FN Thomson Reuters Web of Science™ VR 1.0 PT J AU Wilson, RM Rittenhouse, ST Bohn, JL AF Wilson, Ryan M. Rittenhouse, Seth T. Bohn, John L. TI A dielectric superfluid of polar molecules SO NEW JOURNAL OF PHYSICS LA English DT Article ID STATE AB We show that, under achievable experimental conditions, a Bose-Einstein condensate of polar molecules can exhibit dielectric character. In particular, we derive a set of self-consistent mean-field equations that couple the condensate density to its electric dipole field, leading to the emergence of polarization modes that are coupled to the rich quasi-particle spectrum of the condensate. While the usual roton instability is suppressed in this system, the coupling can give rise to a phonon-like instability that is characteristic of a dielectric material with a negative static dielectric function. C1 [Wilson, Ryan M.; Bohn, John L.] Univ Colorado, JILA, Boulder, CO 80309 USA. [Wilson, Ryan M.; Bohn, John L.] Univ Colorado, Dept Phys, Boulder, CO 80309 USA. [Rittenhouse, Seth T.] Harvard Smithsonian Ctr Astrophys, ITAMP, Cambridge, MA 02138 USA. RP Wilson, RM (reprint author), Univ Colorado, JILA, Boulder, CO 80309 USA. EM rmw@colorado.edu FU NSF through ITAMP at Harvard University; Smithsonian Astrophysical Observatory; NSF FX We acknowledge fruitful discussions with Hossein R Sadeghpour, Dominic Meiser and John Corson. STR acknowledges the financial support of an NSF grant through ITAMP at Harvard University and the Smithsonian Astrophysical Observatory. RMW and JLB acknowledge the financial support of the NSF. NR 26 TC 4 Z9 4 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 1367-2630 J9 NEW J PHYS JI New J. Phys. PD APR 17 PY 2012 VL 14 AR 043018 DI 10.1088/1367-2630/14/4/043018 PG 12 WC Physics, Multidisciplinary SC Physics GA 937QT UT WOS:000303673900006 ER PT J AU Stier, AC Gil, MA McKeon, CS Lemer, S Leray, M Mills, SC Osenberg, CW AF Stier, Adrian C. Gil, Michael A. McKeon, C. Seabird Lemer, Sarah Leray, Matthieu Mills, Suzanne C. Osenberg, Craig W. TI Housekeeping Mutualisms: Do More Symbionts Facilitate Host Performance? SO PLOS ONE LA English DT Article ID ANTAGONISTIC INTERACTIONS; SCLERACTINIAN CORALS; COMMUNITY STRUCTURE; SEDIMENT-REJECTION; AFRICAN SAVANNA; ANT-PLANT; GROWTH; BRACHYURA; PRODUCTIVITY; METAANALYSIS AB Mutualisms often involve one host supporting multiple symbionts, whose identity, density and intraguild interactions can influence the nature of the mutualism and performance of the host. However, the implications of multiple co-occurring symbionts on services to a host have rarely been quantified. In this study, we quantified effects of decapod symbionts on removal of sediment from their coral host. Our field survey showed that all common symbionts typically occur as pairs and never at greater abundances. Two species, the crab Trapezia serenei and the shrimp Alpheus lottini, were most common and co-occurred more often than expected by chance. We conducted a mesocosm experiment to test for effects of decapod identity and density on sediment removal. Alone, corals removed 10% of sediment, but removal increased to 30% and 48% with the presence of two and four symbionts, respectively. Per-capita effects of symbionts were independent of density and identity. Our results suggest that symbiont density is restricted by intraspecific competition. Thus, increased sediment removal from a coral host can only be achieved by increasing the number of species of symbionts on that coral, even though these species are functionally equivalent. Symbiont diversity plays a key role, not through added functionality but by overcoming density limitation likely imposed by intraspecific mating systems. C1 [Stier, Adrian C.; Gil, Michael A.; McKeon, C. Seabird; Osenberg, Craig W.] Univ Florida, Dept Biol, Gainesville, FL 32610 USA. [Lemer, Sarah; Leray, Matthieu; Mills, Suzanne C.] Univ Perpignan, Lab Excellence CORAIL, USR 3278, CNRS,EPHE,CBETM, F-66025 Perpignan, France. [McKeon, C. Seabird] Smithsonian Marine Stn, Smithsonian Inst Marine Sci Network, Ft Pierce, FL USA. RP Stier, AC (reprint author), Univ Florida, Dept Biol, Gainesville, FL 32610 USA. EM adrian.stier@gmail.com RI Osenberg, Craig/M-9904-2013; Mills, Suzanne/K-5538-2012; OI Osenberg, Craig/0000-0003-1918-7904 FU Partnership University Fund of the French American Cultural Exchange (Ocean Bridges Program); National Science Foundation [OCE-1130359, DGE-0802270] FX Financial support was provided by the Partnership University Fund of the French American Cultural Exchange (Ocean Bridges Program, http://facecouncil.org/puf/) and the National Science Foundation (Grant No. OCE-1130359; and a Graduate Research Fellowship awarded to Dr. Gil, Grant No. DGE-0802270) for financial support. The funders had no role in the study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 42 TC 13 Z9 13 U1 1 U2 32 PU PUBLIC LIBRARY SCIENCE PI SAN FRANCISCO PA 1160 BATTERY STREET, STE 100, SAN FRANCISCO, CA 94111 USA SN 1932-6203 J9 PLOS ONE JI PLoS One PD APR 16 PY 2012 VL 7 IS 4 AR e32079 DI 10.1371/journal.pone.0032079 PG 6 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 959VO UT WOS:000305345000005 PM 22523536 ER PT J AU Merot, C Collin, R AF Merot, Claire Collin, Rachel TI Effects of stress on sex change in Crepidula cf. marginalis (Gastropoda: Calyptraeidae) SO JOURNAL OF EXPERIMENTAL MARINE BIOLOGY AND ECOLOGY LA English DT Article DE Desiccation stress; Food stress; Panama; Plasticity; Protandry ID SOCIAL-CONTROL; SIZE; HERMAPHRODITE; ALLOCATION; RATIO; REPRODUCTION; ANIMALS; LIMPET; ADULT; FISH AB It is well known that interactions with conspecifics can affect the size and timing of sex change but the potential effects of other environmental influences on sex change are rarely examined. Sex allocation theory predicts that increased mortality rates should decrease the optimal size at sex change. Therefore we examined how stress (early starvation and exposure to desiccation) affects the size at sex change in Crepidula cf. marginalis a protandrous marine snail. Our results showed significant effects of early starvation on sex change: animals responded to early starvation by losing male characteristics earlier and at smaller sizes, remaining longer in the transitional phase, and becoming female at larger sizes than animals that were provided adequate food throughout. Desiccation on the other hand, decreased the size at which the female reproductive morphology was attained but no other effects were detected. The results of the desiccation treatment are consistent with theoretical predictions that higher mortality rates should decrease size at sex change. The starvation treatment seems to indicate that animals reduce the allocation to reproduction under extreme stress by entering a non-reproductive transitional stage earlier. Instead of regaining the male phase when conditions improved, they grew and rapidly completed the transition to the female phase. Published by Elsevier B.V. C1 [Merot, Claire; Collin, Rachel] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. [Merot, Claire] Ecole Normale Super, F-75005 Paris, France. RP Collin, R (reprint author), Smithsonian Trop Res Inst, Apartado Postal 0843-03092, Balboa, Ancon, Panama. EM collinr@si.edu OI Collin, Rachel/0000-0001-5103-4460 FU Smithsonian Tropical Research Institute FX We thank Maricela Salazar, Maria Fernanda Vinasco, Maria Lobato and especially Matt Starr for their help in the field and with animal maintenance. Matt Starr and Kaza Ansley commented on the manuscript and we thank them for their comments. This project was conducted as part of a masters internship (for CM.) and the work was supported by the Smithsonian Tropical Research Institute. NR 38 TC 6 Z9 6 U1 3 U2 20 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0022-0981 EI 1879-1697 J9 J EXP MAR BIOL ECOL JI J. Exp. Mar. Biol. Ecol. PD APR 15 PY 2012 VL 416 BP 68 EP 71 DI 10.1016/j.jembe.2012.02.012 PG 4 WC Ecology; Marine & Freshwater Biology SC Environmental Sciences & Ecology; Marine & Freshwater Biology GA 948MB UT WOS:000304506200009 ER PT J AU Power, ML Schulkin, J AF Power, Michael L. Schulkin, Jay TI Maternal obesity, metabolic disease, and allostatic load SO PHYSIOLOGY & BEHAVIOR LA English DT Article DE Maternal obesity; Placenta; Adipose; Metabolism ID 11-BETA-HYDROXYSTEROID DEHYDROGENASE TYPE-1; GESTATIONAL DIABETES-MELLITUS; ADIPOSE-TISSUE INFLAMMATION; CORTISOL METABOLISM; MACROPHAGE ACCUMULATION; INSULIN-RESISTANCE; PLACENTAL WEIGHTS; HUMAN-PREGNANCY; ADULT DISEASE; LEPTIN LEVELS AB Maternal obesity is a risk factor for many metabolic diseases for the mother, both during gestation and post partum, and for the child in later life. Obesity and pregnancy both result in altered physiological states, significantly different from the state of the non-obese, non-reproductive adult female. The concept of allostasis may be more appropriate for understanding the physiology of both pregnancy and obesity. In pregnancy these altered physiological states are adaptive, in both the evolutionary and physiological senses of the word. Obesity, however, represents a state outside of the adaptive evolutionary experience of our species. In both cases the altered physiological state derives at least in part from signals from an active endocrine organ. In obesity this is adipose tissue, and in pregnancy it is the placenta. The signaling molecules from adipose tissue and placenta all have multiple functions and can affect multiple organ systems. Placenta acts as a central regulator of metabolism for both the maternal and fetal compartments, in essence acting as a "third brain" during pregnancy. Both adipose tissue and placenta express many proinflammatory cytokines: obesity and pregnancy are states of low-grade inflammation. Both obesity and pregnancy are also states of insulin resistance, and maternal obesity is associated with fetal insulin resistance. We argue that obesity during pregnancy leads to sustained and inappropriate activation of normally adaptive regulatory circuits due in part to competing and conflicting signaling from adipose tissue and placenta. This results in allostatic load, leading to the eventual break down of regulatory mechanisms. The result is impaired metabolic function of the mother, and altered development of metabolic systems and potentially altered neural appetite circuits for the offspring. (C) 2011 Elsevier Inc. All rights reserved. C1 [Power, Michael L.; Schulkin, Jay] Amer Coll Obstetricians & Gynecologists, Dept Res, Washington, DC 20024 USA. [Power, Michael L.] Smithsonian Conservat Biol Inst, Conservat Ecol Ctr, Washington, DC 20008 USA. [Schulkin, Jay] Georgetown Univ, Dept Neurosci, Washington, DC 20057 USA. RP Power, ML (reprint author), Amer Coll Obstetricians & Gynecologists, Dept Res, 409 12th St SW, Washington, DC 20024 USA. EM mpower@acog.org OI Power, Michael/0000-0002-6120-3528 NR 78 TC 21 Z9 21 U1 2 U2 13 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0031-9384 J9 PHYSIOL BEHAV JI Physiol. Behav. PD APR 12 PY 2012 VL 106 IS 1 SI SI BP 22 EP 28 DI 10.1016/j.physbeh.2011.09.011 PG 7 WC Psychology, Biological; Behavioral Sciences SC Psychology; Behavioral Sciences GA 913XF UT WOS:000301910000004 PM 21939681 ER PT J AU Bailey, JI White, RJ Blake, CH Charbonneau, D Barman, TS Tanner, AM Torres, G AF Bailey, John I., III White, Russel J. Blake, Cullen H. Charbonneau, Dave Barman, Travis S. Tanner, Angelle M. Torres, Guillermo TI PRECISE INFRARED RADIAL VELOCITIES FROM KECK/NIRSPEC AND THE SEARCH FOR YOUNG PLANETS SO ASTROPHYSICAL JOURNAL LA English DT Article DE methods: data analysis; planets and satellites: formation; stars: pre-main sequence; starspots; techniques: radial velocities; techniques: spectroscopic ID LOW-MASS STARS; TW HYDRAE ASSOCIATION; GIANT PLANETS; BETA-PICTORIS; M DWARFS; GRAVITATIONAL-INSTABILITY; PROTOPLANETARY DISKS; SOLAR NEIGHBORHOOD; MAGNETIC-FIELDS; SEQUENCE STARS AB We present a high-precision infrared radial velocity (RV) study of late-type stars using spectra obtained with NIRSPEC at the W. M. Keck Observatory. RV precisions of 50 m s(-1) are achieved for old field mid-M dwarfs using telluric features for wavelength calibration. Using this technique, 20 young stars in the beta Pic (age similar to 12 Myr) and TW Hya (age similar to 8 Myr) Associations were monitored over several years to search for low-mass companions; we also included the chromospherically active field star GJ 873 (EV Lac) in this survey. Based on comparisons with previous optical observations of these young active stars, RV measurements at infrared wavelengths mitigate the RV noise caused by star spots by a factor of similar to 3. Nevertheless, star spot noise is still the dominant source of measurement error for young stars at 2.3 mu m, and limits the precision to similar to 77 m s(-1) for the slowest rotating stars (v sin i < 6 km s(-1)), increasing to similar to 168 m s(-1) for rapidly rotating stars (v sin i> 12 km s(-1)). The observations reveal both GJ 3305 and TWA 23 to be single-lined spectroscopic binaries; in the case of GJ 3305, the motion is likely caused by its 0 ''.09 companion, identified after this survey began. The large amplitude, short-timescale variations of TWA 13A are indicative of a hot Jupiter-like companion, but the available data are insufficient to confirm this. We label it as a candidate RV variable. For the remainder of the sample, these observations exclude the presence of any "hot" (P< 3 days) companions more massive than 8M(Jup) and any "warm" (P< 30 days) companions more massive than 17 M-Jup, on average. Assuming an edge-on orbit for the edge-on disk system AU Mic, these observations exclude the presence of any hot Jupiters more massive than 1.8 M-Jup or warm Jupiters more massive than 3.9 M-Jup. C1 [Bailey, John I., III] Univ Alabama, Dept Phys, Huntsville, AL 35899 USA. [White, Russel J.; Tanner, Angelle M.] Georgia State Univ, Dept Phys & Astron, Atlanta, GA 30303 USA. [Blake, Cullen H.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. [Charbonneau, Dave; Torres, Guillermo] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Barman, Travis S.] Lowell Observ, Flagstaff, AZ 86001 USA. RP Bailey, JI (reprint author), Univ Michigan, Dept Astron, 830 Dennison Bldg,500 Church St, Ann Arbor, MI 48109 USA. EM baileyji@umich.edu; white@chara.gsu.edu FU NSF/AAG [0908018] FX We are grateful to the support staff at Keck Observatory, especially Grant Hill and Jim Lyke, and to the scientists who built and continue to maintain NIRSPEC, especially Dr. Ian McLean. We appreciate the data provided by the NASA/IPAC Infrared Science Archive and the privilege to observe on the revered summit of Mauna Kea. This project was funded by NSF/AAG grant number 0908018. NR 108 TC 35 Z9 35 U1 0 U2 6 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD APR 10 PY 2012 VL 749 IS 1 AR 16 DI 10.1088/0004-637X/749/1/16 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 917KW UT WOS:000302175500016 ER PT J AU Conroy, C van Dokkum, P AF Conroy, Charlie van Dokkum, Pieter TI COUNTING LOW-MASS STARS IN INTEGRATED LIGHT (vol 747, pg 69, 2012) SO ASTROPHYSICAL JOURNAL LA English DT Correction C1 [Conroy, Charlie] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [van Dokkum, Pieter] Yale Univ, Dept Astrophys Sci, New Haven, CT USA. RP Conroy, C (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 1 TC 3 Z9 3 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD APR 10 PY 2012 VL 749 IS 1 AR 95 DI 10.1088/0004-637X/749/1/95 PG 3 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 917KW UT WOS:000302175500095 ER PT J AU Gautier, TN Charbonneau, D Rowe, JF Marcy, GW Isaacson, H Torres, G Fressin, F Rogers, LA Desert, JM Buchhave, LA Latham, DW Quinn, SN Ciardi, DR Fabrycky, DC Ford, EB Gilliland, RL Walkowicz, LM Bryson, ST Cochran, WD Endl, M Fischer, DA Howell, SB Horch, EP Barclay, T Batalha, N Borucki, WJ Christiansen, JL Geary, JC Henze, CE Holman, MJ Ibrahim, K Jenkins, JM Kinemuchi, K Koch, DG Lissauer, JJ Sanderfer, DT Sasselov, DD Seager, S Silverio, K Smith, JC Still, M Stumpe, MC Tenenbaum, P Van Cleve, J AF Gautier, Thomas N., III Charbonneau, David Rowe, Jason F. Marcy, Geoffrey W. Isaacson, Howard Torres, Guillermo Fressin, Francois Rogers, Leslie A. Desert, Jean-Michel Buchhave, Lars A. Latham, David W. Quinn, Samuel N. Ciardi, David R. Fabrycky, Daniel C. Ford, Eric B. Gilliland, Ronald L. Walkowicz, Lucianne M. Bryson, Stephen T. Cochran, William D. Endl, Michael Fischer, Debra A. Howell, Steve B. Horch, Elliott P. Barclay, Thomas Batalha, Natalie Borucki, William J. Christiansen, Jessie L. Geary, John C. Henze, Christopher E. Holman, Matthew J. Ibrahim, Khadeejah Jenkins, Jon M. Kinemuchi, Karen Koch, David G. Lissauer, Jack J. Sanderfer, Dwight T. Sasselov, Dimitar D. Seager, Sara Silverio, Kathryn Smith, Jeffrey C. Still, Martin Stumpe, Martin C. Tenenbaum, Peter Van Cleve, Jeffrey TI KEPLER-20: A SUN-LIKE STAR WITH THREE SUB-NEPTUNE EXOPLANETS AND TWO EARTH-SIZE CANDIDATES SO ASTROPHYSICAL JOURNAL LA English DT Article DE eclipses; planetary systems; stars: individual (Kepler-20, KIC 6850504, 2MASS J19104752+4220194) ID TRANSIT TIMING VARIATIONS; SPITZER-SPACE-TELESCOPE; 1ST 4 MONTHS; PLANET CANDIDATES; EXTRASOLAR PLANET; ADAPTIVE OPTICS; HD 189733B; PHOTOMETRIC VARIABILITY; INITIAL CHARACTERISTICS; UPSILON-ANDROMEDAE AB We present the discovery of the Kepler-20 planetary system, which we initially identified through the detection of five distinct periodic transit signals in the Kepler light curve of the host star 2MASS J19104752+4220194. From high-resolution spectroscopy of the star, we find a stellar effective temperature T-eff = 5455 +/- 100 K, a metallicity of [Fe/H] = 0.01 +/- 0.04, and a surface gravity of log g = 4.4 +/- 0.1. We combine these estimates with an estimate of the stellar density derived from the transit light curves to deduce a stellar mass of M-* = 0.912 +/- 0.034M(circle dot) and a stellar radius of R-* = 0.944(-0.095)(+0.060) R-circle dot. For three of the transit signals, we demonstrate that our results strongly disfavor the possibility that these result from astrophysical false positives. We accomplish this by first identifying the subset of stellar blends that reproduce the precise shape of the light curve and then using the constraints on the presence of additional stars from high angular resolution imaging, photometric colors, and the absence of a secondary component in our spectroscopic observations. We conclude that the planetary scenario is more likely than that of an astrophysical false positive by a factor of 2x10(5) (Kepler-20b), 1x10(5) (Kepler-20c), and 1.1x10(3) (Kepler-20d), sufficient to validate these objects as planetary companions. For Kepler-20c and Kepler-20d, the blend scenario is independently disfavored by the achromaticity of the transit: from Spitzer data gathered at 4.5 mu m, we infer a ratio of the planetary to stellar radii of 0.075 +/- 0.015 (Kepler-20c) and 0.065 +/- 0.011 (Kepler-20d), consistent with each of the depths measured in the Kepler optical bandpass. We determine the orbital periods and physical radii of the three confirmed planets to be 3.70 days and 1.91(-0.21)(+0.12) R-circle plus for Kepler-20b, 10.85 days and 3.07(-0.31)(+0.20) R-circle plus for Kepler-20c, and 77.61 days and 2.75(-0.30)(+0.17) R-circle plus for Kepler-20d. From multi-epoch radial velocities, we determine the masses of Kepler-20b and Kepler-20c to be 8.7 +/- 2.2M(circle plus) and 16.1 +/- 3.5M(circle plus), respectively, and we place an upper limit on the mass of Kepler-20d of 20.1M(circle plus) (2 sigma). C1 [Gautier, Thomas N., III] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Charbonneau, David; Torres, Guillermo; Fressin, Francois; Desert, Jean-Michel; Latham, David W.; Quinn, Samuel N.; Geary, John C.; Holman, Matthew J.; Sasselov, Dimitar D.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Rowe, Jason F.; Bryson, Stephen T.; Howell, Steve B.; Borucki, William J.; Christiansen, Jessie L.; Henze, Christopher E.; Ibrahim, Khadeejah; Koch, David G.; Lissauer, Jack J.; Sanderfer, Dwight T.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Marcy, Geoffrey W.; Isaacson, Howard; Silverio, Kathryn] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Rogers, Leslie A.; Seager, Sara] MIT, Dept Phys, Cambridge, MA 02139 USA. [Buchhave, Lars A.] Univ Copenhagen, Niels Bohr Inst, DK-2100 Copenhagen, Denmark. [Buchhave, Lars A.] Univ Copenhagen, Ctr Star & Planet Format, Nat Hist Museum Denmark, DK-1350 Copenhagen, Denmark. [Ciardi, David R.] CALTECH, NASA Exoplanet Sci Inst, Pasadena, CA 91125 USA. [Fabrycky, Daniel C.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. [Ford, Eric B.] Univ Florida, Dept Astron, Gainesville, FL 32111 USA. [Gilliland, Ronald L.] Penn State Univ, Dept Astron, Davey Lab 525, University Pk, PA 16802 USA. [Walkowicz, Lucianne M.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. [Cochran, William D.; Endl, Michael] Univ Texas Austin, McDonald Observ, Austin, TX 78712 USA. [Fischer, Debra A.] Yale Univ, Dept Astron, New Haven, CT 06511 USA. [Horch, Elliott P.] So Connecticut State Univ, Dept Phys, New Haven, CT 06515 USA. [Barclay, Thomas; Kinemuchi, Karen; Still, Martin] NASA, Ames Res Ctr, Bay Area Environm Res Inst, Moffett Field, CA 94035 USA. [Batalha, Natalie] San Jose State Univ, Dept Phys & Astron, San Jose, CA 95192 USA. [Jenkins, Jon M.; Smith, Jeffrey C.; Stumpe, Martin C.; Tenenbaum, Peter; Van Cleve, Jeffrey] NASA, Ames Res Ctr, SETI Inst, Moffett Field, CA 94035 USA. RP Gautier, TN (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM thomas.n.gautier@jpl.nasa.gov OI Buchhave, Lars A./0000-0003-1605-5666; Ciardi, David/0000-0002-5741-3047; /0000-0001-6545-639X; Fischer, Debra/0000-0003-2221-0861; Fabrycky, Daniel/0000-0003-3750-0183 FU NASA's Science Mission Directorate; NASA through JPL/Caltech; W. M. Keck Foundation FX Kepler was competitively selected as the tenth Discovery mission. Funding for this mission is provided by NASA's Science Mission Directorate. The authors thank many people who gave so generously of their time to make this mission a success. This work is also based in part on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. Support for this work was provided by NASA through an award issued by JPL/Caltech. We thank the Spitzer staff at IPAC and in particular Nancy Silbermann for scheduling the Spitzer observations of this program. Some of the data presented herein were obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California, and the National Aeronautics and Space Administration. The Observatory was made possible by the generous financial support of the W. M. Keck Foundation. NR 96 TC 65 Z9 65 U1 6 U2 30 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD APR 10 PY 2012 VL 749 IS 1 AR 15 DI 10.1088/0004-637X/749/1/15 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 917KW UT WOS:000302175500015 ER PT J AU Hermes, JJ Kilic, M Brown, WR Montgomery, MH Winget, DE AF Hermes, J. J. Kilic, Mukremin Brown, Warren R. Montgomery, M. H. Winget, D. E. TI TWO NEW TIDALLY DISTORTED WHITE DWARFS SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries: close; Galaxy: stellar content; stars: individual (SDSS J174140.49+652638.7, SDSS J211921.96-001825.8); stars: neutron; stars: variables: general; white dwarfs ID BINARY NLTT 11748; ECLIPSING BINARY; SYSTEM; HELIUM; STARS; DISCOVERY; KEPLER; VARIABILITY; EVOLUTION; COMPANION AB We identify two new tidally distorted white dwarfs (WDs), SDSS J174140.49+652638.7 and J211921.96-001825.8 (hereafter J1741 and J2119). Both stars are extremely low mass (ELM, <= 0.2 M-circle dot)WDs in short-period, detached binary systems. High-speed photometric observations obtained at the McDonald Observatory reveal ellipsoidal variations and Doppler beaming in both systems; J1741, with a minimum companion mass of 1.1 M-circle dot, has one of the strongest Doppler beaming signals ever observed in a binary system (0.59% +/- 0.06% amplitude). We use the observed ellipsoidal variations to constrain the radius of each WD. For J1741, the star's radius must exceed 0.074R(circle dot). For J2119, the radius exceeds 0.10R(circle dot). These indirect radius measurements are comparable to the radius measurements for the bloated WD companions to A-stars found by the Kepler spacecraft, and they constitute some of the largest radii inferred for any WD. Surprisingly, J1741 also appears to show a 0.23% +/- 0.06% reflection effect, and we discuss possible sources for this excess heating. Both J1741 and J2119 are strong gravitational wave sources, and the time-of-minimum of the ellipsoidal variations can be used to detect the orbital period decay. This may be possible on a timescale of a decade or less. C1 [Hermes, J. J.; Montgomery, M. H.; Winget, D. E.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA. [Hermes, J. J.; Montgomery, M. H.; Winget, D. E.] McDonald Observ, Ft Davis, TX 79734 USA. [Kilic, Mukremin] Univ Oklahoma, Homer L Dodge Dept Phys & Astron, Norman, OK 73019 USA. [Brown, Warren R.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Hermes, JJ (reprint author), Univ Texas Austin, Dept Astron, RLM 15308, Austin, TX 78712 USA. EM jjhermes@astro.as.utexas.edu FU NSF [AST-0909107]; Norman Hackerman Advanced Research Program [003658-0252-2009] FX The observations of J2119 in 2011 July were assisted by G. Miller, S. Wang, G. Earle, J. Pelletier, and A. Rost, undergraduate students at the University of Texas Freshmen Research Initiative. J.J.H., M.H.M., and D.E.W. gratefully acknowledge the support of the NSF under grant AST-0909107 and the Norman Hackerman Advanced Research Program under grant 003658-0252-2009. NR 35 TC 12 Z9 12 U1 0 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD APR 10 PY 2012 VL 749 IS 1 AR 42 DI 10.1088/0004-637X/749/1/42 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 917KW UT WOS:000302175500042 ER PT J AU Hsieh, BC Wang, WH Yan, HJ Lin, LW Karoji, H Lim, J Ho, PTP Tsai, CW AF Hsieh, Bau-Ching Wang, Wei-Hao Yan, Haojing Lin, Lihwai Karoji, Hiroshi Lim, Jeremy Ho, Paul T. P. Tsai, Chao-Wei TI THE TAIWAN ECDFS NEAR-INFRARED SURVEY: VERY BRIGHT END OF THE LUMINOSITY FUNCTION AT z > 7 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: evolution; galaxies: formation; galaxies: high-redshift ID LY-ALPHA EMITTERS; ULTRA-DEEP-FIELD; LYMAN-BREAK GALAXIES; STAR-FORMING GALAXIES; HUBBLE-SPACE-TELESCOPE; SIMILAR-TO 7-10; HIGH-REDSHIFT GALAXIES; STELLAR MASS DENSITY; YALE-CHILE MUSYC; DROPOUT GALAXIES AB The primary goal of the Taiwan ECDFS Near-Infrared Survey (TENIS) is to find well-screened galaxy candidates at z > 7 (z' dropout) in the Extended Chandra Deep Field-South (ECDFS). To this end, TENIS provides relatively deep J and K-s data (similar to 25.3 ABmag, 5 sigma) for an area of 0.5 x 0.5 deg. Leveraged with existing data at mid-infrared to optical wavelengths, this allows us to screen for the most luminous high-z objects, which are rare and thus require a survey over a large field to be found. We introduce new color selection criteria to select a z > 7 sample with minimal contaminations from low-z galaxies and Galactic cool stars; to reduce confusion in the relatively low angular resolution Infrared Array Camera (IRAC) images, we introduce a novel deconvolution method to measure the IRAC fluxes of individual sources. Illustrating perhaps the effectiveness at which we screen out interlopers, we find only one z > 7 candidate, TENIS-ZD1. The candidate has a weighted z(phot) of 7.8, and its colors and luminosity indicate a young (45M years old) starburst galaxy with a stellar mass of 3.2 x 10(10) M-circle dot. The result matches with the observational luminosity function analysis and the semianalytic simulation result based on the Millennium Simulations, which may over predict the volume density for high-z massive galaxies. The existence of TENIS-ZD1, if confirmed spectroscopically to be at z > 7, therefore poses a challenge to current theoretical models for how so much mass can accumulate in a galaxy at such a high redshift. C1 [Hsieh, Bau-Ching; Wang, Wei-Hao; Lin, Lihwai; Lim, Jeremy; Ho, Paul T. P.] Acad Sinica, Inst Astron & Astrophys, Taipei 106, Taiwan. [Yan, Haojing] Univ Missouri, Dept Phys & Astron, Columbia, MO 65211 USA. [Karoji, Hiroshi] Natl Astron Observ Japan, Mitaka, Tokyo 1818588, Japan. [Karoji, Hiroshi] Univ Tokyo, Inst Phys & Math Universe, Kashiwa, Chiba 2778583, Japan. [Lim, Jeremy] Univ Hong Kong, Dept Phys, Hong Kong, Hong Kong, Peoples R China. [Ho, Paul T. P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Tsai, Chao-Wei] CALTECH, Ctr Infrared Proc & Anal, Pasadena, CA 91125 USA. RP Hsieh, BC (reprint author), Acad Sinica, Inst Astron & Astrophys, POB 23-141, Taipei 106, Taiwan. FU National Science Council of Taiwan [98-2112-M-001-003-MY2, 99-2112-M-001-012-MY3]; Japanese Government FIRST FX We thank the referee for comments that greatly improved the manuscript. We are grateful to the CFHT staff for their help obtaining the data, and H. K. C. Yee and Y. T. Lin for useful discussions. This paper is based on observations obtained with the WIRCam, a joint project of CFHT, Taiwan, Korea, Canada, France, and the Canada-France-Hawaii Telescope (CFHT) which is operated by the National Research Council (NRC) of Canada, the Institute National des Sciences de l'Univers of the Centre National de la Recherche Scientifique of France, and the University of Hawaii. Access to the CFHT was made possible by the Ministry of Education, the National Science Council of Taiwan as part of the Cosmology and Particle Astrophysics (CosPA), the Institute of Astronomy and Astrophysics, Academia Sinica, and National Tsing Hua University, Taiwan. We gratefully acknowledge support from the National Science Council of Taiwan Grant 98-2112-M-001-003-MY2 (W.H.W.), 99-2112-M-001-012-MY3 (W.H.W), and Japanese Government FIRST program (H.K.). NR 78 TC 8 Z9 8 U1 1 U2 9 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD APR 10 PY 2012 VL 749 IS 1 AR 88 DI 10.1088/0004-637X/749/1/88 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 917KW UT WOS:000302175500088 ER PT J AU Kraft, RP Birkinshaw, M Nulsen, PEJ Worrall, DM Croston, JH Forman, WR Hardcastle, MJ Jones, C Murray, SS AF Kraft, R. P. Birkinshaw, M. Nulsen, P. E. J. Worrall, D. M. Croston, J. H. Forman, W. R. Hardcastle, M. J. Jones, C. Murray, S. S. TI AN ACTIVE GALACTIC NUCLEUS DRIVEN SHOCK IN THE INTRACLUSTER MEDIUM AROUND THE RADIO GALAXY 3C 310 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: individual (3C 310); galaxies: jets; hydrodynamics; X-rays: galaxies: clusters ID X-RAY-EMISSION; DEEP CHANDRA OBSERVATION; HOT-GAS; SOURCE COUNTERPARTS; GASEOUS ATMOSPHERE; PERSEUS CLUSTER; HIGH-RESOLUTION; SNAPSHOT SURVEY; COOLING-FLOW; JET AB We present results from a 57.6 ks Chandra observation of the cluster gas associated with the fat-double radio galaxy 3C 310. We find a surface brightness discontinuity in the gas outside the southern radio lobe that we attribute to a shock driven by the supersonic inflation of this lobe similar to 180 kpc from the nucleus. Modeling the surface brightness/density jump, the shock has Mach number 1.5-1.9, depending on the assumptions one makes about the density profile and the nature of the energy input. There are not sufficient counts in the image to detect conclusively the temperature jump associated with the shock. The total mechanical energy of the outburst is 5 x 10(60) erg. Assuming a Mach 1.9 shock, the age of the outburst is similar to 100 million yrs, and the time-averaged power of the outburst is similar to 1.3 x 10(45) erg s(-1). The power input is 100 times greater than the radiative losses of the gas within the radius of the shock. Most importantly, the equivalent heat input due to the entropy increase is roughly 10% of the thermal energy of the gas to the radius of the shock. 3C 310 is another example where regular outbursts of the observed strength with a duty cycle of 0.1 could offset the radiative losses of the gas near the Bondi radius and regulate feedback. We also detect a cool filamentary X-ray arm along the eastern periphery of the southern radio lobe. This arm is probably composed of low-entropy gas dredged up in the inflation of the radio plasma, similar to features seen in M87. C1 [Kraft, R. P.; Nulsen, P. E. J.; Forman, W. R.; Jones, C.; Murray, S. S.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Birkinshaw, M.; Worrall, D. M.] Univ Bristol, HH Wills Phys Lab, Bristol BS8 1TL, Avon, England. [Croston, J. H.] Univ Southampton, Sch Phys & Astron, Southampton SO17 1SJ, Hants, England. [Hardcastle, M. J.] Univ Hertfordshire, Sch Phys Astron & Math, Hatfield AL10 9AB, Herts, England. [Murray, S. S.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. RP Kraft, RP (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS 4, Cambridge, MA 02138 USA. RI Hardcastle, Martin/E-2264-2012; OI Hardcastle, Martin/0000-0003-4223-1117; Nulsen, Paul/0000-0003-0297-4493 FU NASA [NAS8-03060] FX This work was supported by NASA grant NAS8-03060. We thank the anonymous referee for comments that improved this manuscript. NR 46 TC 8 Z9 8 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD APR 10 PY 2012 VL 749 IS 1 AR 19 DI 10.1088/0004-637X/749/1/19 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 917KW UT WOS:000302175500019 ER PT J AU Murase, K Dermer, CD Takami, H Migliori, G AF Murase, Kohta Dermer, Charles D. Takami, Hajime Migliori, Giulia TI BLAZARS AS ULTRA-HIGH-ENERGY COSMIC-RAY SOURCES: IMPLICATIONS FOR TeV GAMMA-RAY OBSERVATIONS SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmic rays; galaxies: active; gamma rays: galaxies ID ACTIVE GALACTIC NUCLEI; LARGE-AREA TELESCOPE; EXTRAGALACTIC MAGNETIC-FIELDS; BL-LAC OBJECTS; SIMULTANEOUS MULTIWAVELENGTH OBSERVATIONS; SELF-COMPTON MODEL; RADIO GALAXY M87; MARKARIAN 501; X-RAY; NGC 1275 AB The spectra of BL Lac objects and Fanaroff-Riley I radio galaxies are commonly explained by the one-zone leptonic synchrotron self-Compton (SSC) model. Spectral modeling of correlated multiwavelength data gives the comoving magnetic field strength, the bulk outflow Lorentz factor, and the emission region size. Assuming the validity of the SSC model, the Hillas condition shows that only in rare cases such sources accelerate protons to much above 10(19) eV, so greater than or similar to 10(20) eV ultra-high-energy cosmic rays (UHECRs) are likely to be heavy ions if powered by this type of radio-loud active galactic nuclei (AGNs). Survival of nuclei is shown to be possible in TeV BL Lacs and misaligned counterparts with weak photohadronic emissions. Another signature of hadronic production is intergalactic UHECR-induced cascade emission, which is an alternative explanation of the TeV spectra of some extreme non-variable blazars such as 1ES 0229+200 or 1ES 1101-232. We study this kind of cascade signal, taking into account effects of the structured extragalactic magnetic fields in which the sources should be embedded. We demonstrate the importance of cosmic-ray deflections on the gamma-ray flux, and show that required absolute cosmic-ray luminosities are larger than the average UHECR luminosity inferred from UHECR observations and can even be comparable to the Eddington luminosity of supermassive black holes. Future TeV gamma-ray observations using the Cerenkov Telescope Array and the High Altitude Water Cerenkov detector array can test for UHECR acceleration by observing >25 TeV photons from relatively low redshift sources such as 1ES 0229+200, and greater than or similar to TeV photons from more distant radio-loud AGNs. C1 [Murase, Kohta] Ohio State Univ, Dept Phys, Ctr Cosmol & Astroparticle Phys, Columbus, OH 43210 USA. [Dermer, Charles D.] USN, Div Space Sci, Res Lab, Washington, DC 20375 USA. [Takami, Hajime] Max Planck Inst Phys & Astrophys, D-80805 Munich, Germany. [Migliori, Giulia] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Murase, K (reprint author), Ohio State Univ, Dept Phys, Ctr Cosmol & Astroparticle Phys, 174 W 18th Ave, Columbus, OH 43210 USA. RI Murase, Kohta/B-2710-2016 OI Murase, Kohta/0000-0002-5358-5642 FU JSPS; CCAPP; NRL; Office of Naval Research; National Aeronautics and Space Administration (NASA) [GO2-3148A, GO8-9125A, GO0-11133X] FX K.M. acknowledges financial support by a Grant-in-Aid from JSPS, CCAPP, and NRL. The work of C.D. is supported by the Office of Naval Research and NASA Fermi Guest Investigator grants. The work of G.M. is supported by the National Aeronautics and Space Administration through Chandra Award numbers GO2-3148A and GO8-9125A, GO0-11133X issued by the Chandra X-Ray Observatory Center. We thank John Beacom, Adrian Biland, Alexander Kusenko, Gernot Maier, and Soebur Razzaque for discussions. We are also grateful to the anonymous referee. NR 147 TC 70 Z9 71 U1 0 U2 10 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD APR 10 PY 2012 VL 749 IS 1 AR 63 DI 10.1088/0004-637X/749/1/63 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 917KW UT WOS:000302175500063 ER PT J AU Lepine, S DiStefano, R AF Lepine, Sebastien DiStefano, Rosanne TI ON THE DETECTABILITY OF A PREDICTED MESOLENSING EVENT ASSOCIATED WITH THE HIGH PROPER MOTION STAR VB 10 SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE astrometry; gravitational lensing: micro; planetary systems; stars: low-mass ID DIGITIZED SKY SURVEY; SPACE-INTERFEROMETRY-MISSION; PLANETARY SYSTEMS; MICROLENSING EVENTS; GALACTIC BULGE; DATA RELEASE; MASS PLANET; M-DWARFS; YR(-1); CANDIDATES AB Extrapolation of the astrometric motion of the nearby low-mass star VB 10 indicates that sometime in late 2011 December or during the first 2-3 months of 2012, the star will make a close approach to a background point source. Based on astrometric uncertainties, we estimate a 1 in 2 chance that the distance of closest approach rho(min) will be less than 100 mas, a 1 in 5 chance that rho(min) < 50 mas, and a 1 in 10 chance that rho(min) < 20 mas. The last would result in a microlensing event with a 6% magnification in the light from the background source and an astrometric shift of 3.3 mas. The lensing signal will however be significantly diluted by the light from VB 10, which is 1.5 mag brighter than the background source in B band, 5 mag brighter in I band, and 10 mag brighter in K band, making the event undetectable in all but the bluer optical bands. However, we show that if VB 10 happens to harbor a similar to 1 M-J planet on a moderately wide (approximate to 0.18 AU-0.84 AU) orbit, there is a chance (1% to more than 10%, depending on the distance of closest approach and orbital period and inclination) that a passage of the planet closer to the background source will result in a secondary event of higher magnification. The detection of secondary events could be made possible with a several-times-per-night multi-site monitoring campaign. C1 [Lepine, Sebastien] Amer Museum Nat Hist, Dept Astrophys, New York, NY 10024 USA. [Lepine, Sebastien] CUNY, New York, NY 10016 USA. [DiStefano, Rosanne] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Lepine, S (reprint author), Amer Museum Nat Hist, Dept Astrophys, Cent Pk W & 79th St, New York, NY 10024 USA. EM lepine@amnh.org; rd@cfa.harvard.edu FU United States National Science Foundation (NSF) at AMNH [AST 06-07757, AST 09-08419]; NSF at the CfA [AST 07-08924, AST 09-08878] FX This research was supported at AMNH by grants AST 06-07757 and AST 09-08419 from the United States National Science Foundation (NSF). Support was also provided in part by NSF grants AST 07-08924 and AST 09-08878 at the CfA. NR 35 TC 4 Z9 4 U1 1 U2 6 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD APR 10 PY 2012 VL 749 IS 1 AR L6 DI 10.1088/2041-8205/749/1/L6 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 917AA UT WOS:000302143100006 ER PT J AU Odeen, A Pruett-Jones, S Driskell, AC Armenta, JK Hastad, O AF Odeen, Anders Pruett-Jones, Stephen Driskell, Amy C. Armenta, Jessica K. Hastad, Olle TI Multiple shifts between violet and ultraviolet vision in a family of passerine birds with associated changes in plumage coloration SO PROCEEDINGS OF THE ROYAL SOCIETY B-BIOLOGICAL SCIENCES LA English DT Article DE UV vision; SWS1 opsin sequencing; plumage spectrophotometry; Maluridae; Malurus; fairy-wren ID SENSITIVE VISUAL PIGMENTS; CONE PHOTORECEPTOR DISTRIBUTION; OIL DROPLETS; SPECTRAL SENSITIVITY; MOLECULAR EVOLUTION; SEXUAL DICHROMATISM; OCULAR MEDIA; SWS1 OPSIN; PERCEPTION; VERTEBRATES AB Colour vision in diurnal birds falls into two discrete classes, signified by the spectral sensitivity of the violet- (VS) or ultraviolet-sensitive (UVS) short wavelength-sensitive type 1 (SWS1) single cone. Shifts between sensitivity classes are rare; three or four are believed to have happened in the course of avian evolution, one forming UVS higher passerines. Such shifts probably affect the expression of shortwave-dominated plumage signals. We have used genomic DNA sequencing to determine VS or UVS affinity in fairy-wrens and allies, Maluridae, a large passerine family basal to the known UVS taxa. We have also spectrophotometrically analysed male plumage coloration as perceived by the VS and UVS vision systems. Contrary to any other investigated avian genus, Malurus (fairy-wrens) contains species with amino acid residues typical of either VS or UVS cone opsins. Three bowerbird species (Ptilonorhynchidae) sequenced for outgroup comparison carry VS opsin genes. Phylogenetic reconstructions render one UVS gain followed by one or more losses as the most plausible evolutionary scenario. The evolution of avian ultraviolet sensitivity is hence more complex, as a single shift no longer explains its distribution in Passeriformes. Character correlation analysis proposes that UVS vision is associated with shortwave-reflecting plumage, which is widespread in Maluridae. C1 [Odeen, Anders] Uppsala Univ, Dept Anim Ecol, S-75236 Uppsala, Sweden. [Pruett-Jones, Stephen] Univ Chicago, Dept Ecol & Evolut, Chicago, IL 60637 USA. [Driskell, Amy C.] Smithsonian Inst, Natl Museum Nat Hist, Labs Analyt Biol, Suitland, MD 20746 USA. [Armenta, Jessica K.] Lone Star Coll CyFair, Dept Biol, Cypress, TX 77433 USA. [Hastad, Olle] Uppsala Univ, Dept Evolutionary Organismal Biol, S-75236 Uppsala, Sweden. [Hastad, Olle] Swedish Univ Agr Sci, Dept Anat Physiol & Biochem, S-75007 Uppsala, Sweden. RP Odeen, A (reprint author), Uppsala Univ, Dept Anim Ecol, Norbyvagen 18D, S-75236 Uppsala, Sweden. EM anders.odeen@ebc.uu.se FU Swedish Research Council Formas; National Science Foundation (USA); Wettenhall Foundation; Chicago Zoological Society; University of Chicago; Chevron Pty. Ltd.; Carl Tryggers Foundation for Scientific Research FX Niclas Kolm provided valuable help with the character correlation analysis. Comments from three anonymous reviewers improved an earlier version of this article. We thank the following institutions and individuals for provision of tissue samples: Museum Victoria, Australian Museum, Australian National Wildlife Collection (CSIRO), Western Australian Museum, University of Washington Burke Museum, Academy of Natural Sciences Philadelphia, University of Kansas Museum of Natural History and Biodiversity Research Centre, Jordan Karubian and Michael Webster. We also thank the Australian National Wildlife Collection (CSIRO), The Field Museum, Chicago and Museum Victoria for access to specimens for spectrophotometric measurement. This work was supported financially by the Swedish Research Council Formas to A.O. S.P.-J. received financial support from the National Science Foundation (USA), the Wettenhall Foundation, Chicago Zoological Society, University of Chicago and Chevron Pty. Ltd. J.A. was supported by the National Science Foundation (USA) and O.H. by the Carl Tryggers Foundation for Scientific Research. NR 48 TC 23 Z9 23 U1 7 U2 87 PU ROYAL SOC PI LONDON PA 6-9 CARLTON HOUSE TERRACE, LONDON SW1Y 5AG, ENGLAND SN 0962-8452 EI 1471-2954 J9 P ROY SOC B-BIOL SCI JI Proc. R. Soc. B-Biol. Sci. PD APR 7 PY 2012 VL 279 IS 1732 BP 1269 EP 1276 DI 10.1098/rspb.2011.1777 PG 8 WC Biology; Ecology; Evolutionary Biology SC Life Sciences & Biomedicine - Other Topics; Environmental Sciences & Ecology; Evolutionary Biology GA 899NJ UT WOS:000300822400003 PM 21976683 ER PT J AU Antoine, PO Marivaux, L Croft, DA Billet, G Ganerod, M Jaramillo, C Martin, T Orliac, MJ Tejada, J Altamirano, AJ Duranthon, F Fanjat, G Rousse, S Gismondi, RS AF Antoine, Pierre-Olivier Marivaux, Laurent Croft, Darin A. Billet, Guillaume Ganerod, Morgan Jaramillo, Carlos Martin, Thomas Orliac, Maeva J. Tejada, Julia Altamirano, Ali J. Duranthon, Francis Fanjat, Gregory Rousse, Sonia Salas Gismondi, Rodolfo TI Middle Eocene rodents from Peruvian Amazonia reveal the pattern and timing of caviomorph origins and biogeography SO PROCEEDINGS OF THE ROYAL SOCIETY B-BIOLOGICAL SCIENCES LA English DT Article DE South America; Hystricognathi; Mid-Eocene climatic optimum; phylogeny; Platyrrhini ID LAND MAMMAL AGE; NEW-WORLD; HYSTRICOGNATHOUS RODENTS; SOUTH-AMERICA; PRIMATES; DIVERSIFICATION; BIODIVERSITY; ARGENTINA; EVOLUTION; OLIGOCENE AB The long-term isolation of South America during most of the Cenozoic produced a highly peculiar terrestrial vertebrate biota, with a wide array of mammal groups, among which caviomorph rodents and platyrrhine primates are Mid-Cenozoic immigrants. In the absence of indisputable pre-Oligocene South American rodents or primates, the mode, timing and biogeography of these extraordinary dispersals remained debated. Here, we describe South America's oldest known rodents, based on a new diverse caviomorph assemblage from the late Middle Eocene (approx. 41 Ma) of Peru, including five small rodents with three stem caviomorphs. Instead of being tied to the Eocene/Oligocene global cooling and drying episode (approx. 34 Ma), as previously considered, the arrival of caviomorphs and their initial radiation in South America probably occurred under much warmer and wetter conditions, around the Mid-Eocene Climatic Optimum. Our phylogenetic results reaffirm the African origin of South American rodents and support a trans-Atlantic dispersal of these mammals during Middle Eocene times. This discovery further extends the gap (approx. 15 Myr) between first appearances of rodents and primates in South America. C1 [Antoine, Pierre-Olivier; Marivaux, Laurent; Orliac, Maeva J.] Univ Montpellier 2, CNRS, UMR 5554, Inst Sci Evolut,CC064, F-34095 Montpellier, France. [Fanjat, Gregory] Univ Montpellier 2, CNRS, FR 2035, CC060, F-34095 Montpellier, France. [Antoine, Pierre-Olivier; Rousse, Sonia] Univ Toulouse, UMR 5563, CNRS, IRD,UR 234, F-31400 Toulouse, France. [Croft, Darin A.] Case Western Reserve Univ, Dept Anat, Sch Med, Cleveland, OH 44106 USA. [Billet, Guillaume; Martin, Thomas] Univ Bonn, Steinmann Inst Geol Mineral & Palaontol, D-53115 Bonn, Germany. [Ganerod, Morgan] Geol Survey Norway, N-7491 Trondheim, Norway. [Jaramillo, Carlos] Smithsonian Trop Res Inst, Ctr Trop Paleoecol & Archeol, Balboa, Ancon, Panama. [Orliac, Maeva J.] SUNY Stony Brook, Dept Anat Sci, Stony Brook, NY 11794 USA. [Tejada, Julia; Altamirano, Ali J.; Salas Gismondi, Rodolfo] Univ Nacl Mayor San Marcos, Museo Hist Nat, Dept Paleontol Vertebrados, Lima 14, Peru. [Tejada, Julia] Inst Francais Etud Andines, Paris 18, France. [Duranthon, Francis] CNRS, Museum Hist Nat, AMIS, UMR 5288, F-31000 Toulouse, France. RP Antoine, PO (reprint author), Univ Montpellier 2, CNRS, UMR 5554, Inst Sci Evolut,CC064, F-34095 Montpellier, France. EM pierre-olivier.antoine@univ-montp2.fr FU CNRS; Toulouse University 'SPAM'; PALASIAFRICA [ANR-08-JCJC-0017]; Alexander von Humboldt-Foundation [ISEM 2011-126] FX We thank the IRD-PeruPetro Convention Programme, the Canaan Shipibo Native Community and Maple Gas Peru S.A. for access to the field, J.-L. Hartenberger, F. Delsuc, M. Steiper and O. Bertrand for fruitful discussion, P. Baby, M. Roddaz, C. Gautheron, Y. Calderon and L. Quiroz for help with fieldwork, F. Leite and D. Carvajal for their work on pollen, and C. Cazevieille (Centre de Ressources en Imagerie Cellulaire, Montpellier) for access to a scanning electron microscope facility. We are much indebted to R. Cifelli for having edited this article, as well as to C. de Muizon and E. F. Seiffert for their constructive remarks on an earlier version of the manuscript. P.-O.A. was supported by CNRS 'Eclipse 2', CNRS 'Paleo2' and Toulouse University 'SPAM'; L.M. and M.J.O. were supported by ANR-08-JCJC-0017 (PALASIAFRICA); G.B. and T.M. were supported by Alexander von Humboldt-Foundation, Bonn. Publication ISEM 2011-126. NR 42 TC 74 Z9 77 U1 2 U2 25 PU ROYAL SOC PI LONDON PA 6-9 CARLTON HOUSE TERRACE, LONDON SW1Y 5AG, ENGLAND SN 0962-8452 EI 1471-2954 J9 P ROY SOC B-BIOL SCI JI Proc. R. Soc. B-Biol. Sci. PD APR 7 PY 2012 VL 279 IS 1732 BP 1319 EP 1326 DI 10.1098/rspb.2011.1732 PG 8 WC Biology; Ecology; Evolutionary Biology SC Life Sciences & Biomedicine - Other Topics; Environmental Sciences & Ecology; Evolutionary Biology GA 899NJ UT WOS:000300822400009 PM 21993503 ER PT J AU Kapheim, KM Smith, AR Ihle, KE Amdam, GV Nonacs, P Wcislo, WT AF Kapheim, Karen M. Smith, Adam R. Ihle, Kate E. Amdam, Gro V. Nonacs, Peter Wcislo, William T. TI Physiological variation as a mechanism for developmental caste-biasing in a facultatively eusocial sweat bee SO PROCEEDINGS OF THE ROYAL SOCIETY B-BIOLOGICAL SCIENCES LA English DT Article DE Megalopta genalis; social evolution; division of labour; ground plan; caste determination; vitellogenin ID DIFFERENTIAL GENE-EXPRESSION; MEGALOPTA-GENALIS; SOCIAL-BEHAVIOR; APIS-MELLIFERA; WORKER CASTE; HONEY-BEES; MOLECULAR CHARACTERISTICS; ECUADORIA HYMENOPTERA; INSECT VITELLOGENINS; LIFE-HISTORY AB Social castes of eusocial insects may have arisen through an evolutionary modification of an ancestral reproductive ground plan, such that some adults emerge from development physiologically primed to specialize on reproduction (queens) and others on maternal care expressed as allo-maternal behaviour (workers). This hypothesis predicts that variation in reproductive physiology should emerge from ontogeny and underlie division of labour. To test these predictions, we identified physiological links to division of labour in a facultatively eusocial sweat bee, Megalopta genalis. Queens are larger, have larger ovaries and have higher vitellogenin titres than workers. We then compared queens and workers with their solitary counterparts-solitary reproductive females and dispersing nest foundresses-to investigate physiological variation as a factor in caste evolution. Within dyads, body size and ovary development were the best predictors of behavioural class. Queens and dispersers are larger, with larger ovaries than their solitary counterparts. Finally, we raised bees in social isolation to investigate the influence of ontogeny on physiological variation. Body size and ovary development among isolated females were highly variable, and linked to differences in vitellogenin titres. As these are key physiological predictors of social caste, our results provide evidence for developmental caste-biasing in a facultatively eusocial bee. C1 [Kapheim, Karen M.; Nonacs, Peter] Univ Calif Los Angeles, Dept Ecol & Evolutionary Biol, Los Angeles, CA 90095 USA. [Smith, Adam R.; Ihle, Kate E.; Wcislo, William T.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. [Ihle, Kate E.; Amdam, Gro V.] Arizona State Univ, Sch Life Sci, Tempe, AZ 85287 USA. [Amdam, Gro V.] Univ Life Sci, Dept Chem Biotechnol & Food Sci, N-1432 As, Norway. RP Kapheim, KM (reprint author), Univ Illinois, Dept Entomol, Inst Genom Biol, 1206 W Gregory, Urbana, IL 61801 USA. EM kapheimk@illinois.edu FU STRI; Smithsonian Institution; UCLA EEB; American Women in Science; US Department of Education; UCLA Graduate Division; Centre for Society and Genetics; NSF [IOS-0642085]; Secretaria Nacional de Ciencia, Tecnologia e Innovacion (SENACYT) of Panama [COL 06-030]; RCN [180504, 185306, 191699]; Wissenschaftskolleg zu Berlin; PEW Charitable Trust FX K.M.K. was supported by a Short Term Fellowship from STRI, a 10-week Graduate Fellowship and a Pre-doctoral Fellowship from the Smithsonian Institution, a Holmes O. Miller grant and a George Bartholomew fellowship from UCLA EEB, a Joan Wright Goodman award from American Women in Science, a GAANN fellowship from US Department of Education, a graduate Mentor fellowship from the UCLA Graduate Division, a graduate fellowship from the Centre for Society and Genetics, and an NSF Doctoral Dissertation Improvement Grant. K.M.K. and P.N. were also supported by NSF grant IOS-0642085. A.R.S. was supported by grant COL 06-030 from the Secretaria Nacional de Ciencia, Tecnologia e Innovacion (SENACYT) of Panama to W.T.W. and A.R.S., a fellowship to A.R.S. from the NSF International Research Fellowship Programme, and a Smithsonian Institution Post-doctoral fellowship. K.E.I. was supported by an NSF Doctoral Dissertation Improvement Grant and a STRI-Arizona State University Post-doctoral award. G.V.A. was supported by RCN nos 180504, 185306 and 191699, Wissenschaftskolleg zu Berlin, and the PEW Charitable Trust. Additional support was provided by general research funds from STRI to W.T.W. We would like to thank Julian Medina Gutierrez, Dyana La Rosa, Sandra Bernal, Damien Jose Ramirez Garcia and Timothy Alvey for assistance in the field, and Ting-Yan Chan for assistance in measuring bees in the laboratory. Oris Acevedo, Belkys Jimenez and Orelis Arosemena and the rest of the STRI staff provided valuable logistic support. Research on BCI was conducted with permission from the Autoridad Nacional del Ambiente under permit no. SEX/A-34-09, in accordance with the laws of the Republic of Panama. We thank Simon Tierney and two anonymous reviewers for useful comments on previous versions of this manuscript. NR 72 TC 18 Z9 19 U1 1 U2 27 PU ROYAL SOC PI LONDON PA 6-9 CARLTON HOUSE TERRACE, LONDON SW1Y 5AG, ENGLAND SN 0962-8452 EI 1471-2954 J9 P ROY SOC B-BIOL SCI JI Proc. R. Soc. B-Biol. Sci. PD APR 7 PY 2012 VL 279 IS 1732 BP 1437 EP 1446 DI 10.1098/rspb.2011.1652 PG 10 WC Biology; Ecology; Evolutionary Biology SC Life Sciences & Biomedicine - Other Topics; Environmental Sciences & Ecology; Evolutionary Biology GA 899NJ UT WOS:000300822400024 PM 22048951 ER PT J AU Linzmeier, AM Konstantinov, AS AF Linzmeier, Adelita M. Konstantinov, Alexander S. TI A new genus of leaf litter inhabiting Neotropical Monoplatina (Coleoptera: Chrysomelidae: Galerucinae: Alticini) SO ZOOTAXA LA English DT Article DE flea beetles; apterous; new genus; new species; leaf litter; Neotropical Region AB A new genus (Andersonaltica) containing five new species (A. denticulata, A. elongata, A. pecki-the type species of the genus, A. tuberosa, and A. valens) from Central America is described and illustrated. It is compared to Aedmon Clark, Apleuraltica Bechyne, Distigmoptera Blake, Hypolampsis Clark, and Pseudolampsis Horn and a key to identification of these genera is provided. C1 [Linzmeier, Adelita M.] Fundacao Univ Fed Grande Dourados, Fac Ciencias Biol & Ambientais, BR-79804980 Dourados, MS, Brazil. [Linzmeier, Adelita M.] ARS, Systemat Entomol Lab, USDA, Smithsonian Inst,Natl Museum Nat Hist, Washington, DC 20013 USA. RP Linzmeier, AM (reprint author), Fundacao Univ Fed Grande Dourados, Fac Ciencias Biol & Ambientais, Caixa Postal 322, BR-79804980 Dourados, MS, Brazil. EM alinzmeier@yahoo.com.br; alex.konstantinov@ars.usda.gov RI Linzmeier, Adelita/A-9239-2013 FU Smithsonian Institution Fellowship Office FX We are grateful to R. Anderson (Canadian Museum of Nature, Ottawa, Canada), J. T. Longino (The Evergreen State College, Olympia WA), and S. Peck (Ottawa, Canada) for their spectacular flea beetle collecting efforts over the years. We thank M. Buffington, M. L. Chamorro, and M. Gates (Systematic Entomology Laboratory, Washington, DC) for help with the digital cameras and image capture and editing. R. Kula and A. Norrbom (Systematic Entomology Laboratory, Washington, DC) and C. Staines (Department of Entomology, Smithsonian Institution, Washington DC, USA) thoroughly reviewed earlier versions of this manuscript and provided valuable suggestions. The Smithsonian Institution Fellowship Office granted a short term fellowship to the first author in March of 2011. USDA is an equal opportunity provider and employer. NR 5 TC 2 Z9 2 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 APR 6 PY 2012 IS 3260 BP 19 EP 32 PG 14 WC Zoology SC Zoology GA 939QL UT WOS:000303828100002 ER PT J AU Cai, ZN Liu, Y Liu, X Chance, K Nowlan, CR Lang, R Munro, R Suleiman, R AF Cai, Zhaonan Liu, Yi Liu, Xiong Chance, Kelly Nowlan, Caroline R. Lang, Ruediger Munro, Rosemary Suleiman, Raid TI Characterization and correction of Global Ozone Monitoring Experiment 2 ultraviolet measurements and application to ozone profile retrievals SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID POLARIZATION MEASUREMENTS; SPECTRAL-RESOLUTION; VALIDATION; SCATTERING; REFLECTANCE; TEMPERATURE; INSTRUMENT; SCIAMACHY; SPACE; MODE AB We present an assessment study of the Global Ozone Monitoring Experiment 2 (GOME-2) reflectance for the wavelength range 270-350 nm by comparing measurements with simulations calculated using the vector linearized discrete ordinate radiative transfer model (VLIDORT) and Microwave Limb Sounder (MLS) ozone profiles. The results indicate wavelength-and cross-track-position-dependent biases. GOME-2 reflectance is overestimated by 10% near 300 nm and by 15%-20% around 270 nm. Stokes fraction measurements made by onboard polarization measurement devices are also validated directly using the VLIDORT model. GOME-2 measurements agree well with the simulated Stokes fractions, with mean biases ranging from -1.0% to similar to 2.9%; the absolute differences are less than 0.05. Cloudiness-dependent biases suggest the existence of uncorrected stray-light errors that vary seasonally and latitudinally. Temporal analysis indicates that reflectance degradation began at the beginning of the mission; the reflectance degrades by 15% around 290 nm and by 2.2% around 325 nm from 2007 through 2009. Degradation shows wavelength-and viewing-angle-dependent features. Preliminary validation of ozone profile retrievals with MLS, Michelson Interferometer for Passive Atmospheric Sounding, and ozonesonde reveals that the application of radiometric recalibration improves the ozone profile retrievals as well as reduces fitting residuals by 30% in band 2b. C1 [Cai, Zhaonan; Liu, Yi] Chinese Acad Sci, Key Lab Middle Atmosphere & Global Environm Obser, Inst Atmospher Phys, Beijing 100029, Peoples R China. [Liu, Xiong; Chance, Kelly; Nowlan, Caroline R.; Suleiman, Raid] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Lang, Ruediger; Munro, Rosemary] EUMETSAT, D-64295 Darmstadt, Germany. RP Cai, ZN (reprint author), Chinese Acad Sci, Key Lab Middle Atmosphere & Global Environm Obser, Inst Atmospher Phys, Beijing 100029, Peoples R China. EM liuyi@mail.iap.ac.cn RI Liu, Xiong/P-7186-2014 OI Nowlan, Caroline/0000-0002-8718-9752; Chance, Kelly/0000-0002-7339-7577; Liu, Xiong/0000-0003-2939-574X FU National Science Foundation of China [41075014]; Public Meteorology Special Foundation of MOST [GYHY201106045]; NASA; Smithsonian Institution FX This study was supported by the National Science Foundation of China under grant 41075014 and the Public Meteorology Special Foundation of MOST (grant GYHY201106045). Research at the Smithsonian Astrophysical Observatory was funded by NASA and the Smithsonian Institution. We thank EUMETSAT for providing GOME-2 level 1 data and the OMI science team, MLS science team, and WOUDC for providing the satellite data and ozonesonde data. We thank C. G. Wang, H. B. Chen, and C. J. Bian for providing ozonesonde data at Beijing. We also thank R. J. D. Spurr for providing the VLIDORT code. NR 47 TC 17 Z9 19 U1 0 U2 8 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD APR 5 PY 2012 VL 117 AR D07305 DI 10.1029/2011JD017096 PG 16 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 922EC UT WOS:000302528600005 ER PT J AU Hystad, P Demers, PA Johnson, KC Brook, J van Donkelaar, A Lamsal, L Martin, R Brauer, M AF Hystad, Perry Demers, Paul A. Johnson, Kenneth C. Brook, Jeff van Donkelaar, Aaron Lamsal, Lok Martin, Randall Brauer, Michael TI Spatiotemporal air pollution exposure assessment for a Canadian population-based lung cancer case-control study SO ENVIRONMENTAL HEALTH LA English DT Article DE Air pollution; Canada; Exposure assessment; Lung cancer; Residential mobility; Spatiotemporal ID LONG-TERM EXPOSURE; RESIDENTIAL-MOBILITY; DRINKING-WATER; FOLLOW-UP; MORTALITY; DISEASE; RISK; LYMPHOMA; CITIES; COHORT AB Background: Few epidemiological studies of air pollution have used residential histories to develop long-term retrospective exposure estimates for multiple ambient air pollutants and vehicle and industrial emissions. We present such an exposure assessment for a Canadian population-based lung cancer case-control study of 8353 individuals using self-reported residential histories from 1975 to 1994. We also examine the implications of disregarding and/or improperly accounting for residential mobility in long-term exposure assessments. Methods: National spatial surfaces of ambient air pollution were compiled from recent satellite-based estimates (for PM2.5 and NO2) and a chemical transport model (for O-3). The surfaces were adjusted with historical annual air pollution monitoring data, using either spatiotemporal interpolation or linear regression. Model evaluation was conducted using an independent ten percent subset of monitoring data per year. Proximity to major roads, incorporating a temporal weighting factor based on Canadian mobile-source emission estimates, was used to estimate exposure to vehicle emissions. A comprehensive inventory of geocoded industries was used to estimate proximity to major and minor industrial emissions. Results: Calibration of the national PM2.5 surface using annual spatiotemporal interpolation predicted historical PM2.5 measurement data best (R-2 = 0.51), while linear regression incorporating the national surfaces, a time-trend and population density best predicted historical concentrations of NO2 (R-2 = 0.38) and O-3 (R-2 = 0.56). Applying the models to study participants residential histories between 1975 and 1994 resulted in mean PM2.5, NO2 and O-3 exposures of 11.3 mu g/m(3) (SD = 2.6), 17.7 ppb (4.1), and 26.4 ppb (3.4) respectively. On average, individuals lived within 300 m of a highway for 2.9 years (15% of exposure-years) and within 3 km of a major industrial emitter for 6.4 years (32% of exposure-years). Approximately 50% of individuals were classified into a different PM2.5, NO2 and O-3 exposure quintile when using study entry postal codes and spatial pollution surfaces, in comparison to exposures derived from residential histories and spatiotemporal air pollution models. Recall bias was also present for self-reported residential histories prior to 1975, with cases recalling older residences more often than controls. Conclusions: We demonstrate a flexible exposure assessment approach for estimating historical air pollution concentrations over large geographical areas and time-periods. In addition, we highlight the importance of including residential histories in long-term exposure assessments. For submission to: Environmental Health C1 [Hystad, Perry; Brauer, Michael] Univ British Columbia, Sch Populat & Publ Hlth, Vancouver, BC V6T 1Z3, Canada. [Demers, Paul A.] Canc Care Ontario, Occupat Canc Res Ctr, Toronto, ON, Canada. [Johnson, Kenneth C.] Publ Hlth Agcy Canada, Ctr Chron Dis Prevent & Control, Sci Integrat Div, Toronto, ON, Canada. [Brook, Jeff] Air Qual Res Div, Toronto, ON, Canada. [van Donkelaar, Aaron] Dalhousie Univ, Dept Phys & Atmospher Sci, Halifax, NS B3H 3J5, Canada. [Lamsal, Lok] NASA, Goddard Space Flight Ctr, Atmospher Chem & Dynam Branch, Greenbelt, MD 20771 USA. [Martin, Randall] Harvard Smithsonian Ctr Astrophys, Cambridge, MA USA. [Martin, Randall] Dalhousie Univ, Dept Phys & Atmospher Sci, Halifax, NS B3H 3J5, Canada. RP Hystad, P (reprint author), Univ British Columbia, Sch Populat & Publ Hlth, 2206 E Mall, Vancouver, BC V6T 1Z3, Canada. EM phystad@gmail.com RI Lamsal, Lok/G-4781-2012; OI Brauer, Michael/0000-0002-9103-9343 FU UBC; Michael Smith Foundation for Health Research; Canadian Institute of Health Research FX We would like to thank: the Canadian Cancer Registries Epidemiologic Research Group for the lung cancer case-control data; the National Air Pollution Surveillance (NAPS) program for the air pollution monitoring data; and Qian Li and Ilan Levy for helping create the O3 spatial surface. PH is supported a UBC Bridge scholarship, a Michael Smith Foundation for Health Research senior graduate trainee award, and a Canadian Institute of Health Research Frederick Banting and Best research scholarship. NR 39 TC 21 Z9 22 U1 3 U2 38 PU BIOMED CENTRAL LTD PI LONDON PA 236 GRAYS INN RD, FLOOR 6, LONDON WC1X 8HL, ENGLAND SN 1476-069X J9 ENVIRON HEALTH-GLOB JI Environ. Health PD APR 4 PY 2012 VL 11 AR 22 DI 10.1186/1476-069X-11-22 PG 13 WC Environmental Sciences; Public, Environmental & Occupational Health SC Environmental Sciences & Ecology; Public, Environmental & Occupational Health GA 957GW UT WOS:000305149200001 PM 22475580 ER PT J AU Knapp, LW AF Knapp, Leslie W. TI Rogadius fehlmanni, a new flathead fish (Scorpaeniformes: Platycephalidae) from Somalia SO PROCEEDINGS OF THE BIOLOGICAL SOCIETY OF WASHINGTON LA English DT Article DE flathead fish; Pisces; western Indian Ocean AB Three species of Rogadius Jordan & Richardson, 1908, with antrorse preopercular spines have been previously known from the western Indian Ocean (WIO). A new species, Rogadius fehlmanni, is described from eight specimens taken at three localities off Somalia. It is distinguished from its congeners by the following combination of characters: lower edge of preopercle developed as a stout antrorse spine; preocular spines 2-4, usually with accessory spines on base of the largest; 5-6 diagonal scale rows between second dorsal fin and lateral line; pelvic fins blackish, lacking individual dark spots. A key separating the four species is provided. C1 Smithsonian Inst, Natl Museum Nat Hist, Div Fishes, MRC 534, Washington, DC 20013 USA. RP Knapp, LW (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Div Fishes, MRC 534, POB 37012, Washington, DC 20013 USA. EM knappl@si.edu NR 9 TC 0 Z9 0 U1 0 U2 0 PU BIOL SOC WASHINGTON PI WASHINGTON PA NAT MUSEUM NAT HIST SMITHSONIAN INST, WASHINGTON, DC 20560 USA SN 0006-324X J9 P BIOL SOC WASH JI Proc. Biol. Soc. Wash. PD APR 4 PY 2012 VL 125 IS 1 BP 61 EP 65 PG 5 WC Biology SC Life Sciences & Biomedicine - Other Topics GA 925JY UT WOS:000302758700006 ER PT J AU Britz, R Johnson, GD AF Britz, Ralf Johnson, G. David TI The caudal skeleton of a 20 mm Triodon and homology of its components SO PROCEEDINGS OF THE BIOLOGICAL SOCIETY OF WASHINGTON LA English DT Article DE Triodon; caudal fin; plesiomorphy; Tetraodontiformes; phylogeny ID ACTINOPTERYGIAN FISHES; TETRAODONTIFORMES; PLECTOGNATHI; REEVALUATION; TELEOSTEI; ELEMENTS AB We provide a detailed description of the caudal skeleton of the smallest specimen of a three-tooth puffer on record, a 20 mm standard length Triodon macropterus. The compound centrum supports the parhypural and five hypurals. Hypural five, which has a cartilaginous core, was interpreted erroneously by Tyler (1970, 1980) as uroneural 2, a structure that is not preformed in cartilage in acanthomorphs. We also found a second epural in Triodon, which was not reported by Tyler (1970, 1980). Both hypural 5 and epural 2 are also present in the two larger specimens of Triodon we studied. We discuss previous descriptions of the caudal-fin skeleton of Triodon and conclude by re-emphasizing the unexpectedly large number of putatively plesiomorphic characters of Triodon compared to all other plectognaths. C1 [Britz, Ralf] Nat Hist Museum, Dept Zool, London SW7 5BD, England. [Johnson, G. David] Smithsonian Inst, Natl Museum Nat Hist, Div Fishes, MRC 159, Washington, DC 20013 USA. RP Britz, R (reprint author), Nat Hist Museum, Dept Zool, Cromwell Rd, London SW7 5BD, England. EM r.britz@nhm.ac.uk NR 23 TC 3 Z9 3 U1 0 U2 4 PU BIOL SOC WASHINGTON PI WASHINGTON PA NAT MUSEUM NAT HIST SMITHSONIAN INST, WASHINGTON, DC 20560 USA SN 0006-324X J9 P BIOL SOC WASH JI Proc. Biol. Soc. Wash. PD APR 4 PY 2012 VL 125 IS 1 BP 66 EP 73 PG 8 WC Biology SC Life Sciences & Biomedicine - Other Topics GA 925JY UT WOS:000302758700007 ER PT J AU Zug, GR AF Zug, George R. TI A new species of treeskink (Squamata: Scincidae: Emoia samoensis species group) from Rotuma, south-central Pacific SO PROCEEDINGS OF THE BIOLOGICAL SOCIETY OF WASHINGTON LA English DT Article DE Fiji; lizard; Oceania; Pacific; Reptilia ID COOK ISLANDS AB Rotuma, the northern-most Fijian island, reportedly has two resident species of treeskinks of the Emoia samoensis species group. One species is a member of the Emoia concolor species subgroup and was last reported from Rotuma in the 1890s. The other species is a member of the Emoia samoensis subgroup. Members of the latter subgroup are robust-bodied skinks in contrast to the more slender-bodied concolor. The abundant treeskink on Rotuma is more slender-bodied than other samoensis subgroup members but clearly belongs to this subgroup. It possesses other differences, particularly in scalation, that demonstrate its differentiation and speciation in the remote and isolated Rotuma Islands. It is recognized herein as a new species Emoia oriva. A key to the members of the Emoia samoensis species group provides a current summary of phenetic relationships in this group although on-going studies suggest at least a half-dozen species remain undescribed in the samoensis species group. C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Washington, DC 20013 USA. RP Zug, GR (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, POB 37012, Washington, DC 20013 USA. EM zugg@si.edu FU Max & Victoria Dreyfus Foundation; Smithsonian Scholarly Studies Program; National Museum of Natural History; My home institution; Smithsonian Institution FX Our visit and biological survey on Rotuma was possible only through the courtesy of the chief and elders of the Malha'a District and Mr. Rave Fonmoa. We received encouragement and exceptional logistic support from the Fijian Marine Fisheries Laboratory of the Ministry of Primary Industries and its director Dr. A. E. Lewis. Additionally, field studies of the Fijian herpetofauna were approved and encouraged by the Ministry of Primary Industries, Forestry & Cooperatives. The Rotuman Survey was funded entirely by Max & Victoria Dreyfus Foundation.; My research into the biology and evolution of Pacific lizards received support from numerous sources, e.g., Smithsonian Scholarly Studies Program, and NMNH-Research Opportunities Fund. My home institution, the Smithsonian Institution and the National Museum of Natural History, provided decades of research support through its many bureaus, offices, branches, and especially its staff. I am most appreciative of this past and ongoing support. Thank you all. NR 8 TC 0 Z9 0 U1 1 U2 3 PU BIOL SOC WASHINGTON PI WASHINGTON PA NAT MUSEUM NAT HIST SMITHSONIAN INST, WASHINGTON, DC 20560 USA SN 0006-324X EI 1943-6327 J9 P BIOL SOC WASH JI Proc. Biol. Soc. Wash. PD APR 4 PY 2012 VL 125 IS 1 BP 74 EP 84 PG 11 WC Biology SC Life Sciences & Biomedicine - Other Topics GA 925JY UT WOS:000302758700008 ER PT J AU Olson, SL Wingate, DB AF Olson, Storrs L. Wingate, David B. TI A new species of towhee (Aves: Emberizidae: Pipilo) from Quaternary deposits on Bermuda SO PROCEEDINGS OF THE BIOLOGICAL SOCIETY OF WASHINGTON LA English DT Article DE extinction; fossil birds; Holocene; paleoecology; Pleistocene ID PLEISTOCENE; POECILOZONITES; GEOCHRONOLOGY; EVOLUTION; RALLIDAE; FOSSIL; GENUS AB Pipilo naufragus, new species, is described from Middle and Late Pleistocene to Holocene cave and pond deposits on the island of Bermuda. It is most similar to the Eastern Towhee P. erythrophthalmus but differs in having a heavier bill, more robust hindlimbs, and reduced wing and pectoral girdle, with the sternum in particular being shorter, wider, and with a much smaller carina. At least one early historical account (1610) contains a description of a large bunting-like bird that almost certainly refers to this species, which would have been exterminated by introduced pigs, rats, and cats following human settlement of Bermuda in 1612. C1 [Olson, Storrs L.] Smithsonian Inst, Dept Vertebrate Zool, Natl Museum Nat Hist, Div Birds NHB MRC 116, Washington, DC 20013 USA. [Wingate, David B.] Bermuda Nat Hist Museum, Flatts, Bermuda. RP Olson, SL (reprint author), Smithsonian Inst, Dept Vertebrate Zool, Natl Museum Nat Hist, Div Birds NHB MRC 116, POB 30712, Washington, DC 20013 USA. EM olsons@si.edu; davidb.wingate@gmail.com NR 28 TC 3 Z9 3 U1 1 U2 6 PU BIOL SOC WASHINGTON PI WASHINGTON PA NAT MUSEUM NAT HIST SMITHSONIAN INST, WASHINGTON, DC 20560 USA SN 0006-324X J9 P BIOL SOC WASH JI Proc. Biol. Soc. Wash. PD APR 4 PY 2012 VL 125 IS 1 BP 85 EP 96 PG 12 WC Biology SC Life Sciences & Biomedicine - Other Topics GA 925JY UT WOS:000302758700009 ER PT J AU Zug, GR Fisher, RN AF Zug, George R. Fisher, Robert N. TI A preliminary assessment of the Nactus pelagicus species group (Squamata: Gekkonidae) in New Guinea and a new species from the Admiralty Islands SO ZOOTAXA LA English DT Article DE Nactus pelagicus group; New Guinea; Admiralty Islands; morphology; geographic variation; new species ID PHYLOGENETIC-RELATIONSHIPS; GENUS NACTUS; POPULATIONS; LACERTILIA; COMPLEX; GECKOS AB The Slender-toed Geckos (Nactus) currently have four recognized species in New Guinea, and these species divide into two sister clades: a pelagicus clade and a vankampeni clade (Heinicke et al. 2010). The latter contains three dwarf species. The former consists of five bisexual populations, of which numerous New Guinea populations are uncharacterized nomenclaturally and lumped under the epithet 'pelagicus.' This report and description of a new species of the pelagicus group from Manus Island in the Admiralty Islands encourages us to offer a preliminary assessment of morphology and diversity in New Guinea 'pelagicus' populations. C1 [Zug, George R.] Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Washington, DC 20013 USA. [Fisher, Robert N.] US Geol Survey, Western Ecol Res Ctr, San Diego Field Stn, San Diego, CA 92101 USA. RP Zug, GR (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Washington, DC 20013 USA. EM zugg@si.edu; rfisher@usgs.gov FU SERDP; Smithsonian Scholarly Studies Program; NMNH FX Our research into the biology and evolution of Pacific lizards has received support from several sources: SERDP to RNF and the Smithsonian Scholarly Studies Program and NMNH-Research Opportunities Fund to GRZ. We thank these organization and their representatives for enabling our biodiversity research. Any use of trade, product, or firm names is for descriptive purposes only and does not imply an endorsement by the US Government. NR 21 TC 4 Z9 5 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 APR 4 PY 2012 IS 3257 BP 22 EP 37 PG 16 WC Zoology SC Zoology GA 939PM UT WOS:000303824700002 ER PT J AU Liu, XJ Swenson, NG Wright, SJ Zhang, LW Song, K Du, YJ Zhang, JL Mi, XC Ren, HB Ma, KP AF Liu, Xiaojuan Swenson, Nathan G. Joseph Wright, S. Zhang, Liwen Song, Kai Du, Yanjun Zhang, Jinlong Mi, Xiangcheng Ren, Haibao Ma, Keping TI Covariation in Plant Functional Traits and Soil Fertility within Two Species-Rich Forests SO PLOS ONE LA English DT Article ID WOOD SPECIFIC-GRAVITY; ECONOMICS SPECTRUM; GLOBAL PATTERNS; TROPICAL TREES; LEAF TRAITS; TRADE-OFF; SEED SIZE; WORLDWIDE; LATITUDE; CLIMATE AB The distribution of plant species along environmental gradients is expected to be predictable based on organismal function. Plant functional trait research has shown that trait values generally vary predictably along broad-scale climatic and soil gradients. This work has also demonstrated that at any one point along these gradients there is a large amount of interspecific trait variation. The present research proposes that this variation may be explained by the local-scale sorting of traits along soil fertility and acidity axes. Specifically, we predicted that trait values associated with high resource acquisition and growth rates would be found on soils that are more fertile and less acidic. We tested the expected relationships at the species-level and quadrat-level (20 x 20 m) using two large forest plots in Panama and China that contain over 450 species combined. Predicted relationships between leaf area and wood density and soil fertility were supported in some instances, but the majority of the predicted relationships were rejected. Alternative resource axes, such as light gradients, therefore likely play a larger role in determining the interspecific variability in plant functional traits in the two forests studied. C1 [Liu, Xiaojuan; Song, Kai; Du, Yanjun; Zhang, Jinlong; Mi, Xiangcheng; Ren, Haibao; Ma, Keping] Chinese Acad Sci, Inst Bot, State Key Lab Vegetat & Environm Change, Beijing, Peoples R China. [Swenson, Nathan G.] Michigan State Univ, Dept Plant Biol, E Lansing, MI 48824 USA. [Joseph Wright, S.] Smithsonian Trop Res Inst, Balboa, Panama. [Zhang, Liwen] Chinese Acad Sci, Yantai Inst Coastal Zone Res, Yantai, Shandong, Peoples R China. [Liu, Xiaojuan] Chinese Acad Sci, Grad Univ, Beijing, Peoples R China. RP Liu, XJ (reprint author), Chinese Acad Sci, Inst Bot, State Key Lab Vegetat & Environm Change, Beijing, Peoples R China. EM kpma@ibcas.ac.cn RI Swenson, Nathan/A-3514-2012; Wright, Stuart/M-3311-2013; Liu, Xiaojuan/B-4947-2017; OI Swenson, Nathan/0000-0003-3819-9767; Wright, Stuart/0000-0003-4260-5676; Zhang, Jinlong/0000-0002-1161-5460 FU Chinese Academy of Sciences [KZCX2-YW-430]; Center for Tropical Forest Science (CTFS); F. H. Levinson Fund; Biodiversity Committee of the Chinese Academy of Sciences; National Science Foundation; MacArthur Foundation; Smithsonian Tropical Research Institute FX This work was supported by a key innovation project of the Chinese Academy of Sciences (KZCX2-YW-430) and a research grant from the Center for Tropical Forest Science (CTFS). The F. H. Levinson Fund supported functional traits measurements at Barro Colorado Island (BCI). The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript.; We thank Fang Teng, Chen Shengwen, Lai Zhenxi and Jiang Zhiyong for species identification and data collection at Gutianshan. The Administration Bureau of the Gutianshan National Nature Reserve and the Smithsonian Tropical Research Institute provided local support. The Biodiversity Committee of the Chinese Academy of Sciences supported the GTS plot. The National Science Foundation, the MacArthur Foundation and the Smithsonian Tropical Research Institute supported the BCI plot. NR 45 TC 16 Z9 21 U1 7 U2 50 PU PUBLIC LIBRARY SCIENCE PI SAN FRANCISCO PA 1160 BATTERY STREET, STE 100, SAN FRANCISCO, CA 94111 USA SN 1932-6203 J9 PLOS ONE JI PLoS One PD APR 3 PY 2012 VL 7 IS 4 AR e34767 DI 10.1371/journal.pone.0034767 PG 9 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 952PZ UT WOS:000304805900058 PM 22509355 ER PT J AU Erwin, TL Ball, GE AF Erwin, Terry L. Ball, George E. TI Hybopteroides, a new genus in the Cryptobatida group of subtribe Agrina, with three new species and notes on their way of life (Insecta: Coleoptera, Carabidae, Lebiini) SO PAN-PACIFIC ENTOMOLOGIST LA English DT Article DE Ecuador; Peru; rainforest canopy/understory; Hyboptera Chaudoir; Thoasia Liebke; Embioptera ID GENERIC SYNOPSIS; NATURAL-HISTORY; RAIN-FOREST; BEETLES; CLASSIFICATION; CICINDINI; EVOLUTION; TRIBE AB Hybopteroides gen. nov., with three new species in the Cryptobatida group of subtribe Agrina, Lebiini, living in the lowland rain forest canopy of Ecuador and Peru are diagnosed, described and illustrated. The new genus is likely the adelphotaxon of Hyboptera Chaudoir 1872 + Thoasia Liebke 1939. Hybopteroides biolat sp. nov., the type species, is now known from the Rio Manu watershed in Peru; Hybopteroides karolynae sp. nov. is now known from the Rio Tambopata watershed in Peru; and Hybopteroides penrosei sp. nov. is now known from the upper and mid Rio Napo watershed in Ecuador. The species of this new genus are known from insecticidal fogging collections from the rainforest canopy and upper understory and from two specimens collected by E. S. Ross at his ecotourism lodge at Alinahui, Ecuador, found in his live embiid colonies. C1 [Erwin, Terry L.] Smithsonian Inst, Natl Museum Nat Hist, Hyperdivers Grp, Dept Entomol, Washington, DC 20013 USA. [Ball, George E.] Univ Alberta, EH Strickland Entomol Museum, Dept Biol Sci, Edmonton, AB T6G 2E9, Canada. RP Erwin, TL (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Hyperdivers Grp, Dept Entomol, MRC 187,POB 37012, Washington, DC 20013 USA. EM erwint@si.edu; gball@ualberta.ca NR 29 TC 0 Z9 0 U1 0 U2 4 PU PACIFIC COAST ENTOMOL SOC PI SAN FRANCISCO PA C/O CALIFORNIA ACADEMY SCIENCES, 875 HOWARD STREET, SAN FRANCISCO, CA 94103-3009 USA SN 0031-0603 J9 PAN-PAC ENTOMOL JI Pan-Pacific Entomol. PD APR PY 2012 VL 88 IS 2 BP 188 EP 201 PG 14 WC Entomology SC Entomology GA 009JD UT WOS:000309021200009 ER PT J AU Skevington, JH Thompson, FC AF Skevington, Jeffrey H. Thompson, F. Christian TI Review of New World Sericomyia (Diptera: Syrphidae), including description of a new species SO CANADIAN ENTOMOLOGIST LA English DT Review ID DNA BARCODES AB The 19 New World species of Sericomyia Meigen are reviewed, including one species new to North America (Sericomyia jakutica (Stackelberg)) and one previously undescribed species (Sericomyia vockerothi Skevington sp. nov. from Alberta, Minnesota, Northwest Territories, Quebec, and Yukon Territory). Mallota powelli Nayar and Cole is recognized as a junior synonym of Sericomyia flagrans (Osten Sacken). A description and illustrations of S. vockerothi and an illustrated key to New World Sericomyia are presented. DNA barcode data are presented for 14 New World species and a cytochrome oxidase subunit I gene tree is presented and discussed. Genetic evidence supports the contention that the subgenera of Sericomyia are not monophyletic. Arctophila Schiner and Conosyprhus Frey are thus proposed as junior synonyms of Sericomyia. C1 [Skevington, Jeffrey H.] Agr & Agri Food Canada, Canadian Natl Collect Insects Arachnids & Nematod, Ottawa, ON K1A 0C6, Canada. [Thompson, F. Christian] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20013 USA. RP Skevington, JH (reprint author), Agr & Agri Food Canada, Canadian Natl Collect Insects Arachnids & Nematod, 960 Carling Ave, Ottawa, ON K1A 0C6, Canada. EM jeffrey.skevington@agr.gc.ca FU Agriculture and Agri-Food Canada; International Barcode of Life Project (iBOL) through the Canadian Centre for DNA Barcoding, from the Ontario Genomics Institute, Genome Canada; Ontario Ministry of Research and Innovation; Natural Sciences and Engineering Research Council of Canada FX Thanks to Barry Flahey for producing the excellent genitalia drawings and to Scott Kelso for developing protocols for sequencing historical pinned specimens and for collecting the COI barcoding data for many of the species of Sericomyia. This study was supported by funding to Agriculture and Agri-Food Canada, the International Barcode of Life Project (iBOL) through the Canadian Centre for DNA Barcoding, from the Ontario Genomics Institute, Genome Canada, the Ontario Ministry of Research and Innovation, and the Natural Sciences and Engineering Research Council of Canada. NSERC Canpolin provided the framework for this and other current research on Syrphidae (this is Canpolin publication no. 22). The following curators and curatorial assistants provided specimens and data used in this study: V. Levesque-Beaudin (BIOUG), S.A. Marshall (DEBU), B. Hubley (ROME), and F. Sperling and D. Shpeley (UASM). Steve Marshall, Jason Dombroski, Dave Cheung, and John Davis provided some of the field photographs. We first discovered John's excellent photo of Sericomyia chalcopyga on BugGuide (http://bugguide.net). Martin Hauser, Ximo Menguel, Bradley Sinclair, and Robb Bennett reviewed the manuscript and helped to improve the final product. Skevington was responsible for the DNA work and took the lead in the preparation of the manuscript. Thompson contributed to the morphological work and the identification key. NR 50 TC 7 Z9 7 U1 1 U2 9 PU CAMBRIDGE UNIV PRESS PI NEW YORK PA 32 AVENUE OF THE AMERICAS, NEW YORK, NY 10013-2473 USA SN 0008-347X J9 CAN ENTOMOL JI Can. Entomol. PD APR PY 2012 VL 144 IS 2 BP 216 EP 247 DI 10.4039/tce.2012.24 PG 32 WC Entomology SC Entomology GA 984ZJ UT WOS:000307232200004 ER PT J AU Gelhaus, JK Ruggeri, A AF Gelhaus, Jon K. Ruggeri, Anthony TI A review of the crane fly genus Epiphragma (Diptera: Tipulidae s.l.) in North America (including Mexico) SO CANADIAN ENTOMOLOGIST LA English DT Article ID LIMONIIDAE AB This study examines the seven described species of Epiphragma Osten Sacken (Diptera: Tipulidae s.l.) known to occur in North America including Mexico. A key to species, descriptions, distributional ranges, habitat information, and literature references are given and the wing patterning and male genitalia are illustrated. The male of Epiphragma celator Alexander is described for the first time and the species range is extended north from Michoacan, Mexico to southern Arizona, United States of America. The range of Epiphragma arizonense Alexander is extended from southern Arizona south to Sinaloa, Mexico. The male hypopygium of Epiphragma nebulosum (Bellardi) and wing and hypopygium of Epiphragma oreonympha Alexander are illustrated for the first time. C1 [Gelhaus, Jon K.; Ruggeri, Anthony] Acad Nat Sci Philadelphia, Dept Entomol, Philadelphia, PA 19103 USA. [Gelhaus, Jon K.] Smithsonian Inst, Washington, DC 20560 USA. RP Gelhaus, JK (reprint author), Acad Nat Sci Philadelphia, Dept Entomol, 1900 Benjamin Franklin Pkwy, Philadelphia, PA 19103 USA. EM gelhaus@ansp.org NR 38 TC 0 Z9 0 U1 1 U2 3 PU CAMBRIDGE UNIV PRESS PI NEW YORK PA 32 AVENUE OF THE AMERICAS, NEW YORK, NY 10013-2473 USA SN 0008-347X EI 1918-3240 J9 CAN ENTOMOL JI Can. Entomol. PD APR PY 2012 VL 144 IS 2 BP 353 EP 375 DI 10.4039/tce.2012.32 PG 23 WC Entomology SC Entomology GA 984ZJ UT WOS:000307232200012 ER PT J AU Cardoso, I Lemaitre, R AF Cardoso, Irene Lemaitre, Rafael TI FIRST REPORTS OF DEEP-WATER HERMIT CRABS PARAPAGURUS SMITH, 1879 (DECAPODA, PARAPAGURIDAE) AND COELENTERATE ASSOCIATES FROM THE MID-ATLANTIC RIDGE AND SOUTH ATLANTIC SO CRUSTACEANA LA English DT Article ID PAGUROIDEA; ANOMURA AB Three species of deep water hermit crabs of the genus Parapagurus Smith, 1879, family Parapaguridae, were collected in the South Atlantic during studies of the fauna and ecology of the Mid-Atlantic Ridge, a seamount chain that is an important habitat, feeding ground, and site of reproduction for many open ocean and deep-sea species. The three species collected, P abyssorum (Filhol, 1885), P nudus (A. Milne-Edwards, 1891), and P pilosimanus Smith, 1879, are known to range broadly in the Atlantic, but only one, P. pilosimanus, was previously reported from the South Atlantic. Thus, P. abyssorum and P nudus arc reported for the first time from the Mid-Atlantic Ridge and the South Atlantic. These three species live in association with zoanthids or actinians that produce carcinoecia and serve as housing. The carcinoecia found with the specimens are also reported. C1 [Cardoso, Irene] Univ Fed Rio de Janeiro, Museu Nacl, Setor Carcinol, Dept Invertebrados, Rio de Janeiro, RJ, Brazil. [Lemaitre, Rafael] Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, Suitland, MD 20746 USA. RP Cardoso, I (reprint author), Univ Fed Rio de Janeiro, Museu Nacl, Setor Carcinol, Dept Invertebrados, Quinta da Boa Vista S-N, Rio de Janeiro, RJ, Brazil. EM irenecardoso@mn.ufrj.br; lemaitrr@si.edu RI Cardoso, Irene/F-4323-2014 OI Cardoso, Irene/0000-0001-7072-0175 NR 19 TC 4 Z9 4 U1 1 U2 6 PU BRILL ACADEMIC PUBLISHERS PI LEIDEN PA PLANTIJNSTRAAT 2, P O BOX 9000, 2300 PA LEIDEN, NETHERLANDS SN 0011-216X J9 CRUSTACEANA JI Crustaceana PD APR PY 2012 VL 85 IS 4-5 BP 591 EP 600 DI 10.1163/156854012X634384 PG 10 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA 967SU UT WOS:000305928900012 ER PT J AU Ferrari, FD AF Ferrari, Frank D. TI IMPORTANCE OF MODELS OF DEVELOPMENT FOR DETERMINING HOMOLOGIES SO CRUSTACEANA LA English DT Article ID COPEPODS; LIMBS; BRANCHIOPODA; MORPHOLOGY; CRUSTACEA C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, Suitland, MD 20746 USA. RP Ferrari, FD (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, MRC-534,4210 Silver Hill Rd, Suitland, MD 20746 USA. EM ferrarif@si.edu NR 14 TC 0 Z9 0 U1 0 U2 0 PU BRILL ACADEMIC PUBLISHERS PI LEIDEN PA PLANTIJNSTRAAT 2, P O BOX 9000, 2300 PA LEIDEN, NETHERLANDS SN 0011-216X EI 1568-5403 J9 CRUSTACEANA JI Crustaceana PD APR PY 2012 VL 85 IS 4-5 BP 617 EP 620 DI 10.1163/156854012X643744 PG 4 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA 967SU UT WOS:000305928900015 ER PT J AU Nakatani, A Kondo, S Hayashida, S Nagashima, T Sudo, K Liu, X Chance, K Hirota, I AF Nakatani, Aya Kondo, Sayako Hayashida, Sachiko Nagashima, Tatsuya Sudo, Kengo Liu, Xiong Chance, Kelly Hirota, Isamu TI Enhanced Mid-Latitude Tropospheric Column Ozone over East Asia: Coupled Effects of Stratospheric Ozone Intrusion and Anthropogenic Sources SO JOURNAL OF THE METEOROLOGICAL SOCIETY OF JAPAN LA English DT Article ID SATELLITE DATA; GLOBAL-MODEL; TRANSPORT; CHEMISTRY; EMISSIONS; TRACE; OZONESONDES; SIMULATION; INVENTORY; TROPICS AB We analyze tropospheric column ozone (TCO) data observed by satellite instruments over East Asia for 15 years (from 1995 to 2009), and investigate the relationship between enhanced TCO (E-TCO) and ozone intrusion from the stratosphere near the subtropical jet (STJ). A belt of E-TCO is observed at mid-latitude over East Asia throughout the year; the belt is located at latitudes approximately equal to that of the STJ on seasonal, monthly, and daily timescales. The observed results are compared with a tagged tracer simulation by using a global chemical transport model. The simulation for East Asia indicates that the contribution from tropospheric origin to the enhancement of TCO is comparable to that from stratospheric origin at latitudes close to the STJ, resulting in the high correlation of the E-TCO belt and the STJ. The two origins of ozone cannot be differentiated in the tropospheric column ozone observed by a satellite, especially over East Asia where the anthropogenic source regions of ozone precursors are situated close to the latitudes of the STJ. Some occasional data, however, indicate split origins on a daily timescale, suggesting that the two origins really contribute to the enhancement of TCO. Our results strongly suggests an urgent need to develop a new satellite sensor and/or a new algorithm to distinguish boundary layer ozone from free tropospheric ozone in order to promote our understanding of atmospheric pollution over East Asia. C1 [Nakatani, Aya; Kondo, Sayako; Hayashida, Sachiko] Nara Womens Univ, Fac Sci, Nara 6308506, Japan. [Nagashima, Tatsuya] Natl Inst Environm Studies, Asian Environm Res Grp, Tsukuba, Ibaraki, Japan. [Sudo, Kengo] Nagoya Univ, Grad Sch Environm Studies, Nagoya, Aichi 4648601, Japan. [Liu, Xiong; Chance, Kelly] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Hirota, Isamu] Kyoto Univ, Kyoto, Japan. RP Hayashida, S (reprint author), Nara Womens Univ, Fac Sci, Kita Uoya Nishi Machi, Nara 6308506, Japan. EM sachiko@ics.nara-wu.ac.jp RI Liu, Xiong/P-7186-2014; OI Liu, Xiong/0000-0003-2939-574X; Chance, Kelly/0000-0002-7339-7577 FU Japan Society for the Promotion of Science (JSPS) [21540454]; Ministry of the Environment (MOE), Japan [S-7]; NASA; Smithsonian Institution FX Programs for determining the ozonesonde-based tropopause height were provided by Dr. Katsuyuki Noguchi. We thank Dr. Makoto Kuji for helpful discussions. This research was supported by the Grant-in-Aid for Scientific Research (C) 21540454 by the Japan Society for the Promotion of Science (JSPS) and the Global Environment Research Fund (S-7) by the Ministry of the Environment (MOE), Japan. The CHASER calculations were performed on the NIES supercomputer system (NEC SX-8R). Research at the SAO was supported by NASA and the Smithsonian Institution. NR 43 TC 5 Z9 5 U1 0 U2 10 PU METEOROLOGICAL SOC JAPAN PI TOKYO PA C/O JAPAN METEOROLOGICAL AGENCY 1-3-4 OTE-MACHI, CHIYODA-KU, TOKYO, 100-0004, JAPAN SN 0026-1165 EI 2186-9057 J9 J METEOROL SOC JPN JI J. Meteorol. Soc. Jpn. PD APR PY 2012 VL 90 IS 2 BP 207 EP 222 DI 10.2151/jmsj.2012-204 PG 16 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 964AB UT WOS:000305665000004 ER PT J AU Raymond, JC AF Raymond, J. C. TI X-rays from charge transfer in astrophysics: Overview SO ASTRONOMISCHE NACHRICHTEN LA English DT Article DE atomic processes; X-rays: ISM; X-rays: diffuse background ID EMISSION AB X-rays produced by charge transfer provide a major fraction of the soft X-ray background. If they contribute significantly to emission from other astrophysical sources, then model fits that ignore them will yield wrong answers, and an important diagnostic opportunity will be missed. Several recent papers suggest charge transfer contributions to observed X-ray spectra. This informal overview discusses analysis that might confirm the charge transfer interpretation and carry it toward the status of a useful diagnostic. (c) 2012 WILEY-VCH Verlag GmbH&Co. KGaA, Weinheim C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Raymond, JC (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM jraymond@cfa.harvard.edu NR 17 TC 3 Z9 3 U1 1 U2 3 PU WILEY-V C H VERLAG GMBH PI WEINHEIM PA BOSCHSTRASSE 12, D-69469 WEINHEIM, GERMANY SN 0004-6337 J9 ASTRON NACHR JI Astro. Nachr. PD APR PY 2012 VL 333 IS 4 BP 290 EP 291 DI 10.1002/asna.201211677 PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 959RE UT WOS:000305329700002 ER PT J AU Smith, RK Foster, AR Brickhouse, NS AF Smith, R. K. Foster, A. R. Brickhouse, N. S. TI Approximating the X-ray spectrum emitted from astrophysical charge exchange SO ASTRONOMISCHE NACHRICHTEN LA English DT Article DE atomic processes; radiation mechanism: non-thermal; solar wind; X-rays: general ID COLLISIONAL IONIZATION EQUILIBRIUM; SOLAR-WIND IONS; RATE COEFFICIENTS; LOCAL BUBBLE; EMISSION; RECOMBINATION; COMETS; ISM AB Charge exchange (CX), both onto ions in the solar wind and potentially in other astrophysical contexts, can create X-ray emission lines largely indistinguishable from those created in collisional or photoionized plasmas. The prime distinguishing characteristic is in the distinctly different line ratios generated by the CX process. A complete astrophysical model of the process would require a vast number of atomic calculations; we describe here an approximate approach that will allow astronomers to evaluate the likely contribution of CX to an observed spectrum. The method relies upon an approximate calculation of the CX cross section paired with detailed atomic structure calculations used to determine the emission lines. Simulated spectra based on observed solar wind CX data are shown for both current (Suzaku) and near-term (Astro-H) missions. (c) 2012 WILEY-VCH Verlag GmbH&Co. KGaA, Weinheim C1 [Smith, R. K.; Foster, A. R.; Brickhouse, N. S.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Smith, RK (reprint author), Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA. EM rsmith@cfa.harvard.edu RI XRAY, SUZAKU/A-1808-2009; OI Brickhouse, Nancy/0000-0002-8704-4473 FU NASA ADP [NNX09AC71G]; Chandra GO Theory program [TM4-5004X] FX We gratefully acknowledge many helpful discussions with John Raymond. Support for this project came from NASA ADP grant #NNX09AC71G and the Chandra GO Theory program, grant #TM4-5004X. NR 23 TC 14 Z9 14 U1 0 U2 4 PU WILEY-V C H VERLAG GMBH PI WEINHEIM PA POSTFACH 101161, 69451 WEINHEIM, GERMANY SN 0004-6337 EI 1521-3994 J9 ASTRON NACHR JI Astro. Nachr. PD APR PY 2012 VL 333 IS 4 BP 301 EP 304 DI 10.1002/asna.201211673 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 959RE UT WOS:000305329700005 ER PT J AU Raymond, JC AF Raymond, J. C. TI Charge transfer X-rays in solar and stellar flares SO ASTRONOMISCHE NACHRICHTEN LA English DT Article DE atomic processes; stars: flare; Sun: flares; Sun: particle emission; Sun: X-rays, gamma rays ID TRANSITION REGION EMISSION; WHITE-LIGHT; GAMMA-RAY; CHROMOSPHERIC EVAPORATION; PARTICLE-ACCELERATION; MAGNETIC RECONNECTION; IMPULSIVE PHASE; ALPHA EMISSION; SPECTROSCOPY; IONS AB Most of the energy in a solar flare, and presumably a stellar flare as well, takes the form of a power law of energetic particles. The energetic electrons produce a bremsstrahlung continuum, while the most energetic nuclei produce gamma-rays. Nuclei around 1 MeV/AMU can produce X-rays during and after charge transfer with neutrals. This paper predicts the fluxes for some prominent X-ray lines and compares them to existing spectra. (c) 2012 WILEY-VCH Verlag GmbH&Co. KGaA, Weinheim C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Raymond, JC (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM jraymond@cfa.harvard.edu FU NASA [NNX09AB17G-R] FX This work was performed under NASA grant NNX09AB17G-R to the Smithsonian Astrophysical Observatory. NR 39 TC 5 Z9 5 U1 0 U2 3 PU WILEY-V C H VERLAG GMBH PI WEINHEIM PA BOSCHSTRASSE 12, D-69469 WEINHEIM, GERMANY SN 0004-6337 J9 ASTRON NACHR JI Astro. Nachr. PD APR PY 2012 VL 333 IS 4 BP 305 EP 308 DI 10.1002/asna.201211670 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 959RE UT WOS:000305329700006 ER PT J AU Dennerl, K Lisse, CM Bhardwaj, A Christian, DJ Wolk, SJ Bodewits, D Zurbuchen, TH Combi, M Lepri, S AF Dennerl, K. Lisse, C. M. Bhardwaj, A. Christian, D. J. Wolk, S. J. Bodewits, D. Zurbuchen, T. H. Combi, M. Lepri, S. TI Solar system X-rays from charge exchange processes SO ASTRONOMISCHE NACHRICHTEN LA English DT Article DE atomic processes; comets: general; planets and satellites: general; radiation mechanism: non-thermal; solar wind; X-rays: general ID EXTREME-ULTRAVIOLET EMISSION; XMM-NEWTON; CHANDRA OBSERVATIONS; COMET HYAKUTAKE; 1ST OBSERVATION; DEEP-IMPACT; HEAVY-IONS; WIND; JUPITER; DISCOVERY AB While X-ray astronomy began in 1962 and has made fast progress since then in expanding our knowledge about where in the Universe X-rays are generated by which processes, it took one generation before the importance of a fundamentally different process was recognized. This happened in our immediate neighborhood, when in 1996 comets were discovered as a new class of X-ray sources, directing our attention to charge exchange reactions. Charge exchange is fundamentally different from other processes which lead to the generation of X-rays, because the X-rays are not produced by hot electrons, but by ions picking up electrons from cold gas. Thus it opens up a new window, making it possible to detect cool gas in X-rays (like in comets), while all the other processes require extremely high temperatures or otherwise extreme conditions. After having been overlooked for a long time, the astrophysical importance of charge exchange for the generation of X-rays is now receiving increased general attention. In our solar system, charge exchange induced X-rays have now been established to originate in comets, in all the planets from Venus to Jupiter, and even in the heliosphere itself. In addition to that, evidence for this X-ray emission mechanism has been found at various locations across the Universe. Here we summarize the current knowledge about solar system X-rays resulting from charge exchange processes. (c) 2012 WILEY-VCH Verlag GmbH&Co. KGaA, Weinheim C1 [Dennerl, K.] Max Planck Inst Extraterr Phys, D-85741 Garching, Germany. [Lisse, C. M.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. [Bhardwaj, A.] Vikram Sarabhai Space Ctr, Space Phys Lab, Trivandrum 695022, Kerala, India. [Christian, D. J.] Calif State Univ Northridge, Dept Phys & Astron, Northridge, CA 91330 USA. [Wolk, S. J.] Harvard Smithsonian Ctr Astrophys, Chandra Xray Ctr, Cambridge, MA 02138 USA. [Bodewits, D.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Zurbuchen, T. H.; Combi, M.; Lepri, S.] Univ Michigan, Ann Arbor, MI 48109 USA. RP Dennerl, K (reprint author), Max Planck Inst Extraterr Phys, Postfach 1312,Giessenbachstr, D-85741 Garching, Germany. EM kod@mpe.mpg.de RI Lepri, Susan/I-8611-2012; Combi, Michael/J-1697-2012; Lisse, Carey/B-7772-2016; OI Combi, Michael/0000-0002-9805-0078; Lisse, Carey/0000-0002-9548-1526; Bhardwaj, Anil/0000-0003-1693-453X; Wolk, Scott/0000-0002-0826-9261; Bodewits, Dennis/0000-0002-2668-7248; Christian, Damian/0000-0003-1746-3020 NR 63 TC 6 Z9 6 U1 0 U2 7 PU WILEY-V C H VERLAG GMBH PI WEINHEIM PA BOSCHSTRASSE 12, D-69469 WEINHEIM, GERMANY SN 0004-6337 J9 ASTRON NACHR JI Astro. Nachr. PD APR PY 2012 VL 333 IS 4 BP 324 EP 334 DI 10.1002/asna.201211663 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 959RE UT WOS:000305329700010 ER PT J AU Bodewits, D Christian, DJ Carter, JA Dennerl, K Ewing, I Hoekstra, R Lepri, ST Lisse, CM Wolk, SJ AF Bodewits, D. Christian, D. J. Carter, J. A. Dennerl, K. Ewing, I. Hoekstra, R. Lepri, S. T. Lisse, C. M. Wolk, S. J. TI Cometary charge exchange diagnostics in UV and X-ray SO ASTRONOMISCHE NACHRICHTEN LA English DT Article DE atomic processes; comets: general; radiation mechanism: non-thermal; solar wind ID ULTRAVIOLET-SPECTROSCOPIC-EXPLORER; C/HYAKUTAKE 1996 B2; SOLAR-WIND IONS; O1 HALE-BOPP; C/1999 S4; CHANDRA OBSERVATIONS; DEEP-IMPACT; XMM-NEWTON; EMISSION; HYAKUTAKE AB Since the initial discovery of cometary charge exchange emission, more than 20 comets have been observed with a variety of X-ray and UV observatories. This observational sample offers a broad variety of comets, solar wind environments and observational conditions. It clearly demonstrates that solar wind charge exchange emission provides a wealth of diagnostics, which are visible as spatial, temporal, and spectral emission features. We review the possibilities and limitations of each of those in this contribution. (c) 2012 WILEY-VCH Verlag GmbH&Co. KGaA, Weinheim C1 [Bodewits, D.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Christian, D. J.; Ewing, I.] Calif State Univ Northridge, Dept Phys & Astron, Northridge, CA 91330 USA. [Carter, J. A.] Univ Leicester, Dept Phys & Astron, Leicester LE1 1RH, Leics, England. [Dennerl, K.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Hoekstra, R.] Univ Groningen, KVI Atom Phys, NL-9747 AA Groningen, Netherlands. [Lepri, S. T.] Univ Michigan, Ann Arbor, MI 48109 USA. [Lisse, C. M.] JHU APL, Dept Space, Planetary Explorat Grp, Laurel, MD 20723 USA. [Wolk, S. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Bodewits, D (reprint author), Univ Maryland, Dept Astron, College Pk, MD 20742 USA. EM dennis@astro.umd.edu RI Hoekstra, Ronnie/E-9279-2012; Lepri, Susan/I-8611-2012; Lisse, Carey/B-7772-2016; OI Lisse, Carey/0000-0002-9548-1526; Wolk, Scott/0000-0002-0826-9261; Bodewits, Dennis/0000-0002-2668-7248; Christian, Damian/0000-0003-1746-3020 NR 65 TC 0 Z9 0 U1 0 U2 5 PU WILEY-V C H VERLAG GMBH PI WEINHEIM PA BOSCHSTRASSE 12, D-69469 WEINHEIM, GERMANY SN 0004-6337 J9 ASTRON NACHR JI Astro. Nachr. PD APR PY 2012 VL 333 IS 4 BP 335 EP 340 DI 10.1002/asna.201211659 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 959RE UT WOS:000305329700011 ER PT J AU Buzas, MA Parrish, M AF Buzas, Martin A. Parrish, Mary TI MEMORIAL TO LAWRENCE B. ISHAM (1922-2011) SO JOURNAL OF FORAMINIFERAL RESEARCH LA English DT Biographical-Item C1 [Buzas, Martin A.; Parrish, Mary] Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20013 USA. RP Buzas, MA (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, POB 37012,MRC 121, Washington, DC 20013 USA. NR 1 TC 0 Z9 0 U1 0 U2 1 PU CUSHMAN FOUNDATION FORAMINIFERAL RES PI CAMBRIDGE PA MUSEUM COMPARATIVE ZOOLOGY, DEPT INVERTEBRATE PALEONTOLOGY 26 OXFORD ST, HARVARD UNIV, CAMBRIDGE, MA 02138 USA SN 0096-1191 J9 J FORAMIN RES JI J. Foraminifer. Res. PD APR PY 2012 VL 42 IS 2 BP 107 EP 108 PG 2 WC Paleontology SC Paleontology GA 955SM UT WOS:000305041200001 ER PT J AU Culver, SJ Mallinson, DJ Corbett, DR Leorri, E Rouf, AA Shazili, NAM Yaacob, R Whittaker, JE Buzas, MA Parham, PR AF Culver, Stephen J. Mallinson, David J. Corbett, D. Reide Leorri, Eduardo Rouf, Ajm A. Shazili, Noor Azhar Mohd Yaacob, Rosnan Whittaker, John E. Buzas, Martin A. Parham, Peter R. TI DISTRIBUTION OF FORAMINIFERA IN THE SETIU ESTUARY AND LAGOON, TERENGGANU, MALAYSIA SO JOURNAL OF FORAMINIFERAL RESEARCH LA English DT Article ID BENTHIC FORAMINIFERA; BILBAO ESTUARY; ASSEMBLAGES; AQUACULTURE; POLLUTION; IMPACT; BAY; RECONSTRUCTIONS; ENVIRONMENTS; HISTORY AB The Setiu wetland of peninsular Malaysia is threatened by expansion of aquaculture. Water quality of the estuary-lagoon complex is becoming affected by nutrients introduced into the system at floating fish cages and by the clear-cutting of large areas of fringing mangrove forest for the creation of land-based fish and shrimp pens. We report here on the distribution of benthic foraminifera in the estuary-lagoon and related environmental variables. These data will form the baseline against which future environmental monitoring will be compared. Four thanatofacies are recognized by cluster analysis of the dead foraminiferal abundance data; their distribution is closely related to variations in salinity and other parameters related to the hydrodynamics of the region. This relation is confirmed by DCA and DCCA analyses. A low salinity estuarine thanatofacies (D1) has a low diversity assemblage dominated by the agglutinated taxa Ammotium directum, Trochammina amnicola, Miliammina fusca and Ammobaculites exiguus. A medium salinity lagoon thanatofacies (D2) has low diversity and is strongly dominated by the agglutinated Ammobaculites exiguus. Ammobaculites exiguus and Ammonia aff. A. aoteana dominate a high diversity, high salinity thanatofacies (D3) in both the estuary and the lagoon. A normal marine salinity thanatofacies (D4), found at an inlet and in the immediately adjacent lagoon, has a high diversity assemblage dominated by the calcareous taxa Amphistegina lessonii and Ammonia aff. A. aoteana. Five biofacies recognized by cluster analysis of live foraminiferal data exhibit similar salinity-related distribution patterns as the thanatofacies. C1 [Culver, Stephen J.; Mallinson, David J.; Corbett, D. Reide; Leorri, Eduardo; Parham, Peter R.] E Carolina Univ, Dept Geol Sci, Greenville, NC 27858 USA. [Corbett, D. Reide] E Carolina Univ, Inst Coastal Sci & Policy, Greenville, NC 27858 USA. [Rouf, Ajm A.; Shazili, Noor Azhar Mohd; Yaacob, Rosnan] Univ Malaysia Terengganu, Inst Oceanog, Kuala Terengganu 21030, Terengganu, Malaysia. [Whittaker, John E.] Nat Hist Museum, Dept Palaeontol, London SW7 5BD, England. [Buzas, Martin A.] Smithsonian Inst, Dept Paleobiol, Washington, DC 20560 USA. RP Culver, SJ (reprint author), E Carolina Univ, Dept Geol Sci, Greenville, NC 27858 USA. EM culvers@ecu.edu RI Leorri, Eduardo/B-4805-2010 OI Leorri, Eduardo/0000-0002-7475-6279 FU University Malaysia, Terengganu; East Carolina University FX We thank the University Malaysia, Terengganu, and East Carolina University for funding this research and Dr. Khawar Sultan, Joseph Anak Bidai, Mohd Nasir Mohammad, Asmadi bin Salleh, Ahmad Nazi la bin Ali, Mohd Zaini bin Mustapa, Kasim bin Muda, Adnan bin Abdulla Ghani, Che Mohd Kamarul Anuar bin Che Abdullah, Katie McDowell, Guy Iverson, Ray Tichenor, Katrina Rabien, and Alisha Ellis for support in the Field and laboratory. Clive Jones kindly provided access to the foraminiferal collections at The Natural History Museum, London. We thank Jean-Pierre Debenay, Justin Parker, and an anonymous reviewer for their constructive comments and Bruce Hayward for taxonomic advice. This is a contribution to IGCP Project 588 and to the Geo-Q Research Unit (Joaquin Gomez de Llarena Laboratory). NR 109 TC 13 Z9 14 U1 0 U2 7 PU CUSHMAN FOUNDATION FORAMINIFERAL RES PI CAMBRIDGE PA MUSEUM COMPARATIVE ZOOLOGY, DEPT INVERTEBRATE PALEONTOLOGY 26 OXFORD ST, HARVARD UNIV, CAMBRIDGE, MA 02138 USA SN 0096-1191 J9 J FORAMIN RES JI J. Foraminifer. Res. PD APR PY 2012 VL 42 IS 2 BP 109 EP 133 PG 25 WC Paleontology SC Paleontology GA 955SM UT WOS:000305041200002 ER PT J AU Petrizzo, MR Huber, BT Gale, AS Barchetta, A Jenkyns, HC AF Petrizzo, Maria Rose Huber, Brian T. Gale, Andrew S. Barchetta, Alessia Jenkyns, Hugh C. TI Abrupt planktic foraminiferal turnover across the Niveau Kilian at Col de Pre-Guittard (Vocontian Basin, southeast France): new criteria for defining the Aptian/Albian boundary SO NEWSLETTERS ON STRATIGRAPHY LA English DT Article DE Aptian/Albian boundary; planktic foraminifera; biostratigraphy; species turnover; absolute abundance; chemostratigraphy ID SE FRANCE; NORTH-ATLANTIC; INTEGRATED STRATIGRAPHY; ALBIAN STAGE; NANNOFOSSILS; ZONATION; SECTION; BIOSTRATIGRAPHY; AMMONITES; POSITION AB A detailed and quantitative study of foraminiferal assemblages across the Niveau Kilian in the Col de Pre-Guittard section (Vocontian Basin, southeast France) ably documents the planktic foraminiferal turnover across the Aptian-Albian boundary interval. The latest Aptian assemblage is dominated by few long-ranging Hedbergella and large-sized Paraticinella that completely disappear near the base of the Niveau Kilian organic-rich level. Planktic foraminiferal assemblages from across the Niveau Kilian to the top of the studied section are composed of minute, but very distinctive smooth-surfaced species of Microhedbergella miniglobularis and Mi. renilaevis. The appearance of Mi. renilaevis in the middle part of the Niveau Kilian represents a major step in the evolution and diversification of the Albian planktic fauna. The lowest occurrence of this taxon is recorded immediately above the extinction level of the Aptian hedbergellids and corresponds with a dramatic decrease in the number of planktic and benthic foraminifera specimens, with a 1 parts per thousand negative delta C-13 excursion in bulk carbonate, and evidence for regional rise in sea-surface temperature. Our careful study of the species composition permits refinement of the previous biozonation by using the appearance datum of Mi. renilaevis as a zonal boundary event. Changes include redefinition of the top of the Microhedbergella miniglobularis Zone and designation of a new Microhedbergella renilaevis Zone. The same sequence of events was reported from several deep-sea sites in the Atlantic and Indian Oceans. Therefore; documentation of the planktic foraminiferal turnover, combined with the carbon-isotope stratigraphy in the Col de Pre-Guittard section, provide new criteria for defining the Global Boundary Stratotype Section and Point for the base of the Albian Stage in a stratigraphically complete succession. C1 [Petrizzo, Maria Rose; Barchetta, Alessia] Univ Milan, Dipartimento Sci Terra A Desio, I-20133 Milan, Italy. [Huber, Brian T.] Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20013 USA. [Gale, Andrew S.] Univ Portsmouth, Sch Earth & Environm Sci, Portsmouth PO1 3QL, Hants, England. [Jenkyns, Hugh C.] Univ Oxford, Dept Earth Sci, Oxford OX1 3AN, England. RP Petrizzo, MR (reprint author), Univ Milan, Dipartimento Sci Terra A Desio, Via Mangiagalli 34, I-20133 Milan, Italy. EM mrose.petrizzo@unimi.it RI Petrizzo, Maria Rose/M-8672-2013; OI Petrizzo, Maria Rose/0000-0002-9584-8471; Jenkyns, Hugh/0000-0002-2728-0984 FU PUR FX We thank Isabella Premoli Silva and Paul Bown for valuable discussion and suggestions. Helpful comments and suggestions of R. Mark Leckie and one anonymous reviewer as well as from the editor, Jochen Erbacher, are highly appreciated. We are grateful to Norman Charnley for his help with stable-isotope analyses. Financial support of PUR 2008 to MRP is acknowledged. NR 47 TC 18 Z9 18 U1 0 U2 4 PU GEBRUDER BORNTRAEGER PI STUTTGART PA JOHANNESSTR 3A, D-70176 STUTTGART, GERMANY SN 0078-0421 J9 NEWSL STRATIGR JI Newsl. Stratigr. PD APR PY 2012 VL 45 IS 1 BP 55 EP 74 DI 10.1127/0078-0421/2012/0013 PG 20 WC Geology SC Geology GA 956TR UT WOS:000305112500003 ER PT J AU Funk, VA Kelloff, C Chan, R AF Funk, Vicki A. Kelloff, Carol Chan, Raymund TI Phylogeny and biogeography of the tribe Liabeae (Compositae subfamily Cichorioideae) SO TAXON LA English DT Article DE Asteraceae; Caribbean; molecular systematics; North America; South America ID CHAIN MONTE-CARLO; DNA-SEQUENCES; TRNL-F; MAXIMUM-LIKELIHOOD; SOUTH-AMERICA; ASTERACEAE; GENUS; INFERENCE; ANDES; MATK AB The tribe Liabeae (Compositae) contains ca. 175 species distributed in 18 genera and its members occupy a variety of habitats in the Andes of South America as well as in Mexico, Central America, and the West Indies. The tribe is recognizable by a combination of morphological characters. DNA sequence data from the nuclear ribosomal ITS region and three chloroplast regions (trnL-F, 3' end of ndhF, matK; a total of more than 5 kb of sequence data) were used to infer a phylogeny. The data were analyzed using maximum parsimony, maximum likelihood, and Bayesian inference. The results support the monophyly of the tribe and show a consistent placement for all genera except Cacosmia. Four well-supported clades are recovered in the remainder of the tribe, all recognized as subtribes. Liabineae (Ferreyranthus, Dillandia, Oligactis, Sampera, Liabum) are the sister group of the rest of the tribe. Sinclairineae (Sinclairiopsis and Sinclairia with segregates Liabellum and Megaliabum) are the sister group of Munnoziinae (Chrysactinium nested inside Munnozia s.l.) plus Paranepheliinae (Stephenbeckia, Microliabum, Pseudonoseris, Paranephelius, Chionopappus, Philoglossa, Erato). Cacosmia is placed as the sister group of either all the rest of the tribe or of subtribe Liabineae; morphologically its characters are either autapomorphic or plesiomorphic. Bishopanthus could not be confidently placed in any of the subtribes; it is only known from scraps of the type and a molecular study is not possible. The phylogeny slightly alters previous assumptions about the biogeography and it seems that Liabeae originated in the central and northern Andes and spread north and south with several independent introductions into Mexico and Central America and one into the Caribbean. With the exception of the Liabeae (Andes) and Moquineae (Brazil), all of the tribes in the subfamily Cichorioideae are either restricted to or have their basal grade in Africa. C1 [Funk, Vicki A.; Kelloff, Carol; Chan, Raymund] Smithsonian Inst, Dept Bot, US Natl Herbarium, Washington, DC 20013 USA. RP Funk, VA (reprint author), Smithsonian Inst, Dept Bot, US Natl Herbarium, MRC 166,POB 37012, Washington, DC 20013 USA. EM funkv@si.edu FU Smithsonian Institution (Scholarly Studies, Restricted Endowment, Lowland Tropical Ecosystem, and NMNH); LAB at the NMNH FX Funk wishes to thank her colleagues from a number of herbaria throughout Latin America for their help over the last twenty years in the field and in processing collected specimens (in alphabetical order based on herbarium abbreviation): COL-Herbario Nacional Colombian, Universidad Nacional de Colombia, Bogota; CR-Museo Nacional de Costa Rica, San Jose, Costa Rica; INB-Instituto Nacional de Biodiversidad, Santo Domingo, Costa Rica; LP-Herbario, Division Plantas Vasculares, Museo de La Plata, Argentina; LPB-Herbario Nacional de Bolivia, Universidad Mayor de San Andres, Bolivia; MEXU-Herbario Nacional at Universidad Nacional Autonoma de Mexico; QCA-Herbario, Pontificia Universidad Catolica del Ecuador, Quito, Ecuador; USM-Herbario, Museo de Historia Natural, Universidad Nacional Mayor de San Marcos, Lima, Peru. Sadly, Raymund Ramirez Deluadillo (ENSJ) who accompanied Funk and A. Delgado S. (MEXU) into the field in Mexico in 2005 died suddenly in 2010. Without his help we would never have found so many of the plants we were looking for. We are grateful that fieldwork was made possible by a variety of grants from the Smithsonian Institution (Scholarly Studies, Restricted Endowment, Lowland Tropical Ecosystem, and NMNH Research Opportunity Fund and its successors). The cost of the lab work was defrayed by funds from the LAB at the NMNH. We thank I. Ventosa (HAC) and M. Dillon (F) who kindly sent samples of leaf material from Cuba and Peru, respectively. We are grateful for the DNA for Hesperomannia that was supplied by the Hawaiian Plant DNA Library (Morden & al., 1996; Randell & Morden, 1999; http://www.botany.hawai.edu/faculty/morden/HPDL.htm); S.C. Harbin collected the Hesperomannia sample, extracted the DNA, and allowed us to use it before her project was finished. We also thank R. Capers (CONN), M. Dillon (F), N. Hind (K), L. Katinas (LP), S. Keeley (HAW), S. Knap (BM), G. McPherson (MO), P.B. Phillipson (MO), R. Rabeler (MICH), N. Roque (SPF), G. Schatz (MO), J. Soloman (MO), and T. Wendt (TEX) who helped track down vouchers and types. NR 76 TC 3 Z9 3 U1 2 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 APR PY 2012 VL 61 IS 2 BP 437 EP 455 PG 19 WC Plant Sciences; Evolutionary Biology SC Plant Sciences; Evolutionary Biology GA 959ZP UT WOS:000305357200013 ER PT J AU Buarpung, S Tharasanit, T Comizzoli, P Techakumphu, M AF Buarpung, Sirirak Tharasanit, Theerawat Comizzoli, Pierre Techakumphu, Mongkol TI Effects of cold storage on plasma membrane, DNA integrity and fertilizing ability of feline testicular spermatozoa SO ANIMAL REPRODUCTION SCIENCE LA English DT Article DE Cat; Testicular spermatozoa; Cold storage; Membrane integrity; DNA integrity; Intracytoplasmic sperm injection ID INTRACYTOPLASMIC SPERM INJECTION; IN-VITRO; DOMESTIC CAT; EMBRYO DEVELOPMENT; PREGNANCY RATE; DEGREES-C; OOCYTES; CELLS; SEMEN; FRAGMENTATION AB This study examined the effects of cold storage on plasma membrane, DNA integrity, and fertilizing ability of domestic cat spermatozoa. Intact cat testes were stored at 4 degrees C in Dulbecco's phosphate buffered saline (DPBS) for 7 days. Membrane integrity (experiment 1) and DNA integrity (experiment 2) of extracted spermatozoa were assessed over time during storage. Testicular spermatozoa were also tested for their fertilizing ability via intracytoplasmic sperm injection (ICSI) in term of gamete activation and early embryonic development at 18 h (experiment 3). The membrane integrity of testicular spermatozoa was well preserved in DPBS for 4 days compared to non-preserved control (Day 0) (P < 0.05). The incidence of testicular sperm DNA fragmentation was <1% after 7 days of cold storage and was not significantly affected by the duration of cold storage (P > 0.05). Finally, testicular spermatozoa could form pronuclei and sustain embryo development following ICSI regardless of the storage time (P > 0.05). In conclusion, cat testicular spermatozoa can be preserved at 4 degrees C for up to 7 days without severely compromising of plasma membrane and DNA integrity while retaining a normal fertilizing ability. (C) 2012 Elsevier B.V. All rights reserved. C1 [Buarpung, Sirirak; Tharasanit, Theerawat; Techakumphu, Mongkol] Chulalongkorn Univ, Dept Obstet Gynaecol & Reprod, Fac Vet Sci, Bangkok 10330, Thailand. [Comizzoli, Pierre] Smithsonian Conservat Biol Inst, Dept Reprod Sci, Ctr Species Survival, Washington, DC USA. RP Techakumphu, M (reprint author), Chulalongkorn Univ, Dept Obstet Gynaecol & Reprod, Fac Vet Sci, Bangkok 10330, Thailand. EM tmongkol@chula.ac.th FU Higher Education Research Promotion and National Research University Project of Thailand; Office of the Higher Education Commission [HR11661-55] FX This study was supported by the Higher Education Research Promotion and National Research University Project of Thailand, Office of the Higher Education Commission (HR11661-55). Sirirak Buarpung is a PhD student of RGJ-PhD program, Thailand Research Fund (TRF), Thailand. We would like to thank the Fertility and Neutering Clinic, Small Animal Teaching Hospital, the Faculty of Veterinary Science, Chulalongkorn University and The Veterinary Public Health Division of The Bangkok Metropolitan Administration, Thailand for sample collection. NR 35 TC 4 Z9 4 U1 0 U2 9 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0378-4320 J9 ANIM REPROD SCI JI Anim. Reprod. Sci. PD APR PY 2012 VL 131 IS 3-4 BP 219 EP 227 DI 10.1016/j.anireprosci.2012.03.011 PG 9 WC Agriculture, Dairy & Animal Science; Reproductive Biology SC Agriculture; Reproductive Biology GA 950WL UT WOS:000304681800015 PM 22516231 ER PT J AU Hauber, ME Strausberger, BM Feldheim, KA Lock, J Cassey, P AF Hauber, Mark E. Strausberger, Bill M. Feldheim, Kevin A. Lock, Justin Cassey, Phillip TI Indirect estimates of breeding and natal philopatry in an obligate avian brood parasite SO JOURNAL OF ORNITHOLOGY LA English DT Article DE Breeding range; Brood parasite; Dispersal; Site fidelity; Territoriality ID BROWN-HEADED COWBIRDS; SCALE GENETIC-STRUCTURE; MICROSATELLITE DNA MARKERS; MOLOTHRUS-ATER; SONG SPARROWS; SPECIES RECOGNITION; SECONDARY CONTACT; NEST PREDATION; COMMON CUCKOO; HOST USE AB In theory, obligate brood parasitic birds are freed from several of the temporal and spatial constraints of parental care for dependent young. Yet, similar to parental bird species, adults in several avian brood parasites show a territorial spacing system while breeding, including site fidelity within and across years. Banding-based capture and sighting studies are also suggestive of non-parasite-like lower levels of natal philopatry in avian brood parasites. We analyzed the potential correlation of physical distance with genetic structure of a Brown-headed Cowbird Molothrus ater population, sampling parasitic chicks from nests across different temporal and spatial scales of its common host, the Eastern Phoebe Sayornis phoebe, near Ithaca, New York, USA. In support of extensive breeding but not historical patterns of natal philopatry, we detected no significant covariation of genetic similarity by distance of nestling parasites at the scale beyond that of individual host nest sites. These results contribute towards a baseline for future behavioral and genetic comparisons of whether and how parasitic versus parental reproductive strategies impact patterns of avian population genetic structure across space and time. C1 [Hauber, Mark E.] CUNY Hunter Coll, Dept Psychol, New York, NY 10065 USA. [Strausberger, Bill M.; Feldheim, Kevin A.] Field Museum Nat Hist, Pritzker Lab Mol Systemat & Evolut, Chicago, IL 60605 USA. [Lock, Justin] Smithsonian Inst, Washington, DC 20008 USA. [Cassey, Phillip] Univ Adelaide, Sch Earth & Environm Sci, Adelaide, SA 5005, Australia. RP Hauber, ME (reprint author), CUNY Hunter Coll, Dept Psychol, 695 Pk Ave, New York, NY 10065 USA. EM mark.hauber@hunter.cuny.edu FU Howard Hughes Medical Institute; Human Frontier Science Program; Miller Institute of UC Berkeley; PSC-CUNY FX Funding was provided by the Howard Hughes Medical Institute (to M.E.H.), the Human Frontier Science Program (to M.E.H. and P.C.), the Miller Institute of UC Berkeley (to M.E.H.) and the PSC-CUNY grant award scheme (to M.E.H.). Molecular work was conducted in the Pritzker Laboratory for Molecular Systematics and Evolution, operated with support from the Pritzker Foundation. For discussions and comments we are grateful to C. Tonra, R. Fleischer, S. Heath, E. A. Lacey, C. Millar, J. Oursler, and many other colleagues. This research was approved by federal, state, and institutional animal ethics protocols. NR 80 TC 7 Z9 7 U1 2 U2 37 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0021-8375 EI 1439-0361 J9 J ORNITHOL JI J. Ornithol. PD APR PY 2012 VL 153 IS 2 BP 467 EP 475 DI 10.1007/s10336-011-0762-6 PG 9 WC Ornithology SC Zoology GA 951QI UT WOS:000304734700023 ER PT J AU Alvarado, JJ Guzman, HM Breedy, O AF Jose Alvarado, Juan Guzman, Hector M. Breedy, Odalisca TI Distribution and diversity of echinoderms (Asteroidea, Echinoidea, Holothuroidea) in the islands of the Gulf of Chiriqui, Panama SO REVISTA DE BIOLOGIA MARINA Y OCEANOGRAFIA LA English DT Article DE Diadema mexicanum; Acanthaster planci; coral reef; Eastern Tropical Pacific; seascape ID CORAL-REEFS; EASTERN PACIFIC; SEA-URCHINS; CARBONATE BUDGETS; UVA ISLAND; COSTA-RICA; EL-NINO; MODEL; CONSERVATION; ARCHIPELAGO AB Studies on echinoderms along the Panamanian Pacific coast have focused mainly on evolutionary and molecular analyses, however little ecological research has been done and mainly only on 2 species: Diadema mexicanum and Acanthaster planci. Herein, we describe for the first time the diversity (based on Margalef, Shannon and Pielou indices), distribution and density of echinoderms for some islands of the Gulf of Chiriqui, implementing a standard regional methodology used for the Eastern Tropical Pacific Conservation Seascape. Fifty-three reef sites were surveyed, of which 17 echinoderm species were found: 6 asteroids, 6 echinoids and 5 holothuroids. The average species richness, Shannon diversity, and Pielou's evenness indices were 0.43 +/- 0.04, 0.187 +/- 0.020, and 0.421 +/- 0.035 respectively. On average there were 3 species and 176 individuals per site. Three echinoid species were the most abundant: D. mexicanum, Eucidaris thoaursii and Echinometra vanbrunti, with 7909, 771 and 569 individuals respectively. Despite the high abundance observed, their impact on the reefs as well as other corallivores species (e. g., A. planci) is low, and for the moment they are not considered a threat to the reefs. Reef zones with greater richness and diversity of echinoderm species are associated with sites showing higher coral diversity and moderate to high live coral cover. We suggest a continuous assessment of the populations possibly damaging these ecosystems, as well those species that may be under illegal extraction. C1 [Jose Alvarado, Juan; Breedy, Odalisca] Univ Costa Rica, Ctr Invest Ciencias Mar & Limnol CIMAR, San Jose 115012060, Costa Rica. [Jose Alvarado, Juan] Univ Autonoma Baja California Sur, La Paz, Mexico. [Guzman, Hector M.; Breedy, Odalisca] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. [Breedy, Odalisca] Univ Costa Rica, Museo Zool, Escuela Biol, San Jose, Costa Rica. RP Alvarado, JJ (reprint author), Univ Costa Rica, Ctr Invest Ciencias Mar & Limnol CIMAR, San Jose 115012060, Costa Rica. EM juan.alvarado@ucr.ac.cr FU Conservation International; Smithsonian Tropical Research Institute FX This study would not have been possible without the help of the crew of the R/V Urraca. We want to thank C. Guevara, A. Chiriboga, G. Edgar and J. Cortes for their help with field work. We give special thanks to J. Cortes and two anonymous reviewers for all the comments that enriched this manuscript. This study was partially funded by Conservation International and the Smithsonian Tropical Research Institute. JJA is grateful with the Ministerio de Ciencia y Tecnologia de Costa Rica (MICIT), Consejo Nacional para Investigaciones Cienti-ficas y Tecnologicas de Costa Rica (CONICIT) and Consejo Nacional de Ciencia y Tecnologia de Mexico (CONACYT). NR 52 TC 5 Z9 5 U1 2 U2 17 PU UNIV VALPARAISO PI VINA DEL MAR PA FACULTAD CIENCIAS MAR RECURSOS NATURALES, CASILLA 5080 - RENACA, VINA DEL MAR, 00000, CHILE SN 0717-3326 J9 REV BIOL MAR OCEANOG JI Rev. Biol. Mar. Oceanogr. PD APR PY 2012 VL 47 IS 1 BP 13 EP 22 PG 10 WC Marine & Freshwater Biology; Oceanography SC Marine & Freshwater Biology; Oceanography GA 945AI UT WOS:000304244800002 ER PT J AU Huang, YM Mathis, WN Wilkerson, RC AF Huang, Yiau-Min Mathis, Wayne N. Wilkerson, Richard C. TI SUBGENERIC POSITION OF AEDES DUFOURI HAMON WITH NOTES ON THE SUBGENUS LEVUA STONE AND BOHART (DIPTERA: CULICIDAE) SO PROCEEDINGS OF THE ENTOMOLOGICAL SOCIETY OF WASHINGTON LA English DT Article DE Aedes (Levua) geoskusea (=suvae); Afrotropical Region; characterization; classification; dufouri group; Levua; Ochlerotatus; Reunion ID ALLIED TAXA DIPTERA; LIFE STAGES; MORPHOLOGICAL DATA; AEDINI DIPTERA; CLASSIFICATION; PHYLOGENY; OCHLEROTATUS AB Aedes dufouri Hamon, heretofore placed in the subgenus Levua Stone and Bohart, is transferred back to the subgenus Ochlerotatus Lynch Arribalzaga, where it is placed in a new monotypic lineage, the dufouri group, based on a morphological assessment of characters of specimens, including the type species, Aedes (Levua) suvae Stone and Bohart, 1944, from Suva, Fiji. Aedes fryeri (Theobald) was previously removed from the subgenus Levua (Huang et al. 2010). Thus, no members of the subgenus Levua (genus Aedes Meigen) are now known to occur in the Afrotropical Region. The female and the male genitalia of Ae. dufouri are redescribed and illustrated, and the dufouri group is diagnosed. Some morphological characters of adult males and females, as well as larvae, of the subgenera Ochlerotatus and Levua (genus Aedes Meigen) are tabulated. C1 [Huang, Yiau-Min; Mathis, Wayne N.] Smithsonian Inst, Dept Entomol, Washington, DC 20013 USA. [Wilkerson, Richard C.] Smithsonian Inst, WRBU, Museum Support Ctr, Suitland, MD 20746 USA. [Wilkerson, Richard C.] Walter Reed Army Inst Res, Entomol Branch, Silver Spring, MD 20910 USA. RP Huang, YM (reprint author), Smithsonian Inst, Dept Entomol, POB 37012,MSC C1109,MRC 534, Washington, DC 20013 USA. EM huangy@si.edu; mathisw@si.edu; wilkersonr@si.edu FU Walter Reed Biosystematics Unit (WRBU) FX We express our sincere appreciation and gratitude to the Walter Reed Biosystematics Unit (WRBU) for providing funding for the publication; to Dr. Leopoldo M. Rueda, Walter Reed Biosystematics Unit (WRBU), and Dr. Maria Anice Mureb Sallum, University of Sao Paulo, Sao Paulo, Brazil, for critically reviewing this manuscript and for their valuable comments; to Drs. Raymond J. Gagne and Alexander Konstantinov, Research Entomologists, Systematic Entomology Laboratory, U. S. Department of Agriculture, for translating French and Russian. NR 16 TC 1 Z9 1 U1 0 U2 2 PU ENTOMOL SOC WASHINGTON PI WASHINGTON PA SMITHSONIAN INSTITUTION DEPT ENTOMOLOGY, WASHINGTON, DC 20560 USA SN 0013-8797 J9 P ENTOMOL SOC WASH JI Proc. Entomol. Soc. Wash. PD APR PY 2012 VL 114 IS 2 BP 194 EP 204 DI 10.4289/0013-8797.114.2.194 PG 11 WC Entomology SC Entomology GA 942DP UT WOS:000304022800003 ER PT J AU Smith, DR Sanchez-Martinez, G Ojeda-Aguilera, A AF Smith, David R. Sanchez-Martinez, Guillermo Ojeda-Aguilera, Amelia TI A NEW SPECIES OF ZADIPRION (HYMENOPTERA: DIPRIONIDAE) ON PINUS DURANGENSIS FROM CHIHUAHUA, MEXICO, AND A REVIEW OF OTHER SPECIES OF THE GENUS SO PROCEEDINGS OF THE ENTOMOLOGICAL SOCIETY OF WASHINGTON LA English DT Review DE falsus; howdeni; rohweri; roteus; townsendi; Guatemala; United States ID SAWFLIES AB Zadipion ojedae Smith and Sanchez-Martinez, n. sp., reared from larvae feeding on Pinus durangensis Martinez in Chihuahua, Mexico, is described, and notes on its life history are provided. Hosts, distributions, and remarks on the other five species of Zadiprion are given, and the females, ovipositors, and male genitalia of all six species are illustrated. An identification key is given for all species. C1 [Smith, David R.] USDA, Systemat Entomol Lab, PSI,Smithsonian Inst, Agr Res Serv,Natl Museum Nat Hist, Washington, DC 20013 USA. [Sanchez-Martinez, Guillermo] Inst Nacl Invest Forestales Agr & Pecuarias, Aguascalientes 20660, Mexico. [Ojeda-Aguilera, Amelia] Secretaria Medio Ambiente & Recursos Nat, Lab Anal & Referencia Sanidad Forestal, Mexico City 04119, DF, Mexico. RP Smith, DR (reprint author), USDA, Systemat Entomol Lab, PSI,Smithsonian Inst, Agr Res Serv,Natl Museum Nat Hist, POB 37012,MRC 168, Washington, DC 20013 USA. EM dave.smith@ars.usda.gov; sanchezm.guillermo@inifap.gob.mx; ojedaamelia@hotmail.com FU Chihuahua State Government FX Hector E. Alanis Morales and Miguel Cano Rodriguez assisted in the biological observations of Zadiprion ojedae. This research was partially funded by the Chihuahua State Government. Henri Goulet, Canadian National Collection of Insects, Ottawa, kindly loaned the holotype of Z. roteus. Michele Touchet (Systematic Entomology Laboratory, USDA, Washington, DC [SEL]) assisted with the images. We appreciate reviews by the following: N. M. Schiff (U.S. Forest Service, Stoneville, MS) and D. A. Nickle and T. J. Henry (SEL, Beltsville, MD, and Washington, DC, respectively). USDA is an equal opportunity provider and employer. NR 20 TC 1 Z9 1 U1 0 U2 1 PU ENTOMOL SOC WASHINGTON PI WASHINGTON PA SMITHSONIAN INSTITUTION DEPT ENTOMOLOGY, WASHINGTON, DC 20560 USA SN 0013-8797 J9 P ENTOMOL SOC WASH JI Proc. Entomol. Soc. Wash. PD APR PY 2012 VL 114 IS 2 BP 224 EP 237 DI 10.4289/0013-8797.114.2.224 PG 14 WC Entomology SC Entomology GA 942DP UT WOS:000304022800006 ER PT J AU Vining, M AF Vining, Margaret TI Grace Hopper and the Invention of the Information Age SO TECHNOLOGY AND CULTURE LA English DT Book Review C1 [Vining, Margaret] Smithsonian Inst, Natl Museum Amer Hist, Washington, DC 20560 USA. RP Vining, M (reprint author), Smithsonian Inst, Natl Museum Amer Hist, Washington, DC 20560 USA. NR 1 TC 0 Z9 0 U1 1 U2 4 PU JOHNS HOPKINS UNIV PRESS PI BALTIMORE PA JOURNALS PUBLISHING DIVISION, 2715 NORTH CHARLES ST, BALTIMORE, MD 21218-4363 USA SN 0040-165X J9 TECHNOL CULT JI Technol. Cult. PD APR PY 2012 VL 53 IS 2 BP 516 EP 517 PG 2 WC History & Philosophy Of Science SC History & Philosophy of Science GA 944EV UT WOS:000304183000037 ER PT J AU Moser, WE Richardson, DJ Hammond, CI Lazo-Wasem, EA AF Moser, William E. Richardson, Dennis J. Hammond, Charlotte I. Lazo-Wasem, Eric A. TI Redescription of Placobdella ornata (Verrill, 1872) (Hirudinida: Glossiphoniidae) SO BULLETIN OF THE PEABODY MUSEUM OF NATURAL HISTORY LA English DT Article DE Placobdella ornata; Placobdella phalera; Desserobdella; Batracobdella; Glossiphoniidae; Hirudinida; Hirudinea; Annelida; leeches; Verrill; Clepsine ID OLIGACANTHORHYNCHIDAE AB The taxonomy of papillated leeches of the genus Placobdella has been extremely problematic, confounded by vague descriptions, redescriptions of species using material across a wide geographic range without reference to type material, and a plethora of dubious taxonomic acts over the course of more than a century. Leeches collected between 2008 and 2011 from the West River, New Haven, New Haven County, Connecticut-the type locality of Placobdella ornata (Verrill, 1872)-were determined lobe conspecific with P. ornata (Verrill, 1872) on the basis of comparison to the syntype series. The acquisition of these specimens from the type locality facilitated redescription of P. ornata. The striking similarity of P. ornata to P. phalera (Graf, 1899) prompted comparison of the two species. Specimens conforming to the description of P. phalera were collected from Shivericks Pond in Falmouth, Massachusetts, the type locality of P. phalera. Comparison of these specimens to Graf's (1899) original description of P. phalera (particularly figure 116, which was subsequently designated as the lectotype of P. phalera in the absence of type material) revealed the specimens to be conspecific with the concept of P. phalera articulated by Graf (1899) and with P. ornata (Verrill, 1872). Thus, P. phalera is considered a junior synonym of P. ornata. Molecular comparison of the specimens collected from the type localities of P. ornata and P. phalera using the highly conserved gene cytochrome c oxidase subunit I revealed similarities in base sequences of greater than 99.5%, substantiating the synonymy of the species. C1 [Moser, William E.] Museum Support Ctr MRC 534, Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, Suitland, MD 20746 USA. [Richardson, Dennis J.; Hammond, Charlotte I.] Quinnipiac Univ, Sch Biol Sci, Hamden, CT 06518 USA. [Lazo-Wasem, Eric A.] Yale Univ, Peabody Museum Nat Hist, Div Invertebrate Zool, New Haven, CT 06520 USA. RP Moser, WE (reprint author), Museum Support Ctr MRC 534, Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, 4210 Silver Hill Rd, Suitland, MD 20746 USA. EM moserw@si.edu; Dennis.Richardson@quinnipiac.edu; Charlotte.Hammond@quinnipiac.edu; eric.lazo-wasem@yale.edu FU Department of Biological Sciences; Schools of Arts and Sciences and Health Sciences, Quinnipiac University, Hamden, Connecticut FX Kristen E. Richardson and Krystal A. Lazos, Quinnipiac University, assisted in field collection. Lourdes M. Rojas, Division of Invertebrate Zoology, Peabody Museum of Natural History, Yale University, provided valuable assistance in specimen management. Harry Coyle, New Haven Parks and Recreation, provided valuable logistic insight. Allen Collins, National Systematics Laboratory, National Marine Fisheries Service, Washington, DC, provided valuable assistance and insight with molecular data analyses. The State of Connecticut Department of Energy and Environmental Protection provided permission to collect leeches. Funding for this project was provided in part by the Department of Biological Sciences and Schools of Arts and Sciences and Health Sciences, Quinnipiac University, Hamden, Connecticut. NR 19 TC 9 Z9 9 U1 2 U2 6 PU PEABODY MUSEUM NATURAL HISTORY-YALE UNIV PI NEW HAVEN PA 170 WHITNEY AVE, PO BOX 208118, NEW HAVEN, CT 06520-8118 USA SN 0079-032X J9 B PEABODY MUS NAT HI JI Bull. Peabody Mus. Natl. Hist. PD APR PY 2012 VL 53 IS 1 BP 325 EP 330 PG 6 WC Biodiversity Conservation; Ecology SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 937BG UT WOS:000303633400003 ER PT J AU Velazco, PM Gardner, AL AF Velazco, Paul M. Gardner, Alfred L. TI A new species of Lophostoma d'Orbigny, 1836 (Chiroptera: Phyllostomidae) from Panama SO JOURNAL OF MAMMALOGY LA English DT Article DE dichotomous key; Lophostoma; masculinization; Panama; Phyllostomidae; Phyllostominae; taxonomy ID ACTIVE TERMITE NESTS; ROUND-EARED BAT; TONATIA-SCHULZI; FRENCH-GUIANA; MAMMALS; ROOST; VENEZUELA; BEHAVIOR; FOREST AB We report the discovery of a new species of Lophostoma from Panama, which we name L. kalkoae. This new species resembles L. carrikeri and L. yasuni in possessing a white venter, but is distinguishable from both by external and cranial characteristics. The new species is similar in size to L. carrikeri and L. schulzi. Lophostoma sp. nov. can be most easily recognized by its combination of white venter, postauricular patches connected by a thin line of pale hair to the white fur on the chest, elongated clitoris and swollen labia, less strongly developed lateral projection of mastoid processes, well-marked indentation on the lingual cingulum of the upper canine, well-developed P3, well-developed posterior lingual cusp on the cingulum of P4, and parastyle absent on M1 and M2. We present a dichotomous key for the genus Lophostoma and a map showing all the localities where white-bellied Lophostoma have been recorded. C1 [Velazco, Paul M.] Amer Museum Nat Hist, Dept Mammal, New York, NY 10024 USA. [Gardner, Alfred L.] US Geol Survey, Patuxent Wildlife Res Ctr, Natl Museum Nat Hist MRC 111, Smithsonian Inst, Washington, DC 20013 USA. RP Velazco, PM (reprint author), Amer Museum Nat Hist, Dept Mammal, New York, NY 10024 USA. EM pvelazco@amnh.org RI Velazco, Paul/K-4186-2012 OI Velazco, Paul/0000-0001-7195-7422 FU American Museum of Natural History FX The following curators and collection staff graciously provided access to specimens under their care: N. B. Simmons and E. Westwig, American Museum of Natural History, New York; B. D. Patterson and J. Phelps, Field Museum of Natural History, Chicago; M. S. Hafner, Museum of Natural Science, Louisiana State University, Baton Rouge; V. Pacheco, Museo de Historia Natural de la Universidad Nacional Mayor de San Marcos, Lima; S. Burneo, Museo de Zoologia, Pontificia Universidad Cato Ilea del Ecuador, Quito; R. J. Baker, Museum of Texas Tech University, Lubbock; and S. C. Peurach, Patuxent Wildlife Research Center, United States Geological Survey. We thank P. J. Wynne for the illustration of Fig. 2, J. P. Carrera and C. M. Pinto for their measurements of the holotypes of Lophostoma aequatorialis and L. yasuni, and D. von Staden for the live bat photographs. For critical comments on an early draft of this manuscript, we thank T. Chesser, K. Kline, R. Pine, N. Woodman, and 1 anonymous reviewer. Funding for this project was provided to PMV by the Gerstner and Roosevelt postdoctoral fellowships at the American Museum of Natural History. NR 44 TC 2 Z9 3 U1 1 U2 14 PU OXFORD UNIV PRESS INC PI CARY PA JOURNALS DEPT, 2001 EVANS RD, CARY, NC 27513 USA SN 0022-2372 EI 1545-1542 J9 J MAMMAL JI J. Mammal. PD APR PY 2012 VL 93 IS 2 BP 605 EP 614 DI 10.1644/11-MAMM-A-217.1 PG 10 WC Zoology SC Zoology GA 937VI UT WOS:000303690700032 ER PT J AU Zug, GR Ineich, I Pregill, G Hamilton, AM AF Zug, George R. Ineich, Ivan Pregill, Gregory Hamilton, Alison M. TI Lizards of Tonga with Description of a New Tongan Treeskink (Squamata: Scincidae: Emoia samoensis Group) SO PACIFIC SCIENCE LA English DT Article ID MORPHOLOGICAL VARIATION; PREHISTORIC EXTINCTION; PACIFIC; IGUANAS; ISLANDS; GEHYRA AB The present-day vertebrate fauna of Tonga contains 17 species of lizards from three families: Gekkonidae, Iguanidae, and Scincidae. Are any of these lizard species members of a fauna before: humans arrived? This question is examined and partially resolved. Endemic taxa, such as Lepidodactylus euaensis, Emoia adspersa, and E. tongana, are likely inhabitants whose ancestors arrived, before the arrival of humans, via waif dispersal and subsequently differentiated in isolation. Recognition of these species is essential to interpret correctly the evolutionary history of the Tongan herpetofauna. The largest surviving Tongan skink previously has been identified incorrectly as a population of the Fijian Emoia trossula lineage. It is not and, herein, is differentiated from Emoia trossula and other central Pacific members of the Emoia samoensis species group and subgroup. Emoia mokolabi Zug, Ineich, Pregill & Hamilton, n. sp., differs from its sister taxa in the Emoia samoensis species subgroup by body size, dorsal and digital scalation, and coloration. C1 [Zug, George R.] Smithsonian Inst, Dept Vertebrate Zool, Natl Museum Nat Hist, Washington, DC 20013 USA. [Ineich, Ivan] UMR 7205 OSEB, Dept Systemat & Evolut, Museum Natl Hist Nat, F-75005 Paris, France. [Pregill, Gregory] Univ San Diego, Dept Biol, San Diego, CA 92110 USA. [Hamilton, Alison M.] Univ Calif Los Angeles, Dept Ecol & Evolutionary Biol, Los Angeles, CA 90095 USA. RP Zug, GR (reprint author), Smithsonian Inst, Dept Vertebrate Zool, Natl Museum Nat Hist, Washington, DC 20013 USA. EM zugG@si.edu FU Smithsonian Visiting Scholars program; Action Transversal du MNHN (ATM) "Biodivesite actuelle et fossile"; National Geographic Society [5032-93]; University of San Diego; National Science Foundation [DEB 0408010, DEB 0445213, DBI 0400797]; EPSCoR; Graduate Women in Science, American Society of Ichthyologists and Herpetologists; Society for the Study of Amphibians and Reptiles; Sigma Xi (LSU chapter); Louisiana State University (Museum of Natural Science and BioGrads); National Geographic Society; NMNH FX Research supported by Smithsonian Visiting Scholars program and Action Transversal du MNHN (ATM) "Biodivesite actuelle et fossile" to I.I.; National Geographic Society 5032-93, University Professorship University of San Diego for G.P.; National Science Foundation (DEB 0408010, DEB 0445213, DBI 0400797) to Christopher C. Austin and A.M.H.; an EPSCoR Fellowship to A.M.H.; grants from Graduate Women in Science, American Society of Ichthyologists and Herpetologists, Society for the Study of Amphibians and Reptiles, Sigma Xi (LSU chapter), and Louisiana State University (Museum of Natural Science and BioGrads) to A.M.H.; and the National Geographic Society, Smithsonian Scholarly Studies Program, and NMNH-Research Opportunities Fund to G.R.Z. Manuscript accepted 30 June 2011. NR 23 TC 3 Z9 3 U1 0 U2 5 PU UNIV HAWAII PRESS PI HONOLULU PA 2840 KOLOWALU ST, HONOLULU, HI 96822 USA SN 0030-8870 J9 PAC SCI JI Pac. Sci. PD APR PY 2012 VL 66 IS 2 BP 225 EP 237 DI 10.2984/66.2.9 PG 13 WC Marine & Freshwater Biology; Zoology SC Marine & Freshwater Biology; Zoology GA 936YH UT WOS:000303625400009 ER PT J AU Ascenso, J Lombardi, M Lada, CJ Alves, J AF Ascenso, J. Lombardi, M. Lada, C. J. Alves, J. TI The extinction law from photometric data: linear regression methods SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE methods: data analysis; ISM: clouds; dust, extinction; stars: formation ID STAR-FORMING REGIONS; TAURUS DARK CLOUDS; K-S BANDS; 8.0 MU-M; INTERSTELLAR EXTINCTION; GALACTIC-CENTER; INFRARED EXTINCTION; MOLECULAR CLOUDS; DUST; POLARIZATION AB Context. The properties of dust grains, in particular their size distribution, are expected to differ from the interstellar medium to the high-density regions within molecular clouds. Since the extinction at near-infrared wavelengths is caused by dust, the extinction law in cores should depart from that found in low-density environments if the dust grains have different properties. Aims. We explore methods to measure the near-infrared extinction law produced by dense material in molecular cloud cores from photometric data. Methods. Using controlled sets of synthetic and semi-synthetic data, we test several methods for linear regression applied to the specific problem of deriving the extinction law from photometric data. We cover the parameter space appropriate to this type of observations. Results. We find that many of the common linear-regression methods produce biased results when applied to the extinction law from photometric colors. We propose and validate a new method, LinES, as the most reliable for this effect. We explore the use of this method to detect whether or not the extinction law of a given reddened population has a break at some value of extinction. C1 [Ascenso, J.] European So Observ, D-85748 Garching, Germany. [Ascenso, J.; Lada, C. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Ascenso, J.] Univ Porto, Ctr Astrofis, P-4150762 Oporto, Portugal. [Lombardi, M.] Univ Milan, Dept Phys, I-20133 Milan, Italy. [Alves, J.] Univ Vienna, A-1180 Vienna, Austria. RP Ascenso, J (reprint author), European So Observ, Karl Schwarzschild Str 2, D-85748 Garching, Germany. EM jascenso@eso.org OI LOMBARDI, MARCO/0000-0002-3336-4965; Alves, Joao/0000-0002-4355-0921 FU FCT [SFRH/BPD/62983/2009]; European Community [229517]; NASA through JPL/Caltech [1279166] FX We thank C. Roman-Zuniga for kindly providing the SOFI data, and the referee, L. Cambresy, for helpful comments that contributed to making the paper more robust. J. Ascenso acknowledges financial support from FCT grant number SFRH/BPD/62983/2009. The research leading to these results has received funding from the European Community's Seventh Framework Programme (/FP7/2007-2013/) under grant agreement No. 229517. Support for this work was also provided by NASA through an award issued by JPL/Caltech, contract 1279166. NR 29 TC 1 Z9 1 U1 0 U2 0 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD APR PY 2012 VL 540 AR A139 DI 10.1051/0004-6361/201118355 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 932UG UT WOS:000303315400153 ER PT J AU Mashonkina, L Ryabtsev, A Frebel, A AF Mashonkina, L. Ryabtsev, A. Frebel, A. TI Non-LTE effects on the lead and thorium abundance determinations for cool stars SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE line: formation; nuclear reactions, nucleosynthesis, abundances; Sun: abundances; stars: abundances; stars: atmospheres ID NEUTRON-CAPTURE ELEMENTS; MULTILEVEL RADIATIVE-TRANSFER; RESOLVED LASER SPECTROSCOPY; GALACTIC CHEMICAL EVOLUTION; SPECTRAL-LINE FORMATION; LAMBDA ITERATION METHOD; GIANT BRANCH STARS; METAL-POOR; S-PROCESS; STELLAR ATMOSPHERES AB Context. Knowing accurate lead abundances of metal-poor stars provides constraints on the Pb production mechanisms in the early Galaxy. Accurately deriving thorium abundances permits a nucleo-chronometric age determination of the star. Aims. We aim to improve the calculation of the Pb I and Th II lines in stellar atmospheres based on non-local thermodynamic equilibrium (non-LTE) line formation, and to evaluate the influence of departures from LTE on Pb and Th abundance determinations for a range of stellar parameters by varying the metallicity from the solar value down to [Fe/H] = -3. Methods. We present comprehensive model atoms for Pb I and Th II and describe calculations of the Pb I energy levels and oscillator strengths. Results. The main non-LTE mechanism for Pb I is the ultraviolet overionization. We find that non-LTE leads to systematically depleted total absorption in the Pb I lines and accordingly, positive abundance corrections. The departures from LTE increase with decreasing metallicity. Using the semi-empirical model atmosphere HM74, we determine the lead non-LTE abundance for the Sun to be log epsilon(Pb,circle dot) = 2.09, in agreement with the meteoritic lead abundance. We revised the Pb and Eu abundances of the two strongly r-process enhanced stars CS 31082-001 and HE 1523-0901 and the metal-poor stellar sample. Our new results provide strong evidence of universal Pb-to-Eu relative r-process yields during the course of Galactic evolution. The stars in the metallicity range -2.3 < [Fe/H] < -1.4 have Pb/Eu abundance ratios that are, on average, 0.51 dex higher than those of strongly r-process enhanced stars. We conclude that the s-process production of lead started as early as the time when Galactic metallicity had reached [Fe/H] = -2.3. The average Pb/Eu abundance ratio of the mildly metal-poor stars, with -1.4 <= [Fe/H] <= -0.59, is very close to the corresponding Solar System value, in line with the theoretical predictions that AGB stars with [Fe/H] similar or equal to -1 provided the largest contribution to the solar abundance of s-nuclei of lead. The departures from LTE for Th II are caused by the pumping transitions from the levels with E-exc < 1 eV. Non-LTE leads to weakened Th II lines and positive abundance corrections. Overall, the abundance correction does not exceed 0.2 dex when collisions with Hi atoms are taken into account in statistical equilibrium calculations. C1 [Mashonkina, L.] Univ Sternwarte Munchen, D-81679 Munich, Germany. [Mashonkina, L.] Russian Acad Sci, Inst Astron, Moscow 119017, Russia. [Ryabtsev, A.] Russian Acad Sci, Inst Spect, Troitsk 142190, Moscow Region, Russia. [Frebel, A.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Frebel, A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Mashonkina, L (reprint author), Univ Sternwarte Munchen, Scheinerstr 1, D-81679 Munich, Germany. EM lyuda@usm.lmu.de; afrebel@mit.edu FU Swiss National Science Foundation (SCOPES) [IZ73Z0-128180/1]; Russian Leading Scientific School [3602.2012.2]; Clay Fellowship FX L.M. is supported by the Swiss National Science Foundation (SCOPES project No. IZ73Z0-128180/1) and the Russian Leading Scientific School grant 3602.2012.2. A.F. is, in part, supported by a Clay Fellowship administered by the Smithsonian Astrophysical Observatory. We used the MARCS model atmosphere library and the NIST and VALD databases. NR 65 TC 21 Z9 21 U1 0 U2 3 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD APR PY 2012 VL 540 AR A98 DI 10.1051/0004-6361/201218790 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 932UG UT WOS:000303315400112 ER PT J AU Morgenthaler, A Petit, P Saar, S Solanki, SK Morin, J Marsden, SC Auriere, M Dintrans, B Fares, R Gastine, T Lanoux, J Lignieres, F Paletou, F Velez, JCR Theado, S Van Grootel, V AF Morgenthaler, A. Petit, P. Saar, S. Solanki, S. K. Morin, J. Marsden, S. C. Auriere, M. Dintrans, B. Fares, R. Gastine, T. Lanoux, J. Lignieres, F. Paletou, F. Ramirez Velez, J. C. Theado, S. Van Grootel, V. TI Long-term magnetic field monitoring of the Sun-like star xi Bootis A SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE stars: activity; stars: atmospheres; stars: chromospheres; stars: imaging; stars: solar-type; stars: magnetic field ID SPECTRAL-LINE ASYMMETRIES; MAIN-SEQUENCE STARS; COOL ACTIVE STARS; CA-II H; DIFFERENTIAL ROTATION; SPECTROPOLARIMETRIC OBSERVATIONS; DYNAMO PROCESSES; ACTIVITY CYCLES; K-DWARF; F-STAR AB Aims. We aim to investigate the long-term temporal evolution of the magnetic field of the solar-type star xi Bootis A, both from direct magnetic field measurements and from the simultaneous estimate of indirect activity indicators. Methods. We obtained seven epochs of high-resolution, circularly-polarized spectra from the NARVAL spectropolarimeter between 2007 and 2011, for a total of 76 spectra. Using approximately 6100 photospheric spectral lines covering the visible domain, we employed a cross-correlation procedure to compute a mean polarized line profile from each spectrum. The large-scale photospheric magnetic field of the star was then modelled by means of Zeeman-Doppler Imaging, allowing us to follow the year-to-year evolution of the reconstructed magnetic topology. Simultaneously, we monitored the width of several magnetically sensitive spectral lines, the radial velocity, the line asymmetry of intensity line profiles, and the chromospheric emission in the cores of the Ca II H and H alpha lines. Results. During the highest observed activity states, in 2007 and 2011, the large-scale field of xi Bootis A is almost completely axisymmetric and is dominated by its toroidal component. The toroidal component persists with a constant polarity, containing a significant fraction of the magnetic energy of the large-scale surface field through all observing epochs. The magnetic topologies reconstructed for these activity maxima are very similar, suggesting a form of short cyclicity in the large-scale field distribution. The mean unsigned large-scale magnetic flux derived from the magnetic maps varies by a factor of about 2 between the lowest and highest observed magnetic states. The chromospheric flux is less affected and varies by a factor of 1.2. Correlated temporal evolution, due to both rotational modulation and seasonal variability, is observed between the Ca II emission, the H alpha emission and the width of magnetically sensitive lines. The rotational dependence of polarimetric magnetic measurements displays a weak correlation with other activity proxies, presumably due to the different spatial scales and centre-to-limb darkening associated with polarimetric signatures, as compared to non-polarized activity indicators. Better agreement is observed on the longer term. When measurable, the differential rotation reveals a strong latitudinal shear in excess of 0.2 rad d(-1). C1 [Morgenthaler, A.; Petit, P.; Auriere, M.; Dintrans, B.; Lanoux, J.; Lignieres, F.; Paletou, F.; Theado, S.] Univ Toulouse, UPS OMP, Inst Rech Astrophys & Planetol, Toulouse, France. [Morgenthaler, A.; Petit, P.; Auriere, M.; Dintrans, B.; Lanoux, J.; Lignieres, F.; Paletou, F.; Theado, S.] CNRS, Inst Rech Astrophys & Planetol, F-31400 Toulouse, France. [Saar, S.