reported in this paper are based on observations made with the Chandra X-ray observatory and on observations obtained with XMM-Newton, an ESA science mission with instruments and contributions directly funded by ESA Member States and NASA. This research has made use of software provided by the Chandra X-ray Center (CXC) in the application packages CIAO and CHIPS, and of the XMM-Newton Science Analysis Software (SAS). This research also made use of the University of Hertfordshire high-performance computing facility (http://stri-cluster.herts.ac.uk/). This research has made use of the following online databases: 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; the SIMBAD database, operated at CDS, Strasbourg, France; the 3CRR catalogue, maintained by M. Hardcastle, University of Hertfordshire, UK; the 3CRR Atlas of DRAGNs, maintained by J. P. Leahy, University of Manchester, UK. Figures were plotted using the VEUSZ package (http://home.gna.org/veusz/). NR 142 TC 5 Z9 5 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 NOV 1 PY 2015 VL 453 IS 3 BP 2682 EP 2706 DI 10.1093/mnras/stv1807 PG 25 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CU6NL UT WOS:000363649000037 ER PT J AU Rivera-Sandoval, LE van den Berg, M Heinke, CO Cohn, HN Lugger, PM Freire, P Anderson, J Serenelli, AM Althaus, LG Cool, AM Grindlay, JE Edmonds, PD Wijnands, R Ivanova, N AF Rivera-Sandoval, L. E. van den Berg, M. Heinke, C. O. Cohn, H. N. Lugger, P. M. Freire, P. Anderson, J. Serenelli, A. M. Althaus, L. G. Cool, A. M. Grindlay, J. E. Edmonds, P. D. Wijnands, R. Ivanova, N. TI Discovery of near-ultraviolet counterparts to millisecond pulsars in the globular cluster 47 Tucanae SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE pulsars: individual: PSR J0024-7204Q; pulsars: individual: PSR J0024-7204S; pulsars: individual: PSR J0024-7204T; pulsars: individual: PSR J0024-7203U; pulsars: individual: PSR J0024-7204Y; globular clusters: individual: 47 Tucanae ID X-RAY BINARIES; WHITE-DWARF STARS; SPACE-TELESCOPE COUNTERPARTS; LOW-MASS; GLOBULAR-CLUSTER-47 TUCANAE; NEUTRON-STAR; OPTICAL COUNTERPART; EXTENSIVE CENSUS; 47-TUCANAE; EVOLUTION AB We report the discovery of the likely white dwarf companions to radio millisecond pulsars 47 Tuc Q and 47 Tuc S in the globular cluster 47 Tucanae. These blue stars were found in near-ultraviolet images from the Hubble Space Telescope for which we derived accurate absolute astrometry, and are located at positions consistent with the radio coordinates to within 0.016 arcsec (0.2 sigma). We present near-ultraviolet and optical colours for the previously identified companion to millisecond pulsar 47 Tuc U, and we unambiguously confirm the tentative prior identifications of the optical counterparts to 47 Tuc T and 47 Tuc Y. For the latter, we present its radio-timing solution for the first time. We find that all five near-ultraviolet counterparts have U-300 - B-390 colours that are consistent with He white dwarf cooling models for masses similar to 0.16-0.3 M-circle dot and cooling ages within similar to 0.1-6 Gyr. The H alpha - R-625 colours of 47 Tuc U and 47 Tuc T indicate the presence of a strong H alpha absorption line, as expected for white dwarfs with an H envelope. C1 [Rivera-Sandoval, L. E.; van den Berg, M.; Wijnands, R.] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 XH Amsterdam, Netherlands. [van den Berg, M.; Grindlay, J. E.; Edmonds, P. D.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Heinke, C. O.; Ivanova, N.] Univ Alberta, Dept Phys, Edmonton, AB T6G 2E1, Canada. [Heinke, C. O.] Max Planck Inst Radio Astron, D-53121 Bonn, Germany. [Cohn, H. N.; Lugger, P. M.] Indiana Univ, Dept Astron, Bloomington, IN 47405 USA. [Anderson, J.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Serenelli, A. M.] Fac Ciencias, CSIC IEEC, Inst Ciencias Espacio, E-08193 Bellaterra, Spain. [Althaus, L. G.] Natl Univ La Plata, CONICET, Fac Ciencias Astron & Geofis, Inst Astrofis La Plata, RA-1900 La Plata, Buenos Aires, Argentina. [Cool, A. M.] San Francisco State Univ, Dept Phys & Astron, San Francisco, CA 94132 USA. RP Rivera-Sandoval, LE (reprint author), Univ Amsterdam, Astron Inst Anton Pannekoek, Sci Pk 904, NL-1098 XH Amsterdam, Netherlands. EM l.e.riverasandoval@uva.nl OI Serenelli, Aldo/0000-0001-6359-2769 FU CONACyT FX We appreciate the comments by the anonymous referee, which improved this work. LER-S acknowledges support from a CONACyT fellowship. We thank Dr. B. Lanzoni for pointing out minor mistakes in Table 2 in an earlier version of the paper. NR 56 TC 2 Z9 2 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 NOV 1 PY 2015 VL 453 IS 3 BP 2707 EP 2717 DI 10.1093/mnras/stv1810 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CU6NL UT WOS:000363649000038 ER PT J AU Loi, ST Murphy, T Bell, ME Kaplan, DL Lenc, E Offringa, AR Hurley-Walker, 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 Murphy, Tara Bell, Martin E. Kaplan, David L. Lenc, Emil Offringa, Andre R. Hurley-Walker, Natasha 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 Quantifying ionospheric effects on time-domain astrophysics with the Murchison Widefield Array SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE atmospheric effects; instrumentation: interferometers; radio continuum: general ID ATMOSPHERIC GRAVITY-WAVES; VLA RADIO INTERFEROMETER; SCATTER-BROADENED IMAGE; SQUARE KILOMETER ARRAY; SPREAD-F; SELF-CALIBRATION; SKY SURVEY; IRREGULARITIES; SCINTILLATION; PLASMASPHERE AB Refraction and diffraction of incoming radio waves by the ionosphere induce time variability in the angular positions, peak amplitudes and shapes of radio sources, potentially complicating the automated cross-matching and identification of transient and variable radio sources. In this work, we empirically assess the effects of the ionosphere on data taken by the Murchison Widefield Array (MWA) radio telescope. We directly examine 51 h of data observed over 10 nights under quiet geomagnetic conditions (global storm index K-p < 2), analysing the behaviour of short-time-scale angular position and peak flux density variations of around ten thousand unresolved sources. We find that while much of the variation in angular position can be attributed to ionospheric refraction, the characteristic displacements (10-20 arcsec) at 154 MHz are small enough that search radii of 1-2 arcmin should be sufficient for cross-matching under typical conditions. By examining bulk trends in amplitude variability, we place upper limits on the modulation index associated with ionospheric scintillation of 1-3 per cent for the various nights. For sources fainter than similar to 1 Jy, this variation is below the image noise at typical MWA sensitivities. Our results demonstrate that the ionosphere is not a significant impediment to the goals of time-domain science with the MWA at 154 MHz. C1 [Loi, Shyeh Tjing; Murphy, Tara; Lenc, Emil; Gaensler, B. M.] Univ Sydney, Sch Phys, Sydney Inst Astron, Sydney, NSW 2006, Australia. [Loi, Shyeh Tjing; Murphy, Tara; Bell, Martin E.; Lenc, Emil; Offringa, Andre R.; Mitchell, D. A.; Ord, S. M.; Subrahmanyan, R.; Tingay, S. J.; Wayth, R. B.; Webster, R. L.] ARC Ctr Excellence All Sky Astrophys CAASTRO, Redfern, NSW 2016, Australia. [Bell, Martin E.; Mitchell, D. A.] CSIRO Astron & Space Sci CASS, Epping, NSW 1710, Australia. [Kaplan, David L.] Univ Wisconsin, Dept Phys, Milwaukee, WI 53201 USA. [Offringa, Andre R.; Briggs, F.; Waterson, M.] Australian Natl Univ, Res Sch Astron & Astrophys, Weston, ACT 2611, Australia. [Offringa, Andre R.] Netherlands Inst Radio Astron ASTRON, NL-7990 AA Dwingeloo, Netherlands. [Hurley-Walker, Natasha; Emrich, D.; Lynch, M. J.; Ord, S. M.; Tingay, S. J.; Waterson, M.; Wayth, R. B.; Williams, A.] Curtin Univ, Int Ctr Radio Astron Res, Bentley, WA 6102, Australia. [Bernardi, G.] Sq Kilometre Array South Africa, ZA-7405 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 85287 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 M5S 3H4, Canada. [Goeke, R.; Williams, C. L.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [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. [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 411007, Maharashtra, India. [Roshi, A.] Natl Radio Astron Observ, Charlottesville, VA 22903 USA. [Roshi, A.] Natl Radio Astron Observ, Greenbank, VA 22903 USA. [Webster, R. L.] Univ Melbourne, Sch Phys, Parkville, Vic 3010, Australia. RP Loi, ST (reprint author), Univ Sydney, Sch Phys, Sydney Inst Astron, Sydney, NSW 2006, Australia. EM sloi5113@uni.sydney.edu.au; tara@physics.usyd.edu.au RI Wayth, Randall/B-2444-2013; Hurley-Walker, Natasha/B-9520-2013; Emrich, David/B-7002-2013; Udayashankar , N/D-4901-2012; Subrahmanyan, Ravi/D-4889-2012; M, Manjunath/N-4000-2014; Deshpande, Avinash/D-4868-2012; OI 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; Loi, Shyeh Tjing/0000-0002-6528-4548; Murphy, Tara/0000-0002-2686-438X; Gaensler, Bryan/0000-0002-3382-9558; Lenc, Emil/0000-0002-9994-1593 FU US National Science Foundation [AST-0457585, PHY-0835713, CAREER-0847753, AST-0908884, AST-1412421]; 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 from the New Zealand Ministry of Economic Development [MED-E1799]; Victoria University of Wellington from IBM Shared University Research Grant; 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 We thank J.-P. Macquart and J. Morgan for useful discussions. 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 US National Science Foundation (grants AST-0457585, PHY-0835713, CAREER-0847753, AST-0908884 and AST-1412421), 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 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 90 TC 12 Z9 12 U1 2 U2 9 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 NOV 1 PY 2015 VL 453 IS 3 BP 2731 EP 2746 DI 10.1093/mnras/stv1808 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CU6NL UT WOS:000363649000040 ER PT J AU Sadowski, A Narayan, R AF Sadowski, Aleksander Narayan, Ramesh TI Powerful radiative jets in supercritical accretion discs around non-spinning black holes SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE accretion, accretion discs; black hole physics; relativistic processes; galaxies: jets; X-rays: individual: Sw J1644+57; X-rays: individual: SS433; X-rays: ULX ID TIDAL DISRUPTION EVENT; X-RAY SOURCES; RELATIVISTIC MAGNETOHYDRODYNAMIC SIMULATIONS; SUPER-EDDINGTON ACCRETION; THICK ACCRETION; NUMERICAL SIMULATIONS; GENERAL-RELATIVITY; PARTICLE BEAMS; FLUID DISKS; M1 CLOSURE AB We describe a set of simulations of supercritical accretion on to a non-rotating supermassive black hole (BH). The accretion flow takes the form of a geometrically thick disc with twin low-density funnels around the rotation axis. For accretion rates greater than or similar to 10. M-Edd, there is sufficient gas in the funnel to make this region optically thick. Radiation from the disc first flows into the funnel, after which it accelerates the optically thick funnel gas along the axis. The resulting jet is baryon loaded and has a terminal density-weighted velocity approximate to 0.3c. Much of the radiative luminosity is converted into kinetic energy by the time the escaping gas becomes optically thin. These jets are not powered by BHrotation or magnetic driving, but purely by radiation. Their characteristic beaming angle is similar to 0.2 rad. For an observer viewing down the axis, the isotropic equivalent luminosity of total energy is as much as 10(48) erg s(-1) for a 10(7) M-circle dot BH accreting at 10(3) Eddington. Therefore, energetically, the simulated jets are consistent with observations of the most powerful tidal disruption events, e.g. Swift J1644. The jet velocity is, however, too low to match the Lorentz factor gamma > 2 inferred in J1644. There is no such conflict in the case of other tidal disruption events. Since favourably oriented observers see isotropic equivalent luminosities that are highly super-Eddington, the simulated models can explain observations of ultraluminous X-ray sources, at least in terms of luminosity and energetics, without requiring intermediate-mass BHs. C1 [Sadowski, Aleksander] MIT Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Narayan, Ramesh] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02134 USA. RP Sadowski, A (reprint author), MIT Kavli Inst Astrophys & Space Res, 77 Massachusetts Ave, Cambridge, MA 02139 USA. EM asadowsk@mit.edu OI Narayan, Ramesh/0000-0002-1919-2730 FU NASA through Einstein Postdoctotral Fellowship - Chandra X-ray Center under NASA [PF4-150126, NAS8-03060]; NSF [AST1312651]; NASA [TCAN NNX14AB47G]; NSF via XSEDE [TG-AST080026N] FX The authors thank Marek Abramowicz, James Guillochon, Herman Marshall, Tsvi Piran, Nir Shaviv and Rashid Sunyaev for helpful discussions. AS acknowledges support for this work from NASA through Einstein Postdoctotral Fellowship number PF4-150126 awarded by the Chandra X-ray Center, which is operated by the Smithsonian Astrophysical Observatory for NASA under contract NAS8-03060. AS thanks Harvard-Smithsonian Center for Astrophysics for hospitality. RN was supported in part by NSF grant AST1312651 and NASA grant TCAN NNX14AB47G. The authors acknowledge computational support from NSF via XSEDE resources (grant TG-AST080026N), and from NASA via the High-End Computing (HEC) Program through the NASA Advanced Supercomputing (NAS) Division at Ames Research Center. NR 57 TC 20 Z9 20 U1 0 U2 1 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD NOV 1 PY 2015 VL 453 IS 3 BP 3213 EP 3221 DI 10.1093/mnras/stv1802 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CU6NL UT WOS:000363649000077 ER PT J AU Plewa, PM Gillessen, S Eisenhauer, F Ott, T Pfuhl, O George, E Dexter, J Habibi, M Genzel, R Reid, MJ Menten, KM AF Plewa, P. M. Gillessen, S. Eisenhauer, F. Ott, T. Pfuhl, O. George, E. Dexter, J. Habibi, M. Genzel, R. Reid, M. J. Menten, K. M. TI Pinpointing the near-infrared location of Sgr A* by correcting optical distortion in the NACO imager SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE methods: data analysis; techniques: high angular resolution; astrometry; Galaxy: centre; infrared: stars ID SUPERMASSIVE BLACK-HOLE; ORTHONORMAL VECTOR POLYNOMIALS; GALACTIC-CENTER; PROPER MOTIONS; STELLAR ORBITS; UNIT-CIRCLE; BASIS-SET; STARS; ASTROMETRY; TELESCOPE AB Near-infrared observations of stellar orbits at the Galactic Center provide conclusive evidence for a massive black hole associated with the compact radio source Sgr A*. The astrometric reference frame for these observations is tied to a set of red giant stars, which are also detectable at radio wavelengths through SiO maser emission in their envelopes. We have improved the precision and long-term stability of this reference frame, in which Sgr A* is localized to within a factor 5 better than previously: similar to 0.17 mas in position (in 2009) and similar to 0.07 mas yr(-1) in velocity. This improvement is the result of modelling and correcting optical distortion in the VLT/NACO imager to a submas level and including new infrared and radio measurements, which now both span more than a decade in time. A further improvement will follow future observations and facilitate the detection of relativistic orbital effects. C1 [Plewa, P. M.; Gillessen, S.; Eisenhauer, F.; Ott, T.; Pfuhl, O.; George, E.; Dexter, J.; Habibi, M.; Genzel, R.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Genzel, R.] Univ Calif Berkeley, Dept Phys & Astron, Berkeley, CA 94720 USA. [Reid, M. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Menten, K. M.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. RP Plewa, PM (reprint author), Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. EM pmplewa@mpe.mpg.de; ste@mpe.mpg.de NR 35 TC 2 Z9 2 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 NOV 1 PY 2015 VL 453 IS 3 BP 3234 EP 3244 DI 10.1093/mnras/stv1910 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CU6NL UT WOS:000363649000079 ER PT J AU O'Connor, S Solazzo, C Collins, M AF O'Connor, Sonia Solazzo, Caroline Collins, Matthew TI Advances in identifying archaeological traces of horn and other keratinous hard tissues SO STUDIES IN CONSERVATION LA English DT Article DE Horn; Hoof; Baleen; Tortoiseshell; Mineral preservation; Keratin; Peptide mass fingerprint; Mass spectrometry ID FLIGHT MASS-SPECTROMETRY; SPECIES IDENTIFICATION; HAIR SHAFTS; ALPHA-KERATIN; WHALE BALEEN; TURTLE SHELL; SEA-TURTLE; EVOLUTION; PROTEINS; BONE AB Despite being widely utilized in the production of cultural objects, keratinous hard tissues, such as horn, baleen, and tortoiseshell, rarely survive in archaeological contexts unless factors combine to inhibit biodeterioration. Even when these materials do survive, working, use, and diagenetic changes combine to make identification difficult. This paper reviews the chemistry and deterioration of keratin and past approaches to the identification of keratinous archaeological remains. It describes the formation of horn, hoof, baleen, and tortoiseshell and demonstrates how identification can be achieved by combining visual observation under low-power magnification with an understanding of the structure and characteristic deterioration of these materials. It also demonstrates how peptide mass fingerprinting of the keratin can be used to identify keratinous tissues, often to species, even when recognizable structural information has not survived. C1 [O'Connor, Sonia] Univ Bradford, Div AGES, Archaeol Sci, Bradford BD7 1DP, W Yorkshire, England. [Solazzo, Caroline; Collins, Matthew] Univ York, Dept Archaeol, BioArCh, York YO10 5DD, N Yorkshire, England. [Solazzo, Caroline] Smithsonian Inst, Museum Conservat Inst, Suitland, MD USA. RP O'Connor, S (reprint author), Univ Bradford, Div AGES, Archaeol Sci, Bradford BD7 1DP, W Yorkshire, England. EM s.oconnor@bradford.ac.uk RI Collins, Matthew/A-7534-2008 OI Collins, Matthew/0000-0003-4226-5501 FU Arts and Humanities Research Council; Engineering and Physical Sciences Research Council; University of York, UK [FP7-PEOPLE-IOF-GA-2009-236425]; AgResearch, NZ [FP7-PEOPLE-IOF-GA-2009-236425]; Smithsonian's Museum Conservation Institute (MCI); Science City York and Yorkshire Forward from the Northern Way Initiative FX We thank Cluny Chapman, the Hawley Collection, the Horniman Museum, Hull Museums, Leeds Museum and Galleries, and the York Archaeological Trust for access to the specimens used in this paper. Other than Fig. 1, for which we thank the Canadian Conservation Institute, all photographs are by O'Connor and all analytical graphics are by Solazzo. The research by O'Connor to evaluate and develop techniques for the identification of keratinous hard tissues was undertaken as part of her post-doctoral fellowship, Cultural Objects Worked in Skeletal Hard Tissues, funded by the Arts and Humanities Research Council and the Engineering and Physical Sciences Research Council, through their Science and Heritage Programme. Solazzo's work was supported by a Marie Curie International Outgoing Fellowship (FP7-PEOPLE-IOF-GA-2009-236425, THREADs) jointly between University of York, UK, and AgResearch, NZ (2009-2012), and a Smithsonian's Museum Conservation Institute (MCI) post-doctoral grant. Analyses were carried out at The Centre of Excellence in Mass Spectrometry, University of York, supported by Science City York and Yorkshire Forward, using funds from the Northern Way Initiative. We particularly thank Dr. David Ashford for carrying out analyses on the maXis instrument. NR 104 TC 0 Z9 0 U1 2 U2 13 PU ROUTLEDGE JOURNALS, TAYLOR & FRANCIS LTD PI ABINGDON PA 4 PARK SQUARE, MILTON PARK, ABINGDON OX14 4RN, OXFORDSHIRE, ENGLAND SN 0039-3630 EI 2047-0584 J9 STUD CONSERV JI Stud. Conserv. PD NOV PY 2015 VL 60 IS 6 BP 393 EP 417 DI 10.1179/2047058414Y.0000000134 PG 25 WC Archaeology; Art; Chemistry, Applied; Chemistry, Analytical; Spectroscopy SC Archaeology; Art; Chemistry; Spectroscopy GA CV4GI UT WOS:000364224600007 ER PT J AU Barry, KE Schnitzer, SA van Breugel, M Hall, JS AF Barry, Kathryn E. Schnitzer, Stefan A. van Breugel, Michiel Hall, Jefferson S. TI Rapid Liana Colonization along a Secondary Forest Chronosequence SO BIOTROPICA LA English DT Article DE Agua Salud; lianas; Panama; species diversity; succession; tropical forests; woody vines ID SELF-SUPPORTING PLANTS; BARRO-COLORADO ISLAND; TROPICAL WET FOREST; TREE REGENERATION; BASAL AREA; PANAMA; DIVERSITY; ABUNDANCE; GROWTH; SUCCESSION AB Lianas (woody vines) can have profound effects on tree recruitment, growth, survival, and diversity in tropical forests. However, the dynamics of liana colonization soon after land abandonment are poorly understood, and thus it is unknown whether lianas alter tree regeneration early in succession. We examined the liana community in 43 forests that ranged from 1 to 31yr old in central Panama to determine how fast lianas colonize young forests and how the liana community changes with forest succession. We found that lianas reached high densities early in succession, commonly exceeding 1000 stems/ha within the first 5yr of forest regeneration. Lianas also increased rapidly during early succession in terms of basal area but did not show evidence of saturation within the 30yr of our chronosequence. The relative contribution of lianas to total woody plant community in terms of basal area and density increased rapidly and reached a saturation point within 5yr (basal area) to 15yr (density) after land abandonment. Our data demonstrate that lianas recruit early and in high density in tropical forest regeneration, and thus lianas may have a large effect on the way in which secondary forests develop both early and throughout succession. C1 [Barry, Kathryn E.] Univ Wisconsin, Dept Biol Sci, Milwaukee, WI 53201 USA. [Schnitzer, Stefan A.] Marquette Univ, Dept Biol Sci, Milwaukee, WI 53201 USA. [Schnitzer, Stefan A.; van Breugel, Michiel; Hall, Jefferson S.] Smithsonian Trop Res Inst, Panama City, Panama. [van Breugel, Michiel] Yale NUS Coll, Singapore 138527, Singapore. [van Breugel, Michiel] Natl Univ Singapore, Dept Biol Sci, Singapore 117543, Singapore. RP Barry, KE (reprint author), Univ Wisconsin, Dept Biol Sci, POB 413, Milwaukee, WI 53201 USA. EM kebarry@uwm.edu OI van Breugel, Michiel/0000-0003-2778-7803 FU ForestGeo of the Smithsonian Global Earth Observatory (SIGEO); NSF [DEB-0845071]; University of Wisconsin-Milwaukee; HSBC Climate Partnership; Smithsonian Tropical Research Institute (STRI); University of Wisconsin-Milwaukee Department of Biological Sciences; Center for Latin American and Caribbean Studies; STRI FX We thank Saara DeWalt, Susan Letcher, and two anonymous reviewers for helpful comments on this manuscript. We are grateful to Mario Bailon and Andres Hernandez for botanical identifications, Anabel Rivas, Miguel Nunez, Johana Balbuena, Guillermo Fernandez, Carlos Diaz, Julia Gonzalez, and a series of interns for their help in inventory work and data entry, as well as Daniela Weber and Federico Davis for their role in project and site management. Funding was provided by ForestGeo of the Smithsonian Global Earth Observatory (SIGEO), NSF DEB-0845071, a Research Growth Initiative grant from the University of Wisconsin-Milwaukee, HSBC Climate Partnership, and the Smithsonian Tropical Research Institute (STRI). Funding for travel for KEB was provided by the University of Wisconsin-Milwaukee Department of Biological Sciences, the Center for Latin American and Caribbean Studies, and a STRI short-term Fellowship. The Agua Salud project is part of the Smithsonian Institution's Forest Global Earth Observatories (ForestGEO), and is a collaboration between STRI, the Panama Canal Authority, the National Environmental Authority of Panama, and other Institutions. NR 52 TC 3 Z9 3 U1 4 U2 16 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0006-3606 EI 1744-7429 J9 BIOTROPICA JI Biotropica PD NOV PY 2015 VL 47 IS 6 BP 672 EP 680 DI 10.1111/btp.12259 PG 9 WC Ecology SC Environmental Sciences & Ecology GA CU8RC UT WOS:000363809800005 ER PT J AU Powell, LL Zurita, G Wolfe, JD Johnson, EI Stouffer, PC AF Powell, Luke L. Zurita, Gustavo Wolfe, Jared D. Johnson, Erik I. Stouffer, Philip C. TI Changes in Habitat Use at Rain Forest Edges Through Succession: a Case Study of Understory Birds in the Brazilian Amazon SO BIOTROPICA LA English DT Article DE antthrush; continuous edge response; fragmentation; Neotropical birds; secondary forest; terrestrial insectivores; woodcreeper ID TERRESTRIAL INSECTIVOROUS BIRDS; SECONDARY FORESTS; ATLANTIC FOREST; FRAGMENTS; MOVEMENT AB Primary tropical rain forests are being rapidly perforated with new edges via roads, logging, and pastures, and vast areas of secondary forest accumulate following abandonment of agricultural lands. To determine how insectivorous Amazonian understory birds respond to edges between primary rain forest and three age classes of secondary forest, we radio-tracked two woodcreepers (Glyphorynchus spirurus, N=17; Xiphorhynchus pardalotus, N=18) and a terrestrial antthrush (Formicarius colma, N=19). We modeled species-specific response to distance to forest edge (a continuous variable) based on observations at varying distances from the primary-secondary forest interface. All species avoided 8-14-yr-old secondary forest. Glyphorynchus spirurus and F.colma mostly remained within primary forest <100m from the young edge. Young F.colma rarely penetrated >100m into secondary forest 27-31yr old. Young Formicarius colma and most G.spirurus showed a unimodal response to 8-14-yr-old secondary forest, with relative activity concentrated just inside primary forest. After land abandonment, G.spirurus was the first to recover to the point where there was no detectable edge response (after 11-14yr), whereas X.pardalotus was intermediate (15-20yr), and F. colma last (28-30yr +). Given the relatively quick recovery by our woodcreeper species, new legislation on protection of secondary forests >20-yr old in Brazil's Para state may represent a new opportunity for conservation and management; however, secondary forest must mature to at least 30yr before the full compliment of rain forest-dependent species can use secondary forest without adverse edge effects. C1 [Powell, Luke L.; Wolfe, Jared D.; Johnson, Erik I.; Stouffer, Philip C.] Louisiana State Univ, 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. [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.] Natl Zool Pk, Smithsonian Migratory Bird Ctr, Washington, DC 20013 USA. [Zurita, Gustavo] Univ Nacl Misiones, Fac Ciencias Forestales, CONICET, Inst Biol Subtrop, RA-3370 Puerto Iguazu, Misiones, Argentina. [Wolfe, Jared D.] US Forest Serv, Redwood Sci Lab, USDA, Pacific Southwest Res Stn, Arcata, CA 95521 USA. [Johnson, Erik I.] Natl Audubon Soc, Baton Rouge, LA 70808 USA. RP Powell, LL (reprint author), Louisiana State Univ, Sch Renewable Nat Resources, RNR 227, Baton Rouge, LA 70803 USA. EM luke.l.powell@gmail.com FU US National Science Foundation [LTREB 0545491]; AOU's Research Award; Frank M. Chapman Award; Paul A. Stewart Award; 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, Kyle Harms, Michael Kaller, Curtis Marantz, James Nichols, Stefan Woltmann, and J. Van Remsen contributed insightful reviews and advice on data analyses. We thank the following funding sources: US National Science Foundation (LTREB 0545491), AOU's Research Award, the Frank M. Chapman Award, the Paul A. Stewart Award, and the Lewis & Clark Fund. We conducted this research under LSU IACUC approval and under applicable Brazilian permits. This is publication number 668 in the BDFFP technical series and number 39 in the Amazonian ornithology technical series. This manuscript was approved for publication by the Director of the Louisiana Agricultural Experimental Station as manuscript number 2015-241-22456. NR 55 TC 3 Z9 3 U1 12 U2 43 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0006-3606 EI 1744-7429 J9 BIOTROPICA JI Biotropica PD NOV PY 2015 VL 47 IS 6 BP 723 EP 732 DI 10.1111/btp.12253 PG 10 WC Ecology SC Environmental Sciences & Ecology GA CU8RC UT WOS:000363809800010 ER PT J AU Salisbury, CL Potvin, C AF Salisbury, Claire L. Potvin, Catherine TI Does Tree Species Composition Affect Productivity in a Tropical Planted Forest? (vol 47, pg 559, 2015) SO BIOTROPICA LA English DT Correction C1 [Salisbury, Claire L.; Potvin, Catherine] McGill Univ, Dept Biol, Montreal, PQ H3A 1B1, Canada. [Potvin, Catherine] Smithsonian Trop Res Inst, Panama City, Panama. RP Salisbury, CL (reprint author), McGill Univ, Dept Biol, 1205 Ave Docteur Penfield, Montreal, PQ H3A 1B1, Canada. NR 2 TC 0 Z9 0 U1 2 U2 9 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0006-3606 EI 1744-7429 J9 BIOTROPICA JI Biotropica PD NOV PY 2015 VL 47 IS 6 BP 783 EP 783 DI 10.1111/btp.12289 PG 1 WC Ecology SC Environmental Sciences & Ecology GA CU8RC UT WOS:000363809800015 ER PT J AU Wen, J Ickert-Bond, SM Appelhans, MS Dorr, LJ Funk, VA AF Wen, Jun Ickert-Bond, Stefanie M. Appelhans, Marc S. Dorr, Laurence J. Funk, Vicki A. TI Collections-based systematics: Opportunities and outlook for 2050 SO JOURNAL OF SYSTEMATICS AND EVOLUTION LA English DT Review DE Biodiversity CyberBank; collections-based systematics; e-monograph; Systematics Agenda 2050; World Organization of Systematic Biology ID INTERNATIONAL BOTANICAL CONGRESS; NATURAL-HISTORY COLLECTIONS; HERBARIUM SPECIMENS; CLIMATE-CHANGE; BIOLOGICAL COLLECTIONS; BIODIVERSITY; DIGITIZATION; BIOSPHERE; TAXONOMY; PUBLICATION AB Systematic biology is a discipline rooted in collections. These collections play important roles in research and conservation and are integral to our efforts to educate society about biodiversity and conservation. Collections provide an invaluable record of the distribution of organisms throughout the world and through recent and geological time, and they are the only direct documentation of the biological, physical, and cultural diversity of the planet: past, present, and future. Recent developments in bioinformatics and cyberinfrastructure are transforming systematics by opening up new opportunities and as a result major digitization efforts have increasingly made available large amounts of biodiversity data. The collections-based systematics community needs to train the next-generation of systematists with integrative skills, address grand questions about biodiversity at different scales, develop a community-wide cyberinfrastructure, effectively disseminate systematic data to biologists and the public, and proactively educate the public and policy makers on the importance of systematics and collections in the biodiversity crisis of the Anthropocene. Specifically, we call for a new global Biodiversity CyberBank, comparable to GenBank for genetic data, to be the repository of all biodiversity data, as well as a World Organization of Systematic Biology to lead major initiatives of the field. We also outline a new workflow for taxonomic monographs, which utilizes both the traditional strengths of synthesizing diverse collections-based taxonomic data and the capacity of online resources and bioinformatics tools. C1 [Wen, Jun; Appelhans, Marc S.; Dorr, Laurence J.; Funk, Vicki A.] Smithsonian Inst, Dept Bot, Washington, DC 20013 USA. [Ickert-Bond, Stefanie M.] Univ Alaska Fairbanks, UA Museum North, Fairbanks, AK 99775 USA. [Ickert-Bond, Stefanie M.] Univ Alaska Fairbanks, Dept Biol & Wildlife, Fairbanks, AK 99775 USA. [Appelhans, Marc S.] Univ Gottingen, Dept Systemat Biodivers & Evolut Plants, Albrecht von Haller Inst Plant Sci, D-37073 Gottingen, Germany. RP Wen, J (reprint author), Smithsonian Inst, Dept Bot, MRC 166,POB 37012, Washington, DC 20013 USA. EM wenj@si.edu RI Ickert-Bond, Stefanie/B-3216-2012 OI Ickert-Bond, Stefanie/0000-0001-8198-8898 NR 83 TC 10 Z9 10 U1 6 U2 36 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1674-4918 EI 1759-6831 J9 J SYST EVOL JI J. Syst. Evol. PD NOV PY 2015 VL 53 IS 6 BP 477 EP 488 DI 10.1111/jse.12181 PG 12 WC Plant Sciences SC Plant Sciences GA CU9OJ UT WOS:000363873600001 ER PT J AU Scharler, UM Ulanowicz, RE Fogel, ML Wooller, MJ Jacobson-Meyers, ME Lovelock, CE Feller, IC Frischer, M Lee, R McKee, K Romero, IC Schmit, JP Shearer, C AF Scharler, U. M. Ulanowicz, R. E. Fogel, M. L. Wooller, M. J. Jacobson-Meyers, M. E. Lovelock, C. E. Feller, I. C. Frischer, M. Lee, R. McKee, K. Romero, I. C. Schmit, J. P. Shearer, C. TI Variable nutrient stoichiometry (carbon:nitrogen:phosphorus) across trophic levels determines community and ecosystem properties in an oligotrophic mangrove system SO OECOLOGIA LA English DT Article DE Oligotrophic environment; Recycling; Nutrient limitation; Mangrove food web; Transfer efficiency ID WOOD-BORING INSECTS; ECOLOGICAL STOICHIOMETRY; FRESH-WATER; ORGANIC-CARBON; RED MANGROVE; NITROGEN; BELIZE; HERBIVORY; FOREST; SEA AB Our study investigated the carbon:nitrogen:phosphorus (C:N:P) stoichiometry of mangrove island of the Mesoamerican Barrier Reef (Twin Cays, Belize). The C:N:P of abiotic and biotic components of this oligotrophic ecosystem was measured and served to build networks of nutrient flows for three distinct mangrove forest zones (tall seaward fringing forest, inland dwarf forests and a transitional zone). Between forest zones, the stoichiometry of primary producers, heterotrophs and abiotic components did not change significantly, but there was a significant difference in C:N:P, and C, N, and P biomass, between the functional groups mangrove trees, other primary producers, heterotrophs, and abiotic components. C:N:P decreased with increasing trophic level. Nutrient recycling in the food webs was highest for P, and high transfer efficiencies between trophic levels of P and N also indicated an overall shortage of these nutrients when compared to C. Heterotrophs were sometimes, but not always, limited by the same nutrient as the primary producers. Mangrove trees and the primary tree consumers were P limited, whereas the invertebrates consuming leaf litter and detritus were N limited. Most compartments were limited by P or N (not by C), and the relative depletion rate of food sources was fastest for P. P transfers thus constituted a bottleneck of nutrient transfer on Twin Cays. This is the first comprehensive ecosystem study of nutrient transfers in a mangrove ecosystem, illustrating some mechanisms (e.g. recycling rates, transfer efficiencies) which oligotrophic systems use in order to build up biomass and food webs spanning various trophic levels. C1 [Scharler, U. M.] Univ KwaZulu Natal, Sch Life Sci, ZA-4001 Durban, South Africa. [Ulanowicz, R. E.] Univ Florida, Dept Biol, Arthur R Marshall Lab, Gainesville, FL 32611 USA. [Ulanowicz, R. E.] Univ Maryland, Ctr Environm Sci, Chesapeake Biol Lab, Solomons, MD 20688 USA. [Fogel, M. L.] Carnegie Inst Sci, Geophys Lab, Washington, DC 20015 USA. [Fogel, M. L.] Univ Calif Merced, Sch Nat Sci, Merced, CA 95343 USA. [Wooller, M. J.] Univ Alaska Fairbanks, Inst Marine Sci, Sch Fisheries & Ocean Sci, Fairbanks, AK 99775 USA. [Wooller, M. J.] Univ Alaska Fairbanks, Alaska Stable Isotope Facil, Water & Environm Res Ctr, Fairbanks, AK 99775 USA. [Jacobson-Meyers, M. E.] Univ So Calif, Dana & David Dornsife Coll Letters, Arts & Sci, Los Angeles, CA 90089 USA. [Lovelock, C. E.] Univ Queensland, Sch Biol Sci, Brisbane, Qld 4072, Australia. [Feller, I. C.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. [Frischer, M.] Skidaway Inst Oceanog, Savannah, GA 31411 USA. [Lee, R.] Univ So Calif, Ctr Dark Energy Biosphere Invest, AHF 209, Los Angeles, CA 90089 USA. [McKee, K.] US Geol Survey, Natl Wetlands Res Ctr, Lafayette, LA 70506 USA. [Romero, I. C.] Univ S Florida, Coll Marine Sci, St Petersburg, FL 33701 USA. [Schmit, J. P.] Natl Pk Serv, Natl Capital Reg Inventory & Monitoring Network, Washington, DC 20007 USA. [Shearer, C.] Univ Illinois, Dept Plant Biol, Urbana, IL 61801 USA. RP Scharler, UM (reprint author), Univ KwaZulu Natal, Sch Life Sci, Westville Campus, ZA-4001 Durban, South Africa. EM scharler@ukzn.ac.za RI Lovelock, Catherine/G-7370-2012; McKee, Karen/D-1365-2014; OI Lovelock, Catherine/0000-0002-2219-6855; McKee, Karen/0000-0001-7042-670X; Wooller, Matthew/0000-0002-5065-4235; Feller, Ilka/0000-0002-6391-1608 FU US-National Science Foundation Biocomplexity grant [DEB-998 1483]; Smithsonian Institution's Loeb Fellowship; Carnegie Institution of Washington FX Funding for this study was provided by a US-National Science Foundation Biocomplexity grant (DEB-998 1483). Fieldwork was conducted on the Carrie Bow Cay field station of the Smithsonian Institute. M. Carpenter and A. Chamberlain, Q. Roberts, V. Brenneis, B. Smallwood and D. Thornton are gratefully acknowledged for assistance in the field. Q. Roberts, V. Brenneis and P. Zelanko helped with C and N elemental analysis at the Geophysical Laboratory, Carnegie institution of Washington. M. F. and M. J. W. gratefully acknowledge support from the Smithsonian Institution's Loeb Fellowship and the Carnegie Institution of Washington, M. E. J. M. gratefully acknowledges the laboratory of D. Capone for material and instrumental support. Any use of trade, product, or firm names is for descriptive purposes only and does not imply endorsement by the US government. NR 76 TC 4 Z9 4 U1 10 U2 57 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0029-8549 EI 1432-1939 J9 OECOLOGIA JI Oecologia PD NOV PY 2015 VL 179 IS 3 BP 863 EP 876 DI 10.1007/s00442-015-3379-2 PG 14 WC Ecology SC Environmental Sciences & Ecology GA CU5GK UT WOS:000363559800023 PM 26183835 ER PT J AU Baggett, LP Powers, SP Brumbaugh, RD Coen, LD DeAngelis, BM Greene, JK Hancock, BT Morlock, SM Allen, BL Breitburg, DL Bushek, D Grabowski, JH Grizzle, RE Grosholz, ED La Peyre, MK Luckenbach, MW McGraw, KA Piehler, MF Westby, SR Ermgassen, PSEZ AF Baggett, Lesley P. Powers, Sean P. Brumbaugh, Robert D. Coen, Loren D. DeAngelis, Bryan M. Greene, Jennifer K. Hancock, Boze T. Morlock, Summer M. Allen, Brian L. Breitburg, Denise L. Bushek, David Grabowski, Jonathan H. Grizzle, Raymond E. Grosholz, Edwin D. La Peyre, Megan K. Luckenbach, Mark W. McGraw, Kay A. Piehler, Michael F. Westby, Stephanie R. Ermgassen, Philine S. E. Zu TI Guidelines for evaluating performance of oyster habitat restoration SO RESTORATION ECOLOGY LA English DT Review DE Crassostrea virginica; criteria; eastern oyster; ecosystem services; monitoring; Olympia oyster; Ostrea lurida; reefs ID SUSPENSION-FEEDING BIVALVES; REEF RESTORATION; CRASSOSTREA-VIRGINICA; CHESAPEAKE BAY; SEAGRASS; ECOSYSTEM; ECOLOGY; MARSH; SHELL; STABILIZATION AB Restoration of degraded ecosystems is an important societal goal, yet inadequate monitoring and the absence of clear performance metrics are common criticisms of many habitat restoration projects. Funding limitations can prevent adequate monitoring, but we suggest that the lack of accepted metrics to address the diversity of restoration objectives also presents a serious challenge to the monitoring of restoration projects. A working group with experience in designing and monitoring oyster reef projects was used to develop standardized monitoring metrics, units, and performance criteria that would allow for comparison among restoration sites and projects of various construction types. A set of four universal metrics (reef areal dimensions, reef height, oyster density, and oyster size-frequency distribution) and a set of three universal environmental variables (water temperature, salinity, and dissolved oxygen) are recommended to be monitored for all oyster habitat restoration projects regardless of their goal(s). In addition, restoration goal-based metrics specific to four commonly cited ecosystem service-based restoration goals are recommended, along with an optional set of seven supplemental ancillary metrics that could provide information useful to the interpretation of prerestoration and postrestoration monitoring data. Widespread adoption of a common set of metrics with standardized techniques and units to assess well-defined goals not only allows practitioners to gauge the performance of their own projects but also allows for comparison among projects, which is both essential to the advancement of the field of oyster restoration and can provide new knowledge about the structure and ecological function of oyster reef ecosystems. C1 [Baggett, Lesley P.; Powers, Sean P.] Univ S Alabama, Mobile, AL 36688 USA. [Baggett, Lesley P.; Powers, Sean P.] Dauphin Isl Sea Lab, Dauphin Isl, AL USA. [Brumbaugh, Robert D.] Nature Conservancy, Big Pine Key, FL USA. [Coen, Loren D.] Florida Atlantic Univ, Dept Biol Sci, Ft Pierce, FL USA. [Coen, Loren D.] Florida Atlantic Univ, Harbor Branch Oceanog Inst, Ft Pierce, FL USA. [DeAngelis, Bryan M.; Hancock, Boze T.] Nature Conservancy, URI Grad Sch Oceanog, Narragansett, RI USA. [Greene, Jennifer K.] Nature Conservancy, Arlington, VA USA. [Morlock, Summer M.; McGraw, Kay A.; Westby, Stephanie R.] NOAA, Silver Spring, MD USA. [Allen, Brian L.] Puget Sound Restorat Fund, Bainbridge Isl, WA USA. [Breitburg, Denise L.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. [Bushek, David] Rutgers State Univ, Haskin Shellfish Res Lab, Point Norris, NJ USA. [Grabowski, Jonathan H.] Northeastern Univ, Boston, MA 02115 USA. [Grizzle, Raymond E.] Univ New Hampshire, Jackson Estuarine Lab, Durham, NH 03824 USA. [Grosholz, Edwin D.] Univ Calif Davis, Davis, CA 95616 USA. [La Peyre, Megan K.] Louisiana State Univ AgCtr, Sch Renewable Nat Resources, Louisiana Cooperat Fish & Wildlife Res Unit, US Geol Survey, Baton Rouge, LA USA. [Luckenbach, Mark W.] Virginia Inst Marine Sci, Coll William & Mary, Gloucester Point, VA 23062 USA. [Piehler, Michael F.] Univ N Carolina, Inst Marine Sci, Moorehead City, NC USA. [Ermgassen, Philine S. E. Zu] Univ Cambridge, Cambridge, England. RP Baggett, LP (reprint author), Univ S Alabama, Mobile, AL 36688 USA. EM lbaggett@umobile.edu NR 60 TC 8 Z9 8 U1 17 U2 67 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1061-2971 EI 1526-100X J9 RESTOR ECOL JI Restor. Ecol. PD NOV PY 2015 VL 23 IS 6 BP 737 EP 745 DI 10.1111/rec.12262 PG 9 WC Ecology SC Environmental Sciences & Ecology GA CU6VA UT WOS:000363671300003 ER PT J AU Crofoot, MC Farine, DR Strandburg-Peshkin, A Brugere, I Li, J Berger-Wolf, TY AF Crofoot, M. C. Farine, D. R. Strandburg-Peshkin, A. Brugere, I. Li, J. Berger-Wolf, T. Y. TI COLLECTIVE MOVEMENT IN SOCIALLY AND ENVIRONMENTALLY HETEROGENEOUS SYSTEMS: A CASE STUDY IN OLIVE BABOONS SO AMERICAN JOURNAL OF PRIMATOLOGY LA English DT Meeting Abstract CT 38th Annual Meeting of the American-Society-of-Primatologists CY JUN 18-21, 2015 CL Bend, OR SP Amer Soc Primatologists, Chimps Inc, Primate Conservat Inc, Purina LabDiet, Res Diets Inc, Carter 2 Syst Inc, S Karger Publishers Inc, Cambridge Univ Press, Unifab Corp, Van Hoang Dao C1 [Crofoot, M. C.; Farine, D. R.] Univ Calif Davis, Dept Anthropol, Davis, CA 95616 USA. [Crofoot, M. C.; Farine, D. R.] Univ Oxford, Smithsonian Trop Res Inst, Oxford OX1 2JD, England. [Farine, D. R.] Univ Oxford, Edward Grey Inst Field Ornithol, Oxford OX1 2JD, England. [Strandburg-Peshkin, A.] Princeton Univ, Dept Ecol & Evolutionary Biol, Princeton, NJ 08544 USA. [Brugere, I.; Li, J.; Berger-Wolf, T. Y.] Univ Illinois, Dept Comp Sci, Chicago, IL USA. NR 0 TC 0 Z9 0 U1 1 U2 7 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0275-2565 EI 1098-2345 J9 AM J PRIMATOL JI Am. J. Primatol. PD NOV PY 2015 VL 77 SU 1 MA 27 BP 41 EP 42 PG 2 WC Zoology SC Zoology GA CU5GQ UT WOS:000363560500012 ER PT J AU Farine, DR Hoppitt, W AF Farine, D. R. Hoppitt, W. TI QUANTIFYING INFORMATION TRANSFER ACROSS SOCIAL NETWORKS: TOOLS, APPLICATIONS AND ECOLOGICAL IMPLICATIONS SO AMERICAN JOURNAL OF PRIMATOLOGY LA English DT Meeting Abstract CT 38th Annual Meeting of the American-Society-of-Primatologists CY JUN 18-21, 2015 CL Bend, OR SP Amer Soc Primatologists, Chimps Inc, Primate Conservat Inc, Purina LabDiet, Res Diets Inc, Carter 2 Syst Inc, S Karger Publishers Inc, Cambridge Univ Press, Unifab Corp, Van Hoang Dao C1 [Farine, D. R.] Univ Calif Davis, Dept Anthropol, Davis, CA 95616 USA. [Farine, D. R.] Univ Oxford, Dept Zool, Edward Grey Inst Field Ornithol, Oxford OX1 2JD, England. [Farine, D. R.] Smithsonian Trop Res Inst, Panama City, Panama. [Hoppitt, W.] Anglia Ruskin Univ, Animal & Environm Res Grp, Cambridge, England. RI Hoppitt, William/A-8216-2008 OI Hoppitt, William/0000-0003-0815-5720 NR 0 TC 0 Z9 0 U1 0 U2 1 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0275-2565 EI 1098-2345 J9 AM J PRIMATOL JI Am. J. Primatol. PD NOV PY 2015 VL 77 SU 1 MA 26 BP 41 EP 41 PG 1 WC Zoology SC Zoology GA CU5GQ UT WOS:000363560500011 ER PT J AU Power, ML Alonge, MM Quinn, EA AF Power, M. L. Alonge, M. M. Quinn, E. A. TI IS AMYLASE EXPRESSION BY THE HUMAN MAMMARY A GENUS HOMO SPECIFIC TRAIT? SO AMERICAN JOURNAL OF PRIMATOLOGY LA English DT Meeting Abstract CT 38th Annual Meeting of the American-Society-of-Primatologists CY JUN 18-21, 2015 CL Bend, OR SP Amer Soc Primatologists, Chimps Inc, Primate Conservat Inc, Purina LabDiet, Res Diets Inc, Carter 2 Syst Inc, S Karger Publishers Inc, Cambridge Univ Press, Unifab Corp, Van Hoang Dao C1 [Power, M. L.; Alonge, M. M.] Smithsonian Conservat Biol Inst, Natl Zool Pk, Conservat Ecol Ctr, Nutr Lab, Washington, DC 20013 USA. [Quinn, E. A.] Washington Univ, Dept Anthropol, St Louis, MO 63130 USA. NR 0 TC 0 Z9 0 U1 0 U2 1 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0275-2565 EI 1098-2345 J9 AM J PRIMATOL JI Am. J. Primatol. PD NOV PY 2015 VL 77 SU 1 MA 94 BP 74 EP 75 PG 2 WC Zoology SC Zoology GA CU5GQ UT WOS:000363560500076 ER PT J AU Power, ML AF Power, M. L. TI GREAT APE MILK DIFFERS FROM HUMAN MILK IN NUTRITIONALLY SIGNIFICANT WAYS SO AMERICAN JOURNAL OF PRIMATOLOGY LA English DT Meeting Abstract CT 38th Annual Meeting of the American-Society-of-Primatologists CY JUN 18-21, 2015 CL Bend, OR SP Amer Soc Primatologists, Chimps Inc, Primate Conservat Inc, Purina LabDiet, Res Diets Inc, Carter 2 Syst Inc, S Karger Publishers Inc, Cambridge Univ Press, Unifab Corp, Van Hoang Dao C1 [Power, M. L.] Natl Zool Pk, Smithsonian Conservat Biol Inst, Conservat Ecol Ctr, Nutr Lab, Washington, DC 20013 USA. NR 0 TC 0 Z9 0 U1 0 U2 2 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0275-2565 EI 1098-2345 J9 AM J PRIMATOL JI Am. J. Primatol. PD NOV PY 2015 VL 77 SU 1 MA 158 BP 102 EP 102 PG 1 WC Zoology SC Zoology GA CU5GQ UT WOS:000363560500128 ER PT J AU Ksepka, DT Werning, S Sclafani, M Boles, ZM AF Ksepka, Daniel T. Werning, Sarah Sclafani, Michelle Boles, Zachary M. TI Bone histology in extant and fossil penguins (Aves: Sphenisciformes) SO JOURNAL OF ANATOMY LA English DT Article DE bone microstructure; flightlessness; Spheniscidae; wing-propelled diving ID NITROGEN TENSIONS; EMPEROR PENGUINS; STEM PENGUINS; ALCIDAE AVES; GROWTH-RATES; LONG BONES; LIFE-STYLE; EVOLUTION; AMNIOTES; MAMMALS AB Substantial changes in bone histology accompany the secondary adaptation to life in the water. This transition is well documented in several lineages of mammals and non-avian reptiles, but has received relatively little attention in birds. This study presents new observations on the long bone microstructure of penguins, based on histological sections from two extant taxa (Spheniscus and Aptenodytes) and eight fossil specimens belonging to stem lineages (dagger Palaeospheniscus and several indeterminate Eocene taxa). High bone density in penguins results from compaction of the internal cortical tissues, and thus penguin bones are best considered osteosclerotic rather than pachyostotic. Although the oldest specimens sampled in this study represent stages of penguin evolution that occurred at least 25million years after the loss of flight, major differences in humeral structure were observed between these Eocene stem taxa and extant taxa. This indicates that the modification of flipper bone microstructure continued long after the initial loss of flight in penguins. It is proposed that two key transitions occurred during the shift from the typical hollow avian humerus to the dense osteosclerotic humerus in penguins. First, a reduction of the medullary cavity occurred due to a decrease in the amount of perimedullary osteoclastic activity. Second, a more solid cortex was achieved by compaction. In extant penguins and dagger Palaeospheniscus, most of the inner cortex is formed by rapid osteogenesis, resulting an initial latticework of woven-fibered bone. Subsequently, open spaces are filled by slower, centripetal deposition of parallel-fibered bone. Eocene stem penguins formed the initial latticework, but the subsequent round of compaction was less complete, and thus open spaces remained in the adult bone. In contrast to the humerus, hindlimb bones from Eocene stem penguins had smaller medullary cavities and thus higher compactness values compared with extant taxa. Although cortical lines of arrested growth have been observed in extant penguins, none was observed in any of the current sampled specimens. Therefore, it is likely that even these giant' penguin taxa completed their growth cycle without a major pause in bone deposition, implying that they did not undergo a prolonged fasting interval before reaching adult size. C1 [Ksepka, Daniel T.] Bruce Museum, Greenwich, CT 06830 USA. [Ksepka, Daniel T.] Smithsonian Natl Museum Nat Hist, Washington, DC USA. [Werning, Sarah] SUNY Stony Brook, Dept Anat Sci, Stony Brook, NY 11794 USA. [Sclafani, Michelle] North Carolina Dept Environm & Nat Resources, Raleigh, NC USA. [Boles, Zachary M.] Drexel Univ, Dept Biol, Philadelphia, PA 19104 USA. RP Ksepka, DT (reprint author), Bruce Museum, 1 Museum Dr, Greenwich, CT 06830 USA. EM dksepka@brucemuseum.org RI Werning, Sarah/E-8157-2016 OI Werning, Sarah/0000-0002-2405-595X FU NSF [DEB 0949899]; NCSU Office of Undergraduate Research FX The authors thank Mark Norell, Joel Cracraft and Peter Sweet (AMNH), and Storrs Olson and Mark Florence (USNM) for access to specimens and permission to take histology samples, Aurore Canoville (Steinmann Institute, Bonn, Germany) for sharing a copy of her dissertation, Laura Wilson (Sternberg Museum of Natural History) for access to comparative images and Piotr Jadwiszczak, N. Adam Smith, Ignacio Cerda, Holly Woodward, Julia Clarke, and an anonymous reviewer for constructive comments and editing. This work was supported by NSF award DEB 0949899 to D.T.K. and NCSU Office of Undergraduate Research grants to Z.B. and M.S. NR 87 TC 1 Z9 1 U1 9 U2 37 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0021-8782 EI 1469-7580 J9 J ANAT JI J. Anat. PD NOV PY 2015 VL 227 IS 5 BP 611 EP 630 DI 10.1111/joa.12367 PG 20 WC Anatomy & Morphology SC Anatomy & Morphology GA CU0ME UT WOS:000363210100003 PM 26360700 ER PT J AU Harasewych, MG Temkin, I AF Harasewych, M. G. Temkin, I. TI The Miocene genus Mantellina (Bivalvia: Limidae) discovered living on the deep reefs off Curacao, with the description of a new species SO JOURNAL OF MOLLUSCAN STUDIES LA English DT Article ID MULTIPLE-SEQUENCE ALIGNMENT; MOLLUSCA; OPTIMIZATION; LIMA; CILIATION; EVOLUTION; PERFORMANCE; MORPHOLOGY; FAUNA AB Mantellina translucens n. sp. inhabits the deep reefs (215-310 m) off southeastern Curacao, occurring singly or in pairs, attached to vertical rock walls and boulders by thin byssal threads. This species differs from all living Limidae in having an exceptionally thin, comarginally corrugated shell that is longer than tall and lacks radial sculpture. This new species possesses a unique suite of characters associated with adaptations to an epibyssate mode of life in bathyal habitats, including simplification of the digestive tract, possibly indicating omnivory. It is assigned to the genus Mantellina Sacco, 1904, previously known only from fossil deposits of Burdigalian to Serravallian Miocene age of the Central Paratethys, on the basis of similar shell morphology. Anatomical characters and ribosomal DNA sequence data (18S and 16S genes) confirm placement of this taxon within the family Limidae, yet its shell superficially resembles those of several genera of the extinct family Inoceramidae, while differing in hinge morphology and shell ultrastructure. A preliminary molecular phylogeny recovered Limidae as a monophyletic clade within Pteriomorphia, with Mantellina derived relative to Limaria, and sister group to a clade containing the remaining representatives of Limidae. Ctenoides was not monophyletic. The phylogenetic tree based on molecular data does not support previously proposed suprageneric relationships based on morphological data. C1 [Harasewych, M. G.; Temkin, I.] Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, MRC 163, Washington, DC 20013 USA. [Temkin, I.] No Virginia Community Coll, Dept Biol, Annandale, VA 22003 USA. RP Harasewych, MG (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, MRC 163, POB 37012, Washington, DC 20013 USA. EM harasewych@si.edu NR 67 TC 2 Z9 2 U1 2 U2 8 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0260-1230 EI 1464-3766 J9 J MOLLUS STUD JI J. Molluscan Stud. PD NOV PY 2015 VL 81 BP 442 EP 454 DI 10.1093/mollus/eyv021 PN 4 PG 13 WC Marine & Freshwater Biology; Zoology SC Marine & Freshwater Biology; Zoology GA CU4RR UT WOS:000363518100003 ER PT J AU Bashforth, AR Nelson, WJ AF Bashforth, Arden R. Nelson, W. John TI A Middle Pennsylvanian macrofloral assemblage from below the Rock Island (No. 1) Coal Member, Illinois: Resolving the Bolsovian-Asturian boundary in the Illinois Basin SO REVIEW OF PALAEOBOTANY AND PALYNOLOGY LA English DT Article DE Bolsovian; Asturian; Atokan; Desmoinesian; Macroflora; Biostratigraphy ID NORTH-AMERICA; WESTPHALIAN-D; FOSSIL PLANTS; SOUTH-WALES; GEN-NOV; SWAMP VEGETATION; CLIMATE-CHANGE; SEA-LEVEL; PATTERNS; COALFIELD AB A taxonomic, quantitative, and biostratigraphic analysis is presented for a macrofloral assemblage collected from below the Rock Island (No.1) Coal Member at the historical Friendship Farm locality in Rock Island County, on the northwestern margin of the Illinois Basin. The Middle Pennsylvanian (middle Moscovian) fossiliferous strata involve the middle Tradewater Formation, and are situated a short distance below the Atokan-Desmoinesian Stage boundary as defined by marine microfossils and palynology. The assemblage of 14 fossil-taxa is overwhelmingly dominated by pteridosperms, including Laveineopteris rarinervis, Neuropteris flexuosa, Alethopteris serlii, Macroneuropteris scheuchzeri, and Mariopteris nervosa, whereas lycopsids, sphenopsids, and ferns are comparatively rare. Homotaxial comparison with the macrofloral biozonation scheme established in Europe indicates an Asturian age for the assemblage, in all likelihood early Asturian (Linopteris obliqua Biozone). Similar comparisons with range limits documented in the Appalachian Basin yield a more ambiguous age, but an early Asturian age is equally probable. These findings indicate that the Bolsovian-Asturian Substage boundary of western Europe lies below the Atokan-Desmoinesian Stage boundary in the Illinois Basin, boundaries that have traditionally been correlated by palynology. The Middle Pennsylvanian interval near these boundaries is being increasingly recognized as one of significant environmental change, reflected in marked lithological and biological modifications throughout tropical Euramerica. However, the fact that the Bolsovian-Asturian and Atokan-Desmoinesian boundaries are not synchronous, albeit being broadly equivalent, suggests that the environmental perturbation was a protracted event that may have had global consequences. Published by Elsevier B.V. C1 [Bashforth, Arden R.; Nelson, W. John] Univ Illinois, Illinois State Geol Survey, Champaign, IL 61820 USA. [Bashforth, Arden R.] Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20560 USA. RP Bashforth, AR (reprint author), Univ Illinois, Illinois State Geol Survey, 615 East Peabody Dr, Champaign, IL 61820 USA. EM bashfortha@si.edu; jnnelson@illinois.edu FU Smithsonian Institution; Paleontological Society FX This project would not have happened without the continued support of William A. DiMichele at the National Museum of Natural History, Smithsonian Institution, which initially funded the Visiting Researcher posting of ARB at the ISGS. Prolongation of the temporary stay was made possible through the generous support of an Arthur James Boucot Research Grant from the Paleontological Society. ARB thanks the ISGS Coal Section staff, especially Scott Elrick and his co-author W. John Nelson, for their enthusiasm and continued encouragement. Access to plant-fossil collections in the ISGS Samples Library was facilitated by Bob Mumm, Rodney D. Norby, and Kristina Bruhn, who are gratefully acknowledged. Access to the photographic facilities of the Illinois Natural History Survey by Sam Heads and Jared Thomas also is appreciated. Hans-Dieter Sues is acknowledged for his assistance with translation, as are Claudine Delcambre Brousmiche, Christopher J. Cleal, and Josef Henitla for their discussions about identifications. Alex Stuedemann, maintenance director of TPC Deere Run Golf Course, is thanked for facilitating access to collecting sites during a return visit by WJN. Finally, B. Mitch Blake and an anonymous reviewer are acknowledged for their constructive reviews. NR 171 TC 1 Z9 1 U1 3 U2 3 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0034-6667 EI 1879-0615 J9 REV PALAEOBOT PALYNO JI Rev. Palaeobot. Palynology PD NOV PY 2015 VL 222 BP 67 EP 83 DI 10.1016/j.revpalbo.2015.07.003 PG 17 WC Plant Sciences; Paleontology SC Plant Sciences; Paleontology GA CT8LR UT WOS:000363068600007 ER PT J AU Subiaul, F Patterson, EM Schilder, B Renner, E Barr, R AF Subiaul, Francys Patterson, Eric M. Schilder, Brian Renner, Elizabeth Barr, Rachel TI Becoming a high-fidelity - super - imitator: what are the contributions of social and individual learning? SO DEVELOPMENTAL SCIENCE LA English DT Article ID AGE-RELATED-CHANGES; WORKING-MEMORY; 36-MONTH-OLD CHILDREN; COGNITIVE-DEVELOPMENT; CUMULATIVE CULTURE; OTHERS ACTIONS; INFANTS; MECHANISMS; GESTURES; HUMANS AB In contrast to other primates, human children's imitation performance goes from low to high fidelity soon after infancy. Are such changes associated with the development of other forms of learning? We addressed this question by testing 215 children (26-59 months) on two social conditions (imitation, emulation) - involving a demonstration - and two asocial conditions (trial-and-error, recall) - involving individual learning - using two touchscreen tasks. The tasks required responding to either three different pictures in a specific picture order (Cognitive: AirplaneBallCow) or three identical pictures in a specific spatial order (Motor-Spatial: UpDownRight). There were age-related improvements across all conditions and imitation, emulation and recall performance were significantly better than trial-and-error learning. Generalized linear models demonstrated that motor-spatial imitation fidelity was associated with age and motor-spatial emulation performance, but cognitive imitation fidelity was only associated with age. While this study provides evidence for multiple imitation mechanisms, the development of one of those mechanisms - motor-spatial imitation - may be bootstrapped by the development of another social learning skill - motor-spatial emulation. Together, these findings provide important clues about the development of imitation, which is arguably a distinctive feature of the human species. C1 [Subiaul, Francys] George Washington Univ, Dept Speech & Hearing Sci, Washington, DC 20052 USA. [Subiaul, Francys; Schilder, Brian; Renner, Elizabeth] George Washington Univ, Dept Anthropol, Ctr Adv Study Hominid Paleobiol, Washington, DC 20052 USA. [Subiaul, Francys] GW Inst Neurosci, Washington, DC USA. [Subiaul, Francys] Mind Brain Inst, Baltimore, MD USA. [Subiaul, Francys] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA. [Patterson, Eric M.] Georgetown Univ, Dept Biol, Washington, DC 20057 USA. [Barr, Rachel] Georgetown Univ, Dept Psychol, Washington, DC 20057 USA. RP Subiaul, F (reprint author), 2115 G St,NW 204, Washington, DC 20052 USA. EM Subiaul@gwu.edu OI Barr, Rachel/0000-0002-5855-9718 FU University Facilitating Funds (GWU); National Science Foundation [BCS-0748717] FX We would like to thank Malathi Thothathiri, Cynthia Core, Kelly Jaakola and four anonymous reviewers for reading earlier drafts of this manuscript as well as the many student volunteers in the Social Cognition Lab of the George Washington University for assisting with recruitment and data collection. Finally, we want to extend our gratitude to the Smithsonian's Institute, National Museum of Natural History, its staff and visiting children whose participation made this study possible. This study was supported by University Facilitating Funds (GWU) and a CAREER grant from the National Science Foundation to F. Subiaul (BCS-0748717). NR 73 TC 5 Z9 6 U1 5 U2 21 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1363-755X EI 1467-7687 J9 DEVELOPMENTAL SCI JI Dev. Sci. PD NOV PY 2015 VL 18 IS 6 BP 1025 EP 1035 DI 10.1111/desc.12276 PG 11 WC Psychology, Developmental; Psychology, Experimental SC Psychology GA CT6GM UT WOS:000362911400015 PM 25545051 ER PT J AU Khan, I Yang, ZK Maldonado, E Li, C Zhang, GJ Gilbert, MTP Jarvis, ED O'Brien, SJ Johnson, WE Antunes, A AF Khan, Imran Yang, Zhikai Maldonado, Emanuel Li, Cai Zhang, Guojie Gilbert, M. Thomas P. Jarvis, Erich D. O'Brien, Stephen J. Johnson, Warren E. Antunes, Agostinho TI Olfactory Receptor Subgenomes Linked with Broad Ecological Adaptations in Sauropsida SO MOLECULAR BIOLOGY AND EVOLUTION LA English DT Article DE olfactory receptors; adaptation; selection; birds ID DROSOPHILA ODORANT RECEPTORS; GENE REPERTOIRES; EVOLUTIONARY DYNAMICS; PHYLOGENETIC ANALYSIS; FORAGING STRATEGIES; MAXIMUM-LIKELIHOOD; ANTARCTIC SEABIRD; MULTIGENE FAMILY; BIRDS; GENOME AB Olfactory receptors (ORs) govern a prime sensory function. Extant birds have distinct olfactory abilities, but the molecular mechanisms underlining diversification and specialization remain mostly unknown. We explored OR diversity in 48 phylogenetic and ecologically diverse birds and 2 reptiles (alligator and green sea turtle). OR subgenomes showed species- and lineage-specific variation related with ecological requirements. Overall 1,953 OR genes were identified in reptiles and 16,503 in birds. The two reptiles had larger OR gene repertoires (989 and 964 genes, respectively) than birds (182-688 genes). Overall, birds had more pseudogenes (7,855) than intact genes (1,944). The alligator had significantly more functional genes than sea turtle, likely because of distinct foraging habits. We found rapid species-specific expansion and positive selection in OR14 (detects hydrophobic compounds) in birds and in OR51 and OR52 (detect hydrophilic compounds) in sea turtle, suggestive of terrestrial and aquatic adaptations, respectively. Ecological partitioning among birds of prey, water birds, land birds, and vocal learners showed that diverse ecological factors determined olfactory ability and influenced corresponding olfactory-receptor subgenome. OR5/8/9 was expanded in predatory birds and alligator, suggesting adaptive specialization for carnivory. OR families 2/13, 51, and 52 were correlated with aquatic adaptations (water birds), OR families 6 and 10 weremore pronounced in vocal-learning birds, whereas most specialized land birds had an expanded OR family 14. Olfactory bulb ratio (OBR) andOR gene repertoire were correlated. Birds that forage for prey (carnivores/piscivores) had relatively complex OBR and OR gene repertoires compared with modern birds, including passerines, perhaps due to highly developed cognitive capacities facilitating foraging innovations. C1 [Khan, Imran; Maldonado, Emanuel; Antunes, Agostinho] Univ Porto, Interdisciplinary Ctr Marine & Environm Res, CIIMAR CIMAR, P-4100 Oporto, Portugal. [Khan, Imran; Antunes, Agostinho] Univ Porto, Fac Sci, Dept Biol, P-4100 Oporto, Portugal. [Yang, Zhikai; Li, Cai; Zhang, Guojie] China Natl Genebank, BGI Shenzhen, Shenzhen 518083, Guangdong, Peoples R China. [Zhang, Guojie] Univ Copenhagen, Dept Biol, Ctr Social Evolut, DK-2100 Copenhagen, Denmark. [Gilbert, M. Thomas P.] Univ Copenhagen, Nat Hist Museum Denmark, Ctr GeoGenet, Copenhagen, Denmark. [Jarvis, Erich D.] Duke Univ, Med Ctr, Howard Hughes Med Inst, Dept Neurobiol, Durham, NC 27706 USA. [O'Brien, Stephen J.] St Petersburg State Univ, Theodosius Dobzhansky Ctr Genome Bioinformat, St Petersburg 199034, Russia. [O'Brien, Stephen J.] Nova SE Univ, Oceanog Ctr, Ft Lauderdale, FL 33314 USA. [Johnson, Warren E.] Natl Zool Pk, Smithsonian Conservat Biol Inst, Front Royal, VA USA. RP Antunes, A (reprint author), Univ Porto, Interdisciplinary Ctr Marine & Environm Res, CIIMAR CIMAR, Rua Campo Alegre 823, P-4100 Oporto, Portugal. EM aantunes@ciimar.up.pt RI Gilbert, Marcus/A-8936-2013; OI Gilbert, Marcus/0000-0002-5805-7195; Li, Cai/0000-0001-7843-2151; Zhang, Guojie/0000-0001-6860-1521; Maldonado, Emanuel/0000-0002-0084-6116 FU Fundacao para a Ciencia e a Tecnologia (FCT) [SFRH/BD/48518/2008]; Russian Ministry of Science [11.G34.31.0068]; European Regional Development Fund (ERDF) through the COMPETE - Operational Competitiveness Programme; FCT [PEst-C/MAR/LA0015/2013, PTDC/AAC-AMB/104983/2008 (FCOMP-01-0124-FEDER-008610), PTDC/AAC-AMB/121301/2010 (FCOMP-01-0124-FEDER-019490), PTDC/AAG-GLO/6887/2014] FX The authors thank Aldo Barreiro for the assistance with some of the statistical analyses. I.K. was funded by a PhD grant (SFRH/BD/48518/2008) from Fundacao para a Ciencia e a Tecnologia (FCT). S.J.O. was supported as Principal Investigator by Russian Ministry of Science Mega-grant no.11.G34.31.0068. A.A. was partially supported by the European Regional Development Fund (ERDF) through the COMPETE - Operational Competitiveness Programme and national funds through FCT under the projects PEst-C/MAR/LA0015/2013, PTDC/AAC-AMB/104983/2008 (FCOMP-01-0124-FEDER-008610), PTDC/AAC-AMB/121301/2010 (FCOMP-01-0124-FEDER-019490) and PTDC/AAG-GLO/6887/2014. NR 88 TC 7 Z9 7 U1 6 U2 25 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0737-4038 EI 1537-1719 J9 MOL BIOL EVOL JI Mol. Biol. Evol. PD NOV PY 2015 VL 32 IS 11 BP 2832 EP 2843 DI 10.1093/molbev/msv155 PG 12 WC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity SC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity GA CT7YZ UT WOS:000363033100003 PM 26219582 ER PT J AU Smith, CR Cahan, SH Kemena, C Brady, SG Yang, W Bornberg-Bauer, E Eriksson, T Gadau, J Helmkampf, M Gotzek, D Miyakawa, MO Suarez, AV Mikheyev, A AF Smith, Chris R. Cahan, Sara Helms Kemena, Carsten Brady, Sean G. Yang, Wei Bornberg-Bauer, Erich Eriksson, Ti Gadau, Juergen Helmkampf, Martin Gotzek, Dietrich Miyakawa, Misato Okamoto Suarez, Andrew V. Mikheyev, Alexander TI How Do Genomes Create Novel Phenotypes? Insights from the Loss of the Worker Caste in Ant Social Parasites SO MOLECULAR BIOLOGY AND EVOLUTION LA English DT Article DE social parasite; ant; caste; phenotypic plasticity; genome ID DIFFERENTIAL EXPRESSION ANALYSIS; DNA-SEQUENCING DATA; RED HARVESTER ANT; RNA-SEQ DATA; GENE-EXPRESSION; HYMENOPTERA-FORMICIDAE; POGONOMYRMEX-BARBATUS; ANNOTATION PIPELINE; VOLLENHOVIA-EMERYI; RELAXED SELECTION AB A central goal of biology is to uncover the genetic basis for the origin of new phenotypes. A particularly effective approach is to examine the genomic architecture of species that have secondarily lost a phenotype with respect to their close relatives. In the eusocial Hymenoptera, queens and workers have divergent phenotypes that may be produced via either expression of alternative sets of caste-specific genes and pathways or differences in expression patterns of a shared set of multifunctional genes. To distinguish between these two hypotheses, we investigated how secondary loss of the worker phenotype in workerless ant social parasites impacted genome evolution across two independent origins of social parasitism in the ant genera Pogonomyrmex and Vollenhovia. We sequenced the genomes of three social parasites and their most-closely related eusocial host species and compared gene losses in social parasites with gene expression differences between host queens and workers. Virtually all annotated genes were expressed to some degree in both castes of the host, with most shifting in queen-worker bias across developmental stages. As a result, despite >1My of divergence from the last common ancestor that had workers, the social parasites showed strikingly little evidence of gene loss, damaging mutations, or shifts in selection regime resulting from loss of the worker caste. This suggests that regulatory changes within a multifunctional genome, rather than sequence differences, have played a predominant role in the evolution of social parasitism, and perhaps also in the many gains and losses of phenotypes in the social insects. C1 [Smith, Chris R.] Earlham Coll, Dept Biol, Richmond, IN 47374 USA. [Cahan, Sara Helms] Univ Vermont, Dept Biol, Burlington, VT 05405 USA. [Kemena, Carsten; Bornberg-Bauer, Erich] Univ Munster, Inst Evolut & Biodivers, D-48149 Munster, Germany. [Brady, Sean G.] Natl Museum Nat Hist, Dept Entomol, Smithsonian Inst, Washington, DC 20560 USA. [Yang, Wei] Univ Illinois, Dept Comp Sci, Urbana, IL USA. [Eriksson, Ti; Gadau, Juergen; Helmkampf, Martin] Arizona State Univ, Sch Life Sci, Tempe, AZ 85287 USA. [Gotzek, Dietrich] Univ Georgia, Dept Entomol, Athens, GA 30602 USA. [Gotzek, Dietrich; Suarez, Andrew V.] Univ Illinois, Dept Anim Biol, Urbana, IL USA. [Miyakawa, Misato Okamoto; Mikheyev, Alexander] Okinawa Inst Sci & Technol, Ecol & Evolut Unit, Onna, Okinawa, Japan. [Suarez, Andrew V.] Univ Illinois, Dept Entomol, Urbana, IL USA. RP Smith, CR (reprint author), Earlham Coll, Dept Biol, Richmond, IN 47374 USA. EM crsmith.ant@gmail.com; alexander.mikheyev@oist.jp RI Bornberg-Bauer, Erich/A-1563-2013 OI Bornberg-Bauer, Erich/0000-0002-1826-3576 FU OIST; JSPS Kakenhi [25221206, 24770034]; NSF [DEB 1020979, DUE 1139893, DEB 0919052] FX The authors thank the OIST sequencing center for preparing the V. emeryi genomic libraries and for carrying out the sequencing. At the University of Illinois, they thank Hugh Robertson and Kim Walden for preparing the P. anergismus genomic libriaries and the Keck Center for carrying out the sequencing. They are grateful to M.M.Y. Tin and M. Grau-Lopez for assistance with laboratory work and bioinformatics, respectively. They thank the OIST workshop committee for helping to organize the Genomics of Social Parasite Evolution workshop. Funding for this project was provided by OIST and JSPS Kakenhi grants to ASM (25221206 and 24770034), and by grants from NSF (DEB 1020979 to AVS, DUE 1139893 to CRS, and DEB 0919052 to SIHC). They thank "Uncle" Bob Johnson for P. anergismus specimens as well as E. Cash and K. E. Anderson for lab colonies, and B. Smith and N. Hamada Fernside for larva collection. NR 83 TC 5 Z9 5 U1 6 U2 45 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0737-4038 EI 1537-1719 J9 MOL BIOL EVOL JI Mol. Biol. Evol. PD NOV PY 2015 VL 32 IS 11 BP 2919 EP 2931 DI 10.1093/molbev/msv165 PG 13 WC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity SC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity GA CT7YZ UT WOS:000363033100010 PM 26226984 ER PT J AU Huang, YJ Liu, YS Wen, J Quan, C AF Huang, Yong-Jiang Liu, Yu-Sheng Wen, Jun Quan, Cheng TI First fossil record of Staphylea L. (Staphyleaceae) from North America, and its biogeographic implications SO PLANT SYSTEMATICS AND EVOLUTION LA English DT Article DE Fossil seed; Gray Fossil Site; Late Neogene; North America; Staphylea ID LATEST MIOCENE; EARLIEST PLIOCENE; UNITED-STATES; TENNESSEE; EVOLUTION; FLORAS; FRUITS; GRAY; USA; ILLICIACEAE AB The occurrences of Staphylea L. (Staphyleaceae) fossils have been abundantly documented from the Cenozoic of Eurasia, but none has been confirmed from North America to date. In this study, we describe Staphylea levisemia sp. nov. on the basis of seed remains from the latest Miocene to earliest Pliocene of northeastern Tennessee, southeastern USA. The seeds are characterized by a smoothly inflated body, a large hilar scar perforated by several vascular traces and bordered by a distinctive lip-like rim, a cuticle coating the seed coat interior, and seed coat section containing weakly developed tiny lumina. According to the paleogeographic distribution of the genus, it is hypothesized that Staphylea originated from western Eurasia no later than the late Oligocene, and arrived in eastern North America no later than the late Neogene, most possibly through the North Atlantic land bridges like many other seed plants. C1 [Huang, Yong-Jiang; Liu, Yu-Sheng] E Tennessee State Univ, Dept Biol Sci, Johnson City, TN 37614 USA. [Huang, Yong-Jiang] Chinese Acad Sci, Key Lab Plant Biodivers & Biogeog East Asia, Kunming Inst Bot, Kunming 650204, Peoples R China. [Wen, Jun] Natl Museum Nat Hist, Dept Bot, Smithsonian Inst, MRC 166, Washington, DC 20560 USA. [Quan, Cheng] Jilin Univ, Res Ctr Paleontol & Stratig, Changchun 130026, Peoples R China. RP Liu, YS (reprint author), E Tennessee State Univ, Dept Biol Sci, Johnson City, TN 37614 USA. EM liuc@etsu.edu; quan@jlu.edu.cn FU NSF [EAR-0746105]; National Natural Science Foundation of China [31300187, 41372002, 41172008] FX The authors thank the Herbarium of East Tennessee State University, the Herbarium of Kunming Institute of Botany, Chinese Academy of Sciences, and Dr. Froster Levy for help with extant seed materials; the Central Lab of Xishuangbanna Tropical Botanical Garden, Chinese Academy of Sciences for technical assistance with the SEM; Dr. Wen-Long He for picturing the fossil seeds; Miss Hai Zhu for observing the extant seeds of Staphylea from herbarium specimens; Dr. Li Wang for scanning the fossil and extant seeds with the SEM; students from Dr. Jun Wen's research group for work on molecular phylogenetic analysis; and the two anonymous reviewers for improving the manuscript. This work was supported by NSF EAR-0746105, and partly by the National Natural Science Foundation of China (Nos. 31300187, 41372002, and 41172008). NR 60 TC 2 Z9 2 U1 0 U2 5 PU SPRINGER WIEN PI WIEN PA SACHSENPLATZ 4-6, PO BOX 89, A-1201 WIEN, AUSTRIA SN 0378-2697 EI 1615-6110 J9 PLANT SYST EVOL JI Plant Syst. Evol. PD NOV PY 2015 VL 301 IS 9 BP 2203 EP 2218 DI 10.1007/s00606-015-1224-z PG 16 WC Plant Sciences; Evolutionary Biology SC Plant Sciences; Evolutionary Biology GA CT2XF UT WOS:000362668300005 ER PT J AU Huffer, D Chappell, D Dzung, LTM Nguyen, HL AF Huffer, Damien Chappell, Duncan Lam Thi My Dzung Nguyen, Hoang Long TI From the Ground, Up: The Looting of Vu'on Chuoi within the Vietnamese and Southeast Asian Antiquities Trade SO PUBLIC ARCHAEOLOGY LA English DT Article DE Vuon Chuoi; Hanoi; antiquities trade; Southeast Asian archaeology; public outreach; cultural property legislation ID CAMBODIA AB The exact nature of the illicit antiquities trade from ground to market in Southeast Asia remains poorly known outside of Thailand and Cambodia, where most research has been focused. This paper helps to address this imbalance by documenting and contextualizing looting activities at the Bronze and Iron Age site of Vuu?n Chu?i, located within urban Hanoi. A brief excavation history is provided so as to place recent looting into archaeological context. The methods used to document the recent and on-going looting observed are then discussed, followed by the nature of the current threat to Vuu?n Chu?i and a summation of what little is known about the Vietnamese antiquities trade in general and its relationship to regional antiquities trafficking. Finally, we discuss the current regulatory landscape in terms of constitutional, ownership, penal and international law, difficulties with enforcement and prosecution, and what course of action is needed not only to protect Vuu?n Chu?i and similar sites in and around Hanoi, but also to continue to raise public awareness of the archaeological repercussions of the trade itself. C1 [Huffer, Damien] Smithsonian Inst, Smithsonian Museum Conservat Inst, Suitland, MD 20746 USA. [Huffer, Damien] Smithsonian Inst, Dept Anthropol, Suitland, MD 20746 USA. [Huffer, Damien] Smithsonian Inst, Museum Support Ctr, Museum Conservat Inst, MRC 534,4210 Silver Hill Rd, Suitland, MD 20746 USA. [Chappell, Duncan] Univ Sydney, Fac Law, Sydney, NSW 2006, Australia. [Lam Thi My Dzung] Vietnam Natl Univ, Univ Social Sci & Humanities, Museum Anthropol, Hanoi, Vietnam. [Nguyen, Hoang Long] Univ Bayreuth, Social & Cultural Anthropol, Bayreuth, Germany. RP Huffer, D (reprint author), Smithsonian Inst, Museum Support Ctr, Museum Conservat Inst, MRC 534,4210 Silver Hill Rd, Suitland, MD 20746 USA. EM hufferd@si.edu NR 37 TC 0 Z9 0 U1 1 U2 1 PU ROUTLEDGE JOURNALS, TAYLOR & FRANCIS LTD PI ABINGDON PA 2-4 PARK SQUARE, MILTON PARK, ABINGDON OX14 4RN, OXON, ENGLAND SN 1465-5187 EI 1753-5530 J9 PUBLIC ARCHAEOL JI Public Archaeol. PD NOV PY 2015 VL 14 IS 4 BP 224 EP 239 DI 10.1080/14655187.2016.1194715 PG 16 WC Archaeology SC Archaeology GA DZ5UV UT WOS:000385928000002 ER PT J AU Ogburn, MB Habegger, LC AF Ogburn, Matthew B. Habegger, Leigh C. TI Reproductive Status of Callinectes sapidus as an Indicator of Spawning Habitat in the South Atlantic Bight, USA SO ESTUARIES AND COASTS LA English DT Article DE Spawning stock; Callinectes sapidus; Habitat; Reproductive status; Stock assessment ID TIDAL-STREAM TRANSPORT; FEMALE BLUE CRABS; LARVAL DEVELOPMENT; MIGRATION; RATHBUN; CONNECTIVITY; ESTUARINE; MOVEMENT; DYNAMICS; PATTERNS AB Stocks of estuarine migrant species can be challenging to assess due to a relative lack of abundance data in offshore areas and complex interactions between spawning behavior and estuarine geomorphology. The blue crab Callinectes sapidus in the South Atlantic Bight (SAB), USA, inhabits estuaries ranging from large semi-enclosed bays to narrow river mouths where estuarine conditions extend onto the continental shelf. Mature female reproductive status was used as an indicator to identify spawning habitat, and data from long-term fishery independent surveys were used to evaluate spatiotemporal trends in abundance of spawning females. Long-term data (1990-2011) were obtained from the Southeast Area Marine Assessment Program (SEAMAP) South Atlantic survey and the Georgia Ecological Monitoring Trawl Survey. Biological samples were obtained from estuarine and offshore areas of Georgia for a detailed analysis of habitat use. Reproductive status of mature female blue crabs (ovigery, ovary development, egg remnants) was indicative of a summer peak in spawning in Georgia that occurred primarily on the continental shelf as far as 13 km offshore. SEAMAP data provide strong evidence that blue crab females spawn on the continental shelf throughout the SAB, with substantial declines in spawner abundance over time. Empirical orthogonal function analysis of SEAMAP time series was indicative of regional spawning areas defined by biogeography which are poorly aligned with fishery management jurisdictions. Indicators of reproductive status provided a powerful method for identifying spawning habitats of an estuarine migrant species, especially when spawners may disperse over the continental shelf and occur at low density. C1 [Ogburn, Matthew B.] Savannah State Univ, Savannah, GA 31404 USA. [Ogburn, Matthew B.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. [Habegger, Leigh C.] Univ Rhode Isl, Kingston, RI 02881 USA. RP Ogburn, MB (reprint author), Smithsonian Environm Res Ctr, 647 Contees Wharf Rd, Edgewater, MD 21037 USA. EM ogburnm@si.edu; leighhabegger@gmail.com OI Ogburn, Matthew/0000-0001-5417-555X FU US Department of Commerce; NOAA National Marine Fisheries Service [PL 88-309, 2-296-R]; NOAA Living Marine Resources Cooperative Science Center [NA05OAR4811017]; Smithsonian Institution Postdoctoral Fellowship FX This project would not have been possible without the extensive sampling efforts and data contributed by the SEAMAP South Atlantic Survey conducted by South Carolina Department of Natural Resources and the Georgia Ecological Monitoring Trawl Survey conducted by the Coastal Resources Division of the Georgia Department of Natural Resources. Jeanne Boylan, Christine Ewers, Pat Geer, Robbie Lowery, Charlie Teeple, and Pearse Webster helped us obtain biological samples and survey data. Richard Forward, Zack Darnell, Mark Ruiz, Brooke Weigel, and three anonymous reviewers provided comments that significantly improved the manuscript. Support for Ogburn was provided by the US Department of Commerce, NOAA National Marine Fisheries Service, under PL 88-309, Project 2-296-R, NOAA Living Marine Resources Cooperative Science Center NA05OAR4811017, and by a Smithsonian Institution Postdoctoral Fellowship. NR 34 TC 2 Z9 2 U1 3 U2 13 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 1559-2723 EI 1559-2731 J9 ESTUAR COAST JI Estuaries Coasts PD NOV PY 2015 VL 38 IS 6 BP 2059 EP 2069 DI 10.1007/s12237-015-9962-2 PG 11 WC Environmental Sciences; Marine & Freshwater Biology SC Environmental Sciences & Ecology; Marine & Freshwater Biology GA CT1SE UT WOS:000362580300019 ER PT J AU Rushing, CS Dudash, MR Marra, PP AF Rushing, Clark S. Dudash, Michele R. Marra, Peter P. TI Habitat features and long-distance dispersal modify the use of social information by a long-distance migratory bird SO JOURNAL OF ANIMAL ECOLOGY LA English DT Article DE conspecific attraction; deuterium; habitat selection; location cues; public information; Setophaga ruticilla; social information ID BREEDING-SITE SELECTION; PUBLIC INFORMATION; CONSPECIFIC ATTRACTION; LESSER KESTRELS; CUES; DYNAMICS; DENSITY; COLONY; MANAGEMENT; SETTLEMENT AB The processes by which individuals select breeding sites have important consequences for individual tness as well as population- and community-dynamics. Although there is increasing evidence that many animal species use information acquired from conspecics to assess the suitability of potential breeding sites, little is known about how the use of this social information is modified by biotic and abiotic conditions. We used an automated playback experiment to simulate two types of social information, post-breeding public information and pre-breeding location cues, to determine the relative importance of these cues for breeding site selection by a migratory songbird, the American redstart (Setophaga ruticilla). In addition, we used stable hydrogen isotopes to determine the dispersal status of individuals that responded to our experimental treatments and quantify whether long-distance dispersers use different social cues to select breeding sites compared to philopatric individuals. We found that points that received pre-breeding location cue treatments were signi cantly more likely to be settled by redstarts than control points that received no playback. However, we found no evidence the redstarts used post-breeding public information gathered during one season to select breeding sites the following year. Breeding site habitat structure was also a strong predictor of settlement probability, indicating that redstarts modi ed the use of social information based on habitat cues. Furthermore, stable hydrogen isotope signatures from individuals that responded to location cue treatments suggest that long-distance dispersers may rely more heavily on these cues than local recruits. Collectively, these results indicate that redstarts use multiple sources of information to select breeding sites, which could buffer individuals from selecting suboptimal sites when they breed in unfamiliar locations or when habitat quality becomes decoupled from social cues. C1 [Rushing, Clark S.; Dudash, Michele R.] Univ Maryland, Grad Program Behav Ecol Evolut & Systemat, College Pk, MD 20742 USA. [Rushing, Clark S.; Marra, Peter P.] Natl Zool Pk, Smithsonian Conservat Biol Inst, Migratory Bird Ctr, Washington, DC 20013 USA. RP Rushing, CS (reprint author), Univ Maryland, Grad Program Behav Ecol Evolut & Systemat, 2101 Biosci Res Bldg, College Pk, MD 20742 USA. EM rushingc@si.edu FU Baltimore Birding Club's Dorothy Martin Memorial Fund; Cosmos Foundation; American Ornithologists Union; Washington Biologists Field Club FX All field methods were reviewed and approved by Animal Care and Use Committees at the Smithsonian Institution (#09-10), the University of Maryland (#325860-3) and the Patuxent Research Refuge (#NSR-NT-CT-0903). Access to the field site and logistical support was provided by the Patuxent Research Refuge. Two anonymous reviewers improved an earlier draft of this manuscript. The authors thank M. Betts and N. Rodenhouse for advice on assembling and operating playback stations. Funding for this project was provided by the Baltimore Birding Club's Dorothy Martin Memorial Fund, the Cosmos Foundation, the American Ornithologists Union and the Washington Biologists Field Club. The authors have no conflict of interests. NR 50 TC 1 Z9 1 U1 4 U2 27 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0021-8790 EI 1365-2656 J9 J ANIM ECOL JI J. Anim. Ecol. PD NOV PY 2015 VL 84 IS 6 BP 1469 EP 1479 DI 10.1111/1365-2656.12395 PG 11 WC Ecology; Zoology SC Environmental Sciences & Ecology; Zoology GA CT3XU UT WOS:000362741000003 PM 26061822 ER PT J AU Reynolds, JJH Hirsch, BT Gehrt, SD Craft, ME AF Reynolds, Jennifer J. H. Hirsch, Ben T. Gehrt, Stanley D. Craft, Meggan E. TI Raccoon contact networks predict seasonal susceptibility to rabies outbreaks and limitations of vaccination SO JOURNAL OF ANIMAL ECOLOGY LA English DT Article DE contact network; epidemiological modelling; host-pathogen interactions; infectious disease management; network modelling; proximity logging collar; rabies; raccoon; transmission; wildlife disease ID FACIAL TUMOR DISEASE; UNITED-STATES; PROCYON-LOTOR; POPULATION; TRANSMISSION; DYNAMICS; BEHAVIOR; EPIDEMIC; WILDLIFE; SURVEILLANCE AB Infectious disease transmission often depends on the contact structure of host populations. Although it is often challenging to capture the contact structure in wild animals, new technology has enabled biologists to obtain detailed temporal information on wildlife social contacts. In this study, we investigated the effects of raccoon contact patterns on rabies spread using network modelling. Raccoons (Procyon lotor) play an important role in the maintenance of rabies in the United States. It is crucial to understand how contact patterns influence the spread of rabies in raccoon populations in order to design effective control measures and to prevent transmission to human populations and other animals. We constructed a dynamic system of contact networks based on empirical data from proximity logging collars on a wild suburban raccoon population and then simulated rabies spread across these networks. Our contact networks incorporated the number and duration of raccoon interactions. We included differences in contacts according to sex and season, and both short-term acquaintances and long-term associations. Raccoons may display different behaviours when infectious, including aggression (furious behaviour) and impaired mobility (dumb behaviour); the network model was used to assess the impact of potential behavioural changes in rabid raccoons. We also tested the effectiveness of different vaccination coverage levels. Our results demonstrate that when rabies enters a suburban raccoon population, the likelihood of a disease outbreak affecting the majority of the population is high. Both the magnitude of rabies outbreaks and the speed of rabies spread depend strongly on the time of year that rabies is introduced into the population. When there is a combination of dumb and furious behaviours in the rabid raccoon population, there are similar outbreak sizes and speed of spread to when there are no behavioural changes due to rabies infection. By incorporating detailed data describing the variation in raccoon contact rates into a network modelling approach, we were able to show that suburban raccoon populations are highly susceptible to rabies outbreaks, that the risk of large outbreaks varies seasonally and that current vaccination target levels may be inadequate to prevent the spread of rabies within these populations. Our findings provide new insights into rabies dynamics in raccoon populations and have important implications for disease control. C1 [Reynolds, Jennifer J. H.; Craft, Meggan E.] Univ Minnesota, Dept Vet Populat Med, St Paul, MN 55108 USA. [Hirsch, Ben T.] Univ Florida, Dept Wildlife Ecol & Conservat, Gainesville, FL USA. [Hirsch, Ben T.] Smithsonian Trop Res Inst, Panama City, Panama. [Gehrt, Stanley D.] Ohio State Univ, Sch Environm & Nat Resources, Columbus, OH 43210 USA. RP Reynolds, JJH (reprint author), Univ Minnesota, Dept Vet Populat Med, St Paul, MN 55108 USA. EM j.j.h.reynolds@dunelm.org.uk FU University of Minnesota's Institute on the Environment; Cook County Animal and Rabies Control office; Max McGraw Wildlife Foundation; National Science Foundation [EF-0425203, DEB-1413925] FX Funds for this research were provided through University of Minnesota's Institute on the Environment and grants from the Cook County Animal and Rabies Control office as administered through the Environmental Research Program, the Max McGraw Wildlife Foundation and by National Science Foundation grants EF-0425203 and DEB-1413925. The Forest Preserve District of Cook County provided access to the field site and provided logistical support. Numerous technicians assisted with fieldwork, and we are particularly grateful for the contributions of Stephanie Hauver and Suzanne Prange. We also extend thanks to Chris Anchor, Eva Enns, Dan Parmer (deceased), Tiffany Wolf, Kimberly VanderWaal and Donna Alexander for their support in various aspects of the project. NR 80 TC 5 Z9 5 U1 11 U2 59 PU WILEY PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0021-8790 EI 1365-2656 J9 J ANIM ECOL JI J. Anim. Ecol. PD NOV PY 2015 VL 84 IS 6 BP 1720 EP 1731 DI 10.1111/1365-2656.12422 PG 12 WC Ecology; Zoology SC Environmental Sciences & Ecology; Zoology GA CT3XU UT WOS:000362741000027 PM 26172427 ER PT J AU Diefendorf, AF Freeman, KH Wing, SL Currano, ED Mueller, KE AF Diefendorf, Aaron F. Freeman, Katherine H. Wing, Scott L. Currano, Ellen D. Mueller, Kevin E. TI Paleogene plants fractionated carbon isotopes similar to modern plants SO EARTH AND PLANETARY SCIENCE LETTERS LA English DT Article DE Paleocene; Eocene; bighorn basin; biomarkers; lipids; compound specific isotope analyses ID WATER-USE EFFICIENCY; EOCENE THERMAL MAXIMUM; ATMOSPHERIC CO2; BIGHORN BASIN; C3 PLANTS; DISCRIMINATION; DELTA-C-13; PALEOCENE; DEPOSITS; TREES AB The carbon isotope composition (delta C-13) of terrestrial plant biomarkers, such as leaf waxes and terpenoids, provides insights into past carbon cycling. The delta C-13 values of modern plant biomarkers are known to be sensitive to climate and vegetation type, both of which influence fractionation during lipid biosynthesis by altering plant carbon supply and its biochemical allocation. It is not known if fractionation observed in living plants can be used to interpret fossil lipids because plant biochemical characteristics may have evolved during the Cenozoic in response to changes in global climate and atmospheric CO2. The goal of this study was to determine if fractionation during photosynthesis (Delta(leaf)) in the Paleogene was consistent with expectations based on living plants. To study plant fractionation during the Paleogene, we collected samples from eight stratigraphic beds in the Bighorn Basin (Wyoming, USA) that ranged in age from 63 to 53 Ma. For each sample, we measured the delta C-13 of angiosperm biomarkers (triterpenoids and n-alkanes) and, abundance permitting, conifer biomarkers (diterpenoids). Leaf delta C-13 values estimated from different angiosperms biomarkers were consistently 2 parts per thousand lower than leaf delta C-13 values for conifers calculated from diterpenoids. This difference is consistent with observations of living conifers and angiosperms and the consistency among different biomarkers suggests ancient epsilon(lipid) values were similar to those in living plants. From these biomarker-based delta C-13(leaf) values and independent records of atmospheric delta C-13 values, we calculated Delta(leaf). These calculated Delta(leaf) values were then compared to Delta(leaf) values modeled by applying the effects that precipitation and major taxonomic group in living plants have on Delta(leaf) values. Calculated and modeled Delta(leaf) values were offset by less than a permil. This similarity suggests that carbon fractionation in Paleogene plants changed with water availability and major taxonomic group to about the same degree it does today. Further, paleoproxy data suggest at least two of the stratigraphic beds were deposited at times when pCO(2) levels were higher than today. Biomarker data from these beds are not consistent with elevated Delta(leaf) values, possibly because plants adapted carbon uptake and assimilation characteristics to pCO(2) changes over long timescales. (C) 2015 Elsevier B.V. All rights reserved. C1 [Diefendorf, Aaron F.] Univ Cincinnati, Dept Geol, Cincinnati, OH 45221 USA. [Freeman, Katherine H.] Penn State Univ, Dept Geosci, University Pk, PA 16802 USA. [Wing, Scott L.] Smithsonian Inst, Dept Paleobiol, NHB121, Washington, DC 20013 USA. [Currano, Ellen D.] Univ Wyoming, Dept Bot, Laramie, WY 82071 USA. [Mueller, Kevin E.] ARS, USDA, Rangeland Resources Res Unit, Ft Collins, CO 80526 USA. RP Diefendorf, AF (reprint author), Univ Cincinnati, Dept Geol, POB 210013, Cincinnati, OH 45221 USA. EM aaron.diefendorf@uc.edu RI Freeman, Katherine/H-5140-2011; OI Freeman, Katherine/0000-0002-3350-7671; Mueller, Kevin/0000-0002-0739-7472; Wing, Scott/0000-0002-2954-8905 FU National Science Foundation (NSF) [EAR-0844212, EAR-1229114]; Penn State Biogeochemical Research Initiative for Education (BRIE) - NSF IGERT Grant [DGE-9972759]; American Chemical Society PRF Grant [51787-DNI2]; Roland W. Brown Fund of the Smithsonian Institution FX We thank Francesca McInerney and Dana Royer for their thoughtful reviews. This research was supported by the National Science Foundation (NSF) Grants EAR-0844212 (K.H.F.) and EAR-1229114 (A.F.D.), fellowship awards from the Penn State Biogeochemical Research Initiative for Education (BRIE) funded by NSF IGERT Grant DGE-9972759, an American Chemical Society PRF Grant #51787-DNI2 (A.F.D.), and the Roland W. Brown Fund of the Smithsonian Institution (E.D.C). NR 51 TC 11 Z9 11 U1 8 U2 30 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0012-821X EI 1385-013X J9 EARTH PLANET SC LETT JI Earth Planet. Sci. Lett. PD NOV 1 PY 2015 VL 429 BP 33 EP 44 DI 10.1016/j.epsl.2015.07.029 PG 12 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA CS4QE UT WOS:000362060200005 ER PT J AU Rehan, SM Tierney, SM Wcislo, WT AF Rehan, S. M. Tierney, S. M. Wcislo, W. T. TI Evidence for social nesting in Neotropical ceratinine bees SO INSECTES SOCIAUX LA English DT Article DE Subsocial; Facultatively social; Small carpenter bee; Ceratinini; Xylocopinae ID HYMENOPTERA-APIDAE; BIOLOGY; XYLOCOPINAE; EVOLUTION; SOLITARY AB Small carpenter bees (Ceratinini) are a key taxon to understanding the transition from subsocial to social behaviour, as all documented groups are long-lived and tend to their young periodically throughout development, though the behaviour of multiple lineages is little known. This study provides the first evidence for social nesting in three Neotropical species of Ceratina (Ceratinula) from Panama. Social nesting was associated with nest reuse, consistent with the hypothesis of kin associations, and the proportion of nests (per species) that displayed sociality was as follows: C. buscki 5 %; C. rectangulifera 0 %; C. tricolor 6 %; and C. zeteki 23 %. Sociality is always a low-frequency phenomenon in ceratinine bee populations, and generally represents a third or less of the population. The fact that the majority of colonies remain solitary indicates that solitary nesting is adaptive in the studied species. C1 [Rehan, S. M.] Univ New Hampshire, Dept Biol Sci, Durham, NH 03824 USA. [Tierney, S. M.] Univ Adelaide, Sch Biol Sci, Adelaide, SA, Australia. [Wcislo, W. T.] Smithsonian Trop Res Inst, Panama City, Panama. RP Rehan, SM (reprint author), Univ New Hampshire, Dept Biol Sci, Durham, NH 03824 USA. EM sandra.rehan@unh.edu OI Tierney, Simon/0000-0002-8812-6753 FU STRI; Sigma Xi FX This research was supported by an STRI short-term fellowship and a Sigma Xi grant to S. M. R., an STRI postdoctoral fellowship to S. M. T., and general research funds from STRI to W. T. W. NR 19 TC 1 Z9 1 U1 4 U2 17 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 NOV PY 2015 VL 62 IS 4 BP 465 EP 469 DI 10.1007/s00040-015-0425-3 PG 5 WC Entomology SC Entomology GA CR6ZE UT WOS:000361496300010 ER PT J AU Turner, BL Cheesman, AW Condron, LM Reitzel, K Richardson, AE AF Turner, Benjamin L. Cheesman, Alexander W. Condron, Leo M. Reitzel, Kasper Richardson, Alan E. TI Introduction to the special issue: Developments in soil organic phosphorus cycling in natural and agricultural ecosystems SO GEODERMA LA English DT Editorial Material ID MAGNETIC-RESONANCE-SPECTROSCOPY; OXYGEN ISOTOPES; TRANSFORMATIONS; PEDOGENESIS; MARINE; LIMITATION; PHOSPHATE C1 [Turner, Benjamin L.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. [Cheesman, Alexander W.] James Cook Univ, Coll Marine & Environm Sci, Cairns, Qld 4878, Australia. [Condron, Leo M.] Lincoln Univ, Fac Agr & Life Sci, Christchurch 7647, New Zealand. [Reitzel, Kasper] Univ Southern Denmark, Inst Biol, DK-5230 Odense M, Denmark. [Richardson, Alan E.] CSIRO Agr, Canberra, ACT 2601, Australia. RP Turner, BL (reprint author), Smithsonian Trop Res Inst, Apartado 0843-03092, Balboa, Ancon, Panama. EM TurnerBL@si.edu RI Turner, Benjamin/E-5940-2011; Richardson, Alan/I-1903-2012; James Cook University, TESS/B-8171-2012; Cheesman, Alexander/H-5918-2013 OI Turner, Benjamin/0000-0002-6585-0722; Cheesman, Alexander/0000-0003-3931-5766 NR 40 TC 2 Z9 2 U1 10 U2 97 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0016-7061 EI 1872-6259 J9 GEODERMA JI Geoderma PD NOV PY 2015 VL 257 SI SI BP 1 EP 3 DI 10.1016/j.geoderma.2015.06.008 PG 3 WC Soil Science SC Agriculture GA CM0GD UT WOS:000357355500001 ER PT J AU Chen, CR Hou, EQ Condron, LM Bacon, G Esfandbod, M Olley, J Turner, BL AF Chen, C. R. Hou, E. Q. Condron, L. M. Bacon, G. Esfandbod, M. Olley, J. Turner, B. L. TI Soil phosphorus fractionation and nutrient dynamics along the Cooloola coastal dune chronosequence, southern Queensland, Australia SO GEODERMA LA English DT Article; Proceedings Paper CT 2013 Ecological Significance of Soil Organic Phosphorus Meeting CY FEB 04-07, 2013 CL Smithsonian Trop Res Inst, Panama City, PANAMA HO Smithsonian Trop Res Inst DE Soil phosphorus fractionation; Organic phosphorus; Occluded phosphorus; Non-occluded phosphorus; Nutrient dynamics; Cooloola sequence ID ORGANIC PHOSPHORUS; NEW-ZEALAND; PODZOL DEVELOPMENT; EASTERN AUSTRALIA; TRANSFORMATIONS; PEDOGENESIS; LIMITATION; FOREST; SAND; BIOGEOCHEMISTRY AB The amounts and forms of soil phosphorus (P) follow predictable patterns during long-term pedogenesis, but have rarely been examined along subtropical chronosequences. We quantified changes in soil nutrient stocks, foliar nutrient concentrations, and the chemical forms of soil P along the Cooloola chronosequence, a series of coastal dunes spanning ca. 500,000 years of pedogenesis in subtropical Queensland. The total P stock in the upper 30 cm of the soil profile declined continuously with soil age, from 229-237 kg ha(-1) on the youngest soils (40 years old) to 24-28 kg ha(-1) on the oldest soils (195->460 ka). In contrast, total carbon (C) and nitrogen (N) stocks increased initially along the chronosequence and then declined in the oldest soils. As a consequence, soil N:P ratios increased continually throughout the sequence, from <= 4 on the youngest soils to 27-30 on the oldest soils. This indication of increasing biological P stress and ultimately P limitation was further supported by a decline in foliar P concentrations and increasing foliar N:P ratios of two common plant genera along the chronosequence. Sequential P fractionation revealed that although all forms of P declined during pedogenesis, young soils contained low concentrations of primary mineral P and relatively high concentrations of occluded P associated with secondary minerals, suggesting that the parent sand originated from strongly-weathered continental soils. We conclude that the Cooloola chronosequence is an important example of long-term ecosystem development under a subtropical climate, although the pre-weathered nature of the parent sand indicates that the sequence represents a modification of the Walker and Syers model of P transformations during pedogenesis. (C) 2015 Elsevier B.V. All rights reserved. C1 [Chen, C. R.; Hou, E. Q.; Bacon, G.; Esfandbod, M.] Griffith Univ, Environm Futures Res Inst, Nathan, Qld 4111, Australia. [Chen, C. R.; Hou, E. Q.; Bacon, G.; Esfandbod, M.] Griffith Univ, Griffith Sch Environm, Nathan, Qld 4111, Australia. [Condron, L. M.] Lincoln Univ, Agr & Life Sci, Christchurch 7647, New Zealand. [Olley, J.] Griffith Univ, Australian Rivers Inst, Nathan, Qld 4111, Australia. [Turner, B. L.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. RP Chen, CR (reprint author), Griffith Univ, Griffith Sch Environm, Nathan, Qld 4111, Australia. EM c.chen@griffith.edu.au RI Turner, Benjamin/E-5940-2011; Hou, Enqing/A-2056-2016 OI Turner, Benjamin/0000-0002-6585-0722; Hou, Enqing/0000-0003-4864-2347 FU Australian Research Council [FT0990547] FX We would like to thank Ernie Rider for his assistance in the field sampling and the survey of plant species and Marijka Heenan, Xien Long and Yumei Zhang for their assistance in the field sampling. We would also like to thanks Queensland National Parks and Wildlife Service for permission to work at the Cooloola sites. This research was supported under Australian Research Council's Future Fellowship funding scheme (project number FT0990547). NR 43 TC 5 Z9 5 U1 10 U2 76 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0016-7061 EI 1872-6259 J9 GEODERMA JI Geoderma PD NOV PY 2015 VL 257 SI SI BP 4 EP 13 DI 10.1016/j.geoderma.2015.04.027 PG 10 WC Soil Science SC Agriculture GA CM0GD UT WOS:000357355500002 ER PT J AU Roberts, K Defforey, D Turner, BL Condron, LM Peek, S Silva, S Kendall, C Paytan, A AF Roberts, Kathryn Defforey, Delphine Turner, Benjamin L. Condron, Leo M. Peek, Sara Silva, Steve Kendall, Carol Paytan, Adina TI Oxygen isotopes of phosphate and soil phosphorus cycling across a 6500 year chronosequence under lowland temperate rainforest SO GEODERMA LA English DT Article; Proceedings Paper CT 2013 Ecological Significance of Soil Organic Phosphorus Meeting CY FEB 04-07, 2013 CL Smithsonian Trop Res Inst, Panama City, PANAMA HO Smithsonian Trop Res Inst DE Phosphorus; Oxygen isotopes of phosphate; Soil phosphorus cycling; Hedley phosphorus fractionation ID COASTAL DUNE CHRONOSEQUENCE; ORGANIC PHOSPHORUS; NEW-ZEALAND; INORGANIC-PHOSPHATE; TROPICAL FOREST; STABLE-ISOTOPE; PRECISE METHOD; PASTURE SOILS; WATER; PEDOGENESIS AB Phosphorus (P) availability declines during ecosystem development due in part to chemical transformations of P in the soil. Here we report changes in soil P pools and the oxygen isotopic signature of inorganic phosphate (delta O-18(p)) in these pools over a 6500-year soil coastal dune chronosequence in a temperate humid environment. Total P declined from 384 to 129 mg P kg(-1) during the first few hundred years of pedogenesis, due mainly to the depletion of primary mineral Pin the HCl-extractable pool. The delta O-18(p) of HCl-extractable inorganic P initially reflected the signature of the parent material, but shifted over time towards (but not reaching) isotopic equilibrium. In contrast, delta O-18(p) signatures of inorganic P extracted in water and NaHCO3 (approximately 9 and 39 mg P kg(-1), respectively) were variable but consistent with isotopic equilibrium with soil water. In the NaOH-extractable P pool, which doubled from 63 to 128 mg P kg(-1) in the early stages of pedogenesis and then gradually declined, the delta O-18(p) of the extracted inorganic P changed from equilibrium values early in the chronosequence to more depleted signatures in older soils, indicating greater rates of hydrolysis of labile organic P compounds such as DNA and increase involvement in P cycling as overall P availability declines through the sequence. In summary, this application of delta O-18(p) to a long-term soil chronosequence provides novel insight into P dynamics, indicating the importance of efficient recycling through tight uptake and mineralization in maintaining a stable bioavailable P pool during long-term ecosystem development. (C) 2015 Elsevier B.V. All rights reserved. C1 [Roberts, Kathryn; Paytan, Adina] Univ Calif Santa Cruz, Inst Marine Sci, Santa Cruz, CA 95064 USA. [Defforey, Delphine; Paytan, Adina] Univ Calif Santa Cruz, Dept Earth & Planetary Sci, Santa Cruz, CA 95064 USA. [Turner, Benjamin L.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. [Condron, Leo M.] Lincoln Univ, Agr & Life Sci, Christchurch 7647, New Zealand. [Peek, Sara; Silva, Steve; Kendall, Carol] US Geol Survey, Menlo Pk, CA 94025 USA. RP Paytan, A (reprint author), Univ Calif Santa Cruz, Inst Marine Sci, 1156 High St, Santa Cruz, CA 95060 USA. EM apaytan@ucsc.edu RI Turner, Benjamin/E-5940-2011 OI Turner, Benjamin/0000-0002-6585-0722 FU NSF [DEB 1019467] FX Funding was provided by NSF Grant DEB 1019467 to A Paytan. NR 56 TC 7 Z9 8 U1 4 U2 65 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0016-7061 EI 1872-6259 J9 GEODERMA JI Geoderma PD NOV PY 2015 VL 257 SI SI BP 14 EP 21 DI 10.1016/j.geoderma.2015.04.010 PG 8 WC Soil Science SC Agriculture GA CM0GD UT WOS:000357355500003 ER PT J AU Jorgensen, C Turner, BL Reitzel, K AF Jorgensen, Charlotte Turner, Benjamin L. Reitzel, Kasper TI Identification of inositol hexakisphosphate binding sites in soils by selective extraction and solution P-31 NMR spectroscopy SO GEODERMA LA English DT Article; Proceedings Paper CT 2013 Ecological Significance of Soil Organic Phosphorus Meeting CY FEB 04-07, 2013 CL Smithsonian Trop Res Inst, Panama City, PANAMA HO Smithsonian Trop Res Inst DE Phytate; myo-, scyllo-, neo-D-chiro-inositol hexakisphosphate; Oxalate-oxalic acid extraction; Hydrofluoric acid; Organic phosphorus ID ORGANIC PHOSPHORUS TRANSFORMATIONS; MYOINOSITOL HEXAKISPHOSPHATE; WETLAND SOILS; HEXAPHOSPHATE; ALUMINUM; SORPTION; GOETHITE; OXALATE; PHOSPHATE; SEDIMENTS AB Inositol hexakisphosphate (IP6) can constitute the majority of the organic phosphorus in soil. Soil IP6 accumulates through a number of mechanisms, including sorption to metal hydroxides and clays, association with organic matter, and precipitation with cations and on surfaces of metal oxides. However, the relative contributions of these processes remain unknown. We quantified IP6 stereoisomers by NaOH-EDTA extraction and solution P-31 NMR spectroscopy in a series of contrasting soils from natural and agricultural ecosystems, and then used selective extractions to identify associations between IP6 and soil components. Oxalic acid, which extracts amorphous and organically complexed iron and aluminum oxides, extracted the majority of the IP6 from temperate grassland and forest soils, but not from strongly weathered tropical rice soils. In contrast, removal of mineral material by pretreatment with hydrofluoric acid completely removed IP6 from temperate forest soils, but not from temperate grasslands or tropical rice soils. We conclude that the relative importance of IP6 stabilization on organic and mineral components varies markedly among soils, and that oxalate extraction provides a selective procedure for the quantification of IP6 associated with amorphous metal oxides and clays. (C) 2015 Elsevier B.V. All rights reserved. C1 [Jorgensen, Charlotte; Reitzel, Kasper] Univ Southern Denmark, Inst Biol, DK-5230 Odense M, Denmark. [Turner, Benjamin L.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. RP Jorgensen, C (reprint author), Univ Southern Denmark, Inst Biol, Campusvej 55, DK-5230 Odense M, Denmark. EM charlottej@biology.sdu.dk RI Turner, Benjamin/E-5940-2011 OI Turner, Benjamin/0000-0002-6585-0722 FU Danish Council for Independent Research Natural Sciences [1637604]; Villum Kann Rasmussen Centre of Excellence: Centre for Lake Restoration (CLEAR) FX We thank Dayana Agudo for laboratory assistance. Kasper Reitzel was funded by grant #1637604 from the Danish Council for Independent Research Natural Sciences. Charlotte Jorgensen was partly financed by the Villum Kann Rasmussen Centre of Excellence: Centre for Lake Restoration (CLEAR). NR 52 TC 6 Z9 6 U1 8 U2 59 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0016-7061 EI 1872-6259 J9 GEODERMA JI Geoderma PD NOV PY 2015 VL 257 SI SI BP 22 EP 28 DI 10.1016/j.geoderma.2015.03.021 PG 7 WC Soil Science SC Agriculture GA CM0GD UT WOS:000357355500004 ER PT J AU Shih, HT Ng, PKL Christy, JH AF Shih, Hsi-Te Ng, Peter K. L. Christy, John H. TI Uca (Petruca), a new subgenus for the rock fiddler crab Uca panamensis (Stimpson, 1859) from Central America, with comments on some species of the American broad-fronted subgenera SO ZOOTAXA LA English DT Article DE Crustacea; Brachyura; systematics; new subgenus; Uca panamensis; molecular evidence; 28S rDNA; 16S rDNA; cytochrome oxidase subunit I AB Among the fiddler crabs from the Americas, Uca panamensis (Stimpson, 1859) (Crustacea: Decapoda: Ocypodidae) is unusual in its behavior and ecology, living in stony habitats rather than sandy or muddy substrates. This species also has several unusual morphological characters of the carapace and major and minor chelae, and had been placed in either the subgenera Minuca Bott, 1954, or Leptuca Bott, 1973. The armature at the inner corner of the orbital floor, as well as the morphology of the urocardiac ossicles of the gastric mill of U. panamensis, are, however, plesiomorphic characters, and are closer to the condition in species belonging the subgenera Uca and Afruca. Phylogenetic relationships, based on mitochondrial 16S rDNA and cytochrome oxidase subunit I, and nuclear 28S rDNA, supported by its unusual morphological features indicate that this species belongs to its own subgenus. A new subgenus Uca (Petruca) subgen. nov. is herein established for U. panamensis. In addition, the status of Uca thayeri Rathbun, 1900, U. umbratila Crane, 1941, U. virens Salmon & Atsaides, 1968, and U. longisignalis Salmon & Atsaides, 1968, are revised and discussed based on a reappraisal of their phylogenetic relationships. C1 [Shih, Hsi-Te] Natl Chung Hsing Univ, Dept Life Sci, Taichung 402, Taiwan. [Ng, Peter K. L.] Natl Univ Singapore, Fac Sci, Lee Kong Chian Nat Hist Museum, Singapore 117377, Singapore. [Christy, John H.] Smithsonian Trop Res Inst, Panama City, Panama. RP Shih, HT (reprint author), Natl Chung Hsing Univ, Dept Life Sci, 250 Kuo Kuang Rd, Taichung 402, Taiwan. EM htshih@dragon.nchu.edu.tw; peterng@nus.edu.sg; christyj@si.edu FU National Science Council [NSC 98-2621-B-005-001-MY3, 101-2621-B-005-001-MY3]; Ministry of Science and Technology, Executive Yuan, Taiwan [MOST 103-2621-B-005-001] FX This study was supported by grants from the National Science Council (NSC 98-2621-B-005-001-MY3, 101-2621-B-005-001-MY3), Ministry of Science and Technology (MOST 103-2621-B-005-001), Executive Yuan, Taiwan, to HTS. The authors wish to express thanks to Min-Yun Liu and the members of the laboratory of HTS for some molecular work; to Carl Thurman for discussing the status of some species around the Gulf of Mexico; to Christoph Schubart for comments on the confirmation of some species; to Zeehan Jaafar, Carl Thurman, Marcos Tavares, Shirley Lim, Adeline Yong, Benny K. K. Chan, and Pablo D. Ribeiro for providing specimen used in this study; and to Patricia Backwell for providing the color photograph of a courting male Uca panamensis. We acknowledge Peter Castro and one anonymous referee who greatly improved the first version of the manuscript. NR 0 TC 4 Z9 4 U1 3 U2 6 PU MAGNOLIA PRESS PI AUCKLAND PA PO BOX 41383, AUCKLAND, ST LUKES 1030, NEW ZEALAND SN 1175-5326 EI 1175-5334 J9 ZOOTAXA JI Zootaxa PD OCT 30 PY 2015 VL 4034 IS 3 BP 471 EP 494 PG 24 WC Zoology SC Zoology GA CU8OT UT WOS:000363803300003 PM 26624453 ER PT J AU Erwin, DH AF Erwin, Douglas H. TI Eric Davidson (1937-2015) SO SCIENCE LA English DT Biographical-Item C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20013 USA. RP Erwin, DH (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20013 USA. EM erwind@si.edu NR 1 TC 0 Z9 0 U1 1 U2 2 PU AMER ASSOC ADVANCEMENT SCIENCE PI WASHINGTON PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA SN 0036-8075 EI 1095-9203 J9 SCIENCE JI Science PD OCT 30 PY 2015 VL 350 IS 6260 BP 517 EP 517 DI 10.1126/science.aad6065 PG 1 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA CU6RG UT WOS:000363660000032 PM 26516272 ER PT J AU Baird, E Fernandez, DC Wcislo, WT Warrant, EJ AF Baird, Emily Fernandez, Diana C. Wcislo, William T. Warrant, Eric J. TI Flight control and landing precision in the nocturnal bee Megalopta is robust to large changes in light intensity SO FRONTIERS IN PHYSIOLOGY LA English DT Article DE flight control; light intensity; neural summation; Megalopta; Bombus ID FLYING SWEAT BEES; HALICTID BEE; VISION; INSECTS; GENALIS; FLOW AB Like their diurnal relatives, Megalopta genalis use visual information to control flight. Unlike their diurnal relatives, however, they do this at extremely low light intensities. Although Megalopta has developed optical specializations to increase visual sensitivity, theoretical studies suggest that this enhanced sensitivity does not enable them to capture enough light to use visual information to reliably control flight in the rainforest at night. It has been proposed that Megalopta gain extra sensitivity by summing visual information over time While enhancing the reliability of vision, this strategy would decrease the accuracy with which they can detect image motion a crucial cue for flight control. Here, we test this temporal summation hypothesis by investigating how Megalopta's flight control and landing precision is affected by light intensity and compare our findings with the results of similar experiments performed on the diurnal bumblebee Bombus terrestris, to explore the extent to which Megalopta's adaptations to dim light affect their precision. We find that, unlike Bombus, light intensity does not affect flight and landing precision in Megalopta. Overall, we find little evidence that Megalopta uses a temporal summation strategy in dim light, while we find strong support for the use of this strategy in Bombus. C1 [Baird, Emily; Warrant, Eric J.] Lund Univ, Dept Biol, Lund, Sweden. [Fernandez, Diana C.] Univ Lethbridge, Dept Biol Sci, Lethbridge, AB T1K 3M4, Canada. [Wcislo, William T.] Smithsonian Trop Res Inst, Panama City, Panama. RP Baird, E (reprint author), Lund Univ, Dept Biol, Lund, Sweden. EM emily.baird@biol.lu.se RI Baird, Emily/G-8763-2014 OI Baird, Emily/0000-0003-3625-3897 FU Air Force Office of Scientific Research/European Office for Aerospace Research and Development [FA865-507-C-4011, FA8655-08-C-4004]; Swedish Foundation for Strategic Research [2014-4762] FX Air Force Office of Scientific Research/European Office for Aerospace Research and Development (grant numbers FA865-507-C-4011, FA8655-08-C-4004). The Swedish Foundation for Strategic Research (2014-4762). NR 20 TC 4 Z9 4 U1 4 U2 6 PU FRONTIERS MEDIA SA PI LAUSANNE PA PO BOX 110, EPFL INNOVATION PARK, BUILDING I, LAUSANNE, 1015, SWITZERLAND SN 1664-042X J9 FRONT PHYSIOL JI Front. Physiol. PD OCT 28 PY 2015 VL 6 AR 305 DI 10.3389/fphys.2015.00305 PG 7 WC Physiology SC Physiology GA CY9PQ UT WOS:000366739200001 PM 26578977 ER PT J AU Keppel, AG Breitburg, DL Wikfors, GH Burrell, RB Clark, VM AF Keppel, Andrew G. Breitburg, Denise L. Wikfors, Gary H. Burrell, Rebecca B. Clark, Virginia M. TI Effects of co-varying diel-cycling hypoxia and pH on disease susceptibility in the eastern oyster Crassostrea virginica SO MARINE ECOLOGY PROGRESS SERIES LA English DT Article DE Hypoxia; pH; Diel cycle; Multiple stressors; Disease; Oyster ID OXYGEN INTERMEDIATE PRODUCTION; FLOW-CYTOMETRIC ANALYSIS; ATLANTIC BLUE-CRAB; PERKINSUS-MARINUS; OCEAN ACIDIFICATION; CHESAPEAKE BAY; HABITAT DEGRADATION; MYTILUS-EDULIS; CALLINECTES-SAPIDUS; HEMOCYTES WITHDRAWN AB Diel-cycling hypoxia co-occurs with diel-cycling pH in shallow waters that are typically considered as refuge from deep-water hypoxia and are, therefore, targeted for restoration. These areas also tend to be heavily impaired by eutrophication from nutrient over-enrichment which increases the occurrence and severity of hypoxia and pH cycles. We used laboratory experiments to investigate the effects of diel-cycling dissolved oxygen (DO) and co-varying diel-cycling pH on infections of Perkinsus spp. and hemocyte activity in the eastern oyster Crassostrea virginica. Perkinsus marinus is the protistan parasite that causes Dermo disease in oysters. Severe diel-cycling DO increased the acquisition and progression of Perkinsus infections during exposure, and had a legacy effect the next year. Diel-cycling pH did not significantly affect infection dynamics either on its own or in combination with diel-cycling DO. Diel-cycling DO and pH both individually and in conjunction stimulated hemocyte activity, although this stimulated activity may not be effective at preventing Perkinsus infection. The magnitude of cycling conditions is an important consideration when choosing restoration sites, as severe cycling may hinder the re-establishment of oysters by creating areas that serve as reservoirs for parasites that can infect nearby populations. C1 [Keppel, Andrew G.; Breitburg, Denise L.; Burrell, Rebecca B.; Clark, Virginia M.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. [Keppel, Andrew G.; Clark, Virginia M.] Univ Maryland, Marine Estuarine & Environm Sci, College Pk, MD 20742 USA. [Wikfors, Gary H.] NOAA, Fisheries Serv, Northeast Fisheries Sci Ctr, Milford, CT 06460 USA. RP Keppel, AG (reprint author), Smithsonian Environm Res Ctr, POB 28, Edgewater, MD 21037 USA. EM keppela@si.edu FU NOAA Center [NA10-NOS4780138] FX This work was funded by the NOAA Center for Sponsored Coastal Ocean Research (NA10-NOS4780138). The authors thank Jennifer Alix, Jayesh Jariwala, Robbie Bourdon, Cecily Steppe, Heather Soulen, Keira Heggie, Julie Walker, John Morgan, and Joe Miklas for help and assistance as well as the Targett Lab at University of Delaware for advice in developing the experimental system. The authors also thank the anonymous reviewers and colleagues who reviewed this paper prior to submission. NR 86 TC 8 Z9 8 U1 1 U2 30 PU INTER-RESEARCH PI OLDENDORF LUHE PA NORDBUNTE 23, D-21385 OLDENDORF LUHE, GERMANY SN 0171-8630 EI 1616-1599 J9 MAR ECOL PROG SER JI Mar. Ecol.-Prog. Ser. PD OCT 28 PY 2015 VL 538 BP 169 EP 183 DI 10.3354/meps11479 PG 15 WC Ecology; Marine & Freshwater Biology; Oceanography SC Environmental Sciences & Ecology; Marine & Freshwater Biology; Oceanography GA CV2MI UT WOS:000364090400013 ER PT J AU Wiersema, JH McNeill, J Turland, NJ Orli, SS Wagner, WL AF Wiersema, John H. McNeill, John Turland, Nicholas J. Orli, Sylvia S. Wagner, Warren L. TI The foundation of the Melbourne Code Appendices: Announcing a new paradigm for tracking nomenclatural decisions SO TAXON LA English DT Article DE Algae; Angiospermae; angiosperms; binding decisions; Bryophyta; bryophytes; conservation proposals; conserved types; Fossil plants; Fungi; Gymnospermae; gymnosperms; nomenclature database; Pteridophyta; pteridophytes; rejection proposals; Spermatophyta; spermatophytes; suppressed works AB A newly expanded digital resource exists for tracking decisions on all nomenclature proposals potentially contributing to Appendices II-VIII of the International Code of Nomenclature for algae, fungi, and plants. This system owes its origins to the Smithsonian Institution's "Proposals and Disposals" website created by Dan H. Nicolson to track conservation/rejection proposals, but now also treats proposals to suppress works or requests for binding decisions. The new resource was created to accommodate the steadily expanding content of the Appendices in relation to the main body of the Code. A database is now available to generate these Appendices, as has been done for the Melbourne Code. A web interface allows users to query database content in various ways to review proposal histories or to extract all or part of the Appendices. An analysis of the underlying data was conducted to make comparisons between proposals submitted for the various editions of the Code. These include the type of nomenclatural remedy sought, the major group concerned, the numbers of names involved, the timeliness of the proposal evaluation process, the proposal success rate, and the diversity of proposal authorship. The success of proposals was also evaluated by the type of remedy sought and by major groups. C1 [Wiersema, John H.] ARS, USDA, Natl Germplasm Resources Lab, Beltsville Agr Res Ctr BARC West, Beltsville, MD 20705 USA. [McNeill, John] Royal Bot Garden Edinburgh, Edinburgh EH3 5LR, Midlothian, Scotland. [McNeill, John] Royal Ontario Museum, Toronto, ON M5S 2C6, Canada. [Turland, Nicholas J.] Bot Garten, D-14195 Berlin, Germany. [Turland, Nicholas J.] Bot Museum Berlin Dahlem, D-14195 Berlin, Germany. [Orli, Sylvia S.; Wagner, Warren L.] Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, Washington, DC 20013 USA. RP Wiersema, JH (reprint author), ARS, USDA, Natl Germplasm Resources Lab, Beltsville Agr Res Ctr BARC West, Bldg 003, Beltsville, MD 20705 USA. EM john.wiersema@ars.usda.gov NR 8 TC 0 Z9 0 U1 4 U2 5 PU INT ASSOC PLANT TAXONOMY-IAPT PI BRATISLAVA PA C/O INST BOTANY, SLOVAK ACAD SCIENCES DUBRAVSKA CESTA 9, SK-845 23 BRATISLAVA, SLOVAKIA SN 0040-0262 EI 1996-8175 J9 TAXON JI Taxon PD OCT 28 PY 2015 VL 64 IS 5 BP 1021 EP 1027 DI 10.12705/645.11 PG 7 WC Plant Sciences; Evolutionary Biology SC Plant Sciences; Evolutionary Biology GA CU9RY UT WOS:000363884000011 ER PT J AU Lemoine, NP Capdevielle, JN Parker, JD AF Lemoine, Nathan P. Capdevielle, Jillian N. Parker, John D. TI Effects of in situ climate warming on monarch caterpillar (Danaus plexippus) development SO PEERJ LA English DT Article DE Temperature; Pupal mass; Survivorship; Climate change; Growth ID MILKWEED ASCLEPIAS-SYRIACA; INSECT HERBIVORES; ELEVATED CO2; TEMPERATURE; GROWTH; BUTTERFLIES; MEXICO AB Climate warming will fundamentally alter basic life history strategies of many ectothermic insects. In the lab, rising temperatures increase growth rates of lepidopteran larvae but also reduce final pupal mass and increase mortality. Using in situ field warming experiments on their natural host plants, we assessed the impact of climate warming on development of monarch (Danaus plexippus) larvae. Monarchs were reared on Asclepias tuberosa grown under 'Ambient' and 'Warmed' conditions. We quantified time to pupation, final pupal mass, and survivorship. Warming significantly decreased time to pupation, such that an increase of 1 degrees C corresponded to a 0.5 day decrease in pupation time. In contrast, survivorship and pupal mass were not affected by warming. Our results indicate that climate warming will speed the developmental rate of monarchs, influencing their ecological and evolutionary dynamics. However, the effects of climate warming on larval development in other monarch populations and at different times of year should be investigated. C1 [Lemoine, Nathan P.] Florida Int Univ, Dept Biol Sci, Miami, FL 33199 USA. [Capdevielle, Jillian N.] Univ Calif Berkeley, Dept Environm Sci Policy & Management, Berkeley, CA 94720 USA. [Parker, John D.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. RP Lemoine, NP (reprint author), Colorado State Univ, Dept Biol, Ft Collins, CO 80523 USA. EM lemoine.nathan@gmail.com RI Parker, John/F-9761-2010 OI Parker, John/0000-0002-3632-7625 FU NSF DDIG [DEB-1311464]; Smithsonian Graduate Research Fellowship; FIU DYF; NSF REU grant [DBI-156799] FX This work was funded by an NSF DDIG (DEB-1311464), a Smithsonian Graduate Research Fellowship, and an FIU DYF to NPL and an NSF REU grant (DBI-156799) to JDP. The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 30 TC 0 Z9 0 U1 18 U2 56 PU PEERJ INC PI LONDON PA 341-345 OLD ST, THIRD FLR, LONDON, EC1V 9LL, ENGLAND SN 2167-8359 J9 PEERJ JI PeerJ PD OCT 27 PY 2015 VL 3 AR e1293 DI 10.7717/peerj.1293 PG 10 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA CX6HJ UT WOS:000365801500001 PM 26528403 ER PT J AU Belden, LK Hughey, MC Rebollar, EA Umile, TP Loftus, SC Burzynski, EA Minbiole, KPC House, LL Jensen, RV Becker, MH Walke, JB Medina, D Ibanez, R Harris, RN AF Belden, Lisa K. Hughey, Myra C. Rebollar, Eria A. Umile, Thomas P. Loftus, Stephen C. Burzynski, Elizabeth A. Minbiole, Kevin P. C. House, Leanna L. Jensen, Roderick V. Becker, Matthew H. Walke, Jenifer B. Medina, Daniel Ibanez, Roberto Harris, Reid N. TI Panamanian frog species host unique skin bacterial communities SO FRONTIERS IN MICROBIOLOGY LA English DT Article DE amphibian; Batrachochytrium dendrobatidis; chytrid fungus; Kolmogorov-Smirnov measure; microbiome; microbiota; structure-function relationship ID PATHOGEN BATRACHOCHYTRIUM-DENDROBATIDIS; AMPHIBIAN POPULATION DECLINES; SALAMANDER PLETHODON-CINEREUS; HUMAN MICROBIOME; ANTIFUNGAL METABOLITES; CUTANEOUS BACTERIA; MARINE SPONGES; DISEASE; DIVERSITY; CHYTRIDIOMYCOSIS AB Vertebrates, including amphibians, host diverse symbiotic microbes that contribute to host disease resistance. Globally, and especially in montane tropical systems, many amphibian species are threatened by a chytrid fungus, Batrachochytrium dendrobatidis (Bd), that causes a lethal skin disease. Bd therefore may be a strong selective agent on the diversity and function of the microbial communities inhabiting amphibian skin. In Panama, amphibian population declines and the spread of Bd have been tracked. In 2012, we completed a field survey in Panama to examine frog skin microbiota in the context of Bd infection. We focused on three frog species and collected two skin swabs per frog from a total of 136 frogs across four sites that varied from west to east in the time since Bd arrival. One swab was used to assess bacterial community structure using 16S rRNA amplicon sequencing and to determine Bd infection status, and one was used to assess metabolite diversity, as the bacterial production of anti fungal metabolites is an important disease resistance function. The skin microbiota of the three Panamanian frog species differed in OTU (operational taxonomic unit, bacterial species) community composition and metabolite profiles, although the pattern was less strong for the metabolites. Comparisons between frog skin bacterial communities from Panama and the US suggest broad similarities at the phylum level, but key differences at lower taxonomic levels. In our field survey in Panama, across all four sites, only 35 individuals (similar to 26%) were Bd infected. There was no clustering of OTUs or metabolite profiles based on Bd infection status and no clear pattern of west east changes in OTUs or metabolite profiles across the four sites. Overall, our field survey data suggest that different bacterial communities might be producing broadly similar sets of metabolites across frog hosts and sites. Community structure and function may not be as tightly coupled in these skin symbiont microbial systems as it is in many macro systems. C1 [Belden, Lisa K.; Hughey, Myra C.; Jensen, Roderick V.; Becker, Matthew H.; Walke, Jenifer B.; Medina, Daniel] Virginia Tech, Dept Biol Sci, Blacksburg, VA 24061 USA. [Belden, Lisa K.; Rebollar, Eria A.; Ibanez, Roberto] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. [Umile, Thomas P.; Burzynski, Elizabeth A.; Minbiole, Kevin P. C.] Villanova Univ, Dept Chem, Villanova, PA 19085 USA. [Loftus, Stephen C.; House, Leanna L.] Virginia Tech, Dept Stat, Blacksburg, VA USA. [Harris, Reid N.] James Madison Univ, Dept Biol, Harrisonburg, VA 22807 USA. RP Belden, LK (reprint author), Virginia Tech, Dept Biol Sci, Blacksburg, VA 24061 USA. EM belden@vt.edu OI Umile, Thomas/0000-0003-3077-6689 FU National Science Foundation [DEB-1136640, DEB-1136662, DEB-1136602] FX This project was funded by the National Science Foundation (DEB-1136640 to LB, LH, and RJ, DEB-1136662 to KM, and DEB-1136602 to RH). NR 74 TC 7 Z9 7 U1 10 U2 38 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 OCT 27 PY 2015 VL 6 AR 1171 DI 10.3389/fmicb.2015.01171 PG 21 WC Microbiology SC Microbiology GA CV3OK UT WOS:000364168300001 PM 26579083 ER PT J AU van der Heijden, GMF Powers, JS Schnitzer, SA AF van der Heijden, Geertje M. F. Powers, Jennifer S. Schnitzer, Stefan A. TI Lianas reduce carbon accumulation and storage in tropical forests SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA LA English DT Article DE lianas; tropical forests; carbon sequestration; carbon storage; carbon balance ID BARRO COLORADO ISLAND; UNCERTAINTY PRINCIPLE; TREE GROWTH; BIOMASS; PANAMA; PRODUCTIVITY; INFESTATION; ALLOMETRY; MORTALITY; PATTERNS AB Tropical forests store vast quantities of carbon, account for one-third of the carbon fixed by photosynthesis, and are a major sink in the global carbon cycle. Recent evidence suggests that competition between lianas (woody vines) and trees may reduce forest-wide carbon uptake; however, estimates of the impact of lianas on carbon dynamics of tropical forests are crucially lacking. Here we used a large-scale liana removal experiment and found that, at 3 y after liana removal, lianas reduced net above-ground carbon uptake (growth and recruitment minus mortality) by similar to 76% per year, mostly by reducing tree growth. The loss of carbon uptake due to liana-induced mortality was four times greater in the control plots in which lianas were present, but high variation among plots prevented a significant difference among the treatments. Lianas altered how aboveground carbon was stored. In forests where lianas were present, the partitioning of forest aboveground net primary production was dominated by leaves (53.2%, compared with 39.2% in liana-free forests) at the expense of woody stems (from 28.9%, compared with 43.9%), resulting in a more rapid return of fixed carbon to the atmosphere. After 3 y of experimental liana removal, our results clearly demonstrate large differences in carbon cycling between forests with and without lianas. Combined with the recently reported increases in liana abundance, these results indicate that lianas are an important and increasing agent of change in the carbon dynamics of tropical forests. C1 [van der Heijden, Geertje M. F.; Schnitzer, Stefan A.] Marquette Univ, Dept Biol, Milwaukee, WI 53201 USA. [van der Heijden, Geertje M. F.; Powers, Jennifer S.; Schnitzer, Stefan A.] Smithsonian Trop Res Inst, Panama City 084303092, Panama. [van der Heijden, Geertje M. F.] Univ Nottingham, Sch Geog, Nottingham NG7 2RD, England. [Powers, Jennifer S.] Univ Minnesota, Dept Plant Biol, St Paul, MN 55108 USA. [Powers, Jennifer S.] Univ Minnesota, Dept Ecol Evolut & Behav, St Paul, MN 55108 USA. RP van der Heijden, GMF (reprint author), Marquette Univ, Dept Biol, Milwaukee, WI 53201 USA. EM g.m.f.vanderheijden@googlemail.com FU National Science Foundation [DEB-0845071, DEB 1019436, DEB-1019441]; University of Wisconsin-Milwaukee (a Research Growth Initiative grant) FX We thank Scott Mangan and Mike Tobin for their help in establishing the plots, and Oldemar Valdez, Evelyn Sanchez, Boris Bernal, Abelino Valdez, Severino Valdez, Salome Perez, and Guadelupe Alvaro for their contributions to the plant censuses and data management and entry. We also thank Bruce Carlisle, Lindsay Banin, Rachael Gallagher, and two anonymous reviewers for their comments on an earlier version of the manuscript. This work was supported by the National Science Foundation (Grants DEB-0845071 and DEB 1019436, to S.A.S., and DEB-1019441, to J.S.P.), and the University of Wisconsin-Milwaukee (a Research Growth Initiative grant, to S.A.S.). NR 45 TC 12 Z9 12 U1 6 U2 38 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 OCT 27 PY 2015 VL 112 IS 43 BP 13267 EP 13271 DI 10.1073/pnas.1504869112 PG 5 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA CU3WY UT WOS:000363458100051 PM 26460031 ER PT J AU Bacon, CD Silvestro, D Jaramillo, C Smith, BT Chakrabarty, P Antonelli, A AF Bacon, Christine D. Silvestro, Daniele Jaramillo, Carlos Smith, Brian Tilston Chakrabarty, Prosanta Antonelli, Alexandre TI Reply to Lessios and Marko et al.: Early and progressive migration across the Isthmus of Panama is robust to missing data and biases SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA LA English DT Letter ID SPECIATION C1 [Bacon, Christine D.; Jaramillo, Carlos] Smithsonian Trop Res Inst, Ctr Trop Paleoecol & Archaeol, Balboa 084303092, Panama. [Bacon, Christine D.; Silvestro, Daniele; Antonelli, Alexandre] Univ Gothenburg, Dept Biol & Environm Sci, SE-41319 Gothenburg, Sweden. [Silvestro, Daniele] Univ Lausanne, Dept Ecol & Evolut, CH-1015 Lausanne, Switzerland. [Silvestro, Daniele] Swiss Inst Bioinformat, CH-1015 Lausanne, Switzerland. [Smith, Brian Tilston] Amer Museum Nat Hist, Dept Ornithol, New York, NY 10024 USA. [Chakrabarty, Prosanta] Louisiana State Univ, Museum Nat Sci, Dept Biol Sci, Baton Rouge, LA 70803 USA. [Antonelli, Alexandre] Gothenburg Bot Garden, SE-41319 Gothenburg, Sweden. RP Bacon, CD (reprint author), Smithsonian Trop Res Inst, Ctr Trop Paleoecol & Archaeol, Balboa 084303092, Panama. EM christinedbacon@gmail.com RI Chakrabarty, Prosanta/E-3307-2010 NR 11 TC 7 Z9 7 U1 3 U2 16 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 OCT 27 PY 2015 VL 112 IS 43 BP E5767 EP E5768 DI 10.1073/pnas.1515451112 PG 2 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA CU3WY UT WOS:000363458100003 PM 26489656 ER PT J AU Lessios, HA AF Lessios, Harilaos A. TI Appearance of an early closure of the Isthmus of Panama is the product of biased inclusion of data in the metaanalysis SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA LA English DT Letter C1 Smithsonian Trop Res Inst, Balboa, Panama. RP Lessios, HA (reprint author), Smithsonian Trop Res Inst, Box 0843-03092, Balboa, Panama. EM Lessiosh@post.harvard.edu NR 2 TC 5 Z9 5 U1 3 U2 14 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 OCT 27 PY 2015 VL 112 IS 43 BP E5765 EP E5765 DI 10.1073/pnas.1514719112 PG 1 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA CU3WY UT WOS:000363458100001 PM 26489658 ER PT J AU Marko, PB Eytan, RI Knowlton, N AF Marko, Peter B. Eytan, Ron I. Knowlton, Nancy TI Do large molecular sequence divergences imply an early closure of the Isthmus of Panama? SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA LA English DT Letter C1 [Marko, Peter B.] Univ Hawaii Manoa, Dept Biol, Honolulu, HI 96822 USA. [Eytan, Ron I.] Texas A&M Univ, Dept Marine Biol, Galveston, TX 77553 USA. [Knowlton, Nancy] Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, Washington, DC 20013 USA. RP Marko, PB (reprint author), Univ Hawaii Manoa, Dept Biol, Honolulu, HI 96822 USA. EM pmarko@hawaii.edu NR 5 TC 7 Z9 7 U1 2 U2 14 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 OCT 27 PY 2015 VL 112 IS 43 BP E5766 EP E5766 DI 10.1073/pnas.1515048112 PG 1 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA CU3WY UT WOS:000363458100002 PM 26489657 ER PT J AU Miller, JM Kaastra, JS Miller, MC Reynolds, MT Brown, G Cenko, SB Drake, JJ Gezari, S Guillochon, J Gultekin, K Irwin, J Levan, A Maitra, D Maksym, WP Mushotzky, R O'Brien, P Paerels, F de Plaa, J Ramirez-Ruiz, E Strohmayer, T Tanvir, N AF Miller, Jon M. Kaastra, Jelle S. Miller, M. Coleman Reynolds, Mark T. Brown, Gregory Cenko, S. Bradley Drake, Jeremy J. Gezari, Suvi Guillochon, James Gultekin, Kayhan Irwin, Jimmy Levan, Andrew Maitra, Dipankar Maksym, W. Peter Mushotzky, Richard O'Brien, Paul Paerels, Frits de Plaa, Jelle Ramirez-Ruiz, Enrico Strohmayer, Tod Tanvir, Nial TI Flows of X-ray gas reveal the disruption of a star by a massive black hole SO NATURE LA English DT Article ID TIDAL DISRUPTION; EVENTS; GALAXY; CALIBRATION; TELESCOPE; OUTBURST; MISSION; WINDS AB Tidal forces close to massive black holes can violently disrupt stars that make a close approach. These extreme events are discovered via bright X-ray(1-4) and optical/ultraviolet(5,6) flares in galactic centres. Prior studies based on modelling decaying flux trends have been able to estimate broad properties, such as the mass accretion rate(6,7). Here we report the detection of flows of hot, ionized gas in high-resolution X-ray spectra of a nearby tidal disruption event, ASASSN-14li in the galaxy PGC043234. Variability within the absorption-dominated spectra indicates that the gas is relatively close to the black hole. Narrow linewidths indicate that the gas does not stretch over a large range of radii, giving a low volume filling factor. Modest outflow speeds of a few hundred kilometres per second are observed; these are below the escape speed from the radius set by variability. The gas flow is consistent with a rotating wind from the inner, super-Eddington region of a nascent accretion disk, or with a filament of disrupted stellar gas near to the apocentre of an elliptical orbit. Flows of this sort are predicted by fundamental analytical theory(8) and more recent numerical simulations(7,9-14). C1 [Miller, Jon M.; Reynolds, Mark T.; Gultekin, Kayhan] Univ Michigan, Dept Astron, Ann Arbor, MI 48103 USA. [Kaastra, Jelle S.; de Plaa, Jelle] SRON Netherlands Inst Space Res, NL-3584 CA Utrecht, Netherlands. [Kaastra, Jelle S.] Univ Utrecht, Dept Phys & Astron, NL-3508 TA Utrecht, Netherlands. [Kaastra, Jelle S.