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Solanki, S. K.; Gastine, T.] Max Planck Inst Sonnensyst Forsch, D-37191 Katlenburg Lindau, Germany. [Morin, J.] Dublin Inst Adv Studies, Sch Cosm Phys, Dublin 2, Ireland. [Morin, J.] Univ Gottingen, Inst Astrophys, D-37077 Gottingen, Germany. [Marsden, S. C.] James Cook Univ, Ctr Astron, Sch Engn & Phys Sci, Townsville, Qld 4811, Australia. [Fares, R.] Univ St Andrews, SUPA, Sch Phys & Astron, St Andrews KY16 9SS, Fife, Scotland. [Ramirez Velez, J. C.] Univ Nacl Autonoma Mexico, Inst Astron, Coyoacan 04510, DF, Mexico. [Van Grootel, V.] Univ Liege, Inst Astrophys & Geophys, B-4000 Liege, Belgium. RP Morgenthaler, A (reprint author), Univ Toulouse, UPS OMP, Inst Rech Astrophys & Planetol, Toulouse, France. EM amorgent@ast.obs-mip.fr; petit@ast.obs-mip.fr RI Petit, Pascal/C-5842-2011; Solanki, Sami/E-2487-2013; Ramirez-Velez, Robinson/D-5311-2016 OI Solanki, Sami/0000-0002-3418-8449; Ramirez-Velez, Robinson/0000-0003-3075-6960 NR 55 TC 29 Z9 29 U1 0 U2 2 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 EI 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD APR PY 2012 VL 540 AR A138 DI 10.1051/0004-6361/201118139 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 932UG UT WOS:000303315400152 ER PT J AU Ricci, L Trotta, F Testi, L Natta, A Isella, A Wilner, DJ AF Ricci, L. Trotta, F. Testi, L. Natta, A. Isella, A. Wilner, D. J. TI The effect of local optically thick regions in the long-wave emission of young circumstellar disks SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE protoplanetary disks ID ORION NEBULA CLUSTER; STAR-FORMING REGION; T-TAURI STARS; PROTOPLANETARY DISKS; PLANET FORMATION; RESOLVED IMAGES; ACCRETION DISKS; SOLID BODIES; GRAIN-GROWTH; FN TAURI AB Multi-wavelength observations of protoplanetary disks in the sub-millimeter continuum have measured spectral indices values which are significantly lower than what is found in the diffuse interstellar medium. Under the assumption that mm-wave emission of disks is mostly optically thin, these data have been generally interpreted as evidence for the presence of mm/cm-sized pebbles in the disk outer regions. In this work we investigate the effect of possible local optically thick regions on the mm-wave emission of protoplanetary disks without mm/cm-sized grains. A significant local increase of the optical depth in the disk can be caused by the concentration of solid particles, as predicted to result from a variety of proposed physical mechanisms. We calculate the filling factors and implied overdensities these optically thick regions would need to significantly affect the millimeter fluxes of disks, and we discuss their plausibility. We find that optically thick regions characterized by relatively small filling factors can reproduce the mm-data of young disks without requesting emission from mm/cm-sized pebbles. However, these optically thick regions require dust overdensities much larger than what predicted by any of the physical processes proposed in the literature to drive the concentration of solids. We find that only for the most massive disks it is possible and plausible to imagine that the presence of optically thick regions in the disk is responsible for the low measured values of the mm spectral index. For the majority of the disk population, optically thin emission from a population of large mm-sized grains remains the most plausible explanation. The results of this analysis further strengthen the scenario for which the measured low spectral indices of protoplanetary disks at mm wavelengths are due to the presence of large mm/cm-sized pebbles in the disk outer regions. C1 [Ricci, L.; Trotta, F.; Testi, L.] European So Observ, D-85748 Garching, Germany. [Ricci, L.; Isella, A.] CALTECH, Div Phys Math & Astron, Pasadena, CA 91125 USA. [Trotta, F.; Testi, L.; Natta, A.] INAF Osservatorio Astrofis Arcetri, I-50125 Florence, Italy. [Natta, A.] Dublin Inst Adv Studies, Sch Cosm Phys, Dublin 2, Ireland. [Wilner, D. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Ricci, L (reprint author), European So Observ, Karl Schwarzschild Str 2, D-85748 Garching, Germany. EM lricci@astro.caltech.edu FU International Max-Planck-Research School; ASI; National Science Foundation FX L.R. aknowledges the Ph.D. fellowship of the International Max-Planck-Research School. L. T. and F. T. acknowledge support from ASI under contract with INAF-Osservatorio Astrofisico di Arcetri. Support for CARMA construction was derived from the states of California, Illinois, and Maryland, the James S. McDonnell Foundation, the Gordon and Betty Moore Foundation, the Kenneth T. and Eileen L. Norris Foundation, the University of Chicago, the Associates of the California Institute of Technology, and the National Science Foundation. Ongoing CARMA development and operations are supported by the National Science Foundation under a cooperative agreement, and by the CARMA partner universities. NR 52 TC 18 Z9 18 U1 0 U2 0 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD APR PY 2012 VL 540 AR A6 DI 10.1051/0004-6361/201118296 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 932UG UT WOS:000303315400020 ER PT J AU Teixeira, PS Lada, CJ Marengo, M Lada, EA AF Teixeira, P. S. Lada, C. J. Marengo, M. Lada, E. A. TI Spitzer observations of NGC2264: the nature of the disk population SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE circumstellar matter; stars: formation; ISM: clouds ID YOUNG STELLAR OBJECTS; LOW-MASS STARS; T-TAURI STARS; SPECTRAL ENERGY-DISTRIBUTIONS; OB1 MOLECULAR CLOUD; SPACE-TELESCOPE; NGC 2264; PROTOPLANETARY DISKS; C2D SURVEY; EVOLUTIONARY MODELS AB Aims. NGC2264 is a young cluster with a rich circumstellar disk population which makes it an ideal target for studying the evolution of stellar clusters. Our goal is to study the star formation history of NGC 2264 and to analyse the primordial disk evolution of its members. Methods. The study presented is based on data obtained with the Infrared Array Camera (IRAC) and the Multiband Imaging Photometer for Spitzer (MIPS) on board the Spitzer Space Telescope, combined with deep near-infrared (NIR) ground-based FLAMINGOS imaging and previously published optical data. Results. We build NIR dust extinction maps of the molecular cloud associated with the cluster, and determine it to have a mass of 2.1 x 10(3) M-circle dot above an AV of 7 mag. Using a differential K-s-band luminosity function (KLF) of the cluster, we estimate the size of the population of NGC2264, within the area observed by FLAMINGOS, to be 1436 +/- 242 members. The star formation efficiency is >=similar to 25%. We identify the disk population and divide it into 3 groups based on their spectral energy distribution slopes from 3.6 mu m to 8 mu m and on the 24 mu m excess emission: (i) optically thick inner disks, (ii) anaemic inner disks, and (iii) disks with inner holes, or transition disks. We analyse the spatial distribution of these sources and find that sources with thick disks segregate into sub-clusterings, whereas sources with anaemic disks do not. Furthermore, sources with anaemic disks are found to be unembedded (i.e., with A(V) < 3 mag), whereas the clustered sources with thick disks are still embedded within the parental cloud. Conclusions. NGC2264 has undergone more than one star-forming event, where the anaemic and extincted thick disk population appear to have formed in separate episodes: the sources with anaemic disks are more evolved and have had time to disperse and populate a halo of the cluster. We also find tentative evidence of triggered star-formation in the Fox Fur Nebula. In terms of disk evolution, our findings support the emerging disk evolution paradigm of two distinct evolutionary paths for primordial optically thick disks: a homologous one where the disk emission decreases uniformly at NIR and mid-infrared (MIR) wavelengths, and a radially differential one where the emission from the inner region of the disk decreases more rapidly than from the outer region (forming transition disks). C1 [Teixeira, P. S.] European So Observ, D-85748 Garching, Germany. [Lada, C. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Marengo, M.] Iowa State Univ, Dept Phys & Astron, Ames, IA USA. [Lada, E. A.] Univ Florida, Dept Astron, Gainesville, FL 32611 USA. RP Teixeira, PS (reprint author), Univ Vienna, Inst Astrophys, Turkenschanzstr 17, A-1180 Vienna, Austria. EM paula.teixeira@univie.ac.at; clada@cfa.harvard.edu; mmarengo@iastate.edu; lada@astro.ufl.edu RI Teixeira, Paula Stella/O-2289-2013 OI Teixeira, Paula Stella/0000-0002-3665-5784 FU Fundacao para a Ciencia e Tecnologia (Portugal) [SFRH/BD/13984/2003]; NASA [1407, 960785, LTSA NNG05D66G]; NSF [AST97-31180, AST97-3367, AST02-02976, AST-1109679]; Kitt Peak National Observatory FX We warmly thank Luisa Rebull for sharing her ancillary data catalogue of NGC2264 with us. We also thank Naomi Ridge for kindly allowing us to directly compare her 13CO and C18O observations of NGC2264 with our data. P. S. T. acknowledges support from the grant SFRH/BD/13984/2003 awarded by the Fundacao para a Ciencia e Tecnologia (Portugal). This work is based on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under NASA contracts 1407 and 960785. FLAMINGOS was designed and constructed by the IR instrumentation group (PI: R. Elston) at the University of Florida, Department of Astronomy, with support from NSF grant AST97-31180 and Kitt Peak National Observatory. The FLAMINGOS data were collected under the NOAO Survey Program, Towards a Complete Near-Infrared Spectroscopic Survey of Giant Molecular Clouds (PI: E. Lada) and supported by NSF grants AST97-3367 and AST02-02976 to the University of Florida. this publication is based in part upon work supported by the National Science Foundation under Grant No. AST-1109679 and NASA grant LTSA NNG05D66G awarded to the University of Florida. 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. NR 81 TC 15 Z9 15 U1 0 U2 0 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD APR PY 2012 VL 540 AR A83 DI 10.1051/0004-6361/201015326 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 932UG UT WOS:000303315400097 ER PT J AU Vinko, J Takats, K Szalai, T Marion, GH Wheeler, JC Sarneczky, K Garnavich, PM Kelemen, J Klagyivik, P Pal, A Szalai, N Vida, K AF Vinko, J. Takats, K. Szalai, T. Marion, G. H. Wheeler, J. C. Sarneczky, K. Garnavich, P. M. Kelemen, J. Klagyivik, P. Pal, A. Szalai, N. Vida, K. TI Improved distance determination to M51 from supernovae 2011dh and 2005cs SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE supernovae: individual: 2011dh; supernovae: individual: 2005cs; galaxies: individual: M51; galaxies: distances and redshifts ID EXPANDING PHOTOSPHERE METHOD; SN 2005CS; II SUPERNOVAE; SUPERGIANT PROGENITOR; ATMOSPHERES; RADIATION; EXPLOSION; EVOLUTION; SN-1993J; PLATEAU AB Aims. The appearance of two recent supernovae, SN 2011dh and 2005cs, both in M51, provides an opportunity to derive an improved distance to their host galaxy by combining the observations of both SNe. Methods. We apply the Expanding Photosphere Method to get the distance to M51 by fitting the data of these two SNe simultaneously. In order to correct for the effect of flux dilution, we use correction factors (zeta) appropriate for standard type II-P SNe atmospheres for 2005cs, but find zeta similar to 1 for the type IIb SN 2011dh, which may be due to the reduced H-content of its ejecta. Results. The EPM analysis resulted in D-M51 = 8.4 +/- 0.7 Mpc. Based on this improved distance, we also re-analyze the HST observations of the proposed progenitor of SN 2011dh. We confirm that the object detected on the pre-explosion HST-images is unlikely to be a compact stellar cluster. In addition, its derived radius (similar to 277 R-circle dot) is too large for being the real (exploded) progenitor of SN 2011dh. Conclusions. The supernova-based distance, D = 8.4 Mpc, is in good agreement with other recent distance estimates to M51. C1 [Vinko, J.; Takats, K.; Szalai, T.] Univ Szeged, Dept Opt & Quantum Elect, H-6720 Szeged, Hungary. [Marion, G. H.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Vinko, J.; Wheeler, J. C.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA. [Sarneczky, K.; Kelemen, J.; Klagyivik, P.; Pal, A.; Szalai, N.; Vida, K.] Hungarian Acad Sci, Konkoly Observ, H-1525 Budapest, Hungary. [Garnavich, P. M.] Univ Notre Dame, Dept Phys, Notre Dame, IN 46556 USA. [Pal, A.] Eotvos Lorand Univ, Dept Astron, H-1518 Budapest, Hungary. RP Vinko, J (reprint author), Univ Szeged, Dept Opt & Quantum Elect, Dom Ter 9, H-6720 Szeged, Hungary. EM vinko@physx.u-szeged.hu FU Hungarian OTKA [K76816, K-081421]; European Union [TAMOP 4.2.2/B-10/1-2010-0012]; NSF [AST 09-07903, AST 11-09801]; ESA [PECS 98073]; Hungarian Academy of Sciences FX We express our thanks to the anonymous referee for the thorough reading of the manuscript, and the useful comments that helped us improving the paper. This project has been supported by Hungarian OTKA grant K76816, and by the European Union together with the European Social Fund through the TAMOP 4.2.2/B-10/1-2010-0012 grant. The CfA Supernova Program is supported by NSF Grant AST 09-07903. J.C.W.'s supernova group at UT Austin is supported by NSF Grant AST 11-09801. A. P. has been supported by the ESA grant PECS 98073 and by the Janos Bolyai Research Scholarship of the Hungarian Academy of Sciences. K. S. and K. V. acknowledge support from the the "Lendulet" Program of the Hungarian Academy of Sciences and Hungarian OTKA Grant K-081421. Thanks are also due to the staff of McDonald and Konkoly Observatories for the prompt scheduling and helpful assistance during the time-critical ToO observations. The SIMBAD database at CDS, the NASA ADS and NED databases have been used to access data and references. The availability of these services is gratefully acknowledged. NR 36 TC 26 Z9 26 U1 0 U2 2 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD APR PY 2012 VL 540 AR A93 DI 10.1051/0004-6361/201118364 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 932UG UT WOS:000303315400107 ER PT J AU Sayer, EJ Wright, SJ Tanner, EVJ Yavitt, JB Harms, KE Powers, JS Kaspari, M Garcia, MN Turner, BL AF Sayer, Emma J. Wright, S. Joseph Tanner, Edmund V. J. Yavitt, Joseph B. Harms, Kyle E. Powers, Jennifer S. Kaspari, Michael Garcia, Milton N. Turner, Benjamin L. TI Variable Responses of Lowland Tropical Forest Nutrient Status to Fertilization and Litter Manipulation SO ECOSYSTEMS LA English DT Article DE nutrient limitation; Panama; litter addition; litter removal; nitrogen; phosphorus; potassium; litterfall; soil nutrients; fine root biomass ID SOIL ORGANIC PHOSPHORUS; RISING ATMOSPHERIC CO2; N-P RATIOS; TERRESTRIAL ECOSYSTEMS; RAIN-FOREST; MOIST FOREST; LEAF-LITTER; CARBON SEQUESTRATION; HAWAIIAN FORESTS; NITROGEN CYCLES AB Predicting future impacts of anthropogenic change on tropical forests requires a clear understanding of nutrient constraints on productivity. We compared experimental fertilization and litter manipulation treatments in an old-growth lowland tropical forest to distinguish between the effects of inorganic nutrient amendments and changes in nutrient cycling via litterfall. We measured the changes in soil and litter nutrient pools, litterfall, and fine root biomass in plots fertilized with nitrogen (N), phosphorus (P), or potassium (K), and in litter addition and litter removal treatments during 7 years. Soil inorganic N and litter N increased in double-litter plots but not in N-fertilized plots. Conversely, litter P and soil pools of P and K increased in fertilized plots but not in the double-litter plots. Soil and litter pools of N and K decreased in the no-litter plots. Changes in litterfall with added nutrients or litter were only marginally significant, but fine root biomass decreased with both the litter and the K addition. Differences between the two experiments are mostly attributable to the coupled cycling of carbon and nutrients in litter. Increased nutrient inputs in litter may improve plant uptake of some nutrients compared to fertilization with similar amounts. The litter layer also appears to play a key role in nutrient retention. We discuss our findings in the context of possible impacts of anthropogenic change on tropical forests. C1 [Sayer, Emma J.] Ctr Ecol & Hydrol, Wallingford OX10 8BB, Oxon, England. [Sayer, Emma J.; Wright, S. Joseph; Harms, Kyle E.; Garcia, Milton N.; Turner, Benjamin L.] Smithsonian Trop Res Inst, Balboa, Panama. [Sayer, Emma J.; Tanner, Edmund V. J.] Univ Cambridge, Dept Plant Sci, Cambridge CB2 3EA, England. [Yavitt, Joseph B.] Cornell Univ, Dept Nat Resources, Ithaca, NY 14853 USA. [Harms, Kyle E.] Louisiana State Univ, Dept Biol Sci, Baton Rouge, LA 70803 USA. [Powers, Jennifer S.] Univ Minnesota, Dept Ecol, St Paul, MN 55108 USA. [Powers, Jennifer S.] Univ Minnesota, Dept Evolut, St Paul, MN 55108 USA. [Powers, Jennifer S.] Univ Minnesota, Dept Behav & Plant Biol, St Paul, MN 55108 USA. [Kaspari, Michael] Univ Oklahoma, Dept Zool, Norman, OK 73019 USA. RP Sayer, EJ (reprint author), Ctr Ecol & Hydrol, Maclean Bldg,Benson Lane, Wallingford OX10 8BB, Oxon, England. EM emsa@ceh.ac.uk RI Turner, Benjamin/E-5940-2011; Sayer, Emma/B-2514-2010; Wright, Stuart/M-3311-2013; OI Turner, Benjamin/0000-0002-6585-0722; Sayer, Emma/0000-0002-3322-4487; Wright, Stuart/0000-0003-4260-5676; Kaspari, Michael/0000-0002-9717-5768 FU Gates Cambridge Scholarship; European Union Marie-Curie [MOIF-CT-2005-21728]; Cambridge Philosophical Society; Andrew W. Mellon Foundation; Gonville and Caius College Cambridge; Department of Plant Sciences, Cambridge; Smithsonian Scholarly Studies Grant; NSF [0212386]; Smithsonian Tropical Research Institute FX We wish to thank O. Hernandez, R. Gonzalez, F. Valdez, J. Valdez, G. Perez, F. Zeugin, D. Urena, A. Vincent, and all Cambridge student volunteers for help in the field. We thank L. Schreeg for information on phosphate sorption, A. Beckermann and J. Staley for statistical advice and M. Heard for useful comments. We are grateful to P. Vitousek and two anonymous reviewers for their helpful suggestions on improving earlier drafts of the manuscript. EJS was funded by a Gates Cambridge Scholarship, a European Union Marie-Curie Outgoing Fellowship MOIF-CT-2005-21728, and a Cambridge Philosophical Society Travel Grant. EVT was funded by the Andrew W. Mellon Foundation, Gonville and Caius College Cambridge and the Department of Plant Sciences, Cambridge. SJW was funded by the Andrew W. Mellon Foundation. SJW, JBY and KEH were funded by a Smithsonian Scholarly Studies Grant. MK was funded by NSF Grant No. 0212386 and JSP was funded by a grant from the Smithsonian Tropical Research Institute. NR 82 TC 41 Z9 46 U1 4 U2 112 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 1432-9840 J9 ECOSYSTEMS JI Ecosystems PD APR PY 2012 VL 15 IS 3 BP 387 EP 400 DI 10.1007/s10021-011-9516-9 PG 14 WC Ecology SC Environmental Sciences & Ecology GA 936PF UT WOS:000303601800003 ER PT J AU Drexler, JF Corman, VM Muller, MA Maganga, GD Vallo, P Binger, T Gloza-Rausch, F Rasche, A Yordanov, S Seebens, A Oppong, S Sarkodie, YA Pongombo, C Lukashev, AN Schmidt-Chanasit, J Stocker, A Carneiro, AJB Erbar, S Maisner, A Fronhoffs, F Buettner, R Kalko, EKV Kruppa, T Franke, CR Kallies, R Yandoko, ERN Herrler, G Reusken, C Hassanin, A Kruger, DH Matthee, S Ulrich, RG Leroy, EM Drosten, C AF Drexler, Jan Felix Corman, Victor Max Mueller, Marcel Alexander Maganga, Gael Darren Vallo, Peter Binger, Tabea Gloza-Rausch, Florian Rasche, Andrea Yordanov, Stoian Seebens, Antje Oppong, Samuel Sarkodie, Yaw Adu Pongombo, Celestin Lukashev, Alexander N. Schmidt-Chanasit, Jonas Stoecker, Andreas Borges Carneiro, Aroldo Jose Erbar, Stephanie Maisner, Andrea Fronhoffs, Florian Buettner, Reinhard Kalko, Elisabeth K. V. Kruppa, Thomas Franke, Carlos Roberto Kallies, Rene Yandoko, Emmanuel R. N. Herrler, Georg Reusken, Chantal Hassanin, Alexandre Krueger, Detlev H. Matthee, Sonja Ulrich, Rainer G. Leroy, Eric M. Drosten, Christian TI Bats host major mammalian paramyxoviruses SO NATURE COMMUNICATIONS LA English DT Article ID EMERGING INFECTIOUS-DISEASES; ANCESTRAL CHARACTER STATES; FRUIT BATS; VIRUS TRANSMISSION; EBOLA-VIRUS; RESERVOIRS; EMERGENCE; PHYLOGENIES; EVOLUTIONARY; MEASLES AB The large virus family Paramyxoviridae includes some of the most significant human and livestock viruses, such as measles-, distemper-, mumps-, parainfluenza-, Newcastle disease-, respiratory syncytial virus and metapneumoviruses. Here we identify an estimated 66 new paramyxoviruses in a worldwide sample of 119 bat and rodent species (9,278 individuals). Major discoveries include evidence of an origin of Hendra-and Nipah virus in Africa, identification of a bat virus conspecific with the human mumps virus, detection of close relatives of respiratory syncytial virus, mouse pneumonia-and canine distemper virus in bats, as well as direct evidence of Sendai virus in rodents. Phylogenetic reconstruction of host associations suggests a predominance of host switches from bats to other mammals and birds. Hypothesis tests in a maximum likelihood framework permit the phylogenetic placement of bats as tentative hosts at ancestral nodes to both the major Paramyxoviridae subfamilies (Paramyxovirinae and Pneumovirinae). Future attempts to predict the emergence of novel paramyxoviruses in humans and livestock will have to rely fundamentally on these data. C1 [Drexler, Jan Felix; Corman, Victor Max; Mueller, Marcel Alexander; Binger, Tabea; Gloza-Rausch, Florian; Kallies, Rene; Drosten, Christian] Univ Bonn, Med Ctr, Inst Virol, D-53127 Bonn, Germany. [Maganga, Gael Darren; Leroy, Eric M.] Ctr Int Rech Med Franceville, Franceville, Gabon. [Vallo, Peter] Acad Sci Czech Republic, Inst Vertebrate Biol, Vvi, Brno, Czech Republic. [Gloza-Rausch, Florian; Seebens, Antje] Ctr Bat Protect & Informat, Bad Segeberg, Germany. [Rasche, Andrea; Herrler, Georg] Univ Vet Med Hannover, Inst Virol, Hannover, Germany. [Yordanov, Stoian] Forestry Board Directorate Strandja Nat Pk, Malko Tarnovo, Bulgaria. [Oppong, Samuel; Sarkodie, Yaw Adu] Kwame Nkrumah Univ Sci & Technol, Kumasi, Ghana. [Pongombo, Celestin] Univ Lubumbashi, Lubumbashi, Zaire. [Lukashev, Alexander N.] Chumakov Inst Poliomyelitis & Viral Encephalitide, Moscow, Russia. [Schmidt-Chanasit, Jonas] Bernhard Nocht Inst Trop Med, Dept Virol, Hamburg, Germany. [Stoecker, Andreas] Univ Fed Bahia, Infect Dis Res Lab, Univ Hosp Prof Edgard Santos, Salvador, BA, Brazil. [Borges Carneiro, Aroldo Jose; Franke, Carlos Roberto] Univ Fed Bahia, Sch Vet Med, Salvador, BA, Brazil. [Erbar, Stephanie; Maisner, Andrea] Univ Marburg, Inst Virol, D-3550 Marburg, Germany. [Fronhoffs, Florian; Buettner, Reinhard] Univ Bonn, Inst Pathol, Med Ctr, Bonn, Germany. [Buettner, Reinhard] Univ Cologne, Inst Pathol, Med Ctr, Cologne, Germany. [Kalko, Elisabeth K. V.] Univ Ulm, Inst Expt Ecol, Ulm, Germany. [Kalko, Elisabeth K. V.] Smithsonian Trop Res Inst, Balboa, Panama. [Kruppa, Thomas] Kumasi Ctr Collaborat Res Trop Med KCCR, Kumasi, Ghana. [Yandoko, Emmanuel R. N.] Inst Pasteur, Bangui, Cent Afr Republ. [Reusken, Chantal] Netherlands Ctr Infect Dis Control, Bilthoven, Netherlands. [Hassanin, Alexandre] Museum Natl Hist Nat, Ctr Natl Rech Sci, UMR 7205, F-75231 Paris, France. [Krueger, Detlev H.] Charite, Inst Med Virol, Berlin, Germany. [Matthee, Sonja] Univ Stellenbosch, Dept Conservat Ecol & Entomol, ZA-7600 Stellenbosch, South Africa. [Ulrich, Rainer G.] Friedrich Loeffler Inst, Inst Novel & Emerging Infect Dis, Greifswald, Germany. [Leroy, Eric M.] IRD CNRS UM1, UMR MIVEGEC 224, Inst Rech Dev, Montpellier, France. RP Drosten, C (reprint author), Univ Bonn, Med Ctr, Inst Virol, D-53127 Bonn, Germany. EM drosten@virology-bonn.de RI Lukashev, Alexander/G-2777-2013; Drexler, Jan Felix/C-1004-2014; Vallo, Peter/F-9650-2014; Knornschild, Mirjam/C-9401-2011; Hassanin, Alexandre/P-3329-2014; LEROY, Eric/I-4347-2016; OI Lukashev, Alexander/0000-0001-7365-0352; Mueller, Marcel/0000-0003-2242-5117; Corman, Victor Max/0000-0002-3605-0136; Hassanin, Alexandre/0000-0002-4905-8540; LEROY, Eric/0000-0003-0022-0890; Schmidt-Chanasit, Jonas/0000-0003-4433-0231 FU European Union [223498]; EVA [228292]; German Federal Ministry of Education and Research (BMBF) [01KIO701]; German Research Foundation (DFG) [DR 772/3-1]; German Federal Ministry of Education and Research (BMBF) through the National Research Platform for Zoonoses [01KI1018]; Umweltbundesamt [FKZ 370941401]; Robert Koch-Institut through the Government of Gabon, Total-Fina-Elf Gabon [FKZ 1362/1-924]; Ministere des Affaires Etrangeres, France FX We would like to thank Sebastian Brunink, Monika Eschbach-Bludau, Tobias Bleicker, Sandra Junglen, Marko Marklewitz, Fabian Ebach, Thierno Diawo Dallo, Adriana Fumie Tateno and Rodrigo Melim Zerbinati at the Institute of Virology, Bonn, for technical assistance. We are grateful to Stefan Klose, Veronika Cottentail und Mirjam Knornschild (University Ulm), Milen Rashkov, Justin Robarge and Lyubomir Zhelyazkov (Strandja Natural Park), Uwe Hermanns (NABU Rostock NGO), Matthias Gottsche (University Kiel), Elena Tilova, Liubomir Ilankov (Green Balkans NGO), Augustina Annan (KCCR), Andreas Kurth (RKI), Kai Fechner and Erik Lattwein (Euroimmun), Anne Ipsen (Noctalis), Andreas Kiefer (Nature Conservation Project Mayen), the volunteers at the Bonn Consortium for Bat Conservation (BAFF), Manfred Braun (Struktur- und Genehmigungsbehorde Nord, Koblenz), Christian Nowak, Lena Grosche, Frauke Meier, and Myriam Gotz (Echolot GbR), Flavia dos Santos (UFBA) Carlos R. Brites, Eduardo M. Netto, Celia Pedroso, Breno Frederico de Carvalho Dominguez Souza, Jefferson Ivan Correa (LAPI), Stephanie Erbar (University Marburg), Thomas Jakel (GTZ, Bangkok), Jean-Paul Gonzalez, Mathieu Bourgarel, Xavier Pourrut, Dieudonne Nkoghe, Peggy Motsch, Andre Delicat, Philippe Engandja (CIRMF), Carine Ngoagouni (Pasteur Bangui), Nicolas Nesi (MNHN) and Didier Tshikung (UNILU), Jorg Thiel (Gotha), Margrit Bemmann (Schwerin), Daniela Reil, Christian Imholt, Jens Jacob, Katarina Kuhn, Engelbert Kampling, Mechthild Budde, Dagmar Funck (JKI, Munster), Jona Freise, Brita Oltmann (LAVES, Oldenburg), Sebastian Guenther, Brigitte Bannert (Berlin), Gerald Heckel (Bern), Matthias Wenk (Eberswalde), Henrike Gregersen (Stuttgart), Johannes Lang (Lich), Anita Plenge-Bonig (Hamburg), Nicole Schauerte (Frankfurt/Main), Susanne Modrow (Regensburg), Gerhard Maluck (Bergatreute), Richard Kruczewski (Borchen), Maria Nemeth (Budapest), Sabrina Schmidt, Ulrike M. Rosenfeld, Anne Balkema-Buschmann, Susanne Jackel, Horst Schirrmeier, Mathias Schlegel, Hanan Sheikh Ali, Christian Kretzschmar, Konrad Wanka, Ute Wessels, Theres Wollny, Kathrin Baumann, Grit Mowert, Franziska Thomas, Barbel Hammerschmidt, Daniel Windolph, Josephine Schlosser, Marc Mertens, Paul Dremsek, Katja Plifke, Kerstin Tauscher, Angele Breithaupt, Nadja Lorenz, Christian Korthase, Andre Schutte, Julie Elkins and Sylvia Ferguson (FLI, Greifswald-Insel Riems) for field work and technical assistance. This study was funded by the European Union FP7 projects EMPERIE (Grant agreement number 223498) and EVA (Grant agreement number 228292), the German Federal Ministry of Education and Research (BMBF; project code 01KIO701), the German Research Foundation (DFG; Grant agreement number DR 772/3-1)to CD; the German Federal Ministry of Education and Research (BMBF) through the National Research Platform for Zoonoses (project code 01KI1018), the Umweltbundesamt (FKZ 370941401) and the Robert Koch-Institut (FKZ 1362/1-924) to RGU; through the Government of Gabon, Total-Fina-Elf Gabon and the Ministere des Affaires Etrangeres, France. This paper is dedicated to the memory of the late Elisabeth Kalko. NR 60 TC 209 Z9 216 U1 11 U2 97 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 2041-1723 J9 NAT COMMUN JI Nat. Commun. PD APR PY 2012 VL 3 AR 796 DI 10.1038/ncomms1796 PG 12 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 934PB UT WOS:000303455200033 PM 22531181 ER PT J AU Rodrigues, RR Zuanon, J Del-Claro, K Carvalho, LN AF Rodrigues, Raoni Rosa Zuanon, Jansen Del-Claro, Kleber Carvalho, Lucelia Nobre TI Reproductive behavior of the Amazonian dwarf cichlid Apistogramma hippolytae Kullander, 1982: offsetting costs and benefits SO ACTA ETHOLOGICA LA English DT Article DE Trade-off; Feeding behavior; Parental care; Reproduction; Cichlidae ID TRADE-OFF; PARENTAL CARE; MATING SYSTEM; FISH; PREDATION; CONFLICT; SIZE AB The reproduction trade-off for an animal is a conflicting choice in which resources (e.g., time and/or energy) allocated to one reproduction trait (e.g., parental care) become unavailable to other traits (e.g., future reproduction events). Here, we tested three hypotheses related to the parental care of the Amazonian dwarf cichlid Apistogramma hippolytae in its natural habitat of Central Amazonia: (1) brood-caring females have a lower feeding frequency than individuals that are not involved in this behavior; (2) females that spend more time on nest defense have lower feeding rates; and (3) females can recognize the species that present the greatest danger to its offspring and move farther from the nest to chase away these piscivorous fishes. We also described for the first time the reproductive behavior (including courtship) and parental care of this species. The results showed that maternal care produces a reduction in the rate of feeding of mothers, a greater amount of time is spent chasing invaders away from the nest, and reproductive females are able to distinguish species-specific predators. These observations support the hypotheses of this study and also suggest a trade-off between current and future reproduction events. C1 [Rodrigues, Raoni Rosa] Univ Fed Minas Gerais, Ctr Transposicao Peixes ICB, BR-31270901 Belo Horizonte, MG, Brazil. [Rodrigues, Raoni Rosa; Del-Claro, Kleber] Univ Fed Uberlandia, LECI Lab Ecol Comportamental & Interacoes, BR-38400902 Uberlandia, MG, Brazil. [Zuanon, Jansen; Carvalho, Lucelia Nobre] Inst Nacl Pesquisas Amazonia INPA, BR-69011970 Manaus, Amazonas, Brazil. [Zuanon, Jansen; Carvalho, Lucelia Nobre] Smithsonian Trop Res Inst, Biol Dynam Forest Fragments Project BDFFP, BR-69011970 Manaus, Amazonas, Brazil. RP Rodrigues, RR (reprint author), Univ Fed Minas Gerais, Ctr Transposicao Peixes ICB, Av Antonio Carlos,6627,Bloco E2,Sala 180, BR-31270901 Belo Horizonte, MG, Brazil. EM raonirosa@yahoo.com.br; zuanon@inpa.gov.br; delclaro@ufu.br; carvalholn@yahoo.com.br RI Del-Claro, Kleber/C-5570-2013; Nobre Carvalho, Lucelia/D-5986-2013; Adapta, Inct/J-8371-2013; Rodrigues, Raoni/O-9810-2015 OI Del-Claro, Kleber/0000-0001-8886-9568; Nobre Carvalho, Lucelia/0000-0002-0673-0165; FU Biological Dynamics of Forest Fragments Project (BDFFP-INPA/Smithsonian Tropical Research Institute); Programa de Educacao Tutorial (PET-SESu/MEC); Brazilian National Council of Scientific and Technological Development (CNPq); Fundacao de Amparo a Pesquisa do Estado de Minas Gerais (FAPEMIG); Fundacao de Amparo a Pesquisa do Estado do Amazonas (FAPEAM); Fundacao "O Boticario" de protecao a Natureza FX We are grateful to Eduardo Barata, Vitor Almada, and two anonymous reviewers for their significant suggestions that improved this manuscript. We also thank the following individuals: Fernando Mendonca for the use of photo illustrations in this paper; Fabricio Tereza, and Rafael Arruda for careful reading and suggestions for this manuscript; Renzo Reis and Ronan Rodrigues for help with the English translation of the text; and the technicians of the BDFFP, especially O.S. Pereira and Sr. Cardoso for their valuable help during the field work. The Biological Dynamics of Forest Fragments Project (BDFFP-INPA/Smithsonian Tropical Research Institute) provided logistical and financial support for the field work and for the stay of RRR in Manaus. The Programa de Educacao Tutorial (PET-SESu/MEC) financed the graduate studies of RRR. The Brazilian National Council of Scientific and Technological Development (CNPq) and Fundacao de Amparo a Pesquisa do Estado de Minas Gerais (FAPEMIG) provided research grants to KDC. CNPq, Fundacao de Amparo a Pesquisa do Estado do Amazonas (FAPEAM) and Fundacao "O Boticario" de protecao a Natureza provided financial support to the Igarapes Project. This is contribution number 573 of the BDFFP and number 18 of the Igarapes Project. NR 42 TC 1 Z9 1 U1 0 U2 11 PU SPRINGER HEIDELBERG PI HEIDELBERG PA TIERGARTENSTRASSE 17, D-69121 HEIDELBERG, GERMANY SN 0873-9749 J9 ACTA ETHOL JI Acta Ethol. PD APR PY 2012 VL 15 IS 1 BP 47 EP 53 DI 10.1007/s10211-011-0107-8 PG 7 WC Behavioral Sciences; Zoology SC Behavioral Sciences; Zoology GA 928VF UT WOS:000303014800007 ER PT J AU Loeb, A Turner, EL AF Loeb, Abraham Turner, Edwin L. TI Detection Technique for Artificially Illuminated Objects in the Outer Solar System and Beyond SO ASTROBIOLOGY LA English DT Article DE Astrobiology; SETI; Kuiper belt objects; Artificial illumination ID EXOPLANET DIRECT CHARACTERIZATION; TRANS-NEPTUNIAN OBJECTS; DISTANT ICY BODIES; EXTRATERRESTRIAL INTELLIGENCE; PHASE CURVES; FAR FUTURE; SEARCH; SETI; WILL AB Existing and planned optical telescopes and surveys can detect artificially illuminated objects, comparable in total brightness to a major terrestrial city, at the outskirts of the Solar System. Orbital parameters of Kuiper belt objects (KBOs) are routinely measured to exquisite precisions of <10(-3). Here, we propose to measure the variation of the observed flux F from such objects as a function of their changing orbital distances D. Sunlight-illuminated objects will show a logarithmic slope alpha equivalent to (d log F/d log D)= -4, whereas artificially illuminated objects should exhibit alpha = -2. The proposed Large Synoptic Survey Telescope (LSST) and other planned surveys will provide superb data and allow measurement of alpha for thousands of KBOs. If objects with alpha = -2 are found, follow-up observations could measure their spectra to determine whether they are illuminated by artificial lighting. The search can be extended beyond the Solar System with future generations of telescopes on the ground and in space that would have the capacity to detect phase modulation due to very strong artificial illumination on the nightside of planets as they orbit their parent stars. C1 [Turner, Edwin L.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. [Turner, Edwin L.] Univ Tokyo, Inst Phys & Math Universe, Kashiwa, Chiba, Japan. [Loeb, Abraham] Harvard Univ, Dept Astron, Cambridge, MA 02138 USA. [Loeb, Abraham] Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, Cambridge, MA 02138 USA. RP Turner, EL (reprint author), Princeton Univ, Dept Astrophys Sci, 208 Peyton Hall,4 Ivy Lane, Princeton, NJ 08544 USA. EM elt@astro.princeton.edu RI Turner, Edwin/A-4295-2011 FU NSF [AST-0907890]; NASA [NNX08AL43G, NNA09D-B30A]; Princeton University; World Premier International Research Center Initiative (WPI Initiative), MEXT, Japan FX We thank F. Dyson, M. Holman, and A. Parker for helpful comments. A.L. was supported in part by NSF grant AST-0907890 and NASA grants NNX08AL43G and NNA09D-B30A. E.L.T. gratefully acknowledges support from a Princeton University Global Collaborative Research Fund grant and the World Premier International Research Center Initiative (WPI Initiative), MEXT, Japan. NR 23 TC 4 Z9 4 U1 0 U2 9 PU MARY ANN LIEBERT INC PI NEW ROCHELLE PA 140 HUGUENOT STREET, 3RD FL, NEW ROCHELLE, NY 10801 USA SN 1531-1074 J9 ASTROBIOLOGY JI Astrobiology PD APR PY 2012 VL 12 IS 4 BP 290 EP 294 DI 10.1089/ast.2011.0758 PG 5 WC Astronomy & Astrophysics; Biology; Geosciences, Multidisciplinary SC Astronomy & Astrophysics; Life Sciences & Biomedicine - Other Topics; Geology GA 929LK UT WOS:000303064900002 PM 22490065 ER PT J AU Huchra, JP Macri, LM Masters, KL Jarrett, TH Berlind, P Calkins, M Crook, AC Cutri, R Erdogdu, P Falco, E George, T Hutcheson, CM Lahav, O Mader, J Mink, JD Martimbeau, N Schneider, S Skrutskie, M Tokarz, S Westover, M AF Huchra, John P. Macri, Lucas M. Masters, Karen L. Jarrett, Thomas H. Berlind, Perry Calkins, Michael Crook, Aidan C. Cutri, Roc Erdogdu, Pirin Falco, Emilio George, Teddy Hutcheson, Conrad M. Lahav, Ofer Mader, Jeff Mink, Jessica D. Martimbeau, Nathalie Schneider, Stephen Skrutskie, Michael Tokarz, Susan Westover, Michael TI THE 2MASS REDSHIFT SURVEY-DESCRIPTION AND DATA RELEASE SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE catalogs; galaxies: distances and redshifts; surveys ID EARLY-TYPE GALAXIES; TULLY-FISHER RELATION; LARGE-SCALE STRUCTURE; ALL-SKY SURVEY; SOUTHERN MILKY-WAY; PISCES-PERSEUS SUPERCLUSTER; BRIGHT-NUCLEUS GALAXIES; EMISSION-LINE GALAXIES; ACTIVE GALACTIC NUCLEI; NEUTRAL HYDROGEN OBSERVATIONS AB We present the results of the 2MASS Redshift Survey (2MRS), a ten-year project to map the full three-dimensional distribution of galaxies in the nearby universe. The Two Micron All Sky Survey (2MASS) was completed in 2003 and its final data products, including an extended source catalog (XSC), are available online. The 2MASS XSC contains nearly a million galaxies with K-s <= 13.5 mag and is essentially complete and mostly unaffected by interstellar extinction and stellar confusion down to a galactic latitude of vertical bar b vertical bar = 5 degrees for bright galaxies. Near-infrared wavelengths are sensitive to the old stellar populations that dominate galaxy masses, making 2MASS an excellent starting point to study the distribution of matter in the nearby universe. We selected a sample of 44,599 2MASS galaxies with K-s <= 11.75 mag and vertical bar b vertical bar >= 5 degrees (>= 8 degrees toward the Galactic bulge) as the input catalog for our survey. We obtained spectroscopic observations for 11,000 galaxies and used previously obtained velocities for the remainder of the sample to generate a redshift catalog that is 97.6% complete to well-defined limits and covers 91% of the sky. This provides an unprecedented census of galaxy (baryonic mass) concentrations within 300 Mpc. Earlier versions of our survey have been used in a number of publications that have studied the bulk motion of the Local Group, mapped the density and peculiar velocity fields out to 50 h(-1) Mpc, detected galaxy groups, and estimated the values of several cosmological parameters. Additionally, we present morphological types for a nearly complete sub-sample of 20,860 galaxies with K-s <= 11.25 mag and vertical bar b vertical bar >= 10 degrees. C1 [Macri, Lucas M.] Texas A&M Univ, George P & Cynthia Woods Mitchell Inst Fundamenta, Dept Phys & Astron, College Stn, TX 77843 USA. [Masters, Karen L.] Univ Portsmouth, Inst Cosmol & Gravitat, Portsmouth PO1 3FX, Hants, England. [Masters, Karen L.; Cutri, Roc] SEPNet SE Phys Network, Southampton, Hants, England. [Jarrett, Thomas H.] CALTECH, Ctr Infrared Proc & Anal, Pasadena, CA 91125 USA. [Crook, Aidan C.] Microsoft Corp, Redmond, WA 98052 USA. [Erdogdu, Pirin; Lahav, Ofer] UCL, Dept Phys & Astron, London WC1E 6BT, England. [George, Teddy] Canada France Hawaii Telescope Corp, Kamuela, HI 96743 USA. [Hutcheson, Conrad M.] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94309 USA. [Mader, Jeff] Keck Observ, Kamuela, HI 96743 USA. [Martimbeau, Nathalie] Planetarium Montreal, Montreal, PQ H3C 1G7, Canada. [Schneider, Stephen] Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA. [Skrutskie, Michael] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA. [Westover, Michael] McKinsey & Co Inc, Seattle, WA 98101 USA. [Huchra, John P.; Berlind, Perry; Calkins, Michael; Falco, Emilio; Mink, Jessica D.; Tokarz, Susan] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. EM lmacri@tamu.edu; karen.masters@port.ac.uk OI Masters, Karen/0000-0003-0846-9578; Mink, Jessica/0000-0003-3594-1823; Macri, Lucas/0000-0002-1775-4859 FU National Science Foundation [AST-0406906]; Smithsonian Institution; NASA from the Space Telescope Science Institute [HST-HF-01153]; National Science Foundation from the National Optical Astronomy Observatory; Texas AM University; Leverhulme Trust; Peter and Patricia Gruber Foundation; Royal Society; National Aeronautics and Space Administration; Australian Research Council [DP-0208876]; National Science Foundation Research Experience for Undergraduates [9731923]; Alfred P. Sloan Foundation; U.S. Department of Energy FX J.P.H., K.L.M., and A.C.C. acknowledge support by the National Science Foundation under grant AST-0406906 and by the Smithsonian Institution.; L.M.M. acknowledges support by the Smithsonian Institution Visiting Scholar program, by NASA through Hubble Fellowship Grant HST-HF-01153 from the Space Telescope Science Institute, by the National Science Foundation through a Goldberg Fellowship from the National Optical Astronomy Observatory, and by the Texas A&M University Mitchell-Heep-Munnerlyn Endowed Career Enhancement Professorship in Physics or Astronomy.; K.L.M. acknowledges funding from the Leverhulme Trust as a 2010 Early Career Fellow and from the Peter and Patricia Gruber Foundation as the 2008 IAU Fellow.; C.M.H. was supported in part by the National Science Foundation Research Experience for Undergraduates under grant No. 9731923.; O.L. acknowledges support from a Royal Society Wolfson Research Merit Award.; This publication has made use of the following resources.; 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 at the California Institute of Technology, funded by the National Aeronautics and Space Administration and the National Science Foundation.; The 6dF Galaxy Survey (DR3), supported by Australian Research Council Discovery Projects Grant (DP-0208876). The 6dFGS web site is http://www.aao.gov.au/local/www/6df/.; The Sloan Digital Sky Survey III (DR8). 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. 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, the Brookhaven National Laboratory, the University of Cambridge, the University of Florida, the French Participation Group, the German Participation Group, the Instituto de Astrofisica de Canarias, the Michigan State/Notre Dame/JINA Participation Group, Johns Hopkins University, the Lawrence Berkeley National Laboratory, the Max Planck Institute for Astrophysics, New Mexico State University, New York University, The Ohio State University, Pennsylvania State University, the University of Portsmouth, Princeton University, the Spanish Participation Group, the University of Tokyo, the University of Utah, Vanderbilt University, the University of Virginia, the University of Washington, and Yale University. NR 632 TC 162 Z9 167 U1 0 U2 8 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 APR PY 2012 VL 199 IS 2 AR 26 DI 10.1088/0067-0049/199/2/26 PG 22 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 929ZT UT WOS:000303105400002 ER PT J AU Nolan, PL Abdo, AA Ackermann, M Ajello, M Allafort, A Antolini, E Atwood, WB Axelsson, M Baldini, L Ballet, J Barbiellini, G Bastieri, D Bechtol, K Belfiore, A Bellazzini, R Berenji, B Bignami, GF Blandford, RD Bloom, ED Bonamente, E Bonnell, J Borgland, AW Bottacini, E Bouvier, A Brandt, TJ Bregeon, J Brigida, M Bruel, P Buehler, R Burnett, TH Buson, S Caliandro, GA Cameron, RA Campana, R Canadas, B Cannon, A Caraveo, PA Casandjian, JM Cavazzuti, E Ceccanti, M Cecchi, C Celik, O Charles, E Chekhtman, A Cheung, CC Chiang, J Chipaux, R Ciprini, S Claus, R Cohen-Tanugi, J Cominsky, LR Conrad, J Corbet, R Cutini, S D'Ammando, F Davis, DS de Angelis, A DeCesar, ME DeKlotz, M De Luca, A den Hartog, PR de Palma, F Dermer, CD Digel, SW Silva, EDE Drell, PS Drlica-Wagner, A Dubois, R Dumora, D Enoto, T Escande, L Fabiani, D Falletti, L Favuzzi, C Fegan, SJ Ferrara, EC Focke, WB Fortin, P Frailis, M Fukazawa, Y Funk, S Fusco, P Gargano, F Gasparrini, D Gehrels, N Germani, S Giebels, B Giglietto, N Giommi, P Giordano, F Giroletti, M Glanzman, T Godfrey, G Grenier, IA Grondin, MH Grove, JE Guillemot, L Guiriec, S Gustafsson, M Hadasch, D Hanabata, Y Harding, AK Hayashida, M Hays, E Hill, AB Horan, D Hou, X Hughes, RE Iafrate, G Itoh, R Johannesson, G Johnson, RP Johnson, TE Johnson, AS Johnson, TJ Kamae, T Katagiri, H Kataoka, J Katsuta, J Kawai, N Kerr, M Knodlseder, J Kocevski, D Kuss, M Lande, J Landriu, D Latronico, L Lemoine-Goumard, M Lionetto, AM Garde, ML Longo, F Loparco, F Lott, B Lovellette, MN Lubrano, P Madejski, GM Marelli, M Massaro, E Mazziotta, MN McConville, W McEnery, JE Mehault, J Michelson, PF Minuti, M Mitthumsiri, W Mizuno, T Moiseev, AA Mongelli, M Monte, C Monzani, ME Morselli, A Moskalenko, IV Murgia, S Nakamori, T Naumann-Godo, M Norris, JP Nuss, E Nymark, T Ohno, M Ohsugi, T Okumura, A Omodei, N Orlando, E Ormes, JF Ozaki, M Paneque, D Panetta, JH Parent, D Perkins, JS Pesce-Rollins, M Pierbattista, M Pinchera, M Piron, F Pivato, G Porter, TA Racusin, JL Raino, S Rando, R Razzano, M Razzaque, S Reimer, A Reimer, O Reposeur, T Ritz, S Rochester, LS Romani, RW Roth, M Rousseau, R Ryde, F Sadrozinski, HFW Salvetti, D Sanchez, DA Parkinson, PMS Sbarra, C Scargle, JD Schalk, TL Sgro, C Shaw, MS Shrader, C Siskind, EJ Smith, DA Spandre, G Spinelli, P Stephens, TE Strickman, MS Suson, DJ Tajima, H Takahashi, H Takahashi, T Tanaka, T Thayer, JG Thayer, JB Thompson, DJ Tibaldo, L Tibolla, O Tinebra, F Tinivella, M Torres, DF Tosti, G Troja, E Uchiyama, Y Vandenbroucke, J Van Etten, A Van Klaveren, B Vasileiou, V Vianello, G Vitale, V Waite, AP Wallace, E Wang, P Werner, M Winer, BL Wood, DL Wood, KS Wood, M Yang, Z Zimmer, S AF Nolan, P. L. Abdo, A. A. Ackermann, M. Ajello, M. Allafort, A. Antolini, E. Atwood, W. B. Axelsson, M. Baldini, L. Ballet, J. Barbiellini, G. Bastieri, D. Bechtol, K. Belfiore, A. Bellazzini, R. Berenji, B. Bignami, G. F. Blandford, R. D. Bloom, E. D. Bonamente, E. Bonnell, J. Borgland, A. W. Bottacini, E. Bouvier, A. Brandt, T. J. Bregeon, J. Brigida, M. Bruel, P. Buehler, R. Burnett, T. H. Buson, S. Caliandro, G. A. Cameron, R. A. Campana, R. Canadas, B. Cannon, A. Caraveo, P. A. Casandjian, J. M. Cavazzuti, E. Ceccanti, M. Cecchi, C. Celik, Oe Charles, E. Chekhtman, A. Cheung, C. C. Chiang, J. Chipaux, R. Ciprini, S. Claus, R. Cohen-Tanugi, J. Cominsky, L. R. Conrad, J. Corbet, R. Cutini, S. D'Ammando, F. Davis, D. S. de Angelis, A. DeCesar, M. E. DeKlotz, M. De Luca, A. den Hartog, P. R. de Palma, F. Dermer, C. D. Digel, S. W. Do Couto E Silva, E. Drell, P. S. Drlica-Wagner, A. Dubois, R. Dumora, D. Enoto, T. Escande, L. Fabiani, D. Falletti, L. Favuzzi, C. Fegan, S. J. Ferrara, E. C. Focke, W. B. Fortin, P. Frailis, M. Fukazawa, Y. Funk, S. Fusco, P. Gargano, F. Gasparrini, D. Gehrels, N. Germani, S. Giebels, B. Giglietto, N. Giommi, P. Giordano, F. Giroletti, M. Glanzman, T. Godfrey, G. Grenier, I. A. Grondin, M. -H. Grove, J. E. Guillemot, L. Guiriec, S. Gustafsson, M. Hadasch, D. Hanabata, Y. Harding, A. K. Hayashida, M. Hays, E. Hill, A. B. Horan, D. Hou, X. Hughes, R. E. Iafrate, G. Itoh, R. Johannesson, G. Johnson, R. P. Johnson, T. E. Johnson, A. S. Johnson, T. J. Kamae, T. Katagiri, H. Kataoka, J. Katsuta, J. Kawai, N. Kerr, M. Knoedlseder, J. Kocevski, D. Kuss, M. Lande, J. Landriu, D. Latronico, L. Lemoine-Goumard, M. Lionetto, A. M. Garde, M. Llena Longo, F. Loparco, F. Lott, B. Lovellette, M. N. Lubrano, P. Madejski, G. M. Marelli, M. Massaro, E. Mazziotta, M. N. McConville, W. McEnery, J. E. Mehault, J. Michelson, P. F. Minuti, M. Mitthumsiri, W. Mizuno, T. Moiseev, A. A. Mongelli, M. Monte, C. Monzani, M. E. Morselli, A. Moskalenko, I. V. Murgia, S. Nakamori, T. Naumann-Godo, M. Norris, J. P. Nuss, E. Nymark, T. Ohno, M. Ohsugi, T. Okumura, A. Omodei, N. Orlando, E. Ormes, J. F. Ozaki, M. Paneque, D. Panetta, J. H. Parent, D. Perkins, J. S. Pesce-Rollins, M. Pierbattista, M. Pinchera, M. Piron, F. Pivato, G. Porter, T. A. Racusin, J. L. Raino, S. Rando, R. Razzano, M. Razzaque, S. Reimer, A. Reimer, O. Reposeur, T. Ritz, S. Rochester, L. S. Romani, R. W. Roth, M. Rousseau, R. Ryde, F. Sadrozinski, H. F. -W. Salvetti, D. Sanchez, D. A. Parkinson, P. M. Saz Sbarra, C. Scargle, J. D. Schalk, T. L. Sgro, C. Shaw, M. S. Shrader, C. Siskind, E. J. Smith, D. A. Spandre, G. Spinelli, P. Stephens, T. E. Strickman, M. S. Suson, D. J. Tajima, H. Takahashi, H. Takahashi, T. Tanaka, T. Thayer, J. G. Thayer, J. B. Thompson, D. J. Tibaldo, L. Tibolla, O. Tinebra, F. Tinivella, M. Torres, D. F. Tosti, G. Troja, E. Uchiyama, Y. Vandenbroucke, J. Van Etten, A. Van Klaveren, B. Vasileiou, V. Vianello, G. Vitale, V. Waite, A. P. Wallace, E. Wang, P. Werner, M. Winer, B. L. Wood, D. L. Wood, K. S. Wood, M. Yang, Z. Zimmer, S. TI FERMI LARGE AREA TELESCOPE SECOND SOURCE CATALOG SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE catalogs; gamma rays: general ID GAMMA-RAY EMISSION; ACTIVE GALACTIC NUCLEI; PULSAR WIND NEBULA; PSR B1259-63/LS 2883; ALL-SKY SURVEY; SUPERNOVA REMNANT; MILLISECOND PULSARS; GLOBULAR-CLUSTERS; MAGELLANIC-CLOUD; SPACE-TELESCOPE AB We present the second catalog of high-energy gamma-ray sources detected by the Large Area Telescope (LAT), the primary science instrument on the Fermi Gamma-ray Space Telescope (Fermi), derived from data taken during the first 24 months of the science phase of the mission, which began on 2008 August 4. Source detection is based on the average flux over the 24 month period. The second Fermi-LAT catalog (2FGL) includes source location regions, defined in terms of elliptical fits to the 95% confidence regions and spectral fits in terms of power-law, exponentially cutoff power-law, or log-normal forms. Also included are flux measurements in five energy bands and light curves on monthly intervals for each source. Twelve sources in the catalog are modeled as spatially extended. We provide a detailed comparison of the results from this catalog with those from the first Fermi-LAT catalog (1FGL). Although the diffuse Galactic and isotropic models used in the 2FGL analysis are improved compared to the 1FGL catalog, we attach caution flags to 162 of the sources to indicate possible confusion with residual imperfections in the diffuse model. The 2FGL catalog contains 1873 sources detected and characterized in the 100 MeV to 100 GeV range of which we consider 127 as being firmly identified and 1171 as being reliably associated with counterparts of known or likely gamma-ray-producing source classes. C1 [Nolan, P. L.; Ajello, M.; Allafort, A.; Bechtol, K.; Berenji, B.; Blandford, R. D.; Bloom, E. D.; Borgland, A. W.; Bottacini, E.; Buehler, R.; Cameron, R. A.; Charles, E.; Chiang, J.; Claus, R.; den Hartog, P. R.; Digel, S. W.; Do Couto E Silva, E.; Drell, P. S.; Drlica-Wagner, A.; Dubois, R.; Enoto, T.; Focke, W. B.; Funk, S.; Glanzman, T.; Godfrey, G.; Hayashida, M.; Johnson, A. S.; Kamae, T.; Katsuta, J.; Kerr, M.; Kocevski, D.; Lande, J.; Madejski, G. M.; Michelson, P. F.; Mitthumsiri, W.; Monzani, M. E.; Moskalenko, I. V.; Murgia, S.; Okumura, A.; Omodei, N.; Orlando, E.; Paneque, D.; Panetta, J. H.; Porter, T. A.; Reimer, A.; Reimer, O.; Rochester, L. S.; Romani, R. W.; Shaw, M. S.; Tajima, H.; Tanaka, T.; Thayer, J. G.; Thayer, J. B.; Uchiyama, Y.; Vandenbroucke, J.; Van Etten, A.; Van Klaveren, B.; Vianello, G.; Waite, A. P.; Wang, P.; Wood, M.] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, WW Hansen Expt Phys Lab, Dept Phys, Stanford, CA 94305 USA. [Nolan, P. L.; Ajello, M.; Allafort, A.; Bechtol, K.; Berenji, B.; Blandford, R. D.; Bloom, E. D.; Borgland, A. W.; Bottacini, E.; Buehler, R.; Cameron, R. A.; Charles, E.; Chiang, J.; Claus, R.; den Hartog, P. R.; Digel, S. W.; Do Couto E Silva, E.; Drell, P. S.; Drlica-Wagner, A.; Dubois, R.; Enoto, T.; Focke, W. B.; Funk, S.; Glanzman, T.; Godfrey, G.; Hayashida, M.; Johnson, A. S.; Kamae, T.; Katsuta, J.; Kerr, M.; Kocevski, D.; Lande, J.; Madejski, G. M.; Michelson, P. F.; Mitthumsiri, W.; Monzani, M. E.; Moskalenko, I. V.; Murgia, S.; Okumura, A.; Omodei, N.; Orlando, E.; Paneque, D.; Panetta, J. H.; Porter, T. A.; Reimer, A.; Reimer, O.; Rochester, L. S.; Romani, R. W.; Shaw, M. S.; Tajima, H.; Tanaka, T.; Thayer, J. G.; Thayer, J. B.; Uchiyama, Y.; Vandenbroucke, J.; Van Etten, A.; Van Klaveren, B.; Vianello, G.; Waite, A. P.; Wang, P.; Wood, M.] Stanford Univ, SLAC Natl Accelerator Lab, Stanford, CA 94305 USA. [Abdo, A. A.; Parent, D.; Razzaque, S.] George Mason Univ, Coll Sci, Ctr Earth Observing & Space Res, Fairfax, VA 22030 USA. [Ackermann, M.] Deutsch Elektronen Synchrotron DESY, D-15738 Zeuthen, Germany. [Antolini, E.; Bonamente, E.; Cecchi, C.; Germani, S.; Lubrano, P.; Tosti, G.] Ist Nazl Fis Nucl, Sez Perugia, I-06123 Perugia, Italy. [Antolini, E.; Bonamente, E.; Cecchi, C.; Ciprini, S.; Germani, S.; Lubrano, P.; Tosti, G.] Univ Perugia, Dipartimento Fis, I-06123 Perugia, Italy. [Atwood, W. B.; Belfiore, A.; Bouvier, A.; Johnson, R. P.; Razzano, M.; Ritz, S.; Sadrozinski, H. F. -W.; Parkinson, P. M. Saz; Schalk, T. L.] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Dept Phys, Santa Cruz, CA 95064 USA. [Atwood, W. B.; Belfiore, A.; Bouvier, A.; Johnson, R. P.; Razzano, M.; Ritz, S.; Sadrozinski, H. F. -W.; Parkinson, P. M. Saz; Schalk, T. L.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. [Axelsson, M.] Stockholm Univ, Dept Astron, SE-10691 Stockholm, Sweden. [Nolan, P. L.; Abdo, A. A.; Axelsson, M.; Conrad, J.; Garde, M. Llena; Nymark, T.; Ryde, F.; Yang, Z.; Zimmer, S.] Oskar Klein Ctr Cosmoparticle Phys, SE-10691 Stockholm, Sweden. [Axelsson, M.; Nymark, T.; Ryde, F.] Royal Inst Technol KTH, Dept Phys, SE-10691 Stockholm, Sweden. [Baldini, L.; Bellazzini, R.; Bregeon, J.; Ceccanti, M.; Fabiani, D.; Kuss, M.; Minuti, M.; Pesce-Rollins, M.; Pinchera, M.; Razzano, M.; Sgro, C.; Spandre, G.; Tinivella, M.] Ist Nazl Fis Nucl, Sez Pisa, I-56127 Pisa, Italy. [Ballet, J.; Casandjian, J. M.; Grenier, I. A.; Landriu, D.; Naumann-Godo, M.; Pierbattista, M.] Univ Paris Diderot, CEA Saclay, Serv Astrophys, Lab AIM,CEA,IRFU,CNRS, F-91191 Gif Sur Yvette, France. [Barbiellini, G.; Iafrate, G.; Longo, F.] Ist Nazl Fis Nucl, Sez Trieste, I-34127 Trieste, Italy. [Barbiellini, G.; Longo, F.] Univ Trieste, Dipartimento Fis, I-34127 Trieste, Italy. [Bastieri, D.; Buson, S.; Gustafsson, M.; Rando, R.; Sbarra, C.; Tibaldo, L.] Ist Nazl Fis Nucl, Sez Padova, I-35131 Padua, Italy. [Bastieri, D.; Buson, S.; Pivato, G.; Rando, R.; Tibaldo, L.] Univ Padua, Dipartimento Fis G Galilei, I-35131 Padua, Italy. [Belfiore, A.] Univ Pavia, Dipartimento Fis Nucl & Teor, I-27100 Pavia, Italy. [Belfiore, A.; Caraveo, P. A.; Marelli, M.; Salvetti, D.] INAF Ist Astrofis Spaziale & Fis Cosm, I-20133 Milan, Italy. [Bignami, G. F.; De Luca, A.] IUSS, I-27100 Pavia, Italy. [Bonnell, J.; Cannon, A.; Celik, Oe; Corbet, R.; Davis, D. S.; DeCesar, M. E.; Ferrara, E. C.; Gehrels, N.; Harding, A. K.; Hays, E.; Johnson, T. E.; McConville, W.; McEnery, J. E.; Moiseev, A. A.; Perkins, J. S.; Racusin, J. L.; Shrader, C.; Stephens, T. E.; Thompson, D. J.; Troja, E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Bonnell, J.; DeCesar, M. E.; McConville, W.; McEnery, J. E.; Moiseev, A. A.] Univ Maryland, Dept Phys, College Pk, MD 20742 USA. [Bonnell, J.; DeCesar, M. E.; McConville, W.; McEnery, J. E.; Moiseev, A. A.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Brandt, T. J.; Knoedlseder, J.] IRAP, CNRS, F-31028 Toulouse 4, France. [Brandt, T. J.; Knoedlseder, J.] Univ Toulouse, UPS OMP, IRAP, GAHEC, Toulouse, France. [Brigida, M.; de Palma, F.; Favuzzi, C.; Fusco, P.; Giglietto, N.; Giordano, F.; Loparco, F.; Monte, C.; Raino, S.; Spinelli, P.] Univ Politecn Bari, Dipartimento Fis M Merlin, I-70126 Bari, Italy. [Brigida, M.; de Palma, F.; Favuzzi, C.; Fusco, P.; Gargano, F.; Giglietto, N.; Giordano, F.; Loparco, F.; Mazziotta, M. N.; Mongelli, M.; Monte, C.; Raino, S.; Spinelli, P.] Ist Nazl Fis Nucl, Sez Bari, I-70126 Bari, Italy. [Bruel, P.; Fegan, S. J.; Fortin, P.; Giebels, B.; Horan, D.] Ecole Polytech, CNRS, IN2P3, Lab Leprince Ringuet, F-91128 Palaiseau, France. [Burnett, T. H.; Roth, M.; Wallace, E.] Univ Washington, Dept Phys, Seattle, WA 98195 USA. [Caliandro, G. A.; Hadasch, D.; Torres, D. F.] CSIC, IEEE, Inst Ciencies Espai, Barcelona 08193, Spain. [Campana, R.; D'Ammando, F.] INAF Ist Astrofis Spaziale & Fis Cosm, I-00133 Rome, Italy. [Canadas, B.; Lionetto, A. M.; Morselli, A.; Vitale, V.] Ist Nazl Fis Nucl, Sez Roma, I-00133 Rome, Italy. [Canadas, B.; Lionetto, A. M.; Vitale, V.] Univ Roma Tor Vergata, Dipartimento Fis, I-00133 Rome, Italy. [Cannon, A.] Natl Univ Ireland Univ Coll Dublin, Expt Phys Dept, Dublin 4, Ireland. [Cavazzuti, E.; Cutini, S.; Gasparrini, D.; Giommi, P.] Agenzia Spaziale Italiana ASI Sci Data Ctr, I-00044 Rome, Italy. [Moiseev, A. A.; Perkins, J. S.; Shrader, C.] CRESST, Greenbelt, MD 20771 USA. [Celik, Oe; Corbet, R.; Davis, D. S.; Perkins, J. S.] Univ Maryland Baltimore Cty, Dept Phys, Baltimore, MD 21250 USA. [Celik, Oe; Corbet, R.; Davis, D. S.; Perkins, J. S.] Univ Maryland Baltimore Cty, Ctr Space Sci & Technol, Baltimore, MD 21250 USA. [Chekhtman, A.] Artep Inc, Ellicott City, MD 21042 USA. [Cheung, C. C.; Johnson, T. J.] Natl Acad Sci, Washington, DC 20001 USA. [Chipaux, R.] CEA Saclay, IRFU SEDI, F-91191 Gif Sur Yvette, France. [Ciprini, S.] ASI Sci Data Ctr, I-00044 Rome, Italy. [Cohen-Tanugi, J.; Falletti, L.; Mehault, J.; Nuss, E.; Piron, F.; Vasileiou, V.] Univ Montpellier 2, CNRS, IN2P3, Lab Univ & Particules Montpellier, Montpellier, France. [Cominsky, L. R.] Sonoma State Univ, Dept Phys & Astron, Rohnert Pk, CA 94928 USA. [Conrad, J.; Garde, M. Llena; Yang, Z.; Zimmer, S.] Stockholm Univ, Dept Phys, SE-10691 Stockholm, Sweden. [D'Ammando, F.] IASF Palermo, I-90146 Palermo, Italy. [de Angelis, A.; Frailis, M.] Univ Udine, Dipartimento Fis, I-33100 Udine, Italy. [de Angelis, A.; Frailis, M.] Ist Nazl Fis Nucl, Sez Trieste, Grp Coll Udine, I-33100 Udine, Italy. [DeKlotz, M.] Stellar Solut Inc, Palo Alto, CA 94306 USA. [Dermer, C. D.; Grove, J. E.; Lovellette, M. N.; Strickman, M. S.; Wood, K. S.] USN, Res Lab, Div Space Sci, Washington, DC 20375 USA. [Dumora, D.; Escande, L.; Hou, X.; Lemoine-Goumard, M.; Lott, B.; Reposeur, T.; Rousseau, R.; Smith, D. A.] Univ Bordeaux 1, CNRS, IN2P3, Ctr Etud Nucl Bordeaux Gradignan, F-33175 Gradignan, France. [Frailis, M.; Iafrate, G.] Ist Nazl Astrofis, Osservatorio Astron Trieste, I-34143 Trieste, Italy. [Fukazawa, Y.; Hanabata, Y.; Itoh, R.; Mizuno, T.] Hiroshima Univ, Dept Phys Sci, Hiroshima 7398526, Japan. [Giroletti, M.] INAF Ist Radioastron, I-40129 Bologna, Italy. [Grondin, M. -H.; Sanchez, D. A.] Max Planck Inst Kernphys, D-69029 Heidelberg, Germany. [Grondin, M. -H.] Heidelberg Univ, Landessternwarte, D-69117 Heidelberg, Germany. [Guillemot, L.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Guiriec, S.] Univ Alabama, Ctr Space Plasma & Aeron Res, Huntsville, AL 35899 USA. [Hayashida, M.] Kyoto Univ, Grad Sch Sci, Dept Astron, Sakyo Ku, Kyoto 6068502, Japan. [Hill, A. B.] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England. [Hughes, R. E.; Winer, B. L.] Ohio State Univ, Ctr Cosmol & Astroparticle Phys, Dept Phys, Columbus, OH 43210 USA. [Johannesson, G.] Univ Iceland, Inst Sci, IS-107 Reykjavik, Iceland. [Katagiri, H.] Ibaraki Univ, Coll Sci, Bunkyo Ku, Mito, Ibaraki 3108512, Japan. [Kataoka, J.; Nakamori, T.] Waseda Univ, Res Inst Sci & Engn, Shinjuku Ku, Tokyo 1698555, Japan. [Kawai, N.] Tokyo Inst Technol, Dept Phys, Meguro, Tokyo 1528551, Japan. [Kawai, N.] RIKEN, Inst Phys & Chem Res, Cosm Radiat Lab, Wako, Saitama 3510198, Japan. [Latronico, L.] Ist Nazl Fis Nucl, Sez Torino, I-10125 Turin, Italy. [Massaro, E.; Tinebra, F.] Univ Roma La Sapienza, Dept Phys, I-00185 Rome, Italy. [Norris, J. P.] Boise State Univ, Dept Phys, Boise, ID 83725 USA. [Ohno, M.; Okumura, A.; Ozaki, M.; Takahashi, T.] JAXA, Inst Space & Astronaut Sci, Chuo Ku, Sagamihara, Kanagawa 2525210, Japan. [Ohsugi, T.; Takahashi, H.] Hiroshima Univ, Hiroshima Astrophys Sci Ctr, Hiroshima 7398526, Japan. [Orlando, E.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Ormes, J. F.] Univ Denver, Dept Phys & Astron, Denver, CO 80208 USA. [Paneque, D.] Max Planck Inst Phys & Astrophys, D-80805 Munich, Germany. [Perkins, J. S.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Reimer, A.; Reimer, O.; Werner, M.] Leopold Franzens Univ Innsbruck, Inst Astro & Teilchenphys, A-6020 Innsbruck, Austria. [Reimer, A.; Reimer, O.; Werner, M.] Leopold Franzens Univ Innsbruck, Inst Theoret Phys, A-6020 Innsbruck, Austria. [Scargle, J. D.] NASA, Ames Res Ctr, Div Space Sci, Moffett Field, CA 94035 USA. [Siskind, E. J.] NYCB Real Time Comp Inc, Lattingtown, NY 11560 USA. [Stephens, T. E.] Wyle Labs, El Segundo, CA 90245 USA. [Suson, D. J.] Purdue Univ Calumet, Dept Chem & Phys, Hammond, IN 46323 USA. [Tajima, H.] Nagoya Univ, Solar Terr Environm Lab, Nagoya, Aichi 4648601, Japan. [Tibolla, O.] Univ Wurzburg, Inst Theoret Phys & Astrophys, D-97074 Wurzburg, Germany. [Torres, D. F.] ICREA, Barcelona, Spain. [Vianello, G.] CIFS, I-10133 Turin, Italy. [Wood, D. L.] Praxis Inc, Alexandria, VA 22303 USA. EM jean.ballet@cea.fr; tburnett@u.washington.edu; digel@stanford.edu; Gino.Tosti@pg.infn.it RI Campana, Riccardo/F-5272-2015; Johannesson, Gudlaugur/O-8741-2015; Loparco, Francesco/O-8847-2015; Gargano, Fabio/O-8934-2015; Moskalenko, Igor/A-1301-2007; Mazziotta, Mario /O-8867-2015; Sgro, Carmelo/K-3395-2016; Torres, Diego/O-9422-2016; Orlando, E/R-5594-2016; Funk, Stefan/B-7629-2015; Chipaux, Remi/G-1145-2010; Baldini, Luca/E-5396-2012; lubrano, pasquale/F-7269-2012; Morselli, Aldo/G-6769-2011; Kuss, Michael/H-8959-2012; giglietto, nicola/I-8951-2012; Racusin, Judith/D-2935-2012; Reimer, Olaf/A-3117-2013; Tosti, Gino/E-9976-2013; Saz Parkinson, Pablo Miguel/I-7980-2013; Ozaki, Masanobu/K-1165-2013; Rando, Riccardo/M-7179-2013; Fabiani, Davide/J-5750-2012 OI Berenji, Bijan/0000-0002-4551-772X; Gasparrini, Dario/0000-0002-5064-9495; Baldini, Luca/0000-0002-9785-7726; Marelli, Martino/0000-0002-8017-0338; Caraveo, Patrizia/0000-0003-2478-8018; Stephens, Thomas/0000-0003-3065-6871; Sgro', Carmelo/0000-0001-5676-6214; Rando, Riccardo/0000-0001-6992-818X; Hill, Adam/0000-0003-3470-4834; Bastieri, Denis/0000-0002-6954-8862; Omodei, Nicola/0000-0002-5448-7577; Pesce-Rollins, Melissa/0000-0003-1790-8018; Axelsson, Magnus/0000-0003-4378-8785; De Luca, Andrea/0000-0001-6739-687X; Giroletti, Marcello/0000-0002-8657-8852; Campana, Riccardo/0000-0002-4794-5453; Johannesson, Gudlaugur/0000-0003-1458-7036; Loparco, Francesco/0000-0002-1173-5673; Gargano, Fabio/0000-0002-5055-6395; Moskalenko, Igor/0000-0001-6141-458X; Mazziotta, Mario /0000-0001-9325-4672; Torres, Diego/0000-0002-1522-9065; Bignami, Giovanni/0000-0001-9582-2450; giommi, paolo/0000-0002-2265-5003; De Angelis, Alessandro/0000-0002-3288-2517; Iafrate, Giulia/0000-0002-6185-8292; Frailis, Marco/0000-0002-7400-2135; Funk, Stefan/0000-0002-2012-0080; lubrano, pasquale/0000-0003-0221-4806; Morselli, Aldo/0000-0002-7704-9553; giglietto, nicola/0000-0002-9021-2888; Reimer, Olaf/0000-0001-6953-1385; FU K. A. Wallenberg Foundation; European Community [ERC-StG-259391]; National Aeronautics and Space Administration; Department of Energy in the United States; Commissariata l'Energie Atomique; Centre National de la Recherche Scientifique/Institut National de Physique Nucleaire et de Physique des Particules in France; Agenzia Spaziale Italiana; Istituto Nazionale di Fisica Nucleare in Italy; Ministry of Education, Culture, Sports, Science and Technology (MEXT); High Energy Accelerator Research Organization (KEK); Japan Aerospace Exploration Agency (JAXA) in Japan; Swedish Research Council; Swedish National Space Board in Sweden.; Istituto Nazionale di Astrofisica in Italy; Centre National d'Etudes Spatiales in France; National Aeronautics and Space Administratio FX Royal Swedish Academy of Sciences Research Fellow, funded by a grant from the K. A. Wallenberg Foundation.; Funded by contract ERC-StG-259391 from the European Community.; The Fermi-LAT Collaboration acknowledges generous ongoing support from a number of agencies and institutes that have supported both the development and the operation of the LAT as well as scientific data analysis. These include the National Aeronautics and Space Administration and the Department of Energy in the United States, the Commissariata l'Energie Atomique and the Centre National de la Recherche Scientifique/Institut National de Physique Nucleaire et de Physique des Particules in France, the Agenzia Spaziale Italiana and the Istituto Nazionale di Fisica Nucleare in Italy, the Ministry of Education, Culture, Sports, Science and Technology (MEXT), High Energy Accelerator Research Organization (KEK) and Japan Aerospace Exploration Agency (JAXA) in Japan, and the K. A. Wallenberg Foundation, the Swedish Research Council and the Swedish National Space Board in Sweden.; Additional support for science analysis during the operations phase is gratefully acknowledged from the Istituto Nazionale di Astrofisica in Italy and the Centre National d'Etudes Spatiales in France.; This work made extensive use of the ATNF pulsar catalog101 (Manchester et al. 2005). This research has made use of the NASA/IPAC Extragalactic Database (NED) which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. NR 118 TC 717 Z9 721 U1 14 U2 56 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 APR PY 2012 VL 199 IS 2 AR 31 DI 10.1088/0067-0049/199/2/31 PG 46 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 929ZT UT WOS:000303105400007 ER PT J AU Thompson, JR Wiek, A Swanson, FJ Carpenter, SR Fresco, N Hollingsworth, T Spies, TA Foster, DR AF Thompson, Jonathan R. Wiek, Arnim Swanson, Frederick J. Carpenter, Stephen R. Fresco, Nancy Hollingsworth, Teresa Spies, Thomas A. Foster, David R. TI Scenario Studies as a Synthetic and Integrative Research Activity for Long-Term Ecological Research SO BIOSCIENCE LA English DT Article DE socioecological systems; science synthesis; participatory engagement; futures ID LAND-USE; SCIENCE; OREGON AB Scenario studies have emerged as a powerful approach for synthesizing diverse forms of research and for articulating and evaluating alternative socioecological futures. Unlike predictive modeling, scenarios do not attempt to forecast the precise or probable state of any variable at a given point in the future. Instead, comparisons among a set of contrasting scenarios are used to understand the systemic relationships and dynamics of complex socioecological systems and to define a range of possibilities and uncertainties in quantitative and qualitative terms. We describe five examples of scenario studies affiliated with the US Long Term Ecological Research (LTER) Network and evaluate them in terms of their ability to advance the LTER Network's capacity for conducting science, promoting social and ecological science synthesis, and increasing the saliency of research through sustained outreach activities. We conclude with an argument that scenario studies should be advanced programmatically within large socioecological research programs to encourage prescient thinking in an era of unprecedented global change. C1 [Thompson, Jonathan R.] Smithsonian Inst, Conservat Biol Inst, Front Royal, VA USA. [Wiek, Arnim] Arizona State Univ, Sch Sustainabil, Tempe, AZ USA. [Swanson, Frederick J.; Spies, Thomas A.] US Forest Serv, Pacific NW Res Stn, Corvallis, OR 97331 USA. [Carpenter, Stephen R.] Univ Wisconsin, Ctr Limnol, Madison, WI 53706 USA. [Fresco, Nancy] Univ Alaska, Sch Nat Resources & Agr Sci, Fairbanks, AK 99701 USA. [Hollingsworth, Teresa] Univ Alaska, Boreal Ecol Cooperat Res Unit, Fairbanks, AK 99701 USA. [Hollingsworth, Teresa] US Forest Serv, Pacific NW Res Stn, Fairbanks, AK USA. [Foster, David R.] Harvard Univ Harvard Forest, Petersham, MA USA. RP Thompson, JR (reprint author), Smithsonian Inst, Conservat Biol Inst, Front Royal, VA USA. EM thompsonjr@si.edu FU US National Science Foundation Long Term Ecological Research Network; US Forest Service FX Support for this work was provided by US National Science Foundation Long Term Ecological Research Network awards to Harvard University, Arizona State University, Oregon State University, the University of Alaska, and the University of Wisconsin and by the US Forest Service. NR 46 TC 26 Z9 26 U1 3 U2 46 PU AMER INST BIOLOGICAL SCI PI WASHINGTON PA 1444 EYE ST, NW, STE 200, WASHINGTON, DC 20005 USA SN 0006-3568 J9 BIOSCIENCE JI Bioscience PD APR PY 2012 VL 62 IS 4 BP 367 EP 376 DI 10.1525/bio.2012.62.4.8 PG 10 WC Biology SC Life Sciences & Biomedicine - Other Topics GA 927RK UT WOS:000302927600008 ER PT J AU Breedy, O Abeytia, R Guzman, HM AF Breedy, Odalisca Abeytia, Rosalinda Guzman, Hector M. TI A NEW SPECIES OF LEPTOGORGIA (CNIDARIA: ANTHOZOA: OCTOCORALLIA) FROM THE MEXICAN PACIFIC COAST SO BULLETIN OF MARINE SCIENCE LA English DT Article ID GORGONIIDAE AB The gorgoniid genus Leptogorgia is found along the Pacific coast of Mexico; 10 species have been reported from Baja California and Acapulco. Leptogorgia ena sp. nov. is a new shallow-water species found at 5-12 m depth at various high energy rocky sites along the coast of San Pedro Pochutla District, Oaxaca. Specimens of the new species were collected by scuba diving and the morphological characters were analyzed and illustrated under light and scanning electron microscopy. The new species can be distinguished from the others by the very small colony, dominance of wide capstans, barrels and double heads, low occurrence of spindles, spindles measuring < 0.10 mm, and presence of tentacular sclerites. With this report, the genus Leptogorgia increases to 11 species for Mexico and 26 for the eastern Pacific. C1 [Breedy, Odalisca] Univ Costa Rica, Ctr Invest Estructuras Microscop, Ctr Invest Ciencias Mar & Limnol, San Jose, Costa Rica. [Abeytia, Rosalinda] Univ Mar, Puerto Angel, Oaxaca, Mexico. [Breedy, Odalisca; Guzman, Hector M.] Smithsonian Trop Res Inst, Panama City, Panama. RP Breedy, O (reprint author), Univ Costa Rica, Ctr Invest Estructuras Microscop, Ctr Invest Ciencias Mar & Limnol, POB 11501-2060, San Jose, Costa Rica. EM odalisca.breedy@ucr.ac.cr FU Universidad del Mar (Puerto Angel); Vicerrectoria de Investigacion, Universidad de Costa Rica; Smithsonian Tropical Research Institute FX We are grateful to S Cairns (National Museum of Natural History, Washington DC), and the anonymous reviewers for their critical review of the manuscript. We thank Imelda Maldonado from Mexico for help in the field and laboratory. We thank Universidad del Mar (Puerto Angel), the Vicerrectoria de Investigacion, Universidad de Costa Rica, and the Smithsonian Tropical Research Institute for funding this project. NR 11 TC 1 Z9 1 U1 3 U2 9 PU ROSENSTIEL SCH MAR ATMOS SCI PI MIAMI PA 4600 RICKENBACKER CAUSEWAY, MIAMI, FL 33149 USA SN 0007-4977 EI 1553-6955 J9 B MAR SCI JI Bull. Mar. Sci. PD APR PY 2012 VL 88 IS 2 BP 319 EP 325 DI 10.5343/bms.2011.1103 PG 7 WC Marine & Freshwater Biology; Oceanography SC Marine & Freshwater Biology; Oceanography GA 932JJ UT WOS:000303287100010 ER PT J AU Bricelj, VM Haubois, AG Sengco, MR Pierce, RH Culter, JK Anderson, DM AF Bricelj, V. M. Haubois, A-G. Sengco, M. R. Pierce, R. H. Culter, J. K. Anderson, D. M. TI Trophic transfer of brevetoxins to the benthic macrofaunal community during a bloom of the harmful dinoflagellate Karenia brevis in Sarasota Bay, Florida SO HARMFUL ALGAE LA English DT Article DE Karenia brevis; Brevetoxins; Benthic trophic transfer ID OYSTER CRASSOSTREA-VIRGINICA; DOMOIC ACID; RED-TIDE; GYMNODINIUM-BREVE; POTENTIAL VECTOR; AUSTROVENUS-STUTCHBURYI; CONTROLLED EXPOSURES; PERNA-CANALICULUS; GREENSHELL MUSSEL; ALGAL BLOOMS AB Harmful algal blooms can cause mass mortalities of top predators such as fish, marine mammals and seabirds but the food web transfer from toxic phytoplankton to these organisms has not been fully elucidated. Macrobenthic invertebrates in coastal waters, including bivalve suspension- and deposit-feeders, carnivorous gastropods, deposit-feeding amphipods and polychaetes, are a major food source for a wide variety of predators and can thus play a critical role in the trophic transfer of algal toxins to higher trophic levels. The objective of this study was to investigate toxin accumulation in transplanted juvenile hard clams, Mercenaria mercenaria, a species naturally occurring in the region, and in various macrobenthic functional groups from Florida coastal waters during a natural bloom of the dinoflagellate, Karenia brevis, a producer of brevetoxins. Bloom concentrations in the water column ranged from 100 to 1200 cells ml(-1) over the course of the experiment. This study revealed that these lipophilic toxins can be rapidly accumulated by both suspension- and deposit-feeding benthos, especially bivalve molluscs [1.9-2.8 mu g PbTx-3 eq (g wet weight)(-1)]. Transplanted M. mercenaria rapidly accumulated toxins from the water column attaining similar to 0.5 mu g PbTx-3 eq (g wet tissue)(-1) after only 4 h-exposure to the K. brevis bloom and a maximum value of 1.5 +/- 0.2 mu g PbTx-3 eq (g wet tissue)(-1) after 72 h. Relatively high brevetoxin concentrations were also measured in co-occurring benthic carnivorous gastropods [1-2.6 mu g PbTx-3 eq (g wet weight, WW)-1]. Mean toxin concentrations in polychaetes and crustaceans varied in the range similar to 0.04-0.2 mu g PbTx-3 eq (g WW)(-1) over the study period, and thus were typically lower than in molluscs. This study demonstrated in situ toxin accumulation by benthic primary and secondary consumers during a natural Florida red tide. Accumulation by primary consumers may be highly variable in space and time (as shown in bivalves from the natural benthic community) and among taxonomic groups. Toxin transfer further up the food web will thus depend on the toxin level accumulated in prey, the number of pathways from which the predator may accumulate toxins and on possible biological magnification of lipophilic toxins. Overall, this study revealed qualitatively and quantitatively that benthic consumers of a number of taxa can serve as vectors for transporting brevetoxins within the food web. (C) 2012 Elsevier B.V. All rights reserved. C1 [Bricelj, V. M.] Rutgers State Univ, Inst Marine & Coastal Sci, New Brunswick, NJ 08901 USA. [Haubois, A-G.] Natl Res Council Canada, Inst Marine Biosci, Halifax, NS B3H 3Z1, Canada. [Sengco, M. R.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. [Pierce, R. H.; Culter, J. K.] Mote Marine Lab, Sarasota, FL 34236 USA. [Anderson, D. M.] Woods Hole Oceanog Inst, Dept Biol, Woods Hole, MA 02543 USA. RP Bricelj, VM (reprint author), Rutgers State Univ, Inst Marine & Coastal Sci, 71 Dudley Rd, New Brunswick, NJ 08901 USA. EM mbricelj@marine.rutgers.edu FU NOAA-ECOHAB [NA16OP2793]; NOAA [NA06NOS4780245] FX Funding for this work was provided by NOAA-ECOHAB Grant No. NA16OP2793 awarded to D. Anderson at WHOI, USA. Additional support was provided to D. Anderson and M. Bricelj by NOAA grant NA06NOS4780245. This manuscript is ECOHAB publication #674. We are very grateful to Michael Henry and Bruce Keafer for their assistance and contribution to the field survey.