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [Miller, M. Coleman; Gezari, Suvi; Mushotzky, Richard] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Brown, Gregory; Levan, Andrew] Univ Warwick, Dept Phys, Coventry CV4 7AL, W Midlands, England. [Cenko, S. Bradley; Strohmayer, Tod] Univ Maryland, Joint Space Sci Inst, College Pk, MD 20742 USA. [Cenko, S. Bradley] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA. [Drake, Jeremy J.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. [Guillochon, James] Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, Cambridge, MA 02138 USA. [Irwin, Jimmy; Maksym, W. Peter] Univ Alabama, Dept Phys & Astron, Tuscaloosa, AL 35487 USA. [Maitra, Dipankar] Wheaton Coll, Dept Phys & Astron, Norton, MA 02766 USA. [O'Brien, Paul; Tanvir, Nial] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. [Paerels, Frits] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA. [Paerels, Frits] Columbia Univ, Dept Astron, New York, NY 10027 USA. [Ramirez-Ruiz, Enrico] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. RP Miller, JM (reprint author), Univ Michigan, Dept Astron, 1085 South Univ Ave, Ann Arbor, MI 48103 USA. EM jonmm@umich.edu OI Maksym, Walter/0000-0002-2203-7889; Guillochon, James/0000-0002-9809-8215; Gultekin, Kayhan/0000-0002-1146-0198 FU NASA [NAS8-03060]; Netherlands Organization for Scientific Research (NWO); University of Alabama Research Stimulation Program FX We thank Chandra Director B. Wilkes and the Chandra team for accepting our request for Director's Discretionary Time, XMM-Newton Director N. Schartel and the XMM-Newton team for executing our approved target-of-opportunity program, and Swift Director N. Gehrels and the Swift team for monitoring this important source. J.M.M. is supported by NASA funding, through Chandra and XMM-Newton guest observer programs. The SRON Netherlands Institute for Space Research is supported by The Netherlands Organization for Scientific Research (NWO). J.J.D. was supported by NASA contract NAS8-03060 to the Chandra X-ray Center. W.P.M. is grateful for support by the University of Alabama Research Stimulation Program. NR 37 TC 21 Z9 21 U1 0 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 OCT 22 PY 2015 VL 526 IS 7574 BP 542 EP U173 DI 10.1038/nature15708 PG 6 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA CV1NX UT WOS:000364026100043 PM 26490619 ER PT J AU Vanderburg, A Johnson, JA Rappaport, S Bieryla, A Irwin, J Lewis, JA Kipping, D Brown, WR Dufour, P Ciardi, DR Angus, R Schaefer, L Latham, DW Charbonneau, D Beichman, C Eastman, J McCrady, N Wittenmyer, RA Wright, JT AF Vanderburg, Andrew Johnson, John Asher Rappaport, Saul Bieryla, Allyson Irwin, Jonathan Lewis, John Arban Kipping, David Brown, Warren R. Dufour, Patrick Ciardi, David R. Angus, Ruth Schaefer, Laura Latham, David W. Charbonneau, David Beichman, Charles Eastman, Jason McCrady, Nate Wittenmyer, Robert A. Wright, Jason T. TI A disintegrating minor planet transiting a white dwarf SO NATURE LA English DT Article ID EXCESS INFRARED RADIATION; DEBRIS DISKS; DUSTY DISK; FREQUENCY; SYSTEMS; GD-362; CANDIDATE; ACCRETION; ASTEROIDS; DIFFUSION AB Most stars become white dwarfs after they have exhausted their nuclear fuel (the Sun will be one such). Between one-quarter and one-half of white dwarfs have elements heavier than helium in their atmospheres(1,2), even though these elements ought to sink rapidly into the stellar interiors (unless they are occasionally replenished) (3-5). The abundance ratios of heavy elements in the atmospheres of white dwarfs are similar to the ratios in rocky bodies in the Solar System(6,7). This fact, together with the existence of warm, dusty debris disks(8-13) surrounding about four per cent of white dwarfs(14-16), suggests that rocky debris from the planetary systems of white-dwarf progenitors occasionally pollutes the atmospheres of the stars(17). The total accreted mass of this debris is sometimes comparable to the mass of large asteroids in the Solar System(1). However, rocky, disintegrating bodies around a white dwarf have not yet been observed. Here we report observations of a white dwarf-WD 1145+017-being transited by at least one, and probably several, disintegrating planetesimals, with periods ranging from 4.5 hours to 4.9 hours. The strongest transit signals occur every 4.5 hours and exhibit varying depths (blocking up to 40 per cent of the star's brightness) and asymmetric profiles, indicative of a small object with a cometary tail of dusty effluent material. The star has a dusty debris disk, and the star's spectrum shows prominent lines from heavy elements such as magnesium, aluminium, silicon, calcium, iron, and nickel. This system provides further evidence that the pollution of white dwarfs by heavy elements might originate from disrupted rocky bodies such as asteroids and minor planets. C1 [Vanderburg, Andrew; Johnson, John Asher; Bieryla, Allyson; Irwin, Jonathan; Lewis, John Arban; Kipping, David; Brown, Warren R.; Angus, Ruth; Schaefer, Laura; Latham, David W.; Charbonneau, David; Eastman, Jason] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Rappaport, Saul] MIT, Dept Phys, Cambridge, MA 02139 USA. [Rappaport, Saul] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Kipping, David] Columbia Univ, Dept Astron, New York, NY 10027 USA. [Dufour, Patrick] Univ Montreal, Dept Phys, Inst Rech Exoplanetes, Montreal, PQ H3C 3J7, Canada. [Ciardi, David R.; Beichman, Charles] CALTECH, NASA, Exoplanet Sci Inst, Pasadena, CA 91125 USA. [Angus, Ruth] Univ Oxford, Dept Phys, Oxford OX1 3RH, England. [McCrady, Nate] Univ Montana, Dept Phys & Astron, Missoula, MT 59812 USA. [Wittenmyer, Robert A.] Univ New S Wales, Sch Phys, Sydney, NSW 2052, Australia. [Wittenmyer, Robert A.] Univ New S Wales, Australian Ctr Astrobiol, Sydney, NSW 2052, Australia. [Wright, Jason T.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Wright, Jason T.] Penn State Univ, Ctr Exoplanets & Habitable Worlds, University Pk, PA 16802 USA. RP Vanderburg, A (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM avanderburg@cfa.harvard.edu OI Lewis, John/0000-0001-5199-3522; Wright, Jason/0000-0001-6160-5888; Schaefer, Laura/0000-0003-2915-5025; Ciardi, David/0000-0002-5741-3047 FU National Science Foundation Graduate Research Fellowship [DGE 1144152]; David and Lucile Packard Foundation; Alfred P. Sloan Foundation; Pennsylvania State University; Eberly College of Science; Pennsylvania Space Grant Consortium; David and Lucile Packard Fellowship for Science and Engineering; National Science Foundation [AST-0807690, AST-1109468, AST-1004488]; John Templeton Foundation FX We thank B. Croll, D. Veras, M. Holman, R. Loomis, J. Becker, K. Deck, H. Schlichting, H. Lin, A. Loeb, and D. Osip for discussions and assistance. We thank C. Allinson, S. Dillet, D. Frostig, A. Johnson, D. Hellstrom, S. Johnson, B. Peak, and T. Reneau for conducting MINERVA observations. We thank M. Wyatt for suggesting how to present Supplementary Fig. 8. A.V. is supported by a National Science Foundation Graduate Research Fellowship (grant DGE 1144152). J. A. J. is supported by grants from the David and Lucile Packard Foundation and the Alfred P. Sloan Foundation. The Center for Exoplanets and Habitable Worlds is supported by Pennsylvania State University, the Eberly College of Science, and the Pennsylvania Space Grant Consortium. The MEarth Team acknowledges funding from the David and Lucile Packard Fellowship for Science and Engineering (to D. C.), the National Science Foundation under grants AST-0807690, AST-1109468, and AST-1004488 (Alan T. Waterman Award), and a grant from the John Templeton Foundation. The opinions expressed here are those of the authors and do not necessarily reflect the views of the John Templeton Foundation. This research has made use of NASA's Astrophysics Data System, the SIMBAD database and VizieR catalog access tool operated at the Centre de Donnees astronomiques de Strasbourg, France. Some of the data presented here were obtained from the Mikulski Archive for Space Telescopes (MAST). This paper includes data from the Kepler/K2 mission, the Wide-field Infrared Survey Explorer, the MMT Observatory, the Sloan Digital Sky Survey (SDSS-III), the National Geographic Society Palomar Observatory Sky Atlas (POSS-I) and the W.M. Keck Observatory. MINERVA is made possible by contributions from its collaborating institutions and Mt Cuba Astronomical Foundation, the David and Lucile Packard Foundation, the National Aeronautics and Space Administration, and the Australian Research Council. We acknowledge the cultural significance of the summit of Maunakea within the indigenous Hawai'ian community. We are grateful for the opportunity to conduct observations from this mountain. NR 30 TC 47 Z9 47 U1 3 U2 11 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 OCT 22 PY 2015 VL 526 IS 7574 BP 546 EP 549 DI 10.1038/nature15527 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA CV1NX UT WOS:000364026100044 PM 26490620 ER PT J AU David, B Aplin, K Petchey, F Skelly, R Mialanes, J Jones-Amin, H Stanisic, J Barker, B Lamb, L AF David, Bruno Aplin, Ken Petchey, Fiona Skelly, Robert Mialanes, Jerome Jones-Amin, Holly Stanisic, John Barker, Bryce Lamb, Lara TI Kumukumu 1, a hilltop site in the Aird Hills: Implications for occupational trends and dynamics in the Kikori River delta, south coast of Papua New Guinea SO QUATERNARY INTERNATIONAL LA English DT Article DE Headhunting; Defensive site; Aird Hills; Papua New Guinea; Archaeology; Porome ID GULF PROVINCE; COLONIZATION; REGION; CULT; OAC; AGE AB We report on archaeological excavations undertaken at Kumukumu 1 atop the dense rainforest-clad Aird Hills of the Kikori river delta islands, south coast of Papua New Guinea. Results indicate exploitation of the nearby environment, including the gathering of some 200 million shellfish from riverine habitats at the base of the hill some 600 years ago, and deposition of shell remains onto hilltop middens. We ask what the implications of such a site in a defensive location on the upper, steep hillslope of Kumukumu hill are for regional occupation and dynamics. We conclude that the hinterland-marine fringe islands of the river deltas that include the site of Kumukumu 1 were especially sensitive to heightened cross-cultural influences and inter-group raids and competition, leading to accelerated processes of centralisation and aggrandisement among some groups, and the subjugation, fragmentation and dispersal of less powerful neighbouring groups. (C) 2014 Elsevier Ltd and INQUA. All rights reserved. C1 [David, Bruno; Skelly, Robert; Mialanes, Jerome; Jones-Amin, Holly] Monash Univ, Monash Indigenous Ctr, Clayton, Vic 3800, Australia. [Aplin, Ken] Smithsonian Inst, Div Mammals, Natl Museum Nat Hist, Washington, DC 20013 USA. [Petchey, Fiona] Univ Waikato, Radiocarbon Dating Lab, Hamilton 3240, New Zealand. [Stanisic, John] Queensland Museum, South Brisbane, Qld 4101, Australia. [Barker, Bryce; Lamb, Lara] Univ So Queensland, Publ Memory Ctr, Sch Humanities & Commun, Toowoomba, Qld 4350, Australia. RP David, B (reprint author), Monash Univ, Monash Indigenous Ctr, Clayton, Vic 3800, Australia. EM bruno.david@monash.edu; aplink@si.edu; fpetchey@waikato.ac.nz; robert.skelly@monash.edu; jerome.mialanes@monash.edu; hjjon2@student.monash.edu; john.stanisic@qm.qld.gov.au; bryce.barker@usq.edu.au; lamb@usq.edu.au OI Mialanes, Jerome/0000-0002-6790-7542; David, Bruno/0000-0002-8567-6135 FU Australian Research Council Discovery grant; QEII Fellowship [DP0877782]; DORA [DP130102514] FX We gratefully thank the people of Ero, Bernard Sanderre, Cathy Alex and the staff at Community Development Initiative (CDI) at Kikori for their support and friendship in the field; Dirio Epi and his family for their welcome in the field; Marawake Umoia, Napai Veiomo and Nick Araho for assisting with the excavations at Kumukumu 1; Ray Cas (Monash University) for identification of the archaeological stone; Ursula Pietrzak and Nicole Pancer for undertaking the particle size analyses and sediment pHs; Steve Morton (Monash University) for taking the photographs for Fig. 5; Kara Rasmanis for drafting Figs. 1, 3 and 7; Georgina Skelly for calculating the area of dense shell midden at Feature 6; Jeff Fox for conserving the bone needle; Angela Frost for assistance with the faunal analysis; and Ian McNiven, Sean Ulm and three anonymous referees for useful comments on an earlier draft of this paper. This project was undertaken with the generous assistance of Australian Research Council Discovery grant and QEII Fellowship DP0877782 and DORA (to BD) DP130102514. NR 45 TC 1 Z9 1 U1 2 U2 3 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 1040-6182 EI 1873-4553 J9 QUATERN INT JI Quat. Int. PD OCT 22 PY 2015 VL 385 BP 7 EP 26 DI 10.1016/j.quaint.2014.06.058 PG 20 WC Geography, Physical; Geosciences, Multidisciplinary SC Physical Geography; Geology GA CT9IH UT WOS:000363130000002 ER PT J AU Boylan-Kolchin, M Weisz, DR Johnson, BD Bullock, JS Conroy, C Fitts, A AF Boylan-Kolchin, Michael Weisz, Daniel R. Johnson, Benjamin D. Bullock, James S. Conroy, Charlie Fitts, Alex TI The Local Group as a time machine: studying the high-redshift Universe with nearby galaxies SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies: evolution; galaxies: high-redshift; Local Group; cosmology: theory ID STAR-FORMATION HISTORIES; MILKY-WAY SATELLITES; UV LUMINOSITY FUNCTION; INITIAL MASS FUNCTION; DEEP FIELD CAMPAIGN; DWARF GALAXIES; COSMIC REIONIZATION; DARK-MATTER; 1ST GALAXIES; POPULATION AB We infer the UV luminosities of Local Group galaxies at early cosmic times (z similar to 2 and z similar to 7) by combining stellar population synthesis modelling with star formation histories derived from deep colour-magnitude diagrams constructed from Hubble Space Telescope (HST) observations. Our analysis provides a basis for understanding high-z galaxies - including those that may be unobservable even with the James Webb Space Telescope (JWST) - in the context of familiar, well-studied objects in the very low-z Universe. We find that, at the epoch of reionization, all Local Group dwarfs were less luminous than the faintest galaxies detectable in deep HST observations of blank fields. We predict that JWST will observe z similar to 7 progenitors of galaxies similar to the Large Magellanic Cloud today; however, the HST Frontier Fields initiative may already be observing such galaxies, highlighting the power of gravitational lensing. Consensus reionization models require an extrapolation of the observed blank-field luminosity function (LF) at z approximate to 7 by at least 2 orders of magnitude in order to maintain reionization. This scenario requires the progenitors of the Fornax and Sagittarius dwarf spheroidal galaxies to be contributors to the ionizing background at z similar to 7. Combined with numerical simulations, our results argue for a break in the UV LF from a faint-end slope of alpha similar to -2 at M-UV less than or similar to -13 to alpha similar to -1.2 at lower luminosities. Applied to photometric samples at lower redshifts, our analysis suggests that HST observations in lensing fields at z similar to 2 are capable of probing galaxies with luminosities comparable to the expected progenitor of Fornax. C1 [Boylan-Kolchin, Michael; Fitts, Alex] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA. [Weisz, Daniel R.; Conroy, Charlie] Univ Washington, Dept Astron, Seattle, WA 98195 USA. [Johnson, Benjamin D.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Bullock, James S.] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA. RP Boylan-Kolchin, M (reprint author), Univ Texas Austin, Dept Astron, 2515 Speedway,Stop C1400, Austin, TX 78712 USA. EM mbk@astro.as.utexas.edu OI Boylan-Kolchin, Michael/0000-0002-9604-343X; Weisz, Daniel/0000-0002-6442-6030 FU NASA through HST from the Space Telescope Science Institute (STScI) under NASA [AR-12836, AR-13888, NAS5-26555]; NASA - STScI [HST-HF-51331.01]; Packard Foundation Fellowship; National Science Foundation [OCI-1053575] FX MB-K thanks Anahita Alavi, Hakim Atek, Steve Finkelstein, and Pascal Oesch for providing data in tabular form and Brant Robertson, Steve Finkelstein, and Cole Miller for helpful discussions. Support for this work was provided by NASA through HST theory grants (programmes AR-12836 and AR-13888) from the Space Telescope Science Institute (STScI), which is operated by the Association of Universities for Research in Astronomy (AURA), Inc., under NASA contract NAS5-26555. DRW is supported by NASA through Hubble Fellowship grant HST-HF-51331.01 awarded by STScI. CC is supported by a Packard Foundation Fellowship. This work used computational resources of the University of Maryland and those granted the Extreme Science and Engineering Discovery Environment (XSEDE), which is supported by National Science Foundation grant number OCI-1053575. Much of the analysis in this paper relied on the PYTHON packages NUMPY (Van Der Walt, Colbert & Varoquaux 2011), SCIPY (Jones et al. 2001), MATPLOTLIB (Hunter 2007), and IPYTHON (Perez & Granger 2007); we are very grateful to the developers of these tools. This research has made extensive use of NASA's Astrophysics Data System and the arXiv eprint service at arxiv.org. NR 82 TC 12 Z9 12 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 OCT 21 PY 2015 VL 453 IS 2 BP 1503 EP 1512 DI 10.1093/mnras/stv1736 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CU4GQ UT WOS:000363486000027 ER PT J AU Smith, DJB Hayward, CC AF Smith, Daniel J. B. Hayward, Christopher C. TI Deriving star formation histories from photometry using energy balance spectral energy distribution modelling SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE radiative transfer; dust, extinction; galaxies: fundamental parameters; galaxies: ISM; galaxies: stellar content; infrared: galaxies ID DIGITAL SKY SURVEY; SMOOTHED PARTICLE HYDRODYNAMICS; DWARF IRREGULAR GALAXIES; COLOR-MAGNITUDE DIAGRAMS; RESOLVED STELLAR POPULATIONS; LARGE-MAGELLANIC-CLOUD; BROAD-BAND PHOTOMETRY; HERSCHEL-ATLAS; MOVING-MESH; METALLICITY HISTORIES AB Panchromatic spectral energy distribution fitting is a critical tool for determining the physical properties of distant galaxies, such as their stellar mass and star formation rate. One widely used method is the publicly available MAGPHYS code. We build on our previous analysis by presenting some modifications which enable MAGPHYS to automatically estimate galaxy star formation histories (SFHs), including uncertainties, based on ultraviolet to far-infrared photometry. We use state-of-the art synthetic photometry derived by performing three-dimensional dust radiative transfer on hydrodynamic simulations of isolated disc and merging galaxies to test how well the modified MAGPHYS is able to recover SFHs under idealized conditions, where the true SFH is known. We find that while the SFH of the model with the best fit to the synthetic photometry is a poor representation of the true SFH (showing large variations with the line of sight to the galaxy and spurious bursts of star formation), median-likelihood SFHs generated by marginalizing over the default MAGPHYS libraries produce robust estimates of the smoothly varying isolated disc simulation SFHs. This preference for the median-likelihood SFH is quantitatively underlined by our estimates of chi(2)(SFH) SFH (analogous to the chi(2) goodness-of-fit estimator) and Delta M/M (the integrated absolute mass discrepancy between the model and true SFH) that strongly prefer the median-likelihood SFHs over those that best fit the UV-to-far-IR photometry. In contrast, we are unable to derive a good estimate of the SFH for the merger simulations (either best fit or median likelihood) despite being able to obtain a reasonable fit to the simulated photometry, likely because the analytic SFHs with bursts superposed in the standard MAGPHYS library are insufficiently general/realistic. C1 [Smith, Daniel J. B.] Univ Hertfordshire, Sci & Technol Res Inst, Ctr Astrophys, Hatfield AL10 9AB, Herts, England. [Hayward, Christopher C.] CALTECH, TAPIR 350 17, Pasadena, CA 91125 USA. [Hayward, Christopher C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Smith, DJB (reprint author), Univ Hertfordshire, Sci & Technol Res Inst, Ctr Astrophys, Hatfield AL10 9AB, Herts, England. EM daniel.j.b.smith@gmail.com OI Smith, Daniel/0000-0001-9708-253X; Hayward, Christopher/0000-0003-4073-3236 FU Santander Universities partnership scheme; Gordon and Betty Moore Foundation FX The authors would like to thank the reviewer, Elisabete da Cunha, for an insightful report that improved the quality of this paper. We also wish to thank Charlie Conroy, Phil Hopkins and Ben Johnson for useful discussions. DJBS and CCH would like to acknowledge a financial award from the Santander Universities partnership scheme. CCH is grateful to the Gordon and Betty Moore Foundation for financial support and the University of Hertfordshire for hospitality. DJBS would like the thank the Theoretical AstroPhysics Including Relativity and Cosmology (TAPIR) group at Caltech for their hospitality. This research has made use of NASA's Astrophysics Data System Bibliographic Services. NR 101 TC 8 Z9 8 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 OCT 21 PY 2015 VL 453 IS 2 BP 1597 EP 1607 DI 10.1093/mnras/stv1727 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CU4GQ UT WOS:000363486000034 ER PT J AU Yamazaki, R Loeb, A AF Yamazaki, Ryo Loeb, Abraham TI Optical inverse-Compton emission from clusters of galaxies SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE acceleration of particles; radiation mechanisms: non-thermal; galaxies: clusters: general; intergalactic medium ID DIFFUSIVE SHOCK ACCELERATION; GAMMA-RAY EMISSION; HARD X-RAY; NONTHERMAL ELECTRON ACCELERATION; LARGE-SCALE STRUCTURE; COMA CLUSTER; INTRACLUSTER LIGHT; PARTICLE-ACCELERATION; MAGNETIC-FIELDS; INTERGALACTIC SHOCKS AB Shocks around clusters of galaxies accelerate electrons which upscatter the cosmic microwave background photons to higher energies. We use an analytical model to calculate this inverse-Compton (IC) emission, taking into account the effects of additional energy losses via synchrotron and Coulomb scattering. We find that the surface brightness of the optical IC emission increases with redshift and halo mass. The IC emission surface brightness, 32-34 mag arcsec(-2), for massive clusters is potentially detectable by the newly developed Dragonfly Telephoto Array. C1 [Yamazaki, Ryo] Aoyama Gakuin Univ, Dept Phys & Math, Sagamihara, Kanagawa 2525258, Japan. [Yamazaki, Ryo; Loeb, Abraham] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Yamazaki, R (reprint author), Aoyama Gakuin Univ, Dept Phys & Math, 5-10-1 Fuchinobe, Sagamihara, Kanagawa 2525258, Japan. EM ryo@phys.aoyama.ac.jp FU Ministry of Education, Culture, Sports, Science, and Technology (MEXT) of Japan [15K05088]; NSF [AST-1312034]; ISSI (Bern) FX We thank Roberto Abraham, Yutaka Fujita, Hyesung Kang, Yutaka Ohira, Kouji Ohta, Dongsu Ryu, Lorenzo Sironi, Shuta Tanaka, Makoto Uemura, and Pieter van Dokkum for valuable comments. We also thank the anonymous referee for valuable comments to improve the paper. This work was supported in part by grant-in-aid from the Ministry of Education, Culture, Sports, Science, and Technology (MEXT) of Japan, no. 15K05088 (RY) and NSF grant AST-1312034 (AL). RY also thank ISSI (Bern) for support of the team 'Physics of the Injection of Particle Acceleration at Astrophysical, Heliospheric, and Laboratory Collisionless Shocks'. NR 89 TC 2 Z9 2 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 OCT 21 PY 2015 VL 453 IS 2 BP 1990 EP 1998 DI 10.1093/mnras/stv1757 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CU4GQ UT WOS:000363486000064 ER PT J AU Szalai, T Vinkoo, J Saarneczky, K Takaats, K Benko, JM Kelemen, J Kuli, Z Silverman, JM Marion, GH Wheeler, C AF Szalai, Tamas Vinko, Jozsef Sarneczky, Krisztian Takats, Katalin Benko, Jozsef M. Kelemen, Janos Kuli, Zoltan Silverman, Jeffrey M. Marion, G. Howie Wheeler, Craig TI The early phases of the Type Iax supernova SN 2011ay SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE supernovae: general; supernovae: individual: SN 2011ay ID HIGH-VELOCITY FEATURES; LOW-LUMINOSITY; LIGHT-CURVE; SPECTRA; 2005HK; EXPLOSION; 2002CX; SPECTROSCOPY; PROGENITOR; TELESCOPE AB We present a detailed study of the early phases of the peculiar supernova (SN) 2011ay based on BVRI photometry obtained at Konkoly Observatory, Hungary, and optical spectra taken with the Hobby-Eberly Telescope at McDonald Observatory, Texas. The spectral analysis carried out with SYN++ and SYNAPPS confirms that SN 2011ay belongs to the recently defined class of SNe Iax, which is also supported by the properties of its light and colour curves. The estimated photospheric temperature around maximum light, T-phot similar to 8000 K, is lower than in most SNe Ia, which results in the appearance of strong Fe II features in the spectra of SN 2011ay, even during the early phases. We also show that strong blending with metal features (those of Ti II, FeII, Co II) makes the direct analysis of the broad spectral features very difficult, and this may be true for all SNe Iax. We find two alternative spectrum models that both describe the observed spectra adequately, but their photospheric velocities differ by at least similar to 3000 km s(-1). The quasi-bolometric light curve of SN 2011ay has been assembled by integrating the ultraviolet-optical spectral energy distributions. Fitting a modified Arnett model to L-bol(t), the moment of explosion and other physical parameters, i. e. the rise time to maximum, the Ni-56 mass and the total ejecta mass are estimated as t(rise) similar to 14 +/- 1 d, M-Ni similar to 0.22 +/- 0.01M(circle dot) and M-ej similar to 0.8M(circle dot), respectively. C1 [Szalai, Tamas; Vinko, Jozsef; Takats, Katalin] Univ Szeged, Dept Opt & Quantum Elect, H-6720 Szeged, Hungary. [Vinko, Jozsef; Silverman, Jeffrey M.; Marion, G. Howie; Wheeler, Craig] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA. [Sarneczky, Krisztian; Benko, Jozsef M.; Kelemen, Janos; Kuli, Zoltan] Konkoly Observ Budapest, MTA CSFK, H-1121 Budapest, Hungary. [Sarneczky, Krisztian] ELTE Gothard Lendulet Res Grp, H-9700 Szombathely, Hungary. [Takats, Katalin] Univ Andres Bello, Dept Ciencias Fis, Santiago, Chile. [Takats, Katalin] Millennium Inst Astrophys, Santiago 7820436, Chile. [Kuli, Zoltan] Hungarian Astron Assoc, H-1300 Budapest, Hungary. [Marion, G. Howie] Harvard Smithsonian Ctr Astrophys, Cambridge, MA USA. RP Szalai, T (reprint author), Univ Szeged, Dept Opt & Quantum Elect, Dom Ter 9, H-6720 Szeged, Hungary. EM szaszi@titan.physx.u-szeged.hu FU Hungarian NKFIH OTKA [NN107637, K104607, K83790, K115709]; OTKA Postdoctoral Fellowship [PD112325]; NSF [AST 11-09881]; Lendulet Young Researchers Program of the Hungarian Academy of Sciences; ESA PECS [4000110889/14/NL/NDe]; NSF Astronomy and Astrophysics Postdoctoral Fellowship [AST-1302771]; Gemini-CONICYT Fund [32110024]; CONICYT through the FONDECYT [3150473]; Ministry of Economy, Development, and Tourism's Millennium Science Initiative [IC12009] FX This work has been supported by the Hungarian NKFIH OTKA Grants NN107637, K104607, K83790 and K115709. TS is supported by the OTKA Postdoctoral Fellowship PD112325. JCW's Supernova group at the UT Austin is supported by NSF Grant AST 11-09881 grant. KS and JMB are supported by the Lendulet-2009 Young Researchers Program of the Hungarian Academy of Sciences. KS is also supported by ESA PECS Contract No. 4000110889/14/NL/NDe. JMS is supported by an NSF Astronomy and Astrophysics Postdoctoral Fellowship under award AST-1302771. KT was supported by the Gemini-CONICYT Fund, allocated to the project no. 32110024, by CONICYT through the FONDECYT grant 3150473 and by the Ministry of Economy, Development, and Tourism's Millennium Science Initiative through grant IC12009, awarded to the Millennium Institute of Astrophysics, MAS. An anonymous referee provided a thorough report that helped us to improve the previous version of this paper. Work of anonymous referee truly appreciated. We also thank R. J. Foley for providing the Lick/Kast spectra of SN 2011ay. NR 57 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 OCT 21 PY 2015 VL 453 IS 2 BP 2103 EP 2114 DI 10.1093/mnras/stv1776 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CU4GQ UT WOS:000363486000076 ER PT J AU De Cicco, M Marinucci, A Bianchi, S Piconcelli, E Violino, G Vignali, C Nicastro, F AF De Cicco, M. Marinucci, A. Bianchi, S. Piconcelli, E. Violino, G. Vignali, C. Nicastro, F. TI Deep X-ray spectroscopy and imaging of the Seyfert 2 galaxy, ESO 138-G001 SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies: active; galaxies: Seyfert; X-rays: individual: ESO138-G001 ID ACTIVE GALACTIC NUCLEI; XMM-NEWTON; WARM ABSORBER; EMISSION-LINE; COLD MATTER; BLACK-HOLE; ABSORPTION; RESOLUTION; CHANDRA; ENERGY AB We present a spectral and imaging analysis of the XMM-Newton and Chandra observations of the Seyfert 2 galaxy ESO138-G001, with the aim of characterizing the circumnuclear material responsible for the soft (0.3-2.0 keV) and hard (5-10 keV) X-ray emission. We confirm that the source is absorbed by Compton-thick gas. However, if a self-consistent model of reprocessing from cold toroidal material is used (MYTORUS), a possible scenario requires the absorber to be inhomogenous, its column density along the line of sight being larger than the average column density integrated over all lines of sight through the torus. The iron emission line may be produced by moderately ionized iron (Fe XII-Fe XIII), as suggested by the shifted centroid energy and the low K beta/K alpha flux ratio. The soft X-ray emission is dominated by emission features, whose main excitation mechanism appears to be photoionization, as confirmed by line diagnostics and the use of self-consistent models (CLOUDY). C1 [De Cicco, M.; Marinucci, A.; Bianchi, S.] Univ Roma Tre, Dipartimento Matemat & Fis, I-00146 Rome, Italy. [Piconcelli, E.] Osserv Astron Roma, INAF, I-00040 Monte Porzio Catone, PM, Italy. [Violino, G.] Univ Hertfordshire, Ctr Astrophys Res, Hatfield AL10 9AB, Herts, England. [Vignali, C.] Univ Bologna, Dipartimento Fis & Astron, I-40127 Bologna, Italy. [Vignali, C.] Osservatorio Astron Bologna, INAF, I-40127 Bologna, Italy. [Nicastro, F.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Nicastro, F.] Univ Crete, Dept Phys, GR-71003 Iraklion, Crete, Greece. RP De Cicco, M (reprint author), Univ Roma Tre, Dipartimento Matemat & Fis, Via Vasca Navale 84, I-00146 Rome, Italy. EM m.decicco89@gmail.com; marinucci@fis.uniroma3.it RI Bianchi, Stefano/B-4804-2010; Vignali, Cristian/J-4974-2012; OI Bianchi, Stefano/0000-0002-4622-4240; Vignali, Cristian/0000-0002-8853-9611; Nicastro, Fabrizio/0000-0002-6896-1364; piconcelli, enrico/0000-0001-9095-2782 NR 52 TC 1 Z9 1 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 OCT 21 PY 2015 VL 453 IS 2 BP 2155 EP 2162 DI 10.1093/mnras/stv1702 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CU4GQ UT WOS:000363486000081 ER PT J AU Medvedev, ES Meshkov, VV Stolyarov, AV Gordon, IE AF Medvedev, Emile S. Meshkov, Vladimir V. Stolyarov, Andrey V. Gordon, Iouli E. TI Peculiarities of high-overtone transition probabilities in carbon monoxide revealed by high-precision calculation SO JOURNAL OF CHEMICAL PHYSICS LA English DT Article ID DIMENSIONAL EIGENVALUE PROBLEM; DIPOLE-MOMENT FUNCTION; LINE LISTS; GROUND-STATE; CO; INTENSITIES; ACCURACY; EQUATION AB In the recent work devoted to the calculation of the rovibrational line list of the CO molecule [G. Li et al., Astrophys. J., Suppl. Ser. 216, 15 (2015)], rigorous validation of the calculated parameters including intensities was carried out. In particular, the Normal Intensity Distribution Law (NIDL) [E. S. Medvedev, J. Chem. Phys. 137, 174307 (2012)] was employed for the validation purposes, and it was found that, in the original CO line list calculated for large changes of the vibrational quantum number up to Delta n = 41, intensities with Delta n > 11 were unphysical. Therefore, very high overtone transitions were removed from the published list in Li et al. Here, we show how this type of validation is carried out and prove that the quadruple precision is indispensably required to predict the reliable intensities using the conventional 32-bit computers. Based on these calculations, the NIDL is shown to hold up for the 0 -> n transitions till the dissociation limit around n = 83, covering 45 orders of magnitude in the intensity. The low-intensity 0 -> n transition predicted in the work of Medvedev [Determination of a new molecular constant for diatomic systems. Normal intensity distribution law for overtone spectra of diatomic and polyatomic molecules and anomalies in overtone absorption spectra of diatomic molecules, Institute of Chemical Physics, Russian Academy of Sciences, Chernogolovka, 1984] at n = 5 is confirmed, and two additional "abnormal" intensities are found at n = 14 and 23. Criteria for the appearance of such "anomalies" are formulated. The results could be useful to revise the high-overtone molecular transition probabilities provided in spectroscopic databases. (C) 2015 AIP Publishing LLC. C1 [Medvedev, Emile S.] Russian Acad Sci, Inst Problems Chem Phys, Chernogolovka 142432, Russia. [Meshkov, Vladimir V.; Stolyarov, Andrey V.] Moscow MV Lomonosov State Univ, Dept Chem, Moscow 119991, Russia. [Gordon, Iouli E.] Harvard Smithsonian Ctr Astrophys, Atom & Mol Phys Div, Cambridge, MA 02138 USA. RP Medvedev, ES (reprint author), Russian Acad Sci, Inst Problems Chem Phys, Prospect Akad Semenova 1, Chernogolovka 142432, Russia. EM esmedved@orc.ru RI Meshkov, Vladimir/H-6713-2012; Stolyarov, Andrey/H-7207-2012; OI Medvedev, Emile/0000-0002-4415-6926; Stolyarov, Andrey/0000-0001-7046-7202 FU Russian Foundation for Basic Research [12-03-00030a, 16-03-00526a]; NASA [NNX13AI59G]; [15-03-03302a] FX The work was supported by grants of the Russian Foundation for Basic Research to E.S.M. (Nos. 12-03-00030a and 16-03-00526a), V.V.M. and A.V.S. (No. 15-03-03302a), and of the NASA Planetary Atmospheres to I.E.G. (No. NNX13AI59G). I.E.G. also thanks Peter Bernath for helpful discussions. NR 40 TC 6 Z9 6 U1 7 U2 21 PU AMER INST PHYSICS PI MELVILLE PA 1305 WALT WHITMAN RD, STE 300, MELVILLE, NY 11747-4501 USA SN 0021-9606 EI 1089-7690 J9 J CHEM PHYS JI J. Chem. Phys. PD OCT 21 PY 2015 VL 143 IS 15 AR 154301 DI 10.1063/1.4933136 PG 7 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA CU3IR UT WOS:000363418400012 PM 26493901 ER PT J AU He, K Woodman, N Boaglio, S Roberts, M Supekar, S Maldonado, JE AF He, Kai Woodman, Neal Boaglio, Sean Roberts, Mariel Supekar, Sunjana Maldonado, Jesus E. TI Molecular Phylogeny Supports Repeated Adaptation to Burrowing within Small-Eared Shrews Genus of Cryptotis (Eulipotyphla, Soricidae) SO PLOS ONE LA English DT Article ID CYTOCHROME-B GENE; CENTRAL-AMERICA; MAMMALIA; SORICOMORPHA; MORPHOLOGY; INSECTIVORA; SOREX AB Small-eared shrews of the New World genus Cryptotis (Eulipotyphla, Soricidae) comprise at least 42 species that traditionally have been partitioned among four or more species groups based on morphological characters. The Cryptotis mexicana species group is of particular interest, because its member species inhibit a subtly graded series of forelimb adaptations that appear to correspond to locomotory behaviors that range from more ambulatory to more fossorial. Unfortunately, the evolutionary relationships both among species in the C. mexicana group and among the species groups remain unclear. To better understand the phylogeny of this group of shrews, we sequenced two mitochondrial and two nuclear genes. To help interpret the pattern and direction of morphological changes, we also generated a matrix of morphological characters focused on the evolutionarily plastic humerus. We found significant discordant between the resulting molecular and morphological trees, suggesting considerable convergence in the evolution of the humerus. Our results indicate that adaptations for increased burrowing ability evolved repeatedly within the genus Cryptotis. C1 [He, Kai; Woodman, Neal; Maldonado, Jesus E.] Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Washington, DC 20560 USA. [He, Kai] Chinese Acad Sci, Kunming Inst Zool, Kunming, Yunnan, Peoples R China. [Woodman, Neal] Smithsonian Inst, Natl Museum Nat Hist, USGS Patuxent Wildlife Res Ctr, Washington, DC 20560 USA. [Boaglio, Sean; Roberts, Mariel; Supekar, Sunjana; Maldonado, Jesus E.] Smithsonian Inst, Natl Zool Pk, Smithsonian Conservat Biol Inst, Ctr Conservat & Evolutionary Genet, Washington, DC 20008 USA. [Boaglio, Sean] Pacific Lutheran Univ, Dept Biol, Tacoma, WA 98447 USA. [Roberts, Mariel] Univ Penn, Philadelphia, PA 19104 USA. [Supekar, Sunjana] Oberlin Coll, Dept Biol, Oberlin, OH 44074 USA. RP He, K (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Washington, DC 20560 USA. EM hek@si.edu OI He, Kai/0000-0002-6234-2589; Woodman, Neal/0000-0003-2689-7373 FU NHRE program at the Smithsonian Institution FX NHRE program at the Smithsonian Institution provided funding internships and supplies to SB, MR, SS. The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 33 TC 1 Z9 1 U1 3 U2 13 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 OCT 21 PY 2015 VL 10 IS 10 AR e0140280 DI 10.1371/journal.pone.0140280 PG 13 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA CU0ZM UT WOS:000363248400048 PM 26489020 ER PT J AU Becker, JC Vanderburg, A Adams, FC Rappaport, SA Schwengeler, HM AF Becker, Juliette C. Vanderburg, Andrew Adams, Fred C. Rappaport, Saul A. Schwengeler, Hans Martin TI WASP-47: A HOT JUPITER SYSTEM WITH TWO ADDITIONAL PLANETS DISCOVERED BY K2 SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE planets and satellites: detection; planets and satellites: dynamical evolution and stability; techniques: photometric ID TERRESTRIAL PLANETS; LIGHT CURVES; MASS; CANDIDATES; EFFICIENT; TRANSITS; SEARCH; KEPLER; STARS; ECCENTRICITY AB Using new data from the K2 mission, we show that WASP-47, a previously known hot Jupiter host, also hosts two additional transiting planets: a Neptune-sized outer planet and a super-Earth inner companion. We measure planetary properties from the K2 light curve and detect transit timing variations (TTVs), confirming the planetary nature of the outer planet. We performed a large number of numerical simulations to study the dynamical stability of the system and to find the theoretically expected TTVs. The theoretically predicted TTVs are in good agreement with those observed, and we use the TTVs to determine the masses of two planets, and place a limit on the third. The WASP-47 planetary system is important because companion planets can both be inferred by TTVs and are also detected directly through transit observations. The depth of the hot Jupiter's transits make ground-based TTV measurements possible, and the brightness of the host star makes it amenable for precise radial velocity measurements. The system serves as a Rosetta Stone for understanding TTVs as a planet detection technique. C1 [Becker, Juliette C.; Adams, Fred C.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Vanderburg, Andrew] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Adams, Fred C.] Univ Michigan, Dept Phys, Ann Arbor, MI 48109 USA. [Rappaport, Saul A.] MIT, Dept Phys, Cambridge, MA 02139 USA. [Rappaport, Saul A.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Schwengeler, Hans Martin] Planet Hunter, Bottmingen, Switzerland. RP Becker, JC (reprint author), Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. EM jcbecker@umich.edu OI Becker, Juliette/0000-0002-7733-4522; Vanderburg, Andrew/0000-0001-7246-5438; Adams, Fred/0000-0002-8167-1767 FU NSF GRFP [DGE 1256260, DGE 1144152]; NASA Science Mission directorate FX We are grateful to Kat Deck and Tim Morton for significant assistance. We thank Marion Neveu-VanMalle, Eric Bell, Moiya McTier, Mark Omohundro, and Alexander Venner for useful conversations. We thank John Johnson for his guidance and the anonymous referee for their very useful comments. We acknowledge the Planet Hunters team for its community. This work used the Extreme Science and Engineering Discovery Environment (NSF ACI-1053575) and the OSG (NSF, DoE). J.B. and A.V. are supported by the NSF GRFP (DGE 1256260, DGE 1144152). This research has used the Exoplanet Data Explorer at http://www.exoplanets.org. The data in this paper were obtained from the Mikulski Archive for Space Telescopes. This paper includes data collected by the Kepler/K2 mission (funding provided by the NASA Science Mission directorate), and we gratefully acknowledge the efforts of the entire Kepler/K2 team. NR 41 TC 42 Z9 42 U1 2 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 OCT 20 PY 2015 VL 812 IS 2 AR L18 DI 10.1088/2041-8205/812/2/L18 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CV7WC UT WOS:000364485600001 ER PT J AU Kewley, LJ Zahid, HJ Geller, MJ Dopita, MA Hwang, HS Fabricant, D AF Kewley, Lisa J. Zahid, H. Jabran Geller, Margaret J. Dopita, Michael A. Hwang, Ho Seong Fabricant, Dan TI A RISE IN THE IONIZING PHOTONS IN STAR-FORMING GALAXIES OVER THE PAST 8 BILLION YEARS SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE galaxies: abundances; galaxies: fundamental parameters; galaxies: starburst ID SIMILAR-TO 2; ACTIVE GALACTIC NUCLEI; MASS-METALLICITY RELATION; EMISSION-LINE GALAXIES; FIBER-FED SPECTROGRAPH; PHYSICAL CONDITIONS; STARBURST GALAXIES; SPECTROSCOPY; EVOLUTION; HECTOSPEC AB We investigate the change in ionizing photons in galaxies in the range 0.2 < z < 0.6 using the F2 field of the SHELS complete galaxy redshift survey. We show, for the first time, that while the [O III]/H beta and [O III]/[O II] ratios rise, the [N II]/H alpha and [S II]/H alpha ratios fall significantly over the 0.2 < z < 0.35 redshift range for stellar masses in the range 9.2 < log(M/M-circle dot) < 10.6. The [O III]/H beta and [O III]/[O II] ratios continue to rise across the full 0.2 < z < 0.6 redshift range for stellar masses in the range 9.8 < log(M/M-circle dot) < 10.0. We conclusively rule out active galactic nucleus contamination, a changing ISM pressure, and a change in the hardness of the EUV radiation field as the cause of the change in the line ratios in the range 0.2 < z < 0.35. We find that the ionization parameter rises significantly with redshift (by 0.1-0.25 dex depending on the stellar mass of the sample). We show that the ionization parameter is strongly correlated with the fraction of young-to-old stars, as traced by the H mu equivalent width. We discuss the implications of this result on higher redshift studies, and we consider the implications on the use of standard optical metallicity diagnostics at high redshift. C1 [Kewley, Lisa J.; Dopita, Michael A.] Australian Natl Univ, RSAA, Weston, ACT 2611, Australia. [Kewley, Lisa J.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Zahid, H. Jabran; Geller, Margaret J.; Fabricant, Dan] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. [Dopita, Michael A.] King Abdulaziz Univ, Dept Astron, Jeddah, Saudi Arabia. [Hwang, Ho Seong] Korea Inst Adv Study, Sch Phys, Seoul 130722, South Korea. RP Kewley, LJ (reprint author), Australian Natl Univ, RSAA, Cotter Rd, Weston, ACT 2611, Australia. EM kewley@mso.anu.edu.au RI Dopita, Michael/P-5413-2014; OI Dopita, Michael/0000-0003-0922-4986; Geller, Margaret/0000-0002-9146-4876 FU ARC Discovery Project [DP130103925]; ARC Future Fellowship; Smithsonian Institution FX M.D. and L.K. are supported by an ARC Discovery Project DP130103925. L.K. gratefully acknowledges an ARC Future Fellowship and the 2014 ANU Academic Women's Writing Workshop. The Smithsonian Institution supports the research of M.G. and D.F. NR 35 TC 11 Z9 11 U1 1 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 OCT 20 PY 2015 VL 812 IS 2 AR L20 DI 10.1088/2041-8205/812/2/L20 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CV7WC UT WOS:000364485600003 ER PT J AU Ade, PAR Aikin, RW Amiri, M Barkats, D Benton, SJ Bischoff, CA Bock, JJ Bonetti, JA Brevik, JA Buder, I Bullock, E Chattopadhyay, G Davis, G Day, PK Dowell, CD Duband, L Filippini, JP Fliescher, S Golwala, SR Halpern, M Hasselfield, M Hildebrandt, SR Hilton, GC Hristov, V Hui, H Irwin, KD Jones, WC Karkare, KS Kaufman, JP Keating, BG Kefeli, S Kernasovskiy, SA Kovac, JM Kuo, CL Leduc, HG Leitch, EM Llombart, N Lueker, M Mason, P Megerian, K Moncelsi, L Netterfield, CB Nguyen, HT O'Brient, R Ogburn, RW Orlando, A Pryke, C Rahlin, AS Reintsema, CD Richter, S Runyan, MC Schwarz, R Sheehy, CD Staniszewski, ZK Sudiwala, RV Teply, GP Tolan, JE Trangsrud, A Tucker, RS Turner, AD Vieregg, AG Weber, A Wiebe, DV Wilson, P Wong, CL Yoon, KW Zmuidzinas, J AF Ade, P. A. R. Aikin, R. W. Amiri, M. Barkats, D. Benton, S. J. Bischoff, C. A. Bock, J. J. Bonetti, J. A. Brevik, J. A. Buder, I. Bullock, E. Chattopadhyay, G. Davis, G. Day, P. K. Dowell, C. D. Duband, L. Filippini, J. P. Fliescher, S. Golwala, S. R. Halpern, M. Hasselfield, M. Hildebrandt, S. R. Hilton, G. C. Hristov, V. Hui, H. Irwin, K. D. Jones, W. C. Karkare, K. S. Kaufman, J. P. Keating, B. G. Kefeli, S. Kernasovskiy, S. A. Kovac, J. M. Kuo, C. L. Leduc, H. G. Leitch, E. M. Llombart, N. Lueker, M. Mason, P. Megerian, K. Moncelsi, L. Netterfield, C. B. Nguyen, H. T. O'Brient, R. Ogburn, R. W. Orlando, A. Pryke, C. Rahlin, A. S. Reintsema, C. D. Richter, S. Runyan, M. C. Schwarz, R. Sheehy, C. D. Staniszewski, Z. K. Sudiwala, R. V. Teply, G. P. Tolan, J. E. Trangsrud, A. Tucker, R. S. Turner, A. D. Vieregg, A. G. Weber, A. Wiebe, D. V. Wilson, P. Wong, C. L. Yoon, K. W. Zmuidzinas, J. CA Bicep2 Collaboration Keck Array Collaboration Spider Collaboration TI ANTENNA-COUPLED TES BOLOMETERS USED IN BICEP2, Keck Array, AND SPIDER SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmic background radiation; instrumentation: detectors; instrumentation: polarimeters; methods: laboratory: solid state; techniques: polarimetric ID THERMAL CONDUCTANCE; QUANTUM; MILLIMETER; NOISE AB We have developed antenna-coupled transition-edge sensor bolometers for a wide range of cosmic microwave background (CMB) polarimetry experiments, including BICEP2, Keck Array, and the balloon borne SPIDER. These detectors have reached maturity and this paper reports on their design principles, overall performance, and key challenges associated with design and production. Our detector arrays repeatedly produce spectral bands with 20%-30% bandwidth at 95, 150, or 230 GHz. The integrated antenna arrays synthesize symmetric co-aligned beams with controlled side-lobe levels. Cross-polarized response on boresight is typically similar to 0.5%, consistent with cross-talk in our multiplexed readout system. End-to-end optical efficiencies in our cameras are routinely 35% or higher, with per detector sensitivities of NET similar to 300 mu K-CMB root s. Thanks to the scalability of this design, we have deployed 2560 detectors as 1280 matched pairs in Keck Array with a combined instantaneous sensitivity of similar to 9 mu K-CMB root s, as measured directly from CMB maps in the 2013 season. Similar arrays have recently flown in the SPIDER instrument, and development of this technology is ongoing. C1 [Ade, P. A. R.; Sudiwala, R. V.] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales. [Aikin, R. W.; Bock, J. J.; Brevik, J. A.; Filippini, J. P.; Golwala, S. R.; Hildebrandt, S. R.; Hristov, V.; Hui, H.; Kefeli, S.; Lueker, M.; Mason, P.; Moncelsi, L.; O'Brient, R.; Runyan, M. C.; Staniszewski, Z. K.; Teply, G. P.; Trangsrud, A.; Tucker, R. S.; Zmuidzinas, J.] CALTECH, Dept Phys, Pasadena, CA 91125 USA. [Amiri, M.; Davis, G.; Halpern, M.; Wiebe, D. V.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V5Z 1M9, Canada. [Barkats, D.] ESO, Joint ALMA Observ, Santiago, Chile. [Benton, S. J.; Netterfield, C. B.] Univ Toronto, Dept Phys, Toronto, ON, Canada. [Bischoff, C. A.; Buder, I.; Karkare, K. S.; Kovac, J. M.; Richter, S.; Wong, C. L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Bock, J. J.; Bonetti, J. A.; Chattopadhyay, G.; Day, P. K.; Dowell, C. D.; Hildebrandt, S. R.; Leduc, H. G.; Llombart, N.; Megerian, K.; Nguyen, H. T.; O'Brient, R.; Runyan, M. C.; Trangsrud, A.; Turner, A. D.; Weber, A.; Wilson, P.; Zmuidzinas, J.] Jet Prop Lab, Pasadena, CA 91109 USA. [Bullock, E.] Univ Minnesota, Minnesota Inst Astrophys, Minneapolis, MN 55455 USA. [Duband, L.] Univ Grenoble Alpes, CEA INAC SBT, F-38000 Grenoble, France. [Filippini, J. P.] Univ Illinois, Dept Phys, Champaign, IL 61820 USA. [Fliescher, S.; Pryke, C.; Schwarz, R.] Univ Minnesota, Dept Phys, Minneapolis, MN 55455 USA. [Hasselfield, M.; Jones, W. C.; Orlando, A.; Rahlin, A. S.] Princeton Univ, Dept Phys, Princeton, NJ 08544 USA. [Hilton, G. C.; Irwin, K. D.; Kuo, C. L.; Reintsema, C. D.] Natl Inst Stand & Technol, Boulder 80305, CO USA. [Irwin, K. D.; Kernasovskiy, S. A.; Kuo, C. L.; Ogburn, R. W.; Tolan, J. E.; Yoon, K. W.] Stanford Univ, Dept Phys, Stanford, CA 94305 USA. [Irwin, K. D.; Ogburn, R. W.; Yoon, K. W.] SLAC Natl Accelerator Lab, Kavli Inst Particle Astrophys & Cosmol, Menlo Pk, CA 94025 USA. [Kaufman, J. P.; Keating, B. G.] Univ Calif San Diego, Dept Phys, La Jolla, CA 92093 USA. [Leitch, E. M.; Sheehy, C. D.; Vieregg, A. G.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Sheehy, C. D.; Vieregg, A. G.] Univ Chicago, Enrico Fermi Inst, Dept Phys, Chicago, IL 60637 USA. RP Ade, PAR (reprint author), Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales. EM rogero@caltech.edu OI Orlando, Angiola/0000-0001-8004-5054; Bischoff, Colin/0000-0001-9185-6514; Barkats, Denis/0000-0002-8971-1954; Karkare, Kirit/0000-0002-5215-6993 FU JPL Research and Technology Development Fund; NASA [06-ARPA206-0040, 10-SAT10-0017]; Gordon and Betty Moore Foundation at Caltech; Canada Foundation for Innovation grant; W. M. Keck Foundation; US National Science Foundation [ANT-0742818, ANT-1044978, ANT-0742592, ANT-1110087] FX The development of antenna-coupled detector technology was supported by the JPL Research and Technology Development Fund and grants 06-ARPA206-0040 and 10-SAT10-0017 from the NASA APRA and SAT programs. The development and testing of focal planes were supported by the Gordon and Betty Moore Foundation at Caltech. Readout electronics were supported by a Canada Foundation for Innovation grant to UBC. The receiver development was supported in part by a grant from the W. M. Keck Foundation. BICEP2 was supported by the US National Science Foundation under grants ANT-0742818 and ANT-1044978 (Caltech/Harvard) and ANT-0742592 and ANT-1110087 (Chicago/Minnesota). Some computations in this paper were run on the Odyssey cluster supported by the FAS Science Division Research Computing Group at Harvard University. We thank Warren Holmes and Matthew Kenyon for discussions on thermal conductivity. Tireless administrative support was provided by Irene Coyle and Kathy Deniston. NR 41 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 OCT 20 PY 2015 VL 812 IS 2 AR 176 DI 10.1088/0004-637X/812/2/176 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CW7VD UT WOS:000365206600088 ER PT J AU Chan, CK Psaltis, D Ozel, F Medeiros, L Marrone, D Sadowski, A Narayan, R AF Chan, Chi-Kwan Psaltis, Dimitrios Oezel, Feryal Medeiros, Lia Marrone, Daniel Sadowski, Aleksander Narayan, Ramesh TI FAST VARIABILITY AND MILLIMETER/IR FLARES IN GRMHD MODELS OF Sgr A* FROM STRONG-FIELD GRAVITATIONAL LENSING SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; black hole physics; Galaxy: center; radiative transfer ID SUPERMASSIVE BLACK-HOLE; NEAR-INFRARED FLARES; X-RAY FLARE; GALACTIC-CENTER; ACCRETION FLOWS; MHD SIMULATIONS; STELLAR ORBITS; IR FLARES; SAGITTARIUS; EMISSION AB We explore the variability properties of long, high-cadence general relativistic magnetohydrodynamic (GRMHD) simulations across the electromagnetic spectrum using an efficient, GPU-based radiative transfer algorithm. We focus on both standard and normal evolution (SANE) and magnetically arrested disk (MAD) simulations with parameters that successfully reproduce the time-averaged spectral properties of Sgr A* and the size of its image at 1.3 mm. We find that the SANE models produce short-timescale variability with amplitudes and power spectra that closely resemble those inferred observationally. In contrast, MAD models generate only slow variability at lower flux levels. Neither set of models shows any X-ray flares, which most likely indicates that additional physics, such as particle acceleration mechanisms, need to be incorporated into the GRMHD simulations to account for them. The SANE models show strong, short-lived millimeter/infrared (IR) flares, with short (less than or similar to 1 hr) time lags between the millimeter and IR wavelengths, that arise from the combination of short-lived magnetic flux tubes and strongfield gravitational lensing near the horizon. Such events provide a natural explanation for the observed IR flares with no X-ray counterparts. C1 [Chan, Chi-Kwan; Psaltis, Dimitrios; Oezel, Feryal; Marrone, Daniel] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Chan, Chi-Kwan; Psaltis, Dimitrios; Oezel, Feryal; Marrone, Daniel] Univ Arizona, Dept Astron, Tucson, AZ 85721 USA. [Medeiros, Lia] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA. [Sadowski, Aleksander] MIT Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Narayan, Ramesh] Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, Cambridge, MA 02138 USA. RP Chan, CK (reprint author), Univ Arizona, Steward Observ, 933 N Cherry Ave, Tucson, AZ 85721 USA. EM chanc@email.arizona.edu OI Narayan, Ramesh/0000-0002-1919-2730 FU NASA/NSF TCAN [NNX14AB48G, NNX14AB47G]; NSF [AST 1108753, AST 1312034, AST-1207752, 1228509]; NFS GRFP [DGE 1144085] FX C.K.C., D.P., and F.O. were partially supported by NASA/NSF TCAN award NNX14AB48G and NSF grants AST 1108753 and AST 1312034. D.M. acknowledges support from NSF grant AST-1207752. R.N. acknowledges support from NASA/NSF TCAN awards NNX14AB47G. L.M. acknowledges support from NFS GRFP grant DGE 1144085. All raytracing calculations were performed with the El Gato GPU cluster at the University of Arizona that is funded by NSF award 1228509. We thank Jon McKinney, Heino Falcke, Jason Dexter, and Ann Mao for valuable comments and discussions. NR 51 TC 8 Z9 7 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 OCT 20 PY 2015 VL 812 IS 2 AR 103 DI 10.1088/0004-637X/812/2/103 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CW7VD UT WOS:000365206600015 ER PT J AU Czekala, I Andrews, SM Mandel, KS Hogg, DW Green, GM AF Czekala, Ian Andrews, Sean M. Mandel, Kaisey S. Hogg, David W. Green, Gregory M. TI CONSTRUCTING A FLEXIBLE LIKELIHOOD FUNCTION FOR SPECTROSCOPIC INFERENCE SO ASTROPHYSICAL JOURNAL LA English DT Article DE methods: data analysis; methods: statistical; stars: fundamental parameters; stars: late-type; stars: statistics; techniques: spectroscopic ID INFRARED TELESCOPE FACILITY; HIGH-RESOLUTION SPECTRA; K-BAND SPECTRA; M-DWARFS; STELLAR PARAMETERS; TEMPERATURE INDICATORS; TRANSITING PLANET; SYNTHETIC SPECTRA; ECCENTRIC ORBIT; COOL STARS AB We present a modular, extensible likelihood framework for spectroscopic inference based on synthetic model spectra. The subtraction of an imperfect model from a continuously sampled spectrum introduces covariance between adjacent datapoints (pixels) into the residual spectrum. For the high signal-to-noise data with large spectral range that is commonly employed in stellar astrophysics, that covariant structure can lead to dramatically underestimated parameter uncertainties (and, in some cases, biases). We construct a likelihood function that accounts for the structure of the covariance matrix, utilizing the machinery of Gaussian process kernels. This framework specifically addresses the common problem of mismatches in model spectral line strengths (with respect to data) due to intrinsic model imperfections (e.g., in the atomic/molecular databases or opacity prescriptions) by developing a novel local covariance kernel formalism that identifies and self-consistently downweights pathological spectral line "outliers." By fitting many spectra in a hierarchical manner, these local kernels provide a mechanism to learn about and build data-driven corrections to synthetic spectral libraries. An open-source software implementation of this approach is available at http://iancze.github.io/Starfish, including a sophisticated probabilistic scheme for spectral interpolation when using model libraries that are sparsely sampled in the stellar parameters. We demonstrate some salient features of the framework by fitting the high-resolution V-band spectrum of WASP-14, an F5 dwarf with a transiting exoplanet, and the moderate-resolution K-band spectrum of Gliese 51, an M5 field dwarf. C1 [Czekala, Ian; Andrews, Sean M.; Mandel, Kaisey S.; Green, Gregory M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Hogg, David W.] NYU, Dept Phys, Ctr Cosmol & Particle Phys, New York, NY 10003 USA. RP Czekala, I (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM iczekala@cfa.harvard.edu OI Green, Gregory/0000-0001-5417-2260; Czekala, Ian/0000-0002-1483-8811 FU NSF Graduate Fellowship; Smithsonian Institution; Harvard by NSF [AST-1211196] FX The authors would like to acknowledge the following people for many extraordinarily helpful discussions and key insights: Daniel Foreman-Mackey, Guillermo Torres, David Latham, Lars Buchhave, John Johnson and the ExoLab, Daniel Eisenstein, Rebekah Dawson, Tom Loredo and the ExoStat group, Allyson Bieryla, and Maxwell Moe. Two anonymous reviewers provided encouraging and very useful comments on the manuscript draft that greatly improved its clarity and focus. I.C. is supported by the NSF Graduate Fellowship and the Smithsonian Institution. K.S.M. is supported at Harvard by NSF grant AST-1211196. This research made extensive use of Astropy (Astropy Collaboration et al. 2013) and the Julia language (Bezanson et al. 2012). NR 58 TC 4 Z9 4 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD OCT 20 PY 2015 VL 812 IS 2 AR 128 DI 10.1088/0004-637X/812/2/128 PG 21 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CW7VD UT WOS:000365206600040 ER PT J AU Ge, C Li, ZY Xu, XJ Gu, QS Wang, QD Roberts, S Kraft, RP Jones, C Forman, WR AF Ge, Chong Li, Zhiyuan Xu, Xiaojie Gu, Qiusheng Wang, Q. Daniel Roberts, Shawn Kraft, Ralph P. Jones, Christine Forman, William R. TI X-RAY EMISSIVITY OF OLD STELLAR POPULATIONS: A LOCAL GROUP CENSUS SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: individual (NGC147, NGC185, NGC205); X-rays: galaxies; X-rays: stars ID EARLY-TYPE GALAXIES; GALACTIC GLOBULAR-CLUSTERS; HOT GAS CONTENT; STAR-FORMATION; BINARY-SYSTEMS; ELLIPTIC GALAXIES; SOMBRERO GALAXY; OMEGA-CENTAURI; CHANDRA SURVEY; POINT SOURCES AB We study the unresolved X-ray emission in three Local Group dwarf elliptical (dE) galaxies (NGC 147, NGC 185, and NGC 205) using XMM-Newton observations; this emission most likely originates from a collection of weak X-ray sources, mainly cataclysmic variables and coronally active binaries. Precise knowledge of this stellar X-ray emission is crucial not only for understanding the relevant stellar astrophysics but also for disentangling and quantifying the thermal emission from diffuse hot gas in nearby galaxies. We find that the integrated X-ray emissivities of the individual dEs agree well with those of the solar vicinity, supporting an often assumed but untested view that the X-ray emissivity of old stellar populations is quasi-universal in normal galactic environments, in which dynamical effects on the formation and destruction of binary systems are not important. The average X-ray emissivity of the dEs studied in the literature, including M32, is measured to be L0.5-2 keV/M-* = (6.0 +/- 0.5 +/- 1.8) x 10(27) erg s(-1) M-circle dot(-1). We also compare this value to the integrated X-ray emissivities of Galactic globular clusters and old open clusters and discuss the role of dynamical effects in these dense stellar systems. C1 [Ge, Chong; Li, Zhiyuan; Xu, Xiaojie; Gu, Qiusheng; Wang, Q. Daniel] Nanjing Univ, Sch Astron & Space Sci, Nanjing 210093, Jiangsu, Peoples R China. [Ge, Chong; Li, Zhiyuan; Xu, Xiaojie; Gu, Qiusheng] Nanjing Univ, Minist Educ, Key Lab Modern Astron & Astrophys, Nanjing 210093, Jiangsu, Peoples R China. [Ge, Chong; Li, Zhiyuan; Xu, Xiaojie; Gu, Qiusheng] Collaborat Innovat Ctr Modern Astron & Space Expl, Nanjing 210093, Jiangsu, Peoples R China. [Ge, Chong; Wang, Q. Daniel; Roberts, Shawn] Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA. [Kraft, Ralph P.; Jones, Christine; Forman, William R.