[SS] NR 62 TC 8 Z9 8 U1 1 U2 41 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 1568-9883 EI 1878-1470 J9 HARMFUL ALGAE JI Harmful Algae PD APR PY 2012 VL 16 BP 27 EP 34 DI 10.1016/j.hal.2012.01.001 PG 8 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA 932NU UT WOS:000303298600004 ER PT J AU Boyle, MJ Rice, ME AF Boyle, M. J. Rice, M. E. TI Life History Evolution: Insights from Comparative Development and Gene Expression in Sipuncula SO INTEGRATIVE AND COMPARATIVE BIOLOGY LA English DT Meeting Abstract CT Annual Meeting of the Society-for-Integrative-and-Comparative-Biology (SICB) CY JAN 03-07, 2012 CL Charleston, SC SP Soc Integrat & Comparat Biol (SICB) C1 [Boyle, M. J.; Rice, M. E.] Smithsonian Marine Stn, Ft Pierce, FL USA. EM boylem@si.edu NR 0 TC 0 Z9 0 U1 0 U2 6 PU OXFORD UNIV PRESS INC PI CARY PA JOURNALS DEPT, 2001 EVANS RD, CARY, NC 27513 USA SN 1540-7063 J9 INTEGR COMP BIOL JI Integr. Comp. Biol. PD APR PY 2012 VL 52 SU 1 BP E18 EP E18 PG 1 WC Zoology SC Zoology GA 930TV UT WOS:000303165000073 ER PT J AU Carmack, CA Redmond, N Thacker, RW Colin, L Colin, P Hill, M Hill, A Lopez, J Diaz, MC Pomponi, S Bangalore, P AF Carmack, C. A. Redmond, N. Thacker, R. W. Colin, L. Colin, P. Hill, M. Hill, A. Lopez, J. Diaz, M. C. Pomponi, S. Bangalore, P. TI Nuclear 28S ribosomal subunit gene sequences support new relationships among families and orders of Porifera SO INTEGRATIVE AND COMPARATIVE BIOLOGY LA English DT Meeting Abstract CT Annual Meeting of the Society-for-Integrative-and-Comparative-Biology (SICB) CY JAN 03-07, 2012 CL Charleston, SC SP Soc Integrat & Comparat Biol (SICB) C1 Univ Alabama Birmingham, Smithsonian Inst, Coral Reef Res Fdn, Birmingham, AL USA. Univ Richmond, Richmond, VA 23173 USA. Nova SE Univ, Museo Margarita, Harbor Branch Oceanog Inst, Ft Lauderdale, FL 33314 USA. EM thacker@uab.edu NR 0 TC 0 Z9 0 U1 1 U2 5 PU OXFORD UNIV PRESS INC PI CARY PA JOURNALS DEPT, 2001 EVANS RD, CARY, NC 27513 USA SN 1540-7063 J9 INTEGR COMP BIOL JI Integr. Comp. Biol. PD APR PY 2012 VL 52 SU 1 BP E221 EP E221 PG 1 WC Zoology SC Zoology GA 930TV UT WOS:000303165001349 ER PT J AU Collin, R AF Collin, R. TI What Can "Intermediates" Tell Us About Evolutionary Transitions Between Modes of Invertebrate Development? SO INTEGRATIVE AND COMPARATIVE BIOLOGY LA English DT Meeting Abstract CT Annual Meeting of the Society-for-Integrative-and-Comparative-Biology (SICB) CY JAN 03-07, 2012 CL Charleston, SC SP Soc Integrat & Comparat Biol (SICB) C1 [Collin, R.] Smithsonian Trop Res Inst, Balboa, Panama. EM collinr@si.edu NR 0 TC 0 Z9 0 U1 0 U2 0 PU OXFORD UNIV PRESS INC PI CARY PA JOURNALS DEPT, 2001 EVANS RD, CARY, NC 27513 USA SN 1540-7063 J9 INTEGR COMP BIOL JI Integr. Comp. Biol. PD APR PY 2012 VL 52 SU 1 BP E33 EP E33 PG 1 WC Zoology SC Zoology GA 930TV UT WOS:000303165000130 ER PT J AU Craft, JD Ritson-Williams, R Langdon, C Paul, V AF Craft, Jonathan D. Ritson-Williams, R. Langdon, C. Paul, V TI Impacts of ocean acidification on growth, calcification, and terpene concentrations in the green alga Halimeda opuntia SO INTEGRATIVE AND COMPARATIVE BIOLOGY LA English DT Meeting Abstract CT Annual Meeting of the Society-for-Integrative-and-Comparative-Biology (SICB) CY JAN 03-07, 2012 CL Charleston, SC SP Soc Integrat & Comparat Biol (SICB) C1 [Craft, Jonathan D.; Ritson-Williams, R.; Langdon, C.; Paul, V] Smithsonian Marine Stn, Ft Pierce, FL USA. EM craftjd@gmail.com NR 0 TC 0 Z9 0 U1 0 U2 8 PU OXFORD UNIV PRESS INC PI CARY PA JOURNALS DEPT, 2001 EVANS RD, CARY, NC 27513 USA SN 1540-7063 J9 INTEGR COMP BIOL JI Integr. Comp. Biol. PD APR PY 2012 VL 52 SU 1 BP E232 EP E232 PG 1 WC Zoology SC Zoology GA 930TV UT WOS:000303165001392 ER PT J AU Devries, MS Christy, JH AF Devries, M. S. Christy, J. H. TI Why stomatopods are striking SO INTEGRATIVE AND COMPARATIVE BIOLOGY LA English DT Meeting Abstract CT Annual Meeting of the Society-for-Integrative-and-Comparative-Biology (SICB) CY JAN 03-07, 2012 CL Charleston, SC SP Soc Integrat & Comparat Biol (SICB) C1 Univ Calif Berkeley, Berkeley, CA 94720 USA. Smithsonian Trop Res Inst, Balboa, Panama. EM msdevries@berkeley.edu NR 0 TC 0 Z9 0 U1 1 U2 3 PU OXFORD UNIV PRESS INC PI CARY PA JOURNALS DEPT, 2001 EVANS RD, CARY, NC 27513 USA SN 1540-7063 J9 INTEGR COMP BIOL JI Integr. Comp. Biol. PD APR PY 2012 VL 52 SU 1 BP E45 EP E45 PG 1 WC Zoology SC Zoology GA 930TV UT WOS:000303165000178 ER PT J AU Hofstee, JC Collin, R AF Hofstee, J. C. Collin, R. TI Modification of velar lobe morphology across different developmental modes in Calpytraeid gastropods SO INTEGRATIVE AND COMPARATIVE BIOLOGY LA English DT Meeting Abstract CT Annual Meeting of the Society-for-Integrative-and-Comparative-Biology (SICB) CY JAN 03-07, 2012 CL Charleston, SC SP Soc Integrat & Comparat Biol (SICB) C1 [Hofstee, J. C.; Collin, R.] Smithsonian Trop Res Inst, Balboa, Panama. EM jeanettehofstee@gmail.com NR 0 TC 0 Z9 0 U1 0 U2 0 PU OXFORD UNIV PRESS INC PI CARY PA JOURNALS DEPT, 2001 EVANS RD, CARY, NC 27513 USA SN 1540-7063 J9 INTEGR COMP BIOL JI Integr. Comp. Biol. PD APR PY 2012 VL 52 SU 1 BP E264 EP E264 PG 1 WC Zoology SC Zoology GA 930TV UT WOS:000303165001521 ER PT J AU Hutchins, ED Stapley, J Eckalbar, WL Kulathinal, RJ Hsieh, ST Denardo, DF Fisher, RE Wilson-Rawls, J Rawls, A Huentelman, MJ Bermingham, E Kusumi, K AF Hutchins, E. D. Stapley, J. Eckalbar, W. L. Kulathinal, R. J. Hsieh, S. T. Denardo, D. F. Fisher, R. E. Wilson-Rawls, J. Rawls, A. Huentelman, M. J. Bermingham, E. Kusumi, K. TI Comparative analysis of genomic sequence and myogenic pathways regulating muscle mass in the green anole, Anolis carolinensis, and the Panamanian slender anole, A. apletophallus SO INTEGRATIVE AND COMPARATIVE BIOLOGY LA English DT Meeting Abstract CT Annual Meeting of the Society-for-Integrative-and-Comparative-Biology (SICB) CY JAN 03-07, 2012 CL Charleston, SC SP Soc Integrat & Comparat Biol (SICB) C1 Arizona State Univ, Smithsonian Trop Res Inst, Tempe, AZ 85287 USA. Temple Univ, Philadelphia, PA 19122 USA. Univ Arizona, Coll Med Phoenix, Tucson, AZ 85721 USA. Arizona State Univ, Translat Genom Res Inst, Tempe, AZ 85287 USA. EM kenro.kusumi@asu.edu RI Kusumi, Kenro/J-2626-2012 OI Kusumi, Kenro/0000-0002-1458-4540 NR 0 TC 0 Z9 0 U1 1 U2 4 PU OXFORD UNIV PRESS INC PI CARY PA JOURNALS DEPT, 2001 EVANS RD, CARY, NC 27513 USA SN 1540-7063 J9 INTEGR COMP BIOL JI Integr. Comp. Biol. PD APR PY 2012 VL 52 SU 1 BP E83 EP E83 PG 1 WC Zoology SC Zoology GA 930TV UT WOS:000303165000330 ER PT J AU Kaiser, SA Webster, MS Sillett, TS AF Kaiser, S. A. Webster, M. S. Sillett, T. S. TI Population-level Variation in Endogenous Testosterone, Mating and Paternal Effort Across an Elevation Gradient SO INTEGRATIVE AND COMPARATIVE BIOLOGY LA English DT Meeting Abstract CT Annual Meeting of the Society-for-Integrative-and-Comparative-Biology (SICB) CY JAN 03-07, 2012 CL Charleston, SC SP Soc Integrat & Comparat Biol (SICB) C1 Cornell Univ, Ithaca, NY USA. Smithsonian Migratory Bird Ctr, Washington, DC USA. EM sak275@cornell.edu NR 0 TC 0 Z9 0 U1 1 U2 5 PU OXFORD UNIV PRESS INC PI CARY PA JOURNALS DEPT, 2001 EVANS RD, CARY, NC 27513 USA SN 1540-7063 J9 INTEGR COMP BIOL JI Integr. Comp. Biol. PD APR PY 2012 VL 52 SU 1 BP E89 EP E89 PG 1 WC Zoology SC Zoology GA 930TV UT WOS:000303165000354 ER PT J AU Mcclintock, JB Amsler, MO Angus, RA Challener, RC Schram, JB Amsler, CD Mah, CJ Cuce, JBBJ AF Mcclintock, J. B. Amsler, M. O. Angus, R. A. Challener, R. C. Schram, J. B. Amsler, C. D. Mah, C. J. Cuce, J. Baker B. J. TI The Mg-Calcite levels of Antarctic echinoderms: implications for ocean acidification and further support for a latitudinal gradient in levels of Mg-Calcite SO INTEGRATIVE AND COMPARATIVE BIOLOGY LA English DT Meeting Abstract CT Annual Meeting of the Society-for-Integrative-and-Comparative-Biology (SICB) CY JAN 03-07, 2012 CL Charleston, SC SP Soc Integrat & Comparat Biol (SICB) C1 Univ Alabama Birmingham, Birmingham, AL USA. Museum Nat Hist, New York, NY USA. Smithsonian Inst, Washington, DC 20560 USA. Univ S Florida, Tampa, FL 33620 USA. EM mcclinto@uab.edu NR 0 TC 0 Z9 0 U1 0 U2 2 PU OXFORD UNIV PRESS INC PI CARY PA JOURNALS DEPT, 2001 EVANS RD, CARY, NC 27513 USA SN 1540-7063 J9 INTEGR COMP BIOL JI Integr. Comp. Biol. PD APR PY 2012 VL 52 SU 1 BP E292 EP E292 PG 1 WC Zoology SC Zoology GA 930TV UT WOS:000303165002075 ER PT J AU Mcdonald, KA AF Mcdonald, K. A. TI Ontogenetic evidence and performance consequences of re-acquisition of planktotrophy in the gastropod family Calyptraeidae SO INTEGRATIVE AND COMPARATIVE BIOLOGY LA English DT Meeting Abstract CT Annual Meeting of the Society-for-Integrative-and-Comparative-Biology (SICB) CY JAN 03-07, 2012 CL Charleston, SC SP Soc Integrat & Comparat Biol (SICB) C1 [Mcdonald, K. A.] Smithsonian Trop Res Inst, Balboa, Panama. EM characterforming@gmail.com NR 0 TC 0 Z9 0 U1 0 U2 1 PU OXFORD UNIV PRESS INC PI CARY PA JOURNALS DEPT, 2001 EVANS RD, CARY, NC 27513 USA SN 1540-7063 J9 INTEGR COMP BIOL JI Integr. Comp. Biol. PD APR PY 2012 VL 52 SU 1 BP E118 EP E118 PG 1 WC Zoology SC Zoology GA 930TV UT WOS:000303165000470 ER PT J AU Pyenson, ND Goldbogen, JA Vogl, AW Szathmary, G Drake, R Shadwick, RE AF Pyenson, N. D. Goldbogen, J. A. Vogl, A. W. Szathmary, G. Drake, R. Shadwick, R. E. TI A putative sensory organ in the mandibular symphysis of rorqual whales (Balaenopteridae) SO INTEGRATIVE AND COMPARATIVE BIOLOGY LA English DT Meeting Abstract CT Annual Meeting of the Society-for-Integrative-and-Comparative-Biology (SICB) CY JAN 03-07, 2012 CL Charleston, SC SP Soc Integrat & Comparat Biol (SICB) C1 Smithsonian Inst, Washington, DC 20560 USA. Univ British Columbia, Vancouver, BC V5Z 1M9, Canada. Cleveland Clin, Cleveland, OH USA. EM pyensonn@si.edu NR 0 TC 0 Z9 0 U1 0 U2 0 PU OXFORD UNIV PRESS INC PI CARY PA JOURNALS DEPT, 2001 EVANS RD, CARY, NC 27513 USA SN 1540-7063 J9 INTEGR COMP BIOL JI Integr. Comp. Biol. PD APR PY 2012 VL 52 SU 1 BP E142 EP E142 PG 1 WC Zoology SC Zoology GA 930TV UT WOS:000303165001036 ER PT J AU Schulze, A Maiorova, A Timm, LE Rice, ME AF Schulze, A. Maiorova, A. Timm, L. E. Rice, M. E. TI Sipunculan Larvae and "Cosmopolitan" Species SO INTEGRATIVE AND COMPARATIVE BIOLOGY LA English DT Meeting Abstract CT Annual Meeting of the Society-for-Integrative-and-Comparative-Biology (SICB) CY JAN 03-07, 2012 CL Charleston, SC SP Soc Integrat & Comparat Biol (SICB) C1 [Schulze, A.; Maiorova, A.; Timm, L. E.; Rice, M. E.] Texas A&M Univ, Inst Marine Biol, Smithsonian Marine Stn Ft Pierce, Galveston, TX USA. EM schulzea@tamug.edu NR 0 TC 0 Z9 0 U1 0 U2 3 PU OXFORD UNIV PRESS INC PI CARY PA JOURNALS DEPT, 2001 EVANS RD, CARY, NC 27513 USA SN 1540-7063 J9 INTEGR COMP BIOL JI Integr. Comp. Biol. PD APR PY 2012 VL 52 SU 1 BP E155 EP E155 PG 1 WC Zoology SC Zoology GA 930TV UT WOS:000303165001086 ER PT J AU Seymoure, B Mcmillan, WO Mcgraw, K Rutowski, R AF Seymoure, Brett Mcmillan, W. Owen Mcgraw, Kevin Rutowski, Ron TI Heliconius mimicry rings in a new Light SO INTEGRATIVE AND COMPARATIVE BIOLOGY LA English DT Meeting Abstract CT Annual Meeting of the Society-for-Integrative-and-Comparative-Biology (SICB) CY JAN 03-07, 2012 CL Charleston, SC SP Soc Integrat & Comparat Biol (SICB) C1 [Seymoure, Brett; Mcmillan, W. Owen; Mcgraw, Kevin; Rutowski, Ron] Arizona State Univ, Smithsonian Trop Res Inst, Tempe, AZ 85287 USA. EM brett.seymoure@gmail.com NR 0 TC 0 Z9 0 U1 1 U2 5 PU OXFORD UNIV PRESS INC PI CARY PA JOURNALS DEPT, 2001 EVANS RD, CARY, NC 27513 USA SN 1540-7063 J9 INTEGR COMP BIOL JI Integr. Comp. Biol. PD APR PY 2012 VL 52 SU 1 BP E157 EP E157 PG 1 WC Zoology SC Zoology GA 930TV UT WOS:000303165001094 ER PT J AU Shishido, CM Collin, R Lesoway, MP AF Shishido, C. M. Collin, R. Lesoway, M. P. TI The Development of Particle Capture and Ingestion Abilities in Calyptraeid Gastropods with Different Modes of Development SO INTEGRATIVE AND COMPARATIVE BIOLOGY LA English DT Meeting Abstract CT Annual Meeting of the Society-for-Integrative-and-Comparative-Biology (SICB) CY JAN 03-07, 2012 CL Charleston, SC SP Soc Integrat & Comparat Biol (SICB) C1 Smithsonian Trop Res Inst, Balboa, Panama. McGill Univ, Montreal, PQ H3A 2T5, Canada. EM csmariko@uw.edu NR 0 TC 0 Z9 0 U1 0 U2 0 PU OXFORD UNIV PRESS INC PI CARY PA JOURNALS DEPT, 2001 EVANS RD, CARY, NC 27513 USA SN 1540-7063 J9 INTEGR COMP BIOL JI Integr. Comp. Biol. PD APR PY 2012 VL 52 SU 1 BP E327 EP E327 PG 1 WC Zoology SC Zoology GA 930TV UT WOS:000303165002214 ER PT J AU Strong, EE AF Strong, E. E. TI Large, common and variable: re-assessing the monophyly and diversity of Cerithiidae (Cerithioidea, Caenogastropoda) SO INTEGRATIVE AND COMPARATIVE BIOLOGY LA English DT Meeting Abstract CT Annual Meeting of the Society-for-Integrative-and-Comparative-Biology (SICB) CY JAN 03-07, 2012 CL Charleston, SC SP Soc Integrat & Comparat Biol (SICB) C1 [Strong, E. E.] Smithsonian Inst, Washington, DC 20560 USA. EM stronge@si.edu NR 0 TC 0 Z9 0 U1 0 U2 1 PU OXFORD UNIV PRESS INC PI CARY PA JOURNALS DEPT, 2001 EVANS RD, CARY, NC 27513 USA SN 1540-7063 J9 INTEGR COMP BIOL JI Integr. Comp. Biol. PD APR PY 2012 VL 52 SU 1 BP E169 EP E169 PG 1 WC Zoology SC Zoology GA 930TV UT WOS:000303165001141 ER PT J AU Young, CM He, R Emlet, RB Li, Y Qian, H Arellano, SM Van Gaest, AL Bennett, K Smart, TI Wolf, M Rice, ME AF Young, C. M. He, R. Emlet, R. B. Li, Y. Qian, H. Arellano, S. M. Van Gaest, A. L. Bennett, K. Smart, T., I Wolf, M. Rice, M. E. TI Larval life and dispersal potential of deep-sea animals from the Intra-American Seas SO INTEGRATIVE AND COMPARATIVE BIOLOGY LA English DT Meeting Abstract CT Annual Meeting of the Society-for-Integrative-and-Comparative-Biology (SICB) CY JAN 03-07, 2012 CL Charleston, SC SP Soc Integrat & Comparat Biol (SICB) C1 Univ Oregon, Eugene, OR 97403 USA. N Carolina State Univ, Raleigh, NC 27695 USA. Smithsonian Marine Stn, Ft Pierce, FL USA. EM cmyoung@uoregon.edu NR 0 TC 0 Z9 0 U1 0 U2 4 PU OXFORD UNIV PRESS INC PI CARY PA JOURNALS DEPT, 2001 EVANS RD, CARY, NC 27513 USA SN 1540-7063 J9 INTEGR COMP BIOL JI Integr. Comp. Biol. PD APR PY 2012 VL 52 SU 1 BP E198 EP E198 PG 1 WC Zoology SC Zoology GA 930TV UT WOS:000303165001260 ER PT J AU Williams, EM Gordon, AD Richmond, BG AF Williams, Erin Marie Gordon, Adam D. Richmond, Brian G. TI Hand pressure distribution during Oldowan stone tool production SO JOURNAL OF HUMAN EVOLUTION LA English DT Article DE Force; Knapping; Pressure; Thumb; Pollical musculature ID HUMAN-EVOLUTION; FUNCTIONAL-ANATOMY; FOSSIL EVIDENCE; MORPHOLOGY; ACCURACY; MUSCLE; KENYA; BIOMECHANICS; TECHNOLOGY; BEHAVIOR AB Modern humans possess a highly derived thumb that is robust and long relative to the other digits, with enhanced pollical musculature compared with extant apes. Researchers have hypothesized that this anatomy was initially selected for in early Homo in part to withstand high forces acting on the thumb during hard hammer percussion when producing stone tools. However, data are lacking on loads experienced during stone tool production and the distribution of these loads across the hand. Here we report the first quantitative data on manual normal forces (N) and pressures (kPa) acting on the hand during Oldowan stone tool production, captured at 200 Hz. Data were collected from six experienced subjects replicating Oldowan bifacial choppers. Our data do not support hypotheses asserting that the thumb experiences relatively high loads when making Oldowan stone tools. Peak normal force, pressure, impulse, and the pressure/time integral are significantly lower on the thumb than on digits 2 and/or digit 3 in every subject. Our findings call into question hypotheses linking modern human thumb robusticity specifically to load resistance during stone tool production. (C) 2012 Elsevier Ltd. All rights reserved. C1 [Williams, Erin Marie; Richmond, Brian G.] George Washington Univ, Dept Anthropol, Ctr Adv Study Hominid Paleobiol, Washington, DC 20052 USA. [Gordon, Adam D.] SUNY Albany, Dept Anthropol, Albany, NY 12222 USA. [Richmond, Brian G.] Smithsonian Inst, Natl Museum Nat Hist, Human Origins Program, Washington, DC 20560 USA. RP Williams, EM (reprint author), George Washington Univ, Dept Anthropol, Ctr Adv Study Hominid Paleobiol, 2110 G St NW, Washington, DC 20052 USA. EM emswill@gwmail.gwu.edu OI Gordon, Adam/0000-0002-1807-4644 FU Wenner-Gren Foundation [7995]; National Science Foundation [BCS-0903652]; Integrative Graduate Education and Research Traineeship (IGERT) [DGE 9987590, DGE 0801634]; George Washington University FX The authors are very grateful to the knappers that participated in this study. Maria Pasquale and Susan Diekrager provided training and significant assistance with the Pliance system, for which we are grateful. We wish to thank Alison Brooks, David Green, Kevin Hatala, Peter Lucas, Daniel Schmitt, Dietrich Stout, Erin Vogel, and the reviewers and editors for their thoughtful comments and suggestions, as well as Craig Ratzat at Neolithics.com for his careful selection of raw materials for this project. This research was supported by the Wenner-Gren Foundation's Dissertation Fieldwork Grant (#7995), the National Science Foundation's Doctoral Dissertation Improvement Grant (# BCS-0903652) and Integrative Graduate Education and Research Traineeship (IGERT # DGE 9987590 and # DGE 0801634), The George Washington University's Research Enhancement Fund, and The George Washington University's Selective Excellence Fund. NR 48 TC 24 Z9 24 U1 0 U2 21 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 APR PY 2012 VL 62 IS 4 BP 520 EP 532 DI 10.1016/j.jhevol.2012.02.005 PG 13 WC Anthropology; Evolutionary Biology SC Anthropology; Evolutionary Biology GA 930XB UT WOS:000303177000007 PM 22446065 ER PT J AU DiMichele, WA Falcon-Lang, HJ AF DiMichele, William A. Falcon-Lang, Howard J. TI Calamitalean "pith casts" reconsidered SO REVIEW OF PALAEOBOTANY AND PALYNOLOGY LA English DT Article DE Calamites; pith cast; fossil forest; plant taphonomy; fossilization; Late Paleozoic ID GENERAL QUANTITATIVE THEORY; SOUTHERN NEW-BRUNSWICK; NOVA-SCOTIA; CALAMITEAN SPHENOPSIDS; JOGGINS FORMATION; GIGAS BRONGNIART; FOREST STRUCTURE; FOSSIL FORESTS; VEGETATION; DYNAMICS AB Sediment-cast calamitalean axes in growth position are one of the most common fossils in the Pennsylvanian coal measures. In this paper, we challenge the long accepted position that these fossils represent "pith casts". If correct, the hypothesis would require the sediment-cast pith to have been surrounded by a cylinder of secondary xylem during life, which later decayed away. However, sedimentary layers and structures developed around upright calamitaleans indicate that fluid flow was interacting directly with the preserved surface of the stem, not a hypothetical woody cylinder that lay external to it. Furthermore, stem diameter-density data for calamitalean stands already lies at the self-thinning threshold, and if actual stem diameters were significantly greater than preserved diameters, this threshold would be significantly exceeded. We also note that measured diameters for upright sediment-cast calamitaleans are more similar to stem diameter data for anatomically preserved calamitalean axes than for pith diameter data from the same axes. Our findings indicate upright calamitaleans are in fact stem casts and their preservation involved a two-stage process. First, stems were buried in flood-deposited sediments, creating a mold of the external surface of the plant. Second, following near-total decay of the axis, which may have occurred in a matter of weeks under tropical conditions, further sedimentation infilled the mold, forming a cast. As such, the preservation of upright calamitaleans was identical to that for arborescent lycopsids, which are commonly found in the same beds. That said, we stress that some transported sediment-cast calamitalean axes preserved in fluvial channel facies are certainly "pith casts" in the traditional sense, however, their morphologies differ from those specimens traditionally called "pith casts". In this context, axes were buried in a single phase of sedimentation under energetic flow conditions, resulting in the pith becoming sediment-filled. However, intriguingly, a review of such genuine pith casts shows that only a tiny proportion preserves large woody cylinders surrounding the pith. This is not a taphonomic feature, but reflects our contention that the great majority of floodplain-based calamitaleans were reed-like plants with relatively small amounts of secondary xylem. Woody calamitaleans, including large tree forms, are documented almost exclusively from petrifactions, and thus from peat-forming environments (coal balls) and, more rarely, floodplain settings under exceptional conditions of preservation (volcanigenic deposits, for example). These may be difficult to recognize in adpression preservation due to the masking, by wood development, of node-internode features. The differing architectures may reflect adaptations to disturbed and undisturbed environments, respectively. (C) 2012 Elsevier B.V. All rights reserved. C1 [Falcon-Lang, Howard J.] Univ London, Dept Earth Sci, Egham TW20 0EX, Surrey, England. [DiMichele, William A.] NMNH Smithsonian Inst, Dept Paleobiol, Washington, DC 20560 USA. RP Falcon-Lang, HJ (reprint author), Univ London, Dept Earth Sci, Egham TW20 0EX, Surrey, England. EM dimichel@si.edu; h.falcon-lang@es.rhul.ac.uk RI DiMichele, William/K-4301-2012 NR 55 TC 12 Z9 12 U1 1 U2 10 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0034-6667 J9 REV PALAEOBOT PALYNO JI Rev. Palaeobot. Palynology PD APR 1 PY 2012 VL 173 BP 1 EP 14 DI 10.1016/j.revpalbo.2012.01.011 PG 14 WC Plant Sciences; Paleontology SC Plant Sciences; Paleontology GA 928LY UT WOS:000302985500001 ER PT J AU Hershler, R Liu, HP AF Hershler, Robert Liu, Hsiu-Ping TI A NEW SPECIES OF SPRINGSNAIL (PYRGULOPSIS) FROM THE OWYHEE RIVER BASIN, NEVADA SO WESTERN NORTH AMERICAN NATURALIST LA English DT Article ID AMERICAN NYMPHOPHILINE GASTROPODS; MITOCHONDRIAL-DNA SEQUENCES; HYDROBIIDAE; RISSOOIDEA; CALIFORNIA; SNAILS AB We describe a new springsnail species, Pyrgulopsis cybele, from the Owyhee River basin (northwestern Nevada) based on morphologic and molecular (mtCOI) evidence. Pyrgulopsis cybele differs from other members of its genus in its unique pattern of penial ornament, which consists of small glands on the distal edge of the penial lobe, base of the pedal filament, and outer edge of the medial section of the penis. It is further differentiated from regional congeners by its thickened inner-shell lip and mtCOI sequences. A Bayesian analysis based on COI data placed P. cybele in a well-supported elude that contained congeners from Snake River, Great Basin, Colorado River, and California Pacific Coastal drainages; the sister taxon of this new species was not resolved. The COI divergence of cybele relative to its most genetically similar congener (P. glandulosa) suggests that it evolved subsequent to emplacement of the Miocene basalt that carpets the upper South Fork Owyhee basin. Pyrgulopsis cybele was collected from 2 closely proximal springs along the South Fork Owyhee River below the Nevada Pipeline Crossing. Although these populations are in a remote wilderness study area, they may be threatened by livestock grazing and human disturbance. C1 [Hershler, Robert] Smithsonian Inst, Dept Invertebrate Zool, Washington, DC 20013 USA. [Liu, Hsiu-Ping] Metropolitan State Coll Denver, Dept Biol, Denver, CO 80217 USA. RP Hershler, R (reprint author), Smithsonian Inst, Dept Invertebrate Zool, Box 37012, Washington, DC 20013 USA. EM hershlerr@si.odu FU Center for Biological Diversity; Oregon Natural Desert Association (ONDA); Western Watersheds Project FX This project was supported (in part) by funds provided by the Center for Biological Diversity, Oregon Natural Desert Association (ONDA), and Western Watersheds Project. Brent Fenty (ONDA) was instrumental in helping to secure this funding. The Bureau of Land Management (Vale District) provided additional logistical support that was facilitated by Shaney Rockefeller. Chris Hansen, Dave Steele, and Dan Thomas provided a large amount of assistance in the field. We thank 2 anonymous reviewers and WNAN editor Chris Walser for their constructive comments on a draft of this manuscript. NR 31 TC 4 Z9 4 U1 0 U2 2 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 APR PY 2012 VL 72 IS 1 BP 21 EP 31 PG 11 WC Biodiversity Conservation; Ecology SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 930KU UT WOS:000303139100003 ER PT J AU Sessa, EB Zimmer, EA Givnish, TJ AF Sessa, Emily B. Zimmer, Elizabeth A. Givnish, Thomas J. TI PHYLOGENY, DIVERGENCE TIMES, AND HISTORICAL BIOGEOGRAPHY OF NEW WORLD DRYOPTERIS (DRYOPTERIDACEAE) SO AMERICAN JOURNAL OF BOTANY LA English DT Article DE divergence time estimates; diversification; Dryopteris; ferns; historical biogeography; long-distance dispersal; neotropics; vicariance; phylogeny; polyploidy; Pteridophyta ID FERN GENUS DRYOPTERIS; ATLANTIC LAND-BRIDGE; NORTHERN-HEMISPHERE; MOLECULAR PHYLOGENY; CHLOROPLAST DNA; MITOCHONDRIAL GENOMES; HOMOSPOROUS FERNS; SPINULOSA COMPLEX; GENETIC-VARIATION; FLOWERING PLANTS AB Premise of the study: Dryopteris is a large, cosmopolitan fern genus ideal for addressing questions about diversification, biogeography, hybridization, and polyploidy, which have historically been understudied in ferns. We constructed a highly resolved, well-supported phylogeny for New World Dryopteris and used it to investigate biogeographic patterns and divergence times. Methods: We analyzed relationships among 97 species of Dryopteris, including taxa from all major biogeographic regions, with analyses based on 5699 aligned nucleotides from seven plastid loci. Phylogenetic analyses used maximum parsimony, maximum likelihood, and Bayesian inference. We conducted divergence time analyses using BEAST and biogeographic analyses using maximum parsimony, maximum likelihood, Bayesian, and S-DIVA approaches. We explored the monophyly of subgenera and sections in the most recent generic classification and of geographic groups of taxa using Templeton tests. Key results: The genus Dryopteris arose ca. 42 million years ago (Ma). Most of the Central and South American species form a well-supported clade which arose 32 Ma, but the remaining New World species are the result of multiple, independent dispersal and vicariance events involving Asia, Europe, and Africa over the last 15 Myr. We identified six long-distance dispersal events and three vicariance events in the immediate ancestry of New World species; reconstructions for another four lineages were ambiguous. Conclusions: New World Dryopteris are not monophyletic; vicariance has dominated the history of the North American species, while long-distance dispersal prevails in the Central and South American species, a pattern not previously seen in plants. C1 [Sessa, Emily B.; Givnish, Thomas J.] Univ Wisconsin, Dept Bot, Madison, WI 53706 USA. [Zimmer, Elizabeth A.] Smithsonian Inst Museum Support Ctr, Dept Bot, Natl Museum Nat Hist, Suitland, MD 20746 USA. RP Sessa, EB (reprint author), Univ Wisconsin, Dept Bot, 430 Lincoln Dr, Madison, WI 53706 USA. EM esessa@wisc.edu FU National Science Foundation (DDIG) [DEB-1110335]; Huron Mountain Wildlife Foundation; Botanical Society of America; American Society of Plant Taxonomists; Torrey Botanical Society; Smithsonian Graduate Research Fellowship FX The authors thank E. Alverson, S. Bornell, B. Gilman, T. Goforth, T. Grabs, A. Jandl, C. Line, S. Lorbeer, B. and A. Manierre, T. Meyer, A. Reznicek, C. Taylor, B. Vesterby, S. Wechsler, D. Werier, F. R. Wesley, and K. Woods for help in the field; J. Geiger, S. Hennequin, C. Rothfels, and J. E. Watkins, Jr. for providing material; D. Giblin, M. McNamara, R. Moran, R. Olmstead, A. Smith, M. Sundue, and S. Vance for help with arranging herbarium visits; staff at herbaria BH, NY, MO, UC, US, WTU for letting us view specimens; and the Finger Lakes Land Trust, Huron Mountain Club, Fernwood Botanical Gardens, and University of Wisconsin-Madison Arboretum for allowing us to visit and collect Dryopteris in the field. Profound thanks to M. Ames, B. Berger, A. Gardner, P. Gonsiska, B. Grady, J. Hunt, R. Jabaily, D. Stein, J. Wen, and especially K. Sytsma for advice and discussion. The authors are thankful for financial support for this research from the National Science Foundation (DDIG award to E.B.S., T.J.G., grant DEB-1110335), the Huron Mountain Wildlife Foundation (E.B.S., T.J.G.), graduate research awards from the Botanical Society of America, American Society of Plant Taxonomists, and Torrey Botanical Society (E.B.S.), and a Smithsonian Graduate Research Fellowship (E.B.S.) NR 133 TC 36 Z9 37 U1 3 U2 31 PU BOTANICAL SOC AMER INC PI ST LOUIS PA PO BOX 299, ST LOUIS, MO 63166-0299 USA SN 0002-9122 EI 1537-2197 J9 AM J BOT JI Am. J. Bot. PD APR PY 2012 VL 99 IS 4 BP 730 EP 750 DI 10.3732/ajb.1100294 PG 21 WC Plant Sciences SC Plant Sciences GA 926DB UT WOS:000302810400025 PM 22434775 ER PT J AU Burke, MJ Raychaudhury, S Kraft, RP Brassington, NJ Hardcastle, MJ Goodger, JL Sivakoff, GR Forman, WR Jones, C Woodley, KA Murray, SS Kainulainen, J Birkinshaw, M Croston, JH Evans, DA Gilfanov, M Jordan, A Sarazin, CL Voss, R Worrall, DM Zhang, ZL AF Burke, Mark J. Raychaudhury, Somak Kraft, Ralph P. Brassington, Nicola J. Hardcastle, Martin J. Goodger, Joanna L. Sivakoff, Gregory R. Forman, William R. Jones, Christine Woodley, Kristin A. Murray, Stephen S. Kainulainen, Jouni Birkinshaw, Mark Croston, Judith H. Evans, Daniel A. Gilfanov, Marat Jordan, Andres Sarazin, Craig L. Voss, Rasmus Worrall, Diana M. Zhang, Zhongli TI A TRANSIENT SUB-EDDINGTON BLACK HOLE X-RAY BINARY CANDIDATE IN THE DUST LANES OF CENTAURUS A SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: elliptical and lenticular, cD; galaxies: individual (Centaurus A, NGC 5128); X-rays: binaries; X-rays: galaxies ID NGC 5128 CENTAURUS; CHANDRA MONITORING OBSERVATIONS; GLOBULAR-CLUSTER; PARTICLE-ACCELERATION; XTE J1701-462; LUMINOUS LMXBS; POINT SOURCES; CIRCINUS X-1; A NGC-5128; MASS AB We report the discovery of a bright X-ray transient CXOU J132527.6-430023 in the nearby early-type galaxy NGC 5128. The source was first detected over the course of five Chandra observations in 2007, reaching an unabsorbed outburst luminosity of (1-2) x 10(38) erg s(-1) in the 0.5-7.0 keV band before returning to quiescence. Such luminosities are possible for both stellar-mass black hole and neutron star (NS) X-ray binary transients. Here, we attempt to characterize the nature of the compact object. No counterpart has been detected in the optical or radio sky, but the proximity of the source to the dust lanes allows for the possibility of an obscured companion. The brightness of the source after a > 100-fold increase in X-ray flux makes it either the first confirmed transient non-ultraluminous X-ray black hole system in outburst to be subject to detailed spectral modeling outside the Local Group, or a bright (> 10(38) erg s(-1)) transient NS X-ray binary, which are very rare. Such a large increase in flux would appear to lend weight to the view that this is a black hole transient. X-ray spectral fitting of an absorbed power law yielded unphysical photon indices, while the parameters of the best-fit absorbed disk blackbody model are typical of an accreting similar to 10 M-circle dot black hole in the thermally dominant state. C1 [Burke, Mark J.; Raychaudhury, Somak] Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England. [Kraft, Ralph P.; Forman, William R.; Jones, Christine; Murray, Stephen S.; Evans, Daniel A.; Jordan, Andres] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Brassington, Nicola J.; Hardcastle, Martin J.; Goodger, Joanna L.] Univ Hertfordshire, Sch Phys Astron & Math, Hatfield AL10 9AB, Herts, England. [Sivakoff, Gregory R.] Univ Alberta, Dept Phys, Edmonton, AB T6G 2E1, Canada. [Woodley, Kristin A.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Murray, Stephen S.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada. [Kainulainen, Jouni] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Birkinshaw, Mark; Worrall, Diana M.] Univ Bristol, HH Wills Phys Lab, Bristol BS8 1TL, Avon, England. [Croston, Judith H.] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England. [Gilfanov, Marat; Zhang, Zhongli] Max Planck Inst Astrophys, D-85741 Garching, Germany. [Gilfanov, Marat] Russian Acad Sci, Space Res Inst, Moscow 117997, Russia. [Jordan, Andres] Pontificia Univ Catolica Chile, Dept Astron & Astrofis, Santiago 7820436, Chile. [Sarazin, Craig L.] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA. [Voss, Rasmus] Univ Nijmegen, Dept Astrophys, IMAPP, NL-6500 GL Nijmegen, Netherlands. RP Burke, MJ (reprint author), Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England. EM mburke@star.sr.bham.ac.uk RI Hardcastle, Martin/E-2264-2012; Sivakoff, Gregory/G-9602-2011; OI Hardcastle, Martin/0000-0003-4223-1117; Sivakoff, Gregory/0000-0001-6682-916X; Goodger, Joanna/0000-0002-5738-4768; Jordan, Andres/0000-0002-5389-3944 FU NASA [NAS8-03060]; STFC; University of Birmingham; NWO [016.093.305]; NSERC FX This work was supported by NASA grant NAS8-03060. M.J.B. thanks the STFC and the University of Birmingham for financial support. R.V. is supported by NWO Vidi grant 016.093.305. G.R.S. acknowledges the support of an NSERC Discovery Grant. We also thank Jeff McClintock, Mike Garcia, Ewan O'Sullivan, Trevor Ponman, & Alastair Sanderson for useful discussions. Finally, we thank the anonymous referee for their very helpful comments. NR 61 TC 3 Z9 3 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD APR PY 2012 VL 749 IS 2 AR 112 DI 10.1088/0004-637X/749/2/112 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 925TY UT WOS:000302785700016 ER PT J AU Howard, AW Bakos, GA Hartman, J Torres, G Shporer, A Mazeh, T Kovacs, G Latham, DW Noyes, RW Fischer, DA Johnson, JA Marcy, GW Esquerdo, GA Beky, B Butler, RP Sasselov, DD Stefanik, RP Perumpilly, G Lazar, J Papp, I Sari, P AF Howard, A. W. Bakos, G. A. Hartman, J. Torres, G. Shporer, A. Mazeh, T. Kovacs, Geza Latham, D. W. Noyes, R. W. Fischer, D. A. Johnson, J. A. Marcy, G. W. Esquerdo, G. A. Beky, B. Butler, R. P. Sasselov, D. D. Stefanik, R. P. Perumpilly, G. Lazar, J. Papp, I. Sari, P. TI HAT-P-17b,c: A TRANSITING, ECCENTRIC, HOT SATURN AND A LONG-PERIOD, COLD JUPITER SO ASTROPHYSICAL JOURNAL LA English DT Article DE planetary systems; stars: individual (HAT-P-17, GSC 2717-00417); techniques: photometric; techniques: spectroscopic ID KEPLER TARGET STARS; BRIGHT K-STAR; EXTRASOLAR PLANETS; MASS; STELLAR; SEARCH; FIELD; SYSTEMS; SPECTRA; CANDIDATES AB We report the discovery of HAT-P-17b,c, a multi-planet system with an inner transiting planet in a short-period, eccentric orbit and an outer planet in a 4.4 yr, nearly circular orbit. The inner planet, HAT-P-17b, transits the bright V = 10.54 early K dwarf star GSC 2717-00417, with an orbital period P = 10.338523 +/- 0.000009 days, orbital eccentricity e = 0.342 +/- 0.006, transit epoch T-c = 2454801.16943 +/- 0.00020 (BJD: barycentric Julian dates throughout the paper are calculated from Coordinated Universal Time (UTC)), and transit duration 0.1690 +/- 0.0009 days. HAT-P-17b has a mass of 0.534 +/- 0.018 MJ and radius of 1.010 +/- 0.029 R-J yielding a mean density of 0.64 +/- 0.05 g cm(-3). This planet has a relatively low equilibrium temperature in the range 780-927 K, making it an attractive target for follow-up spectroscopic studies. The outer planet, HAT-P-17c, has a significantly longer orbital period P-2 = 1610 +/- 20 days and a minimum mass m(2) sin i(2) = 1.31(-0.15)(+0.18) M-J. The orbital inclination of HAT-P-17c is unknown as transits have not been observed and may not be present. The host star has a mass of 0.86 +/- 0.04 M-circle dot, radius of 0.84 +/- 0.02 R-circle dot, effective temperature 5246 +/- 80 K, and metallicity [Fe/H] = 0.00 +/- 0.08. HAT-P-17 is the second multi-planet system detected from ground-based transit surveys. C1 [Howard, A. W.; Marcy, G. W.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Bakos, G. A.; Hartman, J.; Torres, G.; Latham, D. W.; Noyes, R. W.; Esquerdo, G. A.; Beky, B.; Sasselov, D. D.; Stefanik, R. P.; Perumpilly, G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Shporer, A.] LCOGT, Santa Barbara, CA USA. [Shporer, A.] UC Santa Barbara, Dept Phys, Santa Barbara, CA USA. [Mazeh, T.] Tel Aviv Univ, Raymond & Beverly Sackler Fac Exact Sci, Sch Phys & Astron, IL-69978 Tel Aviv, Israel. [Kovacs, Geza] Konkoly Observ Budapest, Budapest, Hungary. [Fischer, D. A.] Yale Univ, Dept Astron, New Haven, CT 06511 USA. [Johnson, J. A.] CALTECH, Dept Astrophys, Pasadena, CA 91125 USA. [Butler, R. P.] Carnegie Inst Sci, Dept Terr Magnetism, Washington, DC 20005 USA. [Lazar, J.; Papp, I.; Sari, P.] Hungarian Astron Assoc, Budapest, Hungary. RP Howard, AW (reprint author), Univ Calif Berkeley, Dept Astron, 601 Campbell Hall, Berkeley, CA 94720 USA. EM howard@astro.berkeley.edu; gbakos@cfa.harvard.edu RI Butler, Robert/B-1125-2009; Howard, Andrew/D-4148-2015; OI Howard, Andrew/0000-0001-8638-0320; Hartman, Joel/0000-0001-8732-6166; Fischer, Debra/0000-0003-2221-0861 FU NASA [NNG04GN74G, NNX08AF23G, NNX09AF59G]; SAO IRD; U. C. Berkeley Space Sciences Laboratory; NSF [AST-0702843, AST-0702821]; Kepler mission under NASA [NCC2-1390]; Hungarian Scientific Research Foundation (OTKA) [K-81373]; Israel Science Foundation [655/07] FX We thank E. Agol, H. Knutson, J. Winn, and J. Wright for helpful conversations. HATNet operations have been funded by NASA grants NNG04GN74G, NNX08AF23G, and SAO IR&D grants. A.W.H. gratefully acknowledges support from a Townes Post-doctoral Fellowship at the U. C. Berkeley Space Sciences Laboratory. Work of G.A.B. and J. Johnson were supported by the Postdoctoral Fellowship of the NSF Astronomy and Astrophysics Program (AST-0702843 and AST-0702821, respectively). G.T. acknowledges partial support from NASA grant NNX09AF59G. We acknowledge partial support also from the Kepler mission under NASA Cooperative Agreement NCC2-1390 (D.W.L.: PI). G. K. thanks the Hungarian Scientific Research Foundation (OTKA) for support through grant K-81373. T.M. acknowledges the Israel Science Foundation (grant 655/07). This research has made use of Keck telescope time granted through NOAO and NASA. We thank Ezra Mashal for his help in operating the Wise-HAT telescope over the past years. We thank the TLC project (M. Holman and J. Winn) for swapping time on the 1.2 m telescope at short notice. This research has made use of the Exoplanet Orbit Database and the Exoplanet Data Explorer at exoplanets.org, the SIMBAD database (operated at CDS, Strasbourg, France), and NASA's Astrophysics Data System Bibliographic Services. Finally, the authors wish to extend special thanks to those of Hawaiian ancestry on whose sacred mountain of Mauna Kea we were privileged to be guests. Without their generous hospitality, the Keck observations presented herein would not have been possible. NR 69 TC 20 Z9 20 U1 0 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD APR PY 2012 VL 749 IS 2 AR 134 DI 10.1088/0004-637X/749/2/134 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 925TY UT WOS:000302785700038 ER PT J AU Liu, JF Di Stefano, R Wang, T Moe, M AF Liu, Jifeng Di Stefano, Rosanne Wang, Tao Moe, Maxwell TI ON THE NATURE OF THE PROGENITOR OF THE Type Ia SN2011fe IN M101 SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries: close; supernovae: general; X-rays: binaries ID X-RAY SOURCES; ACCRETING WHITE-DWARFS; LARGE-MAGELLANIC-CLOUD; RS OPHIUCHI 2006; OPTICAL VARIABILITY; POINT SOURCES; MODELS; SUPERNOVAE; EVOLUTION; CAL-83 AB The explosion of a Type Ia supernova, SN2011fe, in the nearby Pinwheel galaxy (M101 at 6.4Mpc) provides an opportunity to study pre-explosion images and search for the progenitor, which should consist of a white dwarf (WD), possibly surrounded by an accretion disk, in orbit with another star. We report on our use of deep Chandra observations and Hubble Space Telescope observations to limit the luminosity and temperature of the pre-explosion WD. It is found that if the spectrum was a blackbody, then pre-SNWDs with steady nuclear burning of the highest possible temperatures and luminosities are excluded assuming moderate n(H) values, but values of kT between roughly 10 eV and 60 eV are permitted even if the WD was emitting at the Eddington luminosity. This allows the progenitor to be an accreting nuclear-burning WD with an expanded photosphere 4-100 times the WD itself, or a super-critically accreting WD blowing off an optically thick strong wind, or possibly a recurrent nova with luminosities an order of magnitude lower than Eddington. The observations are also consistent with a double degenerate scenario, or a spinning down WD that has been spun up by accretion from the donor. C1 [Liu, Jifeng] Natl Astron Observ China, Beijing 100012, Peoples R China. [Liu, Jifeng; Di Stefano, Rosanne; Wang, Tao; Moe, Maxwell] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Wang, Tao] Nanjing Univ, Dept Astron, Nanjing, Jiangsu, Peoples R China. RP Liu, JF (reprint author), Natl Astron Observ China, Beijing 100012, Peoples R China. FU National Science Foundation of China [11043009, 10873018] FX We thank Alicia Soderberg, Robin Ciardullo, and Kim Herrmann for helpful discussions. We thank the anonymous referee for comments that have led to the improvement of the manuscript. This work is partially supported by the National Science Foundation of China under the grants 11043009 and 10873018. NR 51 TC 13 Z9 13 U1 1 U2 9 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD APR PY 2012 VL 749 IS 2 AR 141 DI 10.1088/0004-637X/749/2/141 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 925TY UT WOS:000302785700045 ER PT J AU Luo, B Fabbiano, G Fragos, T Kim, DW Belczynski, K Brassington, NJ Pellegrini, S Tzanavaris, P Wang, JF Zezas, A AF Luo, B. Fabbiano, G. Fragos, T. Kim, D-W Belczynski, K. Brassington, N. J. Pellegrini, S. Tzanavaris, P. Wang, Junfeng Zezas, A. TI PROBING THE X-RAY BINARY POPULATIONS OF THE RING GALAXY NGC 1291 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: individual (NGC 1291); galaxies: luminosity function, mass function; X-rays: binaries; X-rays: galaxies ID CHANDRA MONITORING OBSERVATIONS; STAR-FORMING GALAXIES; BLACK-HOLE BINARIES; MS SOURCE CATALOGS; LUMINOSITY FUNCTION; ELLIPTIC GALAXIES; NEARBY GALAXIES; DEEP CHANDRA; LENTICULAR GALAXIES; CONFIDENCE-LIMITS AB We present Chandra studies of the X-ray binary (XRB) populations in the bulge and ring regions of the ring galaxy NGC 1291. We detect 169 X-ray point sources in the galaxy, 75 in the bulge and 71 in the ring, utilizing the four available Chandra observations totaling an effective exposure of 179 ks. We report photometric properties of these sources in a point-source catalog. There are approximate to 40% of the bulge sources and approximate to 25% of the ring sources showing >3 sigma long-term variability in their X-ray count rate. The X-ray colors suggest that a significant fraction of the bulge (approximate to 75%) and ring (approximate to 65%) sources are likely low-mass X-ray binaries (LMXBs). The spectra of the nuclear source indicate that it is a low-luminosity active galactic nucleus (AGN) with moderate obscuration; spectral variability is observed between individual observations. We construct 0.3-8.0 keV X-ray luminosity functions (XLFs) for the bulge and ring XRB populations, taking into account the detection incompleteness and background AGN contamination. We reach 90% completeness limits of approximate to 1.5 x 10(37) and approximate to 2.2 x 10(37) erg s(-1) for the bulge and ring populations, respectively. Both XLFs can be fit with a broken power-law model, and the shapes are consistent with those expected for populations dominated by LMXBs. We perform detailed population synthesis modeling of the XRB populations in NGC 1291, which suggests that the observed combined XLF is dominated by an old LMXB population. We compare the bulge and ring XRB populations, and argue that the ring XRBs are associated with a younger stellar population than the bulge sources, based on the relative overdensity of X-ray sources in the ring, the generally harder X-ray color of the ring sources, the overabundance of luminous sources in the combined XLF, and the flatter shape of the ring XLF. C1 [Luo, B.; Fabbiano, G.; Fragos, T.; Kim, D-W; Wang, Junfeng] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Belczynski, K.] Univ Warsaw, Astron Observ, PL-00478 Warsaw, Poland. [Belczynski, K.] Univ Texas Brownsville, Ctr Gravitat Wave Astron, Brownsville, TX 78520 USA. [Brassington, N. J.] Univ Hertfordshire, Sch Phys Astron & Math, Hatfield AL10 9AB, Herts, England. [Pellegrini, S.] Univ Bologna, Dipartimento Astron, I-40127 Bologna, Italy. [Tzanavaris, P.] NASA, Lab Xray Astrophys, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Tzanavaris, P.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Zezas, A.] Univ Crete, Dept Phys, GR-71003 Iraklion, Crete, Greece. RP Luo, B (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Zezas, Andreas/C-7543-2011; Fragos, Tassos/A-3581-2016 OI Zezas, Andreas/0000-0001-8952-676X; Fragos, Tassos/0000-0003-1474-1523 FU NASA [GO0-11104X, NAS8-03060]; CXC; NASA at Goddard Space Flight Center FX This work is supported by NASA grant GO0-11104X. We acknowledge support from the CXC, which is operated by the Smithsonian Astrophysical Observatory (SAO) for and on behalf of NASA under Contract NAS8-03060. S. Pellegrini acknowledges partial support from ASI/INAF grant I/009/10/0. P. Tzanavaris acknowledges support through a NASA Postdoctoral Program Fellowship at Goddard Space Flight Center, administered by Oak Ridge Associated Universities through a contract with NASA. We thank G. Risaliti for helpful discussions. We thank the referee for carefully reviewing the manuscript and providing helpful comments. NR 90 TC 11 Z9 11 U1 0 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD APR PY 2012 VL 749 IS 2 AR 130 DI 10.1088/0004-637X/749/2/130 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 925TY UT WOS:000302785700034 ER PT J AU Migliori, G Siemiginowska, A Celotti, A AF Migliori, Giulia Siemiginowska, Aneta Celotti, Annalisa TI BROADBAND JET EMISSION IN YOUNG AND POWERFUL RADIO SOURCES: THE CASE OF THE COMPACT STEEP SPECTRUM QUASAR 3C 186 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: jets; quasars: individual: (3C 186); X-rays: galaxies ID ACTIVE GALACTIC NUCLEI; X-RAY-EMISSION; HUBBLE-SPACE-TELESCOPE; INVERSE-COMPTON MODEL; LARGE-AREA TELESCOPE; HIGH-ENERGY EMISSION; LARGE-SCALE JETS; ACCRETION-DISK; RELATIVISTIC JETS; GALAXY 3C-31 AB We present the X-ray analysis of a deep (similar to 200 ks) Chandra observation of the compact steep spectrum radio-loud quasar 3C 186 (z = 1.06) and investigate the contribution of the unresolved radio jet to the total X-ray emission. The spectral analysis is not conclusive on the origin of the bulk of the X-ray emission. In order to examine the jet contribution to the X-ray flux, we model the quasar spectral energy distribution, adopting several scenarios for the jet emission. For the values of the main physical parameters favored by the observables, a dominant role of the jet emission in the X-ray band is ruled out when a single-zone (leptonic) scenario is adopted, even including the contribution of the external photon fields as seed photons for inverse Compton emission. We then consider a structured jet, with the blazar component that-although not directly visible in the X-ray band-provides an intense field of seed synchrotron photons Compton-scattered by electrons in a mildly relativistic knot. In this case, the whole X-ray emission can be accounted for if we assume a blazar luminosity within the range observed from flat spectrum radio quasars. The X-ray radiative efficiency of such a (structured) jet is intimately related to the presence of a complex velocity structure. The jet emission can provide a significant contribution in X-rays if it decelerates within the host galaxy on kiloparsec scales. We discuss the implications of this model in terms of jet dynamics and interaction with the ambient medium. C1 [Migliori, Giulia; Siemiginowska, Aneta] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Migliori, Giulia; Celotti, Annalisa] SISSA, I-34136 Trieste, Italy. RP Migliori, G (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM migliori@cfa.harvard.edu FU NASA, Chandra X-Ray Observatory Center [NAS8-39073, GO2-3148A, GO8-9125A, GO0-11133X]; Fermi [NNX10AO60G] FX We thank the anonymous referee for comments that significantly improved the manuscript. The authors thank C.C. Cheung for providing radio fluxes, M. Guainazzi, L. Stawarz for useful discussions, and T. Aldcroft for help in improving the text. G.M. thanks P.Grandi, M.Sobolewska, and F.Massaro for valuable discussions and suggestions. G.M. is grateful to L.Ostorero for insightful comments and great help in improving the manuscript. This research is funded in part by NASA contract NAS8-39073. Partial support for this work was provided by Fermi grant NNX10AO60G. Partial support for this work was provided by the National Aeronautics and Space Administration through Chandra Award Number GO2-3148A and GO8-9125A, GO0-11133X issued by the Chandra X-Ray Observatory Center, which is operated by the Smithsonian Astrophysical Observatory for and on behalf of NASA under contract NAS8-39073. A.C. thanks the Center for Astrophysics for hospitality. NR 108 TC 7 Z9 7 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 APR PY 2012 VL 749 IS 2 AR 107 DI 10.1088/0004-637X/749/2/107 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 925TY UT WOS:000302785700012 ER PT J AU Oberg, KI Qi, CH Wilner, DJ Hogerheijde, MR AF Oeberg, Karin I. Qi, Chunhua Wilner, David J. Hogerheijde, Michiel R. TI EVIDENCE FOR MULTIPLE PATHWAYS TO DEUTERIUM ENHANCEMENTS IN PROTOPLANETARY DISKS SO ASTROPHYSICAL JOURNAL LA English DT Article DE astrochemistry; circumstellar matter; ISM: molecules; molecular processes; stars: pre-main sequence ID 2-DIMENSIONAL DISTRIBUTIONS; DEUTERATED MOLECULES; SUBMILLIMETER ARRAY; GASEOUS MOLECULES; COLUMN DENSITIES; TW HYDRAE; DM TAURI; CHEMISTRY; EVOLUTION; WATER AB The distributions of deuterated molecules in protoplanetary disks are expected to depend on the molecular formation pathways. We use observations of spatially resolved DCN emission from the disk around TW Hya, acquired during ALMA science verification with a similar to 3 '' synthesized beam, together with comparable DCO+ observations from the Submillimeter Array, to investigate differences in the radial distributions of these species and hence differences in their formation chemistry. In contrast to DCO+, which shows an increasing column density with radius, DCN is better fit by a model that is centrally peaked. We infer that DCN forms at a smaller radii and thus at higher temperatures than DCO+. This is consistent with chemical network model predictions of DCO+ formation from H2D+ at T < 30 K and DCN formation from additional pathways involving CH2D+ at higher temperatures. We estimate a DCN/HCN abundance ratio of similar to 0.017, similar to the DCO+/HCO+ abundance ratio. Deuterium fractionation appears to be efficient at a range of temperatures in this protoplanetary disk. These results suggest caution in interpreting the range of deuterium fractions observed in solar system bodies, as multiple formation pathways should be taken into account. C1 [Oeberg, Karin I.; Qi, Chunhua; Wilner, David J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Hogerheijde, Michiel R.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. RP Oberg, KI (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM koberg@cfa.harvard.edu FU NASA; Space Telescope Science Institute [NAS 5-26555]; NASA Origins of Solar Systems [NNX11AK63] FX We thank the anonymous referee for detailed comments on especially the disk chemistry, which have improved the paper considerably. The Atacama Large Millimeter/submillimeter Array (ALMA), an international astronomy facility, is a partnership of Europe, North America, and East Asia in cooperation with the Republic of Chile. This paper makes use of the following ALMA science verification data: ADS/JAO.ALMA#2011.0.00001.SV. Support to K.I.O. is provided by NASA through Hubble Fellowship grant awarded by the Space Telescope Science Institute, operated by the Association of Universities for Research in Astronomy, Inc., for NASA, under contract NAS 5-26555. We acknowledge NASA Origins of Solar Systems grant No. NNX11AK63. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. NR 32 TC 17 Z9 17 U1 1 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD APR PY 2012 VL 749 IS 2 AR 162 DI 10.1088/0004-637X/749/2/162 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 925TY UT WOS:000302785700066 ER PT J AU Slane, P Hughes, JP Temim, T Rousseau, R Castro, D Foight, D Gaensler, BM Funk, S Lemoine-Goumard, M Gelfand, JD Moffett, DA Dodson, RG Bernstein, JP AF Slane, Patrick Hughes, John P. Temim, Tea Rousseau, Romain Castro, Daniel Foight, Dillon Gaensler, B. M. Funk, Stefan Lemoine-Goumard, Marianne Gelfand, Joseph D. Moffett, David A. Dodson, Richard G. Bernstein, Joseph P. TI A BROADBAND STUDY OF THE EMISSION FROM THE COMPOSITE SUPERNOVA REMNANT MSH 11-62 SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM: individual objects (MSH-11-62); ISM: supernova remnants; radiation mechanisms: non-thermal; stars: neutron ID PULSAR WIND NEBULA; LARGE-AREA TELESCOPE; X-RAY-EMISSION; HIGH-ENERGY; RADIO; EVOLUTION; G291.0-0.1; HESS; HYDRODYNAMICS; ACCELERATION AB MSH 11-62 (G291.0-0.1) is a composite supernova remnant for which radio and X-ray observations have identified the remnant shell as well as its central pulsar wind nebula. The observations suggest a relatively young system expanding into a low-density region. Here, we present a study of MSH 11-62 using observations with the Chandra, XMM-Newton, and Fermi observatories, along with radio observations from the Australia Telescope Compact Array. We identify a compact X-ray source that appears to be the putative pulsar that powers the nebula, and show that the X-ray spectrum of the nebula bears the signature of synchrotron losses as particles diffuse into the outer nebula. Using data from the Fermi Large Area Telescope, we identify gamma-ray emission originating from MSH 11-62. With density constraints from the new X-ray measurements of the remnant, we model the evolution of the composite system in order to constrain the properties of the underlying pulsar and the origin of the gamma-ray emission. C1 [Slane, Patrick; Castro, Daniel; Foight, Dillon] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Hughes, John P.] Rutgers State Univ, Dept Phys & Astron, Piscataway, NJ 08854 USA. [Temim, Tea] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Rousseau, Romain; Lemoine-Goumard, Marianne] Univ Bordeaux, CNRS IN2P3, UMR 5797, Ctr Etud Nucl Bordeaux Gradignan, F-33175 Gradignan, France. [Gaensler, B. M.] Univ Sydney, Sydney Inst Astron, Sch Phys A29, Sydney, NSW 2006, Australia. [Funk, Stefan] Stanford Linear Accelerator Ctr, Kavli Inst Particle Astrophys & Cosmol, Menlo Pk, CA 94025 USA. [Gelfand, Joseph D.] New York Univ Abu Dhabi, Abu Dhabi, U Arab Emirates. [Moffett, David A.] Furman Univ, Dept Phys, Greenville, SC 29613 USA. [Dodson, Richard G.] Univ Western Australia, Int Ctr Radio Astron Res, Crawley, WA 6009, Australia. [Bernstein, Joseph P.] Argonne Natl Lab, Div High Energy Phys, Argonne, IL 60439 USA. [Bernstein, Joseph P.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. RP Slane, P (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM slane@cfa.harvard.edu; jph@physics.rutgers.edu; tea.temim@nasa.gov; rousseau@cenbg.in2p3.fr; bryan.gaensler@sydney.edu.au; funk@slac.stanford.edu; lemoine@cenbg.in2p3.fr; jg168@astro.physics.nyu.edu; david.moffett@furman.edu; richard.dodson@icrar.org; jpbernst@anl.gov RI Gaensler, Bryan/F-8655-2010; Funk, Stefan/B-7629-2015; Gelfand, Joseph/F-1110-2015; OI Funk, Stefan/0000-0002-2012-0080; Gelfand, Joseph/0000-0003-4679-1058; Gaensler, Bryan/0000-0002-3382-9558; Temim, Tea/0000-0001-7380-3144 FU NASA [NRA 00-OSS-07/03500279, NNX 11AQ09G, NGT5-159, NAS8-03060]; Commonwealth of Australia FX NASA supported this work via grant numbers NRA 00-OSS-07/03500279, NNX 11AQ09G, and NGT5-159. P.S. acknowledges support from NASA Contract NAS8-03060. The ATCA is funded by the Commonwealth of Australia for operation as a National Facility managed by CSIRO.; R.R., M.L.-G., and SF. have participated as members of the Fermi-LAT Collaboration, which acknowledges generous ongoing support from a number of agencies and institutes that have supported both the development and the operation of the LAT as well as scientific data analysis. These include th United States, the Commissariat a l'Energie Atomique and the Centre National de la Recherche Scientifique/Institut National de Phe National Aeronautics and Space Administration and the Department of Energy in theysique Nucleaire et de Physique des Particules in France, the Agenzia Spaziale Italiana and the Istituto Nazionale di Fisica Nucleare in Italy, the Ministry of Education, Culture, Sports, Science and Technology (MEXT), High Energy Accelerator Research Organization (KEK) and Japan Aerospace NR 41 TC 10 Z9 10 U1 0 U2 8 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD APR PY 2012 VL 749 IS 2 AR 131 DI 10.1088/0004-637X/749/2/131 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 925TY UT WOS:000302785700035 ER PT J AU van der Horst, AJ Kouveliotou, C Gorgone, NM Kaneko, Y Baring, MG Guiriec, S Gogus, E Granot, J Watts, AL Lin, L Bhat, PN Bissaldi, E Chaplin, VL Finger, MH Gehrels, N Gibby, MH Giles, MM Goldstein, A Gruber, D Harding, AK Kaper, L von Kienlin, A van der Klis, M McBreen, S Mcenery, J Meegan, CA Paciesas, WS Pe'er, A Preece, RD Ramirez-Ruiz, E Rau, A Wachter, S Wilson-Hodge, C Woods, PM Wijers, RAMJ AF van der Horst, A. J. Kouveliotou, C. Gorgone, N. M. Kaneko, Y. Baring, M. G. Guiriec, S. Gogus, E. Granot, J. Watts, A. L. Lin, L. Bhat, P. N. Bissaldi, E. Chaplin, V. L. Finger, M. H. Gehrels, N. Gibby, M. H. Giles, M. M. Goldstein, A. Gruber, D. Harding, A. K. Kaper, L. von Kienlin, A. van der Klis, M. McBreen, S. Mcenery, J. Meegan, C. A. Paciesas, W. S. Pe'er, A. Preece, R. D. Ramirez-Ruiz, E. Rau, A. Wachter, S. Wilson-Hodge, C. Woods, P. M. Wijers, R. A. M. J. TI SGRJ 1550-5418 BURSTS DETECTED WITH THE FERMI GAMMA-RAY BURST MONITOR DURING ITS MOST PROLIFIC ACTIVITY SO ASTROPHYSICAL JOURNAL LA English DT Article DE pulsars: individual (SGR J1550-5418, 1E 1547.0-5408, PSR J1550-5418); stars: neutron; X-rays: bursts ID PULSAR 1E 1547.0-5408; MAGNETIZED NEUTRON-STARS; STATISTICAL PROPERTIES; 2009 OUTBURST; EMISSION; REPEATERS; SGR-1900+14; 1E-1547.0-5408; MAGNETARS; SOFT-GAMMA-REPEATER-1806-20 AB We have performed detailed temporal and time-integrated spectral analysis of 286 bursts from SGR J1550-5418 detected with the Fermi Gamma-ray Burst Monitor (GBM) in 2009 January, resulting in the largest uniform sample of temporal and spectral properties of SGR J1550-5418 bursts. We have used the combination of broadband and high time-resolution data provided with GBM to perform statistical studies for the source properties. We determine the durations, emission times, duty cycles, and rise times for all bursts, and find that they are typical of SGR bursts. We explore various models in our spectral analysis, and conclude that the spectra of SGR J1550-5418 bursts in the 8-200 keV band are equally well described by optically thin thermal bremsstrahlung (OTTB), a power law (PL) with an exponential cutoff (Comptonized model), and two blackbody (BB) functions (BB+BB). In the spectral fits with the Comptonized model, we find a mean PL index of -0.92, close to the OTTB index of -1. We show that there is an anti-correlation between the Comptonized E-peak and the burst fluence and average flux. For the BB+BB fits, we find that the fluences and emission areas of the two BB functions are correlated. The low-temperature BB has an emission area comparable to the neutron star surface area, independent of the temperature, while the high-temperature BB has a much smaller area and shows an anti-correlation between emission area and temperature. We compare the properties of these bursts with bursts observed from other SGR sources during extreme activations, and discuss the implications of our results in the context of magnetar burst models. C1 [van der Horst, A. J.; Finger, M. H.; Meegan, C. A.] NSSTC, Univ Space Res Assoc, Huntsville, AL 35805 USA. [van der Horst, A. J.; Watts, A. L.; Kaper, L.; van der Klis, M.; Wijers, R. A. M. J.] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1090 GE Amsterdam, Netherlands. [Kouveliotou, C.; Wilson-Hodge, C.] NASA, Space Sci Off, VP62, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. [Gorgone, N. M.] Connecticut Coll, New London, CT 06320 USA. [Kaneko, Y.; Gogus, E.; Lin, L.] Sabanci Univ, TR-34956 Istanbul, Turkey. [Baring, M. G.] Rice Univ, Dept Phys & Astron, Houston, TX 77251 USA. [Guiriec, S.; Lin, L.; Bhat, P. N.; Chaplin, V. L.; Goldstein, A.; Paciesas, W. S.; Preece, R. D.] Univ Alabama, CSPAR, Huntsville, AL 35805 USA. [Guiriec, S.; Gehrels, N.; Harding, A. K.; Mcenery, J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Granot, J.] Hebrew Univ Jerusalem, Racah Inst Phys, IL-91904 Jerusalem, Israel. [Granot, J.] Tel Aviv Univ, Raymond & Beverly Sackler Sch Phys & Astron, IL-69978 Tel Aviv, Israel. [Granot, J.] Univ Hertfordshire, Ctr Astrophys Res, Hatfield AL10 9AB, Herts, England. [Lin, L.] Chinese Acad Sci, Natl Astron Observ, Beijing 100012, Peoples R China. [Bissaldi, E.; Gruber, D.; von Kienlin, A.; Rau, A.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Gibby, M. H.; Giles, M. M.] Jacobs Technol Inc, Huntsville, AL USA. [McBreen, S.] Univ Coll Dublin, Dublin 4, Ireland. [Pe'er, A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Ramirez-Ruiz, E.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. [Wachter, S.] CALTECH, IPAC, Pasadena, CA 91125 USA. [Woods, P. M.] Corvid Technol, Huntsville, AL 35806 USA. RP van der Horst, AJ (reprint author), NSSTC, Univ Space Res Assoc, Huntsville, AL 35805 USA. EM A.J.VanDerHorst@uva.nl RI McEnery, Julie/D-6612-2012; Bissaldi, Elisabetta/K-7911-2016; OI Bissaldi, Elisabetta/0000-0001-9935-8106; Preece, Robert/0000-0003-1626-7335; Wijers, Ralph/0000-0002-3101-1808 FU NASA [NNH07ZDA001-GLAST, NNX10AC59A]; Scientific and Technological Research Council of Turkey (TUBITAK) [109T755]; NASA at the Goddard Space Flight Center; ERC; NWO FX A.J.v.d.H. thanks Vicky Kaspi for useful discussions. This publication is part of the GBM/Magnetar Key Project (NASA grant NNH07ZDA001-GLAST, PI: C. Kouveliotou). Y.K. and E.G. acknowledge the support from the Scientific and Technological Research Council of Turkey (TUBITAK) through grant 109T755. M.G.B. acknowledges support from NASA through grant NNX10AC59A. S.G. was supported by an appointment to the NASA Postdoctoral Program at the Goddard Space Flight Center, administered by Oak Ridge Associated Universities through a contract with NASA. J.G. is supported by the ERC advanced research grant "GRBs." A.L.W. acknowledges support from an NWO Vidi Grant. NR 63 TC 27 Z9 27 U1 0 U2 10 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD APR PY 2012 VL 749 IS 2 AR 122 DI 10.1088/0004-637X/749/2/122 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 925TY UT WOS:000302785700026 ER PT J AU Wang, XF Wang, LF Filippenko, AV Baron, E Kromer, M Jack, D Zhang, TM Aldering, G Antilogus, P Arnett, WD Baade, D Barris, BJ Benetti, S Bouchet, P Burrows, AS Canal, R Cappellaro, E Carlberg, RG di Carlo, E Challis, PJ Crotts, APS Danziger, JI Della Valle, M Fink, M Foley, RJ Fransson, C Gal-Yam, A Garnavich, PM Gerardy, CL Goldhaber, G Hamuy, M Hillebrandt, W Hoflich, P Holland, ST Holz, DE Hughes, JP Jeffery, DJ Jha, SW Kasen, D Khokhlov, AM Kirshner, RP Knop, RA Kozma, C Krisciunas, K Lee, BC Leibundgut, B Lentz, EJ Leonard, DC Lewin, WHG Li, WD Livio, M Lundqvist, P Maoz, D Matheson, T Mazzali, PA Meikle, P Miknaitis, G Milne, PA Mochnacki, SW Nomoto, K Nugent, PE Oran, ES Panagia, N Perlmutter, S Phillips, MM Pinto, P Poznanski, D Pritchet, CJ Reinecke, M Riess, AG Ruiz-Lapuente, P Scalzo, RA Schlegel, EM Schmidt, BP Siegrist, J Soderberg, AM Sollerman, J Sonneborn, G Spadafora, A Spyromilio, J Sramek, RA Starrfield, SG Strolger, LG Suntzeff, NB Thomas, RC Tonry, JL Tornambe, A Truran, JW Turatto, M Turner, M Van Dyk, SD Weiler, KW Wheeler, JC Wood-Vasey, M Woosley, SE Yamaoka, H AF Wang, Xiaofeng Wang, Lifan Filippenko, Alexei V. Baron, Eddie Kromer, Markus Jack, Dennis Zhang, Tianmeng Aldering, Greg Antilogus, Pierre Arnett, W. David Baade, Dietrich Barris, Brian J. Benetti, Stefano Bouchet, Patrice Burrows, Adam S. Canal, Ramon Cappellaro, Enrico Carlberg, Raymond G. di Carlo, Elisa Challis, Peter J. Crotts, Arlin P. S. Danziger, John I. Della Valle, Massimo Fink, Michael Foley, Ryan J. Fransson, Claes Gal-Yam, Avishay Garnavich, Peter M. Gerardy, Chris L. Goldhaber, Gerson Hamuy, Mario Hillebrandt, Wolfgang Hoeflich, Peter Holland, Stephen T. Holz, Daniel E. Hughes, John P. Jeffery, David J. Jha, Saurabh W. Kasen, Dan Khokhlov, Alexei M. Kirshner, Robert P. Knop, Robert A. Kozma, Cecilia Krisciunas, Kevin Lee, Brian C. Leibundgut, Bruno Lentz, Eric J. Leonard, Douglas C. Lewin, Walter H. G. Li, Weidong Livio, Mario Lundqvist, Peter Maoz, Dan Matheson, Thomas Mazzali, Paolo A. Meikle, Peter Miknaitis, Gajus Milne, Peter A. Mochnacki, Stefan W. Nomoto, Ken'ichi Nugent, Peter E. Oran, Elaine S. Panagia, Nino Perlmutter, Saul Phillips, Mark M. Pinto, Philip Poznanski, Dovi Pritchet, Christopher J. Reinecke, Martin Riess, Adam G. Ruiz-Lapuente, Pilar Scalzo, Richard A. Schlegel, Eric M. Schmidt, Brian P. Siegrist, James Soderberg, Alicia M. Sollerman, Jesper Sonneborn, George Spadafora, Anthony Spyromilio, Jason Sramek, Richard A. Starrfield, Sumner G. Strolger, Louis G. Suntzeff, Nicholas B. Thomas, Rollin C. Tonry, John L. Tornambe, Amedeo Truran, James W. Turatto, Massimo Turner, Michael Van Dyk, Schuyler D. Weiler, Kurt W. Wheeler, J. Craig Wood-Vasey, Michael Woosley, Stanford E. Yamaoka, Hitoshi TI EVIDENCE FOR TYPE Ia SUPERNOVA DIVERSITY FROM ULTRAVIOLET OBSERVATIONS WITH THE HUBBLE SPACE TELESCOPE SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology: observations; distance scale; dust, extinction; supernovae: general; ultraviolet: general ID HIGH-VELOCITY FEATURES; WHITE-DWARF MODELS; LIGHT CURVES; MAXIMUM LIGHT; COSMOLOGICAL PARAMETERS; ABSOLUTE MAGNITUDES; SPECTRAL EVOLUTION; SYNTHETIC SPECTRA; HOST GALAXIES; K-CORRECTIONS AB We present ultraviolet (UV) spectroscopy and photometry of four Type Ia supernovae (SNe 2004dt, 2004ef, 2005M, and 2005cf) obtained with the UV prism of the Advanced Camera for Surveys on the Hubble Space Telescope. This data set provides unique spectral time series down to 2000 angstrom. Significant diversity is seen in the near-maximum-light spectra (similar to 2000-3500 angstrom) for this small sample. The corresponding photometric data, together with archival data from Swift Ultraviolet/Optical Telescope observations, provide further evidence of increased dispersion in the UV emission with respect to the optical. The peak luminositiesmeasured in the uvw1/F250W filter are found to correlate with the B-band light-curve shape parameter Delta m(15)(B), but with much larger scatter relative to the correlation in the broadband B band (e.g., similar to 0.4 mag versus similar to 0.2 mag for those with 0.8 mag < Delta m(15)(B) < 1.7 mag). SN 2004dt is found as an outlier of this correlation (at > 3 sigma), being brighter than normal SNe Ia such as SN 2005cf by similar to 0.9 mag and similar to 2.0 mag in the uvw1/F250W and uvm2/F220W filters, respectively. We show that different progenitor metallicity or line-expansion velocities alone cannot explain such a large discrepancy. Viewing-angle effects, such as due to an asymmetric explosion, may have a significant influence on the flux emitted in the UV region. Detailed modeling is needed to disentangle and quantify the above effects. C1 [Wang, Xiaofeng] Tsinghua Univ, Dept Phys, Beijing 100084, Peoples R China. [Wang, Xiaofeng] Tsinghua Univ, Tsinghua Ctr Astrophys THCA, Beijing 100084, Peoples R China. [Wang, Xiaofeng; Wang, Lifan; Krisciunas, Kevin; Suntzeff, Nicholas B.] Texas A&M Univ, Dept Phys & Astron, College Stn, TX 77843 USA. [Wang, Xiaofeng; Filippenko, Alexei V.; Li, Weidong] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Baron, Eddie] Univ Oklahoma, Dept Phys, Norman, OK 73019 USA. [Kromer, Markus; Hillebrandt, Wolfgang; Mazzali, Paolo A.; Reinecke, Martin] Max Planck Inst Astrophys, D-85748 Garching, Germany. [Jack, Dennis] Hamburger Sternwarte, D-21029 Hamburg, Germany. [Zhang, Tianmeng] Chinese Acad Sci, Natl Astron Observ China, Beijing 100012, Peoples R China. [Aldering, Greg; Goldhaber, Gerson; Lee, Brian C.; Nugent, Peter E.; Perlmutter, Saul; Scalzo, Richard A.; Siegrist, James; Spadafora, Anthony; Thomas, Rollin C.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA. [Antilogus, Pierre] Lab Phys Nucl Hautes Energies, Paris, France. [Arnett, W. David; Milne, Peter A.; Pinto, Philip] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Baade, Dietrich; Leibundgut, Bruno; Spyromilio, Jason] European So Observ, D-85748 Garching, Germany. [Barris, Brian J.; Tonry, John L.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Benetti, Stefano; Cappellaro, Enrico; Mazzali, Paolo A.] Osserv Astron Padova, I-35122 Padua, Italy. [Bouchet, Patrice] CEA, Serv Astrophys, DSM, DAPNIA, F-91191 Gif Sur Yvette, France. [Burrows, Adam S.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. [Canal, Ramon; Ruiz-Lapuente, Pilar] Univ Barcelona, Dept Astron & Meterorol, Barcelona 8007, Spain. [Carlberg, Raymond G.] Univ Toronto, Dept Astron & Astrophys, Toronto, ON M5S 3J3, Canada. [di Carlo, Elisa] Osservatorio Astron Teramo, INAF, I-64100 Treamo, Italy. [Challis, Peter J.; Foley, Ryan J.; Kirshner, Robert P.; Soderberg, Alicia M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Crotts, Arlin P. S.] Columbia Univ, Dept Astron, New York, NY 10025 USA. [Danziger, John I.; Turatto, Massimo] Osserv Astron Trieste, INAF, I-34143 Trieste, Italy. [Della Valle, Massimo] INAF Napoli, Capodimonte Astron Observ, I-80131 Naples, Italy. [Della Valle, Massimo] Int Ctr Relativist Astrophys, I-65122 Pescara, Italy. [Fink, Michael] Univ Wurzburg, Inst Theoret Phys & Astrophys, D-97074 Wurzburg, Germany. [Fransson, Claes; Kozma, Cecilia; Lundqvist, Peter; Sollerman, Jesper] Stockholm Univ, SE-10691 Stockholm, Sweden. [Gal-Yam, Avishay] Weizmann Inst Sci, Fac Phys, Dept Particle Phys & Astrophys, IL-76100 Rehovot, Israel. [Garnavich, Peter M.] Univ Notre Dame, Dept Phys, Notre Dame, IN 46556 USA. [Gerardy, Chris L.; Hoeflich, Peter] Florida State Univ, Dept Phys, Tallahassee, FL 32306 USA. [Hamuy, Mario] Univ Chile, Dept Astron, Santiago, Chile. [Holland, Stephen T.; Sonneborn, George] NASA, Lab Observat Cosmol, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Holz, Daniel E.; Khokhlov, Alexei M.; Truran, James W.; Turner, Michael] Univ Chicago, Enrico Fermi Inst, Dept Phys, Chicago, IL 60637 USA. [Holz, Daniel E.; Khokhlov, Alexei M.; Truran, James W.; Turner, Michael] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Hughes, John P.; Jha, Saurabh W.] Rutgers State Univ, Dept Phys & Astron, Piscataway, NJ 08854 USA. [Jeffery, David J.] No Arizona Univ, Dept Phys & Astron, Flagstaff, AZ 86011 USA. [Kasen, Dan] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. [Knop, Robert A.] Quest Univ Canada, Dept Phys, Squamish, BC, Canada. [Lentz, Eric J.] Univ Tennessee, Dept Phys & Astron, Knoxville, TN 37996 USA. [Leonard, Douglas C.] San Diego State Univ, Dept Astron, San Diego, CA 92182 USA. [Lewin, Walter H. G.] MIT, Cambridge, MA 02139 USA. [Livio, Mario; Panagia, Nino; Riess, Adam G.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Maoz, Dan] Tel Aviv Univ, Wise Observ, IL-69978 Tel Aviv, Israel. [Matheson, Thomas] Natl Opt Astron Observ, Tucson, AZ 85719 USA. [Meikle, Peter] Univ London Imperial Coll Sci Technol & Med, London SW7 2AZ, England. [Miknaitis, Gajus] Ctr Neighborhood Technol, Chicago, IL 60647 USA. [Mochnacki, Stefan W.] Univ Toronto, Dept Astron & Astrophys, Toronto, ON M5S 3G4, Canada. [Nomoto, Ken'ichi; Oran, Elaine S.] Univ Tokyo, IPMU, Kashiwa, Chiba 2778583, Japan. [Phillips, Mark M.] Carnegie Inst Washington, Washington, DC 20005 USA. [Poznanski, Dovi] Tel Aviv Univ, Sch Phys & Astron, IL-69978 Tel Aviv, Israel. [Pritchet, Christopher J.] Univ Victoria, Dept Phys & Astron, Victoria, BC V8W 2Y2, Canada. [Schlegel, Eric M.] Univ Texas San Antonio, Dept Phys & Astron, San Antonio, TX 78249 USA. [Schmidt, Brian P.] Australian Natl Univ, Res Sch Astron & Astrophys, Canberra, ACT 0200, Australia. [Sramek, Richard A.] Natl Radio Astron Observ, Socorro, NM 87801 USA. [Starrfield, Sumner G.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA. [Strolger, Louis G.] Western Kentucky Univ, Dept Phys & Astron, Bowling Green, KY 42101 USA. [Tornambe, Amedeo] Rome Astron Observ, INAF, I-00136 Rome, Italy. [Van Dyk, Schuyler D.] CALTECH, IPAC, Pasadena, CA 91125 USA. [Weiler, Kurt W.] USN, Res Lab, Washington, DC 20375 USA. [Wheeler, J. Craig] Univ Texas Austin, McDonald Observ, Austin, TX 78712 USA. [Wheeler, J. Craig] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA. [Wood-Vasey, Michael] Univ Pittsburgh, Pittsburgh Particle Phys Astrophys & Cosmol Ctr P, Pittsburgh, PA 15260 USA. [Woosley, Stanford E.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95060 USA. [Yamaoka, Hitoshi] Kyushu Univ, Grad Sch Sci, Fukuoka 8128581, Japan. RP Wang, XF (reprint author), Tsinghua Univ, Dept Phys, Beijing 100084, Peoples R China. EM wang_xf@mail.tsinghua.edu.cn RI Carlberg, Raymond/I-6947-2012; Nomoto, Ken'ichi/A-4393-2011; Perlmutter, Saul/I-3505-2015; Wang, Xiaofeng/J-5390-2015; Lentz, Eric/M-7173-2015; Hamuy, Mario/G-7541-2016; OI Cappellaro, Enrico/0000-0001-5008-8619; Turatto, Massimo/0000-0002-9719-3157; Carlberg, Raymond/0000-0002-7667-0081; Perlmutter, Saul/0000-0002-4436-4661; Lentz, Eric/0000-0002-5231-0532; TORNAMBE, AMEDEO/0000-0002-6392-7378; Baron, Edward/0000-0001-5393-1608; Della Valle, Massimo/0000-0003-3142-5020; Schmidt, Brian/0000-0001-6589-1287; Sollerman, Jesper/0000-0003-1546-6615; Scalzo, Richard/0000-0003-3740-1214; Van Dyk, Schuyler/0000-0001-9038-9950; Benetti, Stefano/0000-0002-3256-0016 FU National Science Foundation of China (NSFC) [11178003, 11073013, 10173003]; National Key Basic Research Science Foundation (NKBRSF) [TG199075402]; NSF [AST-0607485, AST-0908886, AST-0708873, AST-0707769]; TABASGO Foundation; US Department of Energy [DE-FC02-06ER41453, DE-FG02-08ER41563]; NASA [GO-10182, AR-12126, NAS 5-26555]; Space Telescope Science Institute [AR-12623]; WPI Initiative, MEXT, Japan; NASA ADP [NNX06AH85G]; ICM [P10-064-F]; CONICYT, Chile [150100003, PFB-06]; [ASI-INAF I/009/10/0] FX We thank Mark Sullivan and Andy Howell for their suggestions. Financial support for this work has been provided by the National Science Foundation of China (NSFC grants 11178003, 11073013, and 10173003) and the National Key Basic Research Science Foundation (NKBRSF TG199075402). A.V.F.'s group at U.C. Berkeley is grateful for the support of NSF grants AST-0607485 and AST-0908886, the TABASGO Foundation, and US Department of Energy grants DE-FC02-06ER41453 (SciDAC) and DE-FG02-08ER41563. Substantial financial support for this work was also provided by NASA through grants GO-10182, AR-12126, and AR-12623 from the Space Telescope Science Institute, which is operated by Associated Universities for Research in Astronomy, Inc., under NASA contract NAS 5-26555. The work of L.W. is supported by NSF grant AST-0708873. J.C.W. is supported by NSF grant AST-0707769. K.N. is supported by WPI Initiative, MEXT, Japan. M.T., S.B., and E.C. are supported by grant ASI-INAF I/009/10/0. P.A.M. is supported by NASA ADP NNX06AH85G. The work of M.H. is supported by ICM grant P10-064-F and CONICYT grants 150100003 and PFB-06, Chile. NR 99 TC 29 Z9 30 U1 1 U2 26 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD APR PY 2012 VL 749 IS 2 AR 126 DI 10.1088/0004-637X/749/2/126 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 925TY UT WOS:000302785700030 ER PT J AU Yamaguchi, H Tanaka, M Maeda, K Slane, PO Foster, A Smith, RK Katsuda, S Yoshii, R AF Yamaguchi, H. Tanaka, M. Maeda, K. Slane, P. O. Foster, A. Smith, R. K. Katsuda, S. Yoshii, R. TI ELEMENTAL ABUNDANCES IN THE POSSIBLE TYPE Ia SUPERNOVA REMNANT G344.7-0.1 SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM: abundances; ISM: individual objects (G344.7-0.1); ISM: supernova remnants; X-rays: ISM ID LARGE-MAGELLANIC-CLOUD; X-RAY-EMISSION; METAL-POOR STARS; GALACTIC PLANE SURVEY; FORMED DENSE SHELL; INTERSTELLAR-MEDIUM; PROGENITOR SYSTEMS; THERMAL CONDUCTION; CHEMICAL EVOLUTION; SUZAKU OBSERVATION AB Recent studies on the Galactic supernova remnant (SNR) G344.7-0.1 have commonly claimed its origin to be a core-collapse supernova (SN) explosion, based on its highly asymmetric morphology and/or proximity to a star-forming region. In this paper, however, we present an X-ray spectroscopic study of this SNR using Suzaku, which is supportive of a Type Ia origin. Strong K-shell emission from lowly ionized Fe has clearly been detected, and its origin is determined, for the first time, to be the Fe-rich SN ejecta. The abundance pattern is highly consistent with that expected for a somewhat-evolved Type Ia SNR. It is suggested, therefore, that the X-ray point-like source CXOU J170357.8-414302 located at the SNR's geometrical center is not associated with the SNR but is likely to be a foreground object. Our result further indicates that G344.7-0.1 is the first possible Type Ia SNR categorized as a member of the so-called mixed-morphology class. In addition, we have detected emission from He-like Al at similar to 1.6 keV, the first clear detection of this element in the spectrum of an extended X-ray source. The possible enhancement of the Al/Mg abundance ratio from the solar value suggests that the ambient interstellar medium has a relatively high metallicity (not less than 10% of the solar value). We also report the marginal detection of Cr and Mn, although the measured fluxes of these lines have large statistical and systematic uncertainties. C1 [Yamaguchi, H.; Slane, P. O.; Foster, A.; Smith, R. K.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Yamaguchi, H.; Katsuda, S.; Yoshii, R.] RIKEN, Inst Phys & Chem Res, Wako, Saitama 3510198, Japan. [Tanaka, M.] Natl Inst Nat Sci, Natl Astron Observ Japan, Mitaka, Tokyo 1818588, Japan. [Tanaka, M.; Maeda, K.] Univ Tokyo, Inst Phys & Math Universe, Kashiwa, Chiba 2778568, Japan. RP Yamaguchi, H (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM hyamaguchi@head.cfa.harvard.edu RI XRAY, SUZAKU/A-1808-2009 FU Japan Society for the Promotion of Science (JSPS); NASA ADP [NNX09AC71G] FX The authors appreciate a number of constructive suggestions from the anonymous referee. We are also grateful to Drs. Laura A. Lopez and Kazimierz J. Borkowski for helpful discussions and Dr. Yoh Takei for providing information about ASTRO-H/SXS. H.Y. is supported by Japan Society for the Promotion of Science (JSPS) Research Fellowship for Research Abroad, and acknowledges funding from NASA ADP grant NNX09AC71G. NR 76 TC 14 Z9 14 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD APR PY 2012 VL 749 IS 2 AR 137 DI 10.1088/0004-637X/749/2/137 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 925TY UT WOS:000302785700041 ER PT J AU Hines, AH Johnson, EG Aguilar, R Kramer, M Goodison, M Roberts, P Richie, K AF Hines, Anson H. Johnson, Eric G. Aguilar, Robert Kramer, Margaret Goodison, Michael Roberts, Paige Richie, Kimberly TI BLUE CRAB FISHERY STOCK DYNAMICS: MANAGING FOR RECRUITMENT LIMITATION SO JOURNAL OF SHELLFISH RESEARCH LA English DT Meeting Abstract C1 [Hines, Anson H.; Aguilar, Robert; Kramer, Margaret; Goodison, Michael; Roberts, Paige; Richie, Kimberly] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. [Johnson, Eric G.] Univ N Florida, Jacksonville, FL 32224 USA. RI Aguilar, Robert/O-2480-2016 OI Aguilar, Robert/0000-0001-8732-5382 NR 0 TC 0 Z9 0 U1 0 U2 1 PU NATL SHELLFISHERIES ASSOC PI GROTON PA C/O DR. SANDRA E. SHUMWAY, UNIV CONNECTICUT, 1080 SHENNECOSSETT RD, GROTON, CT 06340 USA SN 0730-8000 J9 J SHELLFISH RES JI J. Shellfish Res. PD APR PY 2012 VL 31 IS 1 BP 297 EP 297 PG 1 WC Fisheries; Marine & Freshwater Biology SC Fisheries; Marine & Freshwater Biology GA 926QU UT WOS:000302846800165 ER PT J AU Miller, W Riedel, G AF Miller, Whitman Riedel, Gerhardt TI NEARSHORE ACIDIFICATION: WHY COASTAL OCEAN ECOSYSTEMS ARE DIFFERENT SO JOURNAL OF SHELLFISH RESEARCH LA English DT Meeting Abstract C1 [Miller, Whitman; Riedel, Gerhardt] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. NR 0 TC 0 Z9 0 U1 0 U2 13 PU NATL SHELLFISHERIES ASSOC PI GROTON PA C/O DR. SANDRA E. SHUMWAY, UNIV CONNECTICUT, 1080 SHENNECOSSETT RD, GROTON, CT 06340 USA SN 0730-8000 J9 J SHELLFISH RES JI J. Shellfish Res. PD APR PY 2012 VL 31 IS 1 BP 323 EP 324 PG 2 WC Fisheries; Marine & Freshwater Biology SC Fisheries; Marine & Freshwater Biology GA 926QU UT WOS:000302846800258 ER PT J AU Seitz, RD Hines, AH AF Seitz, Rochelle D. Hines, Anson H. TI POPULATION DECLINE AND RESTORATION OF SOFTSHELL CLAMS IN CHESAPEAKE BAY: ROLE OF PREDATION, HABITAT, DISEASE, AND ENVIRONMENTAL FACTORS SO JOURNAL OF SHELLFISH RESEARCH LA English DT Meeting Abstract C1 [Seitz, Rochelle D.] Coll William & Mary, Virginia Inst Marine Sci, Gloucester Point, VA 23062 USA. [Hines, Anson H.] Smithsonian Environm Res Ctr, Smithsonian Inst, Edgewater, MD 21037 USA. NR 0 TC 0 Z9 0 U1 1 U2 9 PU NATL SHELLFISHERIES ASSOC PI GROTON PA C/O DR. SANDRA E. SHUMWAY, UNIV CONNECTICUT, 1080 SHENNECOSSETT RD, GROTON, CT 06340 USA SN 0730-8000 J9 J SHELLFISH RES JI J. Shellfish Res. PD APR PY 2012 VL 31 IS 1 BP 344 EP 345 PG 2 WC Fisheries; Marine & Freshwater Biology SC Fisheries; Marine & Freshwater Biology GA 926QU UT WOS:000302846800330 ER PT J AU Besla, G Kallivayalil, N Hernquist, L van der Marel, RP Cox, TJ Keres, D AF Besla, Gurtina Kallivayalil, Nitya Hernquist, Lars van der Marel, Roeland P. Cox, T. J. Keres, Dusan TI The role of dwarf galaxy interactions in shaping the Magellanic System and implications for Magellanic Irregulars SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Review DE galaxies: evolution; galaxies: interactions; galaxies: irregular; galaxies: kinematics and dynamics; Magellanic Clouds ID STAR-FORMATION HISTORY; N-BODY SIMULATIONS; PARTICLE HYDRODYNAMICS SIMULATIONS; GRAVITATIONAL LENSING EXPERIMENT; NEAR-INFRARED SURVEYS; HIGH-VELOCITY CLOUDS; H-I; LEADING ARM; LOCAL GROUP; MILKY-WAY AB We present a novel pair of numerical models of the interaction history between the Large and Small Magellanic Clouds (LMC and SMC, respectively) and our Milky Way (MW) in light of recent high-precision proper motions from the Hubble Space Telescope. Given the updated velocities, cosmological simulations of hierarchical structure formation favour a scenario where the Magellanic Clouds (MCs) are currently on their first infall towards our Galaxy. We illustrate here that the observed irregular morphology and internal kinematics of the Magellanic System (in gas and stars) are naturally explained by interactions between the LMC and SMC, rather than gravitational interactions with the MW. These conclusions provide further support that the MCs are completing their first infall to our system. In particular, we demonstrate that the Magellanic Stream, a band of H i gas trailing behind the Clouds 150 degrees across the sky, can be accounted for by the action of LMC tides on the SMC before the system was accreted by the MW. We further demonstrate that the off-centre, warped stellar bar of the LMC, and its one-armed spiral can be naturally explained by a recent direct collision with its lower mass companion, the SMC. Such structures are key morphological characteristics of a class of galaxies referred to as Magellanic Irregulars, the majority of which are not associated with massive spiral galaxies. We infer that dwarfdwarf galaxy interactions are important drivers for the morphological evolution of Magellanic Irregulars and can dramatically affect the efficiency of baryon removal from dwarf galaxies via the formation of extended tidal bridges and tails. Such interactions are not only important for the evolution of dwarf galaxies but also have direct consequences for the build-up of baryons in our own MW, as LMC-mass systems are believed to be the dominant building blocks of MW-type haloes. C1 [Besla, Gurtina] Columbia Univ, Dept Astron & Astrophys, New York, NY 10027 USA. [Besla, Gurtina; Hernquist, Lars] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Kallivayalil, Nitya] Yale Univ, Dept Astron, New Haven, CT 06520 USA. [van der Marel, Roeland P.