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Ge, C (reprint author), Nanjing Univ, Sch Astron & Space Sci, Nanjing 210093, Jiangsu, Peoples R China. EM lizy@nju.edu.cn OI Forman, William/0000-0002-9478-1682 FU National Natural Science Foundation of China [11273015, 11133001]; National Basic Research Program [2013CB834905]; program of China Scholarships Council [201206190041]; Recruitment Program of Global Youth Experts FX We thank M. Revnivtsev for valuable comments and the anonymous referee for suggestions that significantly improved our work. This work was partially supported by the National Natural Science Foundation of China under grants 11273015 and 11133001, and the National Basic Research Program No. 2013CB834905. C.G. acknowledges support from the program of China Scholarships Council No. 201206190041 during his visit to UMass. Z.L. acknowledges support from the Recruitment Program of Global Youth Experts. NR 62 TC 3 Z9 3 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 OCT 20 PY 2015 VL 812 IS 2 AR 130 DI 10.1088/0004-637X/812/2/130 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CW7VD UT WOS:000365206600042 ER PT J AU Ghezzi, L Johnson, JA AF Ghezzi, Luan Johnson, John Asher TI BEYOND THE MAIN SEQUENCE: TESTING THE ACCURACY OF STELLAR MASSES PREDICTED BY THE PARSEC EVOLUTIONARY TRACKS SO ASTROPHYSICAL JOURNAL LA English DT Article DE asteroseismology; binaries: general; stars: evolution; stars: fundamental parameters ID SOLAR-LIKE OSCILLATIONS; PRECISE RADIAL-VELOCITIES; SMALL-MAGELLANIC-CLOUD; BINARY AI-PHOENICIS; PLANET-HOST STARS; G-TYPE GIANTS; ECLIPSING-BINARY; RED GIANTS; PHYSICAL PARAMETERS; OPEN CLUSTERS AB Characterizing the physical properties of exoplanets and understanding their formation and orbital evolution requires precise and accurate knowledge of their host stars. Accurately measuring stellar masses is particularly important because they likely influence planet occurrence and the architectures of planetary systems. Single main-sequence stars typically have masses estimated from evolutionary tracks, which generally provide accurate results due to their extensive empirical calibration. However, the validity of this method for subgiants and giants has been called into question by recent studies, with suggestions that the masses of these evolved stars could have been overestimated. We investigate these concerns using a sample of 59 benchmark evolved stars with model-independent masses (from binary systems or asteroseismology) obtained from the literature. We find very good agreement between these benchmark masses and the ones estimated using evolutionary tracks. The average fractional difference in the mass interval similar to 0.7-4.5 M-circle dot is consistent with zero (-1.30 +/- 2.42%), with no significant trends in the residuals relative to the input parameters. A good agreement between model-dependent and -independent radii (-4.81 +/- 1.32%) and surface gravities (0.71 +/- 0.51%) is also found. The consistency between independently determined ages for members of binary systems adds further support for the accuracy of the method employed to derive the stellar masses. Taken together, our results indicate that determination of masses of evolved stars using grids of evolutionary tracks is not significantly affected by systematic errors, and is thus valid for estimating the masses of isolated stars beyond the main sequence. C1 [Ghezzi, Luan; Johnson, John Asher] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Ghezzi, L (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM lghezzi@cfa.harvard.edu FU Coordenacao de Aperfeicoamento de Pessoal de Nivel Superior (CAPES); Ciencia sem Fronteiras; Harvard College Observatory; Fundacao Lemann; Alfred P. Sloan and David & Lucile Packard foundations FX L.G. would like to thank the financial support from Coordenacao de Aperfeicoamento de Pessoal de Nivel Superior (CAPES), Ciencia sem Fronteiras, Harvard College Observatory, and Fundacao Lemann. J. A. J. is grateful for the generous grant support provided by the Alfred P. Sloan and David & Lucile Packard foundations. NR 134 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 OCT 20 PY 2015 VL 812 IS 2 AR 96 DI 10.1088/0004-637X/812/2/96 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CW7VD UT WOS:000365206600008 ER PT J AU Gianninas, A Kilic, M Brown, WR Canton, P Kenyon, SJ AF Gianninas, A. Kilic, Mukremin Brown, Warren R. Canton, Paul Kenyon, Scott J. TI THE ELM SURVEY. VI. ELEVEN NEW DOUBLE DEGENERATES SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries: close; Galaxy: stellar content; gravitational waves; supernovae: general; techniques: spectroscopic; white dwarfs ID EXTREMELY LOW-MASS; WHITE-DWARF BINARY; 3D MODEL ATMOSPHERES; SPECTROSCOPIC ANALYSIS; MODERATE-RESOLUTION; CORONAE-BOREALIS; MERGER SYSTEMS; ORBITAL PERIOD; HELIUM-RICH; NLTT 11748 AB We present the discovery of 11 new double degenerate systems containing extremely low-mass white dwarfs (ELM WDs). Our radial velocity observations confirm that all of the targets have orbital periods <= 1 day. We perform spectroscopic fits and provide a complete set of physical and binary parameters. We review and compare recent evolutionary calculations and estimate that the systematic uncertainty in our mass determinations due to differences in the evolutionary models is small (approximate to 0.01 M-circle dot). Five of the new systems will merge due to gravitational wave radiation within a Hubble time, bringing the total number of merger systems found in the ELM Survey to 38. We examine the ensemble properties of the current sample of ELM WD binaries, including the period distribution as a function of effective temperature, and the implications for the future evolution of these systems. We also revisit the empirical boundaries of instability strip of ELM WDs and identify new pulsating ELM WD candidates. Finally, we consider the kinematic properties of our sample of ELM WDs and estimate that a significant fraction of the WDs from the ELM Survey are members of the Galactic halo. C1 [Gianninas, A.; Kilic, Mukremin; Canton, Paul] Univ Oklahoma, Homer L Dodge Dept Phys & Astron, Norman, OK 73019 USA. [Brown, Warren R.; Kenyon, Scott J.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Gianninas, A (reprint author), Natl Opt Astron Observ, Kitt Peak Natl Observ, La Serena, Chile. EM alexg@nhn.ou.edu RI Alexandros, Gianninas/B-8352-2016; OI Alexandros, Gianninas/0000-0002-8655-4308; Kenyon, Scott/0000-0003-0214-609X FU NSF [AST-1312678]; NASA [NNX14AF65G, NAS 5-26555]; National Science Foundation [PHYS-1066293]; NASA through grant from the Space Telescope Science Institute [HST-GO-13319.01]; AURA through the National Science Foundation under AURA [AST 0132798] FX We would like to thank the referee and statistics consultant for their useful suggestions which helped improve this paper. We also thank the director and staff of Kitt Peak National Observatory for the use of their facilities and their valuable assistance. We gratefully acknowledge the support of the NSF under grant AST-1312678, and NASA under grant NNX14AF65G. This work was supported in part by National Science Foundation Grant No. PHYS-1066293 and the hospitality of the Aspen Center for Physics. A.G. acknowledges support provided by NASA through grant number HST-GO-13319.01 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 by AURA through the National Science Foundation under AURA Cooperative Agreement AST 0132798 as amended. NR 74 TC 15 Z9 15 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 OCT 20 PY 2015 VL 812 IS 2 AR 167 DI 10.1088/0004-637X/812/2/167 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CW7VD UT WOS:000365206600079 ER PT J AU Hales, AS Corder, SA Dent, WRD Andrews, SM Eisner, JA Cieza, LA AF Hales, A. S. Corder, S. A. Dent, W. R. D. Andrews, S. M. Eisner, J. A. Cieza, L. A. TI THE EARLY ALMA VIEW OF THE FU Ori OUTBURST SYSTEM SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; stars: formation ID YOUNG STELLAR OBJECTS; ORIONIS BINARY-SYSTEM; CIRCUMSTELLAR DISKS; STARS; ACCRETION; SUBMILLIMETER; PLANETS; MODELS; TAURUS; DISCS AB We have obtained ALMA Band 7 observations of the FU Ori outburst system at a 0 ''.6 x 0 ''.5 resolution to measure the link between the inner disk instability and the outer disk through submillimeter continuum and molecular line observations. Our observations detect continuum emission that can be well-modeled by two unresolved sources located at the position of each binary component. The interferometric observations recover the entire flux reported in previous single-dish studies, ruling out the presence of a large envelope. Assuming that the dust is optically thin, we derive disk dust masses of 2 x 10(-4) M-circle dot and 8 x 10(-5) M-circle dot for the north and south components, respectively. We place limits on the disks' radii of r < 45 AU. We report the detection of molecular emission from (CO)-C-12(3-2), HCO+(4-3), and from HCN(4-3). The (CO)-C-12 appears widespread across the two binary components and is slightly more extended than the continuum emission. The denser gas tracer HCO+ peaks close to the position of the southern binary component, while HCN appears to be peaked at the position of the northern component. This suggests that the southern binary component is embedded in denser molecular material, consistent with previous studies that indicate a heavily reddened object. At this angular resolution, any interaction between the two unresolved disk components cannot be disentangled. Higher-resolution images are vital for understanding the process of star formation via rapid accretion FU Ori-type episodes. C1 [Hales, A. S.; Corder, S. A.; Dent, W. R. D.] Joint ALMA Observ, Atacama Large Millimeter Submillimeter Array, Santiago 7630355, Chile. [Hales, A. S.; Corder, S. A.] Natl Radio Astron Observ, Charlottesville, VA 22903 USA. [Dent, W. R. D.] European So Observ, D-85748 Garching, Germany. [Andrews, S. M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Eisner, J. A.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Cieza, L. A.] Univ Diego Portales, Fac Ingn, Nucleo Astron, Santiago, Chile. [Cieza, L. A.] Protoplanetary Disks ALMA Early Sci, Millenium Nucleus, Santiago, Chile. RP Hales, AS (reprint author), Joint ALMA Observ, Atacama Large Millimeter Submillimeter Array, Alonso de Cordova 3107, Santiago 7630355, Chile. EM ahales@alma.cl OI Hales, Antonio/0000-0001-5073-2849 FU NSF AAG [1311910]; ALMA-CONICYT [31120009]; CONICYT-FONDECYT [1140109]; Millennium Science Initiative (Chilean Ministry of Economy) [Nucleus RC130007] FX This paper makes use of the following ALMA data: ADS/JAO.ALMA#2011.0.00548.S. ALMA is a partnership of ESO (representing its member states), NSF (USA), and NINS (Japan), together with NRC (Canada) and NSC and ASIAA (Taiwan), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by ESO, AUI/NRAO, and NAOJ. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. This research made use of Astropy, a community-developed core Python package for Astronomy (Astropy Collaboration et al. 2013). J.A.E. acknowledges support from NSF AAG grant 1311910. L.A.C. was supported by ALMA-CONICYT grant number 31120009 and CONICYT-FONDECYT grant number 1140109. L.A.C. also acknowledges support from the Millennium Science Initiative (Chilean Ministry of Economy), through grant "Nucleus RC130007." NR 30 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 OCT 20 PY 2015 VL 812 IS 2 AR 134 DI 10.1088/0004-637X/812/2/134 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CW7VD UT WOS:000365206600046 ER PT J AU Kim, DW Fabbiano, G AF Kim, Dong-Woo Fabbiano, Giuseppina TI X-RAY SCALING RELATIONS OF "CORE" AND "CORELESS" E AND S0 GALAXIES SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: elliptical and lenticular, cD; X-rays: galaxies ID SUPERMASSIVE BLACK-HOLES; ATLAS(3D) PROJECT; ELLIPTIC GALAXIES; HOT GAS; LUMINOSITY FUNCTION; REDSHIFT SURVEY; SAURON PROJECT; SLOW ROTATORS; AGN FEEDBACK; DARK-MATTER AB We have re-examined the two X-ray scaling relations of early-type galaxies (ETGs), L-X,L-GAS-L-K and L-X,L-GAS-T-GAS, using 61 ATLAS(3D) E and S0 galaxies observed with Chandra (including ROSAT results for a few X-ray bright galaxies with extended hot gas). With this sample, which doubles the number of ETGs available for study we confirm the strong, steep correlations reported by Boroson et al. Moreover, the larger sample allows us to investigate the effect of structural and dynamical properties of ETGs in these relations. Using the sub-sample of 11 "genuine" E galaxies with central surface brightness cores, slow stellar rotations and old stellar populations, we find that the scatter of the correlations is strongly reduced, yielding an extremely tight relation of the form L-X,L-GAS similar to T-GAS(4.5 +/- 0.3). The rms deviation is only 0.13 dex. For the gas-rich galaxies in this sample (L-X,L-GAS > 10(40) erg s(-1)), this relation is consistent with recent simulations for velocity dispersion supported E galaxies. However, the tight L-X,L-GAS-T-GAS relation of genuine E galaxies extends down into the L-X similar to 10(38) erg s(-1) range, where simulations predict the gas to be in outflow/wind state, with resulting L-X much lower than observed in our sample. The observed correlation may suggest the presence of small bound hot halos even in this low luminosity range. At the high luminosity end, the L-X,L-GAS-T-GAS correlation of core elliptical galaxies is similar to that found in samples of cD galaxies and groups, but shifted down toward relatively lower L-X,L-GAS for a given T-GAS. In particular cDs, central dominant galaxies sitting at the bottom of the potential well imposed by the group dark matter, have an order of magnitude higher L-X,L-GAS than our sample core galaxies for the same L-K and T-GAS. We suggest that enhanced cooling in cDs, which have higher hot gas densities and lower entropies, could lower T-GAS to the range observed in giant Es; this conclusion is supported by the presence of extended cold gas in several cDs. Instead, in the sub-sample of coreless ETGs-these galaxies also tend to show stellar rotation, a flattened galaxy figure and rejuvenation of the stellar population-L-X,L-GAS and T-GAS are not correlated. The L-X-T-GAS distribution of coreless ETGs is a scatter diagram clustered at L-X,L-GAS < 10(40) erg s(-1), similar to that reported for the hot interstellar medium (ISM) of spiral galaxies, suggesting that both the energy input from star formation and the effect of galactic rotation and flattening may disrupt the hot ISM. C1 [Kim, Dong-Woo; Fabbiano, Giuseppina] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Kim, DW (reprint author), Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA. OI Kim, Dong-Woo/0000-0002-7386-944X; Fabbiano, Giuseppina/0000-0002-3554-3318 FU Chandra GO grant [AR4-15005X]; Smithsonian Competitive Grant Program for Science; NASA [NAS8-03060 (CXC)] FX We thank Silvia Pellegrini for helpful discussions. The data analysis was supported by the CXC CIAO software and CALDB. We have used the NASA NED and ADS facilities, and have extracted archival data from the Chandra Data Archive. This work was supported by the Chandra GO grant AR4-15005X, by 2014 Smithsonian Competitive Grant Program for Science and by NASA contract NAS8-03060 (CXC). NR 65 TC 3 Z9 3 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 OCT 20 PY 2015 VL 812 IS 2 AR 127 DI 10.1088/0004-637X/812/2/127 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CW7VD UT WOS:000365206600039 ER PT J AU Ogrean, GA van Weeren, RJ Jones, C Clarke, TE Sayers, J Mroczkowski, T Nulsen, PEJ Forman, W Murray, SS Pandey-Pommier, M Randall, S Churazov, E Bonafede, A Kraft, R David, L Andrade-Santos, F Merten, J Zitrin, A Umetsu, K Goulding, A Roediger, E Bagchi, J Bulbul, E Donahue, M Ebeling, H Johnston-Hollitt, M Mason, B Rosati, P Vikhlinin, A AF Ogrean, G. A. van Weeren, R. J. Jones, C. Clarke, T. E. Sayers, J. Mroczkowski, T. Nulsen, P. E. J. Forman, W. Murray, S. S. Pandey-Pommier, M. Randall, S. Churazov, E. Bonafede, A. Kraft, R. David, L. Andrade-Santos, F. Merten, J. Zitrin, A. Umetsu, K. Goulding, A. Roediger, E. Bagchi, J. Bulbul, E. Donahue, M. Ebeling, H. Johnston-Hollitt, M. Mason, B. Rosati, P. Vikhlinin, A. TI FRONTIER FIELDS CLUSTERS: CHANDRA AND JVLA VIEW OF THE PRE-MERGING CLUSTER MACS J0416.1-2403 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: clusters: individual; galaxies: clusters: intracluster medium; X-rays: galaxies: clusters ID DIFFUSE RADIO-EMISSION; INTERACTION CROSS-SECTION; XMM-NEWTON OBSERVATIONS; X-RAY-CLUSTERS; GALAXY CLUSTERS; DARK-MATTER; SUNYAEV-ZELDOVICH; SCALING RELATIONS; BULLET CLUSTER; PARTICLE REACCELERATION AB Merging galaxy clusters leave long-lasting signatures on the baryonic and non-baryonic cluster constituents, including shock fronts, cold fronts, X-ray substructure, radio halos, and offsets between the dark matter (DM) and the gas components. Using observations from Chandra, the Jansky Very Large Array, the Giant Metrewave Radio Telescope, and the Hubble Space Telescope, we present a multiwavelength analysis of the merging Frontier Fields cluster MACS J0416.1-2403 (z = 0.396), which consists of NE and SW subclusters whose cores are separated on the sky by similar to 250 kpc. We find that the NE subcluster has a compact core and hosts an X-ray cavity, yet it is not a cool core. Approximately 450 kpc south-southwest of the SW subcluster, we detect a density discontinuity that corresponds to a compression factor of similar to 1.5. The discontinuity was most likely caused by the interaction of the SW subcluster with a less massive structure detected in the lensing maps SW of the subcluster's center. For both the NE and the SW subclusters, the DM and the gas components are well-aligned, suggesting that MACS J0416.1-2403 is a pre-merging system. The cluster also hosts a radio halo, which is unusual for a pre-merging system. The halo has a 1.4 GHz power of (1.3 +/- 0.3) x 10(24)WHz(-1), which is somewhat lower than expected based on the X-ray luminosity of the cluster if the spectrum of the halo is not ultra-steep. We suggest that we are either witnessing the birth of a radio halo, or have discovered a rare ultra-steep spectrum halo. C1 [Ogrean, G. A.; van Weeren, R. J.; Jones, C.; Nulsen, P. E. J.; Forman, W.; Murray, S. S.; Randall, S.; Kraft, R.; David, L.; Andrade-Santos, F.; Goulding, A.; Roediger, E.; Bulbul, E.; Vikhlinin, A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Clarke, T. E.; Mroczkowski, T.] US Naval Res Lab, Washington, DC 20375 USA. [Sayers, J.; Zitrin, A.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA. [Murray, S. S.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Pandey-Pommier, M.] Observ Lyon, Ctr Rech Astrophys Lyon, F-69561 St Genis Laval, France. [Churazov, E.] Max Planck Inst Astrophys, D-85741 Garching, Germany. [Churazov, E.] Space Res Inst, Moscow 117997, Russia. [Bonafede, A.; Roediger, E.] Univ Hamburg, Hamburger Sternwarte, D-21029 Hamburg, Germany. [Merten, J.] Univ Oxford, Dept Phys, Oxford OX1 3RH, England. [Umetsu, K.] Acad Sinica, Inst Astron & Astrophys, Taipei 10617, Taiwan. [Goulding, A.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. [Bagchi, J.] IUCAA, Pune 411007, Maharashtra, India. [Donahue, M.] Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA. [Ebeling, H.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Johnston-Hollitt, M.] Victoria Univ Wellington, Sch Chem & Phys Sci, Wellington 6014, New Zealand. [Mason, B.] Natl Radio Astron Observ, Charlottesville, VA 22903 USA. [Rosati, P.] Univ Ferrara, Dept Phys & Earth Sci, I-44122 Ferrara, Italy. RP Ogrean, GA (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM gogrean@cfa.harvard.edu RI Churazov, Eugene/A-7783-2013; OI Mroczkowski, Tony/0000-0003-3816-5372; Umetsu, Keiichi/0000-0002-7196-4822; Nulsen, Paul/0000-0003-0297-4493; van Weeren, Reinout/0000-0002-0587-1660; Forman, William/0000-0002-9478-1682 FU NASA through a Hubble Fellowship grant by the Space Telescope Science Institute [HST-HF2-51345.001-A]; NASA [NAS5-26555, NAS8-03060]; NASA through the Einstein Postdoctoral grant by the Chandra X-ray Center [PF2-130104]; 6.1 Base funding; Chandra grant [G03-14131X]; [13496] FX G.A.O. acknowledges support by NASA through a Hubble Fellowship grant HST-HF2-51345.001-A awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Incorporated, under NASA contract NAS5-26555. R.J.vW. 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. A.Z. acknowledges support by NASA through a Hubble Fellowship grant HST-HF2-51334.001-A awarded by 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 performed while T.M. held a National Research Council Research Associateship Award at the Naval Research Laboratory (NRL). Basic research in radio astronomy at NRL by T.M. and T.E.C. is supported by 6.1 Base funding. F.A.S. acknowledges support from Chandra grant G03-14131X.; The scientific results reported in this article are based on observations made by the Chandra X-ray Observatory. Part of the reported results are based on observations made with the NASA/ESA Hubble Space Telescope, obtained from the Data Archive at the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-26555. The HST observations are associated with program #13496. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. We thank the staff of the GMRT that made these observations possible. The GMRT is run by the National Centre for Radio Astrophysics of the Tata Institute of Fundamental Research. NR 93 TC 11 Z9 11 U1 1 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD OCT 20 PY 2015 VL 812 IS 2 AR 153 DI 10.1088/0004-637X/812/2/153 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CW7VD UT WOS:000365206600065 ER PT J AU Prestwich, AH Jackson, F Kaaret, P Brorby, M Roberts, TP Saar, SH Yukita, M AF Prestwich, A. H. Jackson, F. Kaaret, P. Brorby, M. Roberts, T. P. Saar, S. H. Yukita, M. TI ULTRA-LUMINOUS X-RAY SOURCES IN HARO 11 AND THE ROLE OF X-RAY BINARIES IN FEEDBACK IN Ly alpha EMITTING GALAXIES SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: clusters: general; galaxies: dwarf; galaxies: starburst; X-rays: binaries; X-rays: galaxies ID STAR-FORMING GALAXIES; LOCAL STARBURST GALAXIES; HIGH-RESOLUTION CAMERA; HIGH-REDSHIFT GALAXIES; LYMAN-BREAK GALAXIES; BLACK-HOLE BINARIES; OPTICAL SPECTROSCOPY; ULTRALUMINOUS STATE; INTERSTELLAR-MEDIUM; YOUNG STARBURST AB Lyman Break Analogs (LBAs) are local proxies of high-redshift Lyman Break Galaxies. Spatially resolved studies of nearby starbursts have shown that Lyman continuum and line emission are absorbed by dust and that the Ly alpha is resonantly scattered by neutral hydrogen. In order to observe Lya emission from star-forming regions, some source of feedback is required to blow the neutral gas away from the starburst to prevent scattering and allow the Ly alpha emission to escape. We show that there are two X-ray point sources embedded in the diffuse emission of the LBA galaxy Haro 11. CXOU J003652.4-333316 (abbreviated to Haro 11 X-1) is an extremely luminous (L-X similar to 10(41) erg s(-1)), spatially compact source with a hard-X-ray spectrum. We suggest that the X-ray emission from Haro 11 X-1 is dominated by a single accretion source. This might be an active galactic nucleus or a source similar to the extreme black hole binary (BHB) M82 X-1. The hard X-ray spectrum indicates that Haro 11 X-1 may be a BHB in a low accretion state. In this case, the very high X-ray luminosity suggests an intermediate mass black hole that could be the seed for formation of a supermassive black hole. Source CXOU J003652.7-33331619.5 (abbreviated Haro 11 X-2) has an X-ray luminosity of L-X similar to 5 x 10(40) erg s(-1) and a soft X-ray spectrum (power-law photon index Gamma similar to 2.2). This strongly suggests that Haro 11 X-2 is an X-ray binary in the ultra luminous state (i.e., an Ultra Luminous X-ray source, ULX). Haro 11 X-2 is coincident with the star-forming knot that is the source of the Ly alpha emission. The association of a ULX with Ly alpha emission raises the possibility that strong winds from X-ray binaries play an important role in injecting mechanical power into the interstellar medium, thus blowing away neutral material from the starburst region and allowing the Ly alpha to escape. We suggest that feedback from X-ray binaries may play a significant role in allowing Ly alpha emission to escape from galaxies in the early universe. C1 [Prestwich, A. H.; Saar, S. H.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Jackson, F.] Univ Toledo, Dept Phys & Astron, Toledo, OH 43606 USA. [Kaaret, P.; Brorby, M.] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA. [Roberts, T. P.] Univ Durham, Dept Phys, Durham DH1 3LE, England. [Yukita, M.] Johns Hopkins Univ, Baltimore, MD 21218 USA. RP Prestwich, AH (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Yukita, Mihoko/E-4135-2017 NR 77 TC 2 Z9 2 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD OCT 20 PY 2015 VL 812 IS 2 AR 166 DI 10.1088/0004-637X/812/2/166 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CW7VD UT WOS:000365206600078 ER PT J AU Sanchis-Ojeda, R Rappaport, S Palle, E Delrez, L DeVore, J Gandolfi, D Fukui, A Ribas, I Stassun, KG Albrecht, S Dai, F Gaidos, E Gillon, M Hirano, T Holman, M Howard, AW Isaacson, H Jehin, E Kuzuhara, M Mann, AW Marcy, GW Miles-Paez, PA Montanes-Rodriguez, P Murgas, F Narita, N Nowak, G Onitsuka, M Paegert, M Van Eylen, V Winn, JN Yu, L AF Sanchis-Ojeda, R. Rappaport, S. Palle, E. Delrez, L. DeVore, J. Gandolfi, D. Fukui, A. Ribas, I. Stassun, K. G. Albrecht, S. Dai, F. Gaidos, E. Gillon, M. Hirano, T. Holman, M. Howard, A. W. Isaacson, H. Jehin, E. Kuzuhara, M. Mann, A. W. Marcy, G. W. Miles-Paez, P. A. Montanes-Rodriguez, P. Murgas, F. Narita, N. Nowak, G. Onitsuka, M. Paegert, M. Van Eylen, V. Winn, J. N. Yu, L. TI THE K2-ESPRINT PROJECT. I. DISCOVERY OF THE DISINTEGRATING ROCKY PLANET K2-22b WITH A COMETARY HEAD AND LEADING TAIL SO ASTROPHYSICAL JOURNAL LA English DT Article DE planetary systems; planets and satellites: atmospheres; planets and satellites: detection ID INFRARED TELESCOPE FACILITY; JOVIAN DUST STREAMS; LIGHT-CURVE PROJECT; EARTH-SIZED PLANET; KIC 12557548 B; M DWARFS; ECLIPSING BINARIES; STELLAR ROTATION; TIDAL FRICTION; CCD PHOTOMETRY AB We present the discovery of a transiting exoplanet candidate in the K2 Field-1 with an orbital period of 9.1457 hr: K2-22b. The highly variable transit depths, ranging from similar to 0% to 1.3%, are suggestive of a planet that is disintegrating via the emission of dusty effluents. We characterize the host star as an M-dwarf with T-eff similar or equal to 3800 K. We have obtained ground-based transit measurements with several 1-m class telescopes and with the GTC. These observations (1) improve the transit ephemeris; (2) confirm the variable nature of the transit depths; (3) indicate variations in the transit shapes; and (4) demonstrate clearly that at least on one occasion the transit depths were significantly wavelength dependent. The latter three effects tend to indicate extinction of starlight by dust rather than by any combination of solid bodies. The K2 observations yield a folded light curve with lower time resolution but with substantially better statistical precision compared with the ground-based observations. We detect a significant "bump" just after the transit egress, and a less significant bump just prior to transit ingress. We interpret these bumps in the context of a planet that is not only likely streaming a dust tail behind it, but also has a more prominent leading dust trail that precedes it. This effect is modeled in terms of dust grains that can escape to beyond the planet's Hill sphere and effectively undergo " Roche lobe overflow," even though the planet's surface is likely underfilling its Roche lobe by a factor of 2. C1 [Sanchis-Ojeda, R.; Isaacson, H.; Marcy, G. W.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Rappaport, S.; Dai, F.; Winn, J. N.; Yu, L.] MIT, Dept Phys, Cambridge, MA 02139 USA. [Rappaport, S.; Dai, F.; Winn, J. N.; Yu, L.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Palle, E.; Miles-Paez, P. A.; Montanes-Rodriguez, P.; Nowak, G.] IAC, E-38205 Tenerife, Spain. [Palle, E.; Gillon, M.; Miles-Paez, P. A.; Montanes-Rodriguez, P.; Nowak, G.] Univ La Laguna, Dept Astrofis, E-38206 Tenerife, Spain. [Delrez, L.; Jehin, E.] Univ Liege, Inst Astrophys & Geophys, B-4000 Liege, Belgium. [DeVore, J.] Visidyne Inc, Burlington, MA 01803 USA. [Gandolfi, D.] Univ Turin, Dipartimento Fis, I-10125 Turin, Italy. [Gandolfi, D.] Heidelberg Univ, Zentrum Astron, Landessternwarte Konigstuhl, D-69117 Heidelberg, Germany. [Fukui, A.] Natl Astron Observ Japan, Okayama Astrophys Observ, Asakuchi, Okayama 7190232, Japan. [Ribas, I.] CSIC IEEC, Inst Ciencies Espai, Fac Ciencias, E-08193 Bellaterra, Spain. [Stassun, K. G.; Paegert, M.] Vanderbilt Univ, Nashville, TN 37235 USA. [Stassun, K. G.] Fisk Univ, Nashville, TN 37208 USA. [Albrecht, S.; Van Eylen, V.] Aarhus Univ, Dept Phys & Astron, Stellar Astrophys Ctr, DK-8000 Aarhus C, Denmark. [Gaidos, E.] Univ Hawaii, Dept Geol & Geophys, Honolulu, HI 96822 USA. [Hirano, T.; Kuzuhara, M.] Tokyo Inst Technol, Dept Earth & Planetary Sci, Meguro Ku, Tokyo 1528551, Japan. [Holman, M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Howard, A. W.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Mann, A. W.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA. [Murgas, F.] Univ Grenoble Alpes, IPAG, F-38000 Grenoble, France. [Murgas, F.] CNRS, IPAG, F-38000 Grenoble, France. [Narita, N.; Onitsuka, M.] Natl Astron Observ Japan, Mitaka, Tokyo 1818588, Japan. [Narita, N.; Onitsuka, M.] SOKENDAI Grad Univ Adv Studies, Mitaka, Tokyo 1818588, Japan. [Narita, N.] Natl Inst Nat Sci, Astrobiol Ctr, Mitaka, Tokyo 1818588, Japan. RP Sanchis-Ojeda, R (reprint author), Univ Calif Berkeley, Dept Astron, 601 Campbell Hall, Berkeley, CA 94720 USA. EM sanchisojeda@berkeley.edu; sar@mit.edu; devore@visidyne.com RI Nowak, Grzegorz/H-8234-2014; OI Nowak, Grzegorz/0000-0002-7031-7754; Gandolfi, Davide/0000-0001-8627-9628; Stassun, Keivan/0000-0002-3481-9052 FU Japan Society for Promotion of Science (JSPS) Fellowship [25-3183]; Spanish Ministry of Economy and Competitiveness (MINECO); Fondo Europeo de Desarrollo Regional (FEDER) [ESP2013-48391-C4-1-R]; NASA through the Sagan Fellowship Program; Spanish MINECO [ESP2013-48391-C4-2-R]; National Aeronautics and Space Administration [NNH14CK55B]; French Agence Nationale de la Recherche (ANR) [ANR-12-BS05-0012 Exo-atmos] FX We thank Joshua Pepper and Smadar Naoz for helpful comments and an anonymous referee for suggestions that greatly improved the presentation of the material. We thank Allyson Bieryla and Dave Latham for helping us with the FLWO observations of the object. We are grateful to Evan Sinukoff, Erik Petigura, and Ian Crossfield for observing this target with Keck/HIRES. We thank Yi Yang for helping with the HSC images, and Takuya Suenaga for volunteering his time to do so. The help from the Subaru Telescope staff is greatly appreciated. We acknowledge Tsuguru Ryu for his support on the Okayama transit observations. T.H. is supported by Japan Society for Promotion of Science (JSPS) Fellowship for Research (No. 25-3183). I.R. acknowledges support from the Spanish Ministry of Economy and Competitiveness (MINECO) and the Fondo Europeo de Desarrollo Regional (FEDER) through grant ESP2013-48391-C4-1-R. We extend special thanks to those of Hawaiian ancestry on whose sacred mountain of Mauna Kea we are privileged to be guests. Without their generous hospitality, the Keck observations presented herein would not have been possible. This work was performed, in part, under contract with the Jet Propulsion Laboratory (JPL) funded by NASA through the Sagan Fellowship Program executed by the NASA Exoplanet Science Institute. This article is partly based on observations made with the Nordic Optical Telescope operated by the Nordic Optical Telescope Scientific Association and the Gran Telescopio Canarias operated on the island of La Palma by the IAC at the Spanish Observatorio del Roque de los Muchachos. This research has been supported by the Spanish MINECO grant number ESP2013-48391-C4-2-R. The Infrared Telescope Facility is operated by the University of Hawaii under contract NNH14CK55B with the National Aeronautics and Space Administration. FM acknowledges the support of the French Agence Nationale de la Recherche (ANR), under the program ANR-12-BS05-0012 Exo-atmos. NR 93 TC 33 Z9 33 U1 1 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD OCT 20 PY 2015 VL 812 IS 2 AR 112 DI 10.1088/0004-637X/812/2/112 PG 22 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CW7VD UT WOS:000365206600024 ER PT J AU Cole, DG AF Cole, Daniel G. TI Introduction to papers from the AutoCarto 2014 conference SO CARTOGRAPHY AND GEOGRAPHIC INFORMATION SCIENCE LA English DT Editorial Material C1 [Cole, Daniel G.] Smithsonian Inst, Washington, DC 20560 USA. RP Cole, DG (reprint author), Smithsonian Inst, Washington, DC 20560 USA. NR 0 TC 0 Z9 0 U1 2 U2 2 PU TAYLOR & FRANCIS INC PI PHILADELPHIA PA 530 WALNUT STREET, STE 850, PHILADELPHIA, PA 19106 USA SN 1523-0406 EI 1545-0465 J9 CARTOGR GEOGR INF SC JI Cartogr. Geogr. Inf. Sci. PD OCT 20 PY 2015 VL 42 IS 5 SI SI BP 379 EP 380 DI 10.1080/15230406.2015.1071561 PG 2 WC Geography SC Geography GA CW4GA UT WOS:000364948200001 ER PT J AU Baron-Szabo, RC AF Baron-Szabo, Rosemarie C. TI Paraclausastrea vorarlbergensis sp nov.; a new coral from the Lower Cretaceous of western Austria (Scleractinia; upper Barremian-lower Aptian; Schrattenkalk Fm.; Vorarlberg) SO ZOOTAXA LA English DT Article DE Lower Cretaceous; Helvetic Unit (Schrattenkalk Fm.); Vorarlberg (Austria); taxonomy; morphology; Scleractinia ID FRANCE; IRAN AB The new taxon Paraclausastrea vorarlbergensis sp. nov. is described from the upper Barremian- lower Aptian (Schrattenkalk Fm.) of western Austria (Vorarlberg). It belongs to the montlivaltiids and is characterized by thamnasterioid to submeandroid corallite integration, diameters of corallites ranging between 3 and 6.5 mm, and septa that are generally developed in 4 incomplete cycles in 6 generally irregular systems. In a small number corallites that are around 6 mm in diameter, 4 complete cycles are present. In corallites that are around 2 mm in diameter, usually between 12 and 18 septa are present. The new species differs from all other forms of Paraclausastrea in having the largest number of septa. This is the first report of this genus for the Schrattenkalk Formation. C1 [Baron-Szabo, Rosemarie C.] Smithsonian Inst, Dept Invertebrate Zool, Washington, DC 20013 USA. [Baron-Szabo, Rosemarie C.] Res Inst Senckenberg, D-60325 Frankfurt, Germany. RP Baron-Szabo, RC (reprint author), Smithsonian Inst, Dept Invertebrate Zool, MRC 163, Washington, DC 20013 USA. EM rosemarie_baronszabo@yahoo.com FU "Inatura" Museum, Dornbirn, Austria; Smithsonian Institution (SI) Washington, DC, USA; Honorary Researcher at the Research Institute Senckenberg, Frankfurt, Germany FX My thanks and gratitude go to DENNIS OPRESKO (Knoxville, Tennessee) and BERNARD LATHUILIERE (Nancy, France) for many discussions on coral taxonomy. Type material and additional study material was made accessible to me by GEORG FRIEBE ("Inatura", Dornbirn, Austria), and SYLVAIN CHARBONNIER and CHRISTINE PERRIN (both Museum d'Histoire Naturelle de Paris, France). For providing constructive reviews, I would like to thank BERNARD LATHUILIERE (Nancy, France) and an anonymous reviewer. As a Research Associate of the Smithsonian Institution (SI) Washington, DC, USA, and an Honorary Researcher at the Research Institute Senckenberg, Frankfurt, Germany, the author would like to express her deep appreciation for the continuing support from these institutions. I am especially grateful for the financial support by the "Inatura" Museum, Dornbirn, Austria. NR 27 TC 0 Z9 0 U1 0 U2 0 PU MAGNOLIA PRESS PI AUCKLAND PA PO BOX 41383, AUCKLAND, ST LUKES 1030, NEW ZEALAND SN 1175-5326 EI 1175-5334 J9 ZOOTAXA JI Zootaxa PD OCT 16 PY 2015 VL 4032 IS 3 BP 327 EP 332 PG 6 WC Zoology SC Zoology GA CT7BF UT WOS:000362967400009 PM 26624368 ER PT J AU Hong, T AF Hong, Terry TI The Hundred-Year Flood 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 OCT 15 PY 2015 VL 140 IS 17 BP 76 EP 76 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA CT8RP UT WOS:000363084400085 ER PT J AU Hong, T AF Hong, Terry TI The Girl Who Wrote Loneliness 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 OCT 15 PY 2015 VL 140 IS 17 BP 81 EP 82 PG 2 WC Information Science & Library Science SC Information Science & Library Science GA CT8RP UT WOS:000363084400113 ER PT J AU Hong, T AF Hong, Terry TI Love Love. 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 OCT 15 PY 2015 VL 140 IS 17 BP 83 EP 84 PG 2 WC Information Science & Library Science SC Information Science & Library Science GA CT8RP UT WOS:000363084400123 ER PT J AU Brodu, E Balat-Pichelin, M Sans, JL Freeman, MD Kasper, JC AF Brodu, E. Balat-Pichelin, M. Sans, J. L. Freeman, M. D. Kasper, J. C. TI Efficiency and behavior of textured high emissivity metallic coatings at high temperature SO MATERIALS & DESIGN LA English DT Article DE Emissivity; Metallic coating; Refractory metal; Surface texturing; Surface roughness ID TUNGSTEN AB Three metallic coatings with textured surfaces, made of rhenium, tungsten and molybdenum, were studied in the frame of the Solar Probe Plus mission (NASA) as candidate materials. The role of these coatings is to dissipate a maximum of energy from a hot instrument facing the Sun, by the mean of their high total hemispherical emissivity. The total hemispherical emissivity of the three coatings was measured in the temperature range 1100-1900 K, as well as over time in order to study their high temperature stability. Various emissivity levels were obtained depending on the surface texture. The highest total hemispherical emissivity was obtained on a rhenium coating, with an emissivity of 0.8 in the temperature range 1300-1700 K. However, this rhenium coating with a fine, sharp surface texture, presented an instability at high temperature, which might limit its optimal operating temperature to about 1500 K. As for the tungsten coating, the total hemispherical emissivity was increased by a factor 2 due to the enhanced surface texturation and its great stability over the whole temperature range was shown. (C) 2015 Elsevier Ltd. All rights reserved. C1 [Brodu, E.; Balat-Pichelin, M.; Sans, J. L.] PROMES CNRS, Lab Proc Mat & Energie Solaire, F-66120 Font Romeu, France. [Brodu, E.; Freeman, M. D.; Kasper, J. C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Balat-Pichelin, M (reprint author), PROMES CNRS, Lab Proc Mat & Energie Solaire, 7 Rue Four Solaire, F-66120 Font Romeu, France. EM marianne.balat@promes.cnrs.fr FU CNES, France FX The authors gratefully acknowledge CNES, France and particularly J.Y. Prado for the support of the PhD of E. Brodu. NR 15 TC 4 Z9 4 U1 4 U2 28 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 0264-1275 EI 1873-4197 J9 MATER DESIGN JI Mater. Des. PD OCT 15 PY 2015 VL 83 BP 85 EP 94 DI 10.1016/j.matdes.2015.05.073 PG 10 WC Materials Science, Multidisciplinary SC Materials Science GA CO7HA UT WOS:000359329000011 ER PT J AU Pinto, CM Ocana-Mayorga, S Tapia, EE Lobos, SE Zurita, AP Aguirre-Villacis, F MacDonald, A Villacis, AG Lima, L Teixeira, MMG Grijalva, MJ Perkins, SL AF Pinto, C. Miguel Ocana-Mayorga, Sofia Tapia, Elicio E. Lobos, Simon E. Zurita, Alejandra P. Aguirre-Villacis, Fernanda MacDonald, Amber Villacis, Anita G. Lima, Luciana Teixeira, Marta M. G. Grijalva, Mario J. Perkins, Susan L. TI Bats, Trypanosomes, and Triatomines in Ecuador: New Insights into the Diversity, Transmission, and Origins of Trypanosoma cruzi and Chagas Disease SO PLOS ONE LA English DT Article ID KINETOPLAST MINICIRCLE DNA; PHYLOGENETIC-RELATIONSHIPS; SOUTHERN ECUADOR; CYTOCHROME-B; RISK-FACTORS; FRUIT BAT; EVOLUTIONARY; INFECTION; AMERICA; GENE AB The generalist parasite Trypanosoma cruzi has two phylogenetic lineages associated almost exclusively with bats-Trypanosoma cruzi Tcbat and the subspecies T. c. marinkellei. We present new information on the genetic variation, geographic distribution, host associations, and potential vectors of these lineages. We conducted field surveys of bats and triatomines in southern Ecuador, a country endemic for Chagas disease, and screened for trypanosomes by microscopy and PCR. We identified parasites at species and genotype levels through phylogenetic approaches based on 18S ribosomal RNA (18S rRNA) and cytochrome b (cytb) genes and conducted a comparison of nucleotide diversity of the cytb gene. We document for the first time T. cruzi Tcbat and T. c. marinkellei in Ecuador, expanding their distribution in South America to the western side of the Andes. In addition, we found the triatomines Cavernicola pilosa and Triatoma dispar sharing shelters with bats. The comparisons of nucleotide diversity revealed a higher diversity for T. c. marinkellei than any of the T. c. cruzi genotypes associated with Chagas disease. Findings from this study increased both the number of host species and known geographical ranges of both parasites and suggest potential vectors for these two trypanosomes associated with bats in rural areas of southern Ecuador. The higher nucleotide diversity of T. c. marinkellei supports a long evolutionary relationship between T. cruzi and bats, implying that bats are the original hosts of this important parasite. C1 [Pinto, C. Miguel; Ocana-Mayorga, Sofia; Lobos, Simon E.; Zurita, Alejandra P.; Aguirre-Villacis, Fernanda; MacDonald, Amber; Villacis, Anita G.; Grijalva, Mario J.] Pontificia Univ Catolica Ecuador, Ctr Invest Enfermedades Infecciosas, Quito, Ecuador. [Pinto, C. Miguel; Perkins, Susan L.] Amer Museum Nat Hist, Sackler Inst Comparat Genom, New York, NY 10024 USA. [Pinto, C. Miguel] Amer Museum Nat Hist, Dept Mammal, New York, NY 10024 USA. [Pinto, C. Miguel] CUNY, Grad Ctr, New York, NY USA. [Pinto, C. Miguel] Smithsonian Inst, Natl Museum Nat Hist, Div Mammals, Washington, DE USA. [Ocana-Mayorga, Sofia; Grijalva, Mario J.] Ohio Univ, Trop Dis Inst, Dept Biomed Sci, Heritage Coll Osteopath Med, Athens, OH 45701 USA. [Tapia, Elicio E.] Fdn Otonga, Quito, Ecuador. [Lima, Luciana; Teixeira, Marta M. G.] Univ Sao Paulo, Inst Ciencias Biomed, Dept Parasitol, BR-05508 Sao Paulo, SP, Brazil. RP Pinto, CM (reprint author), Pontificia Univ Catolica Ecuador, Ctr Invest Enfermedades Infecciosas, Quito, Ecuador. EM pintom@si.edu FU NIH Academic Research Enhancement Award [1R15AI077896-01]; Latin American Student Field Research Award from the American Society of Mammalogists; NSF-DDIG grant [DEB-1311582]; Global Infectious Disease Training Grant of Fogarty International Center [1D43TW008261-01A1]; Graduate Student Fellowship of the American Museum of Natural History; [PUCE I13048] FX Fieldwork support was provided by Proyecto PUCE I13048 to SO-M and MJG, NIH Academic Research Enhancement Award 1R15AI077896-01 to MJG, and a Latin American Student Field Research Award from the American Society of Mammalogists to CMP. Laboratory work was supported by a NSF-DDIG grant DEB-1311582 to SLP and CMP, and Global Infectious Disease Training Grant 1D43TW008261-01A1 of Fogarty International Center to MJG. Data analyses was supported by a Graduate Student Fellowship of the American Museum of Natural History to CMP. The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 66 TC 7 Z9 7 U1 9 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 OCT 14 PY 2015 VL 10 IS 10 AR e0139999 DI 10.1371/journal.pone.0139999 PG 13 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA CU0CK UT WOS:000363183100070 PM 26465748 ER PT J AU Zapata, F Goetz, FE Smith, SA Howison, M Siebert, S Church, SH Sanders, SM Ames, CL McFadden, CS France, SC Daly, M Collins, AG Haddock, SHD Dunn, CW Cartwright, P AF Zapata, Felipe Goetz, Freya E. Smith, Stephen A. Howison, Mark Siebert, Stefan Church, Samuel H. Sanders, Steven M. Ames, Cheryl Lewis McFadden, Catherine S. France, Scott C. Daly, Marymegan Collins, Allen G. Haddock, Steven H. D. Dunn, Casey W. Cartwright, Paulyn TI Phylogenomic Analyses Support Traditional Relationships within Cnidaria SO PLOS ONE LA English DT Article ID CLASS-LEVEL RELATIONSHIPS; PHYLUM-CNIDARIA; ANTHOZOA CNIDARIA; OCTOCORALLIA CNIDARIA; MITOCHONDRIAL GENOME; CHARACTER EVOLUTION; HYDROZOA; RDNA; SEQUENCES; MEDUSOZOA AB Cnidaria, the sister group to Bilateria, is a highly diverse group of animals in terms of morphology, lifecycles, ecology, and development. How this diversity originated and evolved is not well understood because phylogenetic relationships among major cnidarian lineages are unclear, and recent studies present contrasting phylogenetic hypotheses. Here, we use transcriptome data from 15 newly-sequenced species in combination with 26 publicly available genomes and transcriptomes to assess phylogenetic relationships among major cnidarian lineages. Phylogenetic analyses using different partition schemes and models of molecular evolution, as well as topology tests for alternative phylogenetic relationships, support the monophyly of Medusozoa, Anthozoa, Octocorallia, Hydrozoa, and a clade consisting of Staurozoa, Cubozoa, and Scyphozoa. Support for the monophyly of Hexacorallia is weak due to the equivocal position of Ceriantharia. Taken together, these results further resolve deep cnidarian relationships, largely support traditional phylogenetic views on relationships, and provide a historical framework for studying the evolutionary processes involved in one of the most ancient animal radiations. C1 [Zapata, Felipe; Goetz, Freya E.; Smith, Stephen A.; Howison, Mark; Siebert, Stefan; Church, Samuel H.; Dunn, Casey W.] Brown Univ, Dept Ecol & Evolutionary Biol, Providence, RI 02912 USA. [Howison, Mark] Brown Univ, Comp Serv, Providence, RI 02912 USA. [Howison, Mark] Brown Univ, Informat Serv, Providence, RI 02912 USA. [Sanders, Steven M.; Cartwright, Paulyn] Univ Kansas, Dept Ecol & Evolutionary Biol, Lawrence, KS 66045 USA. [Ames, Cheryl Lewis; Collins, Allen G.] Smithsonian Museum Nat Hist, Dept Invertebrate Zool, Washington, DC USA. [Ames, Cheryl Lewis] Univ Maryland, Biol Sci Grad Program, College Pk, MD 20742 USA. [McFadden, Catherine S.] Harvey Mudd Coll, Dept Biol, Claremont, CA 91711 USA. [France, Scott C.] Univ Louisiana Lafayette, Dept Biol, Lafayette, LA 70504 USA. [Daly, Marymegan] Ohio State Univ, Dept Evolut Ecol & Organismal Biol, Columbus, OH 43210 USA. [Collins, Allen G.] NOAA, Natl Systemat Lab, Fisheries Serv, Natl Museum Nat Hist, Washington, DC USA. [Haddock, Steven H. D.] Monterey Bay Aquarium Res Inst, Moss Landing, CA USA. RP Zapata, F (reprint author), Brown Univ, Dept Ecol & Evolutionary Biol, Providence, RI 02912 USA. EM felipe_zapata@brown.edu OI Smith, Stephen/0000-0003-2035-9531; Zapata, Felipe/0000-0002-9386-0573; Dunn, Casey/0000-0003-0628-5150 FU National Science Foundation Cnidarian Tree of Life Project [DEB 05-31799]; National Science Foundation [DEB-0953571, RII-C2 EPS-1005789]; National Science Foundation Alan T Waterman Award; National Institutes of Health [P30RR031153]; National Science Foundation EPSCoR [EPS-1004057]; State of Rhode Island; Smithsonian Peter Buck Fellowship; Iridian Genomes Inc. FX This project was supported by the National Science Foundation (http://www.nsf.gov) Cnidarian Tree of Life Project (DEB 05-31799 to PC and AGC), National Science Foundation DEB-0953571 to PC and the National Science Foundation Alan T Waterman Award to CWD. Sequencing at the Brown Genomics Core facility was supported in part by National Institutes of Health (http://www.nih.gov) P30RR031153 and National Science Foundation EPSCoR EPS-1004057. Data transfer was supported by National Science Foundation RII-C2 EPS-1005789. Analyses were conducted with computational resources and services at the Center for Computation and Visualization at Brown University, supported in part by the National Science Foundation EPSCoR EPS-1004057 and the State of Rhode Island. Cubozoan samples were collected by CLA thanks to research funds from a Smithsonian Peter Buck Fellowship and Iridian Genomes Inc. The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 49 TC 19 Z9 20 U1 11 U2 30 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 OCT 14 PY 2015 VL 10 IS 10 AR e0139068 DI 10.1371/journal.pone.0139068 PG 13 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA CU0CK UT WOS:000363183100037 PM 26465609 ER PT J AU Patrick, CJ Weller, DE AF Patrick, Christopher J. Weller, Donald E. TI Interannual variation in submerged aquatic vegetation and its relationship to water quality in subestuaries of Chesapeake Bay SO MARINE ECOLOGY PROGRESS SERIES LA English DT Article DE Empirical orthogonal function; Aquatic plants; Water clarity; Multiple stressors; Community identity; Time series analysis ID EELGRASS ZOSTERA-MARINA; RHODE RIVER; VALLISNERIA-AMERICANA; LIGHT AVAILABILITY; SEAGRASS MEADOWS; UNITED-STATES; NURSERY ROLE; TIME-SERIES; ABUNDANCE; USA AB The abundance of submerged aquatic vegetation (SAV) fluctuates from year to year, and these fluctuations differ among the tributary embayments within estuaries. Quantifying the causes and spatial patterns of interannual variability in SAV abundance is critical to understanding the dynamics of SAV in complex estuaries. We applied empirical orthogonal function (EOF) analysis to quantify the temporal synchronicity among embayments within each of 3 salinity zones (oligohaline, mesohaline, and polyhaline) of Chesapeake Bay. EOF analysis extracts shared modes of variation among the embayments in each zone. The amount of synchronicity differed among zones, and embayments were most synchronous within the polyhaline zone. The extracted modes of variation showed that fluctuations in SAV abundance are not synchronized among the salinity zones. We detrended the modes of common variation in SAV abundance for each salinity zone and then used cross-correlation analysis to compare the detrended modes to detrended water quality variables (dissolved organic carbon, suspended solids, chlorophyll a, Secchi depth, river nitrogen load, temperature, and salinity). The water quality variables that were significantly related to SAV abundance differed among salinity zones. Chlorophyll a levels in months when seed germination and shoot production rates are high were important negative predictors in the oligohaline and polyhaline zones, possibly because young SAV plants are especially sensitive to even short-term disturbances. As the SAV communities in the 3 salinity zones have different year-to-year dynamics and different responses to stressors, conservation, restoration, and management plans should be tailored to each community. C1 [Patrick, Christopher J.; Weller, Donald E.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. RP Patrick, CJ (reprint author), Smithsonian Environm Res Ctr, POB 28,647 Contees Wharf Rd, Edgewater, MD 21037 USA. EM patrickc@si.edu OI Weller, Donald/0000-0002-7629-5437 FU National Oceanic and Atmospheric Administration (NOAA) Center for Sponsored Coastal Ocean Research (CSCOR) [NA09NOS4780214] FX We thank the Virginia Institute of Marine Sciences, the Maryland Department of Natural Resources, and the Chesapeake Bay Program for providing the data used in our analysis. This work was supported by award number NA09NOS4780214 from the National Oceanic and Atmospheric Administration (NOAA) Center for Sponsored Coastal Ocean Research (CSCOR). Thanks to Matthew Ogburn for statistical consulting, to Robert J. Orth for discussion about SAV data collection and ecology, and to Micah Ryder and Meghan Williams for spatial analysis. NR 67 TC 1 Z9 1 U1 4 U2 21 PU INTER-RESEARCH PI OLDENDORF LUHE PA NORDBUNTE 23, D-21385 OLDENDORF LUHE, GERMANY SN 0171-8630 EI 1616-1599 J9 MAR ECOL PROG SER JI Mar. Ecol.-Prog. Ser. PD OCT 14 PY 2015 VL 537 BP 121 EP 135 DI 10.3354/meps11412 PG 15 WC Ecology; Marine & Freshwater Biology; Oceanography SC Environmental Sciences & Ecology; Marine & Freshwater Biology; Oceanography GA CU0BR UT WOS:000363180900010 ER PT J AU Bariani, F Seok, H Singh, S Vengalattore, M Meystre, P AF Bariani, F. Seok, H. Singh, S. Vengalattore, M. Meystre, P. TI Atom-based coherent quantum-noise cancellation in optomechanics SO PHYSICAL REVIEW A LA English DT Article AB We analyze a quantum force sensor that uses coherent quantum-noise cancellation (CQNC) to beat the standard quantum limit. This sensor, which allows for the continuous, broadband detection of feeble forces, is a hybrid dual-cavity system composed of amesoscopicmechanical resonator optically coupled to an ensemble of ultracold atoms. In contrast to the stringent constraints on dissipation typically associated with purely optical schemes of CQNC, the dissipation rate of the mechanical resonator only needs to be matched to the decoherence rate of the atomic ensemble-a condition that is experimentally achievable even for the technologically relevant regime of low-frequency mechanical resonators with large quality factors. The modular nature of the system further allows the atomic ensemble to aid in the cooling of the mechanical resonator, thereby combining atom-mediated state preparation with sensing deep in the quantum regime. C1 [Bariani, F.; Seok, H.; Meystre, P.] Univ Arizona, Dept Phys, Coll Opt Sci, Tucson, AZ 85721 USA. [Bariani, F.; Seok, H.; Meystre, P.] Univ Arizona, Inst B2, Tucson, AZ 85721 USA. [Seok, H.] Kongju Natl Univ, Dept Phys Educ, Kong Ju 314701, South Korea. [Singh, S.] Harvard Smithsonian Ctr Astrophys, ITAMP, Cambridge, MA 02138 USA. [Vengalattore, M.] Cornell Univ, Lab Atom & Solid State Phys, Ithaca, NY 14853 USA. RP Bariani, F (reprint author), Univ Arizona, Dept Phys, Coll Opt Sci, Tucson, AZ 85721 USA. FU DARPA QuASAR; ORCHID programs through AFOSR; ORCHID programs through ARO; NSF INSPIRE program; U.S. Army Research Office; U.S. NSF; Sloan Foundation FX We thank E. S. Polzik, K. Hammerer, Y. S. Patil, and S. Chakram for useful discussions. This work was supported by the DARPA QuASAR and ORCHID programs through grants from AFOSR and ARO, the NSF INSPIRE program, the U.S. Army Research Office, and the U.S. NSF. M.V. acknowledges support from the Sloan Foundation. NR 30 TC 4 Z9 4 U1 4 U2 11 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 OCT 14 PY 2015 VL 92 IS 4 AR 043817 DI 10.1103/PhysRevA.92.043817 PG 6 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA CT5ZO UT WOS:000362890000012 ER PT J AU Putman, SB Brown, JL Franklin, AD Schneider, EC Boisseau, NP Asa, CS Pukazhenthi, BS AF Putman, Sarah B. Brown, Janine L. Franklin, Ashley D. Schneider, Emily C. Boisseau, Nicole P. Asa, Cheryl S. Pukazhenthi, Budhan S. TI Characterization of Ovarian Steroid Patterns in Female African Lions (Panthera leo), and the Effects of Contraception on Reproductive Function SO PLOS ONE LA English DT Article ID CHEETAH ACINONYX-JUBATUS; GNRH ANALOG DESLORELIN; MELENGESTROL ACETATE; MEGESTROL-ACETATE; INDUCED OVULATION; SEXUAL-BEHAVIOR; ESTROUS-CYCLE; DOMESTIC CAT; SOUTH-AFRICA; ESTRUS AB Because of poor reproduction after the lifting of an 8-year breeding moratorium, a biomedical survey of female lions in U.S. zoos was initiated in 2007. Fecal estrogen (FEM), progestagen (FPM) and glucocorticoid (FGM) metabolites were analyzed in samples collected 3-4 times per wk from 28 lions at 17 facilities (0.9-13.8 yr of age) for 4 mo-3.5 yr and body weights were obtained similar to monthly from 17 animals at eight facilities (0.0-3.0 yr of age). Based on FEM, estrous cycle length averaged 17.5 +/- 0.4 d in duration, with estrus lasting 4.4 +/- 0.2 d. All but one female exhibited waves of estrogenic activity indicative of follicular activity; however, not all females expressed estrous behaviors (73%), suggesting silent estrus was common. Female lions experienced puberty earlier than expected; waves of estrogenic activity were observed as young as 1.1 yr of age, which may be related to a faster growth rate of captive vs. wild lions. Mean gestation length was 109.5 +/- 1.0 d, whereas the non-pregnant luteal phase was less than half (46.0 +/- 1.2 d). Non-mating induced increases in FPM were observed in 33% of females housed without a male, consistent with spontaneous ovulation. A number of study animals had been contracepted, and the return to cyclicity after treatment withdrawal, while variable, was similar to 4.0 yr and longer than the 1-yr expected efficacy, especially for those implanted with Suprelorin. For FGM, there were no differences in overall, baseline or peak mean concentrations among the age groups or across seasons, nor were there any relationships between reproductive parameters and FGM concentrations. Overall, results suggest that poor reproduction in lions after the breeding moratorium was not related to altered adrenal or ovarian steroid activity, but for some females may have been a consequence of individual institutions' management decisions. C1 [Putman, Sarah B.; Brown, Janine L.; Franklin, Ashley D.; Schneider, Emily C.; Boisseau, Nicole P.; Pukazhenthi, Budhan S.] Smithsonian Conservat Biol Inst, Front Royal, VA 22630 USA. [Putman, Sarah B.] George Mason Univ, Fairfax, VA 22030 USA. [Franklin, Ashley D.] Point Defiance Zoo & Aquarium, Tacoma, WA USA. [Schneider, Emily C.] Shady Grove Fertil, Rockville, MD USA. [Asa, Cheryl S.] AZA Wildlife Contracept Ctr, St Louis, MO USA. RP Pukazhenthi, BS (reprint author), Smithsonian Conservat Biol Inst, Front Royal, VA 22630 USA. EM pukazhenthib@si.edu RI Franklin, Ashley/J-3069-2015 OI Franklin, Ashley/0000-0002-0818-5156 FU ASLAN Fund National Zoo; Ritz Carlton FX This work was supported by ASLAN Fund National Zoo and Ritz Carlton. The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 106 TC 0 Z9 0 U1 5 U2 18 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 OCT 13 PY 2015 VL 10 IS 10 AR e0140373 DI 10.1371/journal.pone.0140373 PG 27 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA CT6ZJ UT WOS:000362962300085 PM 26460849 ER PT J AU Babadi, M Demler, E Knap, M AF Babadi, Mehrtash Demler, Eugene Knap, Michael TI Far-from-Equilibrium Field Theory of Many-Body Quantum Spin Systems: Prethermalization and Relaxation of Spin Spiral States in Three Dimensions SO PHYSICAL REVIEW X LA English DT Article ID DYNAMICS; THERMALIZATION; MECHANICS; LATTICE; LOCALIZATION; PROPAGATION; TRANSITIONS; DOMAINS; MODELS AB We study theoretically the far-from-equilibrium relaxation dynamics of spin spiral states in the three-dimensional isotropic Heisenberg model. The investigated problem serves as an archetype for understanding quantum dynamics of isolated many-body systems in the vicinity of a spontaneously broken continuous symmetry. We present a field-theoretical formalism that systematically improves on the mean field for describing the real-time quantum dynamics of generic spin-1/2 systems. This is achieved by mapping spins to Majorana fermions followed by a 1/N expansion of the resulting two-particle-irreducible effective action. Our analysis reveals rich fluctuation-induced relaxation dynamics in the unitary evolution of spin spiral states. In particular, we find the sudden appearance of long-lived prethermalized plateaus with diverging lifetimes as the spiral winding is tuned toward the thermodynamically stable ferro-or antiferromagnetic phases. The emerging prethermalized states are characterized by different bosonic modes being thermally populated at different effective temperatures and by a hierarchical relaxation process reminiscent of glassy systems. Spin-spin correlators found by solving the nonequilibrium Bethe-Salpeter equation provide further insight into the dynamic formation of correlations, the fate of unstable collective modes, and the emergence of fluctuation-dissipation relations. Our predictions can be verified experimentally using recent realizations of spin spiral states with ultracold atoms in a quantum gas microscope. C1 [Babadi, Mehrtash] CALTECH, Inst Quantum Informat & Matter, Pasadena, CA 91125 USA. [Demler, Eugene; Knap, Michael] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. [Knap, Michael] Harvard Smithsonian Ctr Astrophys, ITAMP, Cambridge, MA 02138 USA. [Knap, Michael] Tech Univ Munich, Dept Phys, Walter Schottky Inst, D-85748 Garching, Germany. [Knap, Michael] Tech Univ Munich, Inst Adv Study, D-85748 Garching, Germany. RP Babadi, M (reprint author), CALTECH, Inst Quantum Informat & Matter, Pasadena, CA 91125 USA. RI Knap, Michael/H-3344-2011 OI Knap, Michael/0000-0002-7093-9502 FU Harvard-MIT CUA; NSF [DMR-1308435]; AFOSR Quantum Simulation MURI; ARO-MURI on Atomtronics; ARO MURI Quism program; Humboldt Foundation; Institute for Quantum Information and Matter; Gordon and Betty Moore Foundation; Austrian Science Fund (FWF) Project [J 3361-N20]; Technische Universitat Munchen-Institute for Advanced Study - German Excellence Initiative; European Union [291763]; Walter Haefner Foundation; ETH Foundation; NSF Physics Frontiers Center FX We thank S. Gopalakrishnan, B. I. Halperin, and S. Sachdev for useful discussions. We acknowledge support from Harvard-MIT CUA, NSF Grant No. DMR-1308435, AFOSR Quantum Simulation MURI, the ARO-MURI on Atomtronics, ARO MURI Quism program, Humboldt Foundation, the Institute for Quantum Information and Matter, an NSF Physics Frontiers Center with support of the Gordon and Betty Moore Foundation, the Austrian Science Fund (FWF) Project No. J 3361-N20, as well as Technische Universitat Munchen-Institute for Advanced Study, funded by the German Excellence Initiative and the European Union FP7 under grant agreement No. 291763. E.D. acknowledges support from Dr. Max Rossler, the Walter Haefner Foundation, and the ETH Foundation. NR 81 TC 14 Z9 14 U1 2 U2 11 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 2160-3308 J9 PHYS REV X JI Phys. Rev. X PD OCT 12 PY 2015 VL 5 IS 4 AR 041005 DI 10.1103/PhysRevX.5.041005 PG 18 WC Physics, Multidisciplinary SC Physics GA CT6EZ UT WOS:000362906500001 ER PT J AU Pei, NC Erickson, DL Chen, BF Ge, XJ Mi, XC Swenson, NG Zhang, JL Jones, FA Huang, CL Ye, WH Hao, ZQ Hsieh, CF Lum, S Bourg, NA Parker, JD Zimmerman, JK McShea, WJ Lopez, IC Sun, IF Davies, SJ Ma, KP Kress, WJ AF Pei, Nancai Erickson, David L. Chen, Bufeng Ge, Xuejun Mi, Xiangcheng Swenson, Nathan G. Zhang, Jin-Long Jones, Frank A. Huang, Chun-Lin Ye, Wanhui Hao, Zhanqing Hsieh, Chang-Fu Lum, Shawn Bourg, Norman A. Parker, John D. Zimmerman, Jess K. McShea, William J. Lopez, Ida C. Sun, I-Fang Davies, Stuart J. Ma, Keping Kress, W. John TI Closely-related taxa influence woody species discrimination via DNA barcoding: evidence from global forest dynamics plots SO SCIENTIFIC REPORTS LA English DT Article ID LAND PLANTS; BIODIVERSITY HOTSPOTS; INTEGRATIVE TAXONOMY; TROPICAL FORESTS; DIVERSITY; CHINA; IDENTIFICATION; CONSERVATION; DELIMITATION; TREES AB To determine how well DNA barcodes from the chloroplast region perform in forest dynamics plots (FDPs) from global CTFS-ForestGEO network, we analyzed DNA barcoding sequences of 1277 plant species from a wide phylogenetic range (3 FDPs in tropics, 5 in subtropics and 5 in temperate zone) and compared the rates of species discrimination (RSD). We quantified RSD by two DNA barcode combinations (rbcL + matK and rbcL + matK + trnH-psbA) using a monophyly-based method (GARLI). We defined two indexes of closely-related taxa (G(m)/G(t) and S/G ratios) and correlated these ratios with RSD. The combination of rbcL + matK averagely discriminated 88.65%, 83.84% and 72.51% at the local, regional and global scales, respectively. An additional locus trnH-psbA increased RSD by 2.87%, 1.49% and 3.58% correspondingly. RSD varied along a latitudinal gradient and were negatively correlated with ratios of closely-related taxa. Successes of species discrimination generally depend on scales in global FDPs. We suggested that the combination of rbcL + matK + trnH-psbA is currently applicable for DNA barcoding-based phylogenetic studies on forest communities. C1 [Pei, Nancai; Chen, Bufeng] Chinese Acad Forestry, State Key Lab Tree Genet & Breeding, Beijing 100091, Peoples R China. [Pei, Nancai; Chen, Bufeng] Chinese Acad Forestry, Res Inst Trop Forestry, Guangzhou 510520, Guangdong, Peoples R China. [Erickson, David L.; Lopez, Ida C.; Kress, W. John] Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, Washington, DC 20013 USA. [Ge, Xuejun; Ye, Wanhui] Chinese Acad Sci, South China Bot Garden, Guangzhou 510650, Guangdong, Peoples R China. [Mi, Xiangcheng; Ma, Keping] Chinese Acad Sci, Inst Bot, State Key Lab Vegetat & Environm Change, Beijing 100093, Peoples R China. [Swenson, Nathan G.] Univ Maryland, Dept Biol, College Pk, MD 20742 USA. [Zhang, Jin-Long] Kadoorie Farm & Bot Garden, Flora Conservat Dept, Tai Po, Hong Kong, Peoples R China. [Jones, Frank A.] Oregon State Univ, Dept Bot & Plant Pathol, Corvallis, OR 97331 USA. [Huang, Chun-Lin] Natl Museum Nat Sci, Dept Biol, Lab Mol Phylogenet, Taichung, Taiwan. [Hao, Zhanqing] Chinese Acad Sci, Inst Appl Ecol, State Key Lab Forest & Soil Ecol, Shenyang 110016, Peoples R China. [Hsieh, Chang-Fu] Natl Taiwan Univ, Inst Ecol & Evolutionary Biol, Taipei 10764, Taiwan. [Lum, Shawn] Nanyang Technol Univ, Natl Inst Educ, Singapore 637616, Singapore. [Bourg, Norman A.; McShea, William J.] Smithsonian Conservat Biol Inst, Front Royal, VA USA. [Parker, John D.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. [Zimmerman, Jess K.] Univ Puerto Rico, Inst Trop Ecosyst Studies, San Juan, PR 00936 USA. [Sun, I-Fang] Natl Dong Hwa Univ, Dept Nat Resources & Environm Studies, Hualien 97401, Taiwan. [Davies, Stuart J.] Smithsonian Trop Res Inst, Forest Global Earth Observ, Ctr Trop Forest Sci, Washington, DC 20013 USA. RP Pei, NC (reprint author), Chinese Acad Forestry, State Key Lab Tree Genet & Breeding, Beijing 100091, Peoples R China. EM nancai.pei@gmail.com; kressj@si.edu RI Parker, John/F-9761-2010; OI Parker, John/0000-0002-3632-7625; Zhang, Jinlong/0000-0002-1161-5460; Bourg, Norman/0000-0002-7443-1992 FU Special Fund for Forest Scientific Research in the Public Welfare [20140430105]; NSF-China [31200471]; Ministry of Finance of the People's Republic of China [RITFYWZX201208]; China Scholarship Council [201303270006]; CFERN & GENE Award Funds on Ecological Paper FX Funding was provided by the Special Fund for Forest Scientific Research in the Public Welfare (20140430105), NSF-China (31200471), the Ministry of Finance of the People's Republic of China (RITFYWZX201208), China Scholarship Council (201303270006), and CFERN & GENE Award Funds on Ecological Paper. We appreciate J.L., S.G., H.Y., N.Z., Y.F., Y.Z. and X.Y. for useful discussion, and thank many assistants of CTFS-ForestGEO FDPs in the field and technicians in the lab. We also thank the anonymous reviewers for their valuable comments on the manuscript. NR 61 TC 2 Z9 2 U1 7 U2 42 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 OCT 12 PY 2015 VL 5 AR 15127 DI 10.1038/srep15127 PG 9 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA CT1MV UT WOS:000362563500001 PM 26456472 ER PT J AU Gagne, RJ Etienne, J AF Gagne, Raymond J. Etienne, Jean TI Three new genera and three new species of Lasiopteridi (Diptera: Cecidomyiidae) on Rubiaceae from Guadeloupe, French West Indies, and a key to genera of Neotropical Lasiopteridi unplaced to tribe SO ZOOTAXA LA English DT Article DE Lasiopteridi; Faramea; Psychotria; gall midges; Neotropical AB Three new genera of Lasiopteridi (Diptera: Cecidomyiidae), Faramitella Gagne, new genus, Anapeza Gagne, new genus, and Pellacara Gagne, new genus, each with one new species, are described. The new species are from leaf galls on Rubiaceae collected in Guadeloupe, F.W.I.: Faramitella planicauda Gagne, new species, was reared from Faramea occidentalis (L.) A. Rich.; Anapeza tumida Gagne, new species, and Pellacara postica, new species, were both reared from Psychotria mapourioides DC. The three new genera belong to Lasiopteridi but are unassigned to tribe. A key to the adult stage of these and 23 other Neotropical genera of unplaced Lasiopteridi whose adults are known is provided. C1 [Gagne, Raymond J.] USDA ARS, Systemat Entomol Lab, PSI, Smithsonian Inst, Washington, DC 20013 USA. [Etienne, Jean] Ctr Antilles Guyane, Inst Natl Rech Agron, F-97170 Petit Bourg, Guadeloupe. RP Gagne, RJ (reprint author), USDA ARS, Systemat Entomol Lab, PSI, Smithsonian Inst, MRC 168,POB 37012, Washington, DC 20013 USA. EM raymond.gagne@ars.usda.gov; jean.etienne2@wanadoo.fr NR 13 TC 0 Z9 0 U1 1 U2 2 PU MAGNOLIA PRESS PI AUCKLAND PA PO BOX 41383, AUCKLAND, ST LUKES 1030, NEW ZEALAND SN 1175-5326 EI 1175-5334 J9 ZOOTAXA JI Zootaxa PD OCT 12 PY 2015 VL 4028 IS 4 BP 511 EP 526 PG 16 WC Zoology SC Zoology GA CT2QK UT WOS:000362648100003 PM 26624324 ER PT J AU Wright, CM Maddison, ST Wilner, DJ Burton, MG Lommen, D van Dishoeck, EF Pinilla, P Bourke, TL Menard, F Walsh, C AF Wright, C. M. Maddison, S. T. Wilner, D. J. Burton, M. G. Lommen, D. van Dishoeck, E. F. Pinilla, P. Bourke, T. L. Menard, F. Walsh, C. TI Resolving structure of the disc around HD100546 at 7 mm with ATCA SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE protoplanetary discs; circumstellar matter; planetary systems; stars: pre-main-sequence; radio continuum: stars ID HERBIG-AE/BE STARS; T-TAURI STARS; GIANT PLANET FORMATION; BROWN DWARF DESERT; NEAR-INFRARED SPECTROSCOPY; POLARIZED SCATTERED-LIGHT; RADIO-CONTINUUM EMISSION; TELESCOPE COMPACT ARRAY; INTERMEDIATE-MASS STARS; 206462 HD 135344B AB There is much evidence that planet formation is occurring in the disc around the Herbig Be star HD100546. To learn more about the processes occurring in this disc, we conducted high-resolution imaging at 43/45 GHz with the Australia Telescope Compact Array. Multiple array configurations were used, providing a best spatial resolution of similar to 0.15 arcsec, or 15 au at HD100546's distance of similar to 100 pc. Significant structure is revealed, but its precise form is dependent on the u - v plane sampling used for the image reconstruction. At a resolution of <= 30 au, we detected an inner gap in the disc with a radius of similar to 25 au and a position angle approximately along the known disc major axis. With different weighting, and an achieved resolution of similar to 15 au, emission appears at the centre and the disc takes on the shape of an incomplete ring, much like a horseshoe, again with a gap radius of similar to 25 au. The position angle of the disc major axis and its inclination from face-on are determined to be 140 degrees +/- 5 degrees and 40 degrees +/- 5 degrees, respectively. The similar to 25 au gap radius is confirmed by a null in the real part of the binned visibilities at 320 +/- 10 k lambda, whilst the non-axisymmetric nature is also confirmed through significant structure in the imaginary component. The emission mechanism at the central peak is most likely to be free-free emission from a stellar or disc wind. Overall our data support the picture of at least one, but probably several, giant planets orbiting HD100546 within 25 au. C1 [Wright, C. M.] UNSW ADFA, Sch Phys Environm & Math Sci, Canberra, ACT 2600, Australia. [Maddison, S. T.] Swinburne Univ, Ctr Astrophys & Supercomp, Hawthorn, Vic 3122, Australia. [Wilner, D. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Burton, M. G.] Univ New S Wales, Sch Phys, Sydney, NSW 2000, Australia. [Lommen, D.] Hwa Chong Inst, Singapore 269734, Singapore. [van Dishoeck, E. F.; Pinilla, P.; Walsh, C.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [Bourke, T. L.] Jodrell Bank Observ, SKA Org, Macclesfield SK11 9DL, Cheshire, England. [Menard, F.] Univ Chile, Millenium Nucl Protoplanetary Disks ALMA Early Sc, Santiago, Chile. RP Wright, CM (reprint author), UNSW ADFA, Sch Phys Environm & Math Sci, Canberra, ACT 2600, Australia. EM c.wright@adfa.edu.au; smaddison@swin.edu.au FU Australian Research Council (ARC) [DP0345227, FT100100495]; Swinburne Researcher Development Scheme; Swinburne Special Studies Program FX This research was supported by an Australian Research Council (ARC) Australian Research Fellowship awarded to CMW as part of Discovery Project DP0345227, and subsequently as an ARC Future Fellowship FT100100495. STM acknowledges support from the Swinburne Researcher Development Scheme and Swinburne Special Studies Program. We acknowledge the award of significant amounts of observing time for this project by the ATNF and NANTEN2 Time Assignment Committees. The assistance of Paul Jones and Balthasar Indermuhle in conducting the 2012 May and June 7 mm observations is greatly appreciated. We thank the ATNF staff at Narrabri for their hospitality, assistance and patience, especially Robin Wark, Bob Sault and Phil Edwards. We also thank Hiroaki Yamamoto for assistance during the period over which the NANTEN2 observations were performed, and providing 'first look' spectra. We acknowledge the contribution of Tony Wong, particularly his very user-friendly MIRIAD script for reducing ATCA data. We thank Sean Andrews for providing the IDL script to perform the visibility deprojections. Finally, we appreciate the patience of the referee in reviewing such a long paper. This research has made use of the EOD and the Exoplanet Data Explorer at exoplanets.org. This research has made use of the SIMBAD data base operated at CDS, Strasbourg, France. NR 273 TC 7 Z9 7 U1 2 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 OCT 11 PY 2015 VL 453 IS 1 BP 414 EP 438 DI 10.1093/mnras/stv1619 PG 25 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CY2CD UT WOS:000366215500035 ER PT J AU Chapman, SC Bertoldi, F Smail, I Steidel, CC Blain, AW Geach, JE Gurwell, M Ivison, RJ Petitpas, GR Reddy, N AF Chapman, S. C. Bertoldi, F. Smail, Ian Steidel, C. C. Blain, A. W. Geach, J. E. Gurwell, M. Ivison, R. J. Petitpas, G. R. Reddy, N. TI A millimetre-wave redshift search for the unlensed HyLIRG, HS1700.850.1 SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies: abundances; galaxies: high-redshift; submillimetre: galaxies ID STAR-FORMING GALAXIES; DEEP FIELD-SOUTH; FAR-INFRARED EMISSION; DARK-MATTER HALOS; LUMINOUS SUBMILLIMETER GALAXIES; BARYONIC STRUCTURE SURVEY; SURVEY ALMA RESOLVES; SCUBA SUPER-MAP; TO 2-3 GALAXIES; NUMBER COUNTS AB We report the redshift of an unlensed, highly obscured submillimetre galaxy (SMG), HS1700.850.1, the brightest SMG (S-850 mu m = 19.1 mJy) detected in the James Clerk Maxwell Telescope/Submillimetre Common-user Bolometer Array-2 (JCMT/SCUBA-2) Baryonic Structure Survey, based on the detection of its (CO)-C-12 line emission. Using the Institute Radio Astronomie Millimetrique Plateau de Bure Interferometer with 3.6 GHz band width, we serendipitously detect an emission line at 150.6 GHz. From a search over 14.5 GHz in the 3- and 2-mm atmospheric windows, we confirm the identification of this line as (CO)-C-12(5-4) at z = 2.816, meaning that it does not reside in the z similar to 2.30 proto-cluster in this field. Measurement of the 870 mu m source size (<0.85 arcsec) from the Sub-Millimetre Array (SMA) confirms a compact emission in a S-870 (mu m) = 14.5 mJy, L-IR similar to 10(13) L-circle dot component, suggesting an Eddington-limited starburst. We use the double-peaked (CO)-C-12 line profile measurements along with the SMA size constraints to study the gas dynamics of a HyLIRG, estimating the gas and dynamical masses of HS1700.850.1. While HS1700.850.1 is one of the most extreme galaxies known in the Universe, we find that it occupies a relative void in the Lyman-Break Galaxy distribution in this field. Comparison with other extreme objects at similar epochs (HyLIRG Quasars), and cosmological simulations, suggests such an anti-bias of bright SMGs could be relatively common, with the brightest SMGs rarely occupying the most overdense regions at z = 2-4. C1 [Chapman, S. C.] Dalhousie Univ, Dept Phys & Atmospher Sci, Halifax, NS B3H 4R2, Canada. [Bertoldi, F.] Univ Bonn, Argelander Inst Astron, D-53121 Bonn, Germany. [Smail, Ian] Univ Durham, Dept Phys, Ctr Extragalact Astron, Durham DH1 3LE, England. [Steidel, C. C.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA. [Blain, A. W.] Univ Leicester, Phys & Astron, Leicester LE1 7RH, Leics, England. [Geach, J. E.] Univ Hertfordshire, Sci & Technol Res Inst, Ctr Astrophys Res, Hatfield AL10 9AB, Herts, England. [Gurwell, M.; Petitpas, G. R.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Ivison, R. J.] Univ Edinburgh, Inst Astron, Royal Observ, Edinburgh EH9 3HJ, Midlothian, Scotland. [Ivison, R. J.] European So Observ, D-85748 Garching, Germany. [Reddy, N.] Univ Calif Riverside, Dept Phys & Astron, Riverside, CA 92521 USA. RP Chapman, SC (reprint author), Dalhousie Univ, Dept Phys & Atmospher Sci, Halifax, NS B3H 4R2, Canada. EM scott.chapman@dal.ca RI Smail, Ian/M-5161-2013; Ivison, R./G-4450-2011 OI Smail, Ian/0000-0003-3037-257X; Ivison, R./0000-0001-5118-1313 FU INSU/CNRS (France); MPG (Germany); IGN (Spain); Smithsonian Institution; Academia Sinica; NSERC; CFI; Collaborative Research Centre 956 - Deutsche Forschungsgemeinschaft (DFG). [A1]; STFC; Leverhulme Fellowship; ERC Advanced Investigator programme DUSTYGAL [321334]; Royal Society/Wolfson Merit Award; Royal Society FX We thank an anonymous referee for constructive comments on the manuscript. IRAM is supported by INSU/CNRS (France), MPG (Germany) and IGN (Spain). The submillimetre array (SMA) is a joint project between the Smithsonian Astrophysical Observatory and the Academia Sinica Institute of Astronomy and Astrophysics and is funded by the Smithsonian Institution and the Academia Sinica. We thank summer students K. Lacaille and R. Perry for their work on the KBSS-SCUBA2 survey project. SCC acknowledges NSERC and CFI for support. FB acknowledges support through the Collaborative Research Centre 956, sub-project A1, funded by the Deutsche Forschungsgemeinschaft (DFG). IRS acknowledges support from STFC, a Leverhulme Fellowship, the ERC Advanced Investigator programme DUSTYGAL 321334 and a Royal Society/Wolfson Merit Award. JEG acknowledges support from the Royal Society. NR 74 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 OCT 11 PY 2015 VL 453 IS 1 BP 951 EP 959 DI 10.1093/mnras/stv1618 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CY2CD UT WOS:000366215500074 ER PT J AU Kalari, VM Vink, JS Drew, JE Barentsen, G Drake, JJ Eisloffel, J Martin, EL Parker, QA Unruh, YC Walton, NA Wright, NJ AF Kalari, V. M. Vink, J. S. Drew, J. E. Barentsen, G. Drake, J. J. Eisloeffel, J. Martin, E. L. Parker, Q. A. Unruh, Y. C. Walton, N. A. Wright, N. J. TI Classical T Tauri stars with VPHAS plus - I. H alpha and u-band accretion rates in the Lagoon Nebula M8 SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE accretion, accretion discs; stars: pre-main-sequence; stars: variables: T Tauri, Herbig Ae/Be; open clusters and associations: individual: NGC 6530, Lagoon Nebula, M8 ID MAIN-SEQUENCE STARS; CLUSTER NGC 6530; PROTOPLANETARY DISK EVOLUTION; HUBBLE-SPACE-TELESCOPE; GALACTIC PLANE IPHAS; LOW MASS STARS; FORMING REGION; YOUNG STARS; PHOTOMETRIC-DETERMINATION; STELLAR POPULATIONS AB We estimate the accretion rates of 235 Classical T Tauri star (CTTS) candidates in the Lagoon Nebula using ugri H alpha photometry from the VST Photometric H alpha survey+. Our sample consists of stars displaying H alpha excess, the intensity of which is used to derive accretion rates. For a subset of 87 stars, the intensity of the u-band excess is also used to estimate accretion rates. We find the mean variation in accretion rates measured using H alpha and u-band intensities to be similar to 0.17 dex, agreeing with previous estimates (0.04-0.4 dex) but for a much larger sample. The spatial distribution of CTTS align with the location of protostars and molecular gas suggesting that they retain an imprint of the natal gas fragmentation process. Strong accretors are concentrated spatially, while weak accretors are more distributed. Our results do not support the sequential star-forming processes suggested in the literature. C1 [Kalari, V. M.; Vink, J. S.] Armagh Observ, Armagh BT61 9DG, North Ireland. [Kalari, V. M.] Queens Univ Belfast, Sch Math & Phys, Belfast BT61 7NN, Antrim, North Ireland. [Drew, J. E.; Barentsen, G.; Wright, N. J.] Univ Hertfordshire, Ctr Astron Res, Sci & Technol Res Inst, Hatfield AL10 9AB, Herts, England. [Drake, J. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Eisloeffel, J.] Thuringer Landessternwarte, D-07778 Tautenburg, Germany. [Martin, E. L.] Ctr Astrobiol, Dept Astrofis, E-28550 Madrid, Spain. [Parker, Q. A.] Univ Hong Kong, Dept Phys, Hong Kong, Hong Kong, Peoples R China. [Parker, Q. A.] Australian Astron Observ, N Ryde, NSW 1670, Australia. [Unruh, Y. C.] Univ London Imperial Coll Sci Technol & Med, Dept Phys, Blackett Lab, London SW7 2AZ, England. [Walton, N. A.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. RP Kalari, VM (reprint author), Armagh Observ, Coll Hill, Armagh BT61 9DG, North Ireland. EM vek@arm.ac.uk; jsv@arm.ac.uk FU European Southern Observatory Very Large Telescope in programme [177.D-3023(C)]; DCAL-NI; UK Science and Technology Facilities Council FX Based on observations collected at the European Southern Observatory Very Large Telescope in programme 177.D-3023(C). VMK and JSV acknowledge funding from DCAL-NI and the UK Science and Technology Facilities Council. VMK thanks the anonymous referee, and Drs R. Oudmaijer and G. Ramsay for providing helpful and constructive comments. NR 94 TC 2 Z9 2 U1 0 U2 2 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD OCT 11 PY 2015 VL 453 IS 1 BP 1026 EP 1046 DI 10.1093/mnras/stv1676 PG 21 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CY2CD UT WOS:000366215500079 ER PT J AU Bussmann, RS Riechers, D Fialkov, A Scudder, J Hayward, CC Cowley, WI Bock, J Calanog, J Chapman, SC Cooray, A De Bernardis, F Farrah, D Fu, H Gavazzi, R Hopwood, R Ivison, RJ Jarvis, M Lacey, C Loeb, A Oliver, SJ Perez-Fournon, I Rigopoulou, D Roseboom, IG Scott, D Smith, AJ Vieira, JD Wang, L Wardlow, J AF Bussmann, R. S. Riechers, D. Fialkov, A. Scudder, J. Hayward, C. C. Cowley, W. I. Bock, J. Calanog, J. Chapman, S. C. Cooray, A. De Bernardis, F. Farrah, D. Fu, Hai Gavazzi, R. Hopwood, R. Ivison, R. J. Jarvis, M. Lacey, C. Loeb, A. Oliver, S. J. Perez-Fournon, I. Rigopoulou, D. Roseboom, I. G. Scott, Douglas Smith, A. J. Vieira, J. D. Wang, L. Wardlow, J. TI HerMES: ALMA IMAGING OF HERSCHEL-SELECTED DUSTY STAR-FORMING GALAXIES SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: evolution; submillimeter: galaxies; techniques: interferometric ID DEEP FIELD SOUTH; HIGH-REDSHIFT GALAXIES; DIGITAL SKY SURVEY; DARK-MATTER HALOS; SUBMILLIMETER GALAXIES; MOLECULAR GAS; COSMOS FIELD; INTERACTING GALAXIES; EXTRAGALACTIC SURVEY; FORMATION HISTORY AB The Herschel Multi-tiered Extragalactic Survey (HerMES) has identified large numbers of dusty star-forming galaxies (DSFGs) over a wide range in redshift. A detailed understanding of these DSFGs is hampered by the limited spatial resolution of Herschel. We present 870 mu m 0 ''.45 resolution imaging obtained with the Atacama Large Millimeter/submillimeter Array (ALMA) of a sample of 29 HerMES DSFGs that have far-infrared (FIR) flux densities that lie between the brightest of sources found by Herschel and fainter DSFGs found via ground-based surveys in the submillimeter region. The ALMA imaging reveals that these DSFGs comprise a total of 62 sources (down to the 5 sigma point-source sensitivity limit in our ALMA sample; sigma approximate to 0.2 mJy). Optical or near-infrared imaging indicates that 36 of the ALMA sources experience a significant flux boost from gravitational lensing (mu > 1.1), but only six are strongly lensed and show multiple images. We introduce and make use of UVMCMCFIT, a general-purpose and publicly available Markov chain Monte Carlo visibility-plane analysis tool to analyze the source properties. Combined with our previous work on brighter Herschel sources, the lens models presented here tentatively favor intrinsic number counts for DSFGs with a break near 8 mJy at 880 mu m and a steep fall-off at higher flux densities. Nearly 70% of the Herschel sources break down into multiple ALMA counterparts, consistent with previous research indicating that the multiplicity rate is high in bright sources discovered in single-dish submillimeter or FIR surveys. The ALMA counterparts to our Herschel targets are located significantly closer to each other than ALMA counterparts to sources found in the LABOCA ECDFS Submillimeter Survey. Theoretical models underpredict the excess number of sources with small separations seen in our ALMA sample. The high multiplicity rate and small projected separations between sources seen in our sample argue in favor of interactions and mergers plausibly driving both the prodigious emission from the brightest DSFGs as well as the sharp downturn above S-880 = 8 mJy. C1 [Bussmann, R. S.; Riechers, D.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. [Fialkov, A.] CNRS, Ecole Normale Super, Dept Phys, F-75005 Paris, France. [Scudder, J.; Oliver, S. J.; Roseboom, I. G.; Smith, A. J.] Univ Sussex, Ctr Astron, Dept Phys & Astron, Brighton BN1 9QH, E Sussex, England. [Hayward, C. C.] CALTECH, TAPIR 350 17, Pasadena, CA 91125 USA. [Hayward, C. C.; Loeb, A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Cowley, W. I.; Lacey, C.; Wang, L.] Univ Durham, Dept Phys, Inst Computat Cosmol, Durham DH1 3LE, England. [Bock, J.] CALTECH, Pasadena, CA 91125 USA. [Bock, J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Calanog, J.; Cooray, A.; De Bernardis, F.] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA. [Chapman, S. C.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Farrah, D.] Virginia Tech, Dept Phys, Blacksburg, VA 24061 USA. [Fu, Hai] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA. [Gavazzi, R.] Univ Paris 06, CNRS, UMR 7095, Inst Astrophys Paris, F-75014 Paris, France. [Hopwood, R.] Univ London Imperial Coll Sci Technol & Med, Blackett Lab, Astrophys Grp, London SW7 2AZ, England. [Ivison, R. J.] Royal Observ, UK Astron Technol Ctr, Edinburgh EH9 3HJ, Midlothian, Scotland. [Ivison, R. J.; Roseboom, I. G.] Univ Edinburgh, Inst Astron, Royal Observ, Edinburgh EH9 3HJ, Midlothian, Scotland. [Jarvis, M.; Rigopoulou, D.] Univ Oxford, Dept Astrophys, Oxford OX1 3RH, England. [Jarvis, M.] Univ Western Cape, Astrophys Grp, Dept Phys, Cape Town, South Africa. [Perez-Fournon, I.] Inst Astrofis Canarias, E-38200 Tenerife, Spain. [Perez-Fournon, I.] Univ La Laguna, Dept Astrofis, E-38205 Tenerife, Spain. [Rigopoulou, D.] Rutherford Appleton Lab, RAL Space, Didcot OX11 0QX, Oxon, England. [Scott, Douglas] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada. [Vieira, J. D.] Univ Illinois, Dept Astron, Urbana, IL 61801 USA. [Vieira, J. D.] Univ Illinois, Dept Phys, Urbana, IL 61801 USA. [Wang, L.] SRON Netherlands Inst Space Res, NL-9747 AD Groningen, Netherlands. [Wardlow, J.] Univ Copenhagen, Niels Bohr Inst, Dark Cosmol Ctr, DK-2100 Copenhagen, Denmark. RP Bussmann, RS (reprint author), Cornell Univ, Dept Astron, Space Sci Bldg, Ithaca, NY 14853 USA. RI Ivison, R./G-4450-2011; Wardlow, Julie/C-9903-2015; OI Ivison, R./0000-0001-5118-1313; Wardlow, Julie/0000-0003-2376-8971; Scudder, Jillian/0000-0002-8798-3972; Scott, Douglas/0000-0002-6878-9840; Hayward, Christopher/0000-0003-4073-3236 FU Danish National Research Foundation; European Research Council Advanced Investigator Grant, Cosmicism [321302]; Gordon; Betty Moore Foundation FX The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. The Dark Cosmology Centre is funded by the Danish National Research Foundation. R. J. I. acknowledges support from European Research Council Advanced Investigator Grant, Cosmicism, 321302. C. C. H. is grateful to the Gordon and Betty Moore Foundation for financial support. NR 107 TC 14 Z9 14 U1 2 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 OCT 10 PY 2015 VL 812 IS 1 AR 43 DI 10.1088/0004-637X/812/1/43 PG 23 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CV4KC UT WOS:000364234700043 ER PT J AU Cranmer, SR Woolsey, LN AF Cranmer, Steven R. Woolsey, Lauren N. TI DRIVING SOLAR SPICULES AND JETS WITH MAGNETOHYDRODYNAMIC TURBULENCE: TESTING A PERSISTENT IDEA SO ASTROPHYSICAL JOURNAL LA English DT Article DE Sun: atmosphere; Sun: chromosphere; Sun: corona; turbulence; waves ID POLARIZED ALFVEN WAVES; REGION-IMAGING-SPECTROGRAPH; OPEN FLUX TUBES; NUMERICAL SIMULATIONS; PHOTOSPHERIC MOTIONS; DENSITY-FLUCTUATIONS; WIND ACCELERATION; CORONAL PLUMES; II SPICULES; CHROMOSPHERE AB The solar chromosphere contains thin, highly dynamic strands of plasma known as spicules. Recently, it has been suggested that the smallest and fastest (Type II) spicules are identical to intermittent jets observed by the Interface Region Imaging Spectrograph. These jets appear to expand out along open magnetic field lines rooted in unipolar network regions of coronal holes. In this paper we revisit a thirty-year-old idea that spicules may be caused by upward forces associated with Alfven waves. These forces involve the conversion of transverse Alfven waves into compressive acoustic-like waves that steepen into shocks. The repeated buffeting due to upward shock propagation causes nonthermal expansion of the chromosphere and a transient levitation of the transition region (TR). Some older models of wave-driven spicules assumed sinusoidal wave inputs, but the solar atmosphere is highly turbulent and stochastic. Thus, we model this process using the output of a time-dependent simulation of reduced magnetohydrodynamic turbulence. The resulting mode-converted compressive waves are strongly variable in time, with a higher TR occurring when the amplitudes are large and a lower TR when the amplitudes are small. In this picture, the TR bobs up and down by several Mm on timescales less than a minute. These motions produce narrow, intermittent extensions of the chromosphere that have similar properties as the observed jets and Type II spicules. C1 [Cranmer, Steven R.] Univ Colorado, Dept Astrophys & Planetary Sci, Lab Atmospher & Space Phys, Boulder, CO 80309 USA. [Woolsey, Lauren N.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Cranmer, SR (reprint author), Univ Colorado, Dept Astrophys & Planetary Sci, Lab Atmospher & Space Phys, Boulder, CO 80309 USA. FU NSF SHINE program [AGS-1540094]; NSF Graduate Research Fellowship [DGE-1144152]; start-up funds from the Department of Astrophysical and Planetary Sciences at the University of Colorado Boulder FX The authors gratefully acknowledge Adriaan van Ballegooijen for developing the BRAID code and for decades of valuable collaboration. We also thank Hui Tian, Sean McKillop, Rebecca Arbacher, and the IRIS team for their intrepid efforts to identify and characterize the faint, short-lived network jets. This work was supported by NSF SHINE program grant AGS-1540094, NSF Graduate Research Fellowship grant DGE-1144152, and start-up funds from the Department of Astrophysical and Planetary Sciences at the University of Colorado Boulder. NR 107 TC 10 Z9 10 U1 2 U2 10 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD OCT 10 PY 2015 VL 812 IS 1 AR 71 DI 10.1088/0004-637X/812/1/71 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CV4KC UT WOS:000364234700071 ER PT J AU Furniss, A Noda, K Boggs, S Chiang, J Christensen, F Craig, W Giommi, P Hailey, C Harisson, F Madejski, G Nalewajko, K Perri, M Stern, D Urry, M Verrecchia, F Zhang, W Ahnen, ML Ansoldi, S Antonelli, LA Antoranz, P Babic, A Banerjee, B Bangale, P de Almeida, UB Barrio, JA Gonzalez, JB Bednarek, W Bernardini, E Biasuzzi, B Biland, A Blanch, O Bonnefoy, S Bonnoli, G Borracci, F Bretz, T Carmona, E Carosi, A Chatterjee, A Clavero, R Colin, P Colombo, E Contreras, JL Cortina, J Covino, S Da Vela, P Dazzi, F De Angelis, A De Caneva, G De Lotto, B Wilhelmi, ED Mendez, CD Di Pierro, F Prester, DD Dorner, D Doro, M Einecke, S Glawion, DE Elsaesser, D Fernandez-Barral, A Fidalgo, D Fonseca, MV Font, L Frantzen, K Fruck, C Galindo, D Lopez, RJG Garczarczyk, M Terrats, DG Gaug, M Giammaria, P Godinovic, N Munoz, AG Guberman, D Hanabata, Y Hayashida, M Herrera, J Hose, J Hrupec, D Hughes, G Idec, W Kellermann, H Kodani, K Konno, Y Kubo, H Kushida, J La Barbera, A Lelas, D Lewandowska, N Lindfors, E Lombardi, S Longo, F Lopez, M Lopez-Coto, R Lopez-Oramas, A Lorenz, E Majumdar, P Makariev, M Mallot, K Maneva, G Manganaro, M Mannheim, K Maraschi, L Marcote, B Mariotti, M Martinez, M Mazin, D Menzel, U Miranda, JM Mirzoyan, R Moralejo, A Nakajima, D Neustroev, V Niedzwiecki, A Rosillo, MN Nilsson, K Nishijima, K Orito, R Overkemping, A Paiano, S Palacio, J Palatiello, M Paneque, D Paoletti, R Paredes, JM Paredes-Fortuny, X Persic, M Poutanen, J Moroni, PGP Prandini, E Puljak, I Reinthal, R Rhode, W Ribo, M Rico, J Garcia, JR Saito, T Saito, K Satalecka, K Scapin, V Schultz, C Schweizer, T Shore, SN Sillanpaa, A Sitarek, J Snidaric, I Sobczynska, D Stamerra, A Steinbring, T Strzys, M Takalo, L Takami, H Tavecchio, F Temnikov, P Terzic, T Tescaro, D Teshima, M Thaele, J Torres, DF Toyama, T Treves, A Verguilov, V Vovk, I Will, M Zanin, R Archer, A Benbow, W Bird, R Biteau, J Bugaev, V Cardenzana, JV Cerruti, M Chen, X Ciupik, L Connolly, MP Cui, W Dickinson, HJ Dumm, J Eisch, JD Falcone, A Feng, Q Finley, JP Fleischhack, H Fortin, P Fortson, L Gerard, L Gillanders, GH Griffin, S Griffiths, ST Grube, J Gyuk, G Hakansson, N Holder, J Humensky, TB Johnson, CA Kaaret, P Kertzman, M Kieda, D Krause, M Krennrich, F Lang, MJ Lin, TTY Maier, G McArthur, S McCann, A Meagher, K Moriarty, P Mukherjee, R Nieto, D de Bhroithe, AO Ong, RA Park, N Petry, D Pohl, M Popkow, A Ragan, K Ratliff, G Reyes, LC Reynolds, PT Richards, GT Roache, E Santander, M Sembroski, GH Shahinyan, K Staszak, D Telezhinsky, I Tucci, JV Tyler, J Vassiliev, VV Wakely, SP Weiner, OM Weinstein, A Wilhelm, A Williams, DA Zitzer, B Vince, O Fuhrmann, L Angelakis, E Karamanavis, V Myserlis, I Krichbaum, TP Zensus, JA Ungerechts, H Sievers, A Bachev, R Bottcher, M Chen, WP Damljanovic, G Eswaraiah, C Guver, T Hovatta, T Hughes, Z Ibryamov, SI Joner, MD Jordan, B Jorstad, SG Joshi, M Kataoka, J Kurtanidze, OM Kurtanidze, SO Lahteenmaki, A Latev, G Lin, HC Larionov, VM Mokrushina, AA Morozova, DA Nikolashvili, MG Raiteri, CM Ramakrishnan, V Readhead, ACR Sadun, AC Sigua, LA Semkov, EH Strigachev, A Tammi, J Tornikoski, M Troitskaya, YV Troitsky, IS Villata, M AF Furniss, A. Noda, K. Boggs, S. Chiang, J. Christensen, F. Craig, W. Giommi, P. Hailey, C. Harisson, F. Madejski, G. Nalewajko, K. Perri, M. Stern, D. Urry, M. Verrecchia, F. Zhang, W. Ahnen, M. L. Ansoldi, S. Antonelli, L. A. Antoranz, P. Babic, A. Banerjee, B. Bangale, P. de Almeida, U. Barres Barrio, J. A. Becerra Gonzalez, J. Bednarek, W. Bernardini, E. Biasuzzi, B. Biland, A. Blanch, O. Bonnefoy, S. Bonnoli, G. Borracci, F. Bretz, T. Carmona, E. Carosi, A. Chatterjee, A. Clavero, R. Colin, P. Colombo, E. Contreras, J. L. Cortina, J. Covino, S. Da Vela, P. Dazzi, F. De Angelis, A. De Caneva, G. De Lotto, B. de Ona Wilhelmi, E. Delgado Mendez, C. Di Pierro, F. Prester, D. Dominis Dorner, D. Doro, M. Einecke, S. Eisenacher Glawion, D. Elsaesser, D. Fernandez-Barral, A. Fidalgo, D. Fonseca, M. V. Font, L. Frantzen, K. Fruck, C. Galindo, D. Garcia Lopez, R. J. Garczarczyk, M. Garrido Terrats, D. Gaug, M. Giammaria, P. Godinovic, N. Gonzalez Munoz, A. Guberman, D. Hanabata, Y. Hayashida, M. Herrera, J. Hose, J. Hrupec, D. Hughes, G. Idec, W. Kellermann, H. Kodani, K. Konno, Y. Kubo, H. Kushida, J. La Barbera, A. Lelas, D. Lewandowska, N. Lindfors, E. Lombardi, S. Longo, F. Lopez, M. Lopez-Coto, R. Lopez-Oramas, A. Lorenz, E. Majumdar, P. Makariev, M. Mallot, K. Maneva, G. Manganaro, M. Mannheim, K. Maraschi, L. Marcote, B. Mariotti, M. Martinez, M. Mazin, D. Menzel, U. Miranda, J. M. Mirzoyan, R. Moralejo, A. Nakajima, D. Neustroev, V. Niedzwiecki, A. Nievas Rosillo, M. Nilsson, K. Nishijima, K. Orito, R. Overkemping, A. Paiano, S. Palacio, J. Palatiello, M. Paneque, D. Paoletti, R. Paredes, J. M. Paredes-Fortuny, X. Persic, M. Poutanen, J. Moroni, P. G. Prada Prandini, E. Puljak, I. Reinthal, R. Rhode, W. Ribo, M. Rico, J. Garcia, J. Rodriguez Saito, T. Saito, K. Satalecka, K. Scapin, V. Schultz, C. Schweizer, T. Shore, S. N. Sillanpaa, A. Sitarek, J. Snidaric, I. Sobczynska, D. Stamerra, A. Steinbring, T. Strzys, M. Takalo, L. Takami, H. Tavecchio, F. Temnikov, P. Terzic, T. Tescaro, D. Teshima, M. Thaele, J. Torres, D. F. Toyama, T. Treves, A. Verguilov, V. Vovk, I. Will, M. Zanin, R. Archer, A. Benbow, W. Bird, R. Biteau, J. Bugaev, V. Cardenzana, J. V. Cerruti, M. Chen, X. Ciupik, L. Connolly, M. P. Cui, W. Dickinson, H. J. Dumm, J. Eisch, J. D. Falcone, A. Feng, Q. Finley, J. P. Fleischhack, H. Fortin, P. Fortson, L. Gerard, L. Gillanders, G. H. Griffin, S. Griffiths, S. T. Grube, J. Gyuk, G. Hakansson, N. Holder, J. Humensky, T. B. Johnson, C. A. Kaaret, P. Kertzman, M. Kieda, D. Krause, M. Krennrich, F. Lang, M. J. Lin, T. T. Y. Maier, G. McArthur, S. McCann, A. Meagher, K. Moriarty, P. Mukherjee, R. Nieto, D. de Bhroithe, A. O'Faolain Ong, R. A. Park, N. Petry, D. Pohl, M. Popkow, A. Ragan, K. Ratliff, G. Reyes, L. C. Reynolds, P. T. Richards, G. T. Roache, E. Santander, M. Sembroski, G. H. Shahinyan, K. Staszak, D. Telezhinsky, I. Tucci, J. V. Tyler, J. Vassiliev, V. V. Wakely, S. P. Weiner, O. M. Weinstein, A. Wilhelm, A. Williams, D. A. Zitzer, B. Vince, O. Fuhrmann, L. Angelakis, E. Karamanavis, V. Myserlis, I. Krichbaum, T. P. Zensus, J. A. Ungerechts, H. Sievers, A. Bachev, R. Boettcher, M. Chen, W. P. Damljanovic, G. Eswaraiah, C. Guver, T. Hovatta, T. Hughes, Z. Ibryamov, S. I. Joner, M. D. Jordan, B. Jorstad, S. G. Joshi, M. Kataoka, J. Kurtanidze, O. M. Kurtanidze, S. O. Lahteenmaki, A. Latev, G. Lin, H. C. Larionov, V. M. Mokrushina, A. A. Morozova, D. A. Nikolashvili, M. G. Raiteri, C. M. Ramakrishnan, V. Readhead, A. C. R. Sadun, A. C. Sigua, L. A. Semkov, E. H. Strigachev, A. Tammi, J. Tornikoski, M. Troitskaya, Y. V. Troitsky, I. S. Villata, M. CA NuSTAR Team MAGIC Collaboration VERITAS Collaboration F-Gamma Consortium TI FIRST NuSTAR OBSERVATIONS OF MRK 501 WITHIN A RADIO TO TeV MULTI-INSTRUMENT CAMPAIGN SO ASTROPHYSICAL JOURNAL LA English DT Article DE BL Lacertae objects: general; galaxies: individual (Markarian 501); X-rays: galaxies ID GAMMA-RAY EMISSION; BL LACERTAE OBJECTS; LOG-PARABOLIC SPECTRA; LARGE-AREA TELESCOPE; X-RAY; MULTIWAVELENGTH OBSERVATIONS; PARTICLE-ACCELERATION; MAGIC TELESCOPE; CRAB-NEBULA; FERMI-LAT AB We report on simultaneous broadband observations of the TeV-emitting blazar Markarian 501 between 2013 April 1 and August 10, including the first detailed characterization of the synchrotron peak with Swift and NuSTAR. During the campaign, the nearby BL Lac object was observed in both a quiescent and an elevated state. The broadband campaign includes observations with NuSTAR, MAGIC, VERITAS, the Fermi Large Area Telescope, Swift X-ray Telescope and UV Optical Telescope, various ground-based optical instruments, including the GASP-WEBT program, as well as radio observations by OVRO, Metsahovi, and the F-Gamma consortium. Some of the MAGIC observations were affected by a sand layer from the Saharan desert, and had to be corrected using event-by-event corrections derived with a Light Detection and Ranging (LIDAR) facility. This is the first time that LIDAR information is used to produce a physics result with Cherenkov Telescope data taken during adverse atmospheric conditions, and hence sets a precedent for the current and future ground-based gamma-ray instruments. The NuSTAR instrument provides unprecedented sensitivity in hard X-rays, showing the source to display a spectral energy distribution (SED) between 3 and 79 keV consistent with a log-parabolic spectrum and hard X-ray variability on hour timescales. None (of the four extended NuSTAR observations) show evidence of the onset of inverse-Compton emission at hard X-ray energies. We apply a single-zone equilibrium synchrotron self-Compton (SSC) model to five simultaneous broadband SEDs. We find that the SSC model can reproduce the observed broadband states through a decrease in the magnetic field strength coinciding with an increase in the luminosity and hardness of the relativistic leptons responsible for the high-energy emission. C1 [Furniss, A.] Stanford Univ, Dept Phys, Stanford, CA 94305 USA. [Noda, K.; Bangale, P.; de Almeida, U. Barres; Borracci, F.; Colin, P.; Dazzi, F.; Fruck, C.; Hose, J.; Kellermann, H.; Lorenz, E.; Mazin, D.; Menzel, U.; Mirzoyan, R.; Paneque, D.; Garcia, J. 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G.; Joshi, M.] Dublin Inst Adv Studies, Sch Cosm Phys, Dublin, Ireland. [Jorstad, S. G.] Boston Univ, Inst Astrophys Res, Boston, MA 02215 USA. [Kataoka, J.; Larionov, V. M.; Mokrushina, A. A.; Morozova, D. A.; Troitskaya, Y. V.; Troitsky, I. S.] St Petersburg State Univ, Astron Inst, St Petersburg 198504, Russia. [Kurtanidze, O. M.; Kurtanidze, S. O.; Nikolashvili, M. G.; Sigua, L. A.] Waseda Univ, Res Inst Sci & Engn, Shinjuku Ku, Tokyo 1698555, Japan. [Kurtanidze, O. M.] Abastumani Observ, GE-0301 Mt Kanobili, Abastumani, Rep of Georgia. [Lahteenmaki, A.; Ramakrishnan, V.; Tammi, J.; Tornikoski, M.] Kazan Fed Univ, Engelhardt Astron Observ, Tatarstan, Russia. [Lahteenmaki, A.] Aalto Univ, Dept Radio Sci & Engn, FI-00076 Aalto, Finland. [Latev, G.] BAS, Inst Astron NAO, BG-1784 Sofia, Bulgaria. [Larionov, V. M.; Mokrushina, A. A.] Pulkovo Observ, St Petersburg, Russia. [Larionov, V. M.] Isaac Newton Inst Chile, St Petersburg Branch, Santiago, Chile. [Raiteri, C. M.; Villata, M.] Osserv Astron Torino, INAF, I-10025 Pino Torinese, TO, Italy. [Sadun, A. C.] Univ Colorado, Dept Phys, Denver, CO 80202 USA. RP Furniss, A (reprint author), Stanford Univ, Dept Phys, Stanford, CA 94305 USA. EM amy.@gmail.com; nodak5@gmail.com; josefa.becerra@nasa.gov RI Lahteenmaki, Anne/L-5987-2013; GAug, Markus/L-2340-2014; Nieto, Daniel/J-7250-2015; Manganaro, Marina/B-7657-2011; Boggs, Steven/E-4170-2015; Miranda, Jose Miguel/F-2913-2013; Tammi, Joni/G-2959-2012; Font, Lluis/L-4197-2014; Poutanen, Juri/H-6651-2016; Nievas Rosillo, Mireia/K-9738-2014; Contreras Gonzalez, Jose Luis/K-7255-2014; Lopez Moya, Marcos/L-2304-2014; Temnikov, Petar/L-6999-2016; Maneva, Galina/L-7120-2016; Makariev, Martin/M-2122-2016; Morozova, Daria/H-1298-2013; Torres, Diego/O-9422-2016; Troitskiy, Ivan/K-7979-2013; Delgado, Carlos/K-7587-2014; Barrio, Juan/L-3227-2014; Martinez Rodriguez, Manel/C-2539-2017; Cortina, Juan/C-2783-2017; Ramakrishnan, Venkatessh/C-8628-2017; OI GAug, Markus/0000-0001-8442-7877; Nieto, Daniel/0000-0003-3343-0755; Manganaro, Marina/0000-0003-1530-3031; Boggs, Steven/0000-0001-9567-4224; Miranda, Jose Miguel/0000-0002-1472-9690; Tammi, Joni/0000-0002-9164-2695; Font, Lluis/0000-0003-2109-5961; Poutanen, Juri/0000-0002-0983-0049; Nievas Rosillo, Mireia/0000-0002-8321-9168; Contreras Gonzalez, Jose Luis/0000-0001-7282-2394; Lopez Moya, Marcos/0000-0002-8791-7908; Temnikov, Petar/0000-0002-9559-3384; Morozova, Daria/0000-0002-9407-7804; Torres, Diego/0000-0002-1522-9065; Troitskiy, Ivan/0000-0002-4218-0148; Delgado, Carlos/0000-0002-7014-4101; Barrio, Juan/0000-0002-0965-0259; Cortina, Juan/0000-0003-4576-0452; Ramakrishnan, Venkatessh/0000-0002-9248-086X; LA BARBERA, ANTONINO/0000-0002-5880-8913; Verrecchia, Francesco/0000-0003-3455-5082; Prada Moroni, Pier Giorgio/0000-0001-9712-9916; Villata, Massimo/0000-0003-1743-6946; Stamerra, Antonio/0000-0002-9430-5264; Antonelli, Lucio Angelo/0000-0002-5037-9034; Perri, Matteo/0000-0003-3613-4409; Di Pierro, Federico/0000-0003-4861-432X; Guver, Tolga/0000-0002-3531-9842; Raiteri, Claudia Maria/0000-0003-1784-2784; Krause, Maria/0000-0001-7595-0914; Larionov, Valeri/0000-0002-4640-4356; Bird, Ralph/0000-0002-4596-8563; Karamanavis, Vassilis/0000-0003-3133-2617; Angelakis, Emmanouil/0000-0001-7327-5441; Doro, Michele/0000-0001-9104-3214; Covino, Stefano/0000-0001-9078-5507; de Ona Wilhelmi, Emma/0000-0002-5401-0744; Bonnoli, Giacomo/0000-0003-2464-9077; Prandini, Elisa/0000-0003-4502-9053; Becerra Gonzalez, Josefa/0000-0002-6729-9022 FU NASA [NNG08FD60C, NNX08AW31G, NNX11A043G]; National Aeronautics and Space Administration; German BMBF; German MPG; Italian INFN; Italian INAF; Swiss National Fund SNF; ERDF under the Spanish MINECO; Japanese JSPS; Japanese MEXT; Centro de Excelencia Severo Ochoa project of the Spanish Consolider-Ingenio programme [SEV-2012-0234]; Academy of Finland [268740]; Croatian Science Foundation (HrZZ) Project [09/176]; University of Rijeka Project [13.12.1.3.02]; DFG Collaborative Research Centers [SFB823/C4, SFB876/C3]; Polish MNiSzW grant [745/N-HESS-MAGIC/2010/0]; 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; INSU/CNRS (France); MPG (Germany); IGN (Spain); International Max Planck Research School (IMPRS) for Astronomy and Astrophysics at the University of Bonn; NSF [AST-0808050, AST-1109911]; Istanbul University [49429, 48285]; Bilim Akademisi (BAGEP program); TUBITAK [13AT100-431, 13AT100-466, 13AT60-430]; Russian RFBR grant [15-02-00949]; St. Petersburg University research grant [6.38.335.2015]; NASA Fermi Guest Investigator grant [NNX14AQ58G]; Swift Guest Investigator grant [NNX14AI96G]; BU; Lowell Observatory; Scientific Research Fund of the Bulgarian Ministry of Education and Sciences [DO 02-137 (BIn-13/09)]; Shota Rustaveli National Science Foundation [FR/577/6-320/13]; Institute of Astronomy; Rozhen National Astronomical Observatory, Bulgarian Academy of Sciences; Ministry of Education, Science and Technological Development of the Republic of Serbia [176011, 176004, 176021]; CPAN project of the Spanish Consolider-Ingenio programme [CSD2007-00042]; MultiDark project of the Spanish Consolider-Ingenio programme [CSD2009-00064]; International Max Planck Research School (IMPRS) for Astronomy and Astrophysics at the University of Cologne FX 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).; The MAGIC Collaboration would like to thank the Instituto de Astrofisica de Canarias for the excellent working conditions at the Observatorio del Roque de los Muchachos in La Palma. The financial support of the German BMBF and MPG, the Italian INFN and INAF, the Swiss National Fund SNF, the ERDF under the Spanish MINECO, and the Japanese JSPS and MEXT is gratefully acknowledged. This work was also supported by the Centro de Excelencia Severo Ochoa SEV-2012-0234, CPAN CSD2007-00042, and MultiDark CSD2009-00064 projects of the Spanish Consolider-Ingenio 2010 programme, by grant 268740 of the Academy of Finland, by the Croatian Science Foundation (HrZZ) Project 09/176 and the University of Rijeka Project 13.12.1.3.02, by the DFG Collaborative Research Centers SFB823/C4 and SFB876/C3, and by the Polish MNiSzW grant 745/N-HESS-MAGIC/2010/0.; This research is also 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 VERITAS 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.; This research is partly based on observations with the 100-m telescope of the MPIfR (Max-Planck-Institut fur Radioastronomie) at Effelsberg and with the IRAM 30-m telescope. IRAM is supported by INSU/CNRS (France), MPG (Germany) and IGN (Spain). V. Karamanavis and I. Myserlis are funded by the International Max Planck Research School (IMPRS) for Astronomy and Astrophysics at the Universities of Bonn and Cologne.; The OVRO 40-m monitoring program is supported in part by NASA grants NNX08AW31G and NNX11A043G, and NSF grants AST-0808050 and AST-1109911.; T. G. acknowledges support from Istanbul University (Project numbers 49429 and 48285), Bilim Akademisi (BAGEP program) and TUBITAK (project numbers 13AT100-431, 13AT100-466, and 13AT60-430).; St. Petersburg University team acknowledges support from Russian RFBR grant 15-02-00949 and St. Petersburg University research grant 6.38.335.2015.; The research at Boston University (BU) was funded in part by NASA Fermi Guest Investigator grant NNX14AQ58G and Swift Guest Investigator grant NNX14AI96G. The PRISM camera at Lowell Observatory was developed by K. Janes et al. at BU and Lowell Observatory, with funding from the NSF, BU, and Lowell Observatory.; This research was partially supported by Scientific Research Fund of the Bulgarian Ministry of Education and Sciences under grant DO 02-137 (BIn-13/09). The Skinakas Observatory is a collaborative project of the University of Crete, the Foundation for Research and Technology-Hellas, and the Max-Planck-Institut fur Extraterrestrische Physik.; The Abastumani Observatory team acknowledges financial support by the by Shota Rustaveli National Science Foundation under contract FR/577/6-320/13.; G. Damljanovic and O. Vince gratefully acknowledge the observing grant support from the Institute of Astronomy and Rozhen National Astronomical Observatory, Bulgarian Academy of Sciences. This work is in accordance with the Projects No 176011 ("Dynamics and kinematics of celestial bodies and systems"), No 176004 ("Stellar physics") and No 176021 ("Visible and invisible matter in nearby galaxies: theory and observations") supported by the Ministry of Education, Science and Technological Development of the Republic of Serbia. NR 98 TC 7 Z9 7 U1 4 U2 27 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD OCT 10 PY 2015 VL 812 IS 1 AR 65 DI 10.1088/0004-637X/812/1/65 PG 22 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CV4KC UT WOS:000364234700065 ER PT J AU Goicoechea, JR Teyssier, D Etxaluze, M Goldsmith, PF Ossenkopf, V Gerin, M Bergin, EA Black, JH Cernicharo, J Cuadrado, S Encrenaz, P Falgarone, E Fuente, A Hacar, A Lis, DC Marcelino, N Melnick, GJ Muller, HSP Persson, C Pety, J Rollig, M Schilke, P Simon, R Snell, RL Stutzki, J AF Goicoechea, Javier R. Teyssier, D. Etxaluze, M. Goldsmith, P. F. Ossenkopf, V. Gerin, M. Bergin, E. A. Black, J. H. Cernicharo, J. Cuadrado, S. Encrenaz, P. Falgarone, E. Fuente, A. Hacar, A. Lis, D. C. Marcelino, N. Melnick, G. J. Mueller, H. S. P. Persson, C. Pety, J. Roellig, M. Schilke, P. Simon, R. Snell, R. L. Stutzki, J. TI VELOCITY-RESOLVED [CII] EMISSION AND [CII]/FIR MAPPING ALONG ORION WITH HERSCHEL SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: ISM; HII regions; infrared: galaxies; ISM: clouds ID C-II EMISSION; DIFFUSE INTERSTELLAR-MEDIUM; NONEQUILIBRIUM PHOTODISSOCIATION REGIONS; POLYCYCLIC AROMATIC-HYDROCARBONS; ULTRALUMINOUS INFRARED GALAXIES; SPACE-OBSERVATORY MEASUREMENTS; EXTREME L-FIR/M-H2 RATIOS; LASER MAGNETIC-RESONANCE; PHOTON-DOMINATED REGIONS; STAR-FORMATION RATES AB We present the first similar to 7'.5 x 11'.5 velocity-resolved (similar to 0.2 km s(-1)) map of the [C II] 158 mu m line toward the Orion molecular cloud 1 (OMC 1) taken with the Herschel/HIFI instrument. In combination with far-IR (FIR) photometric images and velocity-resolved maps of the H41 alpha hydrogen recombination and CO J = 2-1 lines, this data set provides an unprecedented view of the intricate small-scale kinematics of the ionized/photodissociation region (PDR)/molecular gas interfaces and of the radiative feedback from massive stars. The main contribution to the [C II] luminosity (similar to 85%) is from the extended, FUV-illuminated face of the cloud (G(0) > 500, n(H) > 5 x 10(3) cm(-3)) and from dense PDRs (G(0) greater than or similar to 10(4), n(H) greater than or similar to 10(5) cm(-3)) at the interface between OMC 1 and the H II region surrounding the Trapezium cluster. Around similar to 15% of the [C II] emission arises from a different gas component without a CO counterpart. The [C II] excitation, PDR gas turbulence, line opacity (from [C-13 II]), and role of the geometry of the illuminating stars with respect to the cloud are investigated. We construct maps of the L[C II]/L-FIR and L-FIR/M-Gas ratios and show that L[C II]/L-FIR decreases from the extended cloud component (similar to 10(-2)-10(-3)) to the more opaque star-forming cores (similar to 10(-3)-10(-4)). The lowest values are reminiscent of the "[C II] deficit" seen in local ultraluminous IR galaxies hosting vigorous star formation. Spatial correlation analysis shows that the decreasing L[C II]/L-FIR ratio correlates better with the column density of dust through the molecular cloud than with L-FIR/M-Gas. We conclude that the [C II]-emitting column relative to the total dust column along each line of sight is responsible for the observed L[C II]/L-FIR variations through the cloud. C1 [Goicoechea, Javier R.; Etxaluze, M.; Cernicharo, J.; Cuadrado, S.] CSIC, Inst Ciencia Mat Madrid, E-28049 Madrid, Spain. [Teyssier, D.] ESA ESAC, Herschel Sci Ctr, E-28691 Madrid, Spain. [Etxaluze, M.] Rutherford Appleton Lab, RAL Space, Didcot OX11 0QX, Oxon, England. [Goldsmith, P. F.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Ossenkopf, V.; Mueller, H. S. P.; Roellig, M.; Schilke, P.; Simon, R.; Stutzki, J.] Univ Cologne, Inst Phys 1, D-50937 Cologne, Germany. [Gerin, M.; Encrenaz, P.; Falgarone, E.; Lis, D. C.] Univ Paris 06, Sorbonne Univ, CNRS, LERMA,Observ Paris,PSL Res Univ, F-75014 Paris, France. [Gerin, M.; Falgarone, E.] Ecole Normale Super, F-75005 Paris, France. [Bergin, E. A.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Black, J. H.; Persson, C.] Chalmers, Onsala Space Observ, Dept Earth & Space Sci, SE-43992 Onsala, Sweden. [Fuente, A.] Observ Astron Nacl OAN IGN, E-28803 Alcala De Henares, Spain. [Hacar, A.] Univ Vienna, Inst Astrophys, A-1180 Vienna, Austria. [Marcelino, N.] INAF, Ist Radioastron, I-40129 Bologna, Italy. [Melnick, G. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Pety, J.] Inst Radioastron Millimetr, F-38406 St Martin Dheres, France. [Snell, R. L.] Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA. RP Goicoechea, JR (reprint author), CSIC, Inst Ciencia Mat Madrid, Calle Sor Juana Ines Cruz 3, E-28049 Madrid, Spain. EM jr.goicoechea@icmm.csic.es RI Fuente, Asuncion/G-1468-2016; Goldsmith, Paul/H-3159-2016; OI Fuente, Asuncion/0000-0001-6317-6343; Hacar, Alvaro/0000-0001-5397-6961; Cernicharo, Jose/0000-0002-3518-2524 FU Spanish MINECO [CSD2009-00038, AYA2009-07304, AYA2012-32032]; ERC [ERC-2013-Syg-610256-NANOCOSMOS]; NASA; German Deutsche Forschungsgemeinschaft, DFG [SFB 956]; CNRS program "Physique et Chimie du Milieu Interstellaire (PCMI)" FX We acknowledge helpful comments and suggestions from our referee. We thank Spanish MINECO for funding support under grants CSD2009-00038, AYA2009-07304, and AYA2012-32032. We also thank the ERC for support under grant ERC-2013-Syg-610256-NANOCOSMOS. Part of this research was carried out at the Jet Propulsion Laboratory (JPL), California Institute of Technology (Caltech), under a contract with the National Aeronautics and Space Administration (NASA). Support for this work was provided by NASA through an award issued by JPL/Caltech. This work was supported by the German Deutsche Forschungsgemeinschaft, DFG project number SFB 956, C1. This work was in part also supported by theCNRS program "Physique et Chimie du Milieu Interstellaire (PCMI)." NR 127 TC 12 Z9 12 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 OCT 10 PY 2015 VL 812 IS 1 AR 75 DI 10.1088/0004-637X/812/1/75 PG 21 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CV4KC UT WOS:000364234700075 ER PT J AU Ma, JZ Gonzalez, AH Spilker, JS Strandet, M Ashby, MLN Aravena, M Bethermin, M Bothwell, MS de Breuck, C Brodwin, M Chapman, SC Fassnacht, CD Greve, TR Gullberg, B Hezaveh, Y Malkan, M Marrone, DP Saliwanchik, BR Vieira, JD Weiss, A Welikala, N AF Ma, Jingzhe Gonzalez, Anthony. H. Spilker, J. S. Strandet, M. Ashby, M. L. N. Aravena, M. Bethermin, M. Bothwell, M. S. de Breuck, C. Brodwin, M. Chapman, S. C. Fassnacht, C. D. Greve, T. R. Gullberg, B. Hezaveh, Y. Malkan, M. Marrone, D. P. Saliwanchik, B. R. Vieira, J. D. Weiss, A. Welikala, N. TI STELLAR MASSES AND STAR FORMATION RATES OF LENSED, DUSTY, STAR-FORMING GALAXIES FROM THE SPT SURVEY SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: high-redshift ID LYMAN BREAK GALAXIES; SOUTH-POLE TELESCOPE; FREE-FREE EMISSION; SUBMILLIMETER GALAXIES; REDSHIFT DISTRIBUTION; POPULATION SYNTHESIS; FORMATION HISTORIES; MASSIVE GALAXIES; DISTANT GALAXIES; EVOLUTION AB To understand cosmic mass assembly in the universe at early epochs, we primarily rely on measurements of the stellar masses and star formation rates (SFRs) of distant galaxies. In this paper, we present stellar masses and SFRs of six high-redshift (2.8 <= z <= 5.7) dusty, star-forming galaxies (DSFGs) that are strongly gravitationally lensed by foreground galaxies. These sources were first discovered by the South Pole Telescope (SPT) at millimeter wavelengths and all have spectroscopic redshifts and robust lens models derived from Atacama Large Millimeter/submillimeter Array observations. We have conducted follow-up observations to obtain multi-wavelength imaging data using the Hubble Space Telescope (HST), Spitzer, Herschel, and the Atacama Pathfinder EXperiment. We use the high-resolution HST/Wide Field Camera 3 images to disentangle the background source from the foreground lens in Spitzer/IRAC data. The detections and upper limits provide important constraints on the spectral energy distributions (SEDs) for these DSFGs, yielding stellar masses, IR luminosities, and SFRs. The SED fits of six SPT sources show that the intrinsic stellar masses span a range more than one order of magnitude with a median value similar to 5 x10(10) M-circle dot. The intrinsic IR luminosities range from 4 x 10(12) L-circle dot to 4 x 10(13) L-circle dot. They all have prodigious intrinsic SFRs of 510-4800 M-circle dot yr(-1). Compared to the star-forming main sequence (MS), these six DSFGs have specific SFRs that all lie above the MS, including two galaxies that are a factor of 10 higher than the MS. Our results suggest that we are witnessing ongoing strong starburst events that may be driven by major mergers. C1 [Ma, Jingzhe; Gonzalez, Anthony. H.] Univ Florida, Dept Astron, Gainesville, FL 32611 USA. [Spilker, J. S.; Marrone, D. P.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Strandet, M.; Weiss, A.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Ashby, M. L. N.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Aravena, M.] Univ Diego Portales, Fac Ingn, Nucleo Astron, Santiago, Chile. [Bethermin, M.; de Breuck, C.; Gullberg, B.] European So Observ, D-85748 Garching, Germany. [Bothwell, M. S.] Univ Cambridge, Cavendish Lab, Cambridge CB3 0HA, England. [Brodwin, M.] Univ Missouri, Dept Phys & Astron, Kansas City, MO 64110 USA. [Chapman, S. C.] Dalhousie Univ, Halifax, NS, Canada. [Fassnacht, C. D.] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA. [Greve, T. R.] UCL, Dept Phys & Astron, London WC1E 6BT, England. [Hezaveh, Y.] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94305 USA. [Malkan, M.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. [Saliwanchik, B. R.] Case Western Reserve Univ, Dept Phys, Cleveland, OH 44106 USA. [Vieira, J. D.] Univ Illinois, Dept Astron, Urbana, IL 61801 USA. [Vieira, J. D.] Univ Illinois, Dept Phys, Urbana, IL 61801 USA. [Welikala, N.] Univ Oxford, Dept Phys, Oxford OX1 3RH, England. RP Ma, JZ (reprint author), Univ Florida, Dept Astron, Gainesville, FL 32611 USA. EM jingzhema@ufl.edu OI De Breuck, Carlos/0000-0002-6637-3315; Bethermin, Matthieu/0000-0002-3915-2015 FU NASA [NAS 5-26555]; NASA through Space Telescope Science Institute [12659, 13614]; NASA through JPL/Caltech; U.S. National Science Foundation [AST-1312950]; NRAO [SOSPA1-006]; FONDECYT [1140099]; National Science Foundation [ANT-0638937]; Kavli Foundation; Gordon and Betty Moore Foundation; [PHY-1125897] FX We thank the anonymous referee for useful comments. We thank Sebastien Heinis for sharing the data in Heinis et al. (2014). This work is based on observations made with the NASA/ESA Hubble Space Telescope obtained at the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-26555. These observations are associated with programs #12659 and #13614. Support for programs #12659 and # 13614 was provided by NASA through a grant from the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-26555. This work is based in part on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. Support for this work was provided by NASA through an award issued by JPL/Caltech. Partial support for this work was provided by NASA from awards for Herschel observations for OT1_dmarrone_1, OT1_jvieira_4, and OT2_jvieira_5. Herschel is an ESA space observatory with science instruments provided by European-led Principal Investigator consortia and with important participation from NASA. J.S.S., D.P.M., and J.D.V. acknowledge support from the U.S. National Science Foundation under grant No. AST-1312950 and through award SOSPA1-006 from the NRAO. M.A. acknowledges partial support from FONDECYT through grant 1140099. This paper makes use of the following ALMA data: ADS/JAO.ALMA #2011.0.00957. S and #2011.0.00958. S. ALMA is a partnership of ESO (representing its member states), NSF (USA), and NINS (Japan), together with NRC (Canada) and NSC and ASIAA (Taiwan), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by ESO, AUI/NRAO, and NAOJ. The SPT is supported by the National Science Foundation through grant ANT-0638937, with partial support through PHY-1125897, the Kavli Foundation, and the Gordon and Betty Moore Foundation. This research has made use of NASA's Astrophysics Data System. NR 78 TC 3 Z9 3 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 OCT 10 PY 2015 VL 812 IS 1 AR 88 DI 10.1088/0004-637X/812/1/88 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CV4KC UT WOS:000364234700088 ER PT J AU Madsen, KK Furst, F Walton, DJ Harrison, FA Nalewajko, K Ballantyne, DR Boggs, SE Brenneman, LW Christensen, FE Craig, WW Fabian, AC Forster, K Grefenstette, BW Guainazzi, M Hailey, CJ Madejski, GM Matt, G Stern, D Walter, R Zhang, WW AF Madsen, Kristin K. Fuerst, Felix Walton, Dominic J. Harrison, Fiona A. Nalewajko, Krzysztof Ballantyne, David R. Boggs, Steve E. Brenneman, Laura W. Christensen, Finn E. Craig, William W. Fabian, Andrew C. Forster, Karl Grefenstette, Brian W. Guainazzi, Matteo Hailey, Charles J. Madejski, Greg M. Matt, Giorgio Stern, Daniel Walter, Roland Zhang, William W. TI 3C 273 WITH NuSTAR: UNVEILING THE ACTIVE GALACTIC NUCLEUS SO ASTROPHYSICAL JOURNAL LA English DT Article DE quasars: individual (3C 273); X-rays: individual (3C 273) ID X-RAY-SPECTRUM; LINE RADIO GALAXIES; XMM-NEWTON OBSERVATIONS; CORONAL PROPERTIES; RAPID VARIABILITY; GAMMA-RAYS; JET; 3C-273; EMISSION; TELESCOPE AB We present results from a 244 ks NuSTAR observation of 3C 273 obtained during a cross-calibration campaign with the Chandra, INTEGRAL, Suzaku, Swift, and XMM-Newton observatories. We show that the spectrum, when fit with a power-law model using data from all observatories except INTEGRAL over the 1-78 keV band, leaves significant residuals in the NuSTAR data between 30 and 78 keV. The NuSTAR 3-78 keV spectrum is well. described by an exponentially cutoff power law (Gamma = 1.646 +/- 0.006, E-cutoff = 202(-34)(+51) keV) with a weak reflection component from cold, dense material. There is also evidence for a weak (EW = 23 +/- 11 eV) neutral iron line. We interpret these features as arising from coronal emission plus reflection off an accretion disk or distant material. Beyond 80 keV INTEGRAL data show clear excess flux relative to an extrapolation of the active galactic nucleus model fit to NuSTAR. This high-energy power. law is consistent with the presence of a beamed jet, which begins to dominate over emission from the inner accretion flow at 30-40 keV. Modeling the jet locally (in the NuSTAR + INTEGRAL band) as a power. law, we find that the coronal component is fit by Gamma(AGN) = 1.638 +/- 0.045, E-cutoff = 47 +/- 15 keV, and jet photon index by Gamma(jet) = 1.05 +/- 0.4. We also consider Fermi/LAT observations of 3C 273, and here the broadband spectrum of the jet can be described by a log-parabolic model, peaking at similar to 2 MeV. Finally, we investigate the spectral variability in the NuSTAR band and find an inverse correlation between flux and Gamma. C1 [Madsen, Kristin K.; Fuerst, Felix; Walton, Dominic J.; Harrison, Fiona A.; Forster, Karl; Grefenstette, Brian W.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA. [Walton, Dominic J.; Stern, Daniel] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Nalewajko, Krzysztof; Madejski, Greg M.] SLAC Natl Accelerator Lab, Kavli Inst Particle Astrophys & Cosmol, Menlo Pk, CA 94025 USA. [Ballantyne, David R.] Georgia Inst Technol, Sch Phys, Ctr Relativist Astrophys, Atlanta, GA 30332 USA. [Boggs, Steve E.; Craig, William W.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Brenneman, Laura W.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Christensen, Finn E.] Tech Univ Denmark, Natl Space Inst, DTU Space, DK-2800 Lyngby, Denmark. [Fabian, Andrew C.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Guainazzi, Matteo] European Space Astron Ctr ESA, E-28691 Madrid, Spain. [Hailey, Charles J.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA. [Matt, Giorgio] Univ Roma Tre, Dipartimento Matemat & Fis, I-00146 Rome, Italy. [Walter, Roland] Univ Geneva, Observ Geneva, CH-1290 Versoix, Switzerland. [Zhang, William W.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Madsen, KK (reprint author), CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA. RI Boggs, Steven/E-4170-2015; OI Boggs, Steven/0000-0001-9567-4224; Madsen, Kristin/0000-0003-1252-4891; Ballantyne, David/0000-0001-8128-6976 FU NASA [NNG08FD60C]; National Aeronautics and Space Administration FX We thank Chris Done for bringing to our attention the alternative interpretation of the jet as a two-component inverse Compton model, and the anonymous referee, whose remarks and corrections helped improve the quality of this paper. 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 53 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 OCT 10 PY 2015 VL 812 IS 1 AR 14 DI 10.1088/0004-637X/812/1/14 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CV4KC UT WOS:000364234700014 ER PT J AU Pan, LB Padoan, P AF Pan, Liubin Padoan, Paolo TI TURBULENCE-INDUCED RELATIVE VELOCITY OF DUST PARTICLES V. TESTING PREVIOUS MODELS SO ASTROPHYSICAL JOURNAL LA English DT Article DE minor planets, asteroids: general; planets and satellites: formation; protoplanetary disks; turbulence ID CHONDRULE-SIZED PARTICLES; ISOTROPIC TURBULENCE; PREFERENTIAL CONCENTRATION; PROTOPLANETARY NEBULA; INERTIAL PARTICLES; SOLAR NEBULA; COLLISION; GROWTH; GRAINS; PLANETESIMALS AB Coagulation models for dust growth in protoplanetary disks usually adopt the prediction of Volk et al. or its later developments (hereafter Volk-type models) for the collision velocity of dust particles induced by turbulent motions. We review the formulation and the underlying physical picture of these models, test their predictions against a numerical simulation, and examine the accuracy of the commonly used prescription for dust particle collisions. We show that Volk-type models typically overestimate the rms of the particle relative velocity by a factor of two, if the particle friction times lie in the inertial range of the flow. The commonly used prescription for the collision kernel has several inaccuracies, and, in particular, it neglects the effect of turbulent clustering. Interestingly, for particles of equal sizes, the inaccuracies happen to cancel out, and by coincidence, the commonly used kernel prescription based on Volk-type models is in good agreement with our simulation result. For particles of different sizes, the prescription shows a larger discrepancy from the measured kernel, and may overestimate the collision rate by up to a factor of 2.5. We find that the predicted rms relative velocity by Volk-type models provides reasonable estimates for the average collision velocity per collision. We also make an effort to improve the accuracy of Volk-type models for the rms relative velocity by tuning the correlation time of turbulent eddies and modifying the criterion for eddy classification. C1 [Pan, Liubin] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Padoan, Paolo] Univ Barcelona, IEEC UB, ICREA, E-08028 Barcelona, Spain. [Padoan, Paolo] Univ Barcelona, IEEC UB, Inst Ciencies Cosmos, E-08028 Barcelona, Spain. RP Pan, LB (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM lpan@cfa.harvard.edu; ppadoan@icc.ub.edu OI Padoan, Paolo/0000-0002-5055-5800 FU Clay Fellowship at Harvard-Smithsonian Center for Astrophysics; FP7-PEOPLE-RG grant [PIRG07-GA-2010-261359] FX Resources supporting this work were provided by the NASA High-End Computing (HEC) Program through the NASA Advanced Supercomputing (NAS) Division at Ames Research Center, and by the Port d'Informacio Cientfica (PIC), Spain, maintained by a collaboration of the Institut de Fsica d'Altes Energies (IFAE) and the Centro de Investigaciones Energticas, Medioambientales y Tecnolgicas (CIEMAT). LP is supported by a Clay Fellowship at Harvard-Smithsonian Center for Astrophysics. PP acknowledges support by the FP7-PEOPLE-2010-RG grant PIRG07-GA-2010-261359. NR 34 TC 1 Z9 1 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD OCT 10 PY 2015 VL 812 IS 1 AR 10 DI 10.1088/0004-637X/812/1/10 PG 21 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CV4KC UT WOS:000364234700010 ER PT J AU West, AA Weisenburger, KL Irwin, J Berta-Thompson, ZK Charbonneau, D Dittmann, J Pineda, JS AF West, Andrew A. Weisenburger, Kolby L. Irwin, Jonathan Berta-Thompson, Zachory K. Charbonneau, David Dittmann, Jason Pineda, J. Sebastian TI AN ACTIVITY-ROTATION RELATIONSHIP AND KINEMATIC ANALYSIS OF NEARBY MID-TO-LATE-TYPE M DWARFS SO ASTROPHYSICAL JOURNAL LA English DT Article DE stars: activity; stars: chromospheres; stars: kinematics and dynamics; stars: late-type; stars: low-mass; stars: rotation ID DIGITAL SKY SURVEY; LOW-MASS STARS; ANGULAR-MOMENTUM EVOLUTION; FULLY CONVECTIVE STARS; ORBITING M-DWARFS; FIELD M-DWARFS; MAGNETIC ACTIVITY; CHROMOSPHERIC ACTIVITY; H-ALPHA; SPECTROSCOPIC SURVEY AB Using spectroscopic observations and photometric light curves of 238 nearby M dwarfs from the MEarth exoplanet transit survey, we examine the relationships between magnetic activity (quantified by Ha emission), rotation period, and stellar age. Previous attempts to investigate the relationship between magnetic activity and rotation in these stars were hampered by the limited number of M dwarfs with measured rotation periods (and the fact that v sin i measurements probe only rapid rotation). However, the photometric data from MEarth allows us to probe a wide range of rotation periods for hundreds of M dwarf stars (from shorter than one to longer than 100 days). Over all M spectral types that we probe, we find that the presence of magnetic activity is tied to rotation, including for late-type, fully convective M dwarfs. We also find evidence that the fraction of late-type M dwarfs that are active may be higher at longer rotation periods compared to their early-type counterparts, with several active, late-type, slowly rotating stars present in our sample. Additionally, we find that all M dwarfs with rotation periods shorter than 26 days (early-type; M1-M4) and 86 days (late-type; M5-M8) are magnetically active. This potential mismatch suggests that the physical mechanisms that connect stellar rotation to chromospheric heating may be different in fully convective stars. A kinematic analysis suggests that the magnetically active, rapidly rotating stars are consistent with a kinematically young population, while slow-rotators are less active or inactive and appear to belong to an older, dynamically heated stellar population. C1 [West, Andrew A.; Weisenburger, Kolby L.] Boston Univ, Dept Astron, Boston, MA 02215 USA. [Weisenburger, Kolby L.] Univ Washington, Dept Astron, Seattle, WA 98195 USA. [Irwin, Jonathan; Charbonneau, David; Dittmann, Jason] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Berta-Thompson, Zachory K.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Pineda, J. Sebastian] CALTECH, Dept Astron, Pasadena, CA 91125 USA. RP West, AA (reprint author), Boston Univ, Dept Astron, 725 Commonwealth Ave, Boston, MA 02215 USA. EM aawest@bu.edu OI Berta-Thompson, Zachory/0000-0002-3321-4924; Pineda, J. Sebastian/0000-0002-4489-0135; West, Andrew/0000-0002-5805-6715; Dittmann, Jason/0000-0001-7730-2240 FU NSF grants [AST-1109273, AST-1255568]; Research Corporation for Science Advancement's Cottrell Scholarship; Boston University UROP program; Clare Boothe Luce scholarship; Torres Fellowship for Exoplanetary Research; David and Lucille Packard Fellowship for Science and Engineering; National Science Foundation [AST-0807690, AST-1109468, AST-1004488]; John Templeton Foundation; National Science Foundation Graduate Research Fellowship [DGE-1144469] FX The authors acknowledge Elisabeth Newton, Dylan Morgan, and the other members of the Boston Area Drinking And Society for Stars of Elfin Stature for useful conversations in the preparation of this manuscript. A.A.W. acknowledges the support of NSF grants AST-1109273 and AST-1255568 and the Research Corporation for Science Advancement's Cottrell Scholarship. K.L.W. acknowledges the support of the Boston University UROP program and the Clare Boothe Luce scholarship. Z.K.B.T. gratefully acknowledges support from the Torres Fellowship for Exoplanetary Research. The MEarth Team gratefully acknowledges funding from the David and Lucille Packard Fellowship for Science and Engineering (awarded to D.C.). This material is based upon work supported by the National Science Foundation under grants AST-0807690, AST-1109468, and AST-1004488 (Alan T. Waterman Award). This publication was made possible through the support of a grant from the John Templeton Foundation. The opinions expressed in this publication are those of the authors and do not necessarily reflect the views of the John Templeton Foundation. This material is based upon work supported by the National Science Foundation Graduate Research Fellowship (to JSP) under grant No. DGE-1144469. NR 72 TC 22 Z9 22 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD OCT 10 PY 2015 VL 812 IS 1 AR 3 DI 10.1088/0004-637X/812/1/3 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CV4KC UT WOS:000364234700003 ER PT J AU Yu, L Winn, JN Gillon, M Albrecht, S Rappaport, S Bieryla, A Dai, F Delrez, L Hillenbrand, L Holman, MJ Howard, AW Huang, CX Isaacson, H Jehin, E Lendl, M Montet, BT Muirhead, P Sanchis-Ojeda, R Triaud, AHMJ AF Yu, Liang Winn, Joshua N. Gillon, Michael Albrecht, Simon Rappaport, Saul Bieryla, Allyson Dai, Fei Delrez, Laetitia Hillenbrand, Lynne Holman, Matthew J. Howard, Andrew W. Huang, Chelsea X. Isaacson, Howard Jehin, Emmanuel Lendl, Monika Montet, Benjamin T. Muirhead, Philip Sanchis-Ojeda, Roberto Triaud, Amaury H. M. J. TI TESTS OF THE PLANETARY HYPOTHESIS FOR PTFO 8-8695b SO ASTROPHYSICAL JOURNAL LA English DT Article DE planetary systems; stars: individual (PTFO 8-8695); stars: pre-main sequence ID T-TAURI STAR; PRE-MAIN-SEQUENCE; MAGNETOSPHERIC ACCRETION; LIGHT CURVES; AA TAURI; CSI 2264; B 2; TRANSIT; VARIABILITY; SYSTEM AB The T Tauri star PTFO 8-8695 exhibits periodic fading events that have been interpreted as the transits of a giant planet on a precessing orbit. Here we present three tests of the planet hypothesis. First, we sought evidence for the secular changes in light-curve morphology that are predicted to be a consequence of orbital precession. We observed 28 fading events spread over several years and did not see the expected changes. Instead, we found that the fading events are not strictly periodic. Second, we attempted to detect the planet's radiation, based on infrared observations spanning the predicted times of occultations. We ruled out a signal of the expected amplitude. Third, we attempted to detect the Rossiter-McLaughlin effect by performing high-resolution spectroscopy throughout a fading event. No effect was seen at the expected level, ruling out most (but not all) possible orientations for the hypothetical planetary orbit. Our spectroscopy also revealed strong, time-variable, high-velocity Ha and Ca H & K emission features. All these observations cast doubt on the planetary hypothesis, and suggest instead that the fading events represent starspots, eclipses by circumstellar dust, or occultations of an accretion hotspot. C1 [Yu, Liang; Winn, Joshua N.; Rappaport, Saul; Dai, Fei; Triaud, Amaury H. M. J.] MIT, Dept Phys, Cambridge, MA 02139 USA. [Yu, Liang; Winn, Joshua N.; Rappaport, Saul; Dai, Fei; Triaud, Amaury H. M. J.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Gillon, Michael; Delrez, Laetitia; Jehin, Emmanuel; Lendl, Monika] Univ Liege, Inst Astrophys & Geophys, B-4000 Liege, Belgium. [Albrecht, Simon] Aarhus Univ, Dept Phys & Astron, Stellar Astrophys Ctr, DK-8000 Aarhus C, Denmark. [Bieryla, Allyson; Holman, Matthew J.; Montet, Benjamin T.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Hillenbrand, Lynne; Montet, Benjamin T.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA. [Howard, Andrew W.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Huang, Chelsea X.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. [Isaacson, Howard; Sanchis-Ojeda, Roberto] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Lendl, Monika] Univ Geneva, Astron Observ, CH-1290 Sauverny, Switzerland. [Muirhead, Philip] Boston Univ, Dept Astron, Boston, MA 02215 USA. [Triaud, Amaury H. M. J.] Univ Toronto Scarborough, Ctr Planetary Sci, Toronto, ON M1C 1A4, Canada. [Triaud, Amaury H. M. J.] Univ Toronto, Dept Astron & Astrophys, Toronto, ON M5S 3H4, Canada. RP Yu, L (reprint author), MIT, Dept Phys, Cambridge, MA 02139 USA. EM yuliang@mit.edu RI Muirhead, Philip/H-2273-2014; OI Muirhead, Philip/0000-0002-0638-8822; Montet, Benjamin/0000-0001-7516-8308; /0000-0002-4265-047X; Yu, Liang/0000-0003-1667-5427 FU NASA Origins program [NNX11AG85G]; F.R.I.A. fund of the FNRS; F.R.S-FNRS [FRFC 2.5.594.09.F]; National Science Foundation Graduate Research Fellowship [DGE1144469] FX We thank the referee, Jason W. Barnes, for his comments on the manuscript. We are grateful to Geoff Marcy for helping to arrange the Keck observations, to Aurelie Fumel for helping with the TRAPPIST observations, and to John Johnson and Jon Swift for attempting to perform photometric observations for this project. We thank Greg Herczeg, Hans Moritz Gunther, and Nikku Madhusudhan for helpful discussions, and Julian van Eyken for providing the PTF data in a convenient format. Work by JNW was supported by the NASA Origins program (grant NNX11AG85G). M.G. and E.J. are Research Associates at the Belgian Fund for Scientific Research (Fond National de la Recherche Scientifique, F.R.S-FNRS); L.D. received the support of the F.R.I.A. fund of the FNRS. TRAPPIST is a project funded by the F.R.S-FNRS under grant FRFC 2.5.594.09.F, with the participation of the Swiss National Science Foundation (SNF). B.T.M. is supported by the National Science Foundation Graduate Research Fellowship under grant No. DGE1144469. The authors wish to extend special thanks to those of Hawai'ian ancestry on whose sacred mountain of Mauna Kea we are privileged to be guests. Without their generous hospitality, the Keck observations presented herein would not have been possible. NR 42 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 OCT 10 PY 2015 VL 812 IS 1 AR 48 DI 10.1088/0004-637X/812/1/48 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CV4KC UT WOS:000364234700048 ER PT J AU Grotzinger, JP Gupta, S Malin, MC Rubin, DM Schieber, J Siebach, K Sumner, DY Stack, KM Vasavada, AR Arvidson, RE Calef, F Edgar, L Fischer, WF Grant, JA Griffes, J Kah, LC Lamb, MP Lewis, KW Mangold, N Minitti, ME Palucis, M Rice, M Williams, RME Yingst, RA Blake, D Blaney, D Conrad, P Crisp, J Dietrich, WE Dromart, G Edgett, KS Ewing, RC Gellert, R Hurowitz, JA Kocurek, G Mahaffy, P McBride, MJ McLennan, SM Mischna, M Ming, D Milliken, R Newsom, H Oehler, D Parker, TJ Vaniman, D Wiens, RC Wilson, SA AF Grotzinger, J. P. Gupta, S. Malin, M. C. Rubin, D. M. Schieber, J. Siebach, K. Sumner, D. Y. Stack, K. M. Vasavada, A. R. Arvidson, R. E. Calef, F., III Edgar, L. Fischer, W. F. Grant, J. A. Griffes, J. Kah, L. C. Lamb, M. P. Lewis, K. W. Mangold, N. Minitti, M. E. Palucis, M. Rice, M. Williams, R. M. E. Yingst, R. A. Blake, D. Blaney, D. Conrad, P. Crisp, J. Dietrich, W. E. Dromart, G. Edgett, K. S. Ewing, R. C. Gellert, R. Hurowitz, J. A. Kocurek, G. Mahaffy, P. McBride, M. J. McLennan, S. M. Mischna, M. Ming, D. Milliken, R. Newsom, H. Oehler, D. Parker, T. J. Vaniman, D. Wiens, R. C. Wilson, S. A. TI Deposition, exhumation, and paleoclimate of an ancient lake deposit, Gale crater, Mars SO SCIENCE LA English DT Article ID EARLY MARTIAN CLIMATE; ALLUVIAL ARCHITECTURE; POINT-BAR; EVOLUTION; CANADA; RIVER; ATMOSPHERE; CURIOSITY; SEDIMENT; DELTAS AB The landforms of northern Gale crater on Mars expose thick sequences of sedimentary rocks. Based on images obtained by the Curiosity rover, we interpret these outcrops as evidence for past fluvial, deltaic, and lacustrine environments. Degradation of the crater wall and rim probably supplied these sediments, which advanced inward from the wall, infilling both the crater and an internal lake basin to a thickness of at least 75 meters. This intracrater lake system probably existed intermittently for thousands to millions of years, implying a relatively wet climate that supplied moisture to the crater rim and transported sediment via streams into the lake basin. The deposits in Gale crater were then exhumed, probably by wind-driven erosion, creating Aeolis Mons (Mount Sharp). C1 [Grotzinger, J. P.; Siebach, K.; Fischer, W. F.; Griffes, J.; Lamb, M. P.; Palucis, M.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. [Gupta, S.] Univ London Imperial Coll Sci Technol & Med, Dept Earth Sci & Engn, London SW7 2AZ, England. [Malin, M. C.; Edgett, K. S.; McBride, M. J.] Malin Space Sci Syst, San Diego, CA 92121 USA. [Rubin, D. M.] Univ Calif Santa Cruz, Dept Earth & Planetary Sci, Santa Cruz, CA 95064 USA. [Schieber, J.] Indiana Univ, Dept Geol Sci, Bloomington, IN 47405 USA. [Sumner, D. Y.] Univ Calif Davis, Dept Earth & Planetary Sci, Davis, CA 95616 USA. [Stack, K. M.; Vasavada, A. R.; Calef, F., III; Blaney, D.; Crisp, J.; Mischna, M.; Parker, T. J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Arvidson, R. E.] Washington Univ, Dept Earth & Planetary Sci, St Louis, MO 63130 USA. [Edgar, L.] US Geol Survey, Astrogeol Sci Ctr, Flagstaff, AZ 86001 USA. [Grant, J. A.; Wilson, S. A.] Smithsonian Inst, Ctr Earth & Planetary Studies, Natl Air & Space Museum, Washington, DC 20560 USA. [Kah, L. C.] Univ Tennessee, Dept Earth & Planetary Sci, Knoxville, TN 37996 USA. [Lewis, K. W.] Johns Hopkins Univ, Dept Earth & Planetary Sci, Baltimore, MD 21218 USA. [Mangold, N.] Le Ctr Natl Rech, Lab Planetol & Geodynam Nantes, Unite Mixte Rech 6112, F-44322 Nantes, France. [Mangold, N.] Univ Nantes, F-44322 Nantes, France. [Minitti, M. E.; Williams, R. M. E.; Yingst, R. A.; Vaniman, D.] Planetary Sci Inst, Tucson, AZ 85719 USA. [Rice, M.] Western Washington Univ, Dept Geol, Bellingham, WA 98225 USA. [Blake, D.] NASA, Ames Res Ctr, Dept Space Sci, Moffett Field, CA 94035 USA. [Conrad, P.; Mahaffy, P.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Dietrich, W. E.] Univ Calif Berkeley, Dept Earth & Planetary Sci, Berkeley, CA 94720 USA. [Dromart, G.] Univ Lyon, Lab Geol Lyon, F-69364 Lyon, France. [Ewing, R. C.] Texas A&M Univ, Dept Geol & Geophys, College Stn, TX 77843 USA. [Gellert, R.] Univ Guelph, Dept Phys, Guelph, ON N1G 2W1, Canada. [Hurowitz, J. A.; McLennan, S. M.] SUNY Stony Brook, Dept Geosci, Stony Brook, NY 11794 USA. [Kocurek, G.] Univ Texas Austin, Dept Geol Sci, Austin, TX 78712 USA. [Ming, D.] NASA, Lyndon B Johnson Space Ctr, Astromat Res & Explorat Sci Div, Houston, TX 77058 USA. [Milliken, R.] Brown Univ, Dept Geol Sci, Providence, RI 02912 USA. [Newsom, H.] Univ New Mexico, Inst Meteorit, Albuquerque, NM 87131 USA. [Oehler, D.] NASA, Lyndon B Johnson Space Ctr, LZ Technol, Houston, TX 77058 USA. [Wiens, R. C.] Los Alamos Natl Lab, Space Remote Sensing, Los Alamos, NM 87544 USA. RP Grotzinger, JP (reprint author), CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. RI Crisp, Joy/H-8287-2016; OI Crisp, Joy/0000-0002-3202-4416; Siebach, Kirsten/0000-0002-6628-6297 FU UK Space Agency FX The authors are indebted to the MSL project's engineering and management teams for their exceptionally skilled and diligent efforts in making the mission as effective as possible and enhancing science operations. We are also grateful to all those MSL team members who participated in tactical and strategic operations. Without the support of both the engineering and science teams, the data presented here could not have been collected. Helpful reviews were provided by K. Bohacs and two anonymous reviewers. Some of this research was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA. Work in the UK was funded by the UK Space Agency. Data presented in this paper are archived in the Planetary Data System (pds.nasa.gov). NR 77 TC 52 Z9 54 U1 11 U2 80 PU AMER ASSOC ADVANCEMENT SCIENCE PI WASHINGTON PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA SN 0036-8075 EI 1095-9203 J9 SCIENCE JI Science PD OCT 9 PY 2015 VL 350 IS 6257 AR AAC7575 DI 10.1126/science.aac7575 PG 13 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA CS9JB UT WOS:000362405600029 PM 26450214 ER PT J AU Lee, TE Joglekar, YN AF Lee, Tony E. Joglekar, Yogesh N. TI PT-symmetric Rabi model: Perturbation theory SO PHYSICAL REVIEW A LA English DT Article ID RESONANCE; FIELDS; TIME AB We study a non-Hermitian version of the Rabi model, where a two-level system is periodically driven with an imaginary-valued drive strength, leading to alternating gain and loss. In the Floquet picture, the model exhibits PT symmetry, which can be broken when the drive is sufficiently strong. We derive the boundaries of the PT phase diagram for the different resonances by doing perturbation theory beyond the rotating-wave approximation. For the main resonance, we show that the non-Hermitian analog of the Bloch-Siegert shift corresponds to maximal PT breaking. For the higher-order resonances, we capture the boundaries to lowest order. We also solve the regime of high frequency by mapping to the Wannier-Stark ladder. Our model can be experimentally realized in waveguides with spatially modulated loss or in atoms with time-modulated spontaneous decay. C1 [Lee, Tony E.] Harvard Smithsonian Ctr Astrophys, ITAMP, Cambridge, MA 02138 USA. [Lee, Tony E.; Joglekar, Yogesh N.] Indiana Univ Purdue Univ Indianapolis IUPUI, Dept Phys, Indianapolis, IN 46202 USA. RP Lee, TE (reprint author), Harvard Smithsonian Ctr Astrophys, ITAMP, 60 Garden St, Cambridge, MA 02138 USA. FU NSF [DMR-1054020] FX We thank Peter Rabl for useful comments. This work was supported by NSF through a grant to ITAMP (T.L.) and through DMR-1054020 (Y.J.). NR 31 TC 9 Z9 9 U1 1 U2 8 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 OCT 8 PY 2015 VL 92 IS 4 AR 042103 DI 10.1103/PhysRevA.92.042103 PG 7 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA CS9ZA UT WOS:000362451700001 ER PT J AU Meyer, JL Dillard, BA Rodgers, JM Ritchie, KB Paul, VJ Teplitski, M AF Meyer, Julie L. Dillard, Brian A. Rodgers, John M. Ritchie, Kim B. Paul, Valerie J. Teplitski, Max TI Draft genome sequence of Halomonas meridiana R1t3 isolated from the surface microbiota of the Caribbean Elkhorn coral Acropora palmata SO STANDARDS IN GENOMIC SCIENCES LA English DT Article DE Coral microbiome; Surface mucus layer; Commensal; Oceanospirillales; Florida keys ID WHITE PLAGUE DISEASE; FAMILY HALOMONADACEAE; BACTERIAL COMMUNITIES; MUCUS; ALIGNMENT; SYSTEM AB Members of the gammaproteobacterial genus Halomonas are common in marine environments. Halomonas and other members of the Oceanospirillales have recently been identified as prominent members of the surface microbiota of reef-building corals. Halomonas meridiana strain R1t3 was isolated from the surface mucus layer of the scleractinian coral Acropora palmata in 2005 from the Florida Keys. This strain was chosen for genome sequencing to provide insight into the role of commensal heterotrophic bacteria in the coral holobiont. The draft genome consists of 290 scaffolds, totaling 3.5 Mbp in length and contains 3397 protein-coding genes. C1 [Meyer, Julie L.; Dillard, Brian A.; Rodgers, John M.; Teplitski, Max] Univ Florida, Inst Food & Agr Sci, Soil & Water Sci Dept, Gainesville, FL 32611 USA. [Ritchie, Kim B.] Mote Marine Lab, Sarasota, FL 34236 USA. [Paul, Valerie J.; Teplitski, Max] Smithsonian Marine Stn, Ft Pierce, FL USA. RP Teplitski, M (reprint author), Univ Florida, Inst Food & Agr Sci, Soil & Water Sci Dept, Gainesville, FL 32611 USA. EM maxtep@ufl.edu OI Meyer, Julie/0000-0003-3382-3321 FU Protect Our Reefs grant [2013-2]; George E. Burch Fellowship in Theoretical Medicine FX This research was supported by Protect Our Reefs grant 2013-2 and a George E. Burch Fellowship in Theoretical Medicine. This is a contribution #998 of the Smithsonian Marine Station. NR 33 TC 0 Z9 0 U1 2 U2 5 PU BIOMED CENTRAL LTD PI LONDON PA 236 GRAYS INN RD, FLOOR 6, LONDON WC1X 8HL, ENGLAND SN 1944-3277 J9 STAND GENOMIC SCI JI Stand. Genomic Sci. PD OCT 7 PY 2015 VL 10 AR 75 DI 10.1186/s40793-015-0069-y PG 7 WC Genetics & Heredity; Microbiology SC Genetics & Heredity; Microbiology GA DA7QJ UT WOS:000367998800001 PM 26451236 ER PT J AU Bertolotti, AC Griffiths, SM Truelove, NK Box, SJ Preziosi, RF de Leon, PS AF Bertolotti, Alicia C. Griffiths, Sarah M. Truelove, Nathan K. Box, Stephen J. Preziosi, Richard F. Salinas de Leon, Pelayo TI Isolation and characterization of 10 polymorphic microsatellite loci for the endangered Galapagos-endemic whitespotted sandbass (Paralabrax albomaculatus) SO PEERJ LA English DT Article DE Galapagos; Endemic; Endangered; Microsatellite; Polymorphic; Fisheries; Commercially important AB The white-spotted sandbass (Paralabrax albomaculatus) is a commercially important species in the Galapagos Marine Reserve, but is classified as endangered in the IUCN Red List. For this study, 10 microsatellite loci were isolated and characterized using Illumina paired-end sequencing. These loci can be used for genetic studies of population structure and connectivity to aid in the management of the white-spotted sandbass and other closely-related species. The 10 characterized loci were polymorphic, with 11-49 alleles per locus, and observed heterozygosity ranged from 0.575 to 0.964. This set of markers is the first to be developed for this species. C1 [Bertolotti, Alicia C.; Griffiths, Sarah M.; Preziosi, Richard F.] Univ Manchester, Fac Life Sci, Manchester, Lancs, England. [Truelove, Nathan K.; Box, Stephen J.] Smithsonian, Smithsonian Marine Stn, Ft Pierce, FL USA. [Salinas de Leon, Pelayo] Charles Darwin Res Stn, Santa Cruz, Galapagos Islan, Ecuador. RP Bertolotti, AC (reprint author), Univ Manchester, Fac Life Sci, Manchester, Lancs, England. EM alicia.bertolotti@gmail.com FU University of Manchester; Smithsonian Marine Station; Charles Darwin Research Station FX The University of Manchester, Smithsonian Marine Station and Charles Darwin Research Station provided funding for this work. The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 11 TC 1 Z9 1 U1 0 U2 10 PU PEERJ INC PI LONDON PA 341-345 OLD ST, THIRD FLR, LONDON, EC1V 9LL, ENGLAND SN 2167-8359 J9 PEERJ JI PeerJ PD OCT 6 PY 2015 VL 3 AR e1253 DI 10.7717/peerj.1253 PG 6 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA CV5RO UT WOS:000364329000001 PM 26557418 ER PT J AU Huang, YM Rueda, LM AF Huang, Yiau-Min Rueda, Leopoldo M. TI A pictorial key to the species of the Aedes (Zavortinkius) in the Afrotropical Region (Diptera: Culicidae) SO ZOOTAXA LA English DT Article DE Culicidae; Aedes; mosquitoes; identification key; Africa AB Six species of the subgenus Zavortinkius of Aedes Meigen in the Afrotropical Region are treated in a pictorial key based on diagnostic morphological features. Images of the diagnostic morphological structures of the adult thorax and leg are included. C1 [Huang, Yiau-Min] Smithsonian Inst, Dept Entomol, Washington, DC 20013 USA. [Rueda, Leopoldo M.] Walter Reed Army Inst Res, Entomol Branch, Walter Reed Biosystemat Unit, Silver Spring, MD 20910 USA. RP Huang, YM (reprint author), Smithsonian Inst, Museum Support Ctr MRC 534, Walter Reed Biosystemat Unit, 4210 Silver Hill Rd, Suitland, MD 20746 USA. EM huangy@si.edu; ruedapol@si.edu NR 23 TC 0 Z9 0 U1 0 U2 1 PU MAGNOLIA PRESS PI AUCKLAND PA PO BOX 41383, AUCKLAND, ST LUKES 1030, NEW ZEALAND SN 1175-5326 EI 1175-5334 J9 ZOOTAXA JI Zootaxa PD OCT 6 PY 2015 VL 4027 IS 4 BP 593 EP 599 PG 7 WC Zoology SC Zoology GA CS7PB UT WOS:000362275400009 PM 26624200 ER PT J AU Borges, R Khan, I Johnson, WE Gilbert, MTP Zhang, GJ Jarvis, ED O'Brien, SJ Antunes, A AF Borges, Rui Khan, Imran Johnson, Warren E. Gilbert, M. Thomas P. Zhang, Guojie Jarvis, Erich D. O'Brien, Stephen J. Antunes, Agostinho TI Gene loss, adaptive evolution and the co-evolution of plumage coloration genes with opsins in birds SO BMC GENOMICS LA English DT Article DE Opsin; Vision; Birds; Gene loss; Pseudogenization; Co-evolution; Plumage coloration ID DIM-LIGHT-VISION; VISUAL PIGMENTS; PINEAL-GLAND; ULTRAVIOLET VISION; OIL DROPLETS; SPHENISCUS-HUMBOLDTI; SPECTRAL SENSITIVITY; MOLECULAR EVOLUTION; NOCTURNAL BIRD; SWS1 OPSIN AB Background: The wide range of complex photic systems observed in birds exemplifies one of their key evolutionary adaptions, a well-developed visual system. However, genomic approaches have yet to be used to disentangle the evolutionary mechanisms that govern evolution of avian visual systems. Results: We performed comparative genomic analyses across 48 avian genomes that span extant bird phylogenetic diversity to assess evolutionary changes in the 17 representatives of the opsin gene family and five plumage coloration genes. Our analyses suggest modern birds have maintained a repertoire of up to 15 opsins. Synteny analyses indicate that PARA and PARIE pineal opsins were lost, probably in conjunction with the degeneration of the parietal organ. Eleven of the 15 avian opsins evolved in a non-neutral pattern, confirming the adaptive importance of vision in birds. Visual conopsins sw1, sw2 and lw evolved under negative selection, while the dim-light RH1 photopigment diversified. The evolutionary patterns of sw1 and of violet/ultraviolet sensitivity in birds suggest that avian ancestors had violet-sensitive vision. Additionally, we demonstrate an adaptive association between the RH2 opsin and the MC1R plumage color gene, suggesting that plumage coloration has been photic mediated. At the intra-avian level we observed some unique adaptive patterns. For example, barn owl showed early signs of pseudogenization in RH2, perhaps in response to nocturnal behavior, and penguins had amino acid deletions in RH2 sites responsible for the red shift and retinal binding. These patterns in the barn owl and penguins were convergent with adaptive strategies in nocturnal and aquatic mammals, respectively. Conclusions: We conclude that birds have evolved diverse opsin adaptations through gene loss, adaptive selection and coevolution with plumage coloration, and that differentiated selective patterns at the species level suggest novel photic pressures to influence evolutionary patterns of more-recent lineages. C1 [Borges, Rui; Khan, Imran; Antunes, Agostinho] Univ Porto, Interdisciplinary Ctr Marine & Environm Res, CIIMAR CIMAR, P-4050123 Oporto, Portugal. [Borges, Rui; Khan, Imran; Antunes, Agostinho] Univ Porto, Fac Sci, Dept Biol, P-4169007 Oporto, Portugal. [Johnson, Warren E.] Smithsonian Conservat Biol Inst, Front Royal, VA 22630 USA. [Gilbert, M. Thomas P.] Univ Copenhagen, Nat Hist Museum Denmark, Ctr GeoGenet, DK-1350 Copenhagen, Denmark. [Zhang, Guojie] BGI Shenzhen, China Natl GeneBank, Shenzhen 518083, Peoples R China. [Zhang, Guojie] Univ Copenhagen, Ctr Social Evolut, Dept Biol, DK-2100 Copenhagen, Denmark. [Jarvis, Erich D.] Duke Univ, Med Ctr, Dept Neurobiol, Durham, NC 27710 USA. [Jarvis, Erich D.] Howard Hughes Med Inst, Chevy Chase, MD 20815 USA. [O'Brien, Stephen J.] St Petersburg State Univ, Theodosius Dobzhansky Ctr Genome Bioinformat, St Petersburg 199004, Russia. [O'Brien, Stephen J.] Nova SE Univ, Oceanog Ctr, Ft Lauderdale, FL 33004 USA. RP Antunes, A (reprint author), Univ Porto, Interdisciplinary Ctr Marine & Environm Res, CIIMAR CIMAR, Rua Bragas 177, P-4050123 Oporto, Portugal. EM aantunes@ciimar.up.pt RI Gilbert, Marcus/A-8936-2013; Borges, Rui/H-5873-2016; OI Gilbert, Marcus/0000-0002-5805-7195; Borges, Rui/0000-0003-3931-9476; Zhang, Guojie/0000-0001-6860-1521 FU Fundacao para a Ciencia e a Tecnologia (FCT) [SFRH/BD/79850/2011, SFRH/BD/48518/2008]; Howard Hughes MedicalInstitute; Russian Ministry of Science [11.G34.31.0068]; FCT [UID/Multi/04423/2013, PTDC/AAC-AMB/121301/2010 (FCOMP-01-0124-FEDER-019490), PTDC/AAGGLO/6887/2014]; European Regional Development Fund (ERDF) in the framework of the programme PT2020 FX RB and IK were funded with a PhD grant from Fundacao para a Ciencia e a Tecnologia (FCT) (RB:SFRH/BD/79850/2011 and IK: SFRH/BD/48518/2008). EDJ was supported by the Howard Hughes MedicalInstitute. SJO was supported in part by Russian Ministry of Science Mega-grant no.11.G34.31.0068. AA was partially supported by the Strategic Funding UID/Multi/04423/2013 through national funds provided by FCT and European Regional Development Fund (ERDF) in the framework of the programme PT2020, and the FCT projects PTDC/AAC-AMB/121301/2010 (FCOMP-01-0124-FEDER-019490) and PTDC/AAGGLO/6887/2014. NR 82 TC 5 Z9 5 U1 20 U2 77 PU BIOMED CENTRAL LTD PI LONDON PA 236 GRAYS INN RD, FLOOR 6, LONDON WC1X 8HL, ENGLAND SN 1471-2164 J9 BMC GENOMICS JI BMC Genomics PD OCT 6 PY 2015 VL 16 AR 751 DI 10.1186/s12864-015-1924-3 PG 13 WC Biotechnology & Applied Microbiology; Genetics & Heredity SC Biotechnology & Applied Microbiology; Genetics & Heredity GA CS7GX UT WOS:000362253200001 PM 26438339 ER PT J AU Zalasiewicz, J Waters, CN Williams, M Barnosky, AD Cearreta, A Crutzen, P Ellis, E Ellis, MA Fairchild, IJ Grinevald, J Haff, PK Hajdas, I Leinfelder, R McNeill, J Odada, EO Poirier, C Richter, D Steffen, W Summerhayes, C Syvitski, JPM Vidas, D Wagreich, M Wing, SL Wolfe, AP Zhisheng, A Oreskes, N AF Zalasiewicz, Jan Waters, Colin N. Williams, Mark Barnosky, Anthony D. Cearreta, Alejandro Crutzen, Paul Ellis, Erle Ellis, Michael A. Fairchild, Ian J. Grinevald, Jacques Haff, Peter K. Hajdas, Irka Leinfelder, Reinhold McNeill, John Odada, Eric O. Poirier, Clement Richter, Daniel Steffen, Will Summerhayes, Colin Syvitski, James P. M. Vidas, Davor Wagreich, Michael Wing, Scott L. Wolfe, Alexander P. Zhisheng, An Oreskes, Naomi TI When did the Anthropocene begin? A mid-twentieth century boundary level is stratigraphically optimal SO QUATERNARY INTERNATIONAL LA English DT Article DE Anthropocene; Stratigraphy; GSSP; GSSA ID INTERNATIONAL CHRONOSTRATIGRAPHIC CHART; STRATOTYPE SECTION; MASS EXTINCTION; ICE-CORE; DEFINITION; QUATERNARY; FALLOUT; SERIES/EPOCH; RADIOCARBON; TRANSITION AB We evaluate the boundary of the Anthropocene geological time interval as an epoch, since it is useful to have a consistent temporal definition for this increasingly used unit, whether the presently informal term is eventually formalized or not. Of the three main levels suggested - an 'early Anthropocene' level some thousands of years ago; the beginning of the Industrial Revolution at similar to 1800 CE (Common Era); and the 'Great Acceleration' of the mid-twentieth century - current evidence suggests that the last of these has the most pronounced and globally synchronous signal. A boundary at this time need not have a Global Boundary Stratotype Section and Point (GSSP or 'golden spike') but can be defined by a Global Standard Stratigraphic Age (GSSA), i.e. a point in time of the human calendar. We propose an appropriate boundary level here to be the time of the world's first nuclear bomb explosion, on July 16th 1945 at Alamogordo, New Mexico; additional bombs were detonated at the average rate of one every 9.6 days until 1988 with attendant worldwide fallout easily identifiable in the chemostratigraphic record. Hence, Anthropocene deposits would be those that may include the globally distributed primary artificial radionuclide signal, while also being recognized using a wide range of other stratigraphic criteria. This suggestion for the Holocene-Anthropocene boundary may ultimately be superseded, as the Anthropocene is only in its early phases, but it should remain practical and effective for use by at least the current generation of scientists. (C) 2014 Elsevier Ltd and INQUA. C1 [Zalasiewicz, Jan; Williams, Mark] Univ Leicester, Dept Geol, Leicester LE1 7RH, Leics, England. [Waters, Colin N.; Ellis, Michael A.] British Geol Survey, Nottingham NG12 5GG, England. [Barnosky, Anthony D.] Univ Calif Berkeley, Museum Vertebrate Zool, Museum Paleontol, Dept Integrat Biol, Berkeley, CA 94720 USA. [Cearreta, Alejandro] Univ Pais Vasco UPV EHU, Fac Ciencia & Tecnol, Dept Estratig & Paleontol, Bilbao 48080, Spain. [Crutzen, Paul] Max Planck Inst Chem, Dept Atmospher Chem, D-55020 Mainz, Germany. [Ellis, Erle] Univ Maryland Baltimore Cty, Dept Geog & Environm Syst, Baltimore, MD 21250 USA. [Fairchild, Ian J.] Univ Birmingham, Sch Geog Earth & Environm Sci, Birmingham B15 2TT, W Midlands, England. [Grinevald, Jacques] IHEID, CH-1211 Geneva 11, Switzerland. [Haff, Peter K.] Duke Univ, Nicholas Sch Environm, Div Earth & Ocean Sci, Durham, NC 27516 USA. [Hajdas, Irka] ETH, Lab Ion Beam Phys, CH-8093 Zurich, Switzerland. [Leinfelder, Reinhold] Free Univ Berlin, Dept Geol Sci, D-12249 Berlin, Germany. [McNeill, John] Georgetown Univ, Washington, DC USA. [Odada, Eric O.] Univ Nairobi, Dept Geol, Nairobi, Kenya. [Poirier, Clement] Univ Caen Basse Normandie, Morphodynam Continentale & Cotiere, CNRS, F-14000 Caen, France. [Richter, Daniel] Duke Univ, Nicholas Sch Environm, Durham, NC 27708 USA. [Steffen, Will] Australian Natl Univ, Canberra, ACT 0200, Australia. [Summerhayes, Colin] Univ Cambridge, Scott Polar Res Inst, Cambridge CB2 1ER, England. [Syvitski, James P. M.] Univ Colorado, Boulder, CO 80309 USA. [Vidas, Davor] Fridtjof Nansen Inst Polhogda, Marine Affairs & Law Sea Programme, Nansen, Norway. [Wagreich, Michael] Univ Vienna, Dept Geodynam & Sedimentol, A-1090 Vienna, Austria. [Wing, Scott L.] Smithsonian Inst, Museum Nat Hist, Dept Paleobiol, Washington, DC 20560 USA. [Wolfe, Alexander P.] Univ Alberta, Dept Earth & Atmospher Sci, Edmonton, AB T6G 2E3, Canada. [Zhisheng, An] Chinese Acad Sci, Inst Earth Environm, Xian 710075, Peoples R China. [Oreskes, Naomi] Harvard Univ, Dept Hist Sci, Cambridge, MA 02138 USA. RP Waters, CN (reprint author), British Geol Survey, Nottingham NG12 5GG, England. EM jaz1@leicester.ac.uk RI Hajdas, Irka/C-6696-2011; Williams, Mark/B-7590-2009; AN, Zhisheng/F-8834-2012; OI Williams, Mark/0000-0002-7987-6069; Ellis, Erle/0000-0002-2006-3362; Leinfelder, Reinhold/0000-0002-4107-2161; Fairchild, Ian/0000-0003-4822-2895; Cearreta, Alejandro/0000-0003-0100-1454; Poirier, Clement/0000-0002-8311-8463; Wing, Scott/0000-0002-2954-8905; Wagreich, Michael/0000-0002-8828-0857 FU British Geological Survey's Engineering Geology science programme FX Philip Gibbard is thanked for his comments, as are the two referees, Kim Cohen and Phil Hughes, for very useful and thought-provoking observations and suggestions. Colin Waters and Mike Ellis publish with the permission of the Executive Director, British Geological Survey, Natural Environment Research Council, and funded with the support of the British Geological Survey's Engineering Geology science programme. NR 81 TC 37 Z9 38 U1 39 U2 128 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 1040-6182 EI 1873-4553 J9 QUATERN INT JI Quat. Int. PD OCT 5 PY 2015 VL 383 BP 196 EP 203 DI 10.1016/j.quaint.2014.11.045 PG 8 WC Geography, Physical; Geosciences, Multidisciplinary SC Physical Geography; Geology GA CT9GR UT WOS:000363125500014 ER PT J AU Schachat, SR Brown, RL AF Schachat, Sandra R. Brown, Richard L. TI Color Pattern on the Forewing of Micropterix (Lepidoptera: Micropterigidae): Insights into the Evolution of Wing Pattern and Wing Venation in Moths SO PLOS ONE LA English DT Article ID MORPHOLOGY; BUTTERFLIES; SYSTEMATICS; TORTRICIDAE; PHYLOGENY; BARCODES; ELEMENTS; HUBNER AB Wing patterns are key taxonomic characters that have long been used in descriptions of Lepidoptera; however, wing pattern homologies are not understood among different moth lineages. Here, we examine the relationship between wing venation and wing pattern in the genus Micropterix, among the most basal extant Lepidoptera, in order to evaluate the two existing predictive models that have the potential to establish wing pattern element homologies for the order. The location of wing pattern elements along the costal margin of the wing in Micropterix is consistent with the predictions of the model proposed for Tortricidae by Brown and Powell in 1991, later modified by Baixeras in 2002. The predictive power of this model for such distantly related taxa suggests that the model may hold across various superfamilies within Lepidoptera, and supports the long-held notion that fasciae, not spots, are the most likely primitive wing pattern elements for the order. In addition, the location of wing pattern elements suggests that the wing vein commonly termed Sc-1 may in fact be a different vein, which Comstock identified in Trichoptera and referred to as "a." C1 [Schachat, Sandra R.; Brown, Richard L.] Mississippi Entomol Museum, Mississippi State, MS 39762 USA. [Schachat, Sandra R.] Smithsonian Inst, Dept Paleobiol, Washington, DC 20560 USA. RP Schachat, SR (reprint author), Mississippi Entomol Museum, Mississippi State, MS 39762 USA. EM schachatsr@si.edu RI Schachat, Sandra/M-5399-2014 OI Schachat, Sandra/0000-0003-3237-5619 FU National Institute of Food and Agriculture; United States Department of Agriculture [MIS-012040]; National Science Foundation Graduate Research Fellowship Program [DGE-1125191] FX The research was supported in part by the National Institute of Food and Agriculture (http://nifa.usda.gov), United States Department of Agriculture (http://www.usda.gov), under project MIS-012040. SRS is supported by the National Science Foundation (http://www.nsf.gov) Graduate Research Fellowship Program (https://www.nsfgrfp.org/) under Grant No. DGE-1125191. The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 64 TC 5 Z9 5 U1 1 U2 11 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 OCT 5 PY 2015 VL 10 IS 10 AR e0139972 DI 10.1371/journal.pone.0139972 PG 16 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA CT0PR UT WOS:000362499200067 PM 26437004 ER PT J AU Bekaert, B Kamalandua, A Zapico, SC Van de Voorde, W Decorte, R AF Bekaert, Bram Kamalandua, Aubeline Zapico, Sara C. Van de Voorde, Wim Decorte, Ronny TI Improved age determination of blood and teeth samples using a selected set of DNA methylation markers SO EPIGENETICS LA English DT Article DE CpG marker; DNA-based age prediction; DNA methylation; quadratic regression modeling ID GENE; PREDICTION; DEATH AB Age estimation from DNA methylation markers has seen an exponential growth of interest, not in the least from forensic scientists. The current published assays, however, can still be improved by lowering the number of markers in the assay and by providing more accurate models to predict chronological age. From the published literature we selected 4 age-associated genes (ASPA, PDE4C, ELOVL2, and EDARADD) and determined CpG methylation levels from 206 blood samples of both deceased and living individuals (age range: 0-91years). This data was subsequently used to compare prediction accuracy with both linear and non-linear regression models. A quadratic regression model in which the methylation levels of ELOVL2 were squared showed the highest accuracy with a Mean Absolute Deviation (MAD) between chronological age and predicted age of 3.75years and an adjusted R-2 of 0.95. No difference in accuracy was observed for samples obtained either from living and deceased individuals or between the 2 genders. In addition, 29 teeth from different individuals (age range: 19-70years) were analyzed using the same set of markers resulting in a MAD of 4.86years and an adjusted R-2 of 0.74. Cross validation of the results obtained from blood samples demonstrated the robustness and reproducibility of the assay. In conclusion, the set of 4CpG DNA methylation markers is capable of producing highly accurate age predictions for blood samples from deceased and living individuals C1 [Bekaert, Bram; Kamalandua, Aubeline; Van de Voorde, Wim; Decorte, Ronny] KU Leuven Univ Leuven, Dept Imaging & Pathol, Leuven, Belgium. [Bekaert, Bram; Van de Voorde, Wim; Decorte, Ronny] KU Leuven Univ Leuven, Univ Hosp Leuven, Dept Forens Med, Lab Forens Genet & Mol Archeol, Leuven, Belgium. [Zapico, Sara C.] Smithsonian Inst, NMNH, MRC112, Dept Anthropol, Washington, DC 20560 USA. RP Bekaert, B (reprint author), KU Leuven Univ Leuven, Dept Imaging & Pathol, Leuven, Belgium. EM bram.bekaert@uzleuven.be OI Bekaert, Bram/0000-0002-5370-7363 NR 29 TC 5 Z9 5 U1 2 U2 18 PU TAYLOR & FRANCIS INC PI PHILADELPHIA PA 530 WALNUT STREET, STE 850, PHILADELPHIA, PA 19106 USA SN 1559-2294 EI 1559-2308 J9 EPIGENETICS-US JI Epigenetics PD OCT 3 PY 2015 VL 10 IS 10 BP 922 EP 930 DI 10.1080/15592294.2015.1080413 PG 9 WC Biochemistry & Molecular Biology; Genetics & Heredity SC Biochemistry & Molecular Biology; Genetics & Heredity GA CT1KG UT WOS:000362556600004 PM 26280308 ER PT J AU Reynolds, RR Hawkins, L McDanold, SL Shadle, S Bergstrom, E AF Reynolds, Regina Romano Hawkins, Les McDanold, Shana L. Shadle, Steve Bergstrom, Erik TI The Future of Serials Cataloging, CONSER and the ISSN: Conversations from the Field SO SERIALS REVIEW LA English DT Article DE CONSER; ISSN; serials cataloging AB What does the future hold for the shape of serials to come and for cataloging these and other continuing resources? How should cataloging change to cope with still-unknown types of continuing resources? Will there still be a need for cataloging? For CONSER? For ISSN? How can libraries position themselves to partner with nonlibrary metadata creators in a future linked data environment? Four serials experts discuss these and other questions in a free-ranging conversation about the future of serials cataloging. C1 [Reynolds, Regina Romano] Lib Congress, US ISSN Ctr, Washington, DC 20540 USA. [Hawkins, Les] Lib Congress, Cooperat & Instruct Program Div, Washington, DC 20540 USA. [McDanold, Shana L.] Georgetown Univ Lib, Tech Serv, Washington, DC USA. [Shadle, Steve] Univ Washington, Cataloging & Metadata Serv, Seattle, WA 98195 USA. [Bergstrom, Erik] Smithsonian Lib, Discovery Serv, Washington, DC USA. RP Reynolds, RR (reprint author), Lib Congress, US ISSN Ctr, 101 Independence Ave SE, Washington, DC 20540 USA. EM rrey@loc.gov OI McDanold, Shana/0000-0002-8643-2378 NR 2 TC 1 Z9 1 U1 0 U2 3 PU ROUTLEDGE JOURNALS, TAYLOR & FRANCIS LTD PI ABINGDON PA 4 PARK SQUARE, MILTON PARK, ABINGDON OX14 4RN, OXFORDSHIRE, ENGLAND SN 0098-7913 EI 1879-095X J9 SERIALS REV JI Ser. Rev. PD OCT 2 PY 2015 VL 41 IS 4 BP 224 EP 233 DI 10.1080/00987913.2015.1103633 PG 10 WC Information Science & Library Science SC Information Science & Library Science GA CY9NR UT WOS:000366734100002 ER PT J AU Mawdsley, JR AF Mawdsley, Jonathan R. TI Cladistic analysis and evolutionary relationships of the "Megaxylocopa clade" of the genus Xylocopa Latreille, 1802 (Insecta: Hymenoptera: Apidae) SO TROPICAL ZOOLOGY LA English DT Article ID PASSION-FRUIT C1 [Mawdsley, Jonathan R.] Smithsonian Inst, Dept Entomol, Washington, DC 20560 USA. RP Mawdsley, JR (reprint author), Smithsonian Inst, Dept Entomol, NHB 169, Washington, DC 20560 USA. EM mawdsleyj@si.edu NR 17 TC 0 Z9 0 U1 3 U2 3 PU TAYLOR & FRANCIS LTD PI ABINGDON PA 4 PARK SQUARE, MILTON PARK, ABINGDON OX14 4RN, OXON, ENGLAND SN 0394-6975 EI 1970-9528 J9 TROP ZOOL JI Trop. Zool. PD OCT 2 PY 2015 VL 28 IS 4 BP 163 EP 171 PG 9 WC Zoology SC Zoology GA CY9KJ UT WOS:000366725500003 ER PT J AU West, CF France, CA AF West, Catherine F. France, Christine A. TI HUMAN AND CANID DIETARY RELATIONSHIPS: COMPARATIVE STABLE ISOTOPE ANALYSIS FROM THE KODIAK ARCHIPELAGO, ALASKA SO JOURNAL OF ETHNOBIOLOGY LA English DT Article DE Stable isotope analysis; Canis familiaris; Vulpes vulpes; island ecology ID BONE-COLLAGEN; TROPHIC RELATIONSHIPS; PACIFIC PINNIPEDS; DOGS; NITROGEN; MARINE; ECOSYSTEMS; DELTA-N-15; ECOLOGY; CARBON AB Stable carbon and nitrogen isotopes are used to address the dietary relationship between humans and two canid species at the Uyak site (KOD-145) on Kodiak Island, Alaska: dog (Canis familiaris) and red fox (Vulpes vulpes). We assess the relative contribution of marine and terrestrial protein to each species' diet as a measure of their dietary relationship to people, using zooarchaeological data, food web data, and ethnohistoric observations to interpret the results. The results suggest that dogs and foxes had different diets: the dogs are consistently enriched in both C-13 and N-15, which indicates a heavy dependence on marine protein, while the fox samples produced both marine and terrestrial isotope values. Data from this project have the potential to expand our understanding of human-canid relationships in this island environment and in the greater context of island ecology, and contribute some of the first isotopic data for small terrestrial mammals in the Gulf of Alaska. C1 [West, Catherine F.] Boston Univ, Dept Archaeol, 675 Commonwealth Ave, Boston, MA 02215 USA. [France, Christine A.] Smithsonian Inst, Museum Conservat Inst, Suitland, MD 20746 USA. RP West, CF (reprint author), Boston Univ, Dept Archaeol, 675 Commonwealth Ave, Boston, MA 02215 USA. EM cfwest@bu.edu FU Smithsonian Office of Fellowships; National Museum of Natural History Archaeobiology Program; Smithsonian Museum Conservation Institute FX Our gratitude goes first to the Alutiiq Museum and Archaeological Repository of Kodiak, Alaska for encouraging and supporting work with the Uyak Site collections. Thanks to the Smithsonian Office of Fellowships, the National Museum of Natural History Archaeobiology Program, the Smithsonian Museum Conservation Institute, and Torben Rick, R. Jeff Speakman, and Melinda Zeder for the opportunity and funding to perform this research. Thanks to the National Ocean Sciences Accelerator Mass Spectrometry (NOSAMS) facility at the Woods Hole Oceanographic Institute for providing the AMS analysis, and to the three anonymous reviewers for their comments. NR 77 TC 1 Z9 1 U1 6 U2 9 PU SOC ETHNOBIOLOGY PI DENTON PA UNIV NORTH TEXAS, DEPT GEOGRAPHY, 1155 UNION CIRCLE 305279, DENTON, TX 76203-5017 USA SN 0278-0771 EI 2162-4496 J9 J ETHNOBIOL JI J. Ethnobiol. PD OCT PY 2015 VL 35 IS 3 BP 519 EP 535 PG 17 WC Anthropology; Biology SC Anthropology; Life Sciences & Biomedicine - Other Topics GA DM8DQ UT WOS:000376591300005 ER PT J AU Guainazzi, M David, L Grant, CE Miller, E Natalucci, L Nevalainen, J Petre, R Audard, M AF Guainazzi, Matteo David, Laurence Grant, Catherine E. Miller, Eric Natalucci, Lorenzo Nevalainen, Jukka Petre, Robert Audard, Marc TI On the in-flight calibration plans of modern x-ray observatories SO JOURNAL OF ASTRONOMICAL TELESCOPES INSTRUMENTS AND SYSTEMS LA English DT Article DE x-ray instrumentation; operations; x-rays ID XMM-NEWTON OBSERVATIONS; PHOTON IMAGING CAMERA; CROSS-CALIBRATION; CRAB-NEBULA; EPIC-PN; GRATING SPECTROMETER; GALAXY CLUSTERS; MSH 15-52; 3C 273; CHANDRA AB We present an overview of the set of celestial sources used for in-flight calibration of x-ray detectors by past and operational missions. We show the rationale behind their choice as a guideline for future missions aiming at optimizing the critical early phases of their science operations. (C) 2015 Society of Photo-Optical Instrumentation Engineers (SPIE) C1 [Guainazzi, Matteo] ESA European Space Astron Ctr, E-28692 Madrid, Spain. [Guainazzi, Matteo] Japan Aerosp Explorat Agcy, Inst Space & Astronaut Sci, Chuo Ku, Sagamihara, Kanagawa 2525210, Japan. [David, Laurence] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Grant, Catherine E.; Miller, Eric] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Natalucci, Lorenzo] INAF IAPS, Ist Nazl Astrofis, I-00133 Rome, Italy. [Nevalainen, Jukka] Tartu Observ, EE-61602 Toravere, Estonia. [Petre, Robert] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Audard, Marc] Univ Geneva, Dept Astron, CH-1290 Versoix, Switzerland. RP Guainazzi, M (reprint author), ESA European Space Astron Ctr, E-28692 Madrid, Spain. EM Matteo.Guainazzi@sciops.esa.int NR 80 TC 1 Z9 1 U1 1 U2 1 PU SPIE-SOC PHOTO-OPTICAL INSTRUMENTATION ENGINEERS PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98225 USA SN 2329-4124 EI 2329-4221 J9 J ASTRON TELESC INST JI J. Astron. Telesc. Instrum. Syst. PD OCT PY 2015 VL 1 IS 4 AR 047001 DI 10.1117/1.JATIS.1.4.047001 PG 12 WC Engineering, Aerospace; Instruments & Instrumentation; Optics SC Engineering; Instruments & Instrumentation; Optics GA DJ4QA UT WOS:000374190700013 ER PT J AU Marlowe, H McEntaffer, RL Allured, R DeRoo, CT Donovan, BD Miles, DM Tutt, JH Burwitz, V Menz, B Hartner, GD Smith, RK Cheimets, P Hertz, E Bookbinder, JA Gunther, R Yanson, A Vacanti, G Ackermann, M AF Marlowe, Hannah McEntaffer, Randall L. Allured, Ryan DeRoo, Casey T. Donovan, Benjamin D. Miles, Drew M. Tutt, James H. Burwitz, Vadim Menz, Benedikt Hartner, Gisela D. Smith, Randall K. Cheimets, Peter Hertz, Edward Bookbinder, Jay A. Gunther, Ramses Yanson, Alex Vacanti, Giuseppe Ackermann, Marcelo TI Performance testing of an off-plane reflection grating and silicon pore optic spectrograph at PANTER SO JOURNAL OF ASTRONOMICAL TELESCOPES INSTRUMENTS AND SYSTEMS LA English DT Article DE diffraction; gratings; grazing incidence; x-rays ID X-RAY OPTICS; ROSAT AB An x-ray spectrograph consisting of aligned, radially ruled off-plane reflection gratings and silicon pore optics (SPO) was tested at the Max Planck Institute for Extraterrestrial Physics PANTER x-ray test facility. SPO is a test module for the proposed Arcus mission, which will also feature aligned off-plane reflection gratings. This test is the first time two off-plane gratings were actively aligned to each other and with an SPO to produce an overlapped spectrum. We report the performance of the complete spectrograph utilizing the aligned gratings module and plans for future development. (C) 2015 Society of Photo-Optical Instrumentation Engineers (SPIE) C1 [Marlowe, Hannah; McEntaffer, Randall L.; DeRoo, Casey T.; Donovan, Benjamin D.; Miles, Drew M.; Tutt, James H.] Univ Iowa, Dept Phys & Astron, 210 Van Allen Hall, Iowa City, IA 52242 USA. [Allured, Ryan; Smith, Randall K.; Cheimets, Peter; Hertz, Edward] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Burwitz, Vadim; Menz, Benedikt; Hartner, Gisela D.] MPI Extraterr Phys, D-85748 Garching, Germany. [Bookbinder, Jay A.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Gunther, Ramses; Yanson, Alex; Vacanti, Giuseppe] Cosine Sci & Comp BV, NL-2333 CH Leiden, Netherlands. [Ackermann, Marcelo] Cosine Res BV, NL-2333 CH Leiden, Netherlands. RP Marlowe, H (reprint author), Univ Iowa, Dept Phys & Astron, 210 Van Allen Hall, Iowa City, IA 52242 USA. EM hannah-marlowe@uiowa.edu NR 14 TC 0 Z9 0 U1 0 U2 0 PU SPIE-SOC PHOTO-OPTICAL INSTRUMENTATION ENGINEERS PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98225 USA SN 2329-4124 EI 2329-4221 J9 J ASTRON TELESC INST JI J. Astron. Telesc. Instrum. Syst. PD OCT PY 2015 VL 1 IS 4 AR 045004 DI 10.1117/1.JATIS.1.4.045004 PG 7 WC Engineering, Aerospace; Instruments & Instrumentation; Optics SC Engineering; Instruments & Instrumentation; Optics GA DJ4QA UT WOS:000374190700011 ER PT J AU Schiefer, TL Pollock, DM AF Schiefer, Terence L. Pollock, David M. TI FIRST RECORD OF THE FAMILY TANYPEZIDAE (DIPTERA: SCHIZOPHORA) FROM ALABAMA SO ENTOMOLOGICAL NEWS LA English DT Article DE Tanypezid flies; mesic hardwood forest; southeastern United States; Gulf Coastal Plain; Buhrstone/Lime Hills; disjunct distribution; new state record AB The family Tanypezidae is reported from Alabama for the first time based on a specimen of Tanypeza picticornis Knab and Shannon collected in the Red Hills region of southern Alabama. This record represents a significant southward extension of the known range of T. picticornis, which was previously known only from as far south as Maryland and Virginia. The collecting site of the specimen is the southernmost locality known for the genus Tanypeza. C1 [Schiefer, Terence L.] Mississippi Entomol Museum, Box 9775, Mississippi State, MS 39762 USA. [Pollock, David M.] Natl Museum Nat Hist, Smithsonian Inst, Washington, DC 20013 USA. RP Schiefer, TL (reprint author), Mississippi Entomol Museum, Box 9775, Mississippi State, MS 39762 USA. EM tschiefer@entomology.msstate.edu; pollockd@si.edu FU William H. Cross Expedition Fund; National Institute of Food and Agriculture, United States Department of Agriculture [MIS-012040] FX This article is approved for publication as Journal Article No. J-12639 of the Mississippi Agricultural and Forestry Experiment Station. This research was supported in part by the William H. Cross Expedition Fund and the National Institute of Food and Agriculture, United States Department of Agriculture, under Project No. MIS-012040. NR 14 TC 0 Z9 0 U1 0 U2 1 PU AMER ENTOMOL SOC PI PHILADELPHIA PA 1900 BENJ FRANKLIN PARKWAY, PHILADELPHIA, PA 19103-1195 USA SN 0013-872X EI 2162-3236 J9 ENTOMOL NEWS JI Entomol. News PD OCT PY 2015 VL 125 IS 3 BP 191 EP 193 DI 10.3157/021.125.0307 PG 3 WC Entomology SC Entomology GA DE8OQ UT WOS:000370896300006 ER PT J AU Smith, DR AF Smith, David R. TI A NEW PRISTAULACUS KIEFFER (HYMENOPTERA: AULACIDAE) FROM MEXICO SO PROCEEDINGS OF THE ENTOMOLOGICAL SOCIETY OF WASHINGTON LA English DT Article DE parasitoid; Haematoxylum AB Pristaulacus laetus Smith, n. sp., is described from Sonora, Mexico. The female and male are described, illustrated, and separated from the similar P. mexiuni Smith and other Pristaulacus species. C1 [Smith, David R.] ARS, Systemat Entomol Lab, USDA, Natl Museum Nat Hist,Smithsonian Inst, POB 37012,MRC 168, Washington, DC 20013 USA. RP Smith, DR (reprint author), ARS, Systemat Entomol Lab, USDA, Natl Museum Nat Hist,Smithsonian Inst, POB 37012,MRC 168, Washington, DC 20013 USA. EM sawfly2@aol.com NR 2 TC 0 Z9 0 U1 0 U2 0 PU ENTOMOL SOC WASHINGTON PI WASHINGTON PA SMITHSONIAN INSTITUTION DEPT ENTOMOLOGY, WASHINGTON, DC 20560 USA SN 0013-8797 J9 P ENTOMOL SOC WASH JI Proc. Entomol. Soc. Wash. PD OCT PY 2015 VL 117 IS 4 BP 495 EP 498 DI 10.4289/0013-8797.117.4.495 PG 4 WC Entomology SC Entomology GA DD2SB UT WOS:000369771400008 ER PT J AU Smith, DR AF Smith, David R. TI A NEW MONOPHADNOIDES ASHMEAD (HYMENOPTERA: TENTHREDINIDAE) FROM EASTERN NORTH AMERICA AND NOTES ON OTHER SPECIES SO PROCEEDINGS OF THE ENTOMOLOGICAL SOCIETY OF WASHINGTON LA English DT Article DE Blennocampinae; sawflies ID SYMPHYTA; SAWFLIES AB Monophadnoides inornatus Smith, n. sp., is described from eastern United States, and the previously unknown male of M. conspiculatus MacGillivray is described. Comparisons are made of these two species and M. pauper (Provancher), which are similar sympatric species that might be confused. Females and males of the three species are illustrated for comparison and a revised key to males is provided. C1 [Smith, David R.] ARS, Systemat Entomol Lab, USDA, Natl Museum Nat Hist,Smithsonian Inst, POB 37012,MRC 168, Washington, DC 20013 USA. RP Smith, DR (reprint author), ARS, Systemat Entomol Lab, USDA, Natl Museum Nat Hist,Smithsonian Inst, POB 37012,MRC 168, Washington, DC 20013 USA. EM sawfly2@aol.com NR 17 TC 0 Z9 0 U1 0 U2 0 PU ENTOMOL SOC WASHINGTON PI WASHINGTON PA SMITHSONIAN INSTITUTION DEPT ENTOMOLOGY, WASHINGTON, DC 20560 USA SN 0013-8797 J9 P ENTOMOL SOC WASH JI Proc. Entomol. Soc. Wash. PD OCT PY 2015 VL 117 IS 4 BP 499 EP 507 DI 10.4289/0013-8797.117.4.499 PG 9 WC Entomology SC Entomology GA DD2SB UT WOS:000369771400009 ER PT J AU Banks, A Gates, M AF Banks, Ashley Gates, Michael TI A new distribution record for Mestocharis (Hymenoptera: Eulophidae) in North America SO PROCEEDINGS OF THE ENTOMOLOGICAL SOCIETY OF WASHINGTON LA English DT Editorial Material ID GENUS MESTOCHARIS C1 [Gates, Michael] ARS, Systemat Entomol Lab, USDA, Natl Museum Nat Hist,Smithsonian Inst, POB 37012,MRC-0168, Washington, DC 20013 USA. RP Banks, A (reprint author), 15 West Glebe Rd, Alexandria, VA 22305 USA. EM aminoashley@gmail.com; michael.gates@ars.usda.gov NR 5 TC 0 Z9 0 U1 0 U2 0 PU ENTOMOL SOC WASHINGTON PI WASHINGTON PA SMITHSONIAN INSTITUTION DEPT ENTOMOLOGY, WASHINGTON, DC 20560 USA SN 0013-8797 J9 P ENTOMOL SOC WASH JI Proc. Entomol. Soc. Wash. PD OCT PY 2015 VL 117 IS 4 BP 519 EP 521 DI 10.4289/0013-8797.117.4.519 PG 3 WC Entomology SC Entomology GA DD2SB UT WOS:000369771400011 ER PT J AU Goulet, H Smith, DR Smith, MA Fernandez-Triana, J AF Goulet, Henri Smith, David R. Smith, M. Alex Fernandez-Triana, Jose TI New Country Records for Teredon cubensis (Cresson) (Hymenoptera: Siricidae) SO PROCEEDINGS OF THE ENTOMOLOGICAL SOCIETY OF WASHINGTON LA English DT Editorial Material C1 [Goulet, Henri; Fernandez-Triana, Jose] Canadian Natl Insect Collect, 960 Carling Ave, Ottawa, ON K1A 0C6, Canada. [Smith, David R.] ARS, Systemat Entomol Lab, USDA, Natl Museum Nat Hist,Smithsonian Inst, Washington, DC 20013 USA. [Smith, M. Alex] Univ Guelph, Dept Integrat Biol, Guelph, ON N1G 2W1, Canada. RP Goulet, H (reprint author), Canadian Natl Insect Collect, 960 Carling Ave, Ottawa, ON K1A 0C6, Canada. EM Henri.Goulet@agr.gc.ca; salex@uoguelph.ca; sawfly2@aol.com; jose.fernandez@agr.gc.ca RI Smith, M Alex/B-4468-2013 OI Smith, M Alex/0000-0002-8650-2575 NR 2 TC 0 Z9 0 U1 0 U2 0 PU ENTOMOL SOC WASHINGTON PI WASHINGTON PA SMITHSONIAN INSTITUTION DEPT ENTOMOLOGY, WASHINGTON, DC 20560 USA SN 0013-8797 J9 P ENTOMOL SOC WASH JI Proc. Entomol. Soc. Wash. PD OCT PY 2015 VL 117 IS 4 BP 522 EP 524 DI 10.4289/0013-8797.117.4.522 PG 3 WC Entomology SC Entomology GA DD2SB UT WOS:000369771400012 ER PT J AU Windham, MD Beck, JB Li, FW Allphin, L Carman, JG Sherwood, DA Rushworth, CA Sigel, E Alexander, PJ Bailey, CD Al-Shehbaz, IA AF Windham, Michael D. Beck, James B. Li, Fay-Wei Allphin, Loreen Carman, John G. Sherwood, David A. Rushworth, Catherine A. Sigel, Erin Alexander, Patrick J. Bailey, C. Donovan Al-Shehbaz, Ihsan A. TI Searching for Diamonds in the Apomictic Rough: A Case Study Involving Boechera lignifera (Brassicaceae) SO SYSTEMATIC BOTANY LA English DT Article DE Apomixis; Cytology; microsatellites; PCO-MC; species delimitation ID GENUS BOECHERA; GEOGRAPHIC PARTHENOGENESIS; HOLBOELLII BRASSICACEAE; ARABIS BRASSICACEAE; NATURAL-POPULATIONS; ELYMUS-RECTISETUS; APOMIXIS; HYBRIDIZATION; REPRODUCTION; ARABIDOPSIS AB The genus Boechera is one of the most difficult species complexes in North America, with about 70 sexual diploids and hundreds of apomictic taxa representing diverse combinations of nearly every known sexual genome. In this study, we set out to clarify the taxonomy of Boechera lignifera, which currently includes a small number of sexual diploid populations in addition to the widespread apomictic diploid upon which the name is based. Using data from cytological studies, microsatellite DNA analyses, geography, and morphology, we demonstrate that the apomictic populations are genetically quite divergent from the sexual diploids. We propose the name Boechera kelseyana to accommodate the sexual diploid taxon, which occurs entirely south of the geographic range of B. lignifera. Boechera kelseyana is consistently separable from B. lignifera based on pollen and seed morphology, the length and proximal orientation of fruiting pedicels, differences in the branching and orientation of trichomes on the lowers stems, and the number of flowers and cauline leaves on unbranched fertile stems. C1 [Windham, Michael D.; Li, Fay-Wei; Rushworth, Catherine A.] Duke Univ, Dept Biol, Durham, NC 27708 USA. [Beck, James B.] Wichita State Univ, Dept Biol Sci, Wichita, KS 67260 USA. [Beck, James B.] Bot Res Inst Texas, Ft Worth, TX 76107 USA. [Allphin, Loreen] Brigham Young Univ, Dept Plant & Wildlife Sci, Provo, UT 84602 USA. [Carman, John G.; Sherwood, David A.] Utah State Univ, Plants Soils & Climate Dept, Logan, UT 84322 USA. [Sigel, Erin] Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, Washington, DC 20013 USA. [Alexander, Patrick J.; Bailey, C. Donovan] New Mexico State Univ, Dept Biol, Las Cruces, NM 88003 USA. [Al-Shehbaz, Ihsan A.] Missouri Bot Garden, St Louis, MO 63166 USA. RP Windham, MD (reprint author), Duke Univ, Dept Biol, Durham, NC 27708 USA. EM mdw26@duke.edu FU National Science Foundation [DEB-0816560, DEB-0816789, DEB-0817003]; U.S. Department of Commerce; NIST; Utah Agricultural Experiment Station; [70NANB4H3039] FX The authors thank the curators of the following herbaria for permission to remove pollen and small leaf fragments for molecular analyses: ARIZ, ASC, BRY, CS, DUKE, GH, NY, RM, SJNM, UT, and UTC; we are especially grateful to Ron Hartman for allowing us to sample the lectotype of B. lignifera preserved at RM. Collections from the type locality of B. kelseyana and populations near Wide Ruins, Arizona and Tohdildonih Wash, New Mexico (all on the Navajo Nation) were made under permit to Daniele Roth of the Navajo Natural Heritage Program. We acknowledge Becky Kowallis and Susan Nelson for assistance with the analyses of megagametogenesis. This research was funded by National Science Foundation awards DEB-0816560 (to M. Windham), DEB-0816789 (to L. Allphin), and DEB-0817003 (to C. D. Bailey), as well as support from the U.S. Department of Commerce, NIST, ATP cooperative agreement no. 70NANB4H3039 and the Utah Agricultural Experiment Station (to J. Carman). NR 67 TC 1 Z9 1 U1 1 U2 10 PU AMER SOC PLANT TAXONOMISTS PI LARAMIE PA UNIV WYOMING, DEPT BOTANY 3165, 1000 E UNIVERSITY AVE, LARAMIE, WY 82071 USA SN 0363-6445 EI 1548-2324 J9 SYST BOT JI Syst. Bot. PD OCT-DEC PY 2015 VL 40 IS 4 BP 1031 EP 1044 DI 10.1600/036364415X690076 PG 14 WC Plant Sciences; Evolutionary Biology SC Plant Sciences; Evolutionary Biology GA DD2US UT WOS:000369778300011 ER PT J AU Clark, JL Nee, M Bohs, L Knapp, S AF Clark, John L. Nee, Michael Bohs, Lynn Knapp, Sandra TI A Revision of Solanum section Aculeigerum (the Solanum wendlandii group, Solanaceae) SO SYSTEMATIC BOTANY LA English DT Article DE Central America; heterandry; lianas; South America; vines ID LECTOTYPIFICATION; LEPTOSTEMONUM; CLADE AB Solanum section Aculeigerum (the Solanum wendlandii group, Solanaceae) comprises eight species ranging from Mexico and Central America to Ecuador and Peru with one species in southeastern Brazil, Paraguay and northern Argentina. One species, Solanum wendlandii, is commonly cultivated worldwide in tropical and subtropical regions, and one new species from southern Mexico, Solanum triunfense, is described here. Members of Solanum section Aculeigerum are differentiated from other sections of Solanum by a combination of plurifoliate sympodial units, branched inflorescences, presence of prickles coupled with absence of stellate trichomes, and a vine-like habit. Unlike most other prickly species of Solanum, which are placed into Solanum subgenus Leptostemonum, they lack stellate hairs, and phylogenetic studies suggest that the section is one of several potential sister groups for the spiny solanums. A key, descriptions, habitat and distribution data, preliminary conservation assessments, specimens examined and illustrations are provided for all species in Solanum section Aculeigerum. Lectotypes are designated for the following five names: S. aculeolatum M. Martens & Galeotti, S. mazatenangense Coult. & Donn. Sm., S. molinarum J. L. Gentry, S. pachyandrum Bitter, and S. sagranum A. Rich., and neotypes are designated for S. glaucescens Zucc. and S. wendlandii Hook. f. C1 [Clark, John L.] Univ Alabama, Dept Biol Sci, Tuscaloosa, AL 35487 USA. [Clark, John L.] Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, Washington, DC 20013 USA. [Nee, Michael] New York Bot Garden, Bronx, NY 10458 USA. [Bohs, Lynn] Univ Utah, Dept Biol, Salt Lake City, UT 84112 USA. [Knapp, Sandra] Nat Hist Museum, Dept Life Sci, Cromwell Rd, London SW7 5BD, England. RP Knapp, S (reprint author), Nat Hist Museum, Dept Life Sci, Cromwell Rd, London SW7 5BD, England. EM s.knapp@nhm.ac.uk FU National Science Foundation, Planetary Biodiversity Inventory (PBI) Solanum: A worldwide treatment [DEB-0316614]; SYNTHESYS Project - European Community Research Infrastructure Action under the FP6 "Structuring the European Research Area" Programme FX We thank the herbaria cited in the text for making their material (as specimens and digital images) available; Nicholas Fumeaux and Lorenzo Ramella (G) for help finding and citing specimens; Frances Crawford (K), Leandro Giacomin (UFOP), Tiina Sarkinen (E), Kim Watson (NY), and Maria Vorontsova (K) for photographs of specimens and live plants; Patrick Meyer-Higgins and Pawel Ficinski (BM) for assistance in geo-referencing; Mindy Syfert (BM) for producing the maps; and Paloma Rojas (BM) for databasing much of the material cited here. This project was funded by the National Science Foundation, Planetary Biodiversity Inventory (PBI) Solanum: A worldwide treatment (DEB-0316614) to LB, SK and MN; SK travel to Madrid was funded by the SYNTHESYS Project http://www.synthesys.info/ financed by European Community Research Infrastructure Action under the FP6 "Structuring the European Research Area" Programme. The Department of Botany at the Smithsonian Institution's National Museum of Natural History kindly hosted JLC during his postdoctoral work as part of the PBI Solanum project (2005-2006). NR 53 TC 2 Z9 2 U1 0 U2 0 PU AMER SOC PLANT TAXONOMISTS PI LARAMIE PA UNIV WYOMING, DEPT BOTANY 3165, 1000 E UNIVERSITY AVE, LARAMIE, WY 82071 USA SN 0363-6445 EI 1548-2324 J9 SYST BOT JI Syst. Bot. PD OCT-DEC PY 2015 VL 40 IS 4 BP 1102 EP 1136 DI 10.1600/036364415X690148 PG 35 WC Plant Sciences; Evolutionary Biology SC Plant Sciences; Evolutionary Biology GA DD2US UT WOS:000369778300018 ER PT J AU Paz, RCR Souza, NP Brown, JL AF Paz, Regina C. R. Souza, Nely P. Brown, Janine L. TI Fecal cortisol metabolites as indicators of stress in crabeating-fox (Cerdocyoun thous) in captivity SO PESQUISA VETERINARIA BRASILEIRA LA English DT Article DE Glucocorticoids; noninvasive method; enzyme immunoassay; translocation; reproduction ID ADRENOCORTICAL FUNCTION; LYCAON-PICTUS; CORTICOSTERONE; EXCRETION; FECES AB Blood samples collection is a common method in biological research using domestic animals. However, most blood sampling techniques are complicated and highly invasive and may therefore not be appropriate for wildlife animals in research concerning stress. Thus, a non-invasive method to measure steroid hormones is critically needed. The first goal of this study was to determine how glucocorticoids concentrations are impacted by translocation and reproductive activity in crab-eating-fox (Cerdocyoun thous) in captivity. The physiological relevance of fecal glucocorticoid metabolites was further validated by demonstrating: (1) The translocation of a male to a females enclosure resulted in a 3.5-fold increase compared to baseline concentrations, (2) changes in adrenocortical activity, as reflected in concentrations of fecal cortisol metabolites during reproduction, gestation and lactation in females foxes, indicating that social interactions resulted in large increases of fecal glucocorticoids metabolites during the reproductive season. From these findings we conclude that fecal samples can be used for the non-invasive assessment of adrenocortical status in crab-eating-fox. C1 [Paz, Regina C. R.; Souza, Nely P.] Univ Fed Mato Grosso, Fac Agron Med Vet & Zootecn, BR-78060900 Cuiaba, MT, Brazil. [Brown, Janine L.] Smithsonian Conservat Biol Inst, Ctr Species Survival, Front Royal, VA 22630 USA. RP Paz, RCR (reprint author), Univ Fed Mato Grosso, Fac Agron Med Vet & Zootecn, Av Fernando Correa da Costa, BR-78060900 Cuiaba, MT, Brazil. EM reginacrpaz@gmail.com FU FAPEMAT; CAPES; SMITHSONIAN CBI FX We thank UFMT Zoo staff for providing a crab-eating-fox for the experiments. We are also grateful to Sara Putman and Nicole Presley for patient laboratory assistance. This research was funded by FAPEMAT, CAPES and SMITHSONIAN CBI. NR 20 TC 0 Z9 0 U1 4 U2 10 PU REVISTA PESQUISA VETERINARIA BRASILEIRA PI RIO JANEIRO PA EMBRAPA-SAUDE ANIMAL, KM47 SEROPEDICA, 23851-970 RIO JANEIRO, BRAZIL SN 0100-736X EI 1678-5150 J9 PESQUI VET BRASIL JI Pesqui. Vet. Bras. PD OCT PY 2015 VL 35 IS 10 BP 859 EP 862 DI 10.1590/S0100-736X2015001000007 PG 4 WC Veterinary Sciences SC Veterinary Sciences GA CZ5PD UT WOS:000367153600007 ER PT J AU Mommert, M Harris, AW Mueller, M Hora, JL Trilling, DE Bottke, WF Thomas, CA Delbo, M Emery, JP Fazio, G Smith, HA AF Mommert, M. Harris, A. W. Mueller, M. Hora, J. L. Trilling, D. E. Bottke, W. F. Thomas, C. A. Delbo, M. Emery, J. P. Fazio, G. Smith, H. A. TI EXPLORENEOS. VIII. DORMANT SHORT-PERIOD COMETS IN THE NEAR-EARTH ASTEROID POPULATION SO ASTRONOMICAL JOURNAL LA English DT Article DE comets: general; minor planets, asteroids: general ID SPITZER-SPACE-TELESCOPE; JUPITER-FAMILY COMETS; PHYSICAL-PROPERTIES; WILSON-HARRINGTON; 103P/HARTLEY 2; THERMAL-MODEL; OBJECTS; NUCLEUS; ORBITS; DISTRIBUTIONS AB We perform a search for dormant comets, asteroidal objects of cometary origin, in the near-Earth asteroid (NEA) population based on dynamical and physical considerations. Our study is based on albedos derived within the ExploreNEOs program and is extended by adding data from NEOWISE and the Akari asteroid catalog. We use a statistical approach to identify asteroids on orbits that resemble those of short-period near-Earth comets (NECs) using the Tisserand parameter with respect to Jupiter, the aphelion distance, and the minimum orbital intersection distance with respect to Jupiter. From the sample of NEAs on comet-like orbits, we select those with a geometric albedo p(V) <= 0.064 as dormant comet candidates, and find that only similar to 50% of NEAs on comet-like orbits also have comet-like albedos. We identify a total of 23 NEAs from our sample that are likely to be dormant short-period NECs and, based on a de-biasing procedure applied to the cryogenic NEOWISE survey, estimate both magnitudelimited and size-limited fractions of the NEA population that are dormant short-period comets. We find that 0.3%-3.3% of the NEA population with H <= 21, and (9(-5)(+2))% of the population with diameters d >= 1 km, are dormant short-period NECs. C1 [Mommert, M.; Trilling, D. E.] Univ Arizona, Dept Phys & Astron, Flagstaff, AZ 86011 USA. [Mommert, M.; Harris, A. W.] DLR Inst Planetary Res, D-12489 Berlin, Germany. [Mueller, M.] SRON, Netherlands Inst Space Res, NL-9700 Groningen, Netherlands. [Hora, J. L.; Fazio, G.; Smith, H. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Trilling, D. E.] Univ Western Cape, ZA-7535 Bellville, South Africa. [Bottke, W. F.] Southwest Res Inst, Boulder, CO 80302 USA. [Thomas, C. A.] NASA, Goddard Space Flight Ctr, ORAU, Greenbelt, MD 20771 USA. [Delbo, M.] Univ Nice Sophia Antipolis, CNRS, Observ Cote Azur, F-063044 Nice 4, France. [Emery, J. P.] Univ Tennessee, Dept Earth & Planetary Sci, Knoxville, TN 37996 USA. RP Mommert, M (reprint author), Univ Arizona, Dept Phys & Astron, POB 6010, Flagstaff, AZ 86011 USA. EM michael.mommert@nau.edu OI Mueller, Michael/0000-0003-3217-5385 FU DFG Special Priority Program 1385, "The First 10 Million Years of the solar system-a Planetary Materials Approach"; NASA [NNX10AB23G, NNX12AR54G]; NASA; National Aeronautics and Space Administration FX M.M. acknowledges support by the DFG Special Priority Program 1385, "The First 10 Million Years of the solar system-a Planetary Materials Approach." We would like to thank two anonymous referees for useful suggestions that led to significant improvements of the manuscript. Support for this work was provided by NASA awards NNX10AB23G and NNX12AR54G. 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 publication makes use of data products from the Wide-field Infrared Survey Explorer, which is a joint project of the University of California, Los Angeles, and the Jet Propulsion Laboratory/California Institute of Technology, funded by the National Aeronautics and Space Administration. This research is based on observations with Akari, a JAXA project with the participation of ESA. Support for this work was provided by NASA through an award issued by JPL/Caltech. NR 60 TC 3 Z9 3 U1 1 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 EI 1538-3881 J9 ASTRON J JI Astron. J. PD OCT PY 2015 VL 150 IS 4 AR 106 DI 10.1088/0004-6256/150/4/106 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CX7EF UT WOS:000365863900009 ER PT J AU Poppenhaeger, K Cody, AM Covey, KR Gunther, HM Hillenbrand, LA Plavchan, P Rebull, LM Stauffer, JR Wolk, SJ Espaillat, C Forbrich, J Gutermuth, RA Hora, JL Morales-Calderon, M Song, I AF Poppenhaeger, K. Cody, A. M. Covey, K. R. Guenther, H. M. Hillenbrand, L. A. Plavchan, P. Rebull, L. M. Stauffer, J. R. Wolk, S. J. Espaillat, C. Forbrich, J. Gutermuth, R. A. Hora, J. L. Morales-Calderon, M. Song, Inseok TI YSOVAR: MID-INFRARED VARIABILITY OF YOUNG STELLAR OBJECTS AND THEIR DISKS IN THE CLUSTER IRAS 20050+2720 SO ASTRONOMICAL JOURNAL LA English DT Article DE accretion, accretion disks; infrared: stars; protoplanetary disks; stars: pre-main sequence; stars: variables: general ID T-TAURI STARS; ORION NEBULA CLUSTER; MAIN-SEQUENCE STARS; INFRARED PHOTOMETRIC VARIABILITY; SPITZER-SPACE-TELESCOPE; CIRCUMSTELLAR DISKS; MOLECULAR CLOUD; FORMING REGION; PROTOPLANETARY DISKS; MULTIPOLAR OUTFLOW AB We present a time-variability study of young stellar objects (YSOs) in the cluster IRAS 20050+2720, performed at 3.6 and 4.5 mu m with the Spitzer Space Telescope; this study is part of the Young Stellar Object VARiability (YSOVAR) project. We have collected light curves for 181 cluster members over 60 days. We find a high variability fraction among embedded cluster members of ca. 70%, whereas young stars without a detectable disk display variability less often (in ca. 50% of the cases) and with lower amplitudes. We detect periodic variability for 33 sources with periods primarily in the range of 2-6 days. Practically all embedded periodic sources display additional variability on top of their periodicity. Furthermore, we analyze the slopes of the tracks that our sources span in the color-magnitude diagram (CMD). We find that sources with long variability time scales tend to display CMD slopes that are at least partially influenced by accretion processes, while sources with short variability timescales tend to display extinction-dominated slopes. We find a tentative trend of X-ray detected cluster members to vary on longer timescales than the X-ray undetected members. C1 [Poppenhaeger, K.; Wolk, S. J.; Hora, J. L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Cody, A. M.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Covey, K. R.] Western Washington Univ, Bellingham, WA 98225 USA. [Guenther, H. M.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Hillenbrand, L. A.] CALTECH, Dept Astron, Pasadena, CA 91125 USA. [Plavchan, P.] Missouri State Univ, Springfield, MO 65897 USA. [Rebull, L. M.; Stauffer, J. R.] Spitzer Sci Ctr Caltech, Pasadena, CA 91125 USA. [Espaillat, C.] Boston Univ, Boston, MA 02215 USA. [Forbrich, J.] Univ Vienna, Dept Astrophys, A-1180 Vienna, Austria. [Gutermuth, R. A.] Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA. [Morales-Calderon, M.] CSIC, INTA, Ctr Astrobiol, E-28691 Villanueva De La Canada, Spain. [Song, Inseok] Univ Georgia, Dept Phys & Astron, Athens, GA 30602 USA. RP Poppenhaeger, K (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Morales-Calderon, Maria/C-8384-2017; OI Morales-Calderon, Maria/0000-0001-9526-9499; Poppenhaeger, Katja/0000-0003-1231-2194; Gunther, Hans Moritz/0000-0003-4243-2840; Wolk, Scott/0000-0002-0826-9261; Rebull, Luisa/0000-0001-6381-515X; Plavchan, Peter/0000-0002-8864-1667; Covey, Kevin/0000-0001-6914-7797 FU NASA [NAS8-03060]; National Science Foundation; Jet Propulsion Laboratory (JPL) - NASA through the Sagan Fellowship Program; Spitzer grant [1490851] FX The authors thank Joshua Bloom and Mike Skrutskie for access to the PAIRITEL telescope, and Elaine Winston for helpful comments on the manuscript. This work is based on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. This research made use of Astropy, a community-developed core Python package for Astronomy (Astropy Collaboration et al. 2013). This research has made use of the SIMBAD database and the VizieR catalog access tool (Ochsenbein et al. 2000), both operated at CDS, Strasbourg, France and 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 NASA and the National Science Foundation. K. P.'s work was supported in part by the Jet Propulsion Laboratory (JPL) funded by NASA through the Sagan Fellowship Program executed by the NASA Exoplanet Science Institute. H. M. G. acknowledges Spitzer grant 1490851. P. P. acknowledges the JPL Research and Technology Development and Exoplanet Exploration programs. S. J. W. was supported by NASA contract NAS8-03060. NR 99 TC 6 Z9 6 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 EI 1538-3881 J9 ASTRON J JI Astron. J. PD OCT PY 2015 VL 150 IS 4 AR 118 DI 10.1088/0004-6256/150/4/118 PG 22 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CX7EF UT WOS:000365863900021 ER PT J AU Rice, TS Reipurth, B Wolk, SJ Vaz, LP Cross, NJG AF Rice, Thomas S. Reipurth, Bo Wolk, Scott J. Vaz, Luiz Paulo Cross, N. J. G. TI NEAR-INFRARED VARIABILITY IN THE ORION NEBULA CLUSTER SO ASTRONOMICAL JOURNAL LA English DT Article DE infrared: stars; stars: formation; stars: pre-main sequence; stars: variables: T Tauri, Herbig Ae/Be ID YOUNG STELLAR OBJECTS; SEQUENCE ECLIPSING BINARY; MULTICOLOR OPTICAL SURVEY; WIDE-FIELD CAMERA; T-TAURI STARS; LOW-MASS; MAGNETOSPHERIC ACCRETION; CIRCUMSTELLAR DISKS; TRAPEZIUM CLUSTER; LIGHT CURVES AB Using UKIRT on Mauna Kea, we have carried out a new near-infrared J, H, K monitoring survey of almost a square degree of the star-forming Orion Nebula Cluster with observations on 120 nights over three observing seasons, spanning a total of 894 days. We monitored similar to 15,000 stars down to J approximate to 20 using the WFCAM instrument, and have extracted 1203 significantly variable stars from our data. By studying variability in young stellar objects (YSOs) in the H - K, K color-magnitude diagram, we are able to distinguish between physical mechanisms of variability. Many variables show color behavior indicating either dust-extinction or disk/accretion activity, but we find that when monitored for longer periods of time, a number of stars shift between these two variability mechanisms. Further, we show that the intrinsic timescale of disk/accretion variability in young stars is longer than that of dust-extinction variability. We confirm that variability amplitude is statistically correlated with evolutionary class in all bands and colors. Our investigations of these 1203 variables have revealed 73 periodic AA Tau type variables, many large-amplitude and long-period (P > 15 days) YSOs, including three stars showing widely spaced periodic brightening events consistent with circumbinary disk activity, and four new eclipsing binaries. These phenomena and others indicate the activity of long-term disk/accretion variability processes taking place in young stars. We have made the light curves and associated data for these 1203 variables available online. C1 [Rice, Thomas S.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Reipurth, Bo] Univ Hawaii, Inst Astron Manoa, Hilo, HI 96720 USA. [Reipurth, Bo] Univ Hawaii, NASA Astrobiol Inst, Hilo, HI 96720 USA. [Wolk, Scott J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Vaz, Luiz Paulo] Univ Fed Minas Gerais, Dept Fis, ICEx, BR-30 12397 Belo Horizonte, MG, Brazil. [Cross, N. J. G.] Univ Edinburgh, Scottish Univ Phys Alliance, Inst Astron, Sch Phys,Royal Observ, Edinburgh EH9 3HJ, Midlothian, Scotland. RP Rice, TS (reprint author), Univ Michigan, Dept Astron, 311 West Hall,1085 South Univ Ave, Ann Arbor, MI 48109 USA. EM tsrice@umich.edu; reipurth@ifa.hawaii.edu; swolk@cfa.harvard.edu; vaz@fisica.ufmg.br; njc@roe.ac.uk FU NASA Origins program [NNX11AK55G]; National Aeronautics and Space Administration through the NASA Astrobiology Institute [NNA09DA77A] FX We are grateful to Andy Adamson and the staff at UKIRT for their dedication in obtaining this major set of observations. We thank the referee for detailed comments, which improved this paper. We thank Marcelo Guimaraes for his interest in the early phases of this project. B. R. acknowledges support from the NASA Origins program under grant number NNX11AK55G. This material is based upon work supported by the National Aeronautics and Space Administration through the NASA Astrobiology Institute under Cooperative Agreement No. NNA09DA77A issued through the Office of Space Science. This research has made use of the SIMBAD database, operated at CDS, Strasbourg, France, and of NASA's Astrophysics Data System Bibliographic Services. This research made use of Astropy, a community-developed core Python package for Astronomy (Astropy Collaboration et al. 2013). This research made use of Astroquery, a suite of tools for querying online astronomical data services. This research has made use of the AstroBetter blog and wiki. This research made use of APLpy, an open-source plotting package for Python hosted at http://aplpy.github.com. 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 100 TC 5 Z9 5 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 EI 1538-3881 J9 ASTRON J JI Astron. J. PD OCT PY 2015 VL 150 IS 4 AR 132 DI 10.1088/0004-6256/150/4/132 PG 35 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CX7EF UT WOS:000365863900035 ER PT J AU Ceruzzi, P AF Ceruzzi, Paul TI Delete: A Design History of Computer Vapourware. SO TECHNOLOGY AND CULTURE LA English DT Book Review C1 [Ceruzzi, Paul] Smithsonian Inst, Natl Air & Space Museum, Aerosp Elect & Comp, Washington, DC 20560 USA. RP Ceruzzi, P (reprint author), Smithsonian Inst, Natl Air & Space Museum, Aerosp Elect & Comp, Washington, DC 20560 USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU JOHNS HOPKINS UNIV PRESS PI BALTIMORE PA JOURNALS PUBLISHING DIVISION, 2715 NORTH CHARLES ST, BALTIMORE, MD 21218-4363 USA SN 0040-165X EI 1097-3729 J9 TECHNOL CULT JI Technol. Cult. PD OCT PY 2015 VL 56 IS 4 BP 1013 EP 1015 PG 3 WC History & Philosophy Of Science SC History & Philosophy of Science GA CX2VR UT WOS:000365555400035 ER PT J AU Tavabi, E Koutchmy, S Golub, L AF Tavabi, E. Koutchmy, S. Golub, L. TI Limb Event Brightenings and Fast Ejection Using IRIS Mission Observations SO SOLAR PHYSICS LA English DT Article DE Explosive event; Macrospicule; Jet; Magnetic reconnection; Multi-directional ejection ID X-RAY JETS; SOLAR TRANSITION REGION; HE II 304; MAGNETIC RECONNECTION; EXPLOSIVE EVENTS; SPICULES; MACROSPICULES; TELESCOPE; EVOLUTION; POINTS AB The Interface Region Imaging Spectrograph (IRIS) of the recently commissioned NASA small explorer mission provides significantly more complete and higher resolution spectral coverage of the dynamical conditions inside the chromosphere and transition region (TR) than has been available ever before. High temporal, spatial () and spectral resolution observations from the ultraviolet IRIS spectra near the solar limb reveal high-energy limb event brightenings (LEBs) at low chromospheric heights at about 1 Mm above the limb. They can be characterized as explosive events producing jets. We selected two events showing spectra of a confined eruption just off or near the quiet-Sun limb, the jet part showing obvious moving material with short-duration large Doppler shifts in three directions that were identified as macrospicules on slit-jaw (SJ) images in Si iv and He ii 304 . The events were analyzed from a sequence of very close rasters taken near the central meridian and the South Pole limb. We analyzed the processed SJ images and the simultaneously observed fast spectral sequences, which have large Doppler shifts, with a pair of redshifted elements together with a faster blueshifted element from almost the same position. Shifts correspond to velocities of up to in projection on the plane of the sky. Erupting spicules and macrospicules from these regions are visible in images taken before and after the spectra. The cool low first ionization potential (FIP) element simultaneous line emissions of the Mg ii h and k resonance lines do not clearly show a similar signature because of optical thickness effects, but the Si iv broadband SJ images do. The bidirectional plasma jets ejected from a small reconnection site are interpreted to be the result of coronal loop-loop interactions that lead to reconnection in nearby sites. C1 [Tavabi, E.] PNU, Dept Phys, Tehran 193953697, Iran. [Koutchmy, S.] CNRS, UMR 7095, Inst Astrophys Paris, F-75014 Paris, France. [Koutchmy, S.] UPMC, F-75014 Paris, France. [Golub, L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Tavabi, E (reprint author), PNU, Dept Phys, Tehran 193953697, Iran. EM tavabi@iap.fr FU Institut d'Astrophysique de Paris-CNRS; UPMC; Lockheed Martin FX IRIS is a NASA small explorer mission developed and operated by LMSAL with mission operations executed at NASA ARC with contribution from NSC (Norway). We thank T.M.D. Pereira for his very useful online tutorial for IRIS data analysis (http://folk.uio.no/tiago/naoj2014_exercises/tutorials.html). We are indebted to Boris Filippov, Igor Veselovsky, and Jean-Claude Vial for making meaningful remarks on the paper. We warmly acknowledge the work of our referee, who provided an extended detailed report and added many interesting suggestions and requests. This work has been supported by the Institut d'Astrophysique de Paris-CNRS and UPMC. LG was supported by a contract from Lockheed Martin to SAO. NR 40 TC 2 Z9 2 U1 0 U2 1 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 OCT PY 2015 VL 290 IS 10 BP 2871 EP 2887 DI 10.1007/s11207-015-0771-3 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CW8AE UT WOS:000365220000013 ER PT J AU Liu, HP Hovingh, P Hershler, R AF Liu, Hsiu-Ping Hovingh, Peter Hershler, Robert TI GENETIC EVIDENCE FOR RECENT SPREAD OF SPRINGSNAILS (HYDROBIIDAE: PYRGULOPSIS) ACROSS THE WASATCH DIVIDE SO WESTERN NORTH AMERICAN NATURALIST LA English DT Article ID WESTERN NORTH-AMERICA; AQUATIC GASTROPODS; RIVER-BASIN; RISSOOIDEA; CAENOGASTROPODA; SYSTEMATICS; FISH; DNA AB The biogeographic history of aquatic organisms in relation to the Wasatch Mountains divide (which sepa rates the eastern Great Basin and upper Colorado River basin in Utah) has been little studied aside from a large body of work on fishes. Pyrgulopsis kolobensis is a small springsnail that is distributed (in the eastern portion of its range) along the western flanks of the Wasatch Mountains, with a single population occurring just across the Wasatch divide in Strawberry Valley. Here we analyze the genetic structure of this species across the Wasatch divide (using the mtCOI gene) to discriminate between alternative hypotheses that explain this distributional pattern. The 6 P. kolobensis populations that we sampled were resolved as a single, weakly supported and shallowly structured clade in a Bayesian analysis. Specimens from Strawberry Valley shared a unique haplotype and differed from the other populations by 0.3%-0.8% sequence divergence, suggesting a geologically recent split that well postdated the Miocene inception of the Wasatch divide. This result is consistent with a hypothesis (supported by geological evidence) that the Strawberry Valley population became isolated during the late Quaternary as a result of a headwater transfer across the Wasatch divide. Our findings parallel a recent phylogeographic study of regional pebblesnails (Fluminicola coloradensis) and contrast with the prevailing pattern in fishes, which generally do not cross the Wasatch divide. The ability of these 2 snail species to penetrate into upland headwater habitats appears to be the key to their success in crossing the Wasatch (and other) drainage divides. C1 [Liu, Hsiu-Ping] Metropolitan State Univ Denver, Dept Biol, Denver, CO 80217 USA. [Hershler, Robert] Smithsonian Inst, Dept Invertebrate Zool, Washington, DC 20013 USA. RP Liu, HP (reprint author), Metropolitan State Univ Denver, Dept Biol, Denver, CO 80217 USA. EM hershlerr@si.edu FU LAS Mini-Grant, Metropolitan State University of Denver FX This project was supported in part by an award to HPL from LAS Mini-Grant, Metropolitan State University of Denver. NR 30 TC 0 Z9 0 U1 3 U2 8 PU BRIGHAM YOUNG UNIV PI PROVO PA 290 LIFE SCIENCE MUSEUM, PROVO, UT 84602 USA SN 1527-0904 EI 1944-8341 J9 WEST N AM NATURALIST JI West. North Am. Naturalist PD OCT PY 2015 VL 75 IS 3 BP 325 EP 331 PG 7 WC Biodiversity Conservation; Ecology SC Biodiversity & Conservation; Environmental Sciences & Ecology GA CW8LI UT WOS:000365250700008 ER PT J AU Kivell, TL Deane, AS Tocheri, MW Orr, CM Schmid, P Hawks, J Berger, LR Churchill, SE AF Kivell, Tracy L. Deane, Andrew S. Tocheri, Matthew W. Orr, Caley M. Schmid, Peter Hawks, John Berger, Lee R. Churchill, Steven E. TI The hand of Homo naledi SO NATURE COMMUNICATIONS LA English DT Article ID POLLICAL DISTAL PHALANX; FITTING HR-PCF; AUSTRALOPITHECUS-AFARENSIS; POSITIONAL BEHAVIOR; MORPHOLOGY; EVOLUTION; SHAPE; SIZE; METACARPAL; CURVATURE AB A nearly complete right hand of an adult hominin was recovered from the Rising Star cave system, South Africa. Based on associated hominin material, the bones of this hand are attributed to Homo naledi. This hand reveals a long, robust thumb and derived wrist morphology that is shared with Neandertals and modern humans, and considered adaptive for intensified manual manipulation. However, the finger bones are longer and more curved than in most australopiths, indicating frequent use of the hand during life for strong grasping during locomotor climbing and suspension. These markedly curved digits in combination with an otherwise human-like wrist and palm indicate a significant degree of climbing, despite the derived nature of many aspects of the hand and other regions of the postcranial skeleton in H. naledi. C1 [Kivell, Tracy L.] Univ Kent, Sch Anthropol & Conservat, Skeletal Biol Res Ctr, Anim Postcranial Evolut Lab, Canterbury CT2 7NR, Kent, England. [Kivell, Tracy L.] Max Planck Inst Evolutionary Anthropol, Dept Human Evolut, D-04103 Leipzig, Germany. [Kivell, Tracy L.; Deane, Andrew S.; Schmid, Peter; Hawks, John; Berger, Lee R.; Churchill, Steven E.] Univ Witwatersrand, Evolutionary Studies Inst, ZA-2050 Johannesburg, South Africa. [Kivell, Tracy L.; Deane, Andrew S.; Schmid, Peter; Hawks, John; Berger, Lee R.; Churchill, Steven E.] Univ Witwatersrand, Ctr Excellence PalaeoSci, ZA-2050 Johannesburg, South Africa. [Deane, Andrew S.] Univ Kentucky, Coll Med, Dept Anat & Neurobiol, MN UK Med Ctr 224, Lexington, KY 40536 USA. [Tocheri, Matthew W.] Lakehead Univ, Dept Anthropol, Thunder Bay, ON P7K 1L8, Canada. [Tocheri, Matthew W.] Smithsonian Inst, Natl Museum Nat Hist, Dept Anthropol, Human Origins Program, Washington, DC 20560 USA. [Orr, Caley M.] Univ Colorado, Sch Med, Dept Cell & Dev Biol, Aurora, CO 80045 USA. [Schmid, Peter] Univ Zurich, Anthropol Inst & Museum, CH-8057 Zurich, Switzerland. [Hawks, John] Univ Wisconsin, Dept Anthropol, Madison, WI 53593 USA. [Churchill, Steven E.] Duke Univ, Dept Evolutionary Anthropol, Durham, NC 27708 USA. RP Kivell, TL (reprint author), Univ Kent, Sch Anthropol & Conservat, Skeletal Biol Res Ctr, Anim Postcranial Evolut Lab, Marlowe Bldg, Canterbury CT2 7NR, Kent, England. EM t.l.kivell@kent.ac.uk OI Tocheri, Matthew/0000-0001-7600-8998 FU National Geographic Society; National Research Foundation; European Research Council [336301]; Max Planck Society; Smithsonian Scholarly Studies Program; Canada Research Chairs Program FX We thank the National Geographic Society and the National Research Foundation for particularly significant funding of both the discovery, recovery and analysis of this material. We thank the University of the Witwatersrand and the Evolutionary Studies Institute, as well as the South African National Centre of Excellence in PalaeoSciences for curating the material and hosting the authors while studying the material. We thank S. Potze, L.C. Kgasi and the Ditsong National Museum of Natural History, B. Zipfel and the University of the Witwatersrand, Y. Rak, I. Hershkovitz and Tel Aviv University, T. White, W. Kimbel, B. Asfaw, G. Semishaw, Y. Assefa, G. Shimelies and National Museum of Ethiopia, A. Gidna, A. P. Kweka and Museum and House of Culture Tanzania for access to comparative fossil collections; curators at Museum fur Naturkunde Berlin, Max-Planck-Institut fur evolutionare Anthropologie, Naturhistorisches Museum Wien, Universitat Wien, Musee royal de L'Afrique central, Univesita degli Studi di Firenze and the Powell Cotton Museum for access to comparative extant material; and S. Traynor for help with photography. Partial funding for aspects of this research was provided by the European Research Council Starting Grant Number 336301 (T.L.K.), the Max Planck Society (T.L.K.), Smithsonian Scholarly Studies Program (M.W.T.) and Canada Research Chairs Program (M.W.T.). NR 58 TC 15 Z9 15 U1 10 U2 48 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 OCT PY 2015 VL 6 AR 8431 DI 10.1038/ncomms9431 PG 9 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA CW3WX UT WOS:000364924200002 PM 26441219 ER PT J AU Akamatsu, H van Weeren, RJ Ogrean, GA Kawahara, H Stroe, A Sobral, D Hoeft, M Rottgering, H Bruggen, M Kaastra, JS AF Akamatsu, H. van Weeren, R. J. Ogrean, G. A. Kawahara, H. Stroe, A. Sobral, D. Hoeft, M. Rottgering, H. Brueggen, M. Kaastra, J. S. TI Suzaku X-ray study of the double radio relic galaxy cluster CIZA J2242.8+5301 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE shock waves; methods: data analysis; galaxies: clusters: individual: CIZA J2242.8+5301; X-rays: galaxies: clusters; galaxies: clusters: intracluster medium ID LARGE-SCALE STRUCTURE; NONTHERMAL ELECTRON ACCELERATION; INTRACLUSTER MEDIUM; SHOCK-WAVES; ABELL 3667; HYDRODYNAMIC SIMULATIONS; RELATIVISTIC ELECTRONS; PARTICLE-ACCELERATION; SAUSAGE CLUSTER; ENERGY-SPECTRA AB Context. We present the results from Suzaku observations of the merging cluster of galaxies CIZA J2242.8+5301 at z = 0.192. Aims. To study the physics of gas heating and particle acceleration in cluster mergers, we investigated the X-ray emission from CIZAJ2242.8+5301, which hosts two giant radio relics in the northern and southern part of the cluster. Methods. We analyzed data from three-pointed Suzaku observations of CIZA J2242.8+5301 to derive the temperature distribution in four different directions. Results. The intracluster medium (ICM) temperature shows a remarkable drop from 8.5(-0).(+0.8)(6) keV to 2.7(-0.4)(+0.7) keV across the northern radio relic. The temperature drop is consistent with a Mach number M-n = 2.7(-0.4)(+0.7) and a shock velocity v(shock:n) = 2300(-400)(+700) km s(-1). We also confirm the temperature drop across the southern radio relic. However, the ICM temperature beyond this relic is much higher than beyond the northern relic, which gives a Mach number M-s = 1.7(-0.3)(+0.4) and shock velocity v(shock:s) = 2040(-410)(+550) km s(-1). These results agree with other systems showing a relationship between the radio relics and shock fronts which are induced by merging activity. We compare the X-ray derived Mach numbers with the radio derived Mach numbers from the radio spectral index under the assumption of diffusive shock acceleration in the linear test particle regime. For the northern radio relic, the Mach numbers derived from X-ray and radio observations agree with each other. Based on the shock velocities, we estimate that CIZA J2242.8+5301 is observed approximately 0.6 Gyr after core passage. The magnetic field pressure at the northern relic is estimated to be 9% of the thermal pressure. C1 [Akamatsu, H.; Kaastra, J. S.] SRON Netherlands Inst Space Res, NL-3584 CA Utrecht, Netherlands. [van Weeren, R. J.; Ogrean, G. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Kawahara, H.] Univ Tokyo, Dept Earth & Planetary Sci, Tokyo 1130033, Japan. [Stroe, A.; Sobral, D.; Rottgering, H.; Kaastra, J. S.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [Brueggen, M.] Univ Hamburg, Hamburg Observ, D-21029 Hamburg, Germany. [Hoeft, M.] Thuringer Landessternwarte Tautenburg, D-07778 Tautenburg, Germany. [Sobral, D.] Univ Lisbon, OAL, Inst Astrofis & Ciencias Espaco, P-1349018 Lisbon, Portugal. [Sobral, D.] Univ Lisbon, Fac Ciencias, Dept Fis, P-1749016 Lisbon, Portugal. RP Akamatsu, H (reprint author), SRON Netherlands Inst Space Res, Sorbonnelaan 2, NL-3584 CA Utrecht, Netherlands. EM H.Akamatsu@sron.nl RI Sobral, David/C-7919-2014; OI Sobral, David/0000-0001-8823-4845; van Weeren, Reinout/0000-0002-0587-1660 FU NASA through Einstein Postdoctoral grant [PF2-130104]; NASA [NAS8-03060]; JSPS; MEXT [25800106]; FCT; DFG; Netherlands Organisation for Scientific research (NWO) through a Veni fellowship; [26-606] FX The authors wish to thank the referee for constructive comments that significantly improved the manuscript. The authors thank the Suzaku team members for their support of the Suzaku project and T. H. Reiprich for the data to reproduce temperature profiles obtained with Suzaku. We would also like to thank A. Simionescu and K. Sato for useful discussions. H. A. is supported by a Grant-in-Aid for Japan Society for the Promotion of Science (JSPS) Fellows (26-606). R.J.W. 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. H. K. is supported by the Astrobiology Project of the CNSI, NINS (AB261006) and by Grant-in-Aid for Scientific research from JSPS and from the MEXT (No. 25800106). A.S. acknowledges financial support from NWO. D.S. acknowledges financial support from the Netherlands Organisation for Scientific research (NWO) through a Veni fellowship, from FCT through a FCT Investigator Starting Grant and Start-up Grant (IF/01154/2012/CP0189/CT0010) and from FCT grant PEst-OE/FIS/UI2751/2014. M.H. acknowledges financial support by the DFG, in the framework of the DFG Forschergruppe 1254 "Magnetisation of Interstellar and Intergalactic Media: The Prospects of Low-Frequency Radio Observations". G.A.O. acknowledges support by NASA though a Hubble Fellowship grant HST-HF2-51345.001-A awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555. SRON is supported financially by NWO, the Netherlands Organization for Scientific Research. NR 83 TC 8 Z9 8 U1 2 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 OCT PY 2015 VL 582 AR A87 DI 10.1051/0004-6361/201425209 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CU4YT UT WOS:000363538500087 ER PT J AU Alvarado-Gomez, JD Hussain, GAJ Grunhut, J Fares, R Donati, JF Alecian, E Kochukhov, O Oksala, M Morin, J Redfield, S Cohen, O Drake, JJ Jardine, M Matt, S Petit, P Walter, FM AF Alvarado-Gomez, J. D. Hussain, G. A. J. Grunhut, J. Fares, R. Donati, J. -F. Alecian, E. Kochukhov, O. Oksala, M. Morin, J. Redfield, S. Cohen, O. Drake, J. J. Jardine, M. Matt, S. Petit, P. Walter, F. M. TI Activity and magnetic field structure of the Sun-like planet-hosting star HD 1237 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE stars: activity; stars: magnetic field; stars: solar-type; stars: individual: HD 1237 ID RADIAL-VELOCITY VARIATIONS; EXTRASOLAR GIANT PLANETS; MAIN-SEQUENCE STARS; X-RAY-EMISSION; LOW-MASS STARS; T-TAURI; STELLAR CORONAE; EPSILON-ERIDANI; DOPPLER IMAGES; AGE ESTIMATION AB We analyse the magnetic activity characteristics of the planet-hosting Sun-like star, HD 1237, using HARPS spectro-polarimetric time-series data. We find evidence of rotational modulation of the magnetic longitudinal field measurements that is consistent with our ZDI analysis with a period of 7 days. We investigate the effect of customising the LSD mask to the line depths of the observed spectrum and find that it has a minimal effect on the shape of the extracted Stokes V profile but does result in a small increase in the S/N (similar to 7%). We find that using a Milne-Eddington solution to describe the local line profile provides a better fit to the LSD profiles in this slowly rotating star, which also affects the recovered ZDI field distribution. We also introduce a fit-stopping criterion based on the information content (entropy) of the ZDI map solution set. The recovered magnetic field maps show a strong (+90 G) ring-like azimuthal field distribution and a complex radial field dominating at mid latitudes (similar to 45 degrees). Similar magnetic field maps are recovered from data acquired five months apart. Future work will investigate how this surface magnetic field distribution affeccts the coronal magnetic field and extended environment around this planet-hosting star. C1 [Alvarado-Gomez, J. D.; Hussain, G. A. J.; Grunhut, J.] European So Observ, D-85748 Garching, Germany. [Alvarado-Gomez, J. D.] Univ Munich, Univ Sternwarte Munchen, D-81679 Munich, Germany. [Fares, R.] INAF Osservatorio Astrofis Catania, I-95123 Catania, Italy. [Hussain, G. A. J.; Donati, J. -F.; Petit, P.] Univ Toulouse, UPS OMP, Inst Rech Astrophys & Planetol, F-31400 Toulouse, France. [Donati, J. -F.; Petit, P.] CNRS, Inst Rech Astrophys & Planetol, F-31400 Toulouse, France. [Alecian, E.] UJF Grenoble 1, CNRS, INSU, IPAG,UMR 5274, Grenoble, France. [Alecian, E.; Oksala, M.] Univ Paris Diderot, UPMC, CNRS, LESIA,Observ Paris,UMR 8109, F-92190 Meudon, France. [Kochukhov, O.] Uppsala Univ, Dept Phys & Astron, S-75120 Uppsala, Sweden. [Morin, J.] CNRS, UMR 5299, LUPM, F-34095 Montpellier 05, France. [Morin, J.] Univ Montpellier, F-34095 Montpellier 05, France. [Redfield, S.] Wesleyan Univ, Dept Astron, Van Vleck Observ, Middletown, CT 06459 USA. [Cohen, O.; Drake, J. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Jardine, M.] Univ St Andrews, Sch Phys & Astron, SUPA, St Andrews KY16 9SS, Fife, Scotland. [Matt, S.] Univ Exeter, Dept Phys & Astron, Exeter EX4 4SB, Devon, England. [Walter, F. M.] SUNY Stony Brook, Dept Phys & Astron, Stony Brook, NY 11794 USA. RP Alvarado-Gomez, JD (reprint author), European So Observ, Karl Schwarzschild Str 2, D-85748 Garching, Germany. EM jalvarad@eso.org OI Petit, Pascal/0000-0001-7624-9222; Morin, Julien/0000-0002-4996-6901; Alvarado Gomez, Julian David/0000-0001-5052-3473; Redfield, Seth/0000-0003-3786-3486; Cohen, Ofer/0000-0003-3721-0215; Matt, Sean/0000-0001-9590-2274 FU ESO Telescopes at the La Silla Paranal Observatory [089.D-0138] FX Based on observations made with ESO Telescopes at the La Silla Paranal Observatory under programme ID 089.D-0138. NR 89 TC 6 Z9 7 U1 0 U2 0 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD OCT PY 2015 VL 582 AR A38 DI 10.1051/0004-6361/201525771 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CU4YT UT WOS:000363538500038 ER PT J AU Heald, GH Pizzo, RF Orru, E Breton, RP Carbone, D Ferrari, C Hardcastle, MJ Jurusik, W Macario, G Mulcahy, D Rafferty, D Asgekar, A Brentjens, M Fallows, RA Frieswijk, W Toribio, MC Adebahr, B Arts, M Bell, MR Bonafede, A Bray, J Broderick, J Cantwell, T Carroll, P Cendes, Y Clarke, AO Croston, J Daiboo, S de Gasperin, F Gregson, J Harwood, J Hassall, T Heesen, V Horneffer, A van der Horst, AJ Iacobelli, M Jelic, V Jones, D Kant, D Kokotanekov, G Martin, P McKean, JP Morabito, LK Nikiel-Wroczynski, B Offringa, A Pandey, VN Pandey-Pommier, M Pietka, M Pratley, L Riseley, C Rowlinson, A Sabater, J Scaife, AMM Scheers, LHA Sendlinger, K Shulevski, A Sipior, M Sobey, C Stewart, AJ Stroe, A Swinbank, J Tasse, C Trustedt, J Varenius, E van Velzen, S Vilchez, N van Weeren, RJ Wijnholds, S Williams, WL de Bruyn, AG Nijboer, R Wise, M Alexov, A Anderson, J Avruch, IM Beck, R Bell, ME van Bemmel, I Bentum, MJ Bernardi, G Best, P Breitling, F Brouw, WN Bruggen, M Butcher, HR Ciardi, B Conway, JE de Geus, E de Jong, A de Vos, M Deller, A Dettmar, RJ Duscha, S Eisloffel, J Engels, D Falcke, H Fender, R Garrett, MA Griessmeier, J Gunst, AW Hamaker, JP Hessels, JWT Hoeft, M Horandel, J Holties, HA Intema, H Jackson, NJ Jutte, E Karastergiou, A Klijn, WFA Kondratiev, VI Koopmans, LVE Kuniyoshi, M Kuper, G Law, C van Leeuwen, J Loose, M Maat, P Markoff, S McFadden, R McKay-Bukowski, D Mevius, M Miller-Jones, JCA Morganti, R Munk, H Nelles, A Noordam, JE Norden, MJ Paas, H Polatidis, AG Reich, W Renting, A Rottgering, H Schoenmakers, A Schwarz, D Sluman, J Smirnov, O Stappers, BW Steinmetz, M Tagger, M Tang, Y ter Veen, S Thoudam, S Vermeulen, R Vocks, C Vogt, C Wijers, RAMJ Wucknitz, O Yatawatta, S Zarka, P AF Heald, G. H. Pizzo, R. F. Orru, E. Breton, R. P. Carbone, D. Ferrari, C. Hardcastle, M. J. Jurusik, W. Macario, G. Mulcahy, D. Rafferty, D. Asgekar, A. Brentjens, M. Fallows, R. A. Frieswijk, W. Toribio, M. C. Adebahr, B. Arts, M. Bell, M. R. Bonafede, A. Bray, J. Broderick, J. Cantwell, T. Carroll, P. Cendes, Y. Clarke, A. O. Croston, J. Daiboo, S. de Gasperin, F. Gregson, J. Harwood, J. Hassall, T. Heesen, V. Horneffer, A. van der Horst, A. J. Iacobelli, M. Jelic, V. Jones, D. Kant, D. Kokotanekov, G. Martin, P. McKean, J. P. Morabito, L. K. Nikiel-Wroczynski, B. Offringa, A. Pandey, V. N. Pandey-Pommier, M. Pietka, M. Pratley, L. Riseley, C. Rowlinson, A. Sabater, J. Scaife, A. M. M. Scheers, L. H. A. Sendlinger, K. Shulevski, A. Sipior, M. Sobey, C. Stewart, A. J. Stroe, A. Swinbank, J. Tasse, C. Truestedt, J. Varenius, E. van Velzen, S. Vilchez, N. van Weeren, R. J. Wijnholds, S. Williams, W. L. de Bruyn, A. G. Nijboer, R. Wise, M. Alexov, A. Anderson, J. Avruch, I. M. Beck, R. Bell, M. E. van Bemmel, I. Bentum, M. J. Bernardi, G. Best, P. Breitling, F. Brouw, W. N. Brueggen, M. Butcher, H. R. Ciardi, B. Conway, J. E. de Geus, E. de Jong, A. de Vos, M. Deller, A. Dettmar, R. -J. Duscha, S. Eisloeffel, J. Engels, D. Falcke, H. Fender, R. Garrett, M. A. Griessmeier, J. Gunst, A. W. Hamaker, J. P. Hessels, J. W. T. Hoeft, M. Horandel, J. Holties, H. A. Intema, H. Jackson, N. J. Juette, E. Karastergiou, A. Klijn, W. F. A. Kondratiev, V. I. Koopmans, L. V. E. Kuniyoshi, M. Kuper, G. Law, C. van Leeuwen, J. Loose, M. Maat, P. Markoff, S. McFadden, R. McKay-Bukowski, D. Mevius, M. Miller-Jones, J. C. A. Morganti, R. Munk, H. Nelles, A. Noordam, J. E. Norden, M. J. Paas, H. Polatidis, A. G. Reich, W. Renting, A. Rottgering, H. Schoenmakers, A. Schwarz, D. Sluman, J. Smirnov, O. Stappers, B. W. Steinmetz, M. Tagger, M. Tang, Y. ter Veen, S. Thoudam, S. Vermeulen, R. Vocks, C. Vogt, C. Wijers, R. A. M. J. Wucknitz, O. Yatawatta, S. Zarka, P. TI The LOFAR Multifrequency Snapshot Sky Survey (MSSS) I. Survey description and first results SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE surveys; radio continuum: general ID RADIO-SOURCES; EMISSION; FIELD; VIEW; CALIBRATION; PROJECTION; ALGORITHM; IMAGES; GALAXY; ARRAY AB We present the Multifrequency Snapshot Sky Survey (MSSS), the first northern-sky Low Frequency Array (LOFAR) imaging survey. In this introductory paper, we first describe in detail the motivation and design of the survey. Compared to previous radio surveys, MSSS is exceptional due to its intrinsic multifrequency nature providing information about the spectral properties of the detected sources over more than two octaves (from 30 to 160 MHz). The broadband frequency coverage, together with the fast survey speed generated by LOFAR's multibeaming capabilities, make MSSS the first survey of the sort anticipated to be carried out with the forthcoming Square Kilometre Array (SKA). Two of the sixteen frequency bands included in the survey were chosen to exactly overlap the frequency coverage of large-area Very Large Array (VLA) and Giant Metrewave Radio Telescope (GMRT) surveys at 74MHz and 151MHz respectively. The survey performance is illustrated within the MSSS Verification Field (MVF), a region of 100 square degrees centered at (alpha, delta)(J2000) = (15(h), 69 degrees). The MSSS results from the MVF are compared with previous radio survey catalogs. We assess the flux and astrometric uncertainties in the catalog, as well as the completeness and reliability considering our source finding strategy. We determine the 90% completeness levels within the MVF to be 100 mJy at 135 MHz with 108 '' resolution, and 550 mJy at 50 MHz with 166 '' resolution. Images and catalogs for the full survey, expected to contain 150 000-200 000 sources, will be released to a public web server. We outline the plans for the ongoing production of the final survey products, and the ultimate public release of images and source catalogs. C1 [Heald, G. H.; Pizzo, R. F.; Orru, E.; Asgekar, A.; Brentjens, M.; Fallows, R. A.; Frieswijk, W.; Toribio, M. C.; Arts, M.; Harwood, J.; Iacobelli, M.; Jelic, V.; Kant, D.; McKean, J. P.; Offringa, A.; Pandey, V. N.; Sipior, M.; Sobey, C.; Vilchez, N.; Wijnholds, S.; Williams, W. L.; de Bruyn, A. G.; Nijboer, R.; Wise, M.; van Bemmel, I.; Bentum, M. J.; Brouw, W. N.; de Geus, E.; de Jong, A.; de Vos, M.; Deller, A.; Duscha, S.; Falcke, H.; Garrett, M. A.; Gunst, A. W.; Hamaker, J. P.; Hessels, J. W. T.; Holties, H. A.; Klijn, W. F. A.; Kondratiev, V. I.; Kuper, G.; van Leeuwen, J.; Loose, M.; Maat, P.; McFadden, R.; Mevius, M.; Morganti, R.; Munk, H.; Noordam, J. E.; Norden, M. J.; Polatidis, A. G.; Renting, A.; Schoenmakers, A.; Sluman, J.; Tang, Y.; Vermeulen, R.; Vogt, C.; Yatawatta, S.] ASTRON, NL-7990 AA Dwingeloo, Netherlands. [Heald, G. H.; Jelic, V.; McKean, J. P.; Shulevski, A.; de Bruyn, A. G.; Avruch, I. M.; Brouw, W. N.; Koopmans, L. V. E.; Mevius, M.; Morganti, R.] Univ Groningen, Kapteyn Astron Inst, NL-9700 AV Groningen, Netherlands. [Breton, R. P.; Mulcahy, D.; Bray, J.; Broderick, J.; Cantwell, T.; Clarke, A. O.; Croston, J.; Hassall, T.; Heesen, V.; Martin, P.; Pietka, M.; Riseley, C.; Scaife, A. M. M.; Stewart, A. J.] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England. [Carbone, D.; Cendes, Y.; van der Horst, A. J.; Kokotanekov, G.; Swinbank, J.; Hessels, J. W. T.; van Leeuwen, J.; Markoff, S.; Miller-Jones, J. C. A.; Wijers, R. A. M. J.] Univ Amsterdam, Anton Pannekoek Inst, NL-1090 GE Amsterdam, Netherlands. [Ferrari, C.; Macario, G.] Univ Nice Sophia Antipolis, Lab Lagrange, Observ Cote Azur, UMR 7293,CNRS, F-06300 Nice, France. [Hardcastle, M. J.; Harwood, J.] Univ Hertfordshire, Sch Phys Astron & Math, Hatfield AL10 9AB, Herts, England. [Jurusik, W.; Nikiel-Wroczynski, B.] Jagiellonian Univ, Astron Observ, PL-30244 Krakow, Poland. [Mulcahy, D.; Adebahr, B.; Horneffer, A.; Sobey, C.; Beck, R.; Kuniyoshi, M.; Reich, W.; Wucknitz, O.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Rafferty, D.; Bonafede, A.; de Gasperin, F.; Brueggen, M.] Univ Hamburg, Hamburger Sternwarte, D-21029 Hamburg, Germany. [Bell, M. R.; Ciardi, B.] Max Planck Inst Astrophys, D-85748 Garching, Germany. [Broderick, J.; Pietka, M.; Stewart, A. J.; Fender, R.; Karastergiou, A.] Univ Oxford, Astrophys, Oxford OX1 3RH, England. [Carroll, P.] Univ Washington, Dept Astron, Seattle, WA 98195 USA. [Daiboo, S.; Zarka, P.] Univ Paris Diderot, Observ Paris, LESIA, CNRS,UPMC, F-92195 Meudon, France. [Gregson, J.] Open Univ, Dept Phys & Astron, Milton Keynes MK7 6AA, Bucks, England. [Iacobelli, M.; Morabito, L. K.; Stroe, A.; Williams, W. L.; Garrett, M. A.; Intema, H.; Rottgering, H.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [Jones, D.; Falcke, H.; Horandel, J.; Nelles, A.; ter Veen, S.; Thoudam, S.] Radboud Univ Nijmegen, IMAPP, Dept Astrophys, NL-6500 GL Nijmegen, Netherlands. [Pandey-Pommier, M.] Univ Lyon 1, CRAL, Observ Lyon, F-69561 St Genis Laval, France. [Pratley, L.] Victoria Univ Wellington, Sch Chem & Phys Sci, Wellington 6140, New Zealand. [Rowlinson, A.; Bell, M. E.] CSIRO Astron & Space Sci, Epping, NSW 1710, Australia. [Sabater, J.; Best, P.] Univ Edinburgh, IfA, Royal Observ, Edinburgh EH9 3HJ, Midlothian, Scotland. [Scheers, L. H. A.] Ctr Wiskunde & Informat, NL-1090 GB Amsterdam, Netherlands. [Sendlinger, K.; Dettmar, R. -J.; Juette, E.] Ruhr Univ Bochum, Astron Inst, D-44801 Bochum, Germany. [Tasse, C.] Univ Paris Diderot, GEPI, Observ Paris, CNRS, F-92190 Meudon, France. [Tasse, C.; Smirnov, O.] SKA South Africa, ZA-7405 Pinelands, South Africa. [Tasse, C.; Smirnov, O.] Rhodes Univ, Dept Phys & Elect, ZA-6140 Grahamstown, South Africa. [Truestedt, J.] Univ Erlangen Nurnberg, Dr Remeis Sternwarte & ECAP, D-96049 Bamberg, Germany. [Truestedt, J.] Univ Wurzburg, Inst Theoret Phys & Astrophys, D-97074 Wurzburg, Germany. [Varenius, E.; Conway, J. E.] Chalmers, Dept Earth & Space Sci, Onsala Space Observ, S-43992 Onsala, Sweden. [van Velzen, S.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [van Weeren, R. J.; Bernardi, G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Alexov, A.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Anderson, J.] Deutsch GeoForschungsZentrum GFZ, Helmholtz Zentrum Potsdam, Dept Geodesy & Remote Sensing 1, D-14473 Potsdam, Germany. [Avruch, I. M.] SRON Netherlands Insitute Space Res, NL-9700 AV Groningen, Netherlands. [van Bemmel, I.] Joint Inst VLBI Europe, NL-7990 AA Dwingeloo, Netherlands. [Bentum, M. J.] Univ Twente, NL-7522 NB Enschede, Netherlands. [Breitling, F.; Steinmetz, M.; Vocks, C.] Leibniz Inst Astrophys Potsdam AIP, D-14482 Potsdam, Germany. [Butcher, H. R.] Australian Natl Univ, Res Sch Astron & Astrophys, Mt Stromlo Obs, Weston, ACT 2611, Australia. [de Geus, E.] SmarterVision BV, NL-9401 JX Assen, Netherlands. [Eisloeffel, J.; Hoeft, M.] Thuringer Landessternwarte, D-07778 Tautenburg, Germany. [Engels, D.] Hamburger Sternwarte, D-21029 Hamburg, Germany. [Griessmeier, J.; Tagger, M.] Univ Orleans, LPC2E, CNRS, F-45071 Orleans 2, France. [Griessmeier, J.] Univ Orleans, Stn Radioastron Nancay, Observ Paris, CNRS,INSU,USR 704,OSUC, F-18330 Nancay, France. [Intema, H.] Natl Radio Astron Observ, Charlottesville, VA 22903 USA. [Jackson, N. J.; Stappers, B. W.] Univ Manchester, Sch Phys & Astron, Jodrell Bank Ctr Astrophys, Manchester M13 9PL, Lancs, England. [Kondratiev, V. I.] Lebedev Phys Inst, Ctr Astro Space, Moscow 117997, Russia. [Kuniyoshi, M.] Natl Inst Nat Sci, Natl Astron Observ Japan, Mitaka, Tokyo, Japan. [Law, C.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [McKay-Bukowski, D.] Univ Oulu, Sodankyla Geophys Observ, Sodankyla 99600, Finland. [McKay-Bukowski, D.] STFC Rutherford Appleton Lab, Didcot OX11 0QX, Oxon, England. [Miller-Jones, J. C. A.] Curtin Univ, Int Ctr Radio Astron Res, Perth, WA 6845, Australia. [Paas, H.] Univ Groningen, CIT, NL-9712 CP Groningen, Netherlands. [Schwarz, D.] Univ Bielefeld, Fak Phys, D-33501 Bielefeld, Germany. RP Heald, GH (reprint author), ASTRON, Postbus 2, NL-7990 AA Dwingeloo, Netherlands. EM heald@astron.nl RI Miller-Jones, James/B-2411-2013; Harwood, Jeremy/D-9032-2016; Intema, Huib/D-1438-2012; Kondratiev, Vladislav/N-1105-2015; Jelic, Vibor/B-2938-2014; Breton, Rene/A-5536-2017; Yatawatta, Sarod/E-6037-2013; OI de Gasperin, Francesco/0000-0003-4439-2627; Miller-Jones, James/0000-0003-3124-2814; Harwood, Jeremy/0000-0003-0251-6126; Intema, Huib/0000-0002-5880-2730; Kondratiev, Vladislav/0000-0001-8864-7471; Jelic, Vibor/0000-0002-6034-8610; Breton, Rene/0000-0001-8522-4983; Cantwell, Therese/0000-0001-9159-6599; Wijers, Ralph/0000-0002-3101-1808; Yatawatta, Sarod/0000-0001-5619-4017; Riseley, Christopher/0000-0002-3369-1085; Sabater, Jose/0000-0003-1149-6294; Varenius, Eskil/0000-0002-3248-9467; Deller, Adam/0000-0001-9434-3837; van Weeren, Reinout/0000-0002-0587-1660; Shulevski, Aleksandar/0000-0002-1827-0469; Hardcastle, Martin/0000-0003-4223-1117 FU BQR program of Observatoire de la Cote d'Azur; French A.S. SKA-LOFAR; Agence Nationale de la Recherche [ANR-09-JCJC-0001-01]; European Research Council [247295, 267697]; DFG Research Unit [FOR1254] FX We thank the anonymous referee for comments that have improved this paper. 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. We acknowledge financial support from the BQR program of Observatoire de la Cote d'Azur and from the French A.S. SKA-LOFAR. C.F. and G.M. acknowledge financial support by the "Agence Nationale de la Recherche" through grant ANR-09-JCJC-0001-01. D.C., Y.C., A.J.v.d.H., A.R., and J.S. acknowledge support from the European Research Council via Advanced Investigator Grant no. 247295 (PI: R. Wijers). R.P.B., J.B., T.H., A.J.S., M.P., and R.F. were funded by a European Research Council Advanced Grant 267697 "4 Pi Sky: Extreme Astrophysics with Revolutionary Radio Telescopes" (PI: R. Fender). D.M., B.A., M.R.B., A.B., F.d.G., A.H., M.I., K.S., and C.S. were supported by DFG Research Unit FOR1254 "Magnetisation of Interstellar and Intergalactic Media: The Prospects of Low-Frequency Radio Observations". NR 47 TC 31 Z9 31 U1 1 U2 8 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD OCT PY 2015 VL 582 AR A123 DI 10.1051/0004-6361/201425210 PG 22 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CU4YT UT WOS:000363538500123 ER PT J AU Burkhart, B Lee, MY Murray, CE Stanimirovic, S AF Burkhart, Blakesley Lee, Min-Young Murray, Claire E. Stanimirovic, Snezana TI THE LOGNORMAL PROBABILITY DISTRIBUTION FUNCTION OF THE PERSEUS MOLECULAR CLOUD: A COMPARISON OF HI AND DUST SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE dust, extinction; galaxies: star formation; magnetohydrodynamics (MHD) ID TURBULENT MAGNETIZED CLOUDS; COLUMN DENSITY DISTRIBUTION; STAR-FORMATION; INTERSTELLAR TURBULENCE; LINE SURVEY; TRANSITION; FLOWS; II.; I. AB The shape of the probability distribution function (PDF) of molecular clouds is an important ingredient for modern theories of star formation and turbulence. Recently, several studies have pointed out observational difficulties with constraining the low column density (i.e., A(V) < 1) PDF using dust tracers. In order to constrain the shape and properties of the low column density PDF, we investigate the PDF of multiphase atomic gas in the Perseus molecular cloud using opacity-corrected GALFA-HI data and compare the PDF shape and properties to the total gas PDF and the N(H-2) PDF. We find that the shape of the PDF in the atomic medium of Perseus is well described by a lognormal distribution and not by a power-law or bimodal distribution. The peak of the atomic gas PDF in and around Perseus lies at the HI-H-2 transition column density for this cloud, past which the N(H-2) PDF takes on a power-law form. We find that the PDF of the atomic gas is narrow, and at column densities larger than the HI-H-2 transition, the HI rapidly depletes, suggesting that the HI PDF may be used to find the HI-H-2 transition column density. We also calculate the sonic Mach number of the atomic gas by using HI absorption line data, which yield a median value of M-s = 4.0 for the CNM, while the HI emission PDF, which traces both the WNM and CNM, has a width more consistent with transonic turbulence. C1 [Burkhart, Blakesley] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Lee, Min-Young] CEA IRFU Serv Astrophys, Lab AIM, F-91191 Gif Sur Yvette, France. [Murray, Claire E.; Stanimirovic, Snezana] Univ Wisconsin, Dept Astron, Madison, WI 53706 USA. RP Burkhart, B (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. OI Lee, Min-Young/0000-0002-9888-0784 FU NASA Einstein Postdoctoral Fellowship; SYMPATICO grant from the French Agence Nationale de la Reserche [ANR-11-BS56-0023]; DIM ACAV; NSF Graduate Research Fellowship; NSF Early Career Development (CAREER) Award [AST-1056780] FX B.B. is grateful for valuable discussions with Simon Bihr, David Collins, Alyssa Goodman, Nia Imara, Eric Keto, Charlie Lada, and Phil Myers. The research of B. B. is supported by the NASA Einstein Postdoctoral Fellowship. M.-Y.L. is supported by the SYMPATICO grant (ANR-11-BS56-0023) from the French Agence Nationale de la Reserche and the DIM ACAV. C.E.M acknowledges support from the NSF Graduate Research Fellowship. S.S. acknowledges support from the NSF Early Career Development (CAREER) Award AST-1056780. NR 42 TC 0 Z9 0 U1 2 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 OCT 1 PY 2015 VL 811 IS 2 AR L28 DI 10.1088/2041-8205/811/2/L28 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CV7TR UT WOS:000364478600014 ER PT J AU Guillochon, J Loeb, A AF Guillochon, James Loeb, Abraham TI SETI VIA LEAKAGE FROM LIGHT SAILS IN EXOPLANETARY SYSTEMS SO Astrophysical Journal Letters LA English DT Article DE extraterrestrial intelligence; space vehicles ID OPTIMIZED INTERSTELLAR BEACONS; SEARCH AB The primary challenge of rocket propulsion is the burden of needing to accelerate the spacecraft's own fuel, resulting in only a logarithmic gain in maximum speed as propellant is added to the spacecraft. Light sails offer an attractive alternative in which fuel is not carried by the spacecraft, with acceleration being provided by an external source of light. By artificially illuminating the spacecraft with beamed radiation, speeds are only limited by the area of the sail, heat resistance of its material, and power use of the accelerating apparatus. In this paper, we show that leakage from a light sail propulsion apparatus in operation around a solar system analogue would be detectable. To demonstrate this, we model the launch and arrival of a microwave beam-driven light sail constructed for transit between planets in orbit around a single star, and find an optimal beam frequency on the order of tens of GHz. Leakage from these beams yields transients with flux densities of Jy and durations of tens of seconds at 100 pc. Because most travel within a planetary system would be conducted between the habitable worlds within that system, multiply transiting exoplanetary systems offer the greatest chance of detection, especially when the planets are in projected conjunction as viewed from Earth. If interplanetary travel via beam-driven light sails is commonly employed in our galaxy, this activity could be revealed by radio follow-up of nearby transiting exoplanetary systems. The expected signal properties define a new strategy in the search for extraterrestrial intelligence (SETI). C1 [Guillochon, James; Loeb, Abraham] Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, Cambridge, MA 02138 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; aloeb@cfa.harvard.edu OI Guillochon, James/0000-0002-9809-8215 FU Einstein grant [PF3-140108] FX We thank J. Benford, J. Wright, and the anonymous referee for comments. This work was supported by Einstein grant PF3-140108 (J. G.). NR 15 TC 5 Z9 5 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 OCT 1 PY 2015 VL 811 IS 2 AR L20 DI 10.1088/2041-8205/811/2/L20 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CV7TR UT WOS:000364478600006 ER PT J AU Saucier, JR Sanchez, C Carling, MD AF Saucier, Jacob R. Sanchez, Cesar Carling, Matthew D. TI Patterns of genetic and morphological divergence reveal a species complex in the Plain Wren (Cantorchilus modestus) SO AUK LA English DT Article DE Central America; historical biogeography; mitochondrial DNA; morphometrics; phylogeography; plumage ID AMERICAN BIOTIC INTERCHANGE; MITOCHONDRIAL-DNA; PHYLOGEOGRAPHY; SPECIATION; ISTHMUS; HISTORY; BIRDS; POPULATION; DISPERSAL; BEHAVIOR AB We used morphometrics, plumage color, and mitochondrial DNA to reconstruct the phylogeography of the Plain Wren (Cantorchilus modestus), an abundant bird species of low to middle elevations throughout Central America. Sampling the full geographic range of C. modestus, we uncovered significant phenotypic structure in size, shape, and plumage color that mirrored deep genetic divergences in mitochondrial DNA. This structure was mostly concordant with the 3 most broadly recognized subspecies of Plain Wren (C. m. modestus, C. m. zeledoni, and C. m. elutus), but a potentially undescribed taxon exists in the highlands of Central Belize. We also found evidence of a cryptic phylogeographic break on the Pacific Slope of Costa Rica, between the southernmost populations and the widespread northern populations. This latter discovery likely represents a significant expansion of the known range of the traditionally Panamanian subspecies C. m. elutus, corresponding to a transition between major ecoregions. Topology tests suggested that northern populations of the nominate taxon likely dispersed south into Lower Central America, with subsequent isolation and diversification. We also explored the possible role of adaptation in the phenotypic divergence of the "Canebrake Wren" (C. m. zeledoni) as a result of isolation in the more humid environments of the Caribbean Slope. Our data and analyses suggest that the Plain Wren may consist of multiple biological species that have been diverging since geophysical upheavals in the lower half of Central America approximately 2-3 mya. C1 [Saucier, Jacob R.; Carling, Matthew D.] Univ Wyoming, Dept Zool & Physiol, Laramie, WY 82071 USA. [Sanchez, Cesar] Louisiana State Univ, Museum Nat Sci, Baton Rouge, LA 70803 USA. [Sanchez, Cesar] Louisiana State Univ, Dept Biol Sci, Baton Rouge, LA 70803 USA. RP Saucier, JR (reprint author), Natl Museum Nat Hist, Smithsonian Inst, Div Birds, Washington, DC 20560 USA. EM saucierj@si.edu; mcarling@uwyo.edu FU University of Wyoming FX Our work was funded by the University of Wyoming. NR 79 TC 1 Z9 1 U1 1 U2 7 PU AMER ORNITHOLOGISTS UNION PI LAWRENCE PA ORNITHOLOGICAL SOC NORTH AMER PO BOX 1897, LAWRENCE, KS 66044-8897 USA SN 0004-8038 EI 1938-4254 J9 AUK JI AUK PD OCT PY 2015 VL 132 IS 4 BP 795 EP 807 DI 10.1642/AUK-15-8.1 PG 13 WC Ornithology SC Zoology GA CV8EY UT WOS:000364514600003 ER PT J AU Peele, AM Marra, PM Sillett, TS Sherry, TW AF Peele, Ashley M. Marra, Peter M. Sillett, T. Scott Sherry, Thomas W. TI Combining survey methods to estimate abundance and transience of migratory birds among tropical nonbreeding habitats SO AUK LA English DT Article DE density; distance sampling; mark-recapture; migratory species; nonbreeding season; survey methods; territory mapping; transients ID CAPTURE-RECAPTURE MODELS; REDSTARTS SETOPHAGA-RUTICILLA; POINT-COUNT SURVEYS; N-MIXTURE MODELS; AMERICAN REDSTARTS; LONG-DISTANCE; POPULATION-SIZE; VENEZUELAN MANGROVES; REPLICATED COUNTS; MIGRANT SONGBIRD AB Estimating population abundance for territorial species is challenging because individuals often differ in behavior (e.g., transience, multiterritoriality), and thus in detectability. How well prevailing methods detect and quantify individuals using multiple strategies is rarely addressed. In our effort to efficiently quantify avian abundance and transience among diverse nonbreeding habitats, we combined 'unmarked' (distance sampling) with traditional 'marked' (territory mapping) survey methods using a migratory passerine, the American Redstart (Setophaga ruticilla), wintering in 3 habitats in Jamaica from 2010 to 2012. We predicted that the 'unmarked' survey method would detect not only all known (marked) territorial individuals, but also individuals that were transient or nonterritorial in the same habitats. Comparisons of abundance estimates generated by our best distance sampling (unmarked) model with territory mapping data identified high proportions of transient individuals (up to 50%) in 2 habitats, coastal dry scrub and mangrove, and virtually none in the third habitat, higher-elevation wet limestone forest. Documenting so many nonterritorial individuals, disproportionately weighted toward females and yearlings, in some habitat-year combinations prompts questions of what conditions favor transience and what role these individuals play in population processes. Our results illustrate how unmarked and marked survey methods can be used jointly to establish the number and identity of transients from neighboring areas. The unmarked survey method was sufficient for estimating population size among different habitats, but marked survey methods were necessary to identify and quantify transient individuals. Combined, these methods provide a powerful tool for assessing the range and variation of space-use strategies deployed by nonbreeding individuals. C1 [Peele, Ashley M.; Sherry, Thomas W.] Tulane Univ, Dept Ecol & Evolutionary Biol, New Orleans, LA 70118 USA. [Marra, Peter M.; Sillett, T. Scott] Natl Zool Pk, Smithsonian Conservat Biol Inst, Migratory Bird Ctr, Washington, DC USA. RP Peele, AM (reprint author), Tulane Univ, Dept Ecol & Evolutionary Biol, New Orleans, LA 70118 USA. EM ashpeele25@gmail.com FU National Science Foundation [0717338, 0649679, 0717243, 1242588] FX Our research was supported financially by National Science Foundation grants to P.P.M. and T.S.S. (0717338, 0649679) and T.W.S. (0717243, 1242588). None of our funders had any influence on the content of the submitted or published manuscript, nor required approval of the final manuscript to be published. NR 63 TC 0 Z9 0 U1 6 U2 21 PU AMER ORNITHOLOGISTS UNION PI LAWRENCE PA ORNITHOLOGICAL SOC NORTH AMER PO BOX 1897, LAWRENCE, KS 66044-8897 USA SN 0004-8038 EI 1938-4254 J9 AUK JI AUK PD OCT PY 2015 VL 132 IS 4 BP 926 EP 937 DI 10.1642/AUK-14-282.1 PG 12 WC Ornithology SC Zoology GA CV8EY UT WOS:000364514600014 ER PT J AU Peterson, AT Moyle, RG Lei, FM Campillo, LC Hosner, PA Klicka, LB Lim, HC Nyari, AS Qu, YH Reddy, S Sheldon, FH Zou, FS AF Peterson, A. Townsend Moyle, Robert G. Lei, Fumin Campillo, Luke C. Hosner, Peter A. Klicka, Luke B. Lim, Haw C. Nyari, Arpad S. Qu, Yanhua Reddy, Sushma Sheldon, Frederick H. Zou, Fasheng TI Avian evolution and speciation in the Southeast Asian tropics SO Current Zoology LA English DT Editorial Material ID HISTORICAL DIVERSIFICATION; GENETIC-DIVERGENCE; PLEISTOCENE; POPULATIONS; DEMOGRAPHY; PATTERNS; HIMALAYA; DRIVERS; COMPLEX; MARKERS C1 [Peterson, A. Townsend; Moyle, Robert G.; Campillo, Luke C.; Hosner, Peter A.; Klicka, Luke B.] Univ Kansas, Biodivers Inst, Lawrence, KS 66045 USA. [Lei, Fumin; Qu, Yanhua] Chinese Acad Sci, Key Lab Zool Systemat & Evolut, Beijing 100101, Peoples R China. [Hosner, Peter A.] Univ Florida, Dept Biol, Gainesville, FL 32611 USA. [Lim, Haw C.] Smithsonian Inst, Dept Vertebrate Zool, Washington, DC 20560 USA. [Nyari, Arpad S.] Oklahoma State Univ, Dept Integrat Biol, Stillwater, OK 74078 USA. [Reddy, Sushma] Loyola Univ, Dept Biol, Chicago, IL 60660 USA. [Sheldon, Frederick H.] Louisiana State Univ, Museum Nat Sci, Baton Rouge, LA 70803 USA. [Sheldon, Frederick H.] Louisiana State Univ, Dept Biol Sci, Baton Rouge, LA 70803 USA. [Zou, Fasheng] Guangdong Entomol Inst, Guangzhou 510260, Guangdong, Peoples R China. RP Peterson, AT (reprint author), Univ Kansas, Biodivers Inst, Lawrence, KS 66045 USA. EM town@ku.edu; moyle@ku.edu; leifm@ioz.ac.cn NR 27 TC 1 Z9 1 U1 2 U2 16 PU CURRENT ZOOLOGY PI BEIJING PA CHINESE ACAD SCIENCES, INST ZOOLOGY, BEICHEN XILU, CHAOYANG DISTRICT, BEIJING, 100101, PEOPLES R CHINA SN 1674-5507 J9 CURR ZOOL JI Curr. Zool. PD OCT PY 2015 VL 61 IS 5 BP 898 EP 900 PG 3 WC Zoology SC Zoology GA CV6VI UT WOS:000364409200011 ER PT J AU Lim, HC Zou, FS Sheldon, FH AF Lim, Haw Chuan Zou, Fasheng Sheldon, Frederick H. TI Genetic differentiation in two widespread, open-forest bird species of Southeast Asia (Copsychus saularis and Megalaima haemacephala): Insights from ecological niche modeling SO CURRENT ZOOLOGY LA English DT Article DE Barbet; Indo-Burma; Malay Archipelago; Magpie-robin; Phylogeography; Species distribution modeling ID AVES TURDIDAE COPSYCHUS; HISTORICAL BIOGEOGRAPHY; RAIN-FORESTS; SEA LEVELS; CLIMATE; EVOLUTION; PHYLOGEOGRAPHY; DISTRIBUTIONS; CONSERVATISM; DISPERSAL AB Ecological niche modeling has emerged as an useful tool in the investigation of the phylogeographic histories of species or communities in a region. The high biodiversity (oftentimes cryptic), and complex geography and geological history of Southeast Asia particularly call for multipronged approaches in phylogeographic investigations. Past studies have focused on taxa that are associated with lowland rainforests, which is the dominant natural vegetation type. Here, we combine published phylogenetic data, ecological niche modeling and paleo-climate models to reveal potential drivers of divergence in two open-forest bird species, the oriental magpie-robin Copsychus saularis and Coppersmith barbet Megalaima haemacephala. In spite of broad overlap in current distributions, there are subtle differences in their climatic niches, which result in different responses to past climatic changes. For C. saularis, both Last Glacial Maximum climate models indicated that the entire Sundaland was climatically suitable, while phylogenetic analyses found divergent eastern and western Sundaland lineages. We thus postulate that this genetic divergence was a result of past separations of coastal habitats into eastern and western portions due to the emergence of Sunda shelf as sea-level fell. The current separation of morphological subspecies in Borneo is maintained by low climatic suitability (high annual rainfall) in certain regions. The extirpation of M. haemacephala from Borneo and southern Malay Peninsula might have been driven by unsuitable conditions (high temperature seasonality) in central Sundaland and/or the lack of open woodlands. Our study shows that ecological niche modeling adds a powerful dimension to our attempt to understand lineage evolution in space [Current Zoology 61 (5): 922-934, 2015]. C1 [Lim, Haw Chuan] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA. [Zou, Fasheng] Guangdong Entomol Inst, Guangzhou 510260, Guangdong, Peoples R China. [Sheldon, Frederick H.] Louisiana State Univ, Museum Nat Sci, Baton Rouge, LA 70803 USA. [Sheldon, Frederick H.] Louisiana State Univ, Dept Biol Sci, Baton Rouge, LA 70803 USA. RP Lim, HC (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA. EM limhc@si.edu FU Smithsonian Institution's Molecular Evolution Postdoctoral Fellowship FX We thank Fumin Lei, Robert Moyle and A. Townsend Peterson for their kind invitation to publish our findings in this special issue of Current Zoology. We thank Jerome Fuchs for sharing information on the provenance of one C. saularis sample. HCL is currently supported by Smithsonian Institution's Molecular Evolution Postdoctoral Fellowship. A. Townsend Peterson provided very useful comments that improved the manuscript. NR 61 TC 2 Z9 2 U1 3 U2 10 PU CURRENT ZOOLOGY PI BEIJING PA CHINESE ACAD SCIENCES, INST ZOOLOGY, BEICHEN XILU, CHAOYANG DISTRICT, BEIJING, 100101, PEOPLES R CHINA SN 1674-5507 J9 CURR ZOOL JI Curr. Zool. PD OCT PY 2015 VL 61 IS 5 BP 922 EP 934 PG 13 WC Zoology SC Zoology GA CV6VI UT WOS:000364409200014 ER PT J AU Lovelock, CE Simpson, LT Duckett, LJ Feller, IC AF Lovelock, Catherine E. Simpson, Lorae T. Duckett, Lisa J. Feller, Ilka C. TI Carbon Budgets for Caribbean Mangrove Forests of Varying Structure and with Phosphorus Enrichment SO Forests LA English DT Article DE Rhizophora mangle; respiration; fertilization; carbon burial; Belize ID RISING SEA-LEVEL; RHIZOPHORA-MANGLE; SOIL RESPIRATION; TWIN-CAYS; NUTRIENT ENRICHMENT; ORGANIC-CARBON; NITROGEN; BELIZE; GROWTH; ECOSYSTEMS AB There are few detailed carbon (C) budgets of mangrove forests, yet these are important for understanding C sequestration in mangrove forests, how they support the productivity of the coast and their vulnerability to environmental change. Here, we develop C budgets for mangroves on the islands of Twin Cays, Belize. We consider seaward fringing forests and interior scrub forests that have been fertilized with phosphorus (P), which severely limits growth of trees in the scrub forests. We found that respiration of the aboveground biomass accounted for 60%-80% of the fixed C and that respiration of the canopy and aboveground roots were important components of respiration. Soil respiration accounted for only 7%-11% of total gross primary production (GPP) while burial of C in soils was similar to 4% of GPP. Respiration by roots can account for the majority of soil respiration in fringing forests, while microbial processes may account 80% of respiration in scrub forests. Fertilization of scrub forests with P enhanced GPP but the proportion of C buried declined to similar to 2% of GPP. Net ecosystem production was 17%-27% of GPP similar to that reported for other mangrove forests. Carbon isotope signatures of adjacent seagrass suggest that dissolved C from mangroves is exported into the adjacent ecosystems. Our data indicate that C budgets can vary among mangrove forest types and with nutrient enrichment and that low productivity mangroves provide a disproportionate share of exported C. C1 [Lovelock, Catherine E.] Univ Queensland, Sch Biol Sci, St Lucia, Qld 5072, Australia. [Simpson, Lorae T.; Duckett, Lisa J.; Feller, Ilka C.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. [Simpson, Lorae T.] Smithsonian Marine Stn Ft Pierce, Ft Pierce, FL 34949 USA. RP Lovelock, CE (reprint author), Univ Queensland, Sch Biol Sci, St Lucia, Qld 5072, Australia. EM c.lovelock@uq.edu.au; simpsonl@si.edu; duckettl@si.edu; felleri@si.edu RI Lovelock, Catherine/G-7370-2012; OI Lovelock, Catherine/0000-0002-2219-6855; Feller, Ilka/0000-0002-6391-1608 FU National Science Foundation [DEB-9981535]; Smithsonian Institution's Marine Science Network; Australian Research Council [DP0774491, DP0986179, DP1096749, FS100100024]; Marine and Coastal Carbon Biogeochemistry Cluster FX We thank Anne Chamberlain, Rainer Feller, the participants of the Mangrove Biocomplexity project and the staff of the Carrie Bow Cay Research Station and Pelican Beach Resort. This research was funded by the National Science Foundation (DEB-9981535) and the Smithsonian Institution's Marine Science Network. We thank the Australian Research Council (awards DP0774491, DP0986179, DP1096749 and FS100100024) and the Marine and Coastal Carbon Biogeochemistry Cluster for their support. NR 78 TC 1 Z9 1 U1 7 U2 47 PU MDPI AG PI BASEL PA POSTFACH, CH-4005 BASEL, SWITZERLAND SN 1999-4907 J9 FORESTS JI Forests PD OCT PY 2015 VL 6 IS 10 BP 3528 EP 3546 DI 10.3390/f6103528 PG 19 WC Forestry SC Forestry GA CV4IQ UT WOS:000364230800009 ER PT J AU Craddock, RA Tooth, S Zimbelman, JR Wilson, SA Maxwell, TA Kling, C AF Craddock, Robert A. Tooth, Stephen Zimbelman, James R. Wilson, Sharon A. Maxwell, Ted A. Kling, Corbin TI Temporal observations of a linear sand dune in the Simpson Desert, central Australia: Testing models for dune formation on planetary surfaces SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article ID LONGITUDINAL DUNES; LATERAL MIGRATION; STRZELECKI DESERT; CASSINI RADAR; WIND-RIFT; TITAN; TRANSPORT; DYNAMICS; RECONNAISSANCE; LANDSCAPE AB Linear dunes are the most common dune form found on planetary surfaces, yet questions remain about their formation. Temporal observations of a linear dune located in the Simpson Desert of central Australia were made to monitor dune movement and to test competing hypotheses regarding linear dune formation. Our observations were collected on three separate occasions from 2006 to 2014. Rebar stakes were placed in a gridded pattern so that multiple measurements of sand thickness, GPS surveys, and photographs could be taken at the same locations over time. We observed widespread reworking of sand on and around the dune crest, with sand accumulation locally exceeding a meter between surveys. Overall, the height of the dune crest increased by several centimeters. We also observed fluctuations in the sand cover in the adjacent swales that often exceeded 2-3cm between surveys, yet we did not observe any appreciable changes in the position of the dune's downwind terminus. Weather data indicate that the effective sand-transporting winds in the Simpson are widely unimodal. Net sediment flux (resultant drift direction) is toward the north-northwest, locally at an oblique angle to dune orientation. Collectively, our results suggest that the linear dune is actively maintained by vertical accretion. The implications from our observations are that linear dunes on other planetary surfaces could form in wind regimes that are widely unimodal, even where the resultant drift direction is locally oblique to dune orientation. In particular, such findings may provide support for global circulation models of Titan. C1 [Craddock, Robert A.; Zimbelman, James R.; Wilson, Sharon A.; Maxwell, Ted A.] Smithsonian Inst, Natl Air & Space Museum, Ctr Earth & Planetary Studies, Washington, DC 20560 USA. [Tooth, Stephen] Aberystwyth Univ, Dept Geog & Earth Sci, Aberystwyth, Dyfed, Wales. [Kling, Corbin] Univ Georgia, Dept Geol, Athens, GA 30602 USA. RP Craddock, RA (reprint author), Smithsonian Inst, Natl Air & Space Museum, Ctr Earth & Planetary Studies, Washington, DC 20560 USA. EM craddockb@si.edu FU Smithsonian Institution's George F. Becker Endowment; NASA's Mars Data Analysis Program [NAG5-12180] FX GPS survey data and documentary photographs can be obtained by contacting Bob Craddock (craddockb@si.edu). This research was supported through multiple sources over the years, including grants from the Smithsonian Institution's George F. Becker Endowment and NASA's Mars Data Analysis Program (NAG5-12180). We thank Jani Radebaugh and an anonymous reviewer for their cogent and thoughtful comments that greatly improved our original manuscript. NR 67 TC 0 Z9 0 U1 4 U2 6 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9097 EI 2169-9100 J9 J GEOPHYS RES-PLANET JI J. Geophys. Res.