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Cox, T. J.] Carnegie Observ, Pasadena, CA 91101 USA. [Keres, Dusan] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Keres, Dusan] Univ Calif Berkeley, Theoret Astrophys Ctr, Berkeley, CA 94720 USA. RP Besla, G (reprint author), Columbia Univ, Dept Astron & Astrophys, 550 W 120th St, New York, NY 10027 USA. EM gbesla@astro.columbia.edu FU FAS Science Division Research Computing Group at Harvard University; NASA [HST-HF-51284.01-A] FX The simulations in this paper were run on the Odyssey cluster supported by the FAS Science Division Research Computing Group at Harvard University. We thank Knut Olsen, Alar Toomre, David Nidever, Crystal Martin, Patrik Jonsson, Mary Putman and Dennis Zaritsky for useful discussions that have contributed to this paper. GB acknowledges support from NASA through Hubble Fellowship grant HST-HF-51284.01-A. NR 164 TC 97 Z9 97 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 APR PY 2012 VL 421 IS 3 BP 2109 EP 2138 DI 10.1111/j.1365-2966.2012.20466.x PG 30 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 923LJ UT WOS:000302620500022 ER PT J AU Steffen, JH Fabrycky, DC Ford, EB Carter, JA Desert, JM Fressin, F Holman, MJ Lissauer, JJ Moorhead, AV Rowe, JF Ragozzine, D Welsh, WF Batalha, NM Borucki, WJ Buchhave, LA Bryson, S Caldwell, DA Charbonneau, D Ciardi, DR Cochran, WD Endl, M Everett, ME Gautier, TN Gilliland, RL Girouard, FR Jenkins, JM Horch, E Howell, SB Isaacson, H Klaus, TC Koch, DG Latham, DW Li, J Lucas, P MacQueen, PJ Marcy, GW McCauliff, S Middour, CK Morris, RL Mullally, FR Quinn, SN Quintana, EV Shporer, A Still, M Tenenbaum, P Thompson, SE Twicken, JD Van Cleve, J AF Steffen, Jason H. Fabrycky, Daniel C. Ford, Eric B. Carter, Joshua A. Desert, Jean-Michel Fressin, Francois Holman, Matthew J. Lissauer, Jack J. Moorhead, Althea V. Rowe, Jason F. Ragozzine, Darin Welsh, William F. Batalha, Natalie M. Borucki, William J. Buchhave, Lars A. Bryson, Steve Caldwell, Douglas A. Charbonneau, David Ciardi, David R. Cochran, William D. Endl, Michael Everett, Mark E. Gautier, Thomas N., III Gilliland, Ron L. Girouard, Forrest R. Jenkins, Jon M. Horch, Elliott Howell, Steve B. Isaacson, Howard Klaus, Todd C. Koch, David G. Latham, David W. Li, Jie Lucas, Philip MacQueen, Phillip J. Marcy, Geoffrey W. McCauliff, Sean Middour, Christopher K. Morris, Robert L. Mullally, Fergal R. Quinn, Samuel N. Quintana, Elisa V. Shporer, Avi Still, Martin Tenenbaum, Peter Thompson, Susan E. Twicken, Joseph D. Van Cleve, Jeffery TI Transit timing observations from Kepler - III. Confirmation of four multiple planet systems by a Fourier-domain study of anticorrelated transit timing variations SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE methods: data analysis; celestial mechanics; stars: individual: KIC 4349452; stars: individual: KIC 9757613; stars: individual: KIC 5792202; stars: individual: KIC 6949607 ID SPITZER-SPACE-TELESCOPE; EXOPLANET HD 189733B; SOLAR-TYPE STARS; LIGHT CURVES; CANDIDATES; MISSION; MASS; ATMOSPHERE; SCIENCE; II. AB We present a method to confirm the planetary nature of objects in systems with multiple transiting exoplanet candidates. This method involves a Fourier-domain analysis of the deviations in the transit times from a constant period that result from dynamical interactions within the system. The combination of observed anticorrelations in the transit times and mass constraints from dynamical stability allow us to claim the discovery of four planetary systems, Kepler-25, Kepler-26, Kepler-27 and Kepler-28, containing eight planets and one additional planet candidate. C1 [Steffen, Jason H.; Moorhead, Althea V.] Fermilab Ctr Particle Astrophys, Batavia, IL 60510 USA. [Fabrycky, Daniel C.] Univ Calif Santa Cruz, UCO Lick Observ, Santa Cruz, CA 95064 USA. [Ford, Eric B.] Univ Florida, Dept Astron, Bryant Space Sci Ctr 211, Gainesville, FL 32111 USA. [Carter, Joshua A.; Desert, Jean-Michel; Fressin, Francois; Holman, Matthew J.; Ragozzine, Darin; Charbonneau, David; Quinn, Samuel N.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Lissauer, Jack J.; Rowe, Jason F.; Borucki, William J.; Bryson, Steve; Caldwell, Douglas A.; Girouard, Forrest R.; Jenkins, Jon M.; Howell, Steve B.; Klaus, Todd C.; Koch, David G.; Li, Jie; Middour, Christopher K.; Morris, Robert L.; Mullally, Fergal R.; Quintana, Elisa V.; Still, Martin; Tenenbaum, Peter; Thompson, Susan E.; Twicken, Joseph D.; Van Cleve, Jeffery] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Rowe, Jason F.; Jenkins, Jon M.; Li, Jie; Morris, Robert L.; Mullally, Fergal R.; Quintana, Elisa V.; Tenenbaum, Peter; Thompson, Susan E.; Twicken, Joseph D.; Van Cleve, Jeffery] SETI Inst, Mountain View, CA 94043 USA. [Welsh, William F.; Ciardi, David R.] CALTECH, NASA Exoplanet Sci Inst, Pasadena, CA 91125 USA. [Batalha, Natalie M.] San Diego State Univ, Dept Astron, San Diego, CA 92182 USA. [Buchhave, Lars A.; Shporer, Avi] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA. [Cochran, William D.; Endl, Michael; MacQueen, Phillip J.] Univ Texas Austin, McDonald Observ, Austin, TX 78730 USA. [Everett, Mark E.] Natl Opt Astron Observ, Tucson, AZ 85719 USA. [Gautier, Thomas N., III] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Gilliland, Ron L.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Girouard, Forrest R.; Klaus, Todd C.; Middour, Christopher K.] NASA, Orbital Sci Corp, Ames Res Ctr, Moffett Field, CA 94035 USA. [Horch, Elliott] So Connecticut State Univ, Dept Phys, New Haven, CT 06515 USA. [Isaacson, Howard; Marcy, Geoffrey W.] Univ Calif Berkeley, Berkeley, CA 94720 USA. [Lucas, Philip] Univ Hertfordshire, Ctr Astrophys Res, Hatfield AL10 9AB, Herts, England. [McCauliff, Sean] San Jose State Univ, San Jose, CA 95192 USA. [Shporer, Avi; Still, Martin] Las Cumbres Observ Global Telescope, Goleta, CA 93117 USA. RP Steffen, JH (reprint author), Fermilab Ctr Particle Astrophys, POB 500,MS 127, Batavia, IL 60510 USA. EM jsteffen@fnal.gov RI Steffen, Jason/A-4320-2013; Carter, Joshua/A-8280-2013; Ragozzine, Darin/C-4926-2013; Caldwell, Douglas/L-7911-2014; OI Caldwell, Douglas/0000-0003-1963-9616; Buchhave, Lars A./0000-0003-1605-5666; Ciardi, David/0000-0002-5741-3047; Fabrycky, Daniel/0000-0003-3750-0183 FU NASA's Science Mission Directorate; NASA [NNX08AR04G, HF-51272.01-A, HF-51267.01-A]; Space Telescope Science Institute [NAS 5-26555]; NASA through JPL/Caltech FX Funding for the Kepler mission is provided by NASA's Science Mission Directorate. We thank the entire Kepler team for the many years of work that is proving so successful. JHS acknowledges support by NASA under grant NNX08AR04G issued through the Kepler Participating Scientist Programme. DCF and JAC acknowledge support for this work provided by NASA through Hubble Fellowship grants #HF-51272.01-A and #HF-51267.01-A awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., for NASA, under contract NAS 5-26555. This work is based in part on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA. Support for this work was provided by NASA through an award issued by JPL/Caltech. We would like to thank the Spitzer staff at IPAC and in particular Nancy Silbermann for scheduling the Spitzer observations of this programme. NR 34 TC 83 Z9 83 U1 1 U2 3 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD APR PY 2012 VL 421 IS 3 BP 2342 EP 2354 DI 10.1111/j.1365-2966.2012.20467.x PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 923LJ UT WOS:000302620500038 ER PT J AU Narayanan, D Krumholz, MR Ostriker, EC Hernquist, L AF Narayanan, Desika Krumholz, Mark R. Ostriker, Eve C. Hernquist, Lars TI A general model for the CO-H2 conversion factor in galaxies with applications to the star formation law SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Review DE ISM: clouds; ISM: molecules; galaxies: interactions; galaxies: ISM; galaxies: starburst; galaxies: star formation ID GAMMA-RAY EMISSION; SUPERMASSIVE BLACK-HOLES; GIANT MOLECULAR CLOUDS; REDSHIFT SUBMILLIMETER GALAXIES; ULTRALUMINOUS INFRARED GALAXIES; QUASAR LUMINOSITY FUNCTION; HIGH-RESOLUTION CO; GAS-RICH MERGERS; INTERSTELLAR-MEDIUM; MAJOR MERGERS AB The most common means of converting an observed CO line intensity into a molecular gas mass requires the use of a conversion factor (XCO). While in the Milky Way this quantity does not appear to vary significantly, there is good reason to believe that XCO will depend on the larger-scale galactic environment. With sensitive instruments pushing detections to increasingly high redshift, characterizing XCO as a function of physical conditions is crucial to our understanding of galaxy evolution. Utilizing numerical models, we investigate how varying metallicities, gas temperatures and velocity dispersions in galaxies impacts the way CO line emission traces the underlying H2 gas mass, and under what circumstances XCO may differ from the Galactic mean value. We find that, due to the combined effects of increased gas temperature and velocity dispersion, XCO is depressed below the Galactic mean in high surface density environments such as ultraluminous infrared galaxies (ULIRGs). In contrast, in low-metallicity environments, XCO tends to be higher than in the Milky Way, due to photodissociation of CO in metal-poor clouds. At higher redshifts, gas-rich discs may have gravitationally unstable clumps that are warm (due to increased star formation) and have elevated velocity dispersions. These discs tend to have XCO values ranging between present-epoch gas-rich mergers and quiescent discs at low z. This model shows that on average mergers do have lower XCO values than disc galaxies, though there is significant overlap. XCO varies smoothly with the local conditions within a galaxy, and is not a function of global galaxy morphology. We combine our results to provide a general fitting formula for XCO as a function of CO line intensity and metallicity. We show that replacing the traditional approach of using one constant XCO for starbursts and another for discs with our best-fitting function produces star formation laws that are continuous rather than bimodal, and that have significantly reduced scatter. C1 [Narayanan, Desika] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Krumholz, Mark R.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. [Ostriker, Eve C.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Hernquist, Lars] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Narayanan, D (reprint author), Univ Arizona, Steward Observ, 933 N Cherry Ave, Tucson, AZ 85721 USA. EM dnarayanan@as.arizona.edu FU NSF [AST-1009452, AST-0807739, CAREER-0955300, AST-0908185]; Alfred P. Sloan Fellowship; NASA [NNX09AK31G]; Harvard Faculty of Arts and Sciences Research Computing Group FX This work benefited from work done and conversations had at the Aspen Center for Physics. Emanuele Daddi, Robert Feldmann, Reinhard Genzel, Adam Leroy, Patrik Jonsson, Eric Murphy, Rahul Shetty and Andrew Skemer provided many helpful conversations and suggestions. We additionally thank Reinhard Genzel for providing us with digital copies of the relevant observational data from Tacconi et al. (2008) and Genzel et al. (2012), and Emanuele Daddi for providing us with the data from Daddi et al. (2010a). DN and LH acknowledge support from the NSF via grant AST-1009452. MK acknowledges support from: an Alfred P. Sloan Fellowship; the NSF through grants AST-0807739 and CAREER-0955300; and NASA through Astrophysics Theory and Fundamental Physics grant NNX09AK31G and a Chandra Theoretical Research Program grant. ECO acknowledges support from the NSF via grant AST-0908185. The simulations in this paper were run on the Odyssey cluster, supported by the Harvard Faculty of Arts and Sciences Research Computing Group. NR 188 TC 141 Z9 141 U1 0 U2 2 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD APR PY 2012 VL 421 IS 4 BP 3127 EP 3146 DI 10.1111/j.1365-2966.2012.20536.x PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 923LL UT WOS:000302620700033 ER PT J AU Rosindell, J Hubbell, SP He, FL Harmon, LJ Etienne, RS AF Rosindell, James Hubbell, Stephen P. He, Fangliang Harmon, Luke J. Etienne, Rampal S. TI The case for ecological neutral theory SO TRENDS IN ECOLOGY & EVOLUTION LA English DT Article ID SPECIES ABUNDANCE DISTRIBUTIONS; AREA RELATIONSHIPS; PROTRACTED SPECIATION; COMMUNITY ECOLOGY; NUMBERS ADD; BIODIVERSITY; MODELS; DIVERSITY; PATTERNS; PREDICT AB Ecological neutral theory has elicited strong opinions in recent years. Here, we review these opinions and strip away some unfortunate problems with semantics to reveal three major underlying questions. Only one of these relates to neutral theory and the importance of ecological drift, whereas the others involve the link between pattern and process, the tradeoff between simplicity and complexity in modeling, and the role of stochasticity and drift in ecology. We explain how neutral theory cannot be simultaneously used both as a null hypothesis and as an,approximation. However, we also show how neutral theory always has a valuable use in one of these two roles even though the real world is not neutral. C1 [Rosindell, James] Univ Leeds, Inst Integrat & Comparat Biol, Leeds LS2 9JT, W Yorkshire, England. [Rosindell, James; Harmon, Luke J.] Univ Idaho, Inst Bioinformat & Evolutionary Studies, Moscow, ID 83844 USA. [Rosindell, James] Univ London Imperial Coll Sci Technol & Med, Div Biol, Ascot SL5 7PY, Berks, England. [Hubbell, Stephen P.] Univ Calif Los Angeles, Dept Ecol & Evolutionary Biol, Los Angeles, CA 90095 USA. [Hubbell, Stephen P.] Smithsonian Trop Res Inst, Ctr Trop Forest Sci, Unit 0948, Apo Aa 340020948, Panama. [He, Fangliang] Univ Alberta, Dept Renewable Resources, Edmonton, AB T6G 2H1, Canada. [He, Fangliang] Sun Yat Sen Univ, State Key Lab Biocontrol, SYSU Alberta Joint Lab Biodivers Conservat, Guangzhou 510275, Guangdong, Peoples R China. [Harmon, Luke J.] Univ Idaho, Dept Biol Sci, Moscow, ID 83844 USA. [Etienne, Rampal S.] Univ Groningen, Community & Conservat Ecol Grp, Ctr Ecol & Evolutionary Studies, NL-9700 CC Groningen, Netherlands. RP Rosindell, J (reprint author), Univ Leeds, Inst Integrat & Comparat Biol, Leeds LS2 9JT, W Yorkshire, England. EM james@rosindell.org RI Etienne, Rampal/F-5835-2012; OI Etienne, Rampal/0000-0003-2142-7612; Rosindell, James/0000-0002-5060-9346 FU EPSRC [EP/F043112/1]; NERC; VIDI from NWO-ALW; NSF [DEB-0919499]; NSERC (Canada) FX We thank Bart Haegeman, Omar Al Hammal, Egbert Leigh Jr, Albert Phillimore and Robert Ricklefs for very useful comments on the manuscript. We also thank Jonathan Eastman for interesting and useful discussions. JR was funded by an EPSRC overseas postdoctoral research fellowship at the life sciences interface (grant EP/F043112/1) and is now funded by a NERC fellowship; RSE was funded by a VIDI grant from NWO-ALW, LJH by NSF DEB-0919499 and FH by NSERC (Canada). NR 74 TC 81 Z9 87 U1 12 U2 216 PU ELSEVIER SCIENCE LONDON PI LONDON PA 84 THEOBALDS RD, LONDON WC1X 8RR, ENGLAND SN 0169-5347 J9 TRENDS ECOL EVOL JI Trends Ecol. Evol. PD APR PY 2012 VL 27 IS 4 BP 203 EP 208 DI 10.1016/j.tree.2012.01.004 PG 6 WC Ecology; Evolutionary Biology; Genetics & Heredity SC Environmental Sciences & Ecology; Evolutionary Biology; Genetics & Heredity GA 928II UT WOS:000302976000007 PM 22341498 ER PT J AU David, LP Jones, C Forman, W AF David, Laurence P. Jones, Christine Forman, William TI THE UNIVERSAL GAS MASS FRACTION IN CLUSTERS OF GALAXIES SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology: observations; galaxies: clusters: general; X-rays: galaxies: clusters ID X-RAY LUMINOSITY; INTRACLUSTER GAS; TEMPERATURE RELATION; SCALING RELATIONS; DARK ENERGY; XMM-NEWTON; T RELATION; CHANDRA; SAMPLE; CONSTRAINTS AB We obtained a deep 150 ks Chandra observation of the optically selected cluster of galaxies, RCS 2318+0034, to investigate the gas mass fraction in this system. Combining our deep Chandra observation with an archival 50 ks observation, we derive gas mass fractions of f(gas) = 0.06 +/- .02 and 0.10 +/- .02 within r(2500) and r(500), respectively. The gas mass fraction in RCS 2318+0034 within r(500) is typical of X-ray-selected clusters. Further study shows that the large-scale properties of RCS 2318+0034, including the relations between gas mass, X-ray luminosity, and gas temperature, are also consistent with the observed correlations of X-ray-selected clusters. However, the gas mass fraction within r(2500) is less than most X-ray-selected clusters, as previously reported. The deep Chandra image of RCS 2318+0034 shows that this system is currently undergoing a major merger which may have an impact on the inferred gas mass fraction within r(2500). C1 [David, Laurence P.; Jones, Christine; Forman, William] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP David, LP (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM ldavid@head.cfa.harvard.edu OI Forman, William/0000-0002-9478-1682 FU NASA [GO8-9122X] FX We thank A. Hicks for her help with comparing our results and also A. Vikhlinin for useful comments. This work was supported in part by the NASA grant GO8-9122X. NR 44 TC 7 Z9 7 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD APR 1 PY 2012 VL 748 IS 2 AR 120 DI 10.1088/0004-637X/748/2/120 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 916WZ UT WOS:000302135200048 ER PT J AU Donley, JL Koekemoer, AM Brusa, M Capak, P Cardamone, CN Civano, F Ilbert, O Impey, CD Kartaltepe, JS Miyaji, T Salvato, M Sanders, DB Trump, JR Zamorani, G AF Donley, J. L. Koekemoer, A. M. Brusa, M. Capak, P. Cardamone, C. N. Civano, F. Ilbert, O. Impey, C. D. Kartaltepe, J. S. Miyaji, T. Salvato, M. Sanders, D. B. Trump, J. R. Zamorani, G. TI IDENTIFYING LUMINOUS ACTIVE GALACTIC NUCLEI IN DEEP SURVEYS: REVISED IRAC SELECTION CRITERIA SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: active; infrared: galaxies; X-rays: galaxies ID WIDE-FIELD SURVEY; ULTRALUMINOUS INFRARED GALAXIES; SPITZER-SPACE-TELESCOPE; RAY SPECTRAL PROPERTIES; STAR-FORMATION HISTORY; HIGH-REDSHIFT GALAXIES; EXTENDED GROTH STRIP; DISTANT RED GALAXIES; POWER-LAW GALAXIES; AGN DUSTY TORI AB Spitzer/IRAC selection is a powerful tool for identifying luminous active galactic nuclei (AGNs). For deep IRAC data, however, the AGN selection wedges currently in use are heavily contaminated by star-forming galaxies, especially at high redshift. Using the large samples of luminous AGNs and high-redshift star-forming galaxies in COSMOS, we redefine the AGN selection criteria for use in deep IRAC surveys. The new IRAC criteria are designed to be both highly complete and reliable, and incorporate the best aspects of the current AGN selection wedges and of infrared power-law selection while excluding high-redshift star-forming galaxies selected via the BzK, distant red galaxy, Lyman-break galaxy, and submillimeter galaxy criteria. At QSO luminosities of log L2-10 (keV)(erg s(-1)) >= 44, the new IRAC criteria recover 75% of the hard X-ray and IRAC-detected XMM-COSMOS sample, yet only 38% of the IRAC AGN candidates have X-ray counterparts, a fraction that rises to 52% in regions with Chandra exposures of 50-160 ks. X-ray stacking of the individually X-ray non-detected AGN candidates leads to a hard X-ray signal indicative of heavily obscured to mildly Compton-thick obscuration (log N-H (cm(-2)) = 23.5 +/- 0.4). While IRAC selection recovers a substantial fraction of luminous unobscured and obscured AGNs, it is incomplete to low-luminosity and host-dominated AGNs. C1 [Donley, J. L.; Koekemoer, A. M.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Brusa, M.; Salvato, M.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Capak, P.] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. [Cardamone, C. N.] MIT, Dept Phys, Cambridge, MA 02139 USA. [Civano, F.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Ilbert, O.] Univ Aix Marseille 1, CNRS, Lab Astrophys Marseille, UMR 6110, F-13388 Marseille 13, France. [Impey, C. D.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Kartaltepe, J. S.] Natl Opt Astron Observ, Tucson, AZ 85719 USA. [Miyaji, T.] Univ Nacl Autonoma Mexico, Inst Astron, Ensenada, Baja California, Mexico. [Miyaji, T.] Univ Calif San Diego, Ctr Astrophys & Space Sci, La Jolla, CA 92093 USA. [Sanders, D. B.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Trump, J. R.] Univ Calif Santa Cruz, UCO Lick, Santa Cruz, CA 95064 USA. [Zamorani, G.] INAF Osservatorio Astron Bologna, I-40127 Bologna, Italy. RP Donley, JL (reprint author), Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA. EM donley@stsci.edu OI Koekemoer, Anton/0000-0002-6610-2048; Zamorani, Giovanni/0000-0002-2318-301X; Brusa, Marcella/0000-0002-5059-6848 FU STScI; CONACyT [Apoyo 83564]; DGAPA UNAM [PAPIIT IN110209]; NASA ADP [NNX07AT02G] FX We thank Ranga Chary, Harry Ferguson, Joanna Kuraszkiewicz, Mark Lacy, Daniel Stern, Belinda Wilkes, Steve Willner, and the anonymous referee for helpful discussions and comments that improved this paper. J.L.D. is supported by the Giacconi Fellowship at STScI. This work is partially supported by CONACyT Apoyo 83564, DGAPA UNAM Grant PAPIIT IN110209, and NASA ADP Grant NNX07AT02G. NR 134 TC 186 Z9 186 U1 0 U2 6 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD APR 1 PY 2012 VL 748 IS 2 AR 142 DI 10.1088/0004-637X/748/2/142 PG 22 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 916WZ UT WOS:000302135200070 ER PT J AU Foley, RJ AF Foley, Ryan J. TI THE RELATION BETWEEN EJECTA VELOCITY, INTRINSIC COLOR, AND HOST-GALAXY MASS FOR HIGH-REDSHIFT TYPE Ia SUPERNOVAE SO ASTROPHYSICAL JOURNAL LA English DT Article DE distance scale; dust, extinction; supernovae: general ID LIGHT CURVES; LEGACY SURVEY; DARK ENERGY; ABSOLUTE MAGNITUDES; SYNTHETIC SPECTRA; ESSENCE PROJECT; SPECTROSCOPY; CONSTRAINTS; EVOLUTION; ULTRAVIOLET AB Recently, using a large low-redshift sample of Type Ia supernovae (SNe Ia), we discovered a relation between SN Ia ejecta velocity and intrinsic color that improves the distance precision of SNe Ia and reduces potential systematic biases related to dust reddening. No SN Ia cosmological results have yet made a correction for the "velocity-color" relation. To test the existence of such a relation and constrain its properties at high redshift, we examine a sample of 75 SNe Ia discovered and observed by the Sloan Digital Sky Survey-II Supernova Survey and Supernova Legacy Survey. From each spectrum, we measure ejecta velocities at maximum brightness for the Ca H&K and Si II lambda 6355 features, v(Ca H&K)(0) and v(Si II)(0), respectively. Using SN light curve parameters, we determine the intrinsic B-max - V-max for each SN. Similar to what was found at low redshift, we find that SNe Ia with higher ejecta velocity tend to be intrinsically redder than SNe Ia with lower ejecta velocity. The distributions of ejecta velocities for SNe Ia at low and high redshift are similar, indicating that current cosmological results should have little bias related to the velocity-color relation. Additionally, we find a slight (2.4 sigma significant) trend between SN Ia ejecta velocity and host-galaxy mass such that SNe Ia in high-mass host galaxies tend to have lower ejecta velocities as probed by v(Ca H&K)(0). These results emphasize the importance of spectroscopy for SN Ia cosmology. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Foley, RJ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM rfoley@cfa.harvard.edu FU Clay Fellowship FX R.J.F. is supported by a Clay Fellowship. NR 65 TC 23 Z9 24 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD APR 1 PY 2012 VL 748 IS 2 AR 127 DI 10.1088/0004-637X/748/2/127 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 916WZ UT WOS:000302135200055 ER PT J AU Herve, A Rauw, G Naze, Y Foster, A AF Herve, A. Rauw, G. Naze, Y. Foster, A. TI GLOBAL MODELING OF X-RAY SPECTRA PRODUCED IN O-TYPE STAR WINDS SO ASTROPHYSICAL JOURNAL LA English DT Article DE stars: early-type; stars: mass-loss; X-rays: stars ID HELIUM-LIKE IONS; EMISSION-LINE PROFILES; ZETA-PUPPIS; MASS-LOSS; CHANDRA SPECTRUM; STELLAR WIND; SPECTROSCOPY; ABSORPTION; RATIOS; CLUMPS AB High-resolution X-ray spectra of O-type stars revealed less wind absorption than expected from smooth winds with conventional mass-loss rates. Various solutions have been proposed, including porous winds, optically thick clumps, or an overall reduction of the mass-loss rates. The latter has a strong impact on the evolution of the star. Our final goal is to analyze high-resolution X-ray spectra of O-type stars with a multi-temperature plasma model in order to determine crucial stellar and wind parameters such as the mass-loss rate, the CNO abundances, and the X-ray temperature plasma distribution in the wind. In this context we are developing a modeling tool to calculate synthetic X-ray spectra. We present here the main ingredients and physics necessary for such a work. Our code uses the most recent version of the AtomDB emissivities to compute the intrinsic emissivity of the hot plasma as well as the CMFGEN model atmosphere code to evaluate the opacity of the cool wind. Following the comparison between two formalisms of stellar wind fragmentation, we introduce, for the first time in X-rays, the effects of a tenuous inter-clump medium. We then explore the quantitative impact of different model parameters on the X-ray spectra such as the position in the wind of the X-ray emitting plasma. For the first time, we also show that the two formalisms of stellar wind fragmentation yield different results, although the differences for individual lines are small and can probably not be tested with the current generation of X-ray telescopes. As an illustration of our method, we compare various synthetic line profiles to the observed OVIII lambda 18.97 line in the spectrum of zeta Puppis. We illustrate how different combinations of parameters can actually lead to the same morphology of a single line, underlining the need to analyze the whole spectrum in a consistent way when attempting to constrain the parameters of the wind. C1 [Herve, A.; Rauw, G.; Naze, Y.] Univ Liege, Dept AGO, GAPHE, B-4000 Liege, Belgium. [Foster, A.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Herve, A (reprint author), Univ Liege, Dept AGO, GAPHE, Allee 6 Aout 17,Bat B5C, B-4000 Liege, Belgium. EM herve@astro.ulg.ac.be; afoster@cfa.harvard.edu OI Naze, Yael/0000-0003-4071-9346 FU FNRS ( Belgium); Communaute Francaise de Belgique-Action de recherche concertee (ARC)-Academie Wallonie-Europe; XMM+INTEGRAL PRODEX (Belspo) FX This research is supported by the FNRS (Belgium) and the Communaute Francaise de Belgique-Action de recherche concertee (ARC)-Academie Wallonie-Europe and an XMM+INTEGRAL PRODEX contract (Belspo). NR 27 TC 13 Z9 13 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD APR 1 PY 2012 VL 748 IS 2 AR 89 DI 10.1088/0004-637X/748/2/89 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 916WZ UT WOS:000302135200017 ER PT J AU Marinucci, A Bianchi, S Nicastro, F Matt, G Goulding, AD AF Marinucci, Andrea Bianchi, Stefano Nicastro, Fabrizio Matt, Giorgio Goulding, Andy D. TI THE LINK BETWEEN THE HIDDEN BROAD LINE REGION AND THE ACCRETION RATE IN SEYFERT 2 GALAXIES SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: active; galaxies: Seyfert ID ACTIVE GALACTIC NUCLEI; X-RAY-ABSORPTION; XMM-NEWTON; MU-M; NEARBY GALAXIES; BLACK-HOLES; VELOCITY DISPERSIONS; ENERGY-DISTRIBUTIONS; GASEOUS KINEMATICS; COMPLETE CENSUS AB In the past few years, more and more pieces of evidence have been presented for a revision of the widely accepted unified model of active galactic nuclei. A model based solely on orientation cannot explain all the observed phenomenology. In the following, we will present evidence that accretion rate is also a key parameter for the presence of hidden broad line regions (HBLRs) in Seyfert 2 galaxies. Our sample consists of 21 sources with polarized hidden broad lines and 18 sources without hidden broad lines. We use stellar velocity dispersions from several studies on the Ca II and Mg b triplets in Seyfert 2 galaxies to estimate the mass of the central black holes via the M-BH-sigma(*) relation. The ratio between the bolometric luminosity, derived from the intrinsic (i.e., unabsorbed) X-ray luminosity, and the Eddington luminosity is a measure of the rate at which matter accretes onto the central supermassive black hole. A separation between Compton-thin HBLR and non-HBLR sources is clear, both in accretion rate (log L-bol/L-Edd = -1.9) and in luminosity (log L-bol = 43.90). When properly luminosity-corrected Compton-thick sources are included, the separation between HBLR and non-HBLR is less sharp but no HBLR source falls below the Eddington ratio threshold. We speculate that non-HBLR Compton-thick sources with accretion rate higher than the threshold do possess a BLR, but something, probably related to their heavy absorption, is preventing us from observing it even in polarized light. Our results for Compton-thin sources support theoretical expectations. In a model presented by Nicastro, the presence of broad emission lines is intrinsically connected with disk instabilities occurring in proximity of a transition radius, which is a function of the accretion rate, becoming smaller than the innermost stable orbit for very low accretion rates and therefore luminosities. C1 [Marinucci, Andrea; Bianchi, Stefano; Matt, Giorgio] Univ Roma Tre, Dipartimento Fis, I-00146 Rome, Italy. [Marinucci, Andrea; Nicastro, Fabrizio; Goulding, Andy D.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Bianchi, Stefano] INAF Osservatorio Astron Brera, I-23807 Merate, Italy. [Bianchi, Stefano; Nicastro, Fabrizio] Fdn Res & Technol, IESL, Iraklion 71110, Crete, Greece. [Nicastro, Fabrizio] Osservatorio Astron Roma INAF, I-00040 Monte Porzio Catone, Italy. RP Marinucci, A (reprint author), Univ Roma Tre, Dipartimento Fis, Via Vasca Navale 84, I-00146 Rome, Italy. RI Bianchi, Stefano/B-4804-2010; OI Bianchi, Stefano/0000-0002-4622-4240; Nicastro, Fabrizio/0000-0002-6896-1364 FU ASI [I/088/06/0]; NASA [NNG04GD49G, NNX11AD16G] FX A.M., S.B., and G.M. acknowledge financial support from ASI under grant I/088/06/0. F.N. acknowledges financial support from ASI grants AAE and ADAE, as well as NASA grant NNG04GD49G. A. M. and F.N. acknowledge support from NASA grant NNX11AD16G. We thank M. Elvis for useful advices and discussions. We thank the anonymous referee for his/her important comments that greatly improved this work. NR 77 TC 38 Z9 38 U1 0 U2 6 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD APR 1 PY 2012 VL 748 IS 2 AR 130 DI 10.1088/0004-637X/748/2/130 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 916WZ UT WOS:000302135200058 ER PT J AU Maruca, BA Kasper, JC Gary, SP AF Maruca, Bennett A. Kasper, Justin C. Gary, S. Peter TI INSTABILITY-DRIVEN LIMITS ON HELIUM TEMPERATURE ANISOTROPY IN THE SOLAR WIND: OBSERVATIONS AND LINEAR VLASOV ANALYSIS SO ASTROPHYSICAL JOURNAL LA English DT Article DE instabilities; plasmas; solar wind ID HYBRID SIMULATIONS; PROTON; MAGNETOSHEATH; CONSTRAINTS; PARALLEL; VELOCITY AB Kinetic microinstabilities in the solar wind arise when the plasma deviates too far from thermal equilibrium. Previously published work has provided strong evidence that the cyclotron, mirror, and parallel and oblique firehose instabilities limit proton (i.e., ionized hydrogen) temperature anisotropy. However, few studies have thoroughly explored whether a less-abundant ion species can also trigger these instabilities. This study considered the possibility of similar instability-driven limits on alpha-particle (i.e., fully ionized helium) temperature anisotropy. Linear Vlasov analysis was used to derive the expected threshold conditions for instabilities driven by alpha-particle temperature anisotropy. Measurements in situ of alpha-particle temperature anisotropy from the Wind spacecraft's Faraday cups were found to be consistent with the limits imposed by these instability thresholds. This strongly suggests that alpha-particles, which only constitute similar to 5% of ions in the solar wind, can drive an instability if their temperature anisotropy becomes sufficiently extreme. C1 [Maruca, Bennett A.; Kasper, Justin C.] Harvard Univ, Dept Astron, Cambridge, MA 02138 USA. [Maruca, Bennett A.; Kasper, Justin C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Gary, S. Peter] Los Alamos Natl Lab, Los Alamos, NM 87545 USA. RP Maruca, BA (reprint author), Harvard Univ, Dept Astron, Cambridge, MA 02138 USA. EM bmaruca@cfa.harvard.edu RI Kasper, Justin/D-1152-2010 OI Kasper, Justin/0000-0002-7077-930X FU NASA [NNX08AW07G] FX The authors gratefully acknowledge A. Szabo for his assistance with the Wind/MFI data and thank S. R. Cranmer, D. P. Finkbeiner, A. J. Lazarus, J. M. Moran, J. C. Raymond, and M. L. Stevens for their feedback on this work. Analysis of the Wind/SWE observations at SAO is supported by the NASA grant NNX08AW07G. This research has made use of the SAO/NASA Astrophysics Data System (ADS). NR 28 TC 53 Z9 53 U1 1 U2 11 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD APR 1 PY 2012 VL 748 IS 2 AR 137 DI 10.1088/0004-637X/748/2/137 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 916WZ UT WOS:000302135200065 ER PT J AU Park, S Hughes, JP Slane, PO Burrows, DN Lee, JJ Mori, K AF Park, Sangwook Hughes, John P. Slane, Patrick O. Burrows, David N. Lee, Jae-Joon Mori, Koji TI AN X-RAY STUDY OF SUPERNOVA REMNANT N49 AND SOFT GAMMA-RAY REPEATER 0526-66 IN THE LARGE MAGELLANIC CLOUD SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM: individual objects (N49); ISM: supernova remnants; stars: individual (SGR 0526); stars: magnetars; X-rays: ISM; X-rays: stars ID XMM-NEWTON OBSERVATIONS; HEAVY-ELEMENTS; IA SUPERNOVAE; RICH EJECTA; NUCLEOSYNTHESIS; EMISSION; ABUNDANCES; SPECTROSCOPY; MULTIWAVELENGTH; SGR-0526-66 AB We report on the results from our deep Chandra observation (120 ks) of the supernova remnant (SNR) N49 and soft gamma-ray repeater (SGR) 0526-66 in the Large Magellanic Cloud. We firmly establish the detection of an ejecta "bullet" beyond the southwestern boundary of N49. The X-ray spectrum of the bullet is distinguished from that of the main SNR shell, showing significantly enhanced Si and S abundances. We also detect an ejecta feature in the eastern shell, which shows metal overabundances similar to those of the bullet. If N49 was produced by a core-collapse explosion of a massive star, the detected Si-rich ejecta may represent explosive O-burning or incomplete Si-burning products from deep interior of the SN. On the other hand, the observed Si/S abundance ratio in the ejecta may favor Type Ia origin for N49. We refine the Sedov age of N49, tau(Sed) similar to 4800 yr, with the explosion energy E-0 similar to 1.8 x 10(51) erg. Our blackbody (BB) + power law (PL) model for the quiescent X-ray emission from SGR 0526-66 indicates that the PL photon index (Gamma similar to 2.5) is identical to that of PSR 1E1048.1-5937, the well-known candidate transition object between anomalous X-ray pulsars and SGRs. Alternatively, the two-component BB model implies X-ray emission from a small (R similar to 1 km) hot spot(s) (kT similar to 1 keV) in addition to emission from the neutron star's cooler surface (R similar to 10 km, kT similar to 0.4 keV). There is a considerable discrepancy in the estimated column toward 0526-66 between BB+PL and BB+BB model fits. Discriminating these spectral models would be crucial to test the long-debated physical association between N49 and 0526-66. C1 [Park, Sangwook] Univ Texas Arlington, Dept Phys, Arlington, TX 76019 USA. [Hughes, John P.] Rutgers State Univ, Dept Phys & Astron, Piscataway, NJ 08854 USA. [Slane, Patrick O.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Burrows, David N.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Lee, Jae-Joon] Korea Astron & Space Sci Inst, Taejon 305348, South Korea. [Mori, Koji] Miyazaki Univ, Dept Appl Phys, Miyazaki 8892192, Japan. RP Park, S (reprint author), Univ Texas Arlington, Dept Phys, Box 19059, Arlington, TX 76019 USA. EM s.park@uta.edu FU SAO [GO9-0072A]; [GO9-0072X]; [GO0-11090X] FX This work has been supported in part by the SAO under the Chandra grants GO9-0072A to the University of Texas at Arlington, and GO9-0072X to the Pennsylvania State University. J.P.H. has been supported in part by the Chandra grant GO0-11090X. NR 50 TC 25 Z9 25 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD APR 1 PY 2012 VL 748 IS 2 AR 117 DI 10.1088/0004-637X/748/2/117 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 916WZ UT WOS:000302135200045 ER PT J AU Shen, Y Menard, B AF Shen, Yue Menard, Brice TI ON THE LINK BETWEEN ASSOCIATED Mg II ABSORBERS AND STAR FORMATION IN QUASAR HOSTS SO ASTROPHYSICAL JOURNAL LA English DT Article DE black hole physics; galaxies: active; quasars: absorption lines; quasars: general ID DIGITAL SKY SURVEY; SUPERMASSIVE BLACK-HOLES; ULTRALUMINOUS INFRARED GALAXIES; LENS SYSTEM RXS-J1131-1231; ABSORPTION-LINES; REDDENED QUASARS; STELLAR OBJECTS; DATA RELEASE; EMISSION; REDSHIFT AB A few percent of quasars show strong associated Mg II absorption, with velocities (v(off)) lying within a few thousand km s(-1) from the quasar systemic redshift. These associated absorption line (AAL) systems are usually interpreted as absorbers that are either intrinsic to the quasar and its host, or arising from external galaxies clustering around the quasar. Using composite spectra of similar to 1800 Mg II AAL quasars selected from SDSS DR7 at 0.4 less than or similar to z <= 2, we show that quasars with AALs with v(off) < 1500 km s(-1) have a prominent excess in [O II] lambda 3727 emission (detected at >7 sigma) at rest relative to the quasar host, compared to unabsorbed quasars. We interpret this [O II] excess as due to enhanced star formation in the quasar host. Our results suggest that a significant fraction of AALs with voff < 1500 km s(-1) are physically associated with the quasar and its host. AAL quasars also have dust reddening lying between normal quasars and the so-called dust-reddened quasars. We suggest that the unique properties of AAL quasars can be explained if they are the transitional population from heavily dust-reddened quasars to normal quasars in the formation process of quasars and their hosts. This scenario predicts a larger fraction of young bulges, disturbed morphologies, and interactions of AAL quasar hosts compared to normal quasars. The intrinsic link between associated absorbers and quasar hosts opens a new window to probe massive galaxy formation and galactic-scale feedback processes, and provides a crucial test of the evolutionary picture of quasars. C1 [Shen, Yue] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Menard, Brice] Univ Toronto, CITA, Toronto, ON M5S 3H8, Canada. [Menard, Brice] Univ Tokyo, Inst Cosm Ray Res, Kashiwa, Chiba 2778582, Japan. [Menard, Brice] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. RP Shen, Y (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS-51, Cambridge, MA 02138 USA. EM yshen@cfa.harvard.edu; menard@pha.jhu.edu FU Alfred P. Sloan Foundation; National Science Foundation; U.S. Department of Energy; National Aeronautics and Space Administration; Japanese Monbukagakusho; Max Planck Society; Higher Education Funding Council for England; Smithsonian Astrophysical Observatory (SAO) FX Funding for the SDSS and SDSS-II has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, the U.S. Department of Energy, the National Aeronautics and Space Administration, the Japanese Monbukagakusho, the Max Planck Society, and the Higher Education Funding Council for England. The SDSS Web site is http://www.sdss.org/.; We thank the anonymous referee for suggestions that led to the improvement of the manuscript. We also thank Michael Strauss, Tim Heckman, Gordon Richards, Norm Murray, Martin Elvis, and Yuval Birnboim for useful discussions. Y.S. acknowledges support from the Smithsonian Astrophysical Observatory (SAO) through a Clay Postdoctoral Fellowship. NR 43 TC 18 Z9 18 U1 0 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD APR 1 PY 2012 VL 748 IS 2 AR 131 DI 10.1088/0004-637X/748/2/131 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 916WZ UT WOS:000302135200059 ER PT J AU Young, M Brandt, WN Xue, YQ Paolillo, M Alexander, DM Bauer, FE Lehmer, BD Luo, B Shemmer, O Schneider, DP Vignali, C AF Young, M. Brandt, W. N. Xue, Y. Q. Paolillo, M. Alexander, D. M. Bauer, F. E. Lehmer, B. D. Luo, B. Shemmer, O. Schneider, D. P. Vignali, C. TI VARIABILITY-SELECTED LOW-LUMINOSITY ACTIVE GALACTIC NUCLEI IN THE 4 Ms CHANDRA DEEP FIELD-SOUTH SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: active; X-rays: galaxies ID X-RAY VARIABILITY; BLACK-HOLE MASS; SPECTRAL ENERGY-DISTRIBUTIONS; XMM-NEWTON OBSERVATION; SEYFERT 1 GALAXIES; YALE-CHILE MUSYC; STELLAR-MASS; OPTICAL SPECTROSCOPY; HOST GALAXIES; MULTIWAVELENGTH SURVEY AB The 4 Ms Chandra Deep Field-South (CDF-S) and other deep X-ray surveys have been highly effective at selecting active galactic nuclei (AGNs). However, cosmologically distant low-luminosity AGNs (LLAGNs) have remained a challenge to identify due to significant contribution from the host galaxy. We identify long-term X-ray variability (similar to month-years, observed frame) in 20 of 92 CDF-S galaxies spanning redshifts z approximate to 0.08-1.02 that do not meet other AGN selection criteria. We show that the observed variability cannot be explained by X-ray binary populations or ultraluminous X-ray sources, so the variability is most likely caused by accretion onto a supermassive black hole (SMBH). The variable galaxies are not heavily obscured in general, with a stacked effective power-law photon index of Gamma(stack) approximate to 1.93 +/- 0.13, and are therefore likely LLAGNs. The LLAGNs tend to lie a factor of approximate to 6-80 below the extrapolated linear variability-luminosity relation measured for luminous AGNs. This may be explained by their lower accretion rates. Variability-independent black hole mass and accretion-rate estimates for variable galaxies show that they sample a significantly different black hole mass-accretion-rate space, with masses a factor of 2.4 lower and accretion rates a factor of 22.5 lower than variable luminous AGNs at the same redshift. We find that an empirical model based on a universal broken power-law power spectral density function, where the break frequency depends on SMBH mass and accretion rate, roughly reproduces the shape, but not the normalization, of the variability-luminosity trends measured for variable galaxies and more luminous AGNs. C1 [Young, M.; Brandt, W. N.; Xue, Y. Q.; Schneider, D. P.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Young, M.; Brandt, W. N.; Xue, Y. Q.; Schneider, D. P.] Penn State Univ, Inst Gravitat & Cosmos, University Pk, PA 16802 USA. [Paolillo, M.] Univ Naples Federico 2, Dipartimento Sci Fis, I-80126 Naples, Italy. [Alexander, D. M.] Univ Durham, Dept Phys, Durham DH1 3LE, England. [Bauer, F. E.] Pontificia Univ Catolica Chile, Dept Astron & Astrofis, Santiago 22, Chile. [Bauer, F. E.] Space Sci Inst, Boulder, CO 80301 USA. [Lehmer, B. D.] Johns Hopkins Univ, Baltimore, MD 21218 USA. [Lehmer, B. D.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Luo, B.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Shemmer, O.] Univ N Texas, Dept Phys, Denton, TX 76203 USA. [Vignali, C.] Univ Bologna, Dipartimento Astron, I-40127 Bologna, Italy. RP Young, M (reprint author), Penn State Univ, Dept Astron & Astrophys, 525 Davey Lab, University Pk, PA 16802 USA. RI Paolillo, Maurizio/J-1733-2012; Vignali, Cristian/J-4974-2012; Brandt, William/N-2844-2015; OI Paolillo, Maurizio/0000-0003-4210-7693; Vignali, Cristian/0000-0002-8853-9611; Brandt, William/0000-0002-0167-2453; Shemmer, Ohad/0000-0003-4327-1460; Alexander, David/0000-0002-5896-6313 FU NASA ADP [NNX10AC99G]; Chandra X-ray Center [SP1-12007A]; Italian MIUR; Programa de Financiamiento Basal; CONICYT-Chile [FONDECYT 1101024, ALMA-CONICYT 31100004, FONDAP-CATA 15010003]; Einstein Fellowship Program; Science and Technology Facilities Council (STFC) FX We thank P. Uttley, E. Feigelson, and C. Saez for helpful discussions on variability statistics. We also thank M. Gilfanov for helpful discussions regarding XRB variability. We thank the referee for constructive comments. We acknowledge the financial support of NASA ADP grant NNX10AC99G (M.Y., W.N.B., and Y.Q.X.) and Chandra X-ray Center grant SP1-12007A (W.N.B. and Y.Q.X.). M. P. acknowledges support from PRIN-2009 by the Italian MIUR. F. E. B. acknowledges support from Programa de Financiamiento Basal and CONICYT-Chile under grants FONDECYT 1101024, ALMA-CONICYT 31100004, and FONDAP-CATA 15010003. B. D. L. acknowledges financial support provided by the Einstein Fellowship Program. D. M. A. thanks the Science and Technology Facilities Council (STFC) for support. NR 116 TC 25 Z9 25 U1 0 U2 6 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD APR 1 PY 2012 VL 748 IS 2 AR 124 DI 10.1088/0004-637X/748/2/124 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 916WZ UT WOS:000302135200052 ER PT J AU Barrette, MF Monfort, SL Festa-Bianchet, M Clutton-Brock, TH Russell, AF AF Barrette, Marie-France Monfort, Steven L. Festa-Bianchet, Marco Clutton-Brock, Tim H. Russell, Andrew F. TI Reproductive rate, not dominance status, affects fecal glucocorticoid levels in breeding female meerkats SO HORMONES AND BEHAVIOR LA English DT Article DE Adrenal activity; Corticosterone; Non-invasive; Cooperative breeding; Social status; Reproductive suppression; Reproductive self-restraint; Gestation; Lactation ID PITUITARY-ADRENAL AXIS; MATERNAL CORTICOSTERONE TREATMENT; SURICATA-SURICATTA; STRESS RESPONSES; LATE PREGNANCY; SUPPRESSION; SURVIVAL; BEHAVIOR; HORMONES; COOPERATION AB Glucocorticoid hormones (GCs) have been studied intensively to understand the associations between physiological stress and reproductive skew in animal societies. However, we have little appreciation of the range of either natural levels within and among individuals, or the associations among dominance status, reproductive rate and GCs levels during breeding. To address these shortcomings, we examined varation in fecal glucocorticoid metabolites (fGC) during breeding periods in free-ranging female meerkats (Suricata suricatta) over 11 years. The vast majority of variation in fGC levels was found within breeding events by the same female (similar to 87%), with the remaining variation arising among breeding events and among females. Concentrations of fGC generally tripled as pregnancy progressed. However, females with a high reproductive rate, defined as those conceiving within a month following parturition (mean = 9 days postpartum), showed significant reductions in fGC in the final 2 weeks before parturition. Despite these reductions, females with a high reproductive rate had higher fGC levels at conception of the following litter than those breeding at a low rate. After controlling for the higher reproductive rate of dominants, we found no association between levels of fGC and either age or dominance status. Our results suggest that one should be cautious about interpreting associations between dominance status, reproductive skew and GCs levels, without knowledge of the natural variation in GCs levels within and among females. (C) 2011 Published by Elsevier Inc. C1 [Barrette, Marie-France; Festa-Bianchet, Marco] Univ Sherbrooke, Dept Biol, Sherbrooke, PQ J1K 2R1, Canada. [Barrette, Marie-France; Monfort, Steven L.] Smithsonian Conservat Biol Inst, Front Royal, VA 22630 USA. [Clutton-Brock, Tim H.] Univ Cambridge, Dept Zool, Cambridge CB2 3EJ, England. [Russell, Andrew F.] Univ Exeter, Coll Life & Environm Sci, Ctr Ecol & Conservat, Penryn TR10 9EZ, Cornwall, England. [Russell, Andrew F.] CNRS Moulis, La Stn Ecol Expt, F-09200 Moulis, France. RP Barrette, MF (reprint author), Univ Sherbrooke, Dept Biol, Sherbrooke, PQ J1K 2R1, Canada. EM m-f.barrette@usherbrooke.ca OI Festa-Bianchet, Marco/0000-0002-2352-3379 FU Natural Sciences and Engineering Council of Canada; Smithsonian Institution; Natural Environmental Research Council; Royal Society FX We are grateful to all field volunteers, project managers and graduate students who made this study possible by collecting data and fecal samples from 1997 to 2008. We thank: the Kotze family and Northern Cape Conservation for allowing us to conduct research in the Kalahari; N. Bennett and M. Haupt at the University of Pretoria and L Morse at the Smithsonian Institution for their logistic support in exporting and importing fecal samples from South Africa to the USA; A. Young, M. Szykman Gunther, J. Brown, D. Kersey and N. Presley for guidance with endocrine analyses; and B. Shipley, J. Martin and F. Pelletier for statistical help. Constructive comments from two anonymous reviewers substantially improved the manuscript. This research was funded by the Natural Sciences and Engineering Council of Canada (M-FB), the Smithsonian Institution (M-FB and SM), the Natural Environmental Research Council (TCB) and the Royal Society University Research Fellowship scheme (AFR). NR 68 TC 4 Z9 4 U1 4 U2 26 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0018-506X J9 HORM BEHAV JI Horm. Behav. PD APR PY 2012 VL 61 IS 4 BP 463 EP 471 DI 10.1016/j.yhbeh.2011.12.005 PG 9 WC Behavioral Sciences; Endocrinology & Metabolism SC Behavioral Sciences; Endocrinology & Metabolism GA 925LW UT WOS:000302763700001 PM 22210199 ER PT J AU Jung, K Kaiser, S Bohm, S Nieschulze, J Kalko, EKV AF Jung, Kirsten Kaiser, Sonja Boehm, Stefan Nieschulze, Jens Kalko, Elisabeth K. V. TI Moving in three dimensions: effects of structural complexity on occurrence and activity of insectivorous bats in managed forest stands SO JOURNAL OF APPLIED ECOLOGY LA English DT Article DE bats; Chiroptera; conservation; forest management; LiDAR; forest structure; three-dimensional structure ID PIPISTRELLUS-PIPISTRELLUS; ECHOLOCATION CALLS; SPECIES-DIVERSITY; TROPICAL FOREST; AIRBORNE LIDAR; PREDATION RISK; BOREAL FOREST; CONSERVATION; BIODIVERSITY; VEGETATION AB 1. Forest management determines to a large degree the three-dimensional arrangement of the vegetation in production forest systems and hence has an essential influence on habitat quality for wildlife. We investigated the effects of forest structure on occurrence, activity and species composition of European bats, an ecologically important group of vertebrates known to be affected by the physical clutter of vegetation. 2. Species composition and activity of bats were assessed with acoustic monitoring on 50 one-hectare experimental plots in a biosphere reserve in Germany. Three-dimensional forest structure was assessed by Light Detection and Ranging (LiDAR), and a set of 20 mathematically derived and fine-grained structural parameters with a minimum of collinearity was used for a quantitative description of the vegetation structure. 3. Occurrence and activity of bats were positively associated with the structural parameters canopy height, standard deviation of the canopy surface roughness and edge fraction, indicating older forest stands with patches of different vegetation heights. In addition, species composition in differently managed forest stands was significantly influenced by the relative proportion of structural parameters. Species of one functional group, sharing similar adaptations in wing morphology and foraging strategy, showed similar associations with three-dimensional structural parameters. In addition, we found species-specific structural parameter associations explaining the occurrence and activity levels of individual species in differently managed production forest types. 4. Synthesis and applications. High-resolution LiDAR data are an important tool to assess structural habitat suitability for bat species. Our data revealed that bat occurrence and activity increases with structural heterogeneity in managed forest stands. Given, that bats provide an essential ecosystem service through top-down control of herbivorous insects, increasing stand structural heterogeneity through management practices (e. g. selective harvesting) is a very effective strategy to assure vital ecosystem functioning in production forest systems. C1 [Jung, Kirsten; Boehm, Stefan; Kalko, Elisabeth K. V.] Univ Ulm, Inst Expt Ecol, D-89069 Ulm, Germany. [Kaiser, Sonja; Nieschulze, Jens] Max Planck Inst Biogeochem, D-07745 Jena, Germany. [Kalko, Elisabeth K. V.] Smithsonian Trop Res Inst, Balboa, Panama. RP Jung, K (reprint author), Univ Ulm, Inst Expt Ecol, Albert Einstein Allee 11, D-89069 Ulm, Germany. EM kirsten.jung@uni-ulm.de OI Nieschulze, Jens/0000-0001-7535-6253 FU DFG [1374, P 3141044]; MPI in Jena FX This work was funded by the DFG Priority Program 1374 'Infrastructure-Biodiversity-Exploratories' (P 3141044) and the MPI in Jena. Field work permits were given by the state of Brandenburg (according to 72 BbgNatSchG). We are very grateful for the logistic support of the management team Schorfheide-Chorin, especially U. Pommer and U. Schumacher. We thank R. Zimmermann, A. Borner & E. D. Schulze for providing the vertical transect section (Fig. 1). We cordially thank E. D. Schulze for his support and valuable comments which considerably helped to improve this manuscript. We thank M. Helbig for her commitment during field work and for acoustic data analysis. We also thank K. Wells, J. Hailer and I. Geipel for various scientific discussions. NR 64 TC 61 Z9 61 U1 6 U2 118 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0021-8901 J9 J APPL ECOL JI J. Appl. Ecol. PD APR PY 2012 VL 49 IS 2 BP 523 EP 531 DI 10.1111/j.1365-2664.2012.02116.x PG 9 WC Biodiversity Conservation; Ecology SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 916BF UT WOS:000302070900025 ER PT J AU Hummer, DR Heaney, PJ Post, JE AF Hummer, Daniel R. Heaney, Peter J. Post, Jeffrey E. TI In situ observations of particle size evolution during the hydrothermal crystallization or TiO2: A time-resolved synchrotron SAXS and WAXS study SO JOURNAL OF CRYSTAL GROWTH LA English DT Article DE Hydrothermal crystal growth; SAXS; WAXS; Nanomaterials; Oxides; Titanium compounds ID X-RAY-SCATTERING; SMALL-ANGLE; NANOCRYSTALLINE TIO2; PHASE-STABILITY; CRYSTAL-GROWTH; SUPERCRITICAL WATER; LIGHT-SCATTERING; SOLAR-CELLS; ZEOLITE-A; NANOPARTICLES AB We have monitored the homogeneous crystallization of TiO2 phases from aqueous TiCl4 solutions at 100 degrees C using both time-resolved small-angle X-ray scattering (TR-SAXS) and time-resolved wide-angle X-ray scattering (TR-WAXS). The WAXS data revealed that metastable anatase was the first phase to crystallize, but it began transforming to rutile within the first hour of reaction. Scherrer analysis of WAXS peak widths indicated that anatase particles grew to an average size near 7 nm on a time scale of minutes, after which their size remained static, while rutile grew rapidly from <3 nm to similar to 10 nm within 1 h, followed by slower growth at a rate of similar to 0.15 nm/h. Using a novel sample cell designed to withstand temperatures up to 150 degrees C and hydrothermal vapor pressure, we collected in situ SAXS data for the same conditions as the WAXS experiments. Fourier analyses of the SAXS images revealed the rapid emergence of a broad, Gaussian-type particle size distribution ranging in diameter from 1 to similar to 20 nm with a mean near 7 nm, in excellent agreement with our WAXS analysis. At 0.5 h, a second population of <3 nm particles emerged, and these crystals grew to similar to 9 nm after 7.5 h, which we interpret as the nucleation and growth of rutile (as was also observed in the WAXS patterns). In contrast to studies that presume a solid-state transformation from anatase to rutile during growth, our results suggest that anatase and rutile co-precipitate during the early stages of crystallization, but once anatase crystals grow to a critical size of 7 nm, they dissolve and the solution species re-precipitate onto primary rutile nanocrystals. (C) 2012 Elsevier By. All rights reserved. C1 [Hummer, Daniel R.; Heaney, Peter J.] Penn State Univ, Dept Geosci, University Pk, PA 16802 USA. [Post, Jeffrey E.] Smithsonian Inst, Dept Mineral Sci, Washington, DC 20013 USA. RP Hummer, DR (reprint author), Carnegie Inst Washington, Geophys Lab, 5251 Broad Branch Rd NW, Washington, DC 20015 USA. EM dhummer@ciw.edu FU US Department of Energy, Office of Science. Office of Basic Energy Sciences [DE-AC02-98CH10886]; National Science Foundation [EAR04-17714, EAR07-45374]; Center for Environmental Kinetics Analysis (CEKA); NSF [CHE-0431328]; DOE FX We thank John Pople, Tom Hostettler, Cathie Condron, Kristina Peterson, and Paul Davis for valuable assistance with instrumentation and equipment at beamline 1-4 of SSRL. We also thank Mike Toney, Glenn Waychunas, Young-Shin Jun, and Mark Angelone for helpful conversations and advice regarding data reduction and analysis. We thank Alice Donahlkova for assistance with the TEM imaging. Use of the National Synchrotron Light Source, Brookhaven National Laboratory, was supported by the US Department of Energy, Office of Science. Office of Basic Energy Sciences, under contract no. DE-AC02-98CH10886. Portions of this research were carried out at the Stanford Synchrotron Radiation Light Source, a national user facility operated by Stanford University on behalf of the US Department of Energy. Office of Basic Energy Sciences. This work was made possible by National Science Foundation Grant nos. EAR04-17714 and EAR07-45374, and by the Center for Environmental Kinetics Analysis (CEKA), an NSF- and DOE-sponsored Environmental Molecular Science Institute (NSF CHE-0431328). NR 53 TC 11 Z9 12 U1 3 U2 50 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0022-0248 J9 J CRYST GROWTH JI J. Cryst. Growth PD APR 1 PY 2012 VL 344 IS 1 BP 51 EP 58 DI 10.1016/j.jcrysgro.2012.01.044 PG 8 WC Crystallography; Materials Science, Multidisciplinary; Physics, Applied SC Crystallography; Materials Science; Physics GA 921RH UT WOS:000302494400009 ER PT J AU Lacy, RC Ballou, JD Pollak, JP AF Lacy, Robert C. Ballou, Jonathan D. Pollak, John P. TI PMx: software package for demographic and genetic analysis and management of pedigreed populations SO METHODS IN ECOLOGY AND EVOLUTION LA English DT Article DE conservation breeding; conservation genetics; demographic analysis; pedigree analysis; population management; population modelling ID MINIMIZATION AB 1. The concepts and algorithms for demographic and genetic analysis of pedigreed populations have been evolving rapidly in recent years. 2. The PMx software brings together into one integrated package a number of tools for pedigree analysis, including methods for dealing with missing, uncertain and probabilistic data not previously available in distributed software. 3. PMx provides tools for optimal demographic and genetic management of populations of wildlife species, rare domestic breeds, and other populations for which the primary goal is to conserve genetic diversity, and it is being implemented as the primary pedigree management tool for the breeding programmes of zoo associations around the world. 4. PMx can be used to characterize the demography and genetics of any captive or wild population for which pedigree and life-history data are available. C1 [Lacy, Robert C.] Chicago Zool Soc, Brookfield, IL 60513 USA. [Ballou, Jonathan D.] Smithsonian Conservat Biol Inst, Washington, DC 20008 USA. [Pollak, John P.] Cornell Univ, Ithaca, NY 14853 USA. RP Lacy, RC (reprint author), Chicago Zool Soc, Brookfield, IL 60513 USA. EM rlacy@ix.netcom.com FU Institute of Museum and Library Services, Association of Zoos and Aquariums (AZA); Chicago Zoological Society; Smithsonian Institution/National Zoological Park FX PMx benefited from input and testing by a large number of colleagues, including Rajan Amin, Laurie Bingaman Lackey, Lisa Faust, Jamie Ivy, Kristin Leus, Sarah Long, Colleen Lynch, Jennifer Mickelberg, Kanako Nishimoto, Paul Pearce-Kelly, Kristine Schad and Kathy Traylor-Holzer. PMx was developed with support from the Institute of Museum and Library Services, Association of Zoos and Aquariums (AZA), Chicago Zoological Society and Smithsonian Institution/National Zoological Park. NR 26 TC 14 Z9 16 U1 1 U2 23 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 2041-210X J9 METHODS ECOL EVOL JI Methods Ecol. Evol. PD APR PY 2012 VL 3 IS 2 BP 433 EP 437 DI 10.1111/j.2041-210X.2011.00148.x PG 5 WC Ecology SC Environmental Sciences & Ecology GA 922HR UT WOS:000302538500024 ER PT J AU Churazov, E Vikhlinin, A Zhuravleva, I Schekochihin, A Parrish, I Sunyaev, R Forman, W Bohringer, H Randall, S AF Churazov, E. Vikhlinin, A. Zhuravleva, I. Schekochihin, A. Parrish, I. Sunyaev, R. Forman, W. Boehringer, H. Randall, S. TI X-ray surface brightness and gas density fluctuations in the Coma cluster SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE turbulence; galaxies: clusters: general; galaxies: clusters: intracluster medium; galaxies: individual: Coma cluster; X-rays: galaxies: clusters ID GALAXY CLUSTER; TURBULENCE; PROFILES; CORE AB X-ray surface brightness fluctuations in the core (650 x 650 kpc) region of the Coma cluster observed with XMM-Newton and Chandra are analysed using a 2D power spectrum approach. The resulting 2D spectra are converted to 3D power spectra of gas density fluctuations. Our independent analyses of the XMM-Newton and Chandra observations are in excellent agreement and provide the most sensitive measurements of surface brightness and density fluctuations for a hot cluster. We find that the characteristic amplitude of the volume filling density fluctuations relative to the smooth underlying density distribution varies from 7-10 per cent on scales of similar to 500 kpc down to similar to 5 per cent on scales of similar to 30 kpc. On smaller spatial scales, projection effects smear the density fluctuations by a large factor, precluding strong limits on the fluctuations in 3D. On the largest scales probed (hundreds of kpc), the dominant contributions to the observed fluctuations most likely arise from perturbations of the gravitational potential by the two most massive galaxies in Coma, NGC4874 and NGC4889, and the low-entropy gas brought to the cluster by an infalling group. Other plausible sources of X-ray surface brightness fluctuations are discussed, including turbulence, metal abundance variations and unresolved sources. Despite a variety of possible origins for density fluctuations, the gas in the Coma cluster core is remarkably homogeneous on scales from similar to 500 to similar to 30 kpc. C1 [Churazov, E.; Zhuravleva, I.; Sunyaev, R.] Max Planck Inst Astrophys, D-85741 Garching, Germany. [Churazov, E.; Vikhlinin, A.; Sunyaev, R.] Space Res Inst IKI, Moscow 117997, Russia. [Vikhlinin, A.; Forman, W.; Randall, S.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Schekochihin, A.] Univ Oxford, Rudolf Peierls Ctr Theoret Phys, Oxford OX1 3NP, England. [Parrish, I.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Parrish, I.] Univ Calif Berkeley, Theoret Astrophys Ctr, Berkeley, CA 94720 USA. [Boehringer, H.] MPI Extraterr Phys, D-85740 Garching, Germany. RP Churazov, E (reprint author), Max Planck Inst Astrophys, Karl Schwarzschild Str 1, D-85741 Garching, Germany. EM churazov@mpa-garching.mpg.de RI Churazov, Eugene/A-7783-2013; OI Randall, Scott/0000-0002-3984-4337; Forman, William/0000-0002-9478-1682 FU Leverhulme Trust Network for Magnetized Plasma Turbulence; STFC [ST/F002505/2]; Division of Physical Sciences of the RAS [OFN-16]; Chandra X-ray Center through NASA [NAS8-03060]; Smithsonian Institution FX This research has made use of data obtained from the Chandra and XMM-Newton Archives. This work was supported in part by the Leverhulme Trust Network for Magnetized Plasma Turbulence and STFC Grant ST/F002505/2 (AAS). The work was also supported in part by the Division of Physical Sciences of the RAS (the program 'Extended objects in the Universe', OFN-16). The financial support for SWR was partially provided for by the Chandra X-ray Center through NASA contract NAS8-03060, and the Smithsonian Institution. NR 21 TC 65 Z9 65 U1 0 U2 1 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD APR PY 2012 VL 421 IS 2 BP 1123 EP 1135 DI 10.1111/j.1365-2966.2011.20372.x PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 924MJ UT WOS:000302695600016 ER PT J AU Kipping, DM Dunn, WR Jasinski, JM Manthri, VP AF Kipping, David M. Dunn, William R. Jasinski, Jamie M. Manthri, Varun P. TI A novel method to photometrically constrain orbital eccentricities: Multibody Asterodensity Profiling SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE methods: numerical; techniques: photometric; eclipses; planets and satellites: general; planetary systems ID KEPLER PLANET CANDIDATES; TRANSIT LIGHT-CURVE; EXTRASOLAR PLANETS; MULTIPLE SYSTEM; SUPER-EARTH; STAR; PARAMETERS; NEPTUNES; MASS AB We present a novel method to determine eccentricity constraints of extrasolar planets in systems with multiple transiting planets through photometry alone. Our method is highly model independent, making no assumptions about the stellar parameters and requiring no radial velocity, transit timing or occultation events. Our technique exploits the fact the light-curve-derived stellar density must be the same for all planets transiting a common star. Assuming a circular orbit, the derived stellar density departs from the true value by a predictable factor, Psi, which contains information on the eccentricity of the system. By comparing multiple stellar densities, any differences must be due to eccentricity and thus meaningful constraints can be placed in the absence of any other information. The technique, called 'Multibody Asterodensity Profiling' (MAP), is a new observable which can be used alone or in combination with other observables, such as radial velocities and transit timing variations. An eccentricity prior can also be included as desired. MAP is most sensitive to the minimum pair-combined eccentricity e.g. (e(1) + e(2))(min). Individual eccentricity constraints are less stringent but an empirical eccentricity posterior is always derivable and is freely available from transit photometry alone. We present a description of our technique using both analytic and numerical implementations, followed by two example analyses on synthetic photometry as a proof of principle. We point out that MAP has the potential to constrain the eccentricity, and thus habitability, of Earth-like planets in the absence of radial velocity data, which is likely for terrestrial-mass objects. C1 [Kipping, David M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Dunn, William R.; Jasinski, Jamie M.; Manthri, Varun P.] UCL, Dept Phys & Astron, London WC1E 6BT, England. RP Kipping, DM (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM dkipping@cfa.harvard.edu FU NASA FX DMK is supported by the NASA Carl Sagan fellowship scheme. We thanks G. Bakos for stimulating conversations on this research. WRD, JMJ and VPM would like to thank G. Tinetti for her support and advice during this project. We would like to offer special thanks to our referee, Brandon Tingley, for his insightful comments and suggestions which greatly improved the manuscript. NR 44 TC 21 Z9 21 U1 0 U2 0 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD APR PY 2012 VL 421 IS 2 BP 1166 EP 1188 DI 10.1111/j.1365-2966.2011.20376.x PG 23 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 924MJ UT WOS:000302695600019 ER PT J AU Maughan, BJ Giles, PA Randall, SW Jones, C Forman, WR AF Maughan, B. J. Giles, P. A. Randall, S. W. Jones, C. Forman, W. R. TI Self-similar scaling and evolution in the galaxy cluster X-ray luminosity-temperature relation SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies: clusters: general; galaxies: clusters: intracluster medium; galaxies: high-redshift; cosmology: observations; X-rays: galaxies: cluster ID SURFACE BRIGHTNESS PROFILES; ACTIVE GALACTIC NUCLEI; STATISTICAL PROPERTIES; REPRESENTATIVE SAMPLE; OBSERVED GROWTH; CHANDRA SAMPLE; GAS FRACTION; T RELATION; MASS; ENTROPY AB We investigate the form and evolution of the X-ray luminosity-temperature (L-X-kT) relation of a sample of 114 galaxy clusters observed with Chandra at 0.1 < z < 1.3. The clusters were divided into subsamples based on their X-ray morphology or whether they host strong cool cores. We find that when the core regions are excluded, the most relaxed clusters (or those with the strongest cool cores) follow an L-X-kT relation with a slope that agrees well with simple self-similar expectations. This is supported by an analysis of the gas density profiles of the systems, which shows self-similar behaviour of the gas profiles of the relaxed clusters outside the core regions. By comparing our data with clusters in the Representative XMM-Newton Cluster Structure Survey (REXCESS) sample, which extends to lower masses, we find evidence that the self-similar behaviour of even the most relaxed clusters breaks at around 3.5 keV. By contrast, the L-X-kT slopes of the subsamples of unrelaxed systems (or those without strong cool cores) are significantly steeper than the self-similar model, with lower mass systems appearing less luminous and higher mass systems appearing more luminous than the self-similar relation. We argue that these results are consistent with a model of non-gravitational energy input in clusters that combines central heating with entropy enhancements from merger shocks. Such enhancements could extend the impact of central energy input to larger radii in unrelaxed clusters, as suggested by our data. We also examine the evolution of the L-X-kT relation, and find that while the data appear inconsistent with simple self-similar evolution, the differences can be plausibly explained by selection bias, and thus we find no reason to rule out self-similar evolution. We show that the fraction of cool core clusters in our (non-representative) sample decreases at z > 0.5 and discuss the effect of this on measurements of the evolution in the L-X-kT relation. C1 [Maughan, B. J.; Giles, P. A.] Univ Bristol, HH Wills Phys Lab, Bristol BS8 1TL, Avon, England. [Randall, S. W.; Jones, C.; Forman, W. R.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02140 USA. RP Maughan, BJ (reprint author), Univ Bristol, HH Wills Phys Lab, Tyndall Ave, Bristol BS8 1TL, Avon, England. EM ben.maughan@bristol.ac.uk OI Randall, Scott/0000-0002-3984-4337; Forman, William/0000-0002-9478-1682 FU Chandra X-ray Center through NASA [NAS8-03060]; Smithsonian Institution FX We thank Trevor Ponman, Alastair Sanderson and Gabriel Pratt for useful discussions of this work. The financial support for SWR was partially provided for by the Chandra X-ray Center through NASA contract NAS8-03060, and the Smithsonian Institution. NR 75 TC 60 Z9 60 U1 0 U2 1 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD APR PY 2012 VL 421 IS 2 BP 1583 EP 1602 DI 10.1111/j.1365-2966.2012.20419.x PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 924MJ UT WOS:000302695600052 ER PT J AU Walker, CM King, RS Whigham, DF Baird, SJ AF Walker, Coowe M. King, Ryan S. Whigham, Dennis F. Baird, Steven J. TI Landscape and Wetland Influences on Headwater Stream Chemistry in the Kenai Lowlands, Alaska SO WETLANDS LA English DT Article DE Watersheds; Peatlands; Headwater streams; Nutrients; Water chemistry; Topographic wetness index; Kenai Peninsula; Alaska ID DISSOLVED ORGANIC-CARBON; WATER CHEMISTRY; NITROGEN EXPORT; DENITRIFICATION; AVAILABILITY; PHOSPHORUS; TOPOGRAPHY; CATCHMENTS; SALMONIDS; PEATLAND AB Headwater streams are typically closely connected with the surrounding watershed landscape, making them sensitive to local watershed conditions. Headwater streams of the Kenai Lowlands in Alaska provide important rearing habitat for juvenile salmon and other biota, and understanding the connections between surrounding landscapes and stream conditions will improve management capabilities. We conducted field evaluations of 30 headwater stream sites on the Kenai Lowlands of Alaska, stratified across watersheds and wetland types, and combined these results with GIS analysis of 12 landscape metrics. Flow-weighted slope (FWS), which is an indicator of the combined influence of percentage cover and topographic position of wetlands, was the best predictor of stream chemistry. Our results revealed distinct differences in water chemistry among headwaters that are largely driven by topography and the amount of wetland in the upstream drainage area. Streams with a high FWS (higher gradient, low wetness) had higher dissolved oxygen and dissolved inorganic nitrogen (mostly nitrate-N), and lower temperatures. Lower FWS streams (low gradient, high wetness) had higher dissolved organic carbon, temperatures, and ammonium and lower dissolved oxygen, all of which were consistent with strong connections between wetlands in watershed and headwater streams. The flow-weighted slope metric is a landscape feature that can be easily derived from GIS, and can be used as a spatially explicit approach for predicting landscape connections to headwater streams on the Kenai Lowlands. C1 [Walker, Coowe M.; Baird, Steven J.] Kachemak Bay Natl Estuarine Res Reserve, Homer, AK 99603 USA. [King, Ryan S.] Baylor Univ, Dept Biol, Ctr Reservoir & Aquat Syst Res, Waco, TX 76798 USA. [Whigham, Dennis F.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. RP Walker, CM (reprint author), Kachemak Bay Natl Estuarine Res Reserve, 95 Sterling Highway,Suite 2, Homer, AK 99603 USA. EM coowe.walker@alaska.gov OI Whigham, Dennis/0000-0003-1488-820X FU US EPA [CD-96011801-0]; Baylor University; Kachemak Bay Research Reserve; Smithsonian Environmental Research Center FX This project was funded by a grant from the US EPA grant number CD-96011801-0, and through additional support through Baylor University, the Kachemak Bay Research Reserve and the Smithsonian Environmental Research Center. Many people assisted with the rigorous field work necessary to collect the field data for this project including Amy Alderfer, Jennifer Brewer, Shan Burson, Kim Cooney, Patrick Dougherty, Dwayne Evans, Rachel Hovel, Megan Murphy, Caitlin Schott, Simeon Smith, and Scott Thompson. We appreciate and thank Kathy Boomer, Jay O'Neill, three anonymous reviewers, and especially Scott Leibowitz for providing valuable comments and edits on manuscript drafts. We especially thank Jeff Back and Conrad Field for their field efforts, and Phil North for his support and encouragement. NR 53 TC 9 Z9 9 U1 0 U2 25 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0277-5212 J9 WETLANDS JI Wetlands PD APR PY 2012 VL 32 IS 2 BP 301 EP 310 DI 10.1007/s13157-011-0260-x PG 10 WC Ecology; Environmental Sciences SC Environmental Sciences & Ecology GA 915MR UT WOS:000302031800011 ER PT J AU Coppard, SE Kroh, A Smith, AB AF Coppard, Simon E. Kroh, Andreas Smith, Andrew B. TI The evolution of pedicellariae in echinoids: an arms race against pests and parasites SO ACTA ZOOLOGICA LA English DT Review DE Echinoidea; phylogeny; taxonomy; cladistics; evolution; Mesozoic marine revolution; fossil record ID GLOBIFEROUS PEDICELLARIAE; HOLASTEROID ECHINOIDS; PHYLOGENETIC ANALYSIS; FINE-STRUCTURE; ECHINODERMATA; MORPHOLOGY; BACTERIUM; DIADEMA; GENUS AB Sea urchins ( Echinoidea) have evolved a diverse array of jawed appendages termed pedicellariae to deter pests and predators. Pedicellarial structure and function are reviewed and their distribution mapped in 75 extant genera. Using a phylogeny of echinoids at family level constructed from 353 skeletal characters scored across 162 extant and fossil taxa, the evolution of pedicellarial form and function is reconstructed. For much of the Palaeozoic echinoids possessed a very restricted pedicellarial armament. By the early Mesozoic a diverse array of pedicellarial types had become established, implying that the threat from predators and pests markedly increased at this time. Since the Triassic, echinoids have continued to improve their defensive capability by evolving more effective venom delivery in globiferous pedicellariae, developing spatulate- tips and curved blades for a more efficient grab in tridentate pedicellariae, and stouter, more robust valves with a stronger bite in ophicephalous pedicellariae to disable and remove ectoparasites. However, pedicellarial types are shown to be particularly prone to subsequent secondary loss, especially among infaunal echinoids, and thus have higher homoplasy levels than other phylogenetically useful skeletal structures. C1 [Smith, Andrew B.] Nat Hist Museum, Dept Palaeontol, London SW7 5BD, England. [Coppard, Simon E.