-Planets PD OCT PY 2015 VL 120 IS 10 BP 1736 EP 1750 DI 10.1002/2015JE004892 PG 15 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA CW1YI UT WOS:000364787600008 ER PT J AU Murphy, NA Parnell, CE Haynes, AL AF Murphy, Nicholas A. Parnell, Clare E. Haynes, Andrew L. TI The appearance, motion, and disappearance of three-dimensional magnetic null points SO PHYSICS OF PLASMAS LA English DT Article ID SLIP-RUNNING RECONNECTION; SOLAR-FLARES; TOPOLOGICAL BEHAVIOR; CURRENT SHEETS; NEUTRAL LINE; 3 DIMENSIONS; FIELD LINES; SEPARATORS; PLASMAS; CORONA AB While theoretical models and simulations of magnetic reconnection often assume symmetry such that the magnetic null point when present is co-located with a flow stagnation point, the introduction of asymmetry typically leads to non-ideal flows across the null point. To understand this behavior, we present exact expressions for the motion of three-dimensional linear null points. The most general expression shows that linear null points move in the direction along which the magnetic field and its time derivative are antiparallel. Null point motion in resistive magnetohy-drodynamics results from advection by the bulk plasma flow and resistive diffusion of the magnetic field, which allows non-ideal flows across topological boundaries. Null point motion is described intrinsically by parameters evaluated locally; however, global dynamics help set the local conditions at the null point. During a bifurcation of a degenerate null point into a null-null pair or the reverse, the instantaneous velocity of separation or convergence of the null-null pair will typically be infinite along the null space of the Jacobian matrix of the magnetic field, but with finite components in the directions orthogonal to the null space. Not all bifurcating null-null pairs are connected by a separator. Furthermore, except under special circumstances, there will not exist a straight line separator connecting a bifurcating null-null pair. The motion of separators cannot be described using solely local parameters because the identification of a particular field line as a separator may change as a result of non-ideal behavior elsewhere along the field line. (C) 2015 Author(s). C1 [Murphy, Nicholas A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Parnell, Clare E.; Haynes, Andrew L.] Univ St Andrews, Sch Math & Stat, St Andrews KY16 9SS, Fife, Scotland. RP Murphy, NA (reprint author), Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. EM namurphy@cfa.harvard.edu OI Murphy, Nicholas/0000-0001-6628-8033 FU NASA [NNX11AB61G, NNX12AB25G, NNX15AF43G, NNM07AB07C]; NSF [AGS-1156076, AGS-1358342]; St Andrews STFC consolidated grant FX The authors thank A. Aggarwal, A. Bhattacharjee, A. Boozer, P. Cassak, J. Dorelli, T. Forbes, L. Guo, Y.-M. Huang, J. Lin, V. Lukin, M. Oka, E. Priest, J. Raymond, K. Reeves, C. Shen, V. Titov, D. Wendel, and E. Zweibel for helpful discussions. The authors thank A. Wilmot-Smith and D. Pontin for a discussion that helped elucidate why the motion of separators cannot be described locally. N.A.M. acknowledges the support from NASA grants NNX11AB61G, NNX12AB25G, and NNX15AF43G; NASA contract NNM07AB07C; and NSF SHINE grants AGS-1156076 and AGS-1358342 to SAO. C. E. P. acknowledges support from the St Andrews 2013 STFC consolidated grant. This research has made use of NASA's Astrophysics Data System Bibliographic Services. The authors thank the journal for publishing a manuscript containing only null results. NR 87 TC 2 Z9 2 U1 2 U2 7 PU AMER INST PHYSICS PI MELVILLE PA 1305 WALT WHITMAN RD, STE 300, MELVILLE, NY 11747-4501 USA SN 1070-664X EI 1089-7674 J9 PHYS PLASMAS JI Phys. Plasmas PD OCT PY 2015 VL 22 IS 10 AR 102117 DI 10.1063/1.4934929 PG 9 WC Physics, Fluids & Plasmas SC Physics GA CV6TL UT WOS:000364403600033 ER PT J AU Dandois, JP Olano, M Ellis, EC AF Dandois, Jonathan P. Olano, Marc Ellis, Erle C. TI Optimal Altitude, Overlap, and Weather Conditions for Computer Vision UAV Estimates of Forest Structure SO REMOTE SENSING LA English DT Article DE Ecosynth; UAV; SFM; computer vision; canopy height; point cloud; optimal ID UNMANNED AERIAL VEHICLE; FROM-MOTION PHOTOGRAMMETRY; POINT CLOUDS; CANOPY SURFACE; LOW-COST; VEGETATION; FEATURES; IMAGERY; CAMERA; BIODIVERSITY AB Ecological remote sensing is being transformed by three-dimensional (3D), multispectral measurements of forest canopies by unmanned aerial vehicles (UAV) and computer vision structure from motion (SFM) algorithms. Yet applications of this technology have out-paced understanding of the relationship between collection method and data quality. Here, UAV-SFM remote sensing was used to produce 3D multispectral point clouds of Temperate Deciduous forests at different levels of UAV altitude, image overlap, weather, and image processing. Error in canopy height estimates was explained by the alignment of the canopy height model to the digital terrain model (R-2 = 0.81) due to differences in lighting and image overlap. Accounting for this, no significant differences were observed in height error at different levels of lighting, altitude, and side overlap. Overall, accurate estimates of canopy height compared to field measurements (R-2 = 0.86, RMSE = 3.6 m) and LIDAR (R-2 = 0.99, RMSE = 3.0 m) were obtained under optimal conditions of clear lighting and high image overlap (>80%). Variation in point cloud quality appeared related to the behavior of SFM image features'. Future research should consider the role of image features as the fundamental unit of SFM remote sensing, akin to the pixel of optical imaging and the laser pulse of LIDAR. C1 [Dandois, Jonathan P.; Ellis, Erle C.] Univ Maryland Baltimore Cty, Dept Geog & Environm Syst, Baltimore, MD 21250 USA. [Dandois, Jonathan P.] Smithsonian Trop Res Inst, Ancon 084303092, Panama. [Olano, Marc] Univ Maryland Baltimore Cty, Comp Sci & Elect Engn, Baltimore, MD 21250 USA. RP Dandois, JP (reprint author), Univ Maryland Baltimore Cty, Dept Geog & Environm Syst, 1000 Hilltop Circle, Baltimore, MD 21250 USA. EM jon.dandois@gmail.com; olano@umbc.edu; ece@umbc.edu FU US National Science Foundation [DBI 1147089]; NSF IGERT grant [0549469] FX This material is based upon work supported by the US National Science Foundation under Grant DBI 1147089 awarded March 1, 2012 to Erle Ellis and Marc Olano. Jonathan Dandois was supported by NSF IGERT grant 0549469, PI Claire Welty and hosted by CUERE (Center for Urban Environmental Research and Education). The authors thank the Ecosynth team: Dana Boswell Nadwodny, Stephen Zidek and Lindsay Digman for their help with UAV data collection as well as Yu Wang, Yingying Zhu, Will Bierbower, and Terrence Seneschal for their help with Ecosynther and Ecosynth processing. Graphical abstract UAV image credit: J. Leighton Reid. Data and information on Ecosynth are available online at http://ecosynth.org/. NR 73 TC 10 Z9 10 U1 15 U2 44 PU MDPI AG PI BASEL PA ST ALBAN-ANLAGE 66, CH-4052 BASEL, SWITZERLAND SN 2072-4292 J9 REMOTE SENS-BASEL JI Remote Sens. PD OCT PY 2015 VL 7 IS 10 BP 13895 EP 13920 DI 10.3390/rs71013895 PG 26 WC Remote Sensing SC Remote Sensing GA CV5RK UT WOS:000364328600061 ER PT J AU McCoy, MW Wheat, SK Warkentin, KM Vonesh, JR AF McCoy, Michael W. Wheat, Stefan K. Warkentin, Karen M. Vonesh, James R. TI Risk assessment based on indirect predation cues: revisiting fine-grained variation SO ECOLOGY AND EVOLUTION LA English DT Article DE Inducible defense; phenotypic plasticity; predation; tadpole ID CONSPECIFIC DENSITY; OPPOSITE SHIFTS; PREY DEFENSES; ALARM CUES; PLASTICITY; KAIROMONES; TADPOLES; LARVAL; SIZE AB To adaptively express inducible defenses, prey must gauge risk based on indirect cues of predation. However, the information contained in indirect cues that enable prey to fine-tune their phenotypes to variation in risk is still unclear. In aquatic systems, research has focused on cue concentration as the key variable driving threat-sensitive responses to risk. However, while risk is measured as individuals killed per time, cue concentration may vary with either the number or biomass killed. Alternatively, fine-grained variation in cue, that is, frequency of cue pulses irrespective of concentration, may provide a more reliable signal of risk. Here, we present results from laboratory experiments that examine the relationship between red-eyed treefrog tadpole growth and total cue, cue per pulse, and cue pulse frequency. We also reanalyze an earlier study that examined the effect of fine-grained variation in predator cues on wood frog tadpole growth. Both studies show growth declines with increasing cue pulse frequency, even though individual pulses in high-frequency treatments contained very little cue. This result suggests that counter to earlier conclusions, tadpoles are using fine-grained variation in cue arising from the number of predation events to assess and respond to predation risk, as predicted by consumer-resource theory. C1 [McCoy, Michael W.; Vonesh, James R.] Virginia Commonwealth Univ, Dept Biol, Richmond, VA 23284 USA. [McCoy, Michael W.] E Carolina Univ, Dept Biol, Greenville, NC USA. [Wheat, Stefan K.] Whitman Coll, Dept Biol, Walla Walla, WA 99362 USA. [Warkentin, Karen M.] Boston Univ, Dept Biol, Boston, MA 02215 USA. [Warkentin, Karen M.] Smithsonian Trop Res Inst, Gamboa, Panama. RP Vonesh, JR (reprint author), Virginia Commonwealth Univ, Dept Biol, Richmond, VA 23284 USA. EM jrvonesh@vcu.edu RI Vonesh, James/I-1573-2013 OI Vonesh, James/0000-0003-2481-9988 FU National Science Foundation [0716923, 0717220] FX Funded by National Science Foundation Grants DEB #0716923 & 0717220 NR 26 TC 1 Z9 1 U1 1 U2 8 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 2045-7758 J9 ECOL EVOL JI Ecol. Evol. PD OCT PY 2015 VL 5 IS 20 BP 4523 EP 4528 DI 10.1002/ece3.1552 PG 6 WC Ecology; Evolutionary Biology SC Environmental Sciences & Ecology; Evolutionary Biology GA CU7OP UT WOS:000363731500003 PM 26668719 ER PT J AU Potts, R Faith, JT AF Potts, Richard Faith, J. Tyler TI Alternating high and low climate variability: The context of natural selection and speciation in Plio-Pleistocene hominin evolution SO JOURNAL OF HUMAN EVOLUTION LA English DT Article DE Adaptability; Climate variability stages; East Africa; Environmental dynamics; Null models; Variability selection ID SOUTHERN KENYA RIFT; EARLY HOMO-FOSSILS; KOOBI-FORA; HADAR FORMATION; TURKANA BASIN; OLORGESAILIE FORMATION; AFRICAN CLIMATE; FAUNAL TURNOVER; EASTERN AFRICA; STONE TOOLS AB Interaction of orbital insolation cycles defines a predictive model of alternating phases of high- and low-climate variability for tropical East Africa over the past 5 million years. This model, which is described in terms of climate variability stages, implies repeated increases in landscape/resource instability and intervening periods of stability in East Africa. It predicts eight prolonged (>192 kyr) eras of intensified habitat instability (high variability stages) in which hominin evolutionary innovations are likely to have occurred, potentially by variability selection. The prediction that repeated shifts toward high climate variability affected paleoenvironments and evolution is tested in three ways. In the first test, deep-sea records of northeast African terrigenous dust flux (Sites 721/722) and eastern Mediterranean sapropels (Site 967A) show increased and decreased variability in concert with predicted shifts in climate variability. These regional measurements of climate dynamics are complemented by stratigraphic observations in five basins with lengthy stratigraphic and paleoenvironmental records: the mid-Pleistocene Olorgesailie Basin, the Plio-Pleistocene Turkana and Olduvai Basins, and the Pliocene Tugen Hills sequence and Hadar Basin-all of which show that highly variable landscapes inhabited by hominin populations were indeed concentrated in predicted stages of prolonged high climate variability. Second, stringent null-model tests demonstrate a significant association of currently known first and last appearance datums (FADs and LADs) of the major hominin lineages, suites of technological behaviors, and dispersal events with the predicted intervals of prolonged high climate variability. Palynological study in the Nihewan Basin, China, provides a third test, which shows the occupation of highly diverse habitats in eastern Asia, consistent with the predicted increase in adaptability in dispersing Oldowan hominins. Integration of fossil, archeological, sedimentary, and paleolandscape evidence illustrates the potential influence of prolonged high variability on the origin and spread of critical adaptations and lineages in the evolution of Homo. The growing body of data concerning environmental dynamics supports the idea that the evolution of adaptability in response to climate and overall ecological instability represents a unifying theme in hominin evolutionary history. Published by Elsevier Ltd. C1 [Potts, Richard] Smithsonian Inst, Human Origins Program, Natl Museum Nat Hist, Washington, DC 20013 USA. [Potts, Richard] Natl Museums Kenya, Dept Earth Sci, Nairobi, Kenya. [Faith, J. Tyler] Univ Queensland, Sch Social Sci, Archaeol Program, Brisbane, Qld 4072, Australia. RP Potts, R (reprint author), Smithsonian Inst, Human Origins Program, Natl Museum Nat Hist, Washington, DC 20013 USA. EM pottsr@si.edu FU National Museums of Kenya; Peter Buck Fund for Human Origins Research; NSF HOMINID Program [BCS-0218511]; Ruth and Vernon Taylor Foundation; University of Queensland Postdoctoral Research Fellowship; Smithsonian Institution FX R.P. wishes to thank R.X. Zhu, C.L. Deng, and Y.X. Pan, Institute of Geology and Geophysics, Chinese Academy of Sciences, Beijing, for support, collaboration on the Nihewan Basin research, and Q. Xu for pollen analyses; and Peter deMenocal for discussion of the high/low climate variability model, for sharing data, and inspiring the tests of the model here. The Olorgesailie research is a collaborative project of the National Museums of Kenya and Smithsonian Institution; R.P. thanks Drs. I.O. Farah, E.N. Mbua, F.K. Manthi, and P. Kiura for their long-term support. Much gratitude also goes to Olorgesailie project collaborators A.K. Behrensmeyer, R.B. Owen, and A.L. Deino for paleoenvironmental, stratigraphic, and geochronological studies. We thank J.B. Clark for assistance in producing the figures and logistical support for the research reported here. R.P. also gratefully acknowledges support from the Peter Buck Fund for Human Origins Research, NSF HOMINID Program grant BCS-0218511, and the Ruth and Vernon Taylor Foundation. J.T.F. is supported by a University of Queensland Postdoctoral Research Fellowship. Some of the ideas developed here came to fruition through discussions with participants of the Smithsonian's Evolution of Terrestrial Ecosystems (ETE) workshops on Community Assembly and Disassembly. We thank Ariane Burke and Matt Grove for the invitation to contribute this paper; two anonymous reviewers who contributed valuable comments; and Matt Grove and Mark Teaford for permitting us to revise the manuscript in response to recent discoveries of earliest known Homo and stone artifacts. NR 131 TC 6 Z9 6 U1 12 U2 41 PU ACADEMIC PRESS LTD- ELSEVIER SCIENCE LTD PI LONDON PA 24-28 OVAL RD, LONDON NW1 7DX, ENGLAND SN 0047-2484 J9 J HUM EVOL JI J. Hum. Evol. PD OCT PY 2015 VL 87 SI SI BP 5 EP 20 DI 10.1016/j.jhevol.2015.06.014 PG 16 WC Anthropology; Evolutionary Biology SC Anthropology; Evolutionary Biology GA CV4WD UT WOS:000364266300002 PM 26315724 ER PT J AU Ade, PAR Ahmed, Z Aikin, RW Alexander, KD Barkats, D Benton, SJ Bischoff, CA Bock, JJ Brevik, JA Buder, I Bullock, E Buza, V Connors, J Crill, BP Dowell, CD Dvorkin, C Duband, L Filippini, JP Fliescher, S Golwala, SR Halpern, M Harrison, S Hasselfield, M Hildebrandt, SR Hilton, GC Hristov, VV Hui, H Irwin, KD Karkare, KS Kaufman, JP Keating, BG Kefeli, S Kernasovskiy, SA Kovac, JM Kuo, CL Leitch, EM Lueker, M Mason, P Megerian, KG Netterfield, CB Nguyen, HT O'Brient, R Ogburn, RW Orlando, A Pryke, C Reintsema, CD Richter, S Schwarz, R Sheehy, CD Staniszewski, ZK Sudiwala, RV Teply, GP Thompson, KL Tolan, JE Turner, AD Vieregg, AG Weber, AC Willmert, J Wong, CL Yoon, KW AF Ade, P. A. R. Ahmed, Z. Aikin, R. W. Alexander, K. D. Barkats, D. Benton, S. J. Bischoff, C. A. Bock, J. J. Brevik, J. A. Buder, I. Bullock, E. Buza, V. Connors, J. Crill, B. P. Dowell, C. D. Dvorkin, C. Duband, L. Filippini, J. P. Fliescher, S. Golwala, S. R. Halpern, M. Harrison, S. Hasselfield, M. Hildebrandt, S. R. Hilton, G. C. Hristov, V. V. Hui, H. Irwin, K. D. Karkare, K. S. Kaufman, J. P. Keating, B. G. Kefeli, S. Kernasovskiy, S. A. Kovac, J. M. Kuo, C. L. Leitch, E. M. Lueker, M. Mason, P. Megerian, K. G. Netterfield, C. B. Nguyen, H. T. O'Brient, R. Ogburn, R. W. Orlando, A. Pryke, C. Reintsema, C. D. Richter, S. Schwarz, R. Sheehy, C. D. Staniszewski, Z. K. Sudiwala, R. V. Teply, G. P. Thompson, K. L. Tolan, J. E. Turner, A. D. Vieregg, A. G. Weber, A. C. Willmert, J. Wong, C. L. Yoon, K. W. CA Keck Array Collaboration Bicep2 Collaboration TI BICEP2/KECK ARRAY V: MEASUREMENTS OF B-MODE POLARIZATION AT DEGREE ANGULAR SCALES AND 150 GHz BY THE KECK ARRAY SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmic background radiation; cosmology: observations; gravitational waves; inflation; polarization ID MICROWAVE BACKGROUND POLARIZATION; TRANSITION-EDGE SENSORS; PROBE WMAP OBSERVATIONS; POWER SPECTRA; GRAVITY-WAVES; TEMPERATURE; QUAD; IMAGER; CAPMAP; MAPS AB The Keck Array is a system of cosmic microwave background polarimeters, each similar to the BICEP2 experiment. In this paper we report results from the 2012 to 2013 observing seasons, during which the Keck Array consisted of five receivers all operating in the same (150 GHz) frequency band and observing field as BICEP2. We again find an excess of B-mode power over the lensed-.CDM expectation of >5 sigma in the range 30 < l < 150 and confirm that this is not due to systematics using jackknife tests and simulations based on detailed calibration measurements. In map difference and spectral difference tests these new data are shown to be consistent with BICEP2. Finally, we combine the maps from the two experiments to produce final Q and U maps which have a depth of 57 nK deg (3.4 mu K arcmin) over an effective area of 400 deg(2) for an equivalent survey weight of 250,000 mu K-2. The final BB band powers have noise uncertainty a factor of 2.3 times better than the previous results, and a significance of detection of excess power of >6 sigma. C1 [Ade, P. A. R.; Sudiwala, R. V.] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales. [Ahmed, Z.; Irwin, K. D.; Kernasovskiy, S. A.; Kuo, C. L.; Ogburn, R. W.; Thompson, K. L.; Tolan, J. E.; Yoon, K. W.] Stanford Univ, Dept Phys, Stanford, CA 94305 USA. [Aikin, R. W.; Bock, J. J.; Brevik, J. A.; Crill, B. P.; Filippini, J. P.; Golwala, S. R.; Hildebrandt, S. R.; Hristov, V. V.; Hui, H.; Kefeli, S.; Lueker, M.; Mason, P.; Staniszewski, Z. K.; Teply, G. P.] CALTECH, Dept Phys, Pasadena, CA 91125 USA. [Alexander, K. D.; Bischoff, C. A.; Buder, I.; Buza, V.; Connors, J.; Dvorkin, C.; Harrison, S.; Karkare, K. S.; Kovac, J. M.; Richter, S.; Wong, C. L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Barkats, D.] ESO, Joint ALMA Observ, Santiago, Chile. [Benton, S. J.; Netterfield, C. B.] Univ Toronto, Dept Phys, Toronto, ON, Canada. [Bock, J. J.; Crill, B. P.; Dowell, C. D.; Hildebrandt, S. R.; Megerian, K. G.; Nguyen, H. T.; O'Brient, R.; Staniszewski, Z. K.; Turner, A. D.; Weber, A. C.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Bullock, E.; Pryke, C.] Univ Minnesota, Minnesota Inst Astrophys, Minneapolis, MN 55455 USA. [Duband, L.] Commissariat Energie Atom, SBT, Grenoble, France. [Filippini, J. P.] Univ Illinois, Dept Phys, Champaign, IL 61820 USA. [Fliescher, S.; Pryke, C.; Schwarz, R.; Willmert, J.] Univ Minnesota, Dept Phys, Minneapolis, MN 55455 USA. [Halpern, M.; Hasselfield, M.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V5Z 1M9, Canada. [Hilton, G. C.; Irwin, K. D.; Reintsema, C. D.] NIST, Boulder, CO 80305 USA. [Irwin, K. D.; Kuo, C. L.; Ogburn, R. W.; Yoon, K. W.] SLAC Natl Accelerator Lab, Kavli Inst Particle Astrophys & Cosmol, Menlo Pk, CA 94025 USA. [Kaufman, J. P.; Keating, B. G.; Orlando, A.] Univ Calif San Diego, Dept Phys, La Jolla, CA 92093 USA. [Leitch, E. M.; Sheehy, C. D.; Vieregg, A. G.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Leitch, E. M.; Sheehy, C. D.; Vieregg, A. G.] Univ Chicago, Enrico Fermi Inst, Dept Phys, Chicago, IL 60637 USA. [Netterfield, C. B.] Canadian Inst Adv Res, Toronto, ON, Canada. RP Ade, PAR (reprint author), Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales. EM sstokes@stanford.edu OI Alexander, Kate/0000-0002-8297-2473; Orlando, Angiola/0000-0001-8004-5054; Karkare, Kirit/0000-0002-5215-6993; Bischoff, Colin/0000-0001-9185-6514; Barkats, Denis/0000-0002-8971-1954 FU National Science Foundation (Harvard) [ANT-1145172]; Keck Foundation (Caltech); NASA APRA program [06-ARPA206-0040, 10-SAT10-0017]; NASA SAT program [06-ARPA206-0040, 10-SAT10-0017]; Canada Foundation for Innovation; National Science Foundation (Minnesota) [ANT-1145143]; National Science Foundation (Stanford) [ANT-1145248] FX The Keck Array project has been made possible through support from the National Science Foundation under Grants ANT-1145172 (Harvard), ANT-1145143 (Minnesota) & ANT-1145248 (Stanford), and from the Keck Foundation (Caltech). The development of antenna-coupled detector technology was supported by the JPL Research and Technology Development Fund and Grants No. 06-ARPA206-0040 and 10-SAT10-0017 from the NASA APRA and SAT programs. The development and testing of focal planes were supported by the Gordon and Betty Moore Foundation at Caltech. Readout electronics were supported by a Canada Foundation for Innovation grant to UBC. The computations in this paper were run on the Odyssey cluster supported by the FAS Science Division Research Computing Group at Harvard University. The analysis effort at Stanford and SLAC is partially supported by the U.S. Department of Energy Office of Science. We thank the staff of the U.S. Antarctic Program and in particular the South Pole Station without whose help this research would not have been possible. Most special thanks go to our heroic winter-overs Robert Schwarz and Steffen Richter. We thank all those who have contributed past efforts to the BICEP-Keck Array series of experiments, including the BICEP1 team. NR 58 TC 27 Z9 27 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 OCT 1 PY 2015 VL 811 IS 2 AR 126 DI 10.1088/0004-637X/811/2/126 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CU4QE UT WOS:000363513800054 ER PT J AU Avrett, E Tian, H Landi, E Curdt, W Wulser, JP AF Avrett, E. Tian, H. Landi, E. Curdt, W. Wuelser, J. -P. TI MODELING THE CHROMOSPHERE OF A SUNSPOT AND THE QUIET SUN SO ASTROPHYSICAL JOURNAL LA English DT Article DE Sun: atmosphere; Sun: chromosphere; Sun: UV radiation ID MG-II-H; REGION-IMAGING-SPECTROGRAPH; SOLAR TRANSITION REGION; LOCAL THERMODYNAMIC-EQUILIBRIUM; K LINES; ENERGY-BALANCE; SPECTRAL ATLAS; ATMOSPHERE; RESOLUTION; DIFFUSION AB Semiempirical atmospheric modeling attempts to match an observed spectrum by finding the temperature distribution and other physical parameters along the line of sight through the emitting region such that the calculated spectrum agrees with the observed one. In this paper we take the observed spectrum of a sunspot and the quiet Sun in the EUV wavelength range 668-1475 angstrom from the 2001 SUMER atlas of Curdt et al. to determine models of the two atmospheric regions, extending from the photosphere through the overlying chromosphere into the transition region. We solve the coupled statistical equilibrium and optically thick radiative transfer equations for a set of 32 atoms and ions. The atoms that are part of molecules are treated separately, and are excluded from the atomic abundances and atomic opacities. We compare the Mg II k line profile observations from the Interface Region Imaging Spectrograph with the profiles calculated from the two models. The calculated profiles for the sunspot are substantially lower than the observed ones, based on the SUMER models. The only way we have found to raise the calculated Mg II lines to agree with the observations is to introduce illumination of the sunspot from the surrounding active region. C1 [Avrett, E.; Tian, H.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. [Landi, E.] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA. [Curdt, W.] Max Planck Inst Sonnensyst Foschung, Gottingen, Germany. [Wuelser, J. -P.] Lockheed Martin Adv Techonol Ctr, Palo Alto, CA USA. RP Avrett, E (reprint author), Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. FU NASA [NNX10AM17G, NNX11AC20G, NNG09FA40C]; LMSAL [8100002705]; Norwefian Space Center (NSC, Norway) through an ESA PRODEX contract FX We thank J. M. Fontenla for suggesting the importance of incident radiation in the calculation of the Mg II lines, and for comments on the paper. The work of E.L. is supported by NASA grants NNX10AM17G and NNX11AC20G. H.T. is supported under contract 8100002705 from LMSAL to SAO. J.-P.W. is supported by NASA contract NNG09FA40C. IRIS is a NASA small explorer mission developed and operated by LMSAL with mission operation executed at NASA Ames Research Center and major contributions to downlink communications funded by the Norwefian Space Center (NSC, Norway) through an ESA PRODEX contract. NR 54 TC 2 Z9 2 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD OCT 1 PY 2015 VL 811 IS 2 AR 87 DI 10.1088/0004-637X/811/2/87 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CU4QE UT WOS:000363513800015 ER PT J AU Bray, AD Eisenstein, DJ Skibba, RA Blanton, MR Coil, AL Cool, RJ Mendez, AJ Moustakas, J Zhu, GT AF Bray, Aaron D. Eisenstein, Daniel J. Skibba, Ramin A. Blanton, Michael R. Coil, Alison L. Cool, Richard J. Mendez, Alexander J. Moustakas, John Zhu, Guangtun TI PRIMUS: THE EFFECT OF PHYSICAL SCALE ON THE LUMINOSITY DEPENDENCE OF GALAXY CLUSTERING VIA CROSS-CORRELATIONS SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology: observations; galaxies: statistics; galaxies: evolution; galaxies: high-redshift; cosmology: large-scale structure of universe; surveys ID HALO OCCUPATION DISTRIBUTION; DIGITAL SKY SURVEY; EXTRAGALACTIC SURVEY ESIS; DEEP FIELD SOUTH; LESS-THAN 1.2; REDSHIFT SURVEY; STELLAR MASS; PHOTOMETRIC REDSHIFTS; COLOR DEPENDENCE; GALACTIC CONFORMITY AB We report small-scale clustering measurements from the PRIsm MUlti-object Survey (PRIMUS) spectroscopic redshift survey as a function of color and luminosity. We measure the real-space cross-correlations between 62,106 primary galaxies with PRIMUS redshifts and a tracer population of similar to 545,000 photometric galaxies over redshifts from z = 0.2 to z = 1. We separately fit a power-law model in redshift and luminosity to each of three independent color-selected samples of galaxies. We report clustering amplitudes at fiducial values of z = 0.5 and L = 1.5L*. The clustering of the red galaxies is similar to 3 times as strong as that of the blue galaxies and similar to 1.5 as strong as that of the green galaxies. We also find that the luminosity dependence of the clustering is strongly dependent on physical scale, with greater luminosity dependence being found between r = 0.0625 h(-1) Mpc and r = 0.25 h(-1) Mpc, compared to the r = 0.5 h(-1) Mpc to r = 2h(-1) Mpc range. Moreover, over a range of two orders of magnitude in luminosity, a single power-law fit to the luminosity dependence is not sufficient to explain the increase in clustering at both the bright and faint ends at the smaller scales. We argue that luminosity-dependent clustering at small scales is a necessary component of galaxy-halo occupation models for blue, star-forming galaxies as well as for red, quenched galaxies. C1 [Bray, Aaron D.; Eisenstein, Daniel J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Skibba, Ramin A.; Coil, Alison L.] Univ Calif San Diego, Ctr Astrophys & Space Sci, Dept Phys, La Jolla, CA 92093 USA. [Blanton, Michael R.] NYU, Dept Phys, Ctr Cosmol & Particle Phys, New York, NY 10003 USA. [Cool, Richard J.] Univ Arizona, MMT Observ, Tucson, AZ 85721 USA. [Mendez, Alexander J.; Zhu, Guangtun] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Moustakas, John] Siena Coll, Dept Phys & Astron, Loudonville, NY 12211 USA. RP Bray, AD (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM abray@cfa.harvard.edu OI Zhu, Guangtun/0000-0002-7574-8078 FU NSF [AST-0607541, 0908442, AST-0607701, 0908246, 0908354]; NSF CAREER award [AST-1055081]; NASA - Space Telescope Science Institute [HST-HF2-51351, NAS 5-26555]; NASA [08-ADP08-0019, NNX09AC95G] FX A.D.B. and D.J.E. acknowledge support from NSF grants AST-0607541 and 0908442. A.L.C. acknowledges support from NSF CAREER award AST-1055081. G.Z. 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. Additional PRIMUS funding has been provided by NSF grants AST-0607701, 0908246, and 0908354, and NASA grants 08-ADP08-0019, NNX09AC95G. We thank the staff at Las Campanas Observatory, Chile, where data was taken with the 6.5 m Magellan Telescopes, and we acknowledge Magellan telescope time provided by NOAO community access. We thank the CFHTLS, COSMOS, DEEP2 and SWIRE teams for their public data releases and/or access to early releases of their imaging catalogs. NR 72 TC 2 Z9 2 U1 1 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD OCT 1 PY 2015 VL 811 IS 2 AR 90 DI 10.1088/0004-637X/811/2/90 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CU4QE UT WOS:000363513800018 ER PT J AU Hsieh, PY Ho, PTP Hwang, CY AF Hsieh, Pei-Ying Ho, Paul T. P. Hwang, Chorng-Yuan TI THE CONNECTING MOLECULAR RIDGE IN THE GALACTIC CENTER SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: starburst; Galaxy: center; ISM: clouds ID SAGITTARIUS-A-EAST; SUPERMASSIVE BLACK-HOLE; CENTER REGION; CIRCUMNUCLEAR DISK; STAR-FORMATION; SGR-A; CONTINUUM SURVEY; EXPANDING SHELL; STELLAR ORBITS; MASSIVE STARS AB We report new observations of multiple transitions of the CS molecular lines in the SgrA region of the Galactic center, at an angular resolution of 40 '' (= 1.5 pc). The objective of this paper is to study the polar arc (PA), which is a molecular ridge near the SgrA region with apparent non-coplanar motions and a velocity gradient perpendicular to the Galactic plane. With our high resolution dense-gas maps, we search for the base and the origin of the PA, which is expected to be embedded in the Galactic disk. We find that the PA is connected to a continuous structure from one of the disk rings/arms in both the spatial and velocity domains. This structure near SgrA* has high CS (J = 4-3)/ CS(J = 2-1) ratios >= 1. The fact that this structure has eluded detection in previous observations is likely due to the combination of high excitation and low surface brightness temperature. We call this new structure the connecting ridge. We discuss the possible mechanism for forming this structure and for lifting the gas above the Galactic plane. C1 [Hsieh, Pei-Ying; Ho, Paul T. P.] Acad Sinica, Inst Astron & Astrophys, Taipei 10617, Taiwan. [Hsieh, Pei-Ying; Hwang, Chorng-Yuan] Natl Cent Univ, Inst Astrophys, Jhongli 32001, Taoyuan County, Taiwan. [Ho, Paul T. P.] East Asian Observ, Hilo, HI 96720 USA. [Ho, Paul T. P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Hsieh, PY (reprint author), Acad Sinica, Inst Astron & Astrophys, POB 23-141, Taipei 10617, Taiwan. EM pyhsieh@asiaa.sinica.edu.tw FU National Science Council (NSC) [NSC 100-2112-M-001-006-MY3, NSC 97-2112-M-001-021-MY3]; Ministry of Science and Technology (MoST) of Taiwan [MoST 103-2112-M-001-032-MY3, MoST 99-2119-M-001-002-MY4, MoST 103-2119-M-001-010-MY2, MoST 103-2119-M-008-017-MY3, MoST 104-2811-M-001-171] FX We would like to thank the referee for a constructive report that improved the paper. We thank Simon Radford for the assistance of the CSO observations. We thank Dr. Yusef-Zadeh, F. for providing us the VLA 20 cm continuum map. This material is based upon work at the Caltech Submillimeter Observatory, which is operated by the California Institute of Technology. These observations are part of the East Asia Core Observatories Association (EACOA) project on CSO. P. Y.H. is supported by the National Science Council (NSC) and the Ministry of Science and Technology (MoST) of Taiwan, NSC 100-2112-M-001-006-MY3, NSC 97-2112-M-001-021-MY3, and MoST 103-2112-M-001-032-MY3, MoST 99-2119-M-001-002-MY4, MoST 103-2119-M-001-010-MY2, MoST 103-2119-M-008-017-MY3, and MoST 104-2811-M-001-171. NR 100 TC 2 Z9 2 U1 1 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD OCT 1 PY 2015 VL 811 IS 2 AR 142 DI 10.1088/0004-637X/811/2/142 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CU4QE UT WOS:000363513800070 ER PT J AU Jiang, JC Bambi, C Steiner, JF AF Jiang, Jiachen Bambi, Cosimo Steiner, James F. TI TESTING THE KERR NATURE OF BLACK HOLE CANDIDATES USING IRON LINE SPECTRA IN THE CPR FRAMEWORK SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; black hole physics; gravitation ID NONBARYONIC COMPACT OBJECT; ACCRETION DISC; EVENT-HORIZON; CYGNUS X-1; INNER-DISK; SPIN; MASS; CONSTRAINTS; HAIR AB The iron K alpha line commonly observed in the X-ray spectrum of both stellar-mass and supermassive black hole (BH) candidates originates from X-ray fluorescence of the inner accretion disk. Accordingly, it can be used to map the spacetime geometry around these objects. In this paper, we extend previous work using the iron K alpha line to test the Kerr BH hypothesis. We adopt the Cardoso-Pani-Rico parametrization and we test the possibility of constraining possible deviations from the Kerr solution that can be obtained from observations across the range of BH spins and inclination angles. We confirm previous claims that the iron K alpha line is potentially a quite powerful probe for testing the Kerr metric given sufficiently high quality data and with systematics under control, especially in the case of fast-rotating BHs and high inclination angles since both conditions serve to maximize relativistic effects. We find that some geometric perturbations from Kerr geometry manifest more strongly in the iron line profile than others. While the perturbation parameter epsilon(t)(3) can be well constrained by the iron line profile, an orthogonal data set is necessary to constrain departures from Kerr geometry in epsilon(r)(3). C1 [Jiang, Jiachen; Bambi, Cosimo] Fudan Univ, Ctr Field Theory & Particle Phys, Shanghai 200433, Peoples R China. [Jiang, Jiachen; Bambi, Cosimo] Fudan Univ, Dept Phys, Shanghai 200433, Peoples R China. [Steiner, James F.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Bambi, C (reprint author), Fudan Univ, Ctr Field Theory & Particle Phys, Shanghai 200433, Peoples R China. EM bambi@fudan.edu.cn FU NSFC [11305038]; Shanghai Municipal Education Commission [14ZZ001]; Thousand Young Talents Program; Fudan University; NASA Hubble Fellowship [HST-HF-51315.01] FX J.J. and C.B. were supported by the NSFC grant No. 11305038, the Shanghai Municipal Education Commission grant No. 14ZZ001, the Thousand Young Talents Program, and Fudan University. J.F.S. was supported by the NASA Hubble Fellowship grant HST-HF-51315.01. NR 52 TC 12 Z9 12 U1 0 U2 7 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD OCT 1 PY 2015 VL 811 IS 2 AR 130 DI 10.1088/0004-637X/811/2/130 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CU4QE UT WOS:000363513800058 ER PT J AU Matthews, BC Kennedy, G Sibthorpe, B Holland, W Booth, M Kalas, P MacGregor, M Wilner, D Vandenbussche, B Olofsson, G Blommaert, J Brandeker, A Dent, WRF de Vries, BL Di Francesco, J Fridlund, M Graham, JR Greaves, J Heras, AM Hogerheijde, M Ivison, RJ Pantin, E Pilbratt, GL AF Matthews, Brenda C. Kennedy, Grant Sibthorpe, Bruce Holland, Wayne Booth, Mark Kalas, Paul MacGregor, Meredith Wilner, David Vandenbussche, Bart Olofsson, Goran Blommaert, Joris Brandeker, Alexis Dent, W. R. F. de Vries, Bernard L. Di Francesco, James Fridlund, Malcolm Graham, James R. Greaves, Jane Heras, Ana M. Hogerheijde, Michiel Ivison, R. J. Pantin, Eric Pilbratt, Goran L. TI THE AU MIC DEBRIS DISK: FAR-INFRARED AND SUBMILLIMETER RESOLVED IMAGING SO ASTROPHYSICAL JOURNAL LA English DT Article DE circumstellar matter; stars: individual (AU Mic) ID PICTORIS MOVING GROUP; LOW-MASS STARS; SPITZER-SPACE-TELESCOPE; CIRCLE-DOT STARS; CIRCUMSTELLAR DISK; DUST DISK; COLLISIONAL CASCADES; SCORPIUS-CENTAURUS; PLANET FORMATION; SUPER-EARTHS AB We present far-infrared and submillimeter maps from the Herschel Space Observatory and the James Clerk Maxwell Telescope of the debris disk host star AU Microscopii. Disk emission is detected at 70, 160, 250, 350, 450, 500, and 850 mu m. The disk is resolved at 70, 160, and 450 mu m. In addition to the planetesimal belt, we detect thermal emission from AU Mic's halo for the first time. In contrast to the scattered light images, no asymmetries are evident in the disk. The fractional luminosity of the disk is 3.9 x 10(-4) and its milimeter-grain dust mass is 0.01 M-circle dot (+/- 20%). We create a simple spatial model that reconciles the disk spectral energy distribution as a blackbody of 53 +/- 2K (a composite of 39 and 50 K components) and the presence of small (non-blackbody) grains which populate the extended halo. The best-fit model is consistent with the "birth ring" model explored in earlier works, i.e., an edge-on dust belt extending from 8.8 to 40 AU, but with an additional halo component with an r(-1.5) surface density profile extending to the limits of sensitivity (140 AU). We confirm that AU Mic does not exert enough radiation force to blow out grains. For stellar mass-loss rates of 10-100 times solar, compact (zero porosity) grains can only be removed if they are very small; consistently with previous work, if the porosity is 0.9, then grains approaching 0.1 mu m can be removed via corpuscular forces (i.e., the stellar wind). C1 [Matthews, Brenda C.; Di Francesco, James] Natl Res Council Canada, Herzberg Astron Program, Victoria, BC V9E 2E7, Canada. [Matthews, Brenda C.; Di Francesco, James] Natl Res Council Canada, Herzberg Astrophys Program, Victoria, BC V9E 2E7, Canada. [Matthews, Brenda C.; Di Francesco, James; Ivison, R. J.] Univ Victoria, Victoria, BC V8P 5C2, Canada. [Kennedy, Grant] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Sibthorpe, Bruce] SRON Netherlands Inst Space Res, Groningen, Netherlands. [Holland, Wayne] Univ Edinburgh, Inst Astron, Royal Observ, Edinburgh EH9 3HJ, Midlothian, Scotland. [Holland, Wayne] Royal Observ, Sci & Technol Facil Council, UK Astron Technol Ctr, Edinburgh EH9 3HJ, Midlothian, Scotland. [Booth, Mark] Pontificia Univ Catolica Chile, Inst Astrofs, Santiago 7820436, Chile. [Kalas, Paul; Graham, James R.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Kalas, Paul] SETI Inst, Mountain View, CA 94043 USA. [MacGregor, Meredith; Wilner, David] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Vandenbussche, Bart] Inst Astron KU Leuven, B-3001 Leuven, Belgium. [Olofsson, Goran; Brandeker, Alexis; de Vries, Bernard L.] Stockholm Univ, Dept Astron, AlbaNova Univ Ctr, SE-10691 Stockholm, Sweden. [Blommaert, Joris] Vrije Univ Brussel, Dept Phys & Astrophys, Astron & Astrophys Res Grp, B-1050 Brussels, Belgium. [Blommaert, Joris] Flemish Inst Technol Res VITO, B-2400 Mol, Belgium. [Dent, W. R. F.] Joint ALMA Observ, Santiago 7630355, Chile. [de Vries, Bernard L.] Stockholm Univ, Astrobiol Ctr, SE-10691 Stockholm, Sweden. [Fridlund, Malcolm] Chalmers, Onsala Space Observ, Dept Earth & Space Sci, SE-43992 Onsala, Sweden. [Fridlund, Malcolm; Hogerheijde, Michiel] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [Greaves, Jane] Univ St Andrews, Sch Phys & Astron, St Andrews KY16 9SS, Fife, Scotland. [Heras, Ana M.; Pilbratt, Goran L.] European Space Res & Technol Ctr ESTEC SRE S, Directorate Sci & Robot Explorat, Sci Support Off, ESA, NL-2201 AZ Noordwijk, Netherlands. [Ivison, R. J.] European So Observ, Garching, Germany. [Pantin, Eric] CEA DSM CNRS Univ Paris Diderot, IRFU SAp, Lab AIM, F-91191 Gif Sur Yvette, France. RP Matthews, BC (reprint author), Natl Res Council Canada, Herzberg Astron Program, 5071 W Saanich Rd, Victoria, BC V9E 2E7, Canada. RI Ivison, R./G-4450-2011; OI Ivison, R./0000-0001-5118-1313; Booth, Mark/0000-0001-8568-6336; MacGregor, Meredith/0000-0001-7891-8143; Kennedy, Grant/0000-0001-6831-7547; Brandeker, Alexis/0000-0002-7201-7536 FU European Union through ERC [279973]; FONDECYT [3140479]; NASA [NMO711043]; NSF [AST-0909188]; STScI under NASA [GO-10228, NAS5-26555]; AAS Chretien grant; CSA (Canada); NAOC (China); CEA (France); CNES (France); CNRS (France); ASI (Italy); MCINN (Spain); SNSB (Sweden); STFC (UK); UKSA (UK); NASA (USA); BMVIT (Austria); ESA-PRODEX (Belgium); CEA/CNES (France); DLR (Germany); ASI/INAF (Italy); CICYT/MCYT (Spain) FX We acknowledge the efforts of our referee, whose constructive comments improved and clarified the manuscript. B.C.M. is grateful to Christine Chen for checking the quality of high-res IRS data from Spitzer. G.M.K. acknowledges support from the European Union through ERC grant number 279973. M.B. acknowledges support from a FONDECYT Postdoctral Fellowship, project no. 3140479. P.K. thanks support from NASA NMO711043, NSF AST-0909188, and GO-10228 from STScI under NASA contract NAS5-26555. E.P. is partly supported by a AAS Chretien grant. PACS has been developed by a consortium of institutes led by MPE (Germany) and including UVIE (Austria); KU Leuven, CSL, IMEC (Belgium); CEA, LAM (France); MPIA (Germany); INAF-IFSI/OAA/OAP/OAT, LENS, SISSA (Italy); IAC (Spain). This development has been supported by the funding agencies BMVIT (Austria), ESA-PRODEX (Belgium), CEA/CNES (France), DLR (Germany), ASI/INAF (Italy), and CICYT/MCYT (Spain). SPIRE has been developed by a consortium of institutes led by Cardiff University (UK) and including Univ. Lethbridge (Canada); NAOC (China); CEA, LAM (France); IFSI, Univ. Padua (Italy); IAC (Spain); Stockholm Observatory (Sweden); Imperial College London, RAL, UCL-MSSL, UKATC, Univ. Sussex (UK); and Caltech, JPL, NHSC, Univ. Colorado (USA). This development has been supported by national funding agencies: CSA (Canada); NAOC (China); CEA, CNES, CNRS (France); ASI (Italy); MCINN (Spain); SNSB (Sweden); STFC, UKSA (UK); and NASA (USA). This research used the facilities of the Canadian Astronomy Data Centre operated by the National Research Council of Canada with the support of the Canadian Space Agency. NR 80 TC 2 Z9 2 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 OCT 1 PY 2015 VL 811 IS 2 AR 100 DI 10.1088/0004-637X/811/2/100 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CU4QE UT WOS:000363513800028 ER PT J AU McDonald, M McNamara, BR van Weeren, RJ Applegate, DE Bayliss, M Bautz, MW Benson, BA Carlstrom, JE Bleem, LE Chatzikos, M Edge, AC Fabian, AC Garmire, GP Hlavacek-Larrondo, J Jones-Forman, C Mantz, AB Miller, ED Stalder, B Veilleux, S ZuHone, JA AF McDonald, Michael McNamara, Brian R. van Weeren, Reinout J. Applegate, Douglas E. Bayliss, Matthew Bautz, Marshall W. Benson, Bradford A. Carlstrom, John E. Bleem, Lindsey E. Chatzikos, Marios Edge, Alastair C. Fabian, Andrew C. Garmire, Gordon P. Hlavacek-Larrondo, Julie Jones-Forman, Christine Mantz, Adam B. Miller, Eric D. Stalder, Brian Veilleux, Sylvain ZuHone, John A. TI DEEP CHANDRA, HST-COS, AND MEGACAM OBSERVATIONS OF THE PHOENIX CLUSTER: EXTREME STAR FORMATION AND AGN FEEDBACK ON HUNDRED KILOPARSEC SCALES SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: active; galaxies: starburst; ultraviolet: galaxies; X-rays: galaxies: clusters ID GALACTIC NUCLEUS FEEDBACK; COOLING FLOW CLUSTERS; POLE TELESCOPE SURVEY; X-RAY CAVITIES; SPT-SZ SURVEY; SUPERMASSIVE BLACK-HOLES; H-ALPHA FILAMENTS; RADIO MINI-HALOS; GALAXY CLUSTERS; XMM-NEWTON AB We present new ultraviolet, optical, and X-ray data on the Phoenix galaxy cluster (SPT-CLJ2344-4243). Deep optical imaging reveals previously undetected filaments of star formation, extending to radii of similar to 50-100 kpc in multiple directions. Combined UV-optical spectroscopy of the central galaxy reveals a massive (2 x 10(9) M-circle dot), young (similar to 4.5 Myr) population of stars, consistent with a time-averaged star formation rate of 610 +/- 50 M-circle dot yr(-1). We report a strong detection of O VI lambda lambda 1032,1038, which appears to originate primarily in shock-heated gas, but may contain a substantial contribution (>1000 M-circle dot yr(-1)) from the cooling intracluster medium (ICM). We confirm the presence of deep X-ray cavities in the inner similar to 10 kpc, which are among the most extreme examples of radio-mode feedback detected to date, implying jet powers of 2-7 x 10(45) erg s(-1). We provide evidence that the active galactic nucleus inflating these cavities may have only recently transitioned from "quasar-mode" to "radio-mode," and may currently be insufficient to completely offset cooling. A model-subtracted residual X-ray image reveals evidence for prior episodes of strong radio-mode feedback at radii of similar to 100 kpc, with extended "ghost" cavities indicating a prior epoch of feedback roughly 100 Myr ago. This residual image also exhibits significant asymmetry in the inner similar to 200 kpc (0.15R(500)), reminiscent of infalling cool clouds, either due to minor mergers or fragmentation of the cooling ICM. Taken together, these data reveal a rapidly evolving cool core which is rich with structure (both spatially and in temperature), is subject to a variety of highly energetic processes, and yet is cooling rapidly and forming stars along thin, narrow filaments. C1 [McDonald, Michael; Bautz, Marshall W.; Miller, Eric D.; ZuHone, John A.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [McNamara, Brian R.] Univ Waterloo, Dept Phys & Astron, Waterloo, ON N2L 3G1, Canada. [McNamara, Brian R.] Perimeter Inst Theoret Phys, Waterloo, ON, Canada. [van Weeren, Reinout J.; Bayliss, Matthew; Jones-Forman, Christine] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Applegate, Douglas E.] Argelander Inst Astron, D-53121 Bonn, Germany. [Bayliss, Matthew] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. [Benson, Bradford A.] Fermilab Natl Accelerator Lab, Batavia, IL 60510 USA. [Benson, Bradford A.; Carlstrom, John E.; Mantz, Adam B.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. [Benson, Bradford A.; Carlstrom, John E.; Bleem, Lindsey E.; Mantz, Adam B.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Carlstrom, John E.; Bleem, Lindsey E.] Argonne Natl Lab, Div High Energy Phys, Argonne, IL 60439 USA. [Chatzikos, Marios] Univ Kentucky, Dept Phys & Astron, Lexington, KY 40506 USA. [Edge, Alastair C.] Univ Durham, Dept Phys, Durham DH1 3LE, England. [Fabian, Andrew C.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Garmire, Gordon P.] Huntingdon Inst Xray Astron LLC, Huntingdon, PA 16652 USA. [Hlavacek-Larrondo, Julie] Univ Montreal, Dept Phys, Montreal, PQ H3C 3J7, Canada. [Stalder, Brian] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Veilleux, Sylvain] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Veilleux, Sylvain] Univ Maryland, Joint Space Sci Inst, College Pk, MD 20742 USA. RP McDonald, M (reprint author), MIT, Kavli Inst Astrophys & Space Res, 77 Massachusetts Ave, Cambridge, MA 02139 USA. EM mcdonald@space.mit.edu OI Edge, Alastair/0000-0002-3398-6916; van Weeren, Reinout/0000-0002-0587-1660 FU NASA - Space Telescope Science Institute [HST-GO-13456.002A, GO4-15122A, HST-HF51308.01-A, NAS 5-26555]; Huntingdon Institute for X-ray Astronomy, LLC [SV2-82024]; National Science Foundation [PLR-1248097, PHY-1125897]; Natural Sciences and Engineering Research Council of Canada; NASA - Chandra X-ray Center [PF2-130104, NAS8-03060]; NSERC; Canada Research Chair programs; FRQNT; DLR [50 OR 1210, 1407]; DFG [AP 253/1-1]; STFC [ST/I001573/1] FX M.M. acknowledges support by NASA through contracts HST-GO-13456.002A (Hubble) and GO4-15122A (Chandra), and Hubble Fellowship grant HST-HF51308.01-A awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., for NASA, under contract NAS 5-26555. The Guaranteed Time Observations (GTO) included here were selected by the ACIS Instrument Principal Investigator, Gordon P. Garmire, of the Huntingdon Institute for X-ray Astronomy, LLC, which is under contract to the Smithsonian Astrophysical Observatory; Contract SV2-82024. J.E.C. acknowledges support from National Science Foundation grants PLR-1248097 and PHY-1125897. B.R.M. acknowledges generous financial support from the Natural Sciences and Engineering Research Council of Canada. R.J.W. 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. J.H.-L. is supported by NSERC through the discovery grant and Canada Research Chair programs, as well as FRQNT. D.A. acknowledges support from the DLR under projects 50 OR 1210 and 1407, and from the DFG under project AP 253/1-1. A.C.E. acknowledges support from STFC grant ST/I001573/1. NR 140 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 OCT 1 PY 2015 VL 811 IS 2 AR 111 DI 10.1088/0004-637X/811/2/111 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CU4QE UT WOS:000363513800039 ER PT J AU Ruud, TM Fuskeland, U Wehus, IK Vidal, M Araujo, D Bischoff, C Buder, I Chinone, Y Cleary, K Dumoulin, RN Kusaka, A Monsalve, R Naess, SK Newburgh, LB Reeves, RA Zwart, JTL Bronfman, L Davies, RD Davis, R Dickinson, C Eriksen, HK Gaier, T Gundersen, JO Hasegawa, M Hazumi, M Huffenberger, KM Jones, ME Lawrence, CR Leitch, EM Limon, M Miller, AD Pearson, TJ Piccirillo, L Radford, SJE Readhead, ACS Samtleben, D Seiffert, M Shepherd, MC Staggs, ST Tajima, O Thompson, KL AF Ruud, T. M. Fuskeland, U. Wehus, I. K. Vidal, M. Araujo, D. Bischoff, C. Buder, I. Chinone, Y. Cleary, K. Dumoulin, R. N. Kusaka, A. Monsalve, R. Naess, S. K. Newburgh, L. B. Reeves, R. A. Zwart, J. T. L. Bronfman, L. Davies, R. D. Davis, R. Dickinson, C. Eriksen, H. K. Gaier, T. Gundersen, J. O. Hasegawa, M. Hazumi, M. Huffenberger, K. M. Jones, M. E. Lawrence, C. R. Leitch, E. M. Limon, M. Miller, A. D. Pearson, T. J. Piccirillo, L. Radford, S. J. E. Readhead, A. C. S. Samtleben, D. Seiffert, M. Shepherd, M. C. Staggs, S. T. Tajima, O. Thompson, K. L. CA QUIET Collaboration TI THE Q/U IMAGING EXPERIMENT: POLARIZATION MEASUREMENTS OF THE GALACTIC PLANE AT 43 AND 95 GHz SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmic background radiation; cosmology: observations; Galaxy: center; Galaxy: general; polarization ID PROBE WMAP OBSERVATIONS; MICROWAVE BACKGROUND DATA; RADIO-EMISSION; POWER SPECTRUM; DUST EMISSION; COMPLEX; MAPS; SYNCHROTRON; REGION; IMAGER AB We present polarization observations of two Galactic plane fields centered on Galactic coordinates (l, b) = (0 degrees, 0 degrees) and (329 degrees, 0 degrees) at both Q (43 GHz) and W bands (95 GHz), covering between 301 and 539 square degrees depending on frequency and field. These measurements were made with the QUIET instrument between 2008 October and 2010 December, and include a total of 1263 hr of observations. The resulting maps represent the deepest large-area Galactic polarization observations published to date at the relevant frequencies with instrumental rms noise varying between 1.8 and 2.8 mu K deg, 2.3-6 times deeper than corresponding WMAP and Planck maps. The angular resolution is 27'.3 and 12 8 FWHM at Q and W bands, respectively. We find excellent agreement between the QUIET and WMAP maps over the entire fields, and no compelling evidence for significant residual instrumental systematic errors in either experiment, whereas the Planck 44 GHz map deviates from these in a manner consistent with reported systematic uncertainties for this channel. We combine QUIET and WMAP data to compute inverse-variance-weighted average maps, effectively retaining small angular scales from QUIET and large angular scales from WMAP. From these combined maps, we derive constraints on several important astrophysical quantities, including a robust detection of polarized synchrotron spectral index steepening of approximate to 0.2 off the plane, as well as the Faraday rotation measure toward the Galactic center (RM = -4000 +/- 200 radm(-2)), all of which are consistent with previously published results. Both the raw QUIET and the co-added QUIET+WMAP maps are made publicly available together with all necessary ancillary information. C1 [Ruud, T. M.; Fuskeland, U.; Naess, S. K.; Eriksen, H. K.] Univ Oslo, Inst Theoret Astrophys, N-0315 Oslo, Norway. [Wehus, I. K.; Gaier, T.; Lawrence, C. R.; Leitch, E. M.; Seiffert, M.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Vidal, M.; Davies, R. D.; Davis, R.; Dickinson, C.; Piccirillo, L.] Univ Manchester, Sch Phys & Astron, Jodrell Bank Ctr Astrophys, Manchester M13 9PL, Lancs, England. [Araujo, D.; Dumoulin, R. N.; Zwart, J. T. L.; Limon, M.; Miller, A. D.] Columbia Univ, Dept Phys, New York, NY 10027 USA. [Araujo, D.; Dumoulin, R. N.; Zwart, J. T. L.; Limon, M.; Miller, A. D.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA. [Bischoff, C.; Buder, I.; Tajima, O.] Univ Chicago, Kavli Inst Cosmol Phys, Enrico Fermi Inst, Dept Phys, Chicago, IL 60637 USA. [Bischoff, C.; Buder, I.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Chinone, Y.; Hasegawa, M.; Hazumi, M.; Tajima, O.] High Energy Accelerator Res Org KEK, Oho, Ibaraki 3050801, Japan. [Chinone, Y.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. [Cleary, K.; Pearson, T. J.; Radford, S. J. E.; Readhead, A. C. S.; Shepherd, M. C.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA. [Kusaka, A.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Div Phys, Berkeley, CA 94720 USA. [Kusaka, A.; Staggs, S. T.] Princeton Univ, Joseph Henry Labs Phys, Princeton, NJ 08544 USA. [Monsalve, R.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA. [Naess, S. K.; Jones, M. E.] Univ Oxford, Dept Astrophys, Oxford OX1 3RH, England. [Newburgh, L. B.] Univ Toronto, Dunlap Inst, Toronto, ON M5S 3H4, Canada. [Reeves, R. A.] Univ Concepcion, Dept Astron, CePIA, Concepcion, Chile. [Zwart, J. T. L.] Univ Western Cape, Dept Phys, ZA-7535 Bellville, South Africa. [Zwart, J. T. L.] Univ Cape Town, Dept Astron, Astrophys Cosmol & Grav Ctr, ZA-7701 Rondebosch, South Africa. [Bronfman, L.] Univ Chile, Dept Astron, Santiago, Chile. [Gundersen, J. O.] Univ Miami, Dept Phys, Coral Gables, FL 33146 USA. [Huffenberger, K. M.] Florida State Univ, Phys, Tallahassee, FL 32306 USA. [Samtleben, D.] Leiden Univ, Huygens Kamerlingh Onnes Lab, NL-2300 RA Leiden, Netherlands. [Samtleben, D.] NIKHEF H, NL-1009 DB Amsterdam, Netherlands. [Thompson, K. L.] Stanford Univ, Stanford, CA 94305 USA. [Thompson, K. L.] Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94305 USA. RP Ruud, TM (reprint author), Univ Oslo, Inst Theoret Astrophys, POB 1029 Blindern, N-0315 Oslo, Norway. EM t.m.ruud@astro.uio.no RI Bronfman, Leonardo/H-9544-2013; Pearson, Timothy/N-2376-2015; OI Bronfman, Leonardo/0000-0002-9574-8454; Pearson, Timothy/0000-0001-5213-6231; Limon, Michele/0000-0002-5900-2698; radford, simon/0000-0001-9113-1660; Huffenberger, Kevin/0000-0001-7109-0099; Bischoff, Colin/0000-0001-9185-6514; Zwart, Jonathan/0000-0002-4967-946X FU NSF [PHY-0355328, AST-0448909, AST-1010016, PHY-0551142]; KAKENHI [20244041, 20740158, 21111002]; PRODEX [C90284]; KIPAC Enterprise grant; Strategic Alliance for the Implementation of New Technologies (SAINT); JPL R TD program; ERC Starting Grant under FP7; ERC [307209]; STFC (U.K.); South Africa National Research Foundation; CONICYT [PFB-06] FX Support for the QUIET instrument and operation comes through the NSF cooperative agreement AST-0506648. Support was also provided by NSF awards PHY-0355328, AST-0448909, AST-1010016, and PHY-0551142; KAKENHI 20244041, 20740158, and 21111002; PRODEX C90284; a KIPAC Enterprise grant; and by the Strategic Alliance for the Implementation of New Technologies (SAINT). This work was performed on the Abel cluster, owned and maintained by the University of Oslo and NOTUR (the Norwegian High Performance Computing Consortium). Portions of this work were performed at the Jet Propulsion Laboratory (JPL) and California Institute of Technology, operating under a contract with the National Aeronautics and Space Administration. The Q-band polarimeter modules were developed using funding from the JPL R & TD program. H.K.E. acknowledges an ERC Starting Grant under FP7. C.D. and M.V. acknowledge support from an ERC Starting Grant (no. 307209). C.D. also acknowledges support from the STFC (U.K.). J.Z. gratefully acknowledges a South Africa National Research Foundation Square Kilometre Array Research Fellowship. L.B. acknowledges support from CONICYT Grant PFB-06. A.D.M. acknowledges a Sloan Fellowship. NR 58 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 OCT 1 PY 2015 VL 811 IS 2 AR 89 DI 10.1088/0004-637X/811/2/89 PG 21 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CU4QE UT WOS:000363513800017 ER PT J AU Tian, H Young, PR Reeves, KK Chen, B Liu, W McKillop, S AF Tian, Hui Young, Peter R. Reeves, Katharine K. Chen, Bin Liu, Wei McKillop, Sean TI TEMPORAL EVOLUTION OF CHROMOSPHERIC EVAPORATION: CASE STUDIES OF THE M1.1 FLARE ON 2014 SEPTEMBER 6 AND X1.6 FLARE ON 2014 SEPTEMBER 10 SO ASTROPHYSICAL JOURNAL LA English DT Article DE line: profiles; magnetic reconnection; Sun: chromosphere; Sun: flares; Sun: transition region ID REGION-IMAGING-SPECTROGRAPH; CORONAL DIAGNOSTIC SPECTROMETER; LOOP RADIATIVE HYDRODYNAMICS; GENERAL SPECTRAL PROPERTIES; ANGSTROM WAVELENGTH RANGE; HIGH TIME RESOLUTION; WHITE-LIGHT FLARE; X-RAY-SPECTRA; SOLAR-FLARE; MAGNETIC RECONNECTION AB With observations from the Interface Region Imaging Spectrograph, we track the complete evolution of similar to 11MK evaporation flows in an M1.1 flare on 2014 September 6 and an X1.6 flare on 2014 September 10. These hot flows, as indicated by the blueshifted Fe XXI 1354.08 angstrom line, evolve smoothly with a velocity decreasing exponentially from similar to 200 km s(-1) to almost stationary within a few minutes. We find a good correlation between the flow velocity and energy deposition rate as represented by the hard X-ray flux observed with the Reuven Ramaty High Energy Solar Spectroscopic Imager, or time derivative of the soft X-ray flux observed with the Geostationary Operational Environmental Satellites and the HINODE X-ray Telescope, which is in general agreement with models of nonthermal electron heating. The maximum blueshift of Fe XXI appears approximately at the same time as or slightly after the impulsive enhancement of the ultraviolet continuum and the Mg II 2798.8 angstrom line emission, demonstrating that the evaporation flow is closely related to heating of the lower chromosphere. Finally, while the hot Fe XXI 1354.08 angstrom line is entirely blueshifted with no obvious rest component, cool chromospheric and transition region lines like Si IV 1402.77 angstrom are often not entirely redshifted but just reveal an obvious red wing enhancement at the ribbons, suggesting that the speed of chromospheric condensation might be larger than previously thought. C1 [Tian, Hui; Reeves, Katharine K.; Chen, Bin; McKillop, Sean] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Young, Peter R.] George Mason Univ, Coll Sci, Fairfax, VA 22030 USA. [Liu, Wei] Lockheed Martin Solar & Astrophys Lab, Palo Alto, CA 94305 USA. [Liu, Wei] Stanford Univ, WW Hansen Expt Phys Lab, Stanford, CA 94305 USA. RP Tian, H (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM hui.tian@cfa.harvard.edu OI Reeves, Katharine/0000-0002-6903-6832 FU ESA; Norwegian Space Centre; NASA from LMSAL [8100002705, NNM07AB07C, SP02H1701R]; NASA [NNX13AE06G, NNX15AJ93G]; NSF [AGS-1159353] FX IRIS is a NASA small explorer mission developed and operated by LMSAL with mission operations executed at NASA Ames Research Center and major contributions to downlink communications funded by ESA and the Norwegian Space Centre. Hinode is a Japanese mission developed and launched by ISAS/JAXA, with NAOJ as domestic partner and NASA and STFC (UK) as international partners. It is operated by these agencies in co-operation with ESA and the NSC (Norway). This work is supported by NASA contracts 8100002705, NNM07AB07C and SP02H1701R from LMSAL to SAO, NASA grants NNX13AE06G and NNX15AJ93G, and NSF grant AGS-1159353. H.T. thanks Fatima Rubio da Costa and Xin Cheng for insightful discussion. NR 94 TC 22 Z9 22 U1 5 U2 6 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD OCT 1 PY 2015 VL 811 IS 2 AR 139 DI 10.1088/0004-637X/811/2/139 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CU4QE UT WOS:000363513800067 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, pg 173, 2015) SO ASTROPHYSICAL JOURNAL LA English DT Correction C1 [Tripathi, Anjali; Murray-Clay, Ruth A.] Harvard Smithsonian Ctr Astrophys, 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 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD OCT 1 PY 2015 VL 811 IS 2 AR 159 DI 10.1088/0004-637X/811/2/159 PG 1 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CU4QE UT WOS:000363513800087 ER PT J AU Woolsey, LN Cranmer, SR AF Woolsey, L. N. Cranmer, S. R. TI TIME-DEPENDENT TURBULENT HEATING OF OPEN FLUX TUBES IN THE CHROMOSPHERE, CORONA, AND SOLAR WIND SO ASTROPHYSICAL JOURNAL LA English DT Article DE magnetohydrodynamics (MHD); solar wind; Sun: corona; Sun: magnetic fields; turbulence; waves ID ALFVEN-WAVE TURBULENCE; LOW-FREQUENCY WAVES; MAGNETOHYDRODYNAMIC TURBULENCE; MHD TURBULENCE; INTERSTELLAR-MEDIUM; DRIVEN MODEL; X-RAY; ENERGY; ACCELERATION; HOLES AB We investigate several key questions of plasma heating in open-field regions of the corona that connect to the solar wind. We present results for a model of Alfven-wave-driven turbulence for three typical open magnetic field structures: a polar coronal hole, an open flux tube neighboring an equatorial streamer, and an open flux tube near a strong-field active region. We compare time-steady, one-dimensional turbulent heating models against fully time-dependent three-dimensional reduced-magnetohydrodynamic modeling of BRAID. We find that the time-steady results agree well with time-averaged results from BRAID. The time dependence allows us to investigate the variability of the magnetic fluctuations and of the heating in the corona. The high-frequency tail of the power spectrum of fluctuations forms a power law whose exponent varies with height, and we discuss the possible physical explanation for this behavior. The variability in the heating rate is bursty and nanoflare-like in nature, and we analyze the amount of energy lost via dissipative heating in transient events throughout the simulation. The average energy in these events is 10(21.91) erg, within the "picoflare" range, and many events reach classical "nanoflare" energies. We also estimated the multithermal distribution of temperatures that would result from the heating-rate variability, and found good agreement with observed widths of coronal differential emission measure distributions. The results of the modeling presented in this paper provide compelling evidence that turbulent heating in the solar atmosphere by Alfven waves accelerates the solar wind in open flux tubes. C1 [Woolsey, L. N.; Cranmer, S. R.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Cranmer, S. R.] Univ Colorado, Dept Astrophys & Planetary Sci, Boulder, CO 80309 USA. RP Woolsey, LN (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM lwoolsey@cfa.harvard.edu FU National Science Foundation [DGE-1144152]; NSF SHINE [AGS-1259519]; Harvard Astronomy Department FX This material is based upon work supported by the National Science Foundation Graduate Research Fellowship under grant No. DGE-1144152 and by the NSF SHINE program under grant No. AGS-1259519. L.N.W. also thanks the Harvard Astronomy Department for the student travel grant and Loomis fund. The authors gratefully acknowledge Adriaan van Ballegooijen for many keen insights and for the development of the BRAID model. The authors also thank the anonymous reviewer for helpful comments and suggestions. NR 74 TC 5 Z9 5 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD OCT 1 PY 2015 VL 811 IS 2 AR 136 DI 10.1088/0004-637X/811/2/136 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CU4QE UT WOS:000363513800064 ER PT J AU Giam, X Hadiaty, RK Tan, HH Parenti, LR Wowor, D Sauri, S Chong, KY Yeo, DCJ Wilcove, DS AF Giam, Xingli Hadiaty, Renny K. Tan, Heok Hui Parenti, Lynne R. Wowor, Daisy Sauri, Sopian Chong, Kwek Yan Yeo, Darren C. J. Wilcove, David S. TI Mitigating the impact of oil-palm monoculture on freshwater fishes in Southeast Asia SO CONSERVATION BIOLOGY LA English DT Article DE agriculture; buffers; fishes; functional diversity; land sharing; riparian reserves; stream; structural equation model ID FUNCTIONAL DIVERSITY; BIODIVERSITY CONSERVATION; RIPARIAN RESERVES; MULTIPLE TRAITS; FOREST STREAMS; PLANTATIONS; ECOLOGY; ASSEMBLAGES; FRAMEWORK; MALAYSIA AB Anthropogenic land-cover change is driving biodiversity loss worldwide. At the epicenter of this crisis lies Southeast Asia, where biodiversity-rich forests are being converted to oil-palm monocultures. As demand for palm oil increases, there is an urgent need to find strategies that maintain biodiversity in plantations. Previous studies found that retaining forest patches within plantations benefited some terrestrial taxa but not others. However, no study has focused on aquatic taxa such as fishes, despite their importance to human well-being. We assessed the efficacy of forested riparian reserves in conserving freshwater fish biodiversity in oil-palm monoculture by sampling stream fish communities in an oil-palm plantation in Central Kalimantan, Indonesia. Forested riparian reserves maintained preconversion local fish species richness and functional diversity. In contrast, local and total species richness, biomass, and functional diversity declined markedly in streams without riparian reserves. Mechanistically, riparian reserves appeared to increase local species richness by increasing leaf litter cover and maintaining coarse substrate. The loss of fishes specializing in leaf litter and coarse substrate decreased functional diversity and altered community composition in oil-palm plantation streams that lacked riparian reserves. Thus, a land-sharing strategy that incorporates the retention of forested riparian reserves may maintain the ecological integrity of fish communities in oil-palm plantations. We urge policymakers and growers to make retention of riparian reserves in oil-palm plantations standard practice, and we encourage palm-oil purchasers to source only palm oil from plantations that employ this practice. C1 [Giam, Xingli; Wilcove, David S.] Princeton Univ, Dept Ecol & Evolut, Princeton, NJ 08544 USA. [Giam, Xingli; Tan, Heok Hui] Natl Univ Singapore, Lee Kong Chian Nat Hist Museum, Singapore S117546, Singapore. [Hadiaty, Renny K.; Wowor, Daisy; Sauri, Sopian] Indonesian Inst Sci, Biol Res Ctr, Museum Zool Bogoriense, Cibinong 16911, Indonesia. [Parenti, Lynne R.] Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Div Fishes, Washington, DC 20013 USA. [Chong, Kwek Yan; Yeo, Darren C. J.] Natl Univ Singapore, Dept Biol Sci, Singapore S117543, Singapore. [Wilcove, David S.] Princeton Univ, Woodrow Wilson Sch Publ & Int Affairs, Princeton, NJ 08544 USA. RP Giam, X (reprint author), Univ Washington, Sch Aquat & Fishery Sci, Seattle, WA 98105 USA. EM giamxingli@gmail.com; dwilcove@princeton.edu RI Kwek Yan, Chong/K-8375-2016; Yeo, Darren/H-9790-2012; OI Kwek Yan, Chong/0000-0003-4754-8957; Giam, Xingli/0000-0002-5239-9477 FU Wildlife Reserves Singapore; Mary and Randall Hack '69 Award; High Meadows Foundation; Rufford Foundation; Idea Wild; National Museum of Natural History, Smithsonian Institution FX This research was principally funded by a Wildlife Reserves Singapore grant and the Mary and Randall Hack '69 Award to X.G., and a High Meadows Foundation grant to D.S.W. Rufford Foundation and Idea Wild provided additional funding. The National Museum of Natural History, Smithsonian Institution, supported the