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. [Kroh, Andreas] Nat Hist Museum Vienna, Dept Geol & Palaeontol, A-1010 Vienna, Austria. RP Smith, AB (reprint author), Nat Hist Museum, Dept Palaeontol, Cromwell Rd, London SW7 5BD, England. EM abs@nhm.ac.uk RI Smith, Andrew/B-9849-2009; OI Kroh, Andreas/0000-0002-8566-8848 FU SENACYT (Secretaria Nacional de Ciencia, Tecnologia e Innovacion, Panama) [COL08-002] FX We thank Jorge Ceballos (STRI) for his help with SEM and Mike Reich for pointing out important papers that we might otherwise have missed. Simon Coppard was funded by SENACYT (Secretaria Nacional de Ciencia, Tecnologia e Innovacion, Panama) as part of project COL08-002. We are particularly grateful to Rich Mooi and an anonymous referee for their very helpful and constructive comments that have improved this paper. NR 101 TC 13 Z9 13 U1 3 U2 30 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0001-7272 EI 1463-6395 J9 ACTA ZOOL-STOCKHOLM JI Acta Zool. PD APR PY 2012 VL 93 IS 2 BP 125 EP 148 DI 10.1111/j.1463-6395.2010.00487.x PG 24 WC Anatomy & Morphology; Zoology SC Anatomy & Morphology; Zoology GA 908IS UT WOS:000301484700001 ER PT J AU Mecklenburg, MF del Hoyo-Melendez, JM AF Mecklenburg, Marion F. del Hoyo-Melendez, Julio M. TI Development and application of a mathematical model to explain fading rate inconsistencies observed in light-sensitive materials SO COLORATION TECHNOLOGY LA English DT Article ID FASTNESS; TEXTURE AB Light fastness tests conducted on several areas of a light-sensitive material may sometimes show inconsistent fading rates. These different fading behaviours suggest that colorants are not evenly distributed over the substrate surface or may be attributed to texture variations of the material. A mathematical model has been developed to help explain these discrepancies. Micro-fade testing, a relatively novel technique, has allowed microspectroscopic detection of variations in the initial colour parameters of a sample, permitting assessment of its diverging fading rates. The method has been applied to fading data of various light-sensitive materials resulting in more consistent fading patterns. It has been demonstrated that micro-fading curves obtained for the same material are related by a constant value, which is the ratio of adjusted values of time and ?E*. C1 [Mecklenburg, Marion F.; del Hoyo-Melendez, Julio M.] Smithsonian Inst, Museum Conservat Inst, Suitland, MD 20746 USA. RP del Hoyo-Melendez, JM (reprint author), Smithsonian Inst, Museum Conservat Inst, Suitland, MD 20746 USA. EM jdelhoyo@muzeum.krakow.pl RI del Hoyo-Melendez, Julio/B-1395-2012 OI del Hoyo-Melendez, Julio/0000-0003-2163-2149 FU Smithsonian Institution Office of Research and Training Services FX This research was supported through a Predoctoral Fellowship from the Smithsonian Institution Office of Research and Training Services. The authors express their gratitude to Paul W Whitmore from the Art Conservation Research Center at Carnegie Mellon University in Pittsburgh for providing some of the data used in this study and also for his valuable comments concerning this work. The authors would like to thank Anthony Maiorana for preparing and providing a set of dyed-silk samples for this study during his 2008 summer internship at the Smithsonian Museum Conservation Institute. NR 24 TC 0 Z9 0 U1 0 U2 4 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1472-3581 J9 COLOR TECHNOL JI Color. Technol. PD APR PY 2012 VL 128 IS 2 BP 139 EP 146 DI 10.1111/j.1478-4408.2012.00359.x PG 8 WC Chemistry, Applied; Engineering, Chemical; Materials Science, Textiles SC Chemistry; Engineering; Materials Science GA 902OY UT WOS:000301049000011 ER PT J AU Kay, AD Shik, JZ Van Alst, A Miller, KA Kaspari, M AF Kay, Adam D. Shik, Jonathan Z. Van Alst, Andy Miller, Katie A. Kaspari, Michael TI Diet composition does not affect ant colony tempo SO FUNCTIONAL ECOLOGY LA English DT Article DE Barro Colorado Island; brown food web; carbohydrates; Ectatomma; Geometric Framework; metabolic rate; nutrient balance; nutritional ecology; protein ID NUTRITIONAL ECOLOGY; ARGENTINE ANTS; LIFE-SPAN; CARBOHYDRATE; STOICHIOMETRY; FORMICIDAE; PROTEIN; INSECT; REPRODUCTION; HYMENOPTERA AB 1. Resource availability can influence the structure of animal communities by mediating competitive interactions. An underappreciated aspect of resource ecology is how functional traits are built from particular sets of nutrients and thus are underexpressed when those nutrients are scarce. 2. One idea linking resource availability to competition is the metabolic fuel hypothesis, which posits that access to carbohydrate- rich resources favours high activity rates that increase competitive prowess. One prediction of this hypothesis is that an increase in dietary carbohydrate richness will lead to an increase in consumer metabolic rate (MR). An alternative prediction is that carbohydrate- rich diets will affect biochemical storage. 3. We tested these predictions by examining the effect of dietary protein : carbohydrate (P : C) ratio on the feeding behaviour, demography, physiology and MR of colonies of Ectatomma ruidum, a common tropical ant. We found that rearing colonies for 6 weeks on different P : C diets altered colony demography and worker storage biochemistry, but higher carbohydrate intake did not result in an increase in whole- colonyMR. 4. Our results suggest that dietary carbohydrates may increase colony dominance through changes in colony composition and individual worker longevity rather than changes in worker activity rates. More generally, they illustrate how the identity of scarce nutrients can have particular effects on traits that impact ecological interactions. C1 [Kay, Adam D.; Van Alst, Andy; Miller, Katie A.] Univ St Thomas, Dept Biol, St Paul, MN 55105 USA. [Shik, Jonathan Z.; Kaspari, Michael] Univ Oklahoma, Dept Zool, Grad Program EEB, Norman, OK 73019 USA. [Kaspari, Michael] Smithsonian Trop Res Inst, Balboa, Panama. RP Kay, AD (reprint author), Univ St Thomas, Dept Biol, St Paul, MN 55105 USA. EM adkay@stthomas.edu OI Kaspari, Michael/0000-0002-9717-5768 FU NSF [DEB 0842038] FX We thank Jane Lucas, Tom Marsh, Matt Sweeney and Taylor Zumbusch for help with data collection. We also thank the staff of the Smithsonian Tropical Research Institute on Barro Colorado Island for logistical support. Funding was provided by a grant from the NSF (DEB 0842038) to A. D. Kay and M. Kaspari. NR 46 TC 9 Z9 9 U1 3 U2 58 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0269-8463 J9 FUNCT ECOL JI Funct. Ecol. PD APR PY 2012 VL 26 IS 2 BP 317 EP 323 DI 10.1111/j.1365-2435.2011.01944.x PG 7 WC Ecology SC Environmental Sciences & Ecology GA 915GF UT WOS:000302011400003 ER PT J AU Vrsansky, P Vidlicka, L Ciampor, F Marsh, F AF Vrsansky, Peter Vidlicka, L'ubomir Ciampor, Fedor, Jr. Marsh, Finnegan TI Derived, still living cockroach genus Cariblattoides (Blattida: Blattellidae) from the Eocene sediments of Green River in Colorado, USA SO INSECT SCIENCE LA English DT Article DE Blattida = Blattaria = Blattodea; Cariblattoides; Eocene; fossil insects; Green River; Tertiary cockroaches AB Cariblattoides labandeirai sp.n. from the Eocene sediments of Green River in Colorado, USA bear only two plesiomorphies, but also several significant autapomorphies within the advanced and highly derived living cockroach genus. Thus, Cariblattoides with extant occurrence in the Caribbean and South America was historically common in the Nearctic, and represents important evidence for the occurrence of derived living genera of cockroaches similar to 50 Ma ago. Generally, the vast majority of living genera were absent during the Palaeocene, thus the diversification of most living cockroach lineages near the Palaeocene/Eocene boundary must have been extremely rapid. Females of living C. suave, the type species, have identical (sophisticated) coloration of pronotum, but the most related living taxa are C. piraiensis and C. fontesi from Brazil (supported by phylogenetical analysis). C1 [Vrsansky, Peter] Slovak Acad Sci, Inst Geol, Bratislava 84005, Slovakia. [Vrsansky, Peter] Russian Acad Sci, Inst Paleontol, Moscow V71, Russia. [Vidlicka, L'ubomir; Ciampor, Fedor, Jr.] Slovak Acad Sci, Inst Zool, Bratislava 84005, Slovakia. [Vidlicka, L'ubomir] Comenius Univ, Dept Biol, Fac Educ, Bratislava, Slovakia. [Marsh, Finnegan] Smithsonian Inst, Dept Paleobiol, Natl Museum Nat Hist, Washington, DC 20560 USA. RP Vrsansky, P (reprint author), Slovak Acad Sci, Inst Geol, Dubravska Cesta 9,POB 106, Bratislava 84005, Slovakia. EM geolvrsa@savba.sk FU UNESCO; Amba; National Museum of Natural History, Washington D.C.; VEGA [6002, 2/0125/09, 2/0167/09]; MVTS; Literary Fund FX We thank David Kohls and Louis Pribyl (NMNH Washingtn DC) for collecting the material, and Conrad Labandeira for organising the study; Alexandr P. Rasnitsyn (PIN Moscow), Sonia M. Lopes (MN/UFRJ), Pavel Stys (CU Prague) and Heiko Schmied (SI Bonn) for fruitful advice and revision of the manuscript, and Ladislav Roller (ZI Bratislava) for literature supply. Supported by the UNESCO, Amba, National Museum of Natural History, Washington D.C. award, VEGA 6002, 2/0125/09, 2/0167/09, MVTS and the Literary Fund. NR 23 TC 8 Z9 8 U1 0 U2 5 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 1672-9609 J9 INSECT SCI JI Insect Sci. PD APR PY 2012 VL 19 IS 2 BP 143 EP 152 DI 10.1111/j.1744-7917.2010.01390.x PG 10 WC Entomology SC Entomology GA 917GB UT WOS:000302159500002 ER PT J AU McFrederick, QS Wcislo, WT Taylor, DR Ishak, HD Dowd, SE Mueller, UG AF McFrederick, Quinn S. Wcislo, William T. Taylor, Douglas R. Ishak, Heather D. Dowd, Scot E. Mueller, Ulrich G. TI Environment or kin: whence do bees obtain acidophilic bacteria? SO MOLECULAR ECOLOGY LA English DT Article DE 16S rDNA amplicon 454 pyrosequencing; acidophilic bacteria; insect diseases; insect symbiosis; Lactobacillus; phylogeny ID LACTIC-ACID BACTERIA; 16S RIBOSOMAL-RNA; COLONY COLLAPSE DISORDER; APIS-MELLIFERA; BUMBLE BEES; HONEY-BEES; ECUADORIA HYMENOPTERA; MEGALOPTA-GENALIS; SWEAT BEES; DIVERSITY AB As honey bee populations decline, interest in pathogenic and mutualistic relationships between bees and microorganisms has increased. Honey bees and bumble bees appear to have a simple intestinal bacterial fauna that includes acidophilic bacteria. Here, we explore the hypothesis that sweat bees can acquire acidophilic bacteria from the environment. To quantify bacterial communities associated with two species of North American and one species of Neotropical sweat bees, we conducted 16S rDNA amplicon 454 pyrosequencing of bacteria associated with the bees, their brood cells and their nests. Lactobacillus spp. were the most abundant bacteria in many, but not all, of the samples. To determine whether bee-associated lactobacilli can also be found in the environment, we reconstructed the phylogenetic relationships of the genus Lactobacillus. Previously described groups that associate with Bombus and Apis appeared relatively specific to these genera. Close relatives of several bacteria that have been isolated from flowers, however, were isolated from bees. Additionally, all three sweat bee species associated with lactobacilli related to flower-associated lactobacilli. These data suggest that there may be at least two different means by which bees acquire putative probiotics. Some lactobacilli appear specific to corbiculate apids, possibly because they are largely maternally inherited (vertically transmitted). Other lactobacilli, however, may be regularly acquired from environmental sources such as flowers. Sweat beeassociated lactobacilli were found to be abundant in the pollen and frass inside the nests of halictids, suggesting that they could play a role in suppressing the growth of moulds and other spoilage organisms. C1 [McFrederick, Quinn S.; Ishak, Heather D.; Mueller, Ulrich G.] Univ Texas Austin, Sect Integrat Biol, Austin, TX 78712 USA. [Wcislo, William T.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. [Taylor, Douglas R.] Univ Virginia, Dept Biol, Charlottesville, VA 22904 USA. [Dowd, Scot E.] MR DNA Mol Res, Shallowater, TX 79363 USA. RP McFrederick, QS (reprint author), Univ Texas Austin, Sect Integrat Biol, 2401 Speedway Dr C0930, Austin, TX 78712 USA. EM quinnmcfrederick@gmail.com FU Blandy Experimental Farm; National Science Foundation [PRFB-1003133, DEB-0919519, DDIG-0808454] FX We thank Sabrina Amador and three anonymous reviewers for comments on an earlier draft; Blandy Experimental Farm for access, logistical support and financial support; and the Smithsonian Tropical Research Institute for access to BCI and logistical support. This material is based on work supported by the National Science Foundation under Grant Nos. PRFB-1003133, DEB-0919519 and DDIG-0808454. NR 60 TC 34 Z9 35 U1 2 U2 37 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0962-1083 J9 MOL ECOL JI Mol. Ecol. PD APR PY 2012 VL 21 IS 7 BP 1754 EP 1768 DI 10.1111/j.1365-294X.2012.05496.x PG 15 WC Biochemistry & Molecular Biology; Ecology; Evolutionary Biology SC Biochemistry & Molecular Biology; Environmental Sciences & Ecology; Evolutionary Biology GA 914FB UT WOS:000301933600016 PM 22340254 ER PT J AU Buffington, ML Brady, SG Morita, SI Van Noort, S AF Buffington, Matthew L. Brady, Sean G. Morita, Shelah I. Van Noort, Simon TI Divergence estimates and early evolutionary history of Figitidae (Hymenoptera: Cynipoidea) SO SYSTEMATIC ENTOMOLOGY LA English DT Review ID AUSTRALIAN THRASORINAE HYMENOPTERA; LARVAL-PUPAL PARASITOIDS; RNA SECONDARY STRUCTURE; DUNG-BREEDING DIPTERA; CALIBRATION UNCERTAINTY; WASPS HYMENOPTERA; OAK GALLWASPS; GALL WASPS; FACE FLY; HORN FLY AB We examine the phylogenetic relationships of Figitidae and discuss host use within this group in light of our own and previously published divergence time data. Our results suggest Figitidae, as currently defined, is not monophyletic. Furthermore, Mikeiinae and Pycnostigminae are sister-groups, nested adjacent to Thrasorinae, Plectocynipinae and Euceroptrinae. The recovery of Pycnostigminae as sister-group to Mikeiinae suggests two major patterns of evolution: (i) early Figitidae lineages demonstrate a Gondawanan origin (Plectocynipinae: Neotropical; Mikeiinae and Thrasorinae: Australia; Pycnostigminae: Africa); and (ii) based on host records for Mikeiinae, Thrasorinae and Plectocynipinae, Pycnostigminae are predicted to be parasitic on gall-inducing Hymenoptera. The phylogenetic position of Parnips (Parnipinae) was unstable, and various analyses were conducted to determine the impact of this uncertainty on both the recovery of other clades and inferred divergence times; when Parnips was excluded from the total evidence analysis, Cynipidae was found to be sister-group to [Euceroptrinae + (Plectocynipinae (Thrasorinae + (Mikeiinae + Pycnostigminae)))], with low support. Divergence dating analyses using BEAST indicate the stem-group node of Figitidae to be c. 126 Ma; the dipteran parasitoids (Eucoilinae and Figitinae), were estimated to have a median age of 80 and 88 Ma, respectively; the neuropteran parasitoids (Anacharitinae), were estimated to have a median age of 97 Ma; sternorrhynchan hyperparasitoids (Charipinae), were estimated to have a median age of 110 Ma; the Hymenoptera-parasitic subfamilies (Euceroptinae, Plectocynipinae, Trasorinae, Mikeiinae, Pycnostigminae, and Parnipinae), ranged in median ages from 48 to 108 Ma. Rapid radiation of Eucoilinae subclades appears chronologically synchronized with the origin of their hosts, Schizophora (Diptera). Overall, the exclusion of Parnips from the BEAST analysis did not result in significant changes to divergence estimates. Finally, though sparsely represented in the analysis, our data suggest Cynipidae have a median age of 54 Ma, which is somewhat older than the age of Quercus spp (3050 Ma), their most common host. C1 [Buffington, Matthew L.] USDA, Systemat Entomol Lab, Smithsonian NMNH, Washington, DC 20013 USA. [Brady, Sean G.; Morita, Shelah I.] Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol, Washington, DC 20560 USA. [Morita, Shelah I.] N Carolina State Univ, Dept Entomol, Raleigh, NC 27695 USA. [Van Noort, Simon] Iziko S African Museum, Nat Hist Dept, Cape Town, South Africa. [Van Noort, Simon] Univ Cape Town, Dept Zool, ZA-7700 Rondebosch, South Africa. RP Buffington, ML (reprint author), USDA, Systemat Entomol Lab, Smithsonian NMNH, 10th & Constitut Ave NW, Washington, DC 20013 USA. EM matt.buffington@ars.usda.gov RI van Noort, Simon/C-4006-2017 OI van Noort, Simon/0000-0001-6930-9741 FU National Science Foundation [EF-0431330, DEB-0743542]; Smithsonian Institution Libraries; National Museum of Natural History Diptera Unit; Schultz lab (Smithsonian Institution); Sonja Schaeffer; Alma Solis (Systematic Entomology Lab, ARS, Washington DC) FX MB would like to thank Mark Springer (University of California, Riverside) and Jeff Thorne (North Carolina State University) for assistance and guidance in the early stages of these analyses; John LaSalle (CSIRO/Australian National Insect Collection, Canberra) for fresh samples of Mikeiinae for molecular analyses; and Sonja Scheffer, Matthew Lewis and Andy Carmichael (Systematic Entomology Lab, ARS, Beltsville, MD) for providing sequence data for the Mikeius, Myrtopsen and Pycnostigmus used in this study. SGB would like to thank the Laboratories of Analytical Biology (National Museum of Natural History) for computational resources and the National Science Foundation for research support under grants EF-0431330 and DEB-0743542. SIM would like to thank the Smithsonian Institution Libraries, the National Museum of Natural History Diptera Unit, the Schultz lab (Smithsonian Institution), Sonja Schaeffer and Alma Solis (Systematic Entomology Lab, ARS, Washington DC) for encouragement and in-kind support. John Brown and Thomas J. Henry (Systematic Entomology Lab, ARS, Washington DC), Shaun Winterton (California Department of Food and Agriculture, Sacramento, CA) and Jose-Luis Nieves-Aldrey (University of Madrid, Spain) provided constructive criticism that improved the clarity and quality of this paper. USDA is an equality opportunity employer and provider. NR 162 TC 19 Z9 19 U1 0 U2 11 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0307-6970 EI 1365-3113 J9 SYST ENTOMOL JI Syst. Entomol. PD APR PY 2012 VL 37 IS 2 BP 287 EP 304 DI 10.1111/j.1365-3113.2012.00617.x PG 18 WC Evolutionary Biology; Entomology SC Evolutionary Biology; Entomology GA 917KH UT WOS:000302173200004 ER PT J AU Detto, M Molini, A Katul, G Stoy, P Palmroth, S Baldocchi, D AF Detto, Matteo Molini, Annalisa Katul, Gabriel Stoy, Paul Palmroth, Sari Baldocchi, Dennis TI Causality and Persistence in Ecological Systems: A Nonparametric Spectral Granger Causality Approach SO AMERICAN NATURALIST LA English DT Article DE spectral Granger causality; complex systems; periodic forcing; photosynthesis-respiration coupling ID PRODUCER-DECOMPOSER INTERACTIONS; TIME-SERIES; SOIL RESPIRATION; CARBON-DIOXIDE; ELEVATED CO2; POPULATION-DYNAMICS; ROOT RESPIRATION; FLUX DENSITIES; FOREST; PHOTOSYNTHESIS AB Directionality in coupling, defined as the linkage relating causes to their effects at a later time, can be used to explain the core dynamics of ecological systems by untangling direct and feedback relationships between the different components of the systems. Inferring causality from measured ecological variables sampled through time remains a formidable challenge further made difficult by the action of periodic drivers overlapping the natural dynamics of the system. Periodicity in the drivers can often mask the self-sustained oscillations originating from the autonomous dynamics. While linear and direct causal relationships are commonly addressed in the time domain, using the well-established machinery of Granger causality (G-causality), the presence of periodic forcing requires frequency-based statistics (e. g., the Fourier transform), able to distinguish coupling induced by oscillations in external drivers from genuine endogenous interactions. Recent nonparametric spectral extensions of G-causality to the frequency domain pave the way for the scale-by-scale decomposition of causality, which can improve our ability to link oscillatory behaviors of ecological networks to causal mechanisms. The performance of both spectral G-causality and its conditional extension for multivariate systems is explored in quantifying causal interactions within ecological networks. Through two case studies involving synthetic and actual time series, it is demonstrated that conditional G-causality outperforms standard G-causality in identifying causal links and their concomitant timescales. C1 [Detto, Matteo] Smithsonian Trop Resource Inst, Ancon, Panama. [Detto, Matteo; Baldocchi, Dennis] Univ Calif Berkeley, Dept Environm Sci Policy & Management, Berkeley, CA 94720 USA. [Molini, Annalisa] Masdar Inst Sci & Technol, Abu Dhabi, U Arab Emirates. [Molini, Annalisa; Katul, Gabriel; Palmroth, Sari] Duke Univ, Nicholas Sch Environm, Durham, NC 27708 USA. [Molini, Annalisa; Katul, Gabriel] Duke Univ, Pratt Sch Engn, Dept Civil & Environm Engn, Durham, NC 27708 USA. [Stoy, Paul] Montana State Univ, Dept Land Resources & Environm Sci, Bozeman, MT 59717 USA. RP Detto, M (reprint author), Smithsonian Trop Resource Inst, Apartado Postal 0843-03092 Balboa, Ancon, Panama. EM dettom@si.edu RI Katul, Gabriel/A-7210-2008; Baldocchi, Dennis/A-1625-2009; Molini, Annalisa/E-8235-2016 OI Katul, Gabriel/0000-0001-9768-3693; Baldocchi, Dennis/0000-0003-3496-4919; Molini, Annalisa/0000-0003-3815-3929 FU U.S. Department of Energy through the Office of Biological and Environmental Research [DE-FG02-95ER62083, DE-FC02-06ER64156]; National Science Foundation [0628720, NSF-EAR-10-13339, NSF-CBET-10-3347, NSF-AGS-11-02227] FX We thank M. Dhamala for useful discussions. The data collection at the Duke Forest was supported by the U.S. Department of Energy through the Office of Biological and Environmental Research Terrestrial Carbon Processes program (Free-Air CO2 Enrichment and National Institute for Climatic Change Research grants DE-FG02-95ER62083, DE-FC02-06ER64156). M. D. and D. B. acknowledge funding from the National Science Foundation (grant 0628720). G. K. and A. M. acknowledge funding from the National Science Foundation (grants NSF-EAR-10-13339, NSF-CBET-10-3347, NSF-AGS-11-02227). M. D. also acknowledges the Global Forest Carbon Research Initiative at the Center for Tropical Forest Science. NR 60 TC 25 Z9 26 U1 0 U2 33 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0003-0147 J9 AM NAT JI Am. Nat. PD APR PY 2012 VL 179 IS 4 BP 524 EP 535 DI 10.1086/664628 PG 12 WC Ecology; Evolutionary Biology SC Environmental Sciences & Ecology; Evolutionary Biology GA 914TK UT WOS:000301975200011 PM 22437181 ER PT J AU Riveros, AJ Seid, MA Wcislo, WT AF Riveros, Andre J. Seid, Marc A. Wcislo, William T. TI Evolution of brain size in class-based societies of fungus-growing ants (Attini) SO ANIMAL BEHAVIOUR LA English DT Article DE antennal lobe; Attini; Hymenoptera; scalogram; social brain ID SOCIAL BRAIN; MUSHROOM BODIES; CULTURAL-EVOLUTION; HABITAT COMPLEXITY; ATTA-VOLLENWEIDERI; MEGALOPTA-GENALIS; NEOCORTEX SIZE; SCALE ANALYSIS; ANTENNAL LOBE; INSECTS AB A social lifestyle is often assumed to be more complex than a solitary one, due to social demands that may require increased cognitive capabilities. These nested assumptions underlie hypotheses to explain a correlation between brain size and group size in social vertebrates, using group size and accumulation of social traits, as alternative proxies for social complexity. Eusocial insects challenge the generality of the hypothesis that social complexity relies on increased cognitive capabilities of individuals. We used data from previously published studies to test for an association between sociality and brain size across 18 species (nine genera) of fungus-growing ants (Attini), which range from basal taxa with fewer than 100 monomorphic individuals, to derived colonies containing several million polymorphic, highly specialized individuals. Among monomorphic species, increased colony size was associated with decreased relative brain size and increased olfactory lobe size, although the latter result was sensitive to both the exclusion of potential outliers and whether phylogenetically independent contrasts were used. Within leafcutters (Atta), the relative size of the antennal lobes was also associated with group size, but may also reflect ecological foraging specialization, which may be a confounding variable. Comparisons between class-and individual-based societies highlight the general problem of increasing social structure in proportion to group size and show that there are alternative solutions to this problem: one alternative involves increasing behavioural specialization of individuals and evolved rules; the other involves increased diversification of individual behaviour, social norms and ultimately institutions. The Association for the Study of Animal Behaviour. Published by Elsevier Ltd. C1 [Riveros, Andre J.; Wcislo, William T.] Smithsonian Trop Res Inst, Balboa, Panama. [Seid, Marc A.] Univ Scranton, Dept Biol, Scranton, PA 18510 USA. RP Wcislo, WT (reprint author), Smithsonian Trop Res Inst, Apartado 0843-03092, Balboa, Panama. EM anjosafat@gmail.com; wcislow@si.edu FU Smithsonian Tropical Research Institute (STRI); Smithsonian Institution; F.H. Levinson Fund FX We thank Simon Tierney and anonymous referees for helpful comments of earlier versions of this manuscript. A.J.R. was supported by a Latin American Fellowship from the Smithsonian Tropical Research Institute (STRI), and by the Smithsonian Institution's Scholarly Studies Program (to W. Eberhard, A. J. Riveros and W. Wcislo). We are also grateful for the generous support from the F.H. Levinson Fund to STRI's Laboratory of Behavior & Evolutionary Biology, and for general research funds from STRI. A.J.R. and W.T.W. compiled and analysed the data and wrote the manuscript; M.S. dissected and measured ant brains and analysed data. NR 79 TC 15 Z9 15 U1 4 U2 37 PU ACADEMIC PRESS LTD- ELSEVIER SCIENCE LTD PI LONDON PA 24-28 OVAL RD, LONDON NW1 7DX, ENGLAND SN 0003-3472 J9 ANIM BEHAV JI Anim. Behav. PD APR PY 2012 VL 83 IS 4 BP 1043 EP 1049 DI 10.1016/j.anbehav.2012.01.032 PG 7 WC Behavioral Sciences; Zoology SC Behavioral Sciences; Zoology GA 914TN UT WOS:000301975500026 ER PT J AU Luther, DA Derryberry, EP AF Luther, David A. Derryberry, Elizabeth P. TI Birdsongs keep pace with city life: changes in song over time in an urban songbird affects communication SO ANIMAL BEHAVIOUR LA English DT Article DE ambient noise; birdsong; communication; cultural evolution; signal salience; urban ID WHITE-CROWNED SPARROW; ANTHROPOGENIC NOISE; TRAFFIC NOISE; BIRD SONG; ENVIRONMENTAL NOISE; HIGHER PITCH; GREAT TITS; EVOLUTION; FREQUENCY; DISCRIMINATION AB Animals in urban environments often must adjust their vocalizations to be heard over the din of anthropogenic ambient noise. Most studies of this process use current comparisons of environments that vary in ambient noise; here, we evaluate over time the effects of the urban environment on signal structure and salience. We show that white-crowned sparrow, Zonotrichia leucophrys, song increased in minimum frequency between 1969 and 2005 in San Francisco, California, U.S.A., coincident with rising levels of traffic noise. A higher minimum frequency is less likely to be masked by low-frequency ambient noise and thus is more likely to be effective as a communication signal. To test whether this change in song affects receiver response, we presented territorial males current (2005) and historical (1969) local songs. Males responded more strongly to current than to historical songs, suggesting that current songs communicate more effectively in the current local environment. The results suggest that behavioural adjustment to anthropogenic ambient noise over time can affect cultural evolution and communication. (C) 2012 The Association for the Study of Animal Behaviour. Published by Elsevier Ltd. All rights reserved. C1 [Luther, David A.] George Mason Univ, Dept Biol, Fairfax, VA 22030 USA. [Luther, David A.] Smithsonian Inst, Smithsonian Migratory Bird Ctr, Washington, DC 20560 USA. [Derryberry, Elizabeth P.] Louisiana State Univ, Museum Nat Sci, Baton Rouge, LA 70803 USA. RP Luther, DA (reprint author), George Mason Univ, Dept Biol, Fairfax, VA 22030 USA. EM dluther@gmu.edu NR 51 TC 25 Z9 26 U1 10 U2 137 PU ACADEMIC PRESS LTD- ELSEVIER SCIENCE LTD PI LONDON PA 24-28 OVAL RD, LONDON NW1 7DX, ENGLAND SN 0003-3472 J9 ANIM BEHAV JI Anim. Behav. PD APR PY 2012 VL 83 IS 4 BP 1059 EP 1066 DI 10.1016/j.anbehav.2012.01.034 PG 8 WC Behavioral Sciences; Zoology SC Behavioral Sciences; Zoology GA 914TN UT WOS:000301975500028 ER PT J AU Andrade, SCS Strand, M Schwartz, M Chen, HX Kajihara, H von Dohren, J Sun, SC Junoy, J Thiel, M Norenburg, JL Turbeville, JM Giribet, G Sundberg, P AF Andrade, Sonia C. S. Strand, Malin Schwartz, Megan Chen, Haixia Kajihara, Hiroshi von Doehren, Joern Sun, Shichun Junoy, Juan Thiel, Martin Norenburg, Jon L. Turbeville, James M. Giribet, Gonzalo Sundberg, Per TI Disentangling ribbon worm relationships: multi-locus analysis supports traditional classification of the phylum Nemertea SO CLADISTICS LA English DT Review ID MULTIPLE SEQUENCE ALIGNMENT; RIBOSOMAL-RNA SEQUENCES; 18S RDNA SEQUENCES; PHYLOGENETIC ANALYSIS; TERRESTRIAL NEMERTEANS; CRATENEMERTIDAE NEMERTEA; HOPLONEMERTEAN GENUS; MOLECULAR EVOLUTION; PILIDIUM LARVA; DNA-SEQUENCES AB The phylogenetic relationships of selected members of the phylum Nemertea are explored by means of six markers amplified from the genomic DNA of freshly collected specimens (the nuclear 18S rRNA and 28S rRNA genes, histones H3 and H4, and the mitochondrial genes 16S rRNA and cytochrome c oxidase subunit I). These include all previous markers and regions used in earlier phylogenetic analyses of nemerteans, therefore acting as a scaffold to which one could pinpoint any previously published study. Our results, based on analyses of static and dynamic homology concepts under probabilistic and parsimony frameworks, agree in the non-monophyly of Palaeonemertea and in the monophyly of Heteronemerta and Hoplonemertea. The position of Hubrechtella and the Pilidiophora hypothesis are, however, sensitive to analytical method, as is the monophyly of the non-hubrechtiid palaeonemerteans. Our results are, however, consistent with the main division of Hoplonemertea into Polystilifera and Monostilifera, the last named being divided into Cratenemertea and Distromatonemertea, as well as into the main division of Heteronemertea into Baseodiscus and the remaining species. The study also continues to highlight the deficient taxonomy at the family and generic level within Nemertea and sheds light on the areas of the tree that require further refinement. C1 [Chen, Haixia; Sundberg, Per] Univ Gothenburg, Dept Zool, Gothenburg, Sweden. [Andrade, Sonia C. S.; Giribet, Gonzalo] Harvard Univ, Dept Organism & Evolutionary Biol, Museum Comparat Zool, Cambridge, MA 02138 USA. [Strand, Malin] Univ Gothenburg, Dept Zool, Sven Loven Ctr Marine Sci, Stromstad, Sweden. [Schwartz, Megan] Seattle Univ, Dept Biol, Seattle, WA 98122 USA. [Kajihara, Hiroshi] Hokkaido Univ, Fac Sci, Sapporo, Hokkaido 0600810, Japan. [von Doehren, Joern] Univ Bonn, Inst Evolutionary Biol & Ecol, D-53121 Bonn, Germany. [Sun, Shichun] Ocean Univ China, Inst Evolut & Marine Biodivers, Qingdao 266003, Peoples R China. [Junoy, Juan] Univ Alcala de Henares, Dept Zool & Antropol Fis, E-28871 Alcala De Henares, Spain. [Junoy, Juan] Univ Alcala de Henares, Inst Benjamin Franklin, E-28871 Alcala De Henares, Spain. [Thiel, Martin] Univ Catolica Norte, Fac Ciencias Mar, Coquimbo, Chile. [Norenburg, Jon L.] Natl Museum Nat Hist, Smithsonian Inst, Dept Invertebrate Zool MRC 163, Washington, DC 20560 USA. [Turbeville, James M.] Virginia Commonwealth Univ, Dept Biol, Richmond, VA 23284 USA. RP Sundberg, P (reprint author), Univ Gothenburg, Dept Zool, Gothenburg, Sweden. EM per.sundberg@gu.se RI Giribet, Gonzalo/P-1086-2015; Andrade, Sonia/I-9263-2012; Andrade, Sonia/F-8267-2014; Norenburg, Jon/K-3481-2015 OI Giribet, Gonzalo/0000-0002-5467-8429; Norenburg, Jon/0000-0001-7776-1527 FU Galician Government; SCRIPPS Institution of Oceanography; AToL of the US NSF [EF-0334932, EF-0531757]; MCZ; NSF [EF-0531757, DEB 0844881]; University of Gothenburg; Swedish research Council [621-2008-5658]; German Research Council (DFG) [Ba 1520/11-1,2]; NSFC [30970333]; Smithsonian Scholarly Studies program; Smithsonian Institution's Marine Science Network FX Two anonymous reviewers and the Editor provided comments that helped to improve an earlier version of this article. The Willi Hennig Society is acknowledged for making TNT available for public use. Many colleagues assisted with collection of specimens; our most sincere thanks to them all: Bob Mesibov (Tasmania), Wolfgang Sterrer (Bermuda), Jacinto Perez (Club de Buceo Hydronauta, Ribeira), Thomas Dahlgren (Gothenburg), Christopher Laumer (MCZ), Gisele Kawauchi (MCZ), Yolanda Lucas Rodriguez (Estacion de Bioloxia Marina da Grana) and Katrine Worsaae (Helsingor). Greg Rouse kindly allowed us to see some of his unpublished photographs. Vituco Urgorri invited G. G. to the Oceanographic campaign DIVA-ALTA-BRIA II funded by the Galician Government; Nerida Wilson and Greg Rouse invited G. G. to an Oceanographic campaign to the Santa Rosa-Cortes Ridge, funded by the SCRIPPS Institution of Oceanography. Collecting trips to Beaufort (North Carolina), Kristineberg (Sweden), and Tjarno by G. G. and sequencing of outgroup taxa were funded by the AToL Program of the US NSF (NSF grant nos. EF-0334932 and EF-0531757). Collecting trips to Panama and Bahamas by G. G. were supported by the MCZ and the Faculty of Arts and Sciences (Harvard). DNA sequencing was facilitated by the Bauer Center for Genomics Research (Harvard) and sponsored by the Curator's funds of the MCZ. S. A. was supported by NSF grant nos. EF-0531757 and DEB 0844881. P. S. received grants from the University of Gothenburg (Life Science graduate programme) and the Swedish research Council (no. 621-2008-5658). J.v.D. was funded by a German Research Council grant (DFG, Ba 1520/11-1,2). S.S. was supported by NSFC (no. 30970333). J.N. was supported by funds from the Smithsonian Scholarly Studies program and the Smithsonian Institution's Marine Science Network; this represents contribution no. 866 from the Smithsonian Marine Station at Fort Pierce, Florida. NR 126 TC 42 Z9 49 U1 0 U2 27 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0748-3007 EI 1096-0031 J9 CLADISTICS JI Cladistics PD APR PY 2012 VL 28 IS 2 BP 141 EP 159 DI 10.1111/j.1096-0031.2011.00376.x PG 19 WC Evolutionary Biology SC Evolutionary Biology GA 905OH UT WOS:000301281500005 ER PT J AU McCormack, JE Faircloth, BC Crawford, NG Gowaty, PA Brumfield, RT Glenn, TC AF McCormack, John E. Faircloth, Brant C. Crawford, Nicholas G. Adair Gowaty, Patricia Brumfield, Robb T. Glenn, Travis C. TI Ultraconserved elements are novel phylogenomic markers that resolve placental mammal phylogeny when combined with species-tree analysis SO GENOME RESEARCH LA English DT Article ID MAXIMUM-LIKELIHOOD; BAYESIAN PHYLOGENETICS; HIGH-THROUGHPUT; EARLY HISTORY; HUMAN GENOME; GENE TREES; DIVERSIFICATION; RESOLUTION; LIFE; COALESCENCE AB Phylogenomics offers the potential to fully resolve the Tree of Life, but increasing genomic coverage also reveals conflicting evolutionary histories among genes, demanding new analytical strategies for elucidating a single history of life. Here, we outline a phylogenomic approach using a novel class of phylogenetic markers derived from ultraconserved elements and flanking DNA. Using species-tree analysis that accounts for discord among hundreds of independent loci, we show that this class of marker is useful for recovering deep-level phylogeny in placental mammals. In broad outline, our phylogeny agrees with recent phylogenomic studies of mammals, including several formerly controversial relationships. Our results also inform two outstanding questions in placental mammal phylogeny involving rapid speciation, where species-tree methods are particularly needed. Contrary to most phylogenomic studies, our study supports a first-diverging placental mammal lineage that includes elephants and tenrecs (Afrotheria). The level of conflict among gene histories is consistent with this basal divergence occurring in or near a phylogenetic "anomaly zone" where a failure to account for coalescent stochasticity will mislead phylogenetic inference. Addressing a long-standing phylogenetic mystery, we find some support from a high genomic coverage data set for a traditional placement of bats (Chiroptera) sister to a clade containing Perissodactyla, Cetartiodactyla, and Carnivora, and not nested within the latter clade, as has been suggested recently, although other results were conflicting. One of the most remarkable findings of our study is that ultraconserved elements and their flanking DNA are a rich source of phylogenetic information with strong potential for application across Amniotes. C1 [McCormack, John E.; Brumfield, Robb T.] Louisiana State Univ, Museum Nat Sci, Baton Rouge, LA 70803 USA. [Faircloth, Brant C.] Univ Calif Los Angeles, Dept Ecol & Evolutionary Biol, Los Angeles, CA 90095 USA. [Crawford, Nicholas G.] Boston Univ, Dept Biol, Boston, MA 02215 USA. [Adair Gowaty, Patricia] Smithsonian Trop Res Inst, Panama City, Panama. [Adair Gowaty, Patricia] Univ Calif Los Angeles, Inst Environm, Los Angeles, CA 90095 USA. [Brumfield, Robb T.] Louisiana State Univ, Dept Biol Sci, Baton Rouge, LA 70803 USA. [Glenn, Travis C.] Univ Georgia, Dept Environm Hlth Sci, Athens, GA 30602 USA. RP McCormack, JE (reprint author), Louisiana State Univ, Museum Nat Sci, Baton Rouge, LA 70803 USA. EM mccormack@oxy.edu RI perumal, murugiah/D-1565-2012; McCormack, John/A-6380-2010; Brumfield, Robb/K-6108-2015; OI Brumfield, Robb/0000-0003-2307-0688; Faircloth, Brant/0000-0002-1943-0217 FU Amazon Web Services; Harvard FAS Sciences Division Research Computing Group FX We thank M. Springer for sharing the 20-locus mammal data set and J. Mattick for sharing UCE and exon data. SR Hubbell, S. Edwards, J. Degnan, M. Sheehan, M. Alfaro, B. Carstens, and three anonymous reviewers provided helpful comments. One reviewer suggested the point about selection potentially improving the phylogenetic utility of UCEs. H. Hoekstra provided access to the Odyssey cluster supported by the Harvard FAS Sciences Division Research Computing Group to conduct phylogenetic analysis. A research grant from Amazon Web Services (Amazon.com) also supported phylogenetic computation. We thank the many scientists, institutions, and funding agencies that have contributed genomic data available via the UCSC Genome Browser (see complete list at http://genome.ucsc.edu/goldenPath/credits.html and Supplemental Material). NR 66 TC 116 Z9 118 U1 4 U2 66 PU COLD SPRING HARBOR LAB PRESS, PUBLICATIONS DEPT PI COLD SPRING HARBOR PA 1 BUNGTOWN RD, COLD SPRING HARBOR, NY 11724 USA SN 1088-9051 J9 GENOME RES JI Genome Res. PD APR PY 2012 VL 22 IS 4 BP 746 EP 754 DI 10.1101/gr.125864.111 PG 9 WC Biochemistry & Molecular Biology; Biotechnology & Applied Microbiology; Genetics & Heredity SC Biochemistry & Molecular Biology; Biotechnology & Applied Microbiology; Genetics & Heredity GA 917UJ UT WOS:000302203800015 PM 22207614 ER PT J AU Taufik, E Fukuda, K Senda, A Saito, T Williams, C Tilden, C Eisert, R Oftedal, O Urashima, T AF Taufik, Epi Fukuda, Kenji Senda, Akitsugu Saito, Tadao Williams, Cathy Tilden, Chris Eisert, Regina Oftedal, Olav Urashima, Tadasu TI Structural characterization of neutral and acidic oligosaccharides in the milks of strepsirrhine primates: greater galago, aye-aye, Coquerel's sifaka and mongoose lemur SO GLYCOCONJUGATE JOURNAL LA English DT Article DE Milk oligosaccharides; Lactation; Primates; Strepsirrhines; Phylogeny; Sociality; Greater galago; Aye-aye; Sifaka; Lemur ID N-GLYCOLYLNEURAMINIC ACID; CHEMICAL-CHARACTERIZATION; HUMAN COLOSTRUM; EULEMUR-MONGOZ; SIALIC ACIDS; LACTATION; SIZE; CHROMATOGRAPHY; EVOLUTION; ENZYME AB The structures of milk oligosaccharides were characterized for four strepsirrhine primates to examine the extent to which they resemble milk oligosaccharides in other primates. Neutral and acidic oligosaccharides were isolated from milk of the greater galago (Galagidae: Otolemur crassicaudatus), aye-aye (Daubentoniidae: Daubentonia madagascariensis), Coquerel's sifaka (Indriidae: Propithecus coquereli) and mongoose lemur (Lemuridae: Eulemur mongoz), and their chemical structures were characterized by H-1-NMR spectroscopy. The oligosaccharide patterns observed among strepsirrhines did not appear to correlate to phylogeny, sociality or pattern of infant care. Both type I and type II neutral oligosaccharides were found in the milk of the aye-aye, but type II predominate over type I. Only type II oligosaccharides were identified in other strepsirrhine milks. alpha 3'-GL (isoglobotriose, Gal(alpha 1-3)Gal(beta 1-4)Glc) was found in the milks of Coquerel's sifaka and mongoose lemur, which is the first report of this oligosaccharide in the milk of any primate species. 2'-FL (Fuc(alpha 1-2)Gal(beta 1-4)Glc) was found in the milk of an aye-aye with an ill infant. Oligosaccharides containing the Lewis x epitope were found in aye-aye and mongoose lemur milk. Among acidic oligosaccharides, 3'-N-acetylneuraminyllactose (3'-SL-NAc, Neu5Ac(alpha 2-3)Gal(beta 1-4)Glc) was found in all studied species, whereas 6'-N-acetylneuraminyllactose (6'-SL-NAc, Neu5Ac(alpha 2-6)Gal(beta 1-4)Glc) was found in all species except greater galago. Greater galago milk also contained 3'-N-glycolylneuraminyllactose (3'-SL-NGc, Neu5Gc(alpha 2-3)Gal(beta 1-4)Glc). The finding of a variety of neutral and acidic oligosaccharides in the milks of strepsirrhines, as previously reported for haplorhines, suggests that such constituents are ancient rather than derived features, and are as characteristic of primate lactation is the classic disaccharide, lactose. C1 [Taufik, Epi; Fukuda, Kenji; Senda, Akitsugu; Urashima, Tadasu] Obihiro Univ Agr & Vet Med, Grad Sch Anim & Food Hyg, Obihiro, Hokkaido 0808555, Japan. [Saito, Tadao] Tohoku Univ, Grad Sch Agr, Sendai, Miyagi 980, Japan. [Williams, Cathy; Tilden, Chris] Duke Lemur Ctr, Durham, NC USA. [Eisert, Regina; Oftedal, Olav] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. RP Urashima, T (reprint author), Obihiro Univ Agr & Vet Med, Grad Sch Anim & Food Hyg, Obihiro, Hokkaido 0808555, Japan. EM urashima@obihiro.ac.jp OI Taufik, Epi/0000-0003-4617-9037 FU National Science Foundation [DBI-0549091] FX We thank Global COE Program "Frontier Program for Animal Global Health and Hygiene"; Ministry of Education, Culture, Sports, Science, and Technology, Japan for supporting the travel of Dr. Akitsugu Senda to the Smithsonian National Zoological Park (SNZP) in Washington, DC for the purpose of extracting carbohydrates from milk samples. We thank Kelly Glenn and the staff of the Duke Lemur Center for assistance with milk collection and Michael Jakubasz for his assistance at SNZP. A portion of the work at the Duke Lemur Center was supported by National Science Foundation grant # DBI-0549091. NR 54 TC 12 Z9 12 U1 3 U2 14 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0282-0080 EI 1573-4986 J9 GLYCOCONJUGATE J JI Glycoconjugate J. PD APR PY 2012 VL 29 IS 2-3 BP 119 EP 134 DI 10.1007/s10719-012-9370-9 PG 16 WC Biochemistry & Molecular Biology SC Biochemistry & Molecular Biology GA 917JC UT WOS:000302169200004 PM 22311613 ER PT J AU Torrez, L Robles, N Gonzalez, A Crofoot, MC AF Torrez, Lucia Robles, Nena Gonzalez, Anyuri Crofoot, Margaret C. TI Risky Business? Lethal Attack by a Jaguar Sheds Light on the Costs of Predator Mobbing for Capuchins (Cebus capucinus) SO INTERNATIONAL JOURNAL OF PRIMATOLOGY LA English DT Article DE Antipredator strategies; Barro Colorado Island; Cebus capucinus; Mobbing; Panthera onca ID WHITE-FACED CAPUCHIN; BOA-CONSTRICTOR; ANTIPREDATOR BEHAVIOR; FIELD OBSERVATION; FATAL ATTACK; MOUSE LEMUR; ALARM CALLS; MONKEYS; STRATEGIES; PRIMATE AB While some primates attempt to avoid predation by fleeing or hiding, others actually approach, harass, and sometimes attack potential predators, a behavior known as mobbing. Mobbing seems to invite obvious risks, but predators have rarely been observed to injure or kill animals that harass them. The true costs of predator mobbing and the functional significance of this behavior remain poorly understood. Here, we report a fatal attack by a jaguar (Panthera onca) on a mobbing capuchin (Cebus capucinus) that we observed on Barro Colorado Island, Panama. This rare observation illustrates that mobbing predators such as large felids can, indeed, be costly. However, to understand fully the costs of mobbing, the energetic and opportunity costs that primates incur when they harass predators must also be considered. C1 [Crofoot, Margaret C.] Princeton Univ, Dept Ecol & Evolutionary Biol, Princeton, NJ 08544 USA. [Torrez, Lucia; Robles, Nena; Gonzalez, Anyuri; Crofoot, Margaret C.] Smithsonian Trop Res Inst, Panama City, Panama. [Crofoot, Margaret C.] Max Planck Inst Omithol, Div Migrat & Immunoecol, D-78315 Radolfzell am Bodensee, Germany. RP Crofoot, MC (reprint author), Princeton Univ, Dept Ecol & Evolutionary Biol, Princeton, NJ 08544 USA. EM crofootm@si.edu FU Smithsonian Tropical Research Institute; Wenner-Gren Foundation for Anthropological Research; Princeton University; Max Planck Institute for Ornithology; staff of the Barro Colorado Island research station FX We thank the Autoridad Nacional del Ambiente (ANAM) and the government of the Republic of Panama for permission to conduct this research. We thank the Smithsonian Tropical Research Institute, the Wenner-Gren Foundation for Anthropological Research, Princeton University, and the Max Planck Institute for Ornithology for funding. We also thank the staff of the Barro Colorado Island research station, whose daily help and support was critical to the success of this research. We extend special thanks to Jacalyn Giacalone, Ben Hirsch, Sara Pinzon, Roland Kays, and Oris Acevedo for their helpful comments and suggestions on a previous version of this manuscript. Two anonymous reviewers and Joanna Setchell provided thoughtful and constructive comments and criticisms that we gratefully acknowledge. NR 40 TC 6 Z9 7 U1 3 U2 35 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0164-0291 J9 INT J PRIMATOL JI Int. J. Primatol. PD APR PY 2012 VL 33 IS 2 BP 440 EP 446 DI 10.1007/s10764-012-9588-1 PG 7 WC Zoology SC Zoology GA 914VD UT WOS:000301979800010 ER PT J AU Sharp, KH Distel, D Paul, VJ AF Sharp, Koty H. Distel, Dan Paul, Valerie J. TI Diversity and dynamics of bacterial communities in early life stages of the Caribbean coral Porites astreoides SO ISME JOURNAL LA English DT Article DE Porites astreoides; coral larvae; bacteria; mucus ID BLACK BAND DISEASE; DINOFLAGELLATE PROROCENTRUM-LIMA; VERTICAL TRANSMISSION; SIDERASTREA-SIDEREA; OCULINA-PATAGONICA; SYMBIONTS; HOST; CYANOBACTERIA; LARVAE; POPULATIONS AB In this study, we examine microbial communities of early developmental stages of the coral Porites astreoides by sequence analysis of cloned 16S rRNA genes, terminal restriction fragment length polymorphism (TRFLP), and fluorescence in situ hybridization (FISH) imaging. Bacteria are associated with the ectoderm layer in newly released planula larvae, in 4-day-old planulae, and on the newly forming mesenteries surrounding developing septa in juvenile polyps after settlement. Roseobacter clade-associated (RCA) bacteria and Marinobacter sp. are consistently detected in specimens of P. astreoides spanning three early developmental stages, two locations in the Caribbean and 3 years of collection. Multi-response permutation procedures analysis on the TRFLP results do not support significant variation in the bacterial communities associated with P. astreoides larvae across collection location, collection year or developmental stage. The results are the first evidence of vertical transmission (from parent to offspring) of bacteria in corals. The results also show that at least two groups of bacterial taxa, the RCA bacteria and Marinobacter, are consistently associated with juvenile P. astreoides against a complex background of microbial associations, indicating that some components of the microbial community are long-term associates of the corals and may impact host health and survival. The ISME Journal (2012) 6, 790-801; doi:10.1038/ismej.2011.144; published online 24 November 2011 C1 [Sharp, Koty H.; Paul, Valerie J.] Smithsonian Marine Stn, Ft Pierce, FL USA. [Sharp, Koty H.; Distel, Dan] Ocean Genome Legacy, Ipswich, MA USA. RP Sharp, KH (reprint author), Eckerd Coll, 4200 54th Ave S, St Petersburg, FL 33711 USA. EM kotysharp@gmail.com RI Distel, Daniel/A-8047-2017 OI Distel, Daniel/0000-0002-3860-194X FU Smithsonian Marine Science Network; Mote Protect our Reefs Grants [POR-2007-15, POR-2009-16]; Philip Goelet Foundation; Ocean Genome Legacy FX Funding was provided through a Smithsonian Marine Science Network Postdoctoral Fellowship to KHS and Mote Protect our Reefs Grants (POR-2007-15 and POR-2009-16). KHS was supported by a postdoctoral research fellowship by the Philip Goelet Foundation and the Ocean Genome Legacy. We thank E Bartels and C Walter for their support of P. astreoides larval collection at Mote Marine Laboratory in the Florida Keys. In addition, we thank R Ritson-Williams for collection and maintenance of P. astreoides larvae in the Florida Keys and in Carrie Bow Cay, Belize. L Walters, K Ritchie, K Morrow, M Teplitski, C Krediet, B Engel, A Al-Agely, C Ross, K Grablow, K Arthur and K Semon assisted with P. astreoides larval collection and maintenance in the Florida Keys. We thank Margo Haygood at the Oregon Health and Sciences University for providing access to a Zeiss LSM510 laser confocal scanning microscope system, on which some of the images were taken. The remaining micrographs were taken on a Zeiss LSM510 at the Smithsonian Marine Station at Fort Pierce. We also thank the Belize Fisheries Department for providing us permits and facilitating our research in Belize to work with coral larvae at Carrie Bow Cay, Belize. Coral larvae in the Florida Keys were collected under permits FKNMS-2006-034, FKNMS-2008-018 and FKNMS-2009-031. This is contribution #863 from the Smithsonian Marine Station at Fort Pierce and contribution #910 from the CCRE program. NR 58 TC 42 Z9 43 U1 1 U2 45 PU NATURE PUBLISHING GROUP PI NEW YORK PA 75 VARICK ST, 9TH FLR, NEW YORK, NY 10013-1917 USA SN 1751-7362 J9 ISME J JI ISME J. PD APR PY 2012 VL 6 IS 4 BP 790 EP 801 DI 10.1038/ismej.2011.144 PG 12 WC Ecology; Microbiology SC Environmental Sciences & Ecology; Microbiology GA 914JJ UT WOS:000301945500009 PM 22113375 ER PT J AU Geller, MJ Diaferio, A Kurtz, MJ Dell'Antonio, IP Fabricant, DG AF Geller, Margaret J. Diaferio, Antonaldo Kurtz, Michael J. Dell'Antonio, Ian P. Fabricant, Daniel G. TI THE FAINT END OF THE LUMINOSITY FUNCTION AND LOW SURFACE BRIGHTNESS GALAXIES SO ASTRONOMICAL JOURNAL LA English DT Article DE galaxies: distances and redshifts; galaxies: dwarf; galaxies: fundamental parameters; galaxies: luminosity function, mass function ID FIBER-FED SPECTROGRAPH; PHOTOMETRIC REDSHIFTS; LOCAL UNIVERSE; STAR-FORMATION; SPACE DENSITY; FIELD; HECTOSPEC; CLUSTERS; CATALOG; SELECTION AB Smithsonian Hectospec Lensing Survey (SHELS) is a dense redshift survey covering a 4 deg(2) region to a limiting R = 20.6. In the construction of the galaxy catalog and in the acquisition of spectroscopic targets, we paid careful attention to the survey completeness for lower surface brightness dwarf galaxies. Thus, although the survey covers a small area, it is a robust basis for computation of the slope of the faint end of the galaxy luminosity function to a limiting M-R = -13.3 + 5logh. We calculate the faint-end slope in the R band for the subset of SHELS galaxies with redshifts in the range 0.02 <= z < 0.1, SHELS0.1. This sample contains 532 galaxies withR < 20.6 and with a median surface brightness within the half-light radius of SB50,(R) = 21.82 mag arcsec(-2). We used this sample to make one of the few direct measurements of the dependence of the faint end of the galaxy luminosity function on surface brightness. For the sample as a whole the faint-end slope, alpha = -1.31 +/- 0.04, is consistent with both the Blanton et al. analysis of the Sloan Digital Sky Survey and the Liu et al. analysis of the COSMOS field. This consistency is impressive given the very different approaches of these three surveys. A magnitude-limited sample of 135 galaxies with optical spectroscopic redshifts with mean half-light surface brightness, SB50,R >= 22.5 mag arcsec(-2) is unique to SHELS0.1. The faint-end slope is alpha(22.5) = -1.52 +/- 0.16. SHELS0.1 shows that lower surface brightness objects dominate the faint-end slope of the luminosity function in the field, underscoring the importance of surface brightness limits in evaluating measurements of the faint-end slope and its evolution. C1 [Geller, Margaret J.; Kurtz, Michael J.; Fabricant, Daniel G.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. [Diaferio, Antonaldo] Univ Turin, Dipartimento Fis Gen Amedeo Avogadro, I-10125 Turin, Italy. [Diaferio, Antonaldo] Ist Nazl Fis Nucl, Sez Torino, I-10125 Turin, Italy. [Diaferio, Antonaldo] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Dell'Antonio, Ian P.] Brown Univ, Dept Phys, Providence, RI 02912 USA. RP Geller, MJ (reprint author), Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA. EM mgeller@cfa.harvard.edu; adiaferio@cfa.harvard.edu; mkurtz@cfa.harvard.edu; ian@het.brown.edu; dfabricant@cfa.harvard.edu OI Kurtz, Michael/0000-0002-6949-0090 FU The Smithsonian Institution; NSF [AST-0708433]; INFN [PD51]; MIUR [2008NR3EBK_003] FX We thank Scott Kenyon for many insightful discussions. We thank Beth Willman for a discussion about Local Group dwarfs. We also thank Michael Strauss and Marijn Franx for encouraging us to use the SHELS survey as a basis for studying the local luminosity function. We thank Michael Blanton and his collaborators for providing the NYU-VAGC on line and we thank Martyn Plummer for his publicly available JAGS code. Perry Berlind and Michael Calkins operated the Hectospec efficiently and with extraordinary expertise. We thank Susan Tokarz for her dedication to careful data reduction. Nelson Caldwell deftly manages Hectospec queue scheduling for optimal scientific results. We thank the anonymous referee for urging us to improve the clarity of the presentation here. This paper makes use of data from the Sloan Digital Sky Survey. The Smithsonian Institution partially supported this research. NSF grant AST-0708433 supports Ian Dell'Antonio's research at Brown University. INFN grant PD51 and the PRIN-MIUR-2008 grant 2008NR3EBK_003 "Matter-antimatter asymmetry, dark matter, and dark energy in the LHC era" partially support Antonaldo Diaferio. NR 42 TC 17 Z9 17 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 J9 ASTRON J JI Astron. J. PD APR PY 2012 VL 143 IS 4 AR 102 DI 10.1088/0004-6256/143/4/102 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 913JE UT WOS:000301872800025 ER PT J AU Williams, RJ Mathur, S Poindexter, S Elvis, M Nicastro, F AF Williams, Rik J. Mathur, Smita Poindexter, Shawn Elvis, Martin Nicastro, Fabrizio TI A SPITZER-MIPS SEARCH FOR DUST IN COMPACT HIGH-VELOCITY H I CLOUDS SO ASTRONOMICAL JOURNAL LA English DT Article DE Galaxy: evolution; Galaxy: structure; infrared: ISM; ISM: general ID LOCAL GROUP ANALOGS; WARM-HOT GAS; GALACTIC HALO; MILKY-WAY; COMPLEX-C; MOLECULAR GAS; NEUTRAL HYDROGEN; SATELLITE GALAXIES; ANDROMEDA GALAXY; POPULATIONS AB We employ three-band Spitzer-MIPS observations to search for cold dust emission in three neutral hydrogen compact High-velocity clouds (CHVCs) in the vicinity of the Milky Way. Far-infrared emission correlated with H I column density was previously reported in HVC Complex C, indicating that this object contains dust heated by the Galactic radiation field at its distance of similar to 10 kpc. Assuming published Spitzer, IRAS, and Planck, IR-H I correlations for Complex C, our Spitzer observations are of sufficient depth to directly detect 160 mu m dust emission in the CHVCs if it is present at the same level as in Complex C, but no emission is detected in any of the targets. For one of the targets (CHVC289) which has well-localized H I clumps, we therefore conclude that it is fundamentally different from Complex C, with either a lower dust-to-gas ratio or a greater distance from the Galactic disk (and consequently cooler dust temperature). Firm conclusions cannot be drawn for the other two Spitzer-observed CHVCs since their small-scale H I structures are not sufficiently well known; nonetheless, no extended dust emission is apparent despite their relatively high H I column densities. The lack of dust emission in CHVC289 suggests that at least some compact high-velocity clouds objects may exhibit very low dust-to-gas ratios and/or greater Galactocentric distances than large HVC complexes. C1 [Williams, Rik J.] Carnegie Observ, Pasadena, CA 91101 USA. [Mathur, Smita; Poindexter, Shawn] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. [Mathur, Smita] Ohio State Univ, Ctr Cosmol & AstroParticle Phys, Columbus, OH 43210 USA. [Elvis, Martin; Nicastro, Fabrizio] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Nicastro, Fabrizio] Osserv Astron Roma, INAF, I-00040 Monte Porzio Catone, RM, Italy. RP Williams, RJ (reprint author), Carnegie Observ, 813 Santa Barbara St, Pasadena, CA 91101 USA. EM williams@obs.carnegiescience.edu OI Nicastro, Fabrizio/0000-0002-6896-1364 FU NASA [1289595]; Netherlands Organization for Scientific Research (NWO); Leids Kerkhoven-Bosscha Fonds; NSF [AST-0707417] FX We are grateful to the anonymous referee for comments that substantially improved the manuscript, and to the Spitzer team for their efforts with this remarkable instrument. Financial support for this work was provided by NASA through award number 1289595 issued by JPL/Caltech. R.J.W. acknowledges additional support from the Netherlands Organization for Scientific Research (NWO), the Leids Kerkhoven-Bosscha Fonds, and NSF grant AST-0707417. This research has made use of the NASA/IPAC Extragalactic Database (NED) which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. NR 55 TC 1 Z9 1 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 J9 ASTRON J JI Astron. J. PD APR PY 2012 VL 143 IS 4 AR 82 DI 10.1088/0004-6256/143/4/82 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 913JE UT WOS:000301872800005 ER PT J AU Pask, JD Woodhams, DC Rollins-Smith, LA AF Pask, James D. Woodhams, Douglas C. Rollins-Smith, Louise A. TI The ebb and flow of antimicrobial skin peptides defends northern leopard frogs (Rana pipiens) against chytridiomycosis SO GLOBAL CHANGE BIOLOGY LA English DT Article DE amphibian; antimicrobial peptides; Batrachochytrium dendrobatidis; brevinin; chytridiomycosis; Rana pipiens; ranatuerin; skin defenses ID EMERGING INFECTIOUS-DISEASE; GLOBAL AMPHIBIAN DECLINES; INNATE IMMUNE DEFENSES; YELLOW-LEGGED FROG; BATRACHOCHYTRIUM-DENDROBATIDIS; CHYTRID FUNGUS; POPULATION DECLINES; CENTRAL-AMERICA; MORTALITY; PATHOGENESIS AB Many amphibian species are threatened with extinction by the emerging infectious disease, chytridiomycosis, caused by the fungus Batrachochytrium dendrobatidis. This unprecedented global crisis threatens to reduce the biodiversity of the entire amphibian class. The fungus invades the skin and impairs the uptake and retention of essential ions leading to cardiac arrest. Antimicrobial peptides (AMPs) secreted into the mucus of some amphibians are thought to be an important defense against chytridiomycosis. However, little is known about the quantities of AMPs secreted under natural conditions, whether they are sufficient to protect against this pathogen, and how they interact with commensal microbes. To understand how defensive peptides and skin microbes may interact, it is essential to know the precise quantities of AMPs present under natural conditions. Using matrix-assisted laser desorption time-of-flight mass spectrometry and growth inhibition assays, we show that northern leopard frogs (Rana pipiens) at rest constitutively release low amounts of AMPs that inhibit B. dendrobatidis in vitro, and AMP defenses are elevated following a simulated predator attack. Using a synthetic peptide analogue of brevinin-1Pb as an external control, we quantified the amounts of four previously described AMPs (brevinin 1Pa, brevinin-1Pb, brevinin-1Pd, and ranatuerin-2P) at several time points after secretion. Once secreted onto the skin, the peptides are most active for 15 min, and small quantities persist for at least 2 h. Taken together, our data suggest that small amounts of AMPs are rapidly available and quite stable on the skin of R. pipiens. They are effective inhibitors of B. dendrobatidis at these low constitutive concentrations but degrade within 2 h, protecting the integrity of the skin and commensal bacteria. C1 [Pask, James D.; Rollins-Smith, Louise A.] Vanderbilt Univ, Dept Pathol Microbiol & Immunol, Med Ctr, Nashville, TN 37232 USA. [Woodhams, Douglas C.] Univ Zurich, Inst Evolutionary Biol & Environm Studies, CH-8057 Zurich, Switzerland. [Woodhams, Douglas C.; Rollins-Smith, Louise A.] Smithsonian Inst, Natl Zool Pk, Ctr Species Survival Conservat & Sci, Washington, DC 20013 USA. [Rollins-Smith, Louise A.] Vanderbilt Univ, Dept Pathol, Med Ctr, Nashville, TN 37232 USA. [Rollins-Smith, Louise A.] Vanderbilt Univ, Dept Microbiol & Immunol, Med Ctr, Nashville, TN 37232 USA. [Rollins-Smith, Louise A.] Vanderbilt Univ, Dept Biol Sci, Med Ctr, Nashville, TN 37232 USA. RP Rollins-Smith, LA (reprint author), Vanderbilt Univ, Dept Pathol Microbiol & Immunol, Med Ctr, A-5301 Med Ctr N, Nashville, TN 37232 USA. EM louise.rollins-smith@vanderbilt.edu FU National Science Foundation [IBN-0131184, IOS-0619536, IOS-0843207]; Swiss National Science Foundation [31-125099] FX This research was supported by National Science Foundation Grants IBN-0131184, IOS-0619536, and IOS-0843207 (to L. R-S) and the Swiss National Science Foundation (31-125099 to D. C. W.). We wish to acknowledge the use of the Vanderbilt University Medical Center Mass Spectrometry Core. NR 37 TC 22 Z9 22 U1 5 U2 47 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 1354-1013 J9 GLOBAL CHANGE BIOL JI Glob. Change Biol. PD APR PY 2012 VL 18 IS 4 BP 1231 EP 1238 DI 10.1111/j.1365-2486.2011.02622.x PG 8 WC Biodiversity Conservation; Ecology; Environmental Sciences SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 909AB UT WOS:000301533100003 ER PT J AU Rutz, C Ryder, TB Fleischer, RC AF Rutz, C. Ryder, T. B. Fleischer, R. C. TI Restricted gene flow and fine-scale population structuring in tool using New Caledonian crows SO NATURWISSENSCHAFTEN LA English DT Article DE Bayesian clustering; Culture; Microsatellites; Genetic population structure; Social learning; Tool use ID MULTILOCUS GENOTYPE DATA; CORVUS-MONEDULOIDES; WILD CHIMPANZEES; APHELOCOMA-COERULESCENS; CULTURAL-EVOLUTION; ANIMAL CULTURES; SCRUB-JAYS; BEHAVIOR; MANUFACTURE; MICROSATELLITES AB New Caledonian crows Corvus moneduloides are the most prolific avian tool users. It has been suggested that some aspects of their complex tool use behaviour are under the influence of cultural processes, involving the social transmission-and perhaps even progressive refinement-of tool designs. Using microsatellite and mt-haplotype profiling of crows from three distinct habitats (dry forest, farmland and beachside habitat), we show that New Caledonian crow populations can exhibit significant fine-scale genetic structuring. Our finding that some sites of < 10 km apart were highly differentiated demonstrates considerable potential for genetic and/or cultural isolation of crow groups. Restricted movement of birds between local populations at such small spatial scales, especially across habitat boundaries, illustrates how specific tool designs could be preserved over time, and how tool technologies of different crow groups could diverge due to drift and local selection pressures. Young New Caledonian crows have an unusually long juvenile dependency period, during which they acquire complex tool-related foraging skills. We suggest that the resulting delayed natal dispersal drives population-divergence patterns in this species. Our work provides essential context for future studies that examine the genetic makeup of crow populations across larger geographic areas, including localities with suspected cultural differences in crow tool technologies. C1 [Rutz, C.] Univ Oxford, Dept Zool, Oxford OX1 3PS, England. [Ryder, T. B.; Fleischer, R. C.] Smithsonian Conservat Biol Inst, Ctr Conservat & Evolutionary Genet, Washington, DC 20013 USA. RP Rutz, C (reprint author), Univ Oxford, Dept Zool, S Parks Rd, Oxford OX1 3PS, England. EM christian.rutz@zoo.ox.ac.uk FU BBSRC (Biotechnology and Biological Sciences Research Council) [BB/G023913/1]; Province Sud; Direction de l'Environnement (DENV); SEM Mwe Ara (Gouaro-Deva) FX Special thanks to L. A. Bluff who set up the field project together with C. R. in 2005, and to A. Weir and A. Kacelnik for sharing its early stages. We are also grateful to L. A. Bluff, J. Troscianko, A. Bayern and several field volunteers for assistance with crow trapping over the years; C. Lambert, T. Mennesson, J.-Y. Lemenant, S. Blancher, J. Bourget, N. Barre, J.-P. Richard and J. Paimbou-Ayouma for support in New Caledonia; N. McInerney for help with lab work; and three anonymous referees for excellent comments on the manuscript. This research was funded through a BBSRC (Biotechnology and Biological Sciences Research Council) David Phillips Fellowship to C. R. (BB/G023913/1), with additional generous support in New Caledonia from the Province Sud, the Direction de l'Environnement (DENV) and SEM Mwe Ara (Gouaro-Deva). Research was carried out with permissions from the DENV and the Direction de Resources Naturelles (Province Sud, New Caledonia) and was approved by Oxford University's local ethical review committee. NR 50 TC 11 Z9 11 U1 1 U2 33 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0028-1042 J9 NATURWISSENSCHAFTEN JI Naturwissenschaften PD APR PY 2012 VL 99 IS 4 BP 313 EP 320 DI 10.1007/s00114-012-0904-6 PG 8 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 913BU UT WOS:000301847200008 PM 22418860 ER PT J AU Briceno, RD Eberhard, WG AF Briceno, R. D. Eberhard, W. G. TI Spiders avoid sticking to their webs: clever leg movements, branched drip-tip setae, and anti-adhesive surfaces SO NATURWISSENSCHAFTEN LA English DT Article DE Spider webs; Anti-adhesives; Drip-tip setae; Behavior ID ORB-WEAVING SPIDERS; VISCOUS CAPTURE THREADS AB Orb-weaving spiders construct webs with adhesive silk but are not trapped by it. Previous studies have attributed this defense to an oily coating on their legs that protects against adhesion or, more recently, to behavioral avoidance of sticky lines. The old evidence is very weak, however, and the behavioral avoidance explanation is inadequate because orb-weavers push with their hind legs against sticky lines hundreds or thousands of times during construction of each orb and are not trapped. Video analyses of behavior and experimental observations of isolated legs pulling away from contact with sticky lines showed that the spider uses three anti-adhesion traits: dense arrays of branched setae on the legs that reduce the area of contact with adhesive material; careful engagement and withdrawal movements of its legs that minimize contact with the adhesive and that avoid pulling against the line itself; and a chemical coating or surface layer that reduces adhesion. C1 [Briceno, R. D.; Eberhard, W. G.] Univ Costa Rica, Escuela Biol, San Pedro, Costa Rica. [Eberhard, W. G.] Smithsonian Trop Res Inst, Panama, Costa Rica. RP Briceno, RD (reprint author), Univ Costa Rica, Escuela Biol, San Pedro, Costa Rica. EM daniel.briceno@ucr.ac.cr FU Smithsonian Tropical Research Institute; Universidad de Costa Rica FX We thank Brent Opell, Julio Mata, Mavis Montero, and Jerome Rovner for advice; Diego Gonzalez-Florez for permission to cite unpublished observations; personnel of the Parque Braulio Carillo; and the Smithsonian Tropical Research Institute and the Universidad de Costa Rica for financial support. NR 18 TC 3 Z9 3 U1 1 U2 31 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0028-1042 J9 NATURWISSENSCHAFTEN JI Naturwissenschaften PD APR PY 2012 VL 99 IS 4 BP 337 EP 341 DI 10.1007/s00114-012-0901-9 PG 5 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 913BU UT WOS:000301847200012 PM 22382404 ER PT J AU Hughey, MC Nicolas, A Vonesh, JR Warkentin, KM AF Hughey, Myra C. Nicolas, Angie Vonesh, James R. Warkentin, Karen M. TI Wasp predation drives the assembly of fungal and fly communities on frog egg masses SO OECOLOGIA LA English DT Article DE Processing chain; Colonization; Priority effects; Facilitation; Ephemeral microhabitats ID PROCESSING CHAIN INTERACTION; EYED TREEFROG EGGS; POSITIVE INTERACTIONS; INTERSPECIFIC INTERACTIONS; SPORE DISPERSAL; FOOD-WEB; FACILITATION; PRIORITY; SUCCESSION; DROSOPHILA AB Community ecology aims to understand how species interactions shape species diversity and abundance. Although less studied than predatory or competitive interactions, facilitative interactions can be important in communities associated with ephemeral microhabitats. Successful recruitment from these habitats requires species to rapidly colonize, develop, and disperse during brief periods of habitat suitability. Interactions between organisms, including processing chain interactions whereby initial consumers alter resources in ways that improve their quality for subsequent consumers, could aid these processes. The terrestrial egg masses of red-eyed treefrogs (Agalychnis callidryas) are a resource for predatory wasps (Agelaia spp., Polybia rejecta) and a microhabitat and resource for saprovoric and pathogenic fungi and saprovoric flies (Megaselia spp., Psychoda savaiiensis). We investigate how interactions with wasps might facilitate fly and fungal colonization of and survival on frog egg masses. Our results indicate that wasps facilitate fungal colonization, whereas flies appear not to, and that both wasps and fungi generate frog egg carrion that attracts saprovoric flies to oviposit and increases the survival of fly larvae. While studies of colonization order often focus on inhibition by early colonizers of subsequent arrivals, this study demonstrates how early colonizers can facilitate the establishment of later ones, by modifying resources in ways that promote the location of and survival in habitat patches. This research draws attention to the diversity of interactions that can occur within ephemeral communities and emphasizes the role that positive interactions may play. Processing chain interactions may be a generally important mechanism increasing the diversity of local communities, including very ephemeral ones. C1 [Hughey, Myra C.; Nicolas, Angie; Warkentin, Karen M.] Boston Univ, Dept Biol, Boston, MA 02215 USA. [Vonesh, James R.] Virginia Commonwealth Univ, Dept Biol, Richmond, VA 23284 USA. [Warkentin, Karen M.] Smithsonian Trop Res Inst, Panama City 084303092, Panama. RP Hughey, MC (reprint author), Smithsonian Trop Res Inst, Panama City 084303092, Panama. EM myrahughey@gmail.com RI Vonesh, James/I-1573-2013 OI Vonesh, James/0000-0003-2481-9988 FU National Science Foundation [IOB-0234439, DEB-0716923, DEB-0717220, DEB-0910270]; Lewis and Clark Fund for Exploration Award; American Society of Ichthyologists and Herpetologists; Boston University; Smithsonian Tropical Research Institute FX We thank the Smithsonian Tropical Research Institute for laboratory space and logistical support, and W. Wcislo and M. J. West-Eberhard for advice. B. Brown identified flies. J. Touchon and three anonymous reviewers provided helpful comments on the manuscript. Animal use and collection was permitted by the Autoridad Nacional del Ambiente of Panama (ANAM permits SE/A-54-06 and SE/A-41-08) and approved by the Boston University Institutional Animal Care and Use Committeee (IACUC protocols 05-022 and 08-011). This work was funded by the National Science Foundation (grants IOB-0234439, DEB-0716923, DEB-0717220, DEB-0910270), a Lewis and Clark Fund for Exploration Award, an American Society of Ichthyologists and Herpetologists Gaige Fund Award, Boston University, and a short-term fellowship from the Smithsonian Tropical Research Institute. NR 61 TC 0 Z9 0 U1 2 U2 27 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0029-8549 J9 OECOLOGIA JI Oecologia PD APR PY 2012 VL 168 IS 4 BP 1057 EP 1068 DI 10.1007/s00442-011-2137-3 PG 12 WC Ecology SC Environmental Sciences & Ecology GA 909YR UT WOS:000301604200016 PM 22011841 ER PT J AU Asner, GP Mascaro, J Muller-Landau, HC Vieilledent, G Vaudry, R Rasamoelina, M Hall, JS van Breugel, M AF Asner, Gregory P. Mascaro, Joseph Muller-Landau, Helene C. Vieilledent, Ghislain Vaudry, Romuald Rasamoelina, Maminiaina Hall, Jefferson S. van Breugel, Michiel TI A universal airborne LiDAR approach for tropical forest carbon mapping SO OECOLOGIA LA English DT Article DE Biomass; Carbon emissions; Forest carbon; Light detection and ranging; Rain forest; REDD; Remote sensing ID WOOD DENSITY; ABOVEGROUND BIOMASS; CANOPY STRUCTURE; FOOTPRINT LIDAR; RAIN-FORESTS; PATTERNS; ALLOMETRY; USA AB Airborne light detection and ranging (LiDAR) is fast turning the corner from demonstration technology to a key tool for assessing carbon stocks in tropical forests. With its ability to penetrate tropical forest canopies and detect three-dimensional forest structure, LiDAR may prove to be a major component of international strategies to measure and account for carbon emissions from and uptake by tropical forests. To date, however, basic ecological information such as height-diameter allometry and stand-level wood density have not been mechanistically incorporated into methods for mapping forest carbon at regional and global scales. A better incorporation of these structural patterns in forests may reduce the considerable time needed to calibrate airborne data with ground-based forest inventory plots, which presently necessitate exhaustive measurements of tree diameters and heights, as well as tree identifications for wood density estimation. Here, we develop a new approach that can facilitate rapid LiDAR calibration with minimal field data. Throughout four tropical regions (Panama, Peru, Madagascar, and Hawaii), we were able to predict aboveground carbon density estimated in field inventory plots using a single universal LiDAR model (r (2) = 0.80, RMSE = 27.6 Mg C ha(-1)). This model is comparable in predictive power to locally calibrated models, but relies on limited inputs of basal area and wood density information for a given region, rather than on traditional plot inventories. With this approach, we propose to radically decrease the time required to calibrate airborne LiDAR data and thus increase the output of high-resolution carbon maps, supporting tropical forest conservation and climate mitigation policy. C1 [Asner, Gregory P.; Mascaro, Joseph] Carnegie Inst Sci, Dept Global Ecol, Stanford, CA 94305 USA. [Mascaro, Joseph; Muller-Landau, Helene C.; Hall, Jefferson S.; van Breugel, Michiel] Smithsonian Trop Res Inst, Panama City, Panama. [Vieilledent, Ghislain] CIRAD, Forest Ecosyst Goods & Serv UR105, F-34398 Montpellier 5, France. [Vieilledent, Ghislain] DRP Foret & Biodivers, Antananarivo, Madagascar. [Vaudry, Romuald] GoodPlanet Fdn, F-75116 Paris, France. [Rasamoelina, Maminiaina] World Wide Fund Nat, Antananarivo, Madagascar. RP Asner, GP (reprint author), Carnegie Inst Sci, Dept Global Ecol, 260 Panama St, Stanford, CA 94305 USA. EM gpa@stanford.edu RI Vieilledent, Ghislain/D-8323-2011; Asner, Gregory/G-9268-2013; OI Vieilledent, Ghislain/0000-0002-1685-4997; Asner, Gregory/0000-0001-7893-6421; van Breugel, Michiel/0000-0003-2778-7803 FU Gordon and Betty Moore Foundation; Moore Foundation; John D. and Catherine T. MacArthur Foundation; HSBC; Air France; Smithsonian Tropical Research Institute; Government of Norway; Secretaria Nacional de Ciencia, Tecnologia e Innovacion (SENACYT) of Panama; Carnegie Institution FX We thank J. Jacobson, T. Kennedy-Bowdoin, D. Knapp, and the Carnegie Airborne Observatory team for collecting and processing airborne LiDAR data. We thank two anonymous reviewers, N. Buchmann and C. Korner, for comments that improved the manuscript. This study was supported by the Gordon and Betty Moore Foundation. Previous data collections were supported by the Moore Foundation, the John D. and Catherine T. MacArthur Foundation, the HSBC Climate Partnership, Air France, the Smithsonian Tropical Research Institute, the Government of Norway, the Secretaria Nacional de Ciencia, Tecnologia e Innovacion (SENACYT) of Panama, the Carnegie Institution, and an anonymous donor to the Agua Salud Project. The Carnegie Airborne Observatory is made possible by the W. M. Keck Foundation, the Gordon and Betty Moore Foundation, and William Hearst III. NR 52 TC 110 Z9 116 U1 15 U2 115 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 APR PY 2012 VL 168 IS 4 BP 1147 EP 1160 DI 10.1007/s00442-011-2165-z PG 14 WC Ecology SC Environmental Sciences & Ecology GA 909YR UT WOS:000301604200024 PM 22033763 ER PT J AU Clough, GW AF Clough, G. Wayne TI DISCOVERY'S NEXT MISSION SO SMITHSONIAN LA English DT Editorial Material C1 Smithsonian Inst, Washington, DC 20560 USA. RP Clough, GW (reprint author), Smithsonian Inst, Washington, DC 20560 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU SMITHSONIAN ASSOC PI WASHINGTON PA 900 JEFFERSON DR, WASHINGTON, DC 20560 USA SN 0037-7333 J9 SMITHSONIAN JI Smithsonian PD APR PY 2012 VL 43 IS 1 BP 10 EP 10 PG 1 WC Humanities, Multidisciplinary SC Arts & Humanities - Other Topics GA 126SR UT WOS:000317642000007 ER PT J AU Schemm-Gregory, M Rojas-Briceno, A Patarroyo, P Jaramillo, C AF Schemm-Gregory, Mena Rojas-Briceno, Alexis Patarroyo, Pedro Jaramillo, Carlos TI First report of Hadrosia Cooper, 1983 in South America and its biostratigraphical and palaeobiogeographical implications SO CRETACEOUS RESEARCH LA English DT Article DE Terebratulida; Brachiopoda; Rosablanca Formation; Lower Cretaceous; Colombia ID CRETACEOUS BRACHIOPODS; COLOMBIA; CARBON; GENUS; AFFINITIES; EVENTS; FAUNAS; MEXICO; BASIN AB A new terebratulid species, Hadrosia gracilis, from the Lower Cretaceous Rosablanca Formation in Central Colombia is described. The new method of three-dimensional reconstructions of the internal morphology of this taxon results in the subjective synonymization of the Nerthebrochinae in favour of the Sellithyridinae. The geographical distribution of species of Hadrosia in South America and Western Europe is a further argument for a direct pathway between these two regions during Early Cretaceous time. (C) 2011 Elsevier Ltd. All rights reserved. C1 [Schemm-Gregory, Mena; Rojas-Briceno, Alexis; Jaramillo, Carlos] Smithsonian Trop Res Inst, Panama City, Panama. [Schemm-Gregory, Mena] Senckenberg Forschungsinst, D-60325 Frankfurt, Germany. [Schemm-Gregory, Mena] Nat Museum Frankfurt, D-60325 Frankfurt, Germany. [Patarroyo, Pedro] Univ Nacl Colombia, Dept Geociencias, Bogota 14490, Colombia. RP Schemm-Gregory, M (reprint author), Univ Coimbra, Ctr Geosci, P-3000272 Largo Marques De Pombal, Portugal. EM Mena_Schemm@gmx.de; RojasA@si.edu; pcpatarroyog@unal.edu.co; jaramilloC@si.edu RI Schemm-Gregory, Mena/B-3750-2013 FU Smithsonian Tropical Research Institute FX The research of MS-G in Panama was partly financed by the Smithsonian Tropical Research Institute. The visit of AR-B to the Peabody Museum, Yale University was paid by a Charles Schuchert and Carl O. Dunbar Grant Both authors acknowledge the following at the Senckenberg Forschungsinstitut und Naturmuseum, Frankfurt am Main, Germany: Bernhard Stribrny for providing access to the laboratory; Tina Emmel and Michael Ricker for technical help; Claudia Franz for the SEM images. MS-G is grateful to Eberhard Schindler of the same institute for providing her with working space. Michael Brett-Surman (USNM) took the photographs of the Cooper's material. PP thanks the company of geology students of the Universidad Nacional de Colombia, during the field work in Santa Sofia. The manuscript has greatly benefited from the comments by Robert B. Blodgett (Anchorage, USA) and Miguel O. Mancenido (Museo Ciencias Naturales de La Plata, Argentina). NR 107 TC 2 Z9 2 U1 0 U2 3 PU ACADEMIC PRESS LTD- ELSEVIER SCIENCE LTD PI LONDON PA 24-28 OVAL RD, LONDON NW1 7DX, ENGLAND SN 0195-6671 EI 1095-998X J9 CRETACEOUS RES JI Cretac. Res. PD APR PY 2012 VL 34 BP 257 EP 267 DI 10.1016/j.cretres.2011.11.005 PG 11 WC Geology; Paleontology SC Geology; Paleontology GA 902GS UT WOS:000301027200023 ER PT J AU Averianov, A Sues, HD AF Averianov, Alexander Sues, Hans-Dieter TI Skeletal remains of Tyrannosauroidea (Dinosauria: Theropoda) from the Bissekty Formation (Upper Cretaceous: Turonian) of Uzbekistan SO CRETACEOUS RESEARCH LA English DT Article DE Dinosauria; Theropoda; Tyrannosauroidea; Cretaceous; Uzbekistan ID IREN DABASU FORMATION; MONGOLIA; CHINA AB There exists a major gap in the fossil record of tyrannosauroid theropod dinosaurs spanning the early part of the Late Cretaceous. We report on skeletal remains referable to Tyrannosauroidea indet. from the Turonian Bissekty Formation at Dzharakuduk in the central Kyzylkum Desert of Uzbekistan. Phylogenetic analysis of the hypodigm places the Bissekty tyrannosauroid as a non-tyrannosaurid tyrannosauroid more basal than the Campanian tyrannosauroids Appalachiosaurus and Bistahieversor from North America. (C) 2011 Elsevier Ltd. All rights reserved. C1 [Averianov, Alexander] Russian Acad Sci, Inst Zool, St Petersburg 199034, Russia. [Sues, Hans-Dieter] Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20013 USA. RP Averianov, A (reprint author), Russian Acad Sci, Inst Zool, Univ Skaya Nab 1, St Petersburg 199034, Russia. EM dzharakuduk@mail.ru; suesh@si.edu RI Averianov, Alexander/M-8490-2013 OI Averianov, Alexander/0000-0001-5948-0799 FU National Science Foundation [EAR-9804771, EAR-0207004]; National Geographic Society [5901-97, 6281-98]; Navoi Mining and Metallurgy Combinat; Civilian Research and Development Foundation [RU-G1-2571-ST-04, RUB1-2860-ST-07]; Russian Fund of Basic Research [07-04-91110-AFGIRa]; St. Petersburg State University [NIR 3.39.148.2011]; Ministry of Education and Science of Russian Federation [16.518.11.7070] FX The continued cooperation of the Zoological Institute of the National Academy of Sciences of Uzbekistan, notably D.A. Azimov and Y.A. Chikin, is greatly appreciated. We thank our fellow members of the URBAC expeditions, A.V. Abramov, J.D. Archibald, G.O. Cherepanov, I.G. Danilov, S. Dominguez, C. King, N. Morris, C.M. Redman, AS. Resvyi, C. Skrabec, P.P. Skutschas, E.V. Syromyatnikova, and D.J. Ward, for their efforts in the field, scientific expertise, and camaraderie. We gratefully acknowledge the financial support of the National Science Foundation (EAR-9804771 and EAR-0207004 to J.D. Archibald and H.-D. Sues), the National Geographic Society (#5901-97 and #6281-98 to J.D. Archibald and H.-D. Sues), the Navoi Mining and Metallurgy Combinat, the Civilian Research and Development Foundation (RU-G1-2571-ST-04 and RUB1-2860-ST-07), and the Russian Fund of Basic Research (07-04-91110-AFGIRa). AA also received research support from St. Petersburg State University grant NIR 3.39.148.2011 and Ministry of Education and Science of Russian Federation contract 16.518.11.7070. We thank Thomas D. Carr (Carthage College) for his meticulous review of this paper as well as helpful comments and suggestions. NR 35 TC 9 Z9 9 U1 0 U2 3 PU ACADEMIC PRESS LTD- ELSEVIER SCIENCE LTD PI LONDON PA 24-28 OVAL RD, LONDON NW1 7DX, ENGLAND SN 0195-6671 J9 CRETACEOUS RES JI Cretac. Res. PD APR PY 2012 VL 34 BP 284 EP 297 DI 10.1016/j.cretres.2011.11.009 PG 14 WC Geology; Paleontology SC Geology; Paleontology GA 902GS UT WOS:000301027200025 ER PT J AU Uribe, MC Grier, HJ Parenti, LR AF Carmen Uribe, Mari Grier, Harry J. Parenti, Lynne R. TI Ovarian structure and oogenesis of the oviparous goodeids Crenichthys baileyi (Gilbert, 1893) and Empetrichthys latos Miller, 1948 (teleostei, Cyprinodontiformes) SO JOURNAL OF MORPHOLOGY LA English DT Article DE oogenesis; zona pellucida; micropyle; delle; viviparity; killifish; Atherinomorpha ID FUNDULUS-HETEROCLITUS; VIVIPAROUS TELEOST; OOCYTE GROWTH; XIPHOPHORUS-HELLERI; REPRODUCTIVE-CYCLE; NEOTOCA BILINEATA; CORTICAL ALVEOLI; PRIMARY ENVELOPE; FINE-STRUCTURE; FISHES AB The cyprinodontiform family Goodeidae comprises two biogeographically disjunct subfamilies: the viviparous Goodeinae endemic to the Mexican Plateau, and the oviparous Empetrichthyinae, known only from relict taxa in Nevada and California. Ovarian characteristics of two oviparous species of goodeid, Crenichthys baileyi and Empetrichthys latos, studied using museum collections, are compared with those of viviparous species of goodeids. Both subfamilies have a single, cystovarian ovary. The ovary in the viviparous Goodeinae has an internal septum that divides the ovarian lumen into two compartments, and it may possess oogonia. There is no ovarian septum in the oviparous C. baileyi and E. latos. Oogenesis is similar in both subfamilies with regard to the proliferation of oogonia, initiation of meiosis, primary growth and development of an oocyte during secondary growth in which fluid yolk progressively fuses into a single globule. Notably, eggs of C. baileyi and E. latos are approximately double the size of those of the viviparous Goodeinae in which embryos develop inside the ovarian lumen and are nourished, in part, by nutrients transferred from the maternal tissues, a mode of embryo development called matrotrophy. Egg envelopes of the two subfamilies differ in that those of C. baileyi and E. latos have a relatively thick zona pellucida, attachment fibrils or filaments that develop between the follicle cells during oogenesis, and a micropyle observed only in E. latos. In contrast, viviparous goodeid eggs have a relatively thin zona pellucida, but lack adhesive fibrils, and a micropyle was not observed. These reproductive characters are compared with those of species of the eastern North American Fundulus, a representative oviparous cyprinodontiform. One newlyrecognized shared, derived character, a single, median ovoid ovary with no obvious external evidence of fusion, supports monophyly of the Goodeidae. Differences among the goodeid subfamilies and Fundulus are interpreted relative to the oviparous versus viviparous modes of reproduction. J. Morphol., 2012. (c) 2011 Wiley Periodicals, Inc. C1 [Carmen Uribe, Mari] Univ Nacl Autonoma Mexico, Fac Ciencias, Dept Biol Comparada, Lab Biol Reprod Anim, Mexico City 04510, DF, Mexico. [Grier, Harry J.; Parenti, Lynne R.] Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Div Fishes, Washington, DC 20013 USA. [Grier, Harry J.] Florida Fish & Wildlife Res Inst, St Petersburg, FL 33701 USA. RP Uribe, MC (reprint author), Univ Nacl Autonoma Mexico, Fac Ciencias, Dept Biol Comparada, Lab Biol Reprod Anim, Ciudad Univ,Insurgentes Sur 3000, Mexico City 04510, DF, Mexico. EM uribearanzabal@yahoo.com.mx NR 80 TC 6 Z9 6 U1 1 U2 19 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0362-2525 J9 J MORPHOL JI J. Morphol. PD APR PY 2012 VL 273 IS 4 BP 371 EP 387 DI 10.1002/jmor.11028 PG 17 WC Anatomy & Morphology SC Anatomy & Morphology GA 900GV UT WOS:000300875800002 PM 22109541 ER PT J AU Paerl, HW Paul, VJ AF Paerl, Hans W. Paul, Valerie J. TI Climate change: Links to global expansion of harmful cyanobacteria SO WATER RESEARCH LA English DT Article DE Cyanobacteria; Eutrophication; Climate change; Hydrology; Nutrients; Freshwater; Marine; Water quality management ID BLOOM-FORMING CYANOBACTERIA; NORTH-ATLANTIC OSCILLATION; LARGE SHALLOW LAKE; DUAL NUTRIENT N; LYNGBYA-MAJUSCULA; MICROCYSTIS-AERUGINOSA; NITROGEN-FIXATION; ALGAL BLOOMS; MORETON BAY; BALTIC SEA AB Cyanobacteria are the Earth's oldest (similar to 3.5 bya) oxygen evolving organisms, and they have had major impacts on shaping our modern-day biosphere. Conversely, biospheric environmental perturbations, including nutrient enrichment and climatic changes (e.g. global warming, hydrologic changes, increased frequencies and intensities of tropical cyclones, more intense and persistent droughts), strongly affect cyanobacterial growth and bloom potentials in freshwater and marine ecosystems. We examined human and climatic controls on harmful (toxic, hypoxia-generating, food web disrupting) bloom-forming cyanobacteria (CyanoHABs) along the freshwater to marine continuum. These changes may act synergistically to promote cyanobacterial dominance and persistence. This synergy is a formidable challenge to water quality, water supply and fisheries managers, because bloom potentials and controls may be altered in response to contemporaneous changes in thermal and hydrologic regimes. In inland waters, hydrologic modifications, including enhanced vertical mixing and, if water supplies permit, increased flushing (reducing residence time) will likely be needed in systems where nutrient input reductions are neither feasible nor possible. Successful control of CyanoHABs by grazers is unlikely except in specific cases. Overall, stricter nutrient management will likely be the most feasible and practical approach to long-term CyanoHAB control in a warmer, stormier and more extreme world. (C) 2011 Elsevier Ltd. All rights reserved. C1 [Paerl, Hans W.] Univ N Carolina, Inst Marine Sci, Morehead City, NC 28557 USA. [Paul, Valerie J.] Smithsonian Marine Stn, Ft Pierce, FL 34949 USA. RP Paerl, HW (reprint author), Univ N Carolina, Inst Marine Sci, 3431 Arendell St, Morehead City, NC 28557 USA. EM hpaerl@email.unc.edu; Paul@si.edu RI Osborne, Nicholas/N-4915-2015 OI Osborne, Nicholas/0000-0002-6700-2284 FU National Science Foundation [OCE 07269989, 0812913, 0825466, CBET 0826819]; U.S. Dept. of Agriculture NRI [00-35101-9981]; U.S. EPA-STAR [R82867701]; NOAA/EPA-ECOHAB [NA05NOS4781194]; North Carolina Sea Grant Program [R/MER-47] FX We thank A. Joyner, N. Hall and T. Otten for technical assistance and J. Huisman, J. Dyble Bressie, and A. Wilson for helpful discussions. This work was supported by the National Science Foundation (OCE 07269989, 0812913, 0825466, and CBET 0826819), the U.S. Dept. of Agriculture NRI Project 00-35101-9981, U.S. EPA-STAR project R82867701, NOAA/EPA-ECOHAB Project NA05NOS4781194, and North Carolina Sea Grant Program R/MER-47. This is contribution #853 of the Smithsonian Marine Station at Fort Pierce. NR 160 TC 282 Z9 301 U1 57 U2 399 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0043-1354 J9 WATER RES JI Water Res. PD APR 1 PY 2012 VL 46 IS 5 SI SI BP 1349 EP 1363 DI 10.1016/j.watres.2011.08.002 PG 15 WC Engineering, Environmental; Environmental Sciences; Water Resources SC Engineering; Environmental Sciences & Ecology; Water Resources GA 902DL UT WOS:000301018700002 PM 21893330 ER PT J AU Lambert, JB Tsai, CYH Shah, MC Hurtley, AE Santiago-Blay, JA AF Lambert, J. B. Tsai, C. Y. -H. Shah, M. C. Hurtley, A. E. Santiago-Blay, J. A. TI DISTINGUISHING AMBER AND COPAL CLASSES BY PROTON MAGNETIC RESONANCE SPECTROSCOPY SO ARCHAEOMETRY LA English DT Article DE AMBER; CORRELATION SPECTROSCOPY (COSY); FOSSILIZED RESIN; NUCLEAR MAGNETIC RESONANCE SPECTROSCOPY; PLANT RESIN; PRINCIPAL COMPONENT ANALYSIS ID CHROMATOGRAPHY MASS-SPECTROMETRY; NATURAL RESINS; BALTIC AMBER; IDENTIFICATION; GEOSPHERE; FATE AB Fossilized resin, or amber, has been examined from 120 worldwide sources by 1D and 2D proton magnetic resonance spectroscopy in solution. These spectra fall into five categories, corresponding to the classes already established by mass spectrometry and carbon-13 magnetic resonance spectroscopy. The wide availability of this technique provides a straightforward method to classify amber rapidly and inexpensively. C1 [Lambert, J. B.] Trinity Univ, Dept Chem, San Antonio, TX 78212 USA. [Lambert, J. B.; Tsai, C. Y. -H.; Shah, M. C.; Hurtley, A. E.] Northwestern Univ, Dept Chem, Evanston, IL 60208 USA. [Santiago-Blay, J. A.] Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20013 USA. [Santiago-Blay, J. A.] Univ Puerto Rico, Dept Crops & Agroenvironm Sci, Mayaguez, PR 00681 USA. RP Lambert, JB (reprint author), Trinity Univ, Dept Chem, 1 Trinity Pl, San Antonio, TX 78212 USA. EM jlambert@northwestern.edu; blayj@si.edu RI Tsai, Charlie/C-6385-2013 FU Gallaudet University; Smithsonian Institution FX The authors thank C. Brown (Department of Mineral Sciences) and J. Wingerath (Department of Paleobiology) of the National Museum of Natural History, Smithsonian Institution, Washington, DC, who generously facilitated the loan of dozens of specimens. We also thank Dr Y. Wu of Northwestern University for recording the 13C spectra used in the principal component calculations and Dr M. Regert of the Universite Nice Sophia Antipolis - CNRS for samples from Yemen. We acknowledge financial support from Gallaudet University and the Smithsonian Institution. NR 37 TC 7 Z9 13 U1 2 U2 19 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0003-813X J9 ARCHAEOMETRY JI Archaeometry PD APR PY 2012 VL 54 BP 332 EP 348 DI 10.1111/j.1475-4754.2011.00625.x PN 2 PG 17 WC Archaeology; Chemistry, Analytical; Chemistry, Inorganic & Nuclear; Geosciences, Multidisciplinary SC Archaeology; Chemistry; Geology GA 901NJ UT WOS:000300973500009 ER PT J AU Terrell, KA Wildt, DE Anthony, NM Bavister, BD Leibo, SP Penfold, LM Marker, LL Crosier, AE AF Terrell, Kimberly A. Wildt, David E. Anthony, Nicola M. Bavister, Barry D. Leibo, S. P. Penfold, Linda M. Marker, Laurie L. Crosier, Adrienne E. TI Different patterns of metabolic cryo-damage in domestic cat (Felis catus) and cheetah (Acinonyx jubatus) spermatozoa SO CRYOBIOLOGY LA English DT Article DE Sperm; Cryopreservation; Metabolism; Swim-up; Accudenz; Density gradient; Mitochondria; Lactate; Felid; Teratospermia ID IN-VITRO FERTILIZATION; SPERM CRYOPRESERVATION; ZONA-PELLUCIDA; TERATOSPERMIC DONORS; EJACULATE TRAITS; SWIM-UP; MOTILITY; CAPACITATION; QUALITY; PHOSPHORYLATION AB Felid spermatozoa are sensitive to cryopreservation-induced damage, but functional losses can be mitigated by post-thaw swim-up or density gradient processing methods that selectively recover motile or structurally-normal spermatozoa, respectively. Despite the importance of sperm energy production to achieving fertilization, there is little knowledge about the influence of cryopreservation or post-thaw processing on felid sperm metabolism. We conducted a comparative study of domestic cat and cheetah sperm metabolism after cryopreservation and post-thaw processing. We hypothesized that freezing/thawing impairs sperm metabolism and that swim-up, but not density gradient centrifugation, recovers metabolically-normal spermatozoa. Ejaculates were cryopreserved, thawed, and processed by swim-up, Accudenz gradient centrifugation, or conventional washing (representing the 'control'). Sperm glucose and pyruvate uptake, lactate production, motility, and acrosomal integrity were assessed. Mitochondrial membrane potential (MMP) was measured in cat spermatozoa. In both species, lactate production, motility, and acrosomal integrity were reduced in post-thaw, washed samples compared to freshly-collected ejaculates. Glucose uptake was minimal pre- and post-cryopreservation, whereas pyruvate uptake was similar between treatments due to high coefficients of variation. In the cat, swim-up, but not Accudenz processing, recovered spermatozoa with increased lactate production, pyruvate uptake, and motility compared to controls. Although confounded by differences in non-specific fluorescence among processing methods. MMP values within treatments were positively correlated to sperm motility and acrosomal integrity. Cheetah spermatozoa isolated by either selection method exhibited improved motility and/or acrosomal integrity, but remained metabolically compromised. Collectively, findings revealed a metabolically-robust subpopulation of cryopreserved cat, but not cheetah, spermatozoa, recovered by selecting for motility rather than morphology. Published by Elsevier Inc. C1 [Terrell, Kimberly A.; Wildt, David E.; Crosier, Adrienne E.] Smithsonian Conservat Biol Inst, Ctr Species Survival, Front Royal, VA 22630 USA. [Terrell, Kimberly A.; Anthony, Nicola M.; Leibo, S. P.] Univ New Orleans, Dept Biol Sci, New Orleans, LA 70148 USA. [Bavister, Barry D.] Univ Puerto Rico, San Juan, PR 00936 USA. [Leibo, S. P.] Audubon Ctr Res Endangered Species, New Orleans, LA 70131 USA. [Penfold, Linda M.] White Oak Conservat Ctr, Yulee, FL 32097 USA. [Marker, Laurie L.] Cheetah Conservat Fund, Otjiwarongo, Namibia. RP Terrell, KA (reprint author), Smithsonian Conservat Biol Inst, Ctr Species Survival, 1500 Remount Rd, Front Royal, VA 22630 USA. EM terrellk@si.edu FU National Science Foundation; Louisiana State University; Audubon Center for Research of Endangered Species; Ohrstrom Family Foundation; William H. Donner Foundation, Inc. FX Supported by the National Science Foundation Graduate Research Fellowship Program, Louisiana State University and Audubon Center for Research of Endangered Species Grant Program, the Ohrstrom Family Foundation, and the William H. Donner Foundation, Inc. NR 54 TC 6 Z9 6 U1 0 U2 29 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0011-2240 J9 CRYOBIOLOGY JI Cryobiology PD APR PY 2012 VL 64 IS 2 BP 110 EP 117 DI 10.1016/j.cryobiol.2011.12.006 PG 8 WC Biology; Physiology SC Life Sciences & Biomedicine - Other Topics; Physiology GA 900CW UT WOS:000300865200006 PM 22227231 ER PT J AU Vari, RP Sidlauskas, BL Le Bail, PY AF Vari, Richard P. Sidlauskas, Brian L. Le Bail, Pierre-Yves TI New species of Cyphocharax (Ostariophysi: Characiformes: Curimatidae) from Suriname and French Guiana and a discussion of curimatid diversity on the Guiana Shield SO CYBIUM LA English DT Article DE Curimatidae; Cyphocharax biocellatus; South America; Guiana Shield; Biodiversity; New species ID FISHES AB Cyphocharax biocellatus, a species of curimatid characiform apparently endemic to the Marowijne River/Fleuve Maroni system in Suriname and French Guiana, and the Maim River basin in French Guiana is described as new. The new species is diagnosed from congeners based on meristic and morphometric features and details of pigmentation of the body and dorsal and caudal fins. The description of the new species brings the total number of Cyphocharax species in the drainages overlying the Guiana Shield to 14, with eight species occurring in the northern-flowing river systems of the Guianas. As such, the Guianas demonstrate the highest species-level diversity within Cyphocharax among comparably-sized areas within the range of the genus. The pronounced diversity of the genus Cyphocharax and the family Curimatidae at the level of the Maroni basin, the Guianas and the rivers systems draining the Guiana Shield is discussed. C1 [Vari, Richard P.] Smithsonian Inst, Natl Museum Nat Hist, MRC 159, Div Fishes,Dept Vertebrate Zool, Washington, DC 20013 USA. [Sidlauskas, Brian L.] Oregon State Univ, Dept Fisheries & Wildlife, Corvallis, OR 97331 USA. [Le Bail, Pierre-Yves] INRA, SCRIBE UR1037, F-35000 Rennes, France. RP Vari, RP (reprint author), Smithsonian Inst, Natl Museum Nat Hist, MRC 159, Div Fishes,Dept Vertebrate Zool, POB 37012, Washington, DC 20013 USA. EM varir@si.edu; brian.sidlauskas@oregonstate.edu; pierre-yves.lebail@rennes.inra.fr RI Scribe, Lab/B-3676-2009; OI Sidlauskas, Brian/0000-0003-0597-4085 FU Herbert R. and Evelyn Axelrod Chair in Systematic Ichthyology in the Division of Fishes, National Museum of Natural History of the Smithsonian Institution FX Support for this project was provided by the Herbert R. and Evelyn Axelrod Chair in Systematic Ichthyology in the Division of Fishes, National Museum of Natural History of the Smithsonian Institution (RPV). We thank Mark Sabaj Perez (ANSP) for calling our attention to the specimen that is herein designated as the holotype of Cyphocharax biocellatus, and Philippe Keith for his assistance in collecting various specimens pertinent to this study. T. Britt Griswold prepared figure 1. Sandra Raredon (USMN) assisted with the radiography of specimens and provided other support. NR 18 TC 8 Z9 8 U1 1 U2 5 PU SOC FRANCAISE D ICHTYOLOGIE PI PARIS PA MUSEUM NATL D HISTOIRE NATURELLE, 43 RUE CUVIER, 75231 PARIS, FRANCE SN 0399-0974 J9 CYBIUM JI Cybium PD MAR 31 PY 2012 VL 36 IS 1 BP 63 EP 69 PG 7 WC Zoology SC Zoology GA 941FU UT WOS:000303949900007 ER PT J AU Sidlauskas, BL Vari, RP AF Sidlauskas, Brian L. Vari, Richard P. TI Diversity and distribution of anostomoid fishes (Teleostei: Characiformes) throughout the Guianas SO CYBIUM LA English DT Article DE Biogeography; Dichotomous key; Georeferencing; South America; Synthesis; Taxonomy ID RIO ORINOCO SYSTEM; FRESH-WATER FISH; PHYLOGENETIC-RELATIONSHIPS; LEPORINUS-SPIX; BRAZIL; OSTARIOPHYSI; REDESCRIPTION; CURIMATIDAE; SCHIZODON; PISCES AB Fifty-six species or approximately 20% of the Neotropical characiform superfamily Anostomoidea (families Anostomidae, Chilodontidae, Curimatidae and Prochilodontidae) occur in the freshwaters of French Guiana, Guyana, and Suriname although these regions span only approximately 6% of the native range of this morphologically and ecologically diverse superfamily. As a result of the high diversity of anostomoids in the Guianas, the taxonomic and/or geographic boundaries of many species are poorly understood, particularly within the family Anostomidae. This contribution unites results of prior taxonomic revisions with surveys of the holdings of the superfamily in seven major natural history collections to provide distribution maps and keys to the identification of all anostomoid species known to occur in the Guianas. These maps reveal six major areas of endemism: the Takutu and Ireng rivers (Rio Branco drainage, Amazon basin), the Barima and Waini rivers (Orinoco drainage), the Essequibo-Rupununi River system (including the Demerara and Berbice rivers), a union of the Corantijn, Nickerie, Coppename, Saramacca and Suriname river drainages, the Marowijne/Maroni River system (including the Litani and Mana rivers), and the Oyapock-Approuague River basins. Of these, the Essequibo-Rupununi system harbours the most exceptionally diverse assemblage of anostomoid species, likely as a result of faunal exchange between the Rio Branco and Essequibo River across the Rupununi portal. C1 [Sidlauskas, Brian L.] Oregon State Univ, Dept Fisheries & Wildlife, Corvallis, OR 97331 USA. [Sidlauskas, Brian L.; Vari, Richard P.] Smithsonian Inst, Natl Museum Nat Hist, MRC 159, Dept Vertebrate Zool, Washington, DC 20013 USA. RP Sidlauskas, BL (reprint author), Oregon State Univ, Dept Fisheries & Wildlife, 104 Nash Hall, Corvallis, OR 97331 USA. EM brian.sidlauskas@oregonstate.edu; varir@si.edu OI Sidlauskas, Brian/0000-0003-0597-4085 NR 56 TC 14 Z9 14 U1 2 U2 16 PU SOC FRANCAISE D ICHTYOLOGIE PI PARIS PA MUSEUM NATL D HISTOIRE NATURELLE, 43 RUE CUVIER, 75231 PARIS, FRANCE SN 0399-0974 J9 CYBIUM JI Cybium PD MAR 31 PY 2012 VL 36 IS 1 BP 71 EP 103 PG 33 WC Zoology SC Zoology GA 941FU UT WOS:000303949900008 ER PT J AU Mol, JH Vari, RP Covain, R Willink, PW Fisch-Muller, S AF Mol, Jan H. Vari, Richard P. Covain, Raphael Willink, Philip W. Fisch-Muller, Sonia TI Annotated checklist of the freshwater fishes of Suriname SO CYBIUM LA English DT Article DE Diversity; Ichthyofauna; Guiana Shield; Distribution; South America; Neotropics ID TELEOSTEI CHARACIFORMES CHARACIDAE; NEOTROPICAL ELECTRIC FISH; FRENCH-GUIANA; SILURIFORMES LORICARIIDAE; ARMORED CATFISH; TAXONOMIC REVISION; RIVER DRAINAGE; SOUTH-AMERICA; N.-SP; OSTARIOPHYSI AB Data derived from the literature supplemented by examination of specimens in collections show that 481 species of fish live in the fresh and brackish inland waters of Suriname, with 394 of these restricted to fresh waters. These 481 species represent 16 orders and 64 families. Orders with the largest numbers of freshwater species in the Surinamese inland fish fauna are the Siluriformes (157 species), Characiformes (147 species), Perciformes (40 species), Gymnotiformes (21 species) and Cyprinodontiformes (21 species). At the family level, the Characidae has the greatest number of freshwater species (83 species), followed by the Loricariidae (60 species), the Cichlidae (30 species), the Callichthyidae (23 species), the Heptapteridae (19 species) and the Anostomidae (17 species). Present data indicate that 25 of the species are known solely from locations within Suriname and 89 species solely in Surinamese river systems including the Marowijne/Mana and Corantijn watersheds which in part extend into French Guiana and Guyana, respectively. Of 481 total species, 187 (38.9%) were based on type series that originated within Suriname. Continued descriptions of new species from the inland waters of Suriname demonstrate that the present total most likely distinctly underestimates the species-level diversity of the fish fauna. In terms of species per square kilometer, the presently documented richness of the Surinamese freshwater fish fauna is comparable to, or even greater than, the richness of fish faunas of several other tropical South American countries. C1 [Mol, Jan H.] Anton Kom Univ Suriname, Ctr Agr Res Suriname CELOS, Leysweg, Paramaribo, Surinam. [Mol, Jan H.] Anton Kom Univ Suriname, Dept Biol, Leysweg, Paramaribo, Surinam. [Vari, Richard P.] Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Washington, DC 20560 USA. [Covain, Raphael; Fisch-Muller, Sonia] Museum Hist Nat, Dept Herpetol & Ichtyol, CH-1211 Geneva 6, Switzerland. [Covain, Raphael] Univ Geneva, Dept Genet & Evolut, CH-1211 Geneva 4, Switzerland. [Covain, Raphael] Univ Lyon 1, CNRS, UMR 5558, Lab Biometrie & Biol Evolut, F-69622 Villeurbanne, France. [Willink, Philip W.] Field Museum Nat Hist, Div Fishes, Chicago, IL 60605 USA. RP Mol, JH (reprint author), Anton Kom Univ Suriname, Ctr Agr Res Suriname CELOS, CELOS Bldg, Leysweg, Paramaribo, Surinam. EM fisheco@celos.sr.org; varir@si.edu; Raphael.Covain@ville-ge.ch; pwillink@fieldmuseum.org; Sonia.Fisch-Muller@ville-ge.ch OI Covain, Raphael/0000-0002-8186-8914 NR 126 TC 12 Z9 12 U1 3 U2 9 PU SOC FRANCAISE D ICHTYOLOGIE PI PARIS PA MUSEUM NATL D HISTOIRE NATURELLE, 43 RUE CUVIER, 75231 PARIS, FRANCE SN 0399-0974 J9 CYBIUM JI Cybium PD MAR 31 PY 2012 VL 36 IS 1 BP 263 EP 292 PG 30 WC Zoology SC Zoology GA 941FU UT WOS:000303949900015 ER PT J AU Correa-Metrio, A Bush, MB Cabrera, KR Sully, S Brenner, M Hodell, DA Escobar, J Guilderson, T AF Correa-Metrio, Alexander Bush, Mark B. Cabrera, Kenneth R. Sully, Shannon Brenner, Mark Hodell, David A. Escobar, Jaime Guilderson, Tom TI Rapid climate change and no-analog vegetation in lowland Central America during the last 86,000 years SO QUATERNARY SCIENCE REVIEWS LA English DT Article DE Paleoclimatology; Climate change; Paleoecology; Ecological change; Central America; Last Glacial Maximum; Heinrich stadials ID ATLANTIC WARM POOL; POLLEN RECORD; THERMOHALINE CIRCULATION; YUCATAN PENINSULA; TROPICAL ATLANTIC; GLACIAL MAXIMUM; YOUNGER-DRYAS; NORTH-AMERICA; COSTA-RICA; ICE-AGE AB Glacial-interglacial climate cycles are known to have triggered migrations and reassortments of tropical biota. Although long-term precessionally-driven changes in temperature and precipitation have been demonstrated using tropical sediment records, responses to abrupt climate changes, e.g. the cooling of Heinrich stadials or warmings of the deglaciation, are poorly documented. The best predictions of future forest responses to ongoing warming will rely on evaluating the influences of both abrupt and long-term climate changes on past ecosystems. A sedimentary sequence recovered from Lake Peten-Itza, Guatemalan lowlands, provided a natural archive of environmental history. Pollen and charcoal analyses were used to reconstruct the vegetation and climate history of the area during the last 86,000 years. We found that vegetation composition and air temperature were strongly influenced by millennial-scale changes in the North Atlantic Ocean. Whereas Greenland warm interstadials were associated with warm and relatively wet conditions in the Central American lowlands, cold Greenland stadials, especially those associated with Heinrich events, caused extremely dry and cold conditions. Even though the vegetation seemed to have been highly resilient, plant associations without modern analogs emerged mostly following sharp climate pulses of either warmth or cold, and were paralleled by exceptionally high rates of ecological change. Although pulses of temperature change are evident in this 86,000-year record none matched the rates projected for the 21st Century. According to our findings, the ongoing rapid warming will cause no-modern-analog communities, which given the improbability of returning to lower-than-modern CO2 levels, anthropogenic barriers to migration, and increased anthropogenic fires, will pose immense threats to the biodiversity of the region. (C) 2012 Elsevier Ltd. All rights reserved. C1 [Correa-Metrio, Alexander] Univ Nacl Autonoma Mexico, Inst Geol, Mexico City 04520, DF, Mexico. [Correa-Metrio, Alexander; Bush, Mark B.; Sully, Shannon] Florida Inst Technol, Dept Biol Sci, Melbourne, FL 32901 USA. [Cabrera, Kenneth R.] Univ Nacl Colombia, Escuela Geociencias, Sede Medellin, Colombia. [Brenner, Mark] Univ Florida, Dept Geol Sci, Gainesville, FL 32611 USA. [Brenner, Mark] Univ Florida, Land Use & Environm Change Inst LUECI, Gainesville, FL 32611 USA. [Hodell, David A.] Univ Cambridge, Dept Earth Sci, Godwin Lab Palaeoclimate Res, Cambridge CB2 3EQ, England. [Escobar, Jaime] Univ Bogota Jorge Tadeo Lozano, Dept Ciencias Biol & Ambientales, Bogota, DC, Colombia. [Escobar, Jaime] Smithsonian Trop Res Inst, Ctr Trop Paleoecol & Archaeol, Panama City, Panama. [Guilderson, Tom] Lawrence Livermore Natl Lab, Ctr Accelerator Mass Spectrometry, Livermore, CA 94551 USA. RP Correa-Metrio, A (reprint author), Univ Nacl Autonoma Mexico, Inst Geol, Ciudad Univ, Mexico City 04520, DF, Mexico. EM acorrea@geologia.unam.mx OI Bush, Mark/0000-0001-6894-8613 FU US National Science Foundation [ATM-0502030]; International Continental Scientific Drilling Program; Swiss Federal Institute of Technology; Swiss National Science Foundation FX We are grateful to H. Hooghiemstra, an anonymous reviewer, and J.S. Carrion, handling editor, whose comments strengthened the manuscript. We thank all individuals who participated in the field and laboratory work during the Lake Peten-Itza Scientific Drilling Project. We are also grateful to the numerous agencies and individuals in Guatemala who provided assistance to the project. We also thank our many collaborators from University of Florida, University of Minnesota (Minneapolis/Duluth), Geo-forschungszentrum (Potsdam), Swiss Federal Institute of Technology (Zurich), Universite de Geneve, as well as the personnel of DOSECC. The cores are archived at LacCore (National Lacustrine Core Repository), Department of Geology and Geophysics. University of Minnesota-Twin Cities and we thank Kristina Brady, Amy Myrbo and Anders Noren for their assistance in core description and curation. Anders Noren kindly sampled the cores for this study. This project was funded by grants from the US National Science Foundation (ATM-0502030), the International Continental Scientific Drilling Program, the Swiss Federal Institute of Technology, and the Swiss National Science Foundation. This is publication 66 of the Florida Institute of Technology Institute for Research on Global Climate Change. NR 89 TC 33 Z9 33 U1 3 U2 39 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0277-3791 J9 QUATERNARY SCI REV JI Quat. Sci. Rev. PD MAR 30 PY 2012 VL 38 BP 63 EP 75 DI 10.1016/j.quascirev.2012.01.025 PG 13 WC Geography, Physical; Geosciences, Multidisciplinary SC Physical Geography; Geology GA 927DH UT WOS:000302886700005 ER PT J AU Baldwin, CC Weigt, LA AF Baldwin, Carole C. Weigt, Lee A. TI A New Species of Soapfish (Teleostei: Serranidae: Rypticus), with Redescription of R. subbifrenatus and Comments on the Use of DNA Barcoding in Systematic Studies SO COPEIA LA English DT Article ID ASTRAPTES-FULGERATOR; TAXONOMY; ATLANTIC; IDENTIFICATION; HESPERIIDAE; LEPIDOPTERA; ENTERPRISE; GOBIIDAE; REVEALS; SAMPLES AB A new species of Rypticus is described from the Bahamas, Bermuda, Florida, and the Caribbean Sea. The species previously has been confused with the spotted soapfish, R. subbifrenatus Gill 1861, with which it shares a similar pattern of dark spotting on the body. The new species differs from R. subbifrenatus in having yellow pigment on the pectoral fin and distal portions of the soft dorsal, caudal, and anal fins in life (pale in preservative); a different configuration of dark spots on the head; usually dark spots on the belly and caudal fin; almost always four dorsal-fin spines; and modally 25 total dorsal-fin elements, 15 pectoral-fin rays, and 23 total caudal-fin rays. The lower jaw typically extends further anteriorly beyond the upper jaw in the new species than in R. subbifrenatus, and the caudal peduncle is usually narrower. The new Rypticus typically inhabits deeper waters than R. subbifrenatus, and is commonly found on vertical slopes and walls vs. shallow, flat areas. The new species likely would have continued to go unnoticed without examination of genetic data, as there was little reason to look further at R. subbifrenatus until DNA barcoding revealed two distinct genetic lineages within the species. The value of DNA barcoding data in systematic studies and the need for increased support of taxonomy are highlighted. A neotype for Rypticus subbifrenatus is designated. C1 [Baldwin, Carole C.] Natl Museum Nat Hist, Smithsonian Inst, Dept Vertebrate Zool, Washington, DC 20013 USA. [Weigt, Lee A.] Natl Museum Nat Hist, Museum Support Ctr, Smithsonian Inst, Labs Analyt Biol, Suitland, MD 20746 USA. RP Baldwin, CC (reprint author), Natl Museum Nat Hist, Smithsonian Inst, Dept Vertebrate Zool, POB 37012, Washington, DC 20013 USA. EM baldwinc@si.edu; weigtl@si.edu FU Smithsonian Marine Science Network; Smithsonian DNA Barcoding Initiative; Hunterdon Oceanographic Research Fund; Smithsonian Marine Station at Fort Pierce (SMSFP) [857]; Perry Institute of Marine Science FX W. Smith-Vaniz made helpful comments on drafts of this manuscript. J. Joyeux, S. LeCroy, R. Macieira, R. Robins, R. Singer, W. Smith-Vaniz, and E. Warchol provided specimens on loan. D. Catania, K. Ilves, K. Luckenbill, and J. Wong examined, photographed, and identified specimens. H. Wellendorf provided photographs of the holotype of Rhypticus nigromaculatus at the Naturhistorisches Museum, Vienna. J. Williams allowed us to use his image of Rypticus carpenteri (Fig. 4, 54 mm SL), and Robert Myers, Coral Graphics, gave us permission to use the map featured in Figure 7. C. Castillo, D. Griswold, and B. Luther assisted with photography and radiography of preserved specimens. A. Driskell and A. Ormos provided laboratory and logistical assistance. D. Smith provided field assistance and contributed in numerous other ways to the project. J. Bagley, M. Carpenter, A. Driskell, M. Fagan, Z. Foltz, B. Holt, J. Lang, L. Lang, B. Langton, and J. Mounts provided field assistance. Research in Florida was conducted pursuant to SAL #09SR-1024SR to the first author. A. Gazit, K. Wilson, and M. Kunen facilitated collecting in Curacao through the CAR-MABI laboratory. Fieldwork in the Bahamas was conducted under the auspices of the Perry Institute of Marine Science, with logistical assistance from B. Gadd, E. Lamarre, and D. O'Donnell. R. Langton, J. Gobin, and K. Caesar facilitated collecting in Tobago, and B. Holt provided support and logistical help for research on South Caicos Island. The Smithsonian Marine Science Network provided major funding for fieldwork through a grant to the first author, and the Smithsonian DNA Barcoding Initiative provided funding for COI analyses. This is contribution number 908 of the Caribbean Coral Reef Ecosystems Program (CCRE), Smithsonian Institution, supported in part by the Hunterdon Oceanographic Research Fund, and Smithsonian Marine Station at Fort Pierce (SMSFP) Contribution No. 857. NR 38 TC 21 Z9 22 U1 0 U2 7 PU AMER SOC ICHTHYOLOGISTS & HERPETOLOGISTS PI MIAMI PA MAUREEN DONNELLY, SECRETARY FLORIDA INT UNIV BIOLOGICAL SCIENCES, 11200 SW 8TH STREET, MIAMI, FL 33199 USA SN 0045-8511 EI 1938-5110 J9 COPEIA JI Copeia PD MAR 30 PY 2012 IS 1 BP 23 EP 36 DI 10.1643/CG-11-035 PG 14 WC Zoology SC Zoology GA 920RF UT WOS:000302424100003 ER PT J AU Kraft, NJB Sanders, NJ Stegen, JC Anderson, MJ Crist, TO Cornell, HV Vellend, M Chase, JM Comita, LS Davies, KF Freestone, AL Harrison, SP Inouye, BD Myers, JA Swenson, NG AF Kraft, Nathan J. B. Sanders, Nathan J. Stegen, James C. Anderson, Marti J. Crist, Thomas O. Cornell, Howard V. Vellend, Mark Chase, Jonathan M. Comita, Liza S. Davies, Kendi F. Freestone, Amy L. Harrison, Susan P. Inouye, Brian D. Myers, Jonathan A. Swenson, Nathan G. TI Response to Comments on "Disentangling the Drivers of beta Diversity Along Latitudinal and Elevational Gradients" SO SCIENCE LA English DT Editorial Material ID COMMUNITY ECOLOGY C1 [Kraft, Nathan J. B.; Vellend, Mark] Univ British Columbia, Biodivers Res Ctr, Vancouver, BC V6T 1Z4, Canada. [Kraft, Nathan J. B.] Univ Maryland, Dept Biol, College Pk, MD 20742 USA. [Sanders, Nathan J.] Univ Tennessee, Dept Ecol & Evolutionary Biol, Knoxville, TN 37996 USA. [Sanders, Nathan J.] Univ Copenhagen, Dept Biol, Ctr Macroecol Evolut & Climate, DK-2100 Copenhagen O, Denmark. [Stegen, James C.] Univ N Carolina, Dept Biol, Chapel Hill, NC 27599 USA. [Stegen, James C.] Pacific NW Natl Lab, Div Biol Sci, Fundamental & Computat Sci Directorate, Richland, WA 99352 USA. [Anderson, Marti J.] Massey Univ, New Zealand Inst Adv Study, Auckland, New Zealand. [Crist, Thomas O.] Miami Univ, Inst Environm & Sustainabil, Oxford, OH 45056 USA. [Crist, Thomas O.] Miami Univ, Dept Zool, Oxford, OH 45056 USA. [Cornell, Howard V.; Harrison, Susan P.] Univ Calif Davis, Dept Environm Sci & Policy, Davis, CA 95616 USA. [Vellend, Mark] Univ Sherbrooke, Dept Biol, Sherbrooke, PQ J1K 2R1, Canada. [Chase, Jonathan M.] Washington Univ, Dept Biol, St Louis, MO 63130 USA. [Comita, Liza S.; Myers, Jonathan A.] Ohio State Univ, Dept Evolut Ecol & Organismal Biol, Columbus, OH 43210 USA. [Comita, Liza S.] Smithsonian Trop Res Inst, Balboa Ancon, Panama. [Davies, Kendi F.] Univ Colorado, Dept Ecol & Evolutionary Biol, Boulder, CO 80309 USA. [Freestone, Amy L.] Temple Univ, Dept Biol, Philadelphia, PA 19122 USA. [Inouye, Brian D.] Florida State Univ, Tallahassee, FL 32306 USA. [Swenson, Nathan G.] Michigan State Univ, Dept Plant Biol, E Lansing, MI 48824 USA. RP Kraft, NJB (reprint author), Univ British Columbia, Biodivers Res Ctr, Vancouver, BC V6T 1Z4, Canada. EM nkraft@biodiversity.ubc.ca RI Kraft, Nathan/A-2817-2012; Swenson, Nathan/A-3514-2012; Sanders, Nathan/A-6945-2009; Stegen, James/Q-3078-2016; publist, CMEC/C-3010-2012; publicationpage, cmec/B-4405-2017 OI Kraft, Nathan/0000-0001-8867-7806; Swenson, Nathan/0000-0003-3819-9767; Sanders, Nathan/0000-0001-6220-6731; Stegen, James/0000-0001-9135-7424; NR 9 TC 3 Z9 3 U1 6 U2 65 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 MAR 30 PY 2012 VL 335 IS 6076 DI 10.1126/science.1218697 PG 3 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 915YD UT WOS:000302062600023 ER PT J AU Fattorini, S Cardoso, P Rigal, F Borges, PAV AF Fattorini, Simone Cardoso, Pedro Rigal, Francois Borges, Paulo A. V. TI Use of Arthropod Rarity for Area Prioritisation: Insights from the Azorean Islands SO PLOS ONE LA English DT Article ID BIODIVERSITY CONSERVATION; SPECIES DISTRIBUTIONS; PROTECTED AREAS; BUTTERFLIES; HABITATS; RICHNESS; BEETLES; PREDICTION; ABUNDANCE; PRIORITY AB We investigated the conservation concern of Azorean forest fragments and the entire Terceira Island surface using arthropod species vulnerability as defined by the Kattan index, which is based on species rarity. Species rarity was evaluated according to geographical distribution (endemic vs. non endemic species), habitat specialization (distribution across biotopes) and population size (individuals collected in standardized samples). Geographical rarity was considered at 'global' scale (species endemic to the Azorean islands) and 'regional' scale (single island endemics). Measures of species vulnerability were combined into two indices of conservation concern for each forest fragment: (1) the Biodiversity Conservation Concern index, BCC, which reflects the average rarity score of the species present in a site, and (2) one proposed here and termed Biodiversity Conservation Weight, BCW, which reflects the sum of rarity scores of the same species assemblage. BCW was preferable to prioritise the areas with highest number of vulnerable species, whereas BCC helped the identification of areas with few, but highly threatened species due to a combination of different types of rarity. A novel approach is introduced in which BCC and BCW indices were also adapted to deal with probabilities of occurrence instead of presence/absence data. The new probabilistic indices, termed pBCC and pBCW, were applied to Terceira Island for which we modelled species distributions to reconstruct species occurrence with different degree of probability also in areas from which data were not available. The application of the probabilistic indices revealed that some island sectors occupied by secondary vegetation, and hence not included in the current set of protected areas, may in fact host some rare species. This result suggests that protecting marginal non-natural areas which are however reservoirs of vulnerable species may also be important, especially when areas with well preserved primary habitats are scarce. C1 [Fattorini, Simone; Cardoso, Pedro; Rigal, Francois; Borges, Paulo A. V.] Univ Acores, Azorean Biodivers Grp, Dept Ciencias Agr CITA A, Pico Da Urze, Angra Do Herois, Portugal. [Fattorini, Simone] Univ Milano Bicocca, Dept Biotechnol & Biosci, Water Ecol Team, Milan, Italy. [Cardoso, Pedro] Natl Museum Nat Hist, Smithsonian Inst, Washington, DC 20560 USA. RP Fattorini, S (reprint author), Univ Acores, Azorean Biodivers Grp, Dept Ciencias Agr CITA A, Pico Da Urze, Angra Do Herois, Portugal. EM simone_fattorini@virgilio.it RI Borges, Paulo/B-2780-2008; Fattorini, Simone/E-7075-2012; Cardoso, Pedro/A-8820-2008; OI Borges, Paulo/0000-0002-8448-7623; Fattorini, Simone/0000-0002-4517-2135; Cardoso, Pedro/0000-0001-8119-9960; Rigal, Francois/0000-0001-6882-1591 FU Direccao Regional dos Recursos Florestais [17.01-080203]; Direccao Regional da Ciencia e Tecnologia (Project: "Consequences of land-use change on Azorean fauna and flora) [M.2.1.2/I/003/2008]; Fundacao Ciencia e Tecnologia [SFRH/BPD/40688/2007, PTDC/BIA-BEC/100182/2008]; Azorean Biodiversity Group (CITA-A) FX Data used in this manuscript were obtained in the projects funded by Direccao Regional dos Recursos Florestais (Project: 17.01-080203, 1999-2004) and Direccao Regional da Ciencia e Tecnologia (Project: "Consequences of land-use change on Azorean fauna and flora - the 2010 Target, M.2.1.2/I/003/2008). Grants and fellowships to the authors were provided by Fundacao Ciencia e Tecnologia (SFRH/BPD/40688/2007 and PTDC/BIA-BEC/100182/2008 for PC and FR, respectively) and Azorean Biodiversity Group (CITA-A) (Summer 2010 and Summer 2011 grants to SF). The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 75 TC 12 Z9 14 U1 0 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 MAR 30 PY 2012 VL 7 IS 3 AR e33995 DI 10.1371/journal.pone.0033995 PG 9 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 959UC UT WOS:000305339100092 PM 22479498 ER PT J AU Jamieson, MJ Dalgarno, A AF Jamieson, M. J. Dalgarno, A. TI How a change in the interaction potential affects the p-wave scattering volume SO JOURNAL OF PHYSICS B-ATOMIC MOLECULAR AND OPTICAL PHYSICS LA English DT Article ID LENGTH AB We derive a simple expression for the change in the s-wave scattering length in terms of zero-energy wavefunctions, we generalize it to obtain an expression for the change in the p-wave scattering volume and we use both expressions to derive the first order differential equations of variable phase theory that are satisfied by the closely related accumulated scattering length and volume. We provide numerical demonstrations for the example of a pair of hydrogen atoms interacting via the X-1 Sigma(+)(g) molecular state. C1 [Jamieson, M. J.] Univ Glasgow, Sch Comp Sci, Glasgow G12 8QQ, Lanark, Scotland. [Dalgarno, A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Jamieson, MJ (reprint author), Univ Glasgow, Sch Comp Sci, Glasgow G12 8QQ, Lanark, Scotland. EM mjj@dcs.gla.ac.uk FU Chemical Sciences, Geosciences and Biosciences Division of the Office of Basic Energy Sciences, Office of Science, US Department of Energy; Institute for Theoretical Atomic and Molecular Physics at the Harvard-Smithsonian Center for Astrophysics; National Science Foundation FX We acknowledge the support of the Chemical Sciences, Geosciences and Biosciences Division of the Office of Basic Energy Sciences, Office of Science, US Department of Energy and the Institute for Theoretical Atomic and Molecular Physics at the Harvard-Smithsonian Center for Astrophysics; the institute is supported by a grant from the National Science Foundation. NR 7 TC 0 Z9 0 U1 3 U2 7 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0953-4075 J9 J PHYS B-AT MOL OPT JI J. Phys. B-At. Mol. Opt. Phys. PD MAR 28 PY 2012 VL 45 IS 6 AR 061001 DI 10.1088/0953-4075/45/6/061001 PG 3 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA 905TI UT WOS:000301297200001 ER PT J AU Varughese, T Rios, N Higginbotham, S Arnold, AE Coley, PD Kursar, TA Gerwick, WH Rios, LC AF Varughese, Titto Rios, Nivia Higginbotham, Sarah Arnold, A. Elizabeth Coley, Phyllis D. Kursar, Thomas A. Gerwick, William H. Cubilla Rios, Luis TI Antifungal depsidone metabolites from Cordyceps dipterigena, an endophytic fungus antagonistic to the phytopathogen Gibberella fujikuroi SO TETRAHEDRON LETTERS LA English DT Article DE Fungal metabolite; Cordycepsidone; Cordyceps dipterigena; Gibberella fujikuroi; Antifungal activity AB Among thirty four endophytic fungal strains screened for in vitro antagonism, the endophytic fungus Cordyceps dipterigena was found to strongly inhibit mycelial growth of the plant pathogenic fungus Gibberella fujikuroi. Two new depsidone metabolites, cordycepsidone A (1) and cordycepsidone B (2), were isolated from the PDA culture extract of C. dipterigena and identified as being responsible for the antifungal activity. Elucidation of their chemical structures was carried out using 1D and 2D NMR spectroscopy in combination with IR and MS spectroscopic data. Cordycepsidone A displayed strong and dose-dependent antifungal activity against the plant pathogenic fungus G. fujikuroi. The isolates were inactive in bioassays for malaria (Plasmodium falciparum), leishmaniasis (Leishmania donovani), Chagas's disease (Trypanosoma cruzi), and cytotoxicity at 10 mu g/mL. The compounds were also found to be inactive against several bacterial strains at 50 mu/mL. (C) 2012 Elsevier Ltd. All rights reserved. C1 [Varughese, Titto; Rios, Nivia; Cubilla Rios, Luis] Univ Panama, Lab Trop Bioorgan Chem, Fac Nat Exact Sci & Technol, Panama City, Panama. [Varughese, Titto; Higginbotham, Sarah; Coley, Phyllis D.; Kursar, Thomas A.; Cubilla Rios, Luis] Smithsonian Trop Res Inst, Unit 0948, APO, AA 34002 USA. [Arnold, A. Elizabeth] Univ Arizona, Sch Plant Sci, Tucson, AZ 85721 USA. [Coley, Phyllis D.; Kursar, Thomas A.] Univ Utah, Dept Biol, Salt Lake City, UT 84112 USA. [Gerwick, William H.] Univ Calif San Diego, Ctr Marine Biotechnol & Biomed, Scripps Inst Oceanog, La Jolla, CA 92093 USA. [Gerwick, William H.] Univ Calif San Diego, Skaggs Sch Pharm & Pharmaceut Sci, La Jolla, CA 92093 USA. RP Rios, LC (reprint author), Univ Panama, Lab Trop Bioorgan Chem, Fac Nat Exact Sci & Technol, Panama City, Panama. EM lucr@ancon.up.pa FU US NIH [2 U01 TW006634-06] FX This work was supported by US NIH grant for the International Cooperative Biodiversity Groups Program (ICBG-Panama; 2 U01 TW006634-06). We express our thanks to the personnel of Panama's Autoridad Nacional del Ambiente for facilitating this research. NR 9 TC 7 Z9 9 U1 1 U2 18 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0040-4039 J9 TETRAHEDRON LETT JI Tetrahedron Lett. PD MAR 28 PY 2012 VL 53 IS 13 BP 1624 EP 1626 DI 10.1016/j.tetlet.2012.01.076 PG 3 WC Chemistry, Organic SC Chemistry GA 911BN UT WOS:000301692400024 PM 22707798 ER PT J AU Hostetler, JA Kneip, E Van Vuren, DH Oli, MK AF Hostetler, Jeffrey A. Kneip, Eva Van Vuren, Dirk H. Oli, Madan K. TI Stochastic Population Dynamics of a Montane Ground-Dwelling Squirrel SO PLOS ONE LA English DT Article ID DENSITY-DEPENDENCE; CLIMATE-CHANGE; ENVIRONMENTAL STOCHASTICITY; SPERMOPHILUS-LATERALIS; ANIMAL POPULATIONS; GROWTH-RATE; DEMOGRAPHY; VARIABILITY; RATES; ELASTICITIES AB Understanding the causes and consequences of population fluctuations is a central goal of ecology. We used demographic data from a long-term (1990-2008) study and matrix population models to investigate factors and processes influencing the dynamics and persistence of a golden-mantled ground squirrel (Callospermophilus lateralis) population, inhabiting a dynamic subalpine habitat in Colorado, USA. The overall deterministic population growth rate lambda was 0.946 +/- SE 0.05 but it varied widely over time, ranging from 0.45 +/- 0.09 in 2006 to 1.50 +/- 0.12 in 2003, and was below replacement (lambda < 1) for 9 out of 18 years. The stochastic population growth rate lambda(s) was 0.92, suggesting a declining population; however, the 95% CI on lambda(s) included 1.0 (0.52-1.60). Stochastic elasticity analysis showed that survival of adult females, followed by survival of juvenile females and litter size, were potentially the most influential vital rates; analysis of life table response experiments revealed that the same three life history variables made the largest contributions to year-to year changes in lambda. Population viability analysis revealed that, when the influences of density dependence and immigration were not considered, the population had a high (close to 1.0 in 50 years) probability of extinction. However, probability of extinction declined to as low as zero when density dependence and immigration were considered. Destabilizing effects of stochastic forces were counteracted by regulating effects of density dependence and rescue effects of immigration, which allowed our study population to bounce back from low densities and prevented extinction. These results suggest that dynamics and persistence of our study population are determined synergistically by density-dependence, stochastic forces, and immigration. C1 [Hostetler, Jeffrey A.; Kneip, Eva; Oli, Madan K.] Univ Florida, Dept Wildlife Ecol & Conservat, Gainesville, FL 32610 USA. [Hostetler, Jeffrey A.] Smithsonian Inst, Natl Zool Pk, Migratory Bird Ctr, Smithsonian Conservat Biol Inst, Washington, DC 20008 USA. [Van Vuren, Dirk H.] Univ Calif Davis, Dept Wildlife Fish & Conservat Biol, Davis, CA 95616 USA. RP Hostetler, JA (reprint author), Univ Florida, Dept Wildlife Ecol & Conservat, Gainesville, FL 32610 USA. EM olim@ufl.edu RI Hostetler, Jeffrey/A-3345-2011 OI Hostetler, Jeffrey/0000-0003-3669-1758 FU California Agricultural Experiment Station, University of California Davis; School of Natural Resources and the Environment, University of Florida; Department of Wildlife Ecology and Conservation, University of Florida FX This work was supported by California Agricultural Experiment Station, University of California Davis; School of Natural Resources and the Environment, University of Florida; and the Department of Wildlife Ecology and Conservation, University of Florida. The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 62 TC 7 Z9 7 U1 2 U2 46 PU PUBLIC LIBRARY SCIENCE PI SAN FRANCISCO PA 1160 BATTERY STREET, STE 100, SAN FRANCISCO, CA 94111 USA SN 1932-6203 J9 PLOS ONE JI PLoS One PD MAR 27 PY 2012 VL 7 IS 3 AR e34379 DI 10.1371/journal.pone.0034379 PG 10 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 940MY UT WOS:000303894900086 PM 22479616 ER PT J AU Zimmermann, A Francke, T Elsenbeer, H AF Zimmermann, Alexander Francke, Till Elsenbeer, Helmut TI Forests and erosion: Insights from a study of suspended-sediment dynamics in an overland flow-prone rainforest catchment SO JOURNAL OF HYDROLOGY LA English DT Article DE Rainforest; Overland flow; Erosion; Suspended-sediment yield; Quantile Regression Forest model; Panama Canal watershed ID SELECTIVE TROPICAL FORESTRY; BARRO COLORADO ISLAND; CYPRESS CHAMAECYPARIS-OBTUSA; QUANTILE REGRESSION FORESTS; OREGON COAST RANGE; STORMFLOW GENERATION; RUNOFF GENERATION; NEURAL-NETWORK; WATER-QUALITY; DANUM-VALLEY AB Forests seem to represent low-erosion systems, according to most, but not all, studies of suspended-sediment yield. We surmised that this impression reflects an accidental bias in the selection of monitoring sites towards those with prevailing vertical hydrological flowpaths, rather than a tight causal link between vegetation cover and erosion alone. To evaluate this conjecture, we monitored, over a 2-year period, a 3.3 ha old-growth rainforest catchment prone to frequent and widespread overland flow. We sampled stream flow at two and overland flow at three sites in a nested arrangement on a within-event basis, and monitored the spatial and temporal frequency of overland flow. Suspended-sediment concentrations were modeled with Random Forest and Quantile Regression Forest to be able to estimate the annual yields for the 2 years, which amounted to 1 t ha(-1) and 2 t ha(-1) in a year with below-average and with average precipitation, respectively. These estimates place our monitoring site near the high end of reported suspended-sediment yields and lend credence to the notion that low yields reflect primarily the dominance of vertical flowpaths and not necessarily and exclusively the kind of vegetative cover. Undisturbed forest and surface erosion are certainly no contradiction in terms even in the absence of mass movements. (C) 2012 Elsevier B.V. All rights reserved. C1 [Zimmermann, Alexander; Francke, Till; Elsenbeer, Helmut] Univ Potsdam, Inst Earth & Environm Sci, D-14476 Potsdam, Germany. [Elsenbeer, Helmut] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. RP Zimmermann, A (reprint author), Univ Potsdam, Inst Earth & Environm Sci, Karl Liebknecht Str 24-25, D-14476 Potsdam, Germany. EM alexander.zimmermann.ii@uni-potsdam.de RI Zimmermann, Alexander/B-6831-2011; OI Zimmermann, Alexander/0000-0003-0330-1565 FU German Research Foundation [El 255/6-1] FX This research was funded by the German Research Foundation (El 255/6-1). We thank Anna Schurkmann for participating in the field work. Furthermore, we are indebted to Oris Acevedo (Smithsonian Tropical Research Institute, STRI) for exceptional logistical support and to Sergio dos Santos (Terrestrial Environmental Sciences Program, STRI) for providing long-term rainfall and soil moisture data. Finally, we thank five anonymous reviewers for constructive comments on earlier drafts of this manuscript. NR 91 TC 20 Z9 20 U1 9 U2 98 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0022-1694 EI 1879-2707 J9 J HYDROL JI J. Hydrol. PD MAR 27 PY 2012 VL 428 BP 170 EP 181 DI 10.1016/j.jhydrol.2012.01.039 PG 12 WC Engineering, Civil; Geosciences, Multidisciplinary; Water Resources SC Engineering; Geology; Water Resources GA 921UK UT WOS:000302503100013 ER PT J AU Babich, R Brower, RC Clark, MA Fleming, GT Osborn, JC Rebbi, C Schaich, D AF Babich, Ronald Brower, Richard C. Clark, Michael A. Fleming, George T. Osborn, James C. Rebbi, Claudio Schaich, David TI Exploring strange nucleon form factors on the lattice SO PHYSICAL REVIEW D LA English DT Article ID SIGMA-TERM; QUARK MASSES; WILSON FERMIONS; QCD; SCATTERING; PROTON; IMPROVEMENT; NOISE; LIGHT; SCALE AB We discuss techniques for evaluating sea quark contributions to hadronic form factors on the lattice and apply these to an exploratory calculation of the strange electromagnetic, axial, and scalar form factors of the nucleon. We employ the Wilson gauge and fermion actions on an anisotropic 24(3) x 64 lattice, probing a range of momentum transfer with Q(2) < 1 GeV2. The strange electric and magnetic form factors, G(E)(s)(Q(2)) and G(M)(s)(Q(2)), are found to be small and consistent with zero within the statistics of our calculation. The lattice data favor a small negative value for the strange axial form factor G(A)(s)(Q(2)) and exhibit a strong signal for the bare strange scalar matrix element < N vertical bar(s) over bars vertical bar N >(0). We discuss the unique systematic uncertainties affecting the latter quantity relative to the continuum, as well as prospects for improving future determinations with Wilson-like fermions. C1 [Babich, Ronald; Brower, Richard C.; Rebbi, Claudio] Boston Univ, Ctr Computat Sci, Boston, MA 02215 USA. [Brower, Richard C.; Rebbi, Claudio; Schaich, David] Boston Univ, Dept Phys, Boston, MA 02215 USA. [Clark, Michael A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Fleming, George T.] Yale Univ, Dept Phys, New Haven, CT 06520 USA. [Osborn, James C.] Argonne Leadership Comp Facil, Argonne, IL 60439 USA. RP Babich, R (reprint author), Boston Univ, Ctr Computat Sci, 3 Cummington St, Boston, MA 02215 USA. RI Schaich, David/J-6644-2013; Fleming, George/L-6614-2013 OI Schaich, David/0000-0002-9826-2951; Fleming, George/0000-0002-4987-7167 FU U.S. DOE [DE-FG02-91ER40676, DE-FC02-06ER41440]; NSF [DGE-0221680, PHY-0427646, PHY-0835713]; Office of Science of the U.S. Department of Energy FX We wish to acknowledge useful discussions with Joel Giedt and Stephen Sharpe. This work was supported in part by U.S. DOE Grants No. DE-FG02-91ER40676 and No. DE-FC02-06ER41440; NSF Grants No. DGE-0221680, No. PHY-0427646, and No. PHY-0835713; and by the NSF through TeraGrid resources provided by the Texas Advanced Computing Center [74]. Computations were also carried out on facilities of the USQCD Collaboration, which are funded by the Office of Science of the U.S. Department of Energy, as well as on the Scientific Computing Facilities of Boston University. NR 74 TC 33 Z9 34 U1 0 U2 3 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 2470-0010 EI 2470-0029 J9 PHYS REV D JI Phys. Rev. D PD MAR 27 PY 2012 VL 85 IS 5 AR 054510 DI 10.1103/PhysRevD.85.054510 PG 15 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA 914SR UT WOS:000301973000005 ER PT J AU Bashforth, AR DiMichele, WA AF Bashforth, Arden R. DiMichele, William A. TI Permian Coal Forest offers a glimpse of late Paleozoic ecology SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA LA English DT Editorial Material ID VOLCANIC ASH; BASIN C1 [Bashforth, Arden R.; DiMichele, William A.] Smithsonian Inst, Dept Paleobiol, Natl Museum Nat Hist, Washington, DC 20560 USA. RP Bashforth, AR (reprint author), Smithsonian Inst, Dept Paleobiol, Natl Museum Nat Hist, Washington, DC 20560 USA. EM bashfortha@si.edu RI DiMichele, William/K-4301-2012; Bashforth, Arden/H-6057-2013 OI Bashforth, Arden/0000-0003-3050-7032 NR 21 TC 1 Z9 1 U1 4 U2 10 PU NATL ACAD SCIENCES PI WASHINGTON PA 2101 CONSTITUTION AVE NW, WASHINGTON, DC 20418 USA SN 0027-8424 J9 P NATL ACAD SCI USA JI Proc. Natl. Acad. Sci. U. S. A. PD MAR 27 PY 2012 VL 109 IS 13 BP 4717 EP 4718 DI 10.1073/pnas.1203261109 PG 2 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 917HT UT WOS:000302164200011 PM 22421437 ER PT J AU Lin, GD Yelin, SF AF Lin, G. -D. Yelin, S. F. TI Superradiance in spin-j particles: Effects of multiple levels SO PHYSICAL REVIEW A LA English DT Article ID BOSE-EINSTEIN CONDENSATION; QUANTUM PHASE-TRANSITION; SPONTANEOUS EMISSION; DICKE SUPERRADIANCE; SUPER-RADIANCE; 2-LEVEL ATOMS; TRAPPED IONS; GAS; RADIATION; SCATTERING AB We study the superradiance dynamics in a dense system of atoms each of which can be generally a spin-j particle, with j an arbitrary half-integer. We generalize Dicke's superradiance point of view to multiple-level systems and compare the results based on a novel approach we developed previously [Lin and Yelin, Adv. Atom. Mol. Opt. Phys. 61, in press (2012)]. Using this formalism we derive an effective two-body description that shows cooperative and collective effects for spin-j particles, taking into account the coherence of transitions between different atomic levels. We find that superradiance, which is well known as a many-body phenomenon, can also be modified by multiple-level effects. We also discuss the feasibility and propose that our approach can be applied to polar molecules, for their vibrational states have a multilevel structure which is partially harmonic. C1 [Lin, G. -D.] Univ Connecticut, Dept Phys, Storrs, CT 06269 USA. Harvard Smithsonian Ctr Astrophys, ITAMP, Cambridge, MA 02138 USA. RP Lin, GD (reprint author), Univ Connecticut, Dept Phys, Storrs, CT 06269 USA. EM guindarl@physics.harvard.edu OI LIN, GUIN-DAR/0000-0002-2243-9490 FU NSF FX The authors wish to thank Marc Repp, Juris Ulmanis, Johannes Deiglmayr, and Matthias Weidemuller for helpful input. We thank the NSF for financial support. NR 57 TC 12 Z9 12 U1 0 U2 7 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 1050-2947 J9 PHYS REV A JI Phys. Rev. A PD MAR 26 PY 2012 VL 85 IS 3 AR 033831 DI 10.1103/PhysRevA.85.033831 PG 11 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA 913ZH UT WOS:000301915400011 ER PT J AU Jefcoat, M Tubb, H Madden, OM AF Jefcoat, Marci Tubb, Hannah Madden, Odile M. TI Deciphering polymer composite artifacts by Raman spectroscopy: Creation and free sharing of spectral reference libraries SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY LA English DT Meeting Abstract CT 243rd National Spring Meeting of the American-Chemical-Society CY MAR 25-29, 2012 CL San Diego, CA SP Amer Chem Soc C1 [Madden, Odile M.] Smithsonian Museum Conservat Inst, Suitland, MD 20746 USA. [Jefcoat, Marci] Calif State Univ Sacramento, Dept Chem, Sacramento, CA 95819 USA. [Tubb, Hannah] Grove City Coll, Dept Chem, Grove City, PA 16127 USA. EM mjefcoat24@yahoo.com; tubbhc1@gcc.edu RI Madden, Odile/N-9909-2015 OI Madden, Odile/0000-0003-2322-2522 NR 0 TC 0 Z9 0 U1 0 U2 1 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0065-7727 J9 ABSTR PAP AM CHEM S JI Abstr. Pap. Am. Chem. Soc. PD MAR 25 PY 2012 VL 243 MA 75-POLY PG 1 WC Chemistry, Multidisciplinary SC Chemistry GA 219JX UT WOS:000324503204332 ER PT J AU Potter, IK Hark, RR Tansi, BM Hilferding, K East, LJ Remus, JJ Harmon, RS Wise, MA AF Potter, Ian K. Hark, Richard R. Tansi, Benjamin M. Hilferding, Keith East, Lucille J. Remus, Jeremiah J. Harmon, Russel S. Wise, Michael A. TI Determination of the provenance of cassiterite ore concentrates using laser-induced breakdown spectroscopy (LIBS) SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY LA English DT Meeting Abstract CT 11th International Biorelated Polymer Symposium / 243rd National Spring Meeting of the American-Chemical-Society (ACS) CY MAR 25-29, 2012 CL San Diego, CA SP Amer Chem Soc, Div Polymer Chem Inc, Amer Chem Soc C1 [Potter, Ian K.; Hark, Richard R.; Tansi, Benjamin M.; Hilferding, Keith] Juniata Coll, Dept Chem, Huntingdon, PA 16652 USA. [East, Lucille J.] Appl Spectra Inc, Fremont, CA 94538 USA. [Remus, Jeremiah J.] Clarkson Univ, Dept Elect & Comp Engn, Potsdam, NY 13699 USA. [Harmon, Russel S.] USACE ERDC Int Res Off, London, England. [Wise, Michael A.] Smithsonian Inst, Div Mineral, Washington, DC 20560 USA. EM potteik08@juniata.edu NR 0 TC 0 Z9 0 U1 0 U2 1 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0065-7727 J9 ABSTR PAP AM CHEM S JI Abstr. Pap. Am. Chem. Soc. PD MAR 25 PY 2012 VL 243 MA 38-ANYL PG 1 WC Chemistry, Multidisciplinary SC Chemistry GA 219AH UT WOS:000324475100171 ER PT J AU Tansi, BM Potter, IK East, LJ Remus, JJ Harmon, RS Wise, MS Hark, RR AF Tansi, Benjamin M. Potter, Ian K. East, Lucille J. Remus, Jeremiah J. Harmon, Russell S. Wise, Michael S. Hark, Richard R. TI Laser-induced breakdown spectroscopy (LIBS) for geochemical fingerprinting of columbite-tantalite sources SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY LA English DT Meeting Abstract CT 11th International Biorelated Polymer Symposium / 243rd National Spring Meeting of the American-Chemical-Society (ACS) CY MAR 25-29, 2012 CL San Diego, CA SP Amer Chem Soc, Div Polymer Chem Inc, Amer Chem Soc C1 [Tansi, Benjamin M.; Potter, Ian K.; Hark, Richard R.] Juniata Coll, Dept Chem, Huntingdon, PA 16652 USA. [East, Lucille J.] Appl Spectra Inc, Fremont, CA 94538 USA. [Remus, Jeremiah J.] Clarkson Univ, Dept Elect & Comp Engn, Potsdam, NY 13699 USA. [Harmon, Russell S.] USACE ERDC, Int Res Off, London, England. [Wise, Michael S.] Smithsonian Inst, Div Mineral, Washington, DC 20013 USA. EM hark@juniata.edu NR 0 TC 0 Z9 0 U1 0 U2 0 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0065-7727 J9 ABSTR PAP AM CHEM S JI Abstr. Pap. Am. Chem. Soc. PD MAR 25 PY 2012 VL 243 MA 40-ANYL PG 1 WC Chemistry, Multidisciplinary SC Chemistry GA 219AH UT WOS:000324475100173 ER PT J AU Rodriguez-R, LM Grajales, A Arrieta-Ortiz, ML Salazar, C Restrepo, S Bernal, A AF Rodriguez-R, Luis M. Grajales, Alejandro Arrieta-Ortiz, Mario L. Salazar, Camilo Restrepo, Silvia Bernal, Adriana TI Genomes-based phylogeny of the genus Xanthomonas SO BMC MICROBIOLOGY LA English DT Article ID CAMPESTRIS PV.-CAMPESTRIS; MULTILOCUS SEQUENCE-ANALYSIS; FRAGMENT LENGTH POLYMORPHISM; FUSCANS SUBSP AURANTIFOLII; EVOLUTIONARY TREES; SPECIES DEFINITION; BACTERIAL SPOT; DNA-SEQUENCES; MIXED MODELS; SP-NOV AB Background: The genus Xanthomonas comprises several plant pathogenic bacteria affecting a wide range of hosts. Despite the economic, industrial and biological importance of Xanthomonas, the classification and phylogenetic relationships within the genus are still under active debate. Some of the relationships between pathovars and species have not been thoroughly clarified, with old pathovars becoming new species. A change in the genus name has been recently suggested for Xanthomonas albilineans, an early branching species currently located in this genus, but a thorough phylogenomic reconstruction would aid in solving these and other discrepancies in this genus. Results: Here we report the results of the genome-wide analysis of DNA sequences from 989 orthologous groups from 17 Xanthomonas spp. genomes available to date, representing all major lineages within the genus. The phylogenetic and computational analyses used in this study have been automated in a Perl package designated Unus, which provides a framework for phylogenomic analyses which can be applied to other datasets at the genomic level. Unus can also be easily incorporated into other phylogenomic pipelines. Conclusions: Our phylogeny agrees with previous phylogenetic topologies on the genus, but revealed that the genomes of Xanthomonas citri and Xanthomonas fuscans belong to the same species, and that of Xanthomonas albilineans is basal to the joint clade of Xanthomonas and Xylella fastidiosa. Genome reduction was identified in the species Xanthomonas vasicola in addition to the previously identified reduction in Xanthomonas albilineans. Lateral gene transfer was also observed in two gene clusters. C1 [Rodriguez-R, Luis M.; Arrieta-Ortiz, Mario L.; Restrepo, Silvia; Bernal, Adriana] Univ Los Andes, Dept Biol Sci, Lab Mycol & Plant Pathol, Bogota, Colombia. [Grajales, Alejandro] Amer Museum Nat Hist, Div Invertebrate Zool, New York, NY 10024 USA. [Salazar, Camilo] Smithsonian Trop Res Inst, Panama City 084303092, Panama. [Salazar, Camilo] Univ Cambridge, Old Sch, Cambridge CB2 1TN, England. [Rodriguez-R, Luis M.] Georgia Inst Technol, Dept Biol, Atlanta, GA 30332 USA. RP Bernal, A (reprint author), Univ Los Andes, Dept Biol Sci, Lab Mycol & Plant Pathol, Cra 1 18A-12, Bogota, Colombia. EM abernal@uniandes.edu.co OI Rodriguez-R, Luis M/0000-0001-7603-3093; Restrepo, Silvia/0000-0001-9016-1040; Salazar, Camilo/0000-0001-9217-6588 FU Colombian administrative department of Science, Technology and Innovation (Colciencias); Vice-chancellor's Office of Research at the Universidad de Los Andes FX This project was funded by the Colombian administrative department of Science, Technology and Innovation (Colciencias) and the Vice-chancellor's Office of Research at the Universidad de Los Andes. We would like to thank Andrew Crawford, Ralf Koebnik and two anonymous reviewers for critical reading of the manuscript. We also thank Boris Szurek, Valerie Verdier, Kostantinos Konstantinidis, Catalina Arevalo and Camilo Lopez for comments and discussion on the conception and development of this study. NR 87 TC 12 Z9 12 U1 1 U2 25 PU BIOMED CENTRAL LTD PI LONDON PA 236 GRAYS INN RD, FLOOR 6, LONDON WC1X 8HL, ENGLAND SN 1471-2180 J9 BMC MICROBIOL JI BMC Microbiol. PD MAR 23 PY 2012 VL 12 AR 43 DI 10.1186/1471-2180-12-43 PG 14 WC Microbiology SC Microbiology GA 947IM UT WOS:000304423700001 PM 22443110 ER PT J AU Le Sage, D Pham, LM Bar-Gill, N Belthangady, C Lukin, MD Yacoby, A Walsworth, RL AF Le Sage, D. Pham, L. M. Bar-Gill, N. Belthangady, C. Lukin, M. D. Yacoby, A. Walsworth, R. L. TI Efficient photon detection from color centers in a diamond optical waveguide SO PHYSICAL REVIEW B LA English DT Article ID NANOSCALE RESOLUTION; ELECTRONIC SPIN; SINGLE; MICROSCOPY AB A common limitation of experiments using color centers in diamond is the poor photon collection efficiency of microscope objectives due to refraction at the diamond interface. We present a simple and effective technique to detect a large fraction of photons emitted by color centers within a planar diamond sample by detecting light that is guided to the edges of the diamond via total internal reflection. We describe a prototype device using this "side-collection" technique, which provides a photon collection efficiency approximate to 47% and a photon detection efficiency approximate to 39%. We apply the enhanced signal-to-noise ratio gained from side collection to ac magnetometry using ensembles of nitrogen-vacancy (NV) color centers, and demonstrate an ac magnetic field sensitivity approximate to 100 pT/root Hz, limited by added noise in the prototype side-collection device. Technical optimization should allow significant further improvements in photon collection and detection efficiency as well as subpicotesla NV-diamond magnetic field sensitivity using the side-collection technique. C1 [Le Sage, D.; Bar-Gill, N.; Belthangady, C.; Walsworth, R. L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Le Sage, D.; Bar-Gill, N.; Belthangady, C.; Lukin, M. D.; Yacoby, A.; Walsworth, R. L.] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. [Pham, L. M.] Harvard Univ, Sch Engn & Appl Sci, Cambridge, MA 02138 USA. RP Le Sage, D (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM rwalsworth@cfa.harvard.edu OI Le Sage, David/0000-0003-1678-9491 FU NIST; NSF; DARPA FX We gratefully acknowledge the provision of diamond samples by Apollo Diamond and Element Six; and also informative discussions with Patrick Doering, David Glenn, and Alexei Trifonov. This work was supported by NIST, NSF, and DARPA (QuEST and QuASAR programs). NR 23 TC 33 Z9 33 U1 1 U2 31 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 1098-0121 J9 PHYS REV B JI Phys. Rev. B PD MAR 23 PY 2012 VL 85 IS 12 AR 121202 DI 10.1103/PhysRevB.85.121202 PG 4 WC Physics, Condensed Matter SC Physics GA 912YQ UT WOS:000301838600001 ER PT J AU Miura, O Torchin, ME Bermingham, E Jacobs, DK Hechinger, RF AF Miura, Osamu Torchin, Mark E. Bermingham, Eldredge Jacobs, David K. Hechinger, Ryan F. TI Flying shells: historical dispersal of marine snails across Central America SO PROCEEDINGS OF THE ROYAL SOCIETY B-BIOLOGICAL SCIENCES LA English DT Article DE geminate species; Cerithideopsis; Cerithidea; Isthmus of Panama; Central America ID PHYLOGENETIC TREE SELECTION; LONG-DISTANCE DISPERSAL; GAMETIC INCOMPATIBILITY; MAXIMUM-LIKELIHOOD; GENE GENEALOGIES; PANAMA; BIRDS; POPULATION; INVASION; ISTHMUS AB The geological rise of the Central American Isthmus separated the Pacific and the Atlantic oceans about 3 Ma, creating a formidable barrier to dispersal for marine species. However, similar to Simpson's proposal that terrestrial species can 'win sweepstakes routes'-whereby highly improbable dispersal events result in colonization across geographical barriers-marine species may also breach land barriers given enough time. To test this hypothesis, we asked whether intertidal marine snails have crossed Central America to successfully establish in new ocean basins. We used a mitochondrial DNA genetic comparison of sister snails (Cerithideopsis spp.) separated by the rise of the Isthmus. Genetic variation in these snails revealed evidence of at least two successful dispersal events between the Pacific and the Atlantic after the final closure of the Isthmus. A combination of ancestral area analyses and molecular dating techniques indicated that dispersal from the Pacific to the Atlantic occurred about 750 000 years ago and that dispersal in the opposite direction occurred about 72 000 years ago. The geographical distribution of haplotypes and published field evidence further suggest that migratory shorebirds transported the snails across Central America at the Isthmus of Tehuantepec in southern Mexico. Migratory birds could disperse other intertidal invertebrates this way, suggesting the Central American Isthmus may not be as impassable for marine species as previously assumed. C1 [Miura, Osamu; Torchin, Mark E.; Bermingham, Eldredge] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. [Miura, Osamu] Kochi Univ, Div Marine Biotechnol, Oceanog Sect, Ctr Sci Res, Nankoku, Kochi 7838502, Japan. [Jacobs, David K.] Univ Calif Los Angeles, Dept Ecol & Evolutionary Biol, Los Angeles, CA 90095 USA. [Hechinger, Ryan F.] Univ Calif Santa Barbara, Inst Marine Sci, Santa Barbara, CA 93106 USA. [Hechinger, Ryan F.] Univ Calif Santa Barbara, Dept Ecol Evolut & Marine Biol, Santa Barbara, CA 93106 USA. RP Miura, O (reprint author), Smithsonian Trop Res Inst, Apartado 0843-03092, Balboa, Ancon, Panama. EM miurao@kochi-u.ac.jp FU STRI; Smithsonian Marine Science Network; Japan Society for the Promotion of Science; California Sea Grant; Global Invasions Network NSF RCN [DEB-0541673] FX We thank 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 for field assistance. We are especially indebted to C. Schloder for invaluable field, laboratory and logistical assistance. We are grateful to G. Ruiz for providing us with additional specimens. We thank H. Lessios, O. Sanjur, S. Chiba, O. Puebla, A. Kuris and K. Lafferty and two anonymous reviewers for providing useful comments on the manuscript. We thank 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. Support was provided by the STRI and the Smithsonian Marine Science Network including an MSN Post-doctoral Fellowship and an STRI Hoch fellowship to O.M.; the Japan Society for the Promotion of Science (Grant-in-Aid for JSPS Fellows to O.M.); and the California Sea Grant. This work was facilitated by the Global Invasions Network NSF RCN DEB-0541673. NR 55 TC 19 Z9 22 U1 3 U2 20 PU ROYAL SOC PI LONDON PA 6-9 CARLTON HOUSE TERRACE, LONDON SW1Y 5AG, ENGLAND SN 0962-8452 EI 1471-2954 J9 P ROY SOC B-BIOL SCI JI Proc. R. Soc. B-Biol. Sci. PD MAR 22 PY 2012 VL 279 IS 1731 BP 1061 EP 1067 DI 10.1098/rspb.2011.1599 PG 7 WC Biology; Ecology; Evolutionary Biology SC Life Sciences & Biomedicine - Other Topics; Environmental Sciences & Ecology; Evolutionary Biology GA 894HF UT WOS:000300417000003 PM 21920976 ER PT J AU Puebla, O Bermingham, E Guichard, F AF Puebla, Oscar Bermingham, Eldredge Guichard, Frederic TI Pairing dynamics and the origin of species SO PROCEEDINGS OF THE ROYAL SOCIETY B-BIOLOGICAL SCIENCES LA English DT Article DE speciation; sexual selection; assortative mating; marine; Hypoplectrus; matching ID CORAL-REEF FISH; SYMPATRIC SPECIATION; SEXUAL SELECTION; COMPETITIVE SPECIATION; HAMLETS HYPOPLECTRUS; COLOR MORPHS; SERRANIDAE; EVOLUTION; DIVERGENCE; MODEL AB Whether sexual selection alone can drive the evolution of assortative mating in the presence of gene flow is a long-standing question in evolutionary biology. Here, we report a role for pairing dynamics of individuals when mate choice is mutual, which is sufficient for the evolution of assortative mating by sexual selection alone in the presence of gene flow. Through behavioural observation, individual-based simulation and population genetic analysis, we evaluate the pairing dynamics of coral reef fish in the genus Hypoplectrus (Serranidae), and the role these dynamics can play for the evolution of assortative mating. When mate choice is mutual and the stability of mating pairs is critical for reproductive success, the evolution of assortative mating in the presence of gene flow is not only possible, but is also a robust evolutionary outcome. C1 [Puebla, Oscar; Bermingham, Eldredge] Smithsonian Trop Res Inst, Panama City, Panama. [Bermingham, Eldredge; Guichard, Frederic] McGill Univ, Dept Biol, Montreal, PQ H3A 1B1, Canada. RP Puebla, O (reprint author), Smithsonian Trop Res Inst, Apartado Postal 0843-03092, Panama City, Panama. EM oscar.puebla@mail.mcgill.ca RI Guichard, Frederic/B-6188-2015 OI Guichard, Frederic/0000-0002-7369-482X FU Marine Science Network; government of Panama; government of Belize; government of Barbados; government of Honduras; Kuna General Congress FX The Marine Science Network provided funding for this research. We acknowledge the governments of Panama, Belize, Barbados, Honduras and the Kuna General Congress for supporting our research, as well as the staff of the Bocas del Toro and Carrie Bow Cay research stations. We also acknowledge Myriam Morneau for help in the field and with the illustrations, as well as Edgardo Ochoa and Juan Mate. We also thank Marie-Claude Cote-Laurin and Jose Benchetrit for help in the field and Allen Herre for helpful discussions. NR 42 TC 9 Z9 9 U1 3 U2 34 PU ROYAL SOC PI LONDON PA 6-9 CARLTON HOUSE TERRACE, LONDON SW1Y 5AG, ENGLAND SN 0962-8452 J9 P ROY SOC B-BIOL SCI JI Proc. R. Soc. B-Biol. Sci. PD MAR 22 PY 2012 VL 279 IS 1731 BP 1085 EP 1092 DI 10.1098/rspb.2011.1549 PG 8 WC Biology; Ecology; Evolutionary Biology SC Life Sciences & Biomedicine - Other Topics; Environmental Sciences & Ecology; Evolutionary Biology GA 894HF UT WOS:000300417000006 PM 21937496 ER PT J AU Wurzburger, N Bellenger, JP Kraepiel, AML Hedin, LO AF Wurzburger, Nina Bellenger, Jean Philippe Kraepiel, Anne M. L. Hedin, Lars O. TI Molybdenum and Phosphorus Interact to Constrain Asymbiotic Nitrogen Fixation in Tropical Forests SO PLOS ONE LA English DT Article ID SOIL ORGANIC PHOSPHORUS; RAIN-FORESTS; LEAF-LITTER; LIMITATION; FRACTIONS; DYNAMICS; CYCLES; HAWAII; PANAMA AB Biological di-nitrogen fixation (N-2) is the dominant natural source of new nitrogen to land ecosystems. Phosphorus (P) is thought to limit N-2 fixation in many tropical soils, yet both molybdenum (Mo) and P are crucial for the nitrogenase reaction (which catalyzes N-2 conversion to ammonia) and cell growth. We have limited understanding of how and when fixation is constrained by these nutrients in nature. Here we show in tropical forests of lowland Panama that the limiting element on asymbiotic N-2 fixation shifts along a broad landscape gradient in soil P, where Mo limits fixation in P-rich soils while Mo and P co-limit in P-poor soils. In no circumstance did P alone limit fixation. We provide and experimentally test a mechanism that explains how Mo and P can interact to constrain asymbiotic N-2 fixation. Fixation is uniformly favored in surface organic soil horizons - a niche characterized by exceedingly low levels of available Mo relative to P. We show that soil organic matter acts to reduce molybdate over phosphate bioavailability, which, in turn, promotes Mo limitation in sites where P is sufficient. Our findings show that asymbiotic N-2 fixation is constrained by the relative availability and dynamics of Mo and P in soils. This conceptual framework can explain shifts in limitation status across broad landscape gradients in soil fertility and implies that fixation depends on Mo and P in ways that are more complex than previously thought. C1 [Wurzburger, Nina; Hedin, Lars O.] Princeton Univ, Dept Ecol & Evolutionary Biol, Princeton, NJ 08544 USA. [Wurzburger, Nina] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. [Bellenger, Jean Philippe] Princeton Univ, Dept Geosci, Princeton, NJ 08544 USA. [Kraepiel, Anne M. L.] Princeton Univ, Dept Chem, Princeton, NJ 08544 USA. RP Wurzburger, N (reprint author), Univ Georgia, Odum Sch Ecol, Athens, GA 30602 USA. EM lhedin@princeton.edu FU National Science Foundation [DEB-0614116]; Andrew W. Mellon Foundation FX This work was supported by the National Science Foundation grant #DEB-0614116 to LOH and the Andrew W. Mellon Foundation grant to LOH. The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 40 TC 29 Z9 30 U1 8 U2 91 PU PUBLIC LIBRARY SCIENCE PI SAN FRANCISCO PA 1160 BATTERY STREET, STE 100, SAN FRANCISCO, CA 94111 USA SN 1932-6203 J9 PLOS ONE JI PLoS One PD MAR 21 PY 2012 VL 7 IS 3 AR e33710 DI 10.1371/journal.pone.0033710 PG 7 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 939YN UT WOS:000303857100040 PM 22470462 ER PT J AU Berger, E Zauderer, A Pooley, GG Soderberg, AM Sari, R Brunthaler, A Bietenholz, MF AF Berger, E. Zauderer, A. Pooley, G. G. Soderberg, A. M. Sari, R. Brunthaler, A. Bietenholz, M. F. TI RADIO MONITORING OF THE TIDAL DISRUPTION EVENT SWIFT J164449.3+573451. I. JET ENERGETICS AND THE PRISTINE PARSEC-SCALE ENVIRONMENT OF A SUPERMASSIVE BLACK HOLE SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: nuclei; techniques: interferometric ID RAY BURST AFTERGLOWS; GALACTIC-CENTER; SAGITTARIUS-A; OUTBURST; GALAXY; STARS; MODEL; ATMOSPHERE; SUPERNOVAE AB We present continued radio observations of the tidal disruption event Swift J164449.3+573451 extending to delta t approximate to 216 days after discovery. The data were obtained with the EVLA, AMI Large Array, CARMA, the SMA, and the VLBA+Effelsberg as part of a long-term program to monitor the expansion and energy scale of the relativistic outflow, and to trace the parsec-scale environment around a previously dormant supermassive black hole (SMBH). The new observations reveal a significant change in the radio evolution starting at delta t approximate to 1 month, with a brightening at all frequencies that requires an increase in the energy by about an order of magnitude, and an overall density profile around the SMBH of rho proportional to r(-3/2) (0.1-1.2 pc) with a significant flattening at r approximate to 0.4-0.6 pc. The increase in energy cannot be explained with continuous injection from an L proportional to t(-5/3) tail, which is observed in the X-rays. Instead, we conclude that the relativistic jet was launched with a wide range of Lorentz factors, obeying E(> Gamma(j)) proportional to Gamma(-2.5)(j). The similar ratios of duration to dynamical timescale for Sw 1644+57 and gamma-ray bursts (GRBs) suggest that this result may be applicable to GRB jets as well. The radial density profile may be indicative of Bondi accretion, with the inferred flattening at r similar to 0.5 pc in good agreement with the Bondi radius for a similar to few x 10(6) M-circle dot black hole. The density at similar to 0.5 pc is about a factor of 30 times lower than inferred for the Milky Way Galactic Center, potentially due to a smaller number of mass-shedding massive stars. From our latest observations (delta t approximate to 216 days) we find that the jet energy is E-j,E-iso approximate to 5 x 10(53) erg (E-j approximate to 2.4 x 10(51) erg for theta(j) = 0.1), the radius is r approximate to 1.2 pc, the Lorentz factor is Gamma(j) approximate to 2.2, the ambient density is n approximate to 0.2 cm(-3), and the projected angular size is r(proj) approximate to 25 mu as, below the resolution of the VLBA+Effelsberg. Assuming no future changes in the observed evolution and a final integrated total energy of E-j approximate to 10(52) erg, we predict that the radio emission from Sw 1644+57 should be detectable with the EVLA for several decades and will be resolvable with very long baseline interferometry in a few years. C1 [Berger, E.; Zauderer, A.; Soderberg, A. M.; Sari, R.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Pooley, G. G.] Univ Cambridge, Cavendish Lab, Mullard Radio Astron Observ, Cambridge CB3 0HE, England. [Sari, R.] Hebrew Univ Jerusalem, Racah Inst Phys, IL-91904 Jerusalem, Israel. [Brunthaler, A.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Brunthaler, A.] Natl Radio Astron Observ, Socorro, NM 87801 USA. [Bietenholz, M. F.] York Univ, Dept Phys & Astron, Toronto, ON M3J 2R7, Canada. [Bietenholz, M. F.] Hartebeesthoek Radio Astron Observ, ZA-1740 Krugersdorp, South Africa. RP Berger, E (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. FU Swift AO6 [NNX10AI24G]; National Science Foundation [AST-1107973]; European Union [275596]; Smithsonian Institution; Academia Sinica FX We thank Ramesh Narayan, Ryan Chornock, and Nicholas Stone for helpful discussions, and Glen Petitpas for assistance with the SMA data reduction. E.B. acknowledges support from Swift AO6 Grant NNX10AI24G and from the National Science Foundation through Grant AST-1107973. A.B. is supported by a Marie Curie Outgoing International Fellowship (FP7) of the European Union (project number 275596). This work is partially based on observations with the 100 m telescope of the MPIfR (Max-Planck-Institut fur Radioastronomie) at Effelsberg. The Submillimeter Array is a joint project between the Smithsonian Astrophysical Observatory and the Academia Sinica Institute of Astronomy and Astrophysics, and is funded by the Smithsonian Institution and the Academia Sinica. Support for CARMA construction was derived from the Gordon and Betty Moore Foundation, the Kenneth T. and Eileen L. Norris Foundation, the James S. McDonnell Foundation, the Associates of the California Institute of Technology, the University of Chicago, the states of California, Illinois, and Maryland, and the National Science Foundation. Ongoing CARMA development and operations are supported by the National Science Foundation under a cooperative agreement, and by the CARMApartner universities. The AMI arrays are supported by the University of Cambridge and the STFC. This work made use of data supplied by the UK Swift Science Data Centre at the University of Leicester. NR 35 TC 60 Z9 60 U1 0 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAR 20 PY 2012 VL 748 IS 1 AR 36 DI 10.1088/0004-637X/748/1/36 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 906LU UT WOS:000301347500036 ER PT J AU Cool, RJ Eisenstein, DJ Kochanek, CS Brown, MJI Caldwell, N Dey, A Forman, WR Hickox, RC Jannuzi, BT Jones, C Moustakas, J Murray, SS AF Cool, Richard J. Eisenstein, Daniel J. Kochanek, Christopher S. Brown, Michael J. I. Caldwell, Nelson Dey, Arjun Forman, William R. Hickox, Ryan C. Jannuzi, Buell T. Jones, Christine Moustakas, John Murray, Stephen S. TI THE GALAXY OPTICAL LUMINOSITY FUNCTION FROM THE AGN AND GALAXY EVOLUTION SURVEY SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: luminosity function, mass function; galaxies: statistics ID DIGITAL SKY SURVEY; AUTOFIB REDSHIFT SURVEY; FIBER-FED SPECTROGRAPH; HUBBLE DEEP FIELD; SPECTRAL TYPE; DENSITY; Z-SIMILAR-TO-1; COMBO-17; SAMPLE; CONSTRUCTION AB We present the galaxy optical luminosity function for the redshift range 0.05 < z < 0.75 from the AGN and Galaxy Evolution Survey, a spectroscopic survey of 7.6 deg(2) in the Bootes field of the NOAO Deep Wide- Field Survey. Our statistical sample is composed of 12,473 galaxies with known redshifts down to I = 20.4 (AB). Our results at low redshift are consistent with those from Sloan Digital Sky Survey; at higher redshift, we find strong evidence for evolution in the luminosity function, including differential evolution between blue and red galaxies. We find that the luminosity density evolves as (1 + z)((0.54 +/- 0.64)) for red galaxies and (1 + z)((1.64 +/- 0.39)) for blue galaxies. C1 [Cool, Richard J.] Observ Carnegie Inst Washington, Pasadena, CA 91101 USA. [Eisenstein, Daniel J.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Kochanek, Christopher S.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. [Brown, Michael J. I.] Monash Univ, Sch Phys, Clayton, Vic 3800, Australia. [Caldwell, Nelson; Forman, William R.; Hickox, Ryan C.; Jones, Christine; Murray, Stephen S.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. [Dey, Arjun; Jannuzi, Buell T.] Natl Opt Astron Observ, Tucson, AZ 85726 USA. [Hickox, Ryan C.] Univ Durham, Dept Phys, Durham DH1 3LE, England. [Moustakas, John] Univ Calif San Diego, Ctr Astrophys & Space Sci, La Jolla, CA 92093 USA. [Murray, Stephen S.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21205 USA. RP Cool, RJ (reprint author), Observ Carnegie Inst Washington, 813 Santa Barbara St, Pasadena, CA 91101 USA. RI Brown, Michael/B-1181-2015 OI Brown, Michael/0000-0002-1207-9137 NR 51 TC 19 Z9 19 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAR 20 PY 2012 VL 748 IS 1 AR 10 DI 10.1088/0004-637X/748/1/10 PG 22 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 906LU UT WOS:000301347500010 ER PT J AU Huang, KY Urata, Y Tung, YH Lin, HM Xin, LP Yoshida, M Zheng, W Akerlof, C Wang, SY Ip, WH Lehner, MJ Bianco, FB Kawai, N Kuroda, D Marshall, SL Schwamb, ME Qiu, Y Wang, JH Wen, CY Wei, J Yanagisawa, K Zhang, ZW AF Huang, K. Y. Urata, Y. Tung, Y. H. Lin, H. M. Xin, L. P. Yoshida, M. Zheng, W. Akerlof, C. Wang, S. Y. Ip, W. H. Lehner, M. J. Bianco, F. B. Kawai, N. Kuroda, D. Marshall, S. L. Schwamb, M. E. Qiu, Y. Wang, J. H. Wen, C. Y. Wei, J. Yanagisawa, K. Zhang, Z. W. TI GRB 071112C: A CASE STUDY OF DIFFERENT MECHANISMS IN X-RAY AND OPTICAL TEMPORAL EVOLUTION SO ASTROPHYSICAL JOURNAL LA English DT Article DE gamma-ray burst: individual (GRB 071112C) ID INITIAL LORENTZ FACTOR; BURST AFTERGLOWS; LIGHT CURVES; THEORETICAL IMPLICATIONS; SWIFT; FLARES; ONSET; EMISSION; ORIGIN; SYSTEM AB We present a study on GRB 071112C X-ray and optical light curves. In these two wavelength ranges, we have found different temporal properties. The R-band light curve showed an initial rise followed by a single power-law decay, while the X-ray light curve was described by a single power-law decay plus a flare-like feature. Our analysis shows that the observed temporal evolution cannot be described by the external shock model in which the X-ray and optical emission are produced by the same emission mechanism. No significant color changes in multi-band light curves and a reasonable value of the initial Lorentz factor (Gamma(0) = 275 +/- 20) in a uniform interstellar medium support the afterglow onset scenario as the correct interpretation for the early R band rise. The result suggests that the optical flux is dominated by afterglow. Our further investigations show that the X-ray flux could be created by an additional feature related to energy injection and X-ray afterglow. Different theoretical interpretations indicate the additional feature in X-ray can be explained by either late internal dissipation or local inverse-Compton scattering in the external shock. C1 [Huang, K. Y.; Tung, Y. H.; Lin, H. M.; Wang, S. Y.; Lehner, M. J.; Wang, J. H.; Wen, C. Y.; Zhang, Z. W.] Acad Sinica, Inst Astron & Astrophys, Taipei 106, Taiwan. [Urata, Y.; Lin, H. M.; Ip, W. H.] Natl Cent Univ, Inst Astron, Chungli 32054, Taiwan. [Tung, Y. H.] Natl Tsing Hua Univ, Dept Phys, Hsinchu 30013, Taiwan. [Tung, Y. H.] Natl Tsing Hua Univ, Inst Astron, Hsinchu 30013, Taiwan. [Xin, L. P.; Qiu, Y.; Wei, J.] Chinese Acad Sci, Natl Astron Observ, Beijing 100012, Peoples R China. [Yoshida, M.] Hiroshima Univ, Hiroshima Astrophys Sci Ctr, Hiroshima 7398526, Japan. [Yoshida, M.; Kuroda, D.; Yanagisawa, K.] Natl Astron Observ Japan, Okayama Astrophys Observ, Okayama 7190232, Japan. [Zheng, W.; Akerlof, C.] Univ Michigan, Dept Phys, Ann Arbor, MI 48109 USA. [Lehner, M. J.] Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA. [Lehner, M. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Bianco, F. B.] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA. [Bianco, F. B.] Global Telescope Network Inc, Las Cumbres Observ, Goleta, CA 93117 USA. [Kawai, N.] Tokyo Inst Technol, Dept Phys, Meguro Ku, Tokyo 1528551, Japan. [Marshall, S. L.] Kavli Inst Particle Astrophys & Cosmol, Menlo Pk, CA 94025 USA. [Schwamb, M. E.] Yale Univ, Dept Phys, New Haven, CT 06520 USA. RP Huang, KY (reprint author), Acad Sinica, Inst Astron & Astrophys, POB 23-141, Taipei 106, Taiwan. OI Schwamb, Megan/0000-0003-4365-1455; Lehner, Matthew/0000-0003-4077-0985 FU Academia Sinica [AS-88-TP-A02]; NASA [NNX08AV63G]; NSF [PHY-0801007]; [NSC-99-2112-M-001-002-MY3]; [NSC-99-2112-M-008-003-MY3] FX This work is supported by grants NSC-99-2112-M-001-002-MY3 (K.Y.H.) and NSC-99-2112-M-008-003-MY3 (Y.U.). The TAOS project is supported in part by the thematic research program AS-88-TP-A02 at Academia Sinica and the ROTSE project is supported by NASA Grant NNX08AV63G and NSF Grant PHY-0801007. Access to the CFHT was made possible by the Ministry of Education and the National Science Council of Taiwan as part of the Cosmology and Particle Astrophysics (CosPA) initiative. This work made use of data supplied by the UK Swift Science Data Center at the University of Leicester. NR 57 TC 9 Z9 9 U1 0 U2 6 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAR 20 PY 2012 VL 748 IS 1 AR 44 DI 10.1088/0004-637X/748/1/44 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 906LU UT WOS:000301347500044 ER PT J AU Nelson, T Donato, D Mukai, K Sokoloski, J Chomiuk, L AF Nelson, Thomas Donato, Davide Mukai, Koji Sokoloski, Jennifer Chomiuk, Laura TI X-RAY EMISSION FROM AN ASYMMETRIC BLAST WAVE AND A MASSIVE WHITE DWARF IN THE GAMMA-RAY EMITTING NOVA V407 Cyg SO ASTROPHYSICAL JOURNAL LA English DT Article DE ultraviolet: stars; white dwarfs; X-rays: stars ID RS OPHIUCHI 2006; SWIFT OBSERVATIONS; INTERSTELLAR-MEDIUM; IA SUPERNOVA; V2491 CYG; OUTBURST; SHOCK; SPECTROSCOPY; ABSORPTION; MODELS AB Classical nova events in symbiotic stars, although rare, offer a unique opportunity to probe the interaction between ejecta and a dense environment in stellar explosions. In this work, we use X-ray data obtained with Swift and Suzaku during the recent classical nova outburst in V407 Cyg to explore such an interaction. We find evidence of both equilibrium and non-equilibrium ionization plasmas at the time of peak X-ray brightness, indicating a strong asymmetry in the density of the emitting region. Comparing a simple model to the data, we find that the X-ray evolution is broadly consistent with nova ejecta driving a forward shock into the dense wind of the Mira companion. We detect a highly absorbed soft X-ray component in the spectrum during the first 50 days of the outburst that is consistent with supersoft emission from the nuclear burning white dwarf. The high temperature and short turnoff time of this emission component, in addition to the observed breaks in the optical and UV light curves, indicate that the white dwarf in the binary is extremely massive. Finally, we explore the connections between the X-ray and GeV gamma-ray evolution, and propose that the gamma-ray turnoff is due to the stalling of the forward shock as the ejecta reach the red giant surface. C1 [Nelson, Thomas; Donato, Davide; Mukai, Koji] NASA, Goddard Space Flight Ctr, CRESST, Greenbelt, MD 20771 USA. [Nelson, Thomas; Donato, Davide; Mukai, Koji] NASA, Goddard Space Flight Ctr, Xray Astrophys Lab, Greenbelt, MD 20771 USA. [Nelson, Thomas; Mukai, Koji] Univ Maryland Baltimore Cty, Ctr Space Sci & Technol, Baltimore, MD 21250 USA. [Donato, Davide] Univ Maryland, Dept Phys, College Pk, MD 20742 USA. [Donato, Davide] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Sokoloski, Jennifer] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA. [Chomiuk, Laura] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Chomiuk, Laura] Natl Radio Astron Observ, Socorro, NM 87801 USA. RP Nelson, T (reprint author), Univ Minnesota, Sch Phys & Astron, 115 Church St SE, Minneapolis, MN 55455 USA. EM tnelson@physics.umn.ed RI XRAY, SUZAKU/A-1808-2009 NR 41 TC 24 Z9 24 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAR 20 PY 2012 VL 748 IS 1 AR 43 DI 10.1088/0004-637X/748/1/43 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 906LU UT WOS:000301347500043 ER PT J AU Neufeld, DA Roueff, E Snell, RL Lis, D Benz, AO Bruderer, S Black, JH De Luca, M Gerin, M Goldsmith, PF Gupta, H Indriolo, N Le Bourlot, J Le Petit, F Larsson, B Melnick, GJ Menten, KM Monje, R Nagy, Z Phillips, TG Sandqvist, A Sonnentrucker, P van der Tak, F Wolfire, MG AF Neufeld, David A. Roueff, Evelyne Snell, Ronald L. Lis, Dariusz Benz, Arnold O. Bruderer, Simon Black, John H. De Luca, Massimo Gerin, Maryvonne Goldsmith, Paul F. Gupta, Harshal Indriolo, Nick Le Bourlot, Jacques Le Petit, Franck Larsson, Bengt Melnick, Gary J. Menten, Karl M. Monje, Raquel Nagy, Zsofia Phillips, Thomas G. Sandqvist, Aage Sonnentrucker, Paule van der Tak, Floris Wolfire, Mark G. TI HERSCHEL OBSERVATIONS OF INTERSTELLAR CHLORONIUM SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM: molecules; molecular processes; submillimeter: ISM ID CHLORINE-BEARING MOLECULES; HYDROGEN-CHLORIDE; DIFFUSE CLOUDS; G10.6-0.4 W31C; SIGHT-LINES; ORION-BAR; ABSORPTION; OMC-1; EXCITATION; EMISSION AB Using the Herschel Space Observatory's Heterodyne Instrument for the Far-Infrared, we have observed parachloronium (H2Cl+) toward six sources in the Galaxy. We detected interstellar chloronium absorption in foreground molecular clouds along the sight lines to the bright submillimeter continuum sources Sgr A (+50 km s(-1) cloud) and W31C. Both the para-(H2Cl+)-Cl-35 and para-(H2Cl+)-Cl-37 isotopologues were detected, through observations of their 1(11)-0(00) transitions at rest frequencies of 485.42 and 484.23 GHz, respectively. For an assumed ortho-to-para ratio (OPR) of 3, the observed optical depths imply that chloronium accounts for similar to 4%-12% of chlorine nuclei in the gas phase. We detected interstellar chloronium emission from two sources in the Orion Molecular Cloud 1: the Orion Bar photodissociation region and the Orion South condensation. For an assumed OPR of 3 for chloronium, the observed emission line fluxes imply total beam-averaged column densities of similar to 2 x 10(13) cm(-2) and similar to 1.2 x 10(13) cm(-2), respectively, for chloronium in these two sources. We obtained upper limits on the para-(H2Cl+)-Cl-35 line strengths toward H-2 Peak 1 in the Orion Molecular cloud and toward the massive young star AFGL 2591. The chloronium abundances inferred in this study are typically at least a factor similar to 10 larger than the predictions of steady-state theoretical models for the chemistry of interstellar molecules containing chlorine. Several explanations for this discrepancy were investigated, but none has proven satisfactory, and thus the large observed abundances of chloronium remain puzzling. C1 [Neufeld, David A.; Indriolo, Nick] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Roueff, Evelyne; Le Bourlot, Jacques; Le Petit, Franck] Observ Paris, LUTH UMR 8102, F-92195 Meudon, France. [Snell, Ronald L.] Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA. [Lis, Dariusz; Monje, Raquel; Phillips, Thomas G.] CALTECH, Dept Astron, Pasadena, CA 91125 USA. [Benz, Arnold O.] Swiss Fed Inst Technol, Inst Astron, CH-8092 Zurich, Switzerland. [Bruderer, Simon] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Black, John H.; Larsson, Bengt] Chalmers, Dept Earth & Space Sci, Onsala, Sweden. [De Luca, Massimo; Gerin, Maryvonne] UPMC, Ecole Normale Super, Observ Paris, UMR CNRS 8112,LERMA, Paris, France. [Goldsmith, Paul F.; Gupta, Harshal] CALTECH, JPL, Pasadena, CA 91125 USA. [Melnick, Gary J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Menten, Karl M.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Nagy, Zsofia; van der Tak, Floris] Univ Groningen, Kapteyn Astron Inst, Groningen, Netherlands. [Sandqvist, Aage] Stockholm Univ, Stockholm Observ, AlbaNova Univ Ctr, S-10691 Stockholm, Sweden. [Sonnentrucker, Paule] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [van der Tak, Floris] SRON Netherlands Inst Space Res, NL-9747 AD Groningen, Netherlands. [Wolfire, Mark G.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. RP Neufeld, DA (reprint author), Johns Hopkins Univ, Dept Phys & Astron, 3400 N Charles St, Baltimore, MD 21218 USA. RI Goldsmith, Paul/H-3159-2016; OI Indriolo, Nick/0000-0001-8533-6440; Black, John/0000-0001-7221-7207 FU NASA through JPL/Caltech FX Support for this work was provided by NASA through an award issued by JPL/Caltech. NR 51 TC 26 Z9 26 U1 0 U2 10 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAR 20 PY 2012 VL 748 IS 1 AR 37 DI 10.1088/0004-637X/748/1/37 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 906LU UT WOS:000301347500037 ER PT J AU Romanowsky, AJ Strader, J Brodie, JP Mihos, JC Spitler, LR Forbes, DA Foster, C Arnold, JA AF Romanowsky, Aaron J. Strader, Jay Brodie, Jean P. Mihos, J. Christopher Spitler, Lee R. Forbes, Duncan A. Foster, Caroline Arnold, Jacob A. TI THE ONGOING ASSEMBLY OF A CENTRAL CLUSTER GALAXY: PHASE-SPACE SUBSTRUCTURES IN THE HALO OF M87 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: elliptical and lenticular, cD; galaxies: formation; galaxies: halos; galaxies: individual (M87); galaxies: kinematics and dynamics; galaxies: star clusters: general ID DARK-MATTER HALO; EXTRAGALACTIC GLOBULAR-CLUSTERS; SUPERMASSIVE BLACK-HOLE; GIANT SOUTHERN STREAM; VIRGO-CLUSTER; PLANETARY-NEBULAE; ELLIPTIC GALAXIES; MASSIVE GALAXIES; MILKY-WAY; SIZE EVOLUTION AB The halos of galaxies preserve unique records of their formation histories. We carry out the first combined observational and theoretical study of phase-space halo substructure in an early-type galaxy: M87, the central galaxy in the Virgo cluster. We analyze an unprecedented wide-field, high-precision photometric and spectroscopic data set for 488 globular clusters (GCs), which includes new, large-radius Subaru/Suprime-Cam and Keck/DEIMOS observations. We find signatures of two substructures in position-velocity phase space. One is a small, cold stream associated with a known stellar filament in the outer halo; the other is a large shell-like pattern in the inner halo that implies a massive, hitherto unrecognized accretion event. We perform extensive statistical tests and independent metallicity analyses to verify the presence and characterize the properties of these features, and to provide more general methodologies for future extragalactic studies of phase-space substructure. The cold outer stream is consistent with a dwarf galaxy accretion event, while for the inner shell there is tension between a low progenitor mass implied by the cold velocity dispersion, and a high mass from the large number of GCs, which might be resolved by a similar to 0.5 L* E/S0 progenitor. We also carry out proof-of-principle numerical simulations of the accretion of smaller galaxies in an M87-like gravitational potential. These produce analogous features to the observed substructures, which should have observable lifetimes of similar to 1 Gyr. The shell and stream GCs together support a scenario where the extended stellar envelope of M87 has been built up by a steady rain of material that continues until the present day. This phase-space method demonstrates unique potential for detailed tests of galaxy formation beyond the Local Group. C1 [Romanowsky, Aaron J.; Brodie, Jean P.; Arnold, Jacob A.] Univ Calif Observ, Santa Cruz, CA 95064 USA. [Strader, Jay] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Mihos, J. Christopher] Case Western Reserve Univ, Dept Astron, Cleveland, OH 44106 USA. [Spitler, Lee R.; Forbes, Duncan A.; Foster, Caroline] Swinburne Univ Technol, Ctr Astrophys & Supercomp, Hawthorn, Vic 3122, Australia. [Foster, Caroline] European So Observ, Santiago 19, Chile. RP Romanowsky, AJ (reprint author), Univ Calif Observ, 1156 High St, Santa Cruz, CA 95064 USA. RI Spitler, Lee/A-9867-2013; OI Spitler, Lee/0000-0001-5185-9876; Mihos, Chris/0000-0002-7089-8616; Foster, Caroline/0000-0003-0247-1204 FU NSF [AST-0808099, AST-0909237, AST-1101733, AST-1109878, AST-0607526, AST-0707793]; UCSC University Affiliated Research Center; NASA [NAS5-26555]; W. M. Keck Foundation; Canadian Space Agency FX J.B. and A.J.R. acknowledge support from the NSF through grants AST-0808099, AST-0909237, AST-1101733, and AST-1109878, and by the UCSC University Affiliated Research Center's Aligned Research Program. J.S. was supported by NASA through a Hubble Fellowship, administered by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Incorporated, under NASA Contract NAS5-26555. J.C.M. has been supported by the NSF through grants AST-0607526 and AST-0707793. We acknowledge financial support from the Access to Major Research Facilities Programme, a component of the International Science Linkages Programme established under the Australian Government's innovation statement, Backing Australia's Ability.; Much of the data presented herein were obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California, and the National Aeronautics and Space Administration. The Observatory was made possible by the generous financial support of the W. M. Keck Foundation. Observations reported here were obtained at the MMT Observatory, a joint facility of the Smithsonian Institution and the University of Arizona. Based in part on data collected at Subaru Telescope (which is operated by the National Astronomical Observatory of Japan), via a Gemini Observatory time exchange (GN-2009A-C-204). 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. We acknowledge the usage of the HyperLeda database (http://leda.univ-lyon1.fr). This research has made use of the NASA/IPAC Extragalactic Database (NED) which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. Based on observations made with the NASA/ESA Hubble Space Telescope, and obtained from the Hubble Legacy Archive, which is a collaboration between the Space Telescope Science Institute (STScI/NASA), the Space Telescope European Coordinating Facility (ST-ECF/ESA), and the Canadian Astronomy Data Centre (CADC/NRC/CSA). NR 135 TC 46 Z9 46 U1 0 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAR 20 PY 2012 VL 748 IS 1 AR 29 DI 10.1088/0004-637X/748/1/29 PG 23 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 906LU UT WOS:000301347500029 ER PT J AU Servillat, M Grindlay, J van den Berg, M Hong, J Zhao, P Allen, B AF Servillat, M. Grindlay, J. van den Berg, M. Hong, J. Zhao, P. Allen, B. TI SPECTROSCOPIC FOLLOW-UP OF X-RAY SOURCES IN THE ChaMPlane SURVEY: IDENTIFICATION OF A NEW CATACLYSMIC VARIABLE SO ASTROPHYSICAL JOURNAL LA English DT Article DE novae, cataclysmic variables; stars: late-type; surveys; X-rays: individual (CXOPS J154305.5-522709) ID ALL-SKY SURVEY; GALACTIC-CENTER; LIMITING WINDOW; ORBITAL PERIOD; POINT SOURCES; M-DWARFS; POPULATION; BINARIES; MASS; PHOTOMETRY AB We present a multi-object optical spectroscopy follow-up study of X-ray sources in a field along the Galactic plane (l = 327 degrees.42, b = 2 degrees.26) which is part of the Chandra Multi-wavelength Plane survey (ChaMPlane). We obtained spectra for 46 stars, including 15 likely counterparts to X-ray sources, and sources showing an Ha color excess. This has led to the identification of a new cataclysmic variable (CV), CXOPS J154305.5-522709, also named ChaMPlane Bright Source 7 (CBS 7), and we identified eight X-ray sources in the field as active late-type stars. CBS 7 was previously studied in X-rays and showed a hard spectrum and two periods: 1.22 +/- 0.08 hr and 2.43 +/- 0.26 hr. We present here clear evidence that the source is a CV through the detection of H, He I, and He II emission lines in its optical spectrum. The hard X-ray spectrum and the presence of the He II lambda 4686 in emission with a large equivalent width suggest a magnetic CV. The near-infrared counterpart is significantly variable, and we found a period consistent with the longest X-ray period at 2.39 +/- 0.05 hr but not the shortest X-ray period. If this period is the orbital period, this would place the system in the CV period gap. The possible orbital period suggests a dM4 +/- 1 companion star. The distance is then estimated to be similar to 1 kpc. The system could be a relatively hard and X-ray luminous polar or an intermediate polar, possibly nearly synchronous. C1 [Servillat, M.; Grindlay, J.; van den Berg, M.; Hong, J.; Zhao, P.; Allen, B.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [van den Berg, M.] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 XH Amsterdam, Netherlands. RP Servillat, M (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS-67, Cambridge, MA 02138 USA. EM mservillat@cfa.harvard.edu FU NASA/Chandra [AR9-0013X, GO9-0102X]; NSF [AST-0909073]; Chandra X-ray Center (CXC) FX We thank the anonymous referee for useful comments that helped improve the paper. We acknowledge support from NASA/Chandra grants AR9-0013X, GO9-0102X, and NSF grant AST-0909073. We thank the Chandra X-ray Center (CXC) for support. STSDAS, PyRAF, and Specview are products of the Space Telescope Science Institute, which is operated by AURA for NASA. NR 51 TC 7 Z9 7 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAR 20 PY 2012 VL 748 IS 1 AR 32 DI 10.1088/0004-637X/748/1/32 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 906LU UT WOS:000301347500032 ER PT J AU Takami, M Chen, HH Karr, JL Lee, HT Lai, SP Minh, YC AF Takami, Michihiro Chen, How-Huan Karr, Jennifer L. Lee, Hsu-Tai Lai, Shih-Ping Minh, Young-Chol TI EMISSION MECHANISM OF "GREEN FUZZIES" IN HIGH-MASS STAR-FORMING REGIONS SO ASTROPHYSICAL JOURNAL LA English DT Article DE infrared: ISM; scattering ID YOUNG STELLAR OBJECTS; INFRARED ARRAY CAMERA; 2-DIMENSIONAL RADIATIVE-TRANSFER; DENSE PHOTODISSOCIATION REGIONS; MOLECULAR-HYDROGEN EMISSION; SPITZER-IRAC EMISSION; PROTOSTAR G192.16-3.82; ASTROPHYSICAL MEDIA; OUTFLOW CANDIDATES; INTERSTELLAR DUST AB The Infrared Array Camera (IRAC) on the Spitzer Space Telescope has revealed that a number of high- mass protostars are associated with extended mid- infrared emission, particularly prominent at 4.5 mu m. These are called "Green Fuzzy" emission or "Extended Green Objects." We present color analysis of this emission toward six nearby (d = 2- 3 kpc) well- studied high- mass protostars and three candidate high- mass protostars identified with the Spitzer GLIMPSE survey. In our color- color diagrams, most of the sources show a positive correlation between the [3.6]-[4.5] and [3.5]-[5.8] colors along the extinction vector in all or part of the region. We compare the colors with those of scattered continuum associated with the low- mass protostar L 1527, modeled scattered continuum in cavities, shocked emission associated with low- mass protostars, modeled H2 emission for thermal and fluorescent cases, and modeled polycyclic aromatic hydrocarbon (PAH) emission. Of the emission mechanisms discussed above, scattered continuum provides the simplest explanation for the observed linear correlation. In this case, the color variation within each object is attributed to different foreground extinctions at different positions. Alternative possible emission mechanisms to explain this correlation may be a combination of thermal and fluorescent H2 emission in shocks, and a combination of scattered continuum and thermal H2 emission, but detailed models or spectroscopic follow- up are required to investigate this possibility further. Our color- color diagrams also show possible contributions from PAHs in two objects. However, none of our samples show clear evidence for PAH emission directly associated with the high- mass protostars, several of which should be associated with ionizing radiation. This suggests that these protostars are heavily embedded even at mid- infrared wavelengths. C1 [Takami, Michihiro; Chen, How-Huan; Karr, Jennifer L.; Lee, Hsu-Tai] Acad Sinica, Inst Astron & Astrophys, Taipei 10617, Taiwan. [Chen, How-Huan; Lai, Shih-Ping] Natl Tsing Hua Univ, Dept Phys, Hsinchu 30013, Taiwan. [Chen, How-Huan] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Minh, Young-Chol] Korea Astron & Space Sci Inst, Taejon 305348, South Korea. RP Takami, M (reprint author), Acad Sinica, Inst Astron & Astrophys, POB 23-141, Taipei 10617, Taiwan. EM hiro@asiaa.sinica.edu.tw FU National Science Council of Taiwan [98-2112-M-001-002MY3, 100-2112-M-001-007-MY3] FX We first thank the two anonymous referees for careful reviews and useful discussions. We are grateful for Drs. Ho, Hirashita, and Hirano for useful discussions. The IRAC images were obtained through the Spitzer archive operated by IPAC. This research made use of the Simbad database operated at CDS, Strasbourg, France, and the NASA's Astrophysics Data System Abstract Service. This study is supported by the National Science Council of Taiwan (grant nos. 98-2112-M-001-002MY3 and 100-2112-M-001-007-MY3). NR 81 TC 8 Z9 8 U1 0 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAR 20 PY 2012 VL 748 IS 1 AR 8 DI 10.1088/0004-637X/748/1/8 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 906LU UT WOS:000301347500008 ER PT J AU van den Berg, M Penner, K Hong, J Grindlay, JE Zhao, P Laycock, S Servillat, M AF van den Berg, Maureen Penner, Kyle Hong, JaeSub Grindlay, Jonathan E. Zhao, Ping Laycock, Silas Servillat, Mathieu TI THE ChaMPlane BRIGHT X-RAY SOURCES-GALACTIC LONGITUDES l=2 degrees-358 degrees SO ASTROPHYSICAL JOURNAL LA English DT Article DE novae, cataclysmic variables; stars: flare; stars: individual (CXOPS J154305.5-522709, CXOPS J171340.5-395213, CXOPS J175900.8-334548, HD 9743); surveys; X-rays: binaries; X-rays: stars ID ALL-SKY SURVEY; ACTIVE BINARY CORONAE; PLANE SURVEY; CATACLYSMIC VARIABLES; SOLAR NEIGHBORHOOD; SYMBIOTIC STARS; LIMITING WINDOW; EXTINCTION MAP; POINT SOURCES; L-DWARF AB The Chandra Multi-wavelength Plane (ChaMPlane) survey aims to constrain the Galactic population of mainly accretion-powered, but also coronal, low-luminosity X-ray sources (L-X less than or similar to 10(33) erg s(-1)). To investigate the X-ray source content in the plane at fluxes F-X greater than or similar to 3 x 10(-14) erg s(-1) cm(-2), we study 21 of the brightest ChaMPlane sources, viz., those with >250 net counts (0.3-8 keV). By excluding the heavily obscured central part of the plane, our optical/near-infrared follow-up puts useful constraints on their nature. We have discovered two likely accreting white dwarf binaries. CXOPS J154305.5-522709 (CBS 7) is a cataclysmic variable showing periodic X-ray flux modulations on 1.2 hr and 2.4 hr; given its hard spectrum the system is likely magnetic. We identify CXOPS J175900.8-334548 (CBS 17) with a late-type giant; if the X-rays are indeed accretion powered, it belongs to the small but growing class of symbiotic binaries lacking strong optical nebular emission lines. CXOPS J171340.5-395213 (CBS 14) is an X-ray transient that brightened greater than or similar to 100 times. We tentatively classify it as a very late type (>M7) dwarf, of which few have been detected in X-rays. The remaining sources are (candidate) active galaxies, normal stars and active binaries, and a plausible young T Tauri star. The derived cumulative number density versus flux (log N-log S) relation for the Galactic sources appears flatter than expected for an isotropic distribution, indicating that we are seeing a non-local sample of mostly coronal sources. Our findings define source templates that we can use, in part, to classify the >10(4) fainter sources in ChaMPlane. C1 [van den Berg, Maureen] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 XH Amsterdam, Netherlands. [van den Berg, Maureen; Hong, JaeSub; Grindlay, Jonathan E.; Zhao, Ping; Servillat, Mathieu] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Penner, Kyle] Univ Arizona, Dept Astron, Tucson, AZ 85721 USA. [Laycock, Silas] Univ Massachusetts, Dept Phys, Lowell, MA USA. RP van den Berg, M (reprint author), Univ Amsterdam, Astron Inst Anton Pannekoek, Sci Pk 904, NL-1098 XH Amsterdam, Netherlands. EM maureen@head.cfa.harvard.edu FU NSF [AST-0098683]; Chandra grants [GO3-4033A, GO6-7088X]; Chandra X-ray Center FX This work was supported by NSF grants AST-0098683, Chandra grants GO3-4033A and GO6-7088X, and includes work carried out (by K. Penner) as part of the Research Experience for Undergraduates program at the Harvard-Smithsonian Center for Astrophysics. We thank J. Hernandez for providing the SPTCLASS code and K. Stassun for discussing the optical and near-infrared properties of young stars. We also thank the Chandra X-ray Center for support. NR 76 TC 12 Z9 12 U1 0 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAR 20 PY 2012 VL 748 IS 1 AR 31 DI 10.1088/0004-637X/748/1/31 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 906LU UT WOS:000301347500031 ER PT J AU Carvalho, S Biro, D Cunha, E Hockingss, K McGrew, WC Richmond, BG Matsuzawa, T AF Carvalho, Susana Biro, Dora Cunha, Eugenia Hockingss, Kimberley McGrew, William C. Richmond, Brian G. Matsuzawa, Tetsuro TI Chimpanzee carrying behaviour and the origins of human bipedality SO CURRENT BIOLOGY LA English DT Letter C1 [Carvalho, Susana] Univ Cambridge, Dept Archaeol & Anthropol, Leverhulme Ctr Human Evolutionary Studies, Cambridge CB2 1QH, England. [Carvalho, Susana] Univ Coimbra, Ctr Res Anthropol & Hlth, P-3000056 Coimbra, Portugal. [Biro, Dora] Univ Oxford, Dept Zool, Oxford OX1 3PS, England. [Cunha, Eugenia] Univ Coimbra, Life Sci Dept, P-3000056 Coimbra, Portugal. [Hockingss, Kimberley] Univ Nova Lisboa, FCSH, Ctr Res Anthropol, P-1069061 Lisbon, Portugal. [McGrew, William C.] Univ Cambridge, Dept Archaeol & Anthropol, Cambridge CB2 1QH, England. [Richmond, Brian G.] George Washington Univ, Ctr Adv Study Hominid Paleobiol, Dept Anthropol, Washington, DC 20052 USA. [Richmond, Brian G.] Smithsonian Inst, Natl Museum Nat Hist, Human Origins Program, Washington, DC 20052 USA. [Matsuzawa, Tetsuro] Kyoto Univ, Primate Res Inst, Inuyama, Aichi 4848506, Japan. RP Carvalho, S (reprint author), Univ Cambridge, Dept Archaeol & Anthropol, Leverhulme Ctr Human Evolutionary Studies, Fitzwilliam St, Cambridge CB2 1QH, England. EM scr50@cam.ac.uk; dora.biro@zoo.ox.ac.uk RI Cunha, Eugenia/E-9725-2013; OI Cunha, Eugenia/0000-0003-2998-371X; Biro, Dora/0000-0002-3408-6274; Hockings, Kimberley/0000-0002-6187-644X; Carvalho, Susana/0000-0003-4542-3720 NR 10 TC 18 Z9 20 U1 6 U2 67 PU CELL PRESS PI CAMBRIDGE PA 600 TECHNOLOGY SQUARE, 5TH FLOOR, CAMBRIDGE, MA 02139 USA SN 0960-9822 J9 CURR BIOL JI Curr. Biol. PD MAR 20 PY 2012 VL 22 IS 6 BP R180 EP R181 DI 10.1016/j.cub.2012.01.052 PG 2 WC Biochemistry & Molecular Biology; Cell Biology SC Biochemistry & Molecular Biology; Cell Biology GA 913PW UT WOS:000301890900004 PM 22440797 ER PT J AU Belokobylskij, SA Kula, RR AF Belokobylskij, Sergey A. Kula, Robert R. TI Review of the brachypterous, micropterous, and apterous Braconidae of the cyclostome lineage (Hymenoptera: Ichneumonoidea) from the Palearctic Region SO ZOOTAXA LA English DT Article DE descriptions; distribution; identification; key; new species; new records; parasitoid; taxonomy ID SUBFAMILY DORYCTINAE HYMENOPTERA; RDNA GENE-SEQUENCES; PARTIAL 16S RDNA; SPATHIUS NEES; PHYLOGENETIC-RELATIONSHIPS; WASPS HYMENOPTERA; INSECTA; JAPAN; RNA; D2 AB The Palearctic species of Braconidae with brachypterous, micropterous, or apterous modification are discussed. The following new species are described: Chremylus planispinus Belokobylskij (France, Algeria), Chremylus algecirasus Belokobylskij (Spain), Pambolus erogolus Belokobylskij (Mongolia), Pambolus ovchinnikovi Belokobylskij (Kyrgyzstan), Hormius stauropolicus Belokobylskij (Russia (North Caucasus)), Bracon (Habrobracon) barbieri Belokobylskij (Algeria), and Panerema kamtshatica Belokobylskij (Russia (Kamchatka)). The following species are redescribed: Heterospilus hemipterus (Thomson) (male and female), Chremylus pomonellae (Atanasov) (male, female and macropterous form), Hormius minialatus Tobias (female), and Aleiodes (Chelonorhogas) hemipterus Marshall (male and female). Lituania brachyptera Jakimavicius, 1968 is a new synonym of Eurybolus hemipterus Thomson, 1892. Chremylus pomonellae (Atanasov), new combination, is transferred from Rhyssalus. Aleiodes hemipterus is placed in the subgenus Chelonorhogas Enderlein. Asobara subalata (Zaykov & Fischer) is returned from Phaenocarpa Foerster. New distribution records are reported for Ecphylus (Sactopus) caudatus Ruschka, H. hemipterus, Rhaconotus hispanicus Belokobylskij, Pambolus tricolor (Ruthe), Hormius minialatus Tobias, A. (C.) hemipterus, and Pseudopezomachus kasparyani Tobias. A key for identifying all Palearctic flightless cyclostome braconid species, and the genera in which they are placed, is provided. A discussion about the diversity, morphological characters, and natural history of wing size reduction, and possible reasons for flightlessness, is provided. C1 [Belokobylskij, Sergey A.] Russian Acad Sci, Inst Zool, St Petersburg 199034, Russia. [Belokobylskij, Sergey A.] Polish Acad Sci, Museum & Inst Zool, PL-00679 Warsaw, Poland. [Kula, Robert R.] ARS, Systemat Entomol Lab, Inst Plant Sci, USDA,Natl Museum Nat Hist,Smithsonian Inst, Washington, DC 20013 USA. RP Belokobylskij, SA (reprint author), Russian Acad Sci, Inst Zool, St Petersburg 199034, Russia. EM doryctes@yahoo.com; Robert.Kula@ars.usda.gov FU Russian Foundation for Basic Research [10-04-00265]; Presidium of the Russian Academy of Sciences FX The first author is very thankful to Claire Villemant (Paris, France), Gavin Broad (BMNH), Jeno Papp (Budapest, Hungary), and Alejandro Zaldivar-Riveron (Mexico City, Mexico) for the opportunity to study the types and additional material from collections and for their valuable help. The second author is grateful to Alexander Konstantinov (Systematic Entomology Laboratory [SEL], USDA-ARS, Washington, DC) for interpreting articles published in Russian. Thomas Henry (SEL), Steven Lingafelter, (SEL), and Paul Marsh (Kansas State University, Manhattan) kindly reviewed the manuscript prior to submission. We also thank Gavin Broad (Natural History Museum, London) and John Jennings (University of Adelaide) for useful comments. The present work was partly supported by a grant of the Russian Foundation for Basic Research (No. 10-04-00265) and by the Presidium of the Russian Academy of Sciences Program "Origin of Biosphere and Evolution of Geobiological System." The United States Department of Agriculture is an equal opportunity provider and employer. NR 148 TC 5 Z9 6 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 MAR 20 PY 2012 IS 3240 BP 1 EP 62 PG 62 WC Zoology SC Zoology GA 939LQ UT WOS:000303812700001 ER PT J AU Hubert, N Meyer, CP Bruggemann, HJ Guerin, F Komeno, RJL Espiau, B Causse, R Williams, JT Planes, S AF Hubert, Nicolas Meyer, Christopher P. Bruggemann, Henrich J. Guerin, Fabien Komeno, Roberto J. L. Espiau, Benoit Causse, Romain Williams, Jeffrey T. Planes, Serge TI Cryptic Diversity in Indo-Pacific Coral-Reef Fishes Revealed by DNA-Barcoding Provides New Support to the Centre-of-Overlap Hypothesis SO PLOS ONE LA English DT Article ID BIODIVERSITY HOTSPOTS; MARINE BIODIVERSITY; HISTORICAL BIOGEOGRAPHY; CONSERVATION PRIORITIES; SOUTHEAST-ASIA; TELEOSTEI; PATTERNS; PHYLOGEOGRAPHY; CONSEQUENCES; COLOR AB Diversity in coral reef fishes is not evenly distributed and tends to accumulate in the Indo-Malay-Philippines Archipelago (IMPA). The comprehension of the mechanisms that initiated this pattern is in its infancy despite its importance for the conservation of coral reefs. Considering the IMPA either as an area of overlap or a cradle of marine biodiversity, the hypotheses proposed to account for this pattern rely on extant knowledge about taxonomy and species range distribution. The recent large-scale use of standard molecular data (DNA barcoding), however, has revealed the importance of taking into account cryptic diversity when assessing tropical biodiversity. We DNA barcoded 2276 specimens belonging to 668 coral reef fish species through a collaborative effort conducted concomitantly in both Indian and Pacific oceans to appraise the importance of cryptic diversity in species with an Indo-Pacific distribution range. Of the 141 species sampled on each side of the IMPA, 62 presented no spatial structure whereas 67 exhibited divergent lineages on each side of the IMPA with K2P distances ranging between 1% and 12%, and 12 presented several lineages with K2P distances ranging between 3% and 22%. Thus, from this initial pool of 141 nominal species with Indo-Pacific distribution, 79 dissolved into 165 biological units among which 162 were found in a single ocean. This result is consistent with the view that the IMPA accumulates diversity as a consequence of its geological history, its location on the junction between the two main tropical oceans and the presence of a land bridge during glacial times in the IMPA that fostered allopatric divergence and secondary contacts between the Indian and Pacific oceans. C1 [Hubert, Nicolas; Bruggemann, Henrich J.] Univ La Reunion, Lab ECOMAR, Fac Sci & Technol, St Denis, Reunion. [Hubert, Nicolas; Espiau, Benoit; Planes, Serge] Univ Perpignan, CNRS EPHE, CRIOBE CBETM, F-66025 Perpignan, France. [Meyer, Christopher P.] Smithsonian Inst, Dept Invertebrate Zool, Natl Museum Nat Hist, Washington, DC 20560 USA. [Guerin, Fabien] Univ La Reunion, UMR PVBMT, Fac Sci & Technol, St Denis, Reunion. [Komeno, Roberto J. L.] Univ Toliara, Inst Halieut & Sci Marines, Toliara, Madagascar. [Causse, Romain] Museum Natl Hist Nat, Dept Milieux & Peuplements Aquat, F-75231 Paris, France. [Williams, Jeffrey T.] Smithsonian Inst, Dept Vertebrate Zool, Natl Museum Nat Hist, Washington, DC 20560 USA. RP Hubert, N (reprint author), Univ La Reunion, Lab ECOMAR, Fac Sci & Technol, St Denis, Reunion. EM nicolas.hubert@ird.fr FU French 'Agence Nationale de Recherche' (ANR) [ANR-06-BDIV-002]; Gordon and Betty Moore Foundation; National Museum of Natural History; UMR PVBMT, Universite de la Reunion; Florida Museum of Natural History; University of California Berkeley - Gump Station, Moorea; Universite Paul Sabatier, Toulouse FX Funding was provided by the French 'Agence Nationale de Recherche' (ANR programme BIOTAS, no. ANR-06-BDIV-002) and by the Gordon and Betty Moore Foundation. We thank the Leonard P. Schultz Fund, National Museum of Natural History for providing travel funding for J. T. Williams. The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript.; We thank Dominique Strasberg (UMR PVBMT, Universite de la Reunion), Gustav Paulay (Florida Museum of Natural History), Neil Davies (University of California Berkeley - Gump Station, Moorea) and Christophe Thebaut (Universite Paul Sabatier, Toulouse) for their support; Julien Grignon, David Lecchini, Vanessa Messmer and Rene Galzin from the USR 3278 - CRIOBE (Moorea) for their help during the field sampling in French Polynesia; Jean Maharavo (Centre National de Recherches sur l'Environnement - CNRO, B. P. 7139, Fiadanana - Antananarivo, Madagascar) for his assistance in obtaining research and export permissions in Madagascar; Gisele Bakara (CNRO) for providing assistance in sample collection; the French 'Affaires Maritimes' in Reunion and GIP 'Reserve Naturelle Marine de la Reunion' for delivering sampling permits in Reunion including protected areas; the 'Centre National de Recherches Oceanographiques' (CNRO), B. P. 68, Nosy-Be, Madagascar for providing infrastructure; the french 'Marine Nationale' and 'Forces armees de la zone Sud de l'ocean Indien (FAZSOI) for their logistic support and transport of materials; Christian Desgranges of the NGO 'Coup de pouce' and Herve Prigent for assistance in Nosy-Be. We wish to thank also Dirk Steinke and Robert Hanner (Biodiversity Institute of Ontario) for their support in the Barcode of Life data systems (BOLD); Joyce Gross and John Deck (Museum of Vertebrate Zoology, Berkeley) for their support in the Moorea Biocode database; Amy Driskell, Lee Weigt and Jeff Hunt (Laboratory of Analytical Biology, Smithsonian) for sequencing; Patrice Pruvost (Museum National d'Histoire Naturelle, Paris) for his supports with vouchers storage. NR 52 TC 50 Z9 54 U1 6 U2 58 PU PUBLIC LIBRARY SCIENCE PI SAN FRANCISCO PA 1160 BATTERY STREET, STE 100, SAN FRANCISCO, CA 94111 USA SN 1932-6203 J9 PLOS ONE JI PLoS One PD MAR 15 PY 2012 VL 7 IS 3 AR e28987 DI 10.1371/journal.pone.0028987 PG 8 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 932RU UT WOS:000303309000001 PM 22438862 ER PT J AU Vogt, PR Parrish, M AF Vogt, Peter R. Parrish, Mary TI Driftwood dropstones in Middle Miocene Climate Optimum shallow marine strata (Calvert Cliffs, Maryland Coastal Plain): Erratic pebbles no certain proxy for cold climate SO PALAEOGEOGRAPHY PALAEOCLIMATOLOGY PALAEOECOLOGY LA English DT Article DE Middle Miocene Climate Optimum; Ice-rafted detritus; Driftwood dropstones; Calvert Formation; Columbia River Flood Basalts; East Antarctic ice sheet expansion ID EOCENE THERMAL MAXIMUM; CARBON-DIOXIDE; FLOOD-BASALT; ORIGIN; ATLANTIC; EVOLUTION; SEQUENCES; VOLCANISM; MARGIN; SEA AB Sparse lithic erratics (pebbles to cobbles) sampled from three shallow marine strata deposited during the Middle Miocene Climate Optimum (MMCO, ca. 16-14 Ma) along the western Atlantic margin (exposed in the Calvert Cliffs, Maryland) suggest transport and deposition not from ice but from the roots of trees uprooted during floods and carried out to sea. Evidence for driftwood transport includes carbonized wood in the same strata. More than half the ca. 225 erratics were quarried in the largely metamorphic Piedmont province (including a few from the Port Deposit Gneiss, still outcropping on the lower Susquehanna River). The lowest sampled bed (Parker Creek Bone Bed) is assigned to the ca. 15.7-15.5 Ma peak warmth of the MMCO, which we attribute in part to CO2 from the coevally erupted Grande Ronde flood basalts (GRFB), the peak effusiveness episode of the Columbia River Flood Basalts (CRFB) The three sampled beds predate the ca. 13.9 Ma Antarctic cryosphere expansion, which may be recorded in the Calvert Cliffs by a unique buried channel. (c) 2012 Elsevier B.V. All rights reserved. C1 [Vogt, Peter R.] Univ Calif Santa Barbara, Inst Marine Sci, Santa Barbara, CA 93106 USA. [Vogt, Peter R.; Parrish, Mary] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA. RP Vogt, PR (reprint author), Univ Calif Santa Barbara, Inst Marine Sci, Santa Barbara, CA 93106 USA. EM ptr_vogt@yahoo.com NR 55 TC 5 Z9 5 U1 0 U2 13 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0031-0182 J9 PALAEOGEOGR PALAEOCL JI Paleogeogr. Paleoclimatol. Paleoecol. PD MAR 15 PY 2012 VL 323 BP 100 EP 109 DI 10.1016/j.palaeo.2012.01.035 PG 10 WC Geography, Physical; Geosciences, Multidisciplinary; Paleontology SC Physical Geography; Geology; Paleontology GA 922CI UT WOS:000302524000009 ER PT J AU Hatala, JA Detto, M Sonnentag, O Deverel, SJ Verfaillie, J Baldocchi, DD AF Hatala, Jaclyn A. Detto, Matteo Sonnentag, Oliver Deverel, Steven J. Verfaillie, Joseph Baldocchi, Dennis D. TI Greenhouse gas (CO2, CH4, H2O) fluxes from drained and flooded agricultural peatlands in the Sacramento-San Joaquin Delta SO AGRICULTURE ECOSYSTEMS & ENVIRONMENT LA English DT Article DE Carbon flux; Evaporation; Rice; Peatland; Eddy covariance; Evaporation ID EDDY COVARIANCE TECHNIQUE; NET ECOSYSTEM EXCHANGE; METHANE FLUXES; SEASONAL-VARIATION; CARBON-DIOXIDE; PADDY FIELD; RICE PADDY; ENERGY-BALANCE; ORGANIC SOILS; PEAT MEADOW AB The Sacramento-San Joaquin Delta in California was drained and converted to agriculture more than a century ago, and since then has experienced extreme rates of soil subsidence from peat oxidation. To reverse subsidence and capture carbon there is increasing interest in converting drained agricultural land-use types to flooded conditions. Rice agriculture is proposed as a flooded land-use type with CO2 sequestration potential for this region. We conducted two years of simultaneous eddy covariance measurements at a conventional drained and grazed degraded peatland and a newly converted rice paddy to evaluate the impact of drained to flooded land-use change on CO2, CH4, and evaporation fluxes. We found that the grazed degraded peatland emitted 175-299 g-C m(-2) yr(-1) as CO2 and 3.3 g-C m(-2) yr(-1) as CH4, while the rice paddy sequestered 84-283 g-C m(-2) yr(-1) of CO2 from the atmosphere and released 2.5-6.6 g-C m(-2) yr(-1) as CH4. The rice paddy evaporated 45-95% more water than the grazed degraded peatland. Annual photosynthesis was similar between sites, but flooding at the rice paddy inhibited ecosystem respiration, making it a net CO2 sink. The rice paddy had reduced rates of soil subsidence due to oxidation compared with the drained peatland, but did not completely reverse subsidence. (C) 2012 Elsevier B.V. All rights reserved. C1 [Hatala, Jaclyn A.; Detto, Matteo; Sonnentag, Oliver; Verfaillie, Joseph; Baldocchi, Dennis D.] Univ Calif 130, Ecosyst Sci Div, Dept Environm Sci Policy & Management, Berkeley, CA 94720 USA. [Detto, Matteo] Smithsonian Trop Res Inst, Panama City, Panama. [Sonnentag, Oliver] Univ Montreal, Dept Geog, Montreal, PQ H3C 3J7, Canada. [Deverel, Steven J.] Hydrofocus Inc, Davis, CA USA. RP Hatala, JA (reprint author), Univ Calif 130, Ecosyst Sci Div, Dept Environm Sci Policy & Management, Mulford Hall 3114, Berkeley, CA 94720 USA. EM jhatala@berkeley.edu RI Hatala, Jaclyn/K-6639-2012; Baldocchi, Dennis/A-1625-2009; OI Baldocchi, Dennis/0000-0003-3496-4919; Matthes, Jaclyn/0000-0001-8999-8062 FU National Science Foundation [AGS-0628720]; California Department of Water Resources [006550] FX The authors thank the Department of Water Resources of California for granting access to field sites. The authors extend many thanks to Brian Brock, Jim Casey, and the rest of the management team at Twitchell Island, and Juan Mercado and Walt at Sherman Island, the land managers without whom this work would not be possible. We also thank Alex Christensen, Marga Pretorius, and Sarah Price for assistance with laboratory work. Jaclyn Hatala thanks the National Science Foundation Graduate Fellowship Program for support during this research. This research was supported by National Science Foundation ATM grant number AGS-0628720 and the California Department of Water Resources grant #006550. NR 93 TC 59 Z9 60 U1 7 U2 124 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0167-8809 EI 1873-2305 J9 AGR ECOSYST ENVIRON JI Agric. Ecosyst. Environ. PD MAR 15 PY 2012 VL 150 BP 1 EP 18 DI 10.1016/j.agee.2012.01.009 PG 18 WC Agriculture, Multidisciplinary; Ecology; Environmental Sciences SC Agriculture; Environmental Sciences & Ecology GA 916MC UT WOS:000302106900001 ER PT J AU Hong, T AF Hong, Terry TI Flesh SO LIBRARY JOURNAL LA English DT Book Review C1 [Hong, Terry] Smithsonian BookDragon, Washington, DC USA. RP Hong, T (reprint author), Smithsonian BookDragon, Washington, DC USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU REED BUSINESS INFORMATION PI NEW YORK PA 360 PARK AVENUE SOUTH, NEW YORK, NY 10010 USA SN 0363-0277 J9 LIBR J JI Libr. J. PD MAR 15 PY 2012 VL 137 IS 5 BP 101 EP 102 PG 2 WC Information Science & Library Science SC Information Science & Library Science GA 911AY UT WOS:000301690900043 ER PT J AU Ma, SY Baldocchi, DD Hatala, JA Detto, M Yuste, JC AF Ma, Siyan Baldocchi, Dennis D. Hatala, Jaclyn A. Detto, Matteo Curiel Yuste, Jorge TI Are rain-induced ecosystem respiration pulses enhanced by legacies of antecedent photodegradation in semi-arid environments? SO AGRICULTURAL AND FOREST METEOROLOGY LA English DT Article DE Soil; Respiration; Ecosystem; Labile carbon pool; Mediterranean climate; Drought; Annual grassland; Peatland pasture ID PLANT LITTER DECOMPOSITION; CARBON-DIOXIDE EXCHANGE; SOIL CO2 EFFLUX; PRECIPITATION PULSES; ANNUAL GRASSLAND; ORGANIC-MATTER; TEMPERATURE; CALIFORNIA; FLUXES; MECHANISMS AB Ecosystem respiration (R-eco) is highly variable in semiarid ecosystems. After a period of drought, R-eco can jump to a high value in response to rain events, and afterward it decays exponentially with time. To better understand the timing, size, and duration of rain-induced respiration pulses, we examined 57 rain events from over 23 site-years of eddy covariance measurements at an open annual grassland, a woodland understory, and a peatland pasture in California, USA. To explain these findings, we conducted a factorial litter-watering experiment on grass and soil plots exposure to varying amounts of sunlight and water. To interpret and compare the population of rain-induced respiration pulses, we fitted the data with a two pool, 4-parameter exponential decay model. At the field scale, the total amounts of CO2 emission emanating from a single and sustained respiration pulse (mean+/-standard deviation) were 44.4+/-38.0, 24.2+/-17.8, and 94.6+/-45.8 gC m(-2) at the open grassland, the woodland understory, and the peatland pasture, respectively. The large variations in precipitation of these respiration-triggering rain events were associated with 73-84% of variation in the total amount of CO2 emission. Litter that experienced antecedent photodegradation tended to enhance respiration pulses. Biotic and abiotic processes involved in the dynamic of respiration pulses were pulse-specific, and we summarized them into two pulse scenarios. This study illustrates an emerging connection of ecosystem processes, and these findings may help to improve models on the dynamics of ecosystem CO2 cycling. Published by Elsevier B.V. C1 [Ma, Siyan; Baldocchi, Dennis D.; Hatala, Jaclyn A.] Univ Calif Berkeley, Dept Environm Sci Policy & Management, Ecosyst Sci Div, Berkeley, CA 94720 USA. [Detto, Matteo] Smithsonian Trop Res Inst, DPO, AA 34002 USA. [Curiel Yuste, Jorge] Univ Autonoma Barcelona, CREAF, Unitat Ecofisiol & Canvi Global CREAF CEAB CSIC, Bellaterra 08193, Barcelona, Spain. RP Ma, SY (reprint author), Univ Calif Berkeley, Dept Environm Sci Policy & Management, Ecosyst Sci Div, 130 Mulford Hall 3114, Berkeley, CA 94720 USA. EM syma@berkeley.edu RI Curiel Yuste, Jorge/A-6438-2011; Hatala, Jaclyn/K-6639-2012; Baldocchi, Dennis/A-1625-2009; OI Curiel Yuste, Jorge/0000-0002-3221-6960; Baldocchi, Dennis/0000-0003-3496-4919; Matthes, Jaclyn/0000-0001-8999-8062 FU Office of Science (BER), the U.S. Department of Energy [DE-FG02-03ER63638]; Western Regional Center of the National institute for Global Environmental Change [DE-FC02-03ER63613]; National Science Foundation [DEB-0317139]; Kearney Soil Science Foundation; California Agricultural Experiment Station FX This research was conducted at a site that is a member of the AmeriFlux and FLUXNET networks, and this research was supported in part by the Office of Science (BER), the U.S. Department of Energy (DE-FG02-03ER63638), and the Western Regional Center of the National institute for Global Environmental Change under Cooperative Agreement (DE-FC02-03ER63613). This study is also partially supported by the National Science Foundation (DEB-0317139), the Kearney Soil Science Foundation, and the California Agricultural Experiment Station. We gratefully thank Mr. Ted Hehn for his technical support. Thank you to Mr. Joe Verfaillie for his technical and editorial helps. Thank you to Dr. Laurie Koteen for her comments and editorial help. We appreciate Mr. Russell Tonzi and Mr. Fran Vaira for allowing us to access their ranch for scientific research. NR 38 TC 31 Z9 31 U1 1 U2 63 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0168-1923 J9 AGR FOREST METEOROL JI Agric. For. Meteorol. PD MAR 15 PY 2012 VL 154 BP 203 EP 213 DI 10.1016/j.agrformet.2011.11.007 PG 11 WC Agronomy; Forestry; Meteorology & Atmospheric Sciences SC Agriculture; Forestry; Meteorology & Atmospheric Sciences GA 900XB UT WOS:000300923900021 ER PT J AU Zhu, MQ Farrow, CL Post, JE Livi, KJT Billinge, SJL Ginder-Vogel, M Sparks, DL AF Zhu, Mengqiang Farrow, Christopher L. Post, Jeffrey E. Livi, Kenneth J. T. Billinge, Simon J. L. Ginder-Vogel, Matthew Sparks, Donald L. TI Structural study of biotic and abiotic poorly-crystalline manganese oxides using atomic pair distribution function analysis SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Article ID X-RAY-DIFFRACTION; BIOGENIC MN-OXIDES; NA-RICH BIRNESSITE; HEXAGONAL BIRNESSITE; EXAFS SPECTROSCOPY; PSEUDOMONAS-PUTIDA; LAYER STRUCTURE; HYDROUS OXIDES; HEAVY-METALS; MN(IV) OXIDE AB Manganese (Mn) oxides are among the most reactive natural minerals and play an important role in elemental cycling in oceanic and terrestrial environments. A large portion of naturally-occurring Mn oxides tend to be poorly-crystalline and/or nanocrystalline, with not fully resolved crystal structures. In this study, the crystal structures of their synthetic analogs including acid birnessite (AcidBir), delta-MnO2, polymeric MnO2 (PolyMnO(2)) and a bacteriogenic Mn oxide (BioMnO(x)), have been revealed using atomic pair distribution function (PDF) analysis. Results unambiguously verify that these Mn oxides are layered materials. The best models that accurately allow simulation of pair distribution functions (PDFs) belong to the monoclinic C12/m1 space group with a disk-like shape. The single MnO6 layers in the average structures deviate significantly from hexagonal symmetry, in contrast to the results of previous studies based on X-ray diffraction analysis in reciprocal space. Manganese occupancies in MnO6 layers are estimated to be 0.936, 0.847, 0.930 and 0.935, for AcidBir, BioMnO(x), delta-MnO2 and PolyMnO(2), respectively; however, occupancies of interlayer cations and water molecules cannot be accurately determined using the models in this study. The coherent scattering domains (CSDs) of PolyMnO(2), delta-MnO2 and BioMnO(x) are at the nanometer scale, comprising one to three MnO6 layers stacked with a high disorder in the crystallographic c-axis direction. Overall, the results of this study advance our understanding of the mineralogy of Mn oxide minerals in the environment. (C) 2011 Elsevier Ltd. All rights reserved. C1 [Zhu, Mengqiang; Ginder-Vogel, Matthew; Sparks, Donald L.] Univ Delaware, Dept Plant & Soil Sci, Newark, DE 19716 USA. [Zhu, Mengqiang; Ginder-Vogel, Matthew; Sparks, Donald L.] Univ Delaware, Delaware Environm Inst, Newark, DE 19716 USA. [Farrow, Christopher L.; Billinge, Simon J. L.] Columbia Univ, Dept Appl Phys & Appl Math, New York, NY 10027 USA. [Post, Jeffrey E.] Smithsonian Natl Museum Nat Hist, Washington, DC 20560 USA. [Livi, Kenneth J. T.] Johns Hopkins Univ, HRAEM IIC, Dept Biol, Baltimore, MD 21218 USA. [Livi, Kenneth J. T.] Johns Hopkins Univ, HRAEM IIC, Dept Earth & Planetary Sci, Baltimore, MD 21218 USA. [Billinge, Simon J. L.] Brookhaven Natl Lab, Condensed Matter Phys & Mat Sci Dept, Upton, NY 11973 USA. RP Zhu, MQ (reprint author), Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Div Earth Sci, 307 McCone Hall, Berkeley, CA 94720 USA. EM mzhu@lbl.gov RI Zhu, Mengqiang/G-6614-2011 OI Zhu, Mengqiang/0000-0001-7963-7167 FU U.S. Department of Energy, Office of Science, Office of Basic Energy Sciences [DEAC02-98CH10886, DEAC02-05CH11231]; National Science Foundation EPSCoR [EPS-0814251]; National Science Foundation EAR [0544246]; NSF [DMR-0703940] FX The authors would like to thank beamline scientists, Dr. Karena W. Chapman, Dr. Peter J. Chupas and Kevin A. Beyer at beamline 11-ID-B at the Advanced Photon Source (APS) and Dr. Jonathan Hanson, Dr. Laura Barrio-Pliego and Dr. Gong Zhang at beamline X7B at the National Synchrotron Light Source (NSLS) for their technical assistance with data collection and analyses. Use of the NSLS was supported by the U.S. Department of Energy, Office of Science, Office of Basic Energy Sciences, under Contract No. DEAC02-98CH10886. The Advanced Photon Source is supported by the Director, Office of Science, Office of Basic Energy Sciences, of the U.S. Department of Energy under Contract No. DEAC02-05CH11231. This publication was made possible by National Science Foundation EPSCoR Grant No. EPS-0814251 and the State of Delaware, and National Science Foundation EAR Grant No. 0544246. Work in the Billinge group was supported by NSF grant DMR-0703940. We are also grateful to Prof. Xionghan Feng at Huazhong Agricultural University, China, for providing the cryptomelane sample and helpful discussion on the Mn oxide syntheses. The authors also thank Prof. Alexandra Navrotsky at the University of California-Davis for her comments during the manuscript preparation. NR 71 TC 33 Z9 33 U1 6 U2 62 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0016-7037 J9 GEOCHIM COSMOCHIM AC JI Geochim. Cosmochim. Acta PD MAR 15 PY 2012 VL 81 BP 39 EP 55 DI 10.1016/j.gca.2011.12.006 PG 17 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 894TO UT WOS:000300450000004 ER PT J AU Hesketh, M Sanchez-Azofeifa, GA AF Hesketh, Michael Sanchez-Azofeifa, G. Arturo TI The effect of seasonal spectral variation on species classification in the Panamanian tropical forest SO REMOTE SENSING OF ENVIRONMENT LA English DT Article DE Leaf optical properties; Seasonality; Tropical dry forest; Panama; Spectra-temporal variability; Lianas; Leaf spectroscopy ID LEAF PIGMENT CONTENT; DRY FOREST; HYPERSPECTRAL DISCRIMINATION; REFLECTANCE; TREES; VEGETATION; CANOPY; LIANAS; VARIABILITY; PHENOLOGY AB Variation in the leaf optical properties imposed by variation in genetics and location has been addressed in recent literature, but those stemming from forest seasonality and phenology have been less well explored. Here, we explore the effect of inter-seasonal spectral variation on the potential for automated classification methods to accurately discern species of trees and lianas from high-resolution spectral data collected at the leaf level at two tropical forest sites. Through the application of a set of data reduction techniques and classification methods to leaf-level spectral data collected at both rainforest and seasonally dry sites in Panama, we found that in all cases the structure and organization of spectrally-derived taxonomies varied substantially between seasons. Using principle component analysis and a non-parametric classifier, we found at both sites that species-level classification was possible with a high level of accuracy within a given season. Classification across season was not, however, with accuracy dropping on average by a factor of 10. This study represents one of the first systematic investigations of leaf-level spectro-temporal variability, an appreciation for which is crucial to the advancement of species classification methods, with broad applications within the environmental sciences. (C) 2011 Elsevier Inc. All rights reserved. C1 [Hesketh, Michael; Sanchez-Azofeifa, G. Arturo] Univ Alberta, Ctr Earth Observat Sci CEOS, Edmonton, AB T6G 2E3, Canada. [Hesketh, Michael; Sanchez-Azofeifa, G. Arturo] Univ Alberta, Dept Earth & Atmospher Sci, Edmonton, AB T6G 2E3, Canada. [Sanchez-Azofeifa, G. Arturo] Smithsonian Trop Res Inst STRI, Panama City, Panama. RP Sanchez-Azofeifa, GA (reprint author), Univ Alberta, Ctr Earth Observat Sci CEOS, Edmonton, AB T6G 2E3, Canada. EM arturo.sanchez@ualberta.ca FU Canadian Natural Sciences and Engineering Research Council (NSERC); Inter-American Institute for Global Change Research (IAI) [021]; US National Science Foundation [GEO-0452325] FX We thank Margaret Kalacska and Gregory Asner for their comments and suggestions to early versions of this manuscript. We also thank Ms. Mirna Samarniego for her assistance during the collection of the field data at the Panama canopy cranes. This work was supported by a Discovery Grant from the Canadian Natural Sciences and Engineering Research Council (NSERC), and by a grant from the Inter-American Institute for Global Change Research (IAI) CRN II # 021 which is supported by the US National Science Foundation (Grant GEO-0452325). NR 47 TC 18 Z9 18 U1 0 U2 41 PU ELSEVIER SCIENCE INC PI NEW YORK PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA SN 0034-4257 J9 REMOTE SENS ENVIRON JI Remote Sens. Environ. PD MAR 15 PY 2012 VL 118 BP 73 EP 82 DI 10.1016/j.rse.2011.11.005 PG 10 WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic Technology SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science & Photographic Technology GA 895SW UT WOS:000300517700007 ER PT J AU Bak, J Kim, JH Spurr, RJD Liu, X Newchurch, MJ AF Bak, Juseon Kim, Jae H. Spurr, R. J. D. Liu, X. Newchurch, M. J. TI Sensitivity study of ozone retrieval from UV measurements on geostationary platforms SO REMOTE SENSING OF ENVIRONMENT LA English DT Article DE GEMS; Geostationary orbit; Geosynchronous orbit; Solar zenith angle; Satellite zenith angle; The sensitivity of ozone retrievals; Combination of multiple UV measurements ID MONITORING-EXPERIMENT GOME; TROPOSPHERIC COLUMN OZONE; MAPPING SPECTROMETER; RAMAN-SCATTERING; CLOUD PRESSURE; PROFILE RETRIEVALS; RESOLUTION; TROPICS AB This paper addresses several aspects related to ultraviolet (UV) measurements from art upcoming geostationary orbit (CEO) satellite mission. First, using simulated cloud coverage based on the MTSAT (Multi-functional Transport Satellite 1R) 650 nm channel as a proxy, we find that CEO observations can increase clear-sky coverage by similar to 4 times. Secondly, we examine the feasibility of improved ozone detection with CEO observations, using synthetic GEMS spectra with CEO geometries along with the TOMS total ozone algorithm and an ozone profile algorithm based on the optimal estimation method. The sensitivity of ozone retrievals to the lower troposphere is limited at large solar and satellite zenith angles, especially above 70 under clear-sky conditions. Third, we evaluate two new ideas for improving ozone retrieval sensitivity in the troposphere at large angle geometries: (1) a geosynchronous orbit with an inclination-angle of 30 degrees, with smaller values of viewing zenith angles than those from a geostationary orbit: (2) a combination of UV measurements at multiple solar zenith angles to improve the accuracy of ozone profile retrievals. (C) 2011 Elsevier Inc. All rights reserved. C1 [Bak, Juseon; Kim, Jae H.] Pusan Natl Univ, Dept Atmospher Sci, Pusan 609735, South Korea. [Liu, X.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA USA. [Newchurch, M. J.] Univ Alabama, Dept Atmospher Sci, Huntsville, AL USA. RP Kim, JH (reprint author), Pusan Natl Univ, Dept Atmospher Sci, Pusan 609735, South Korea. EM jaekim@pusan.ac.kr RI Liu, Xiong/P-7186-2014 OI Liu, Xiong/0000-0003-2939-574X FU National Institute of Environmental Research (NIER) of Korea [1600-1637-303-210-13]; Korean Meteorological Administration [RACS 2010-1011] FX This work was supported by the National Institute of Environmental Research (NIER) of Korea (Grant No. 1600-1637-303-210-13) and the Korean Meteorological Administration (RACS 2010-1011). NR 49 TC 4 Z9 4 U1 0 U2 8 PU ELSEVIER SCIENCE INC PI NEW YORK PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA SN 0034-4257 J9 REMOTE SENS ENVIRON JI Remote Sens. Environ. PD MAR 15 PY 2012 VL 118 BP 309 EP 319 DI 10.1016/j.rse.2011.11.010 PG 11 WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic Technology SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science & Photographic Technology GA 895SW UT WOS:000300517700027 ER PT J AU Tang, LY Yan, ZC Shi, TY Babb, JF Mitroy, J AF Tang, Li-Yan Yan, Zong-Chao Shi, Ting-Yun Babb, James F. Mitroy, J. TI The long-range non-additive three-body dispersion interactions for the rare gases, alkali, and alkaline-earth atoms SO JOURNAL OF CHEMICAL PHYSICS LA English DT Article ID DIPOLE OSCILLATOR-STRENGTHS; DER-WAALS COEFFICIENTS; MANY-BODY CALCULATIONS; VANDERWAALS INTERACTIONS; METAL ATOMS; INTERMOLECULAR FORCES; SECONDARY SATELLITES; HYDROGEN-ATOMS; ENERGY; VAN AB The long-range non-additive three-body dispersion interaction coefficients Z(111), Z(112), Z(113), and Z(122) are computed for many atomic combinations using standard expressions. The atoms considered include hydrogen, the rare gases, the alkali atoms (up to Rb), and the alkaline-earth atoms (up to Sr). The term Z(111) arising from three mutual dipole interactions is known as the Axilrod-Teller-Muto coefficient or the DDD (dipole-dipole-dipole) coefficient. Similarly, the terms Z(112), Z(113), and Z(122) arise from the mutual combinations of dipole (1), quadrupole (2), and octupole (3) interactions between atoms and they are sometimes known, respectively, as dipole-dipole-quadrupole, dipole-dipole-octupole, and dipole-quadrupole-quadrupole coefficients. Results for the four Z coefficients are given for the homonuclear trimers, for the trimers involving two like-rare-gas atoms, and for the trimers with all combinations of the H, He, and Li atoms. An exhaustive compilation of all coefficients between all possible atomic combinations is presented as supplementary data. (C) 2012 American Institute of Physics. [http://dx.doi.org/10.1063/1.3691891] C1 [Tang, Li-Yan; Shi, Ting-Yun] Chinese Acad Sci, Wuhan Inst Phys & Math, State Key Lab Magnet Resonance & Atom & Mol Phys, Wuhan 430071, Peoples R China. [Yan, Zong-Chao] Chinese Acad Sci, Ctr Cold Atom Phys, Wuhan 430071, Peoples R China. [Yan, Zong-Chao] Univ New Brunswick, Dept Phys, Fredericton, NB E3B 5A3, Canada. [Babb, James F.] Harvard Smithsonian Ctr Astrophys, ITAMP, Cambridge, MA 02138 USA. [Mitroy, J.] Charles Darwin Univ, Sch Engn, Darwin, NT 0909, Australia. RP Tang, LY (reprint author), Chinese Acad Sci, Wuhan Inst Phys & Math, State Key Lab Magnet Resonance & Atom & Mol Phys, Wuhan 430071, Peoples R China. EM ly-tang@wipm.ac.cn RI Shi, Tingyun/I-6022-2013; Mitroy, James/N-2162-2013; Yan, Zong-Chao/F-6668-2014; OI Mitroy, James/0000-0002-2477-1251; Babb, James/0000-0002-3883-9501 FU National Natural Science Foundation (NNSF) of China [11104323, 11034009]; National Basic Research Program of China [2012CB821305]; NSERC of Canada; Australian Research Council [DP-1092620]; US National Science Foundation (NSF); Smithsonian Astrophysical Observatory FX This work was supported by the National Natural Science Foundation (NNSF) of China under Grant Nos. 11104323 and 11034009, and by the National Basic Research Program of China under Grant No. 2012CB821305. Z.-C.Y. was supported by NSERC of Canada and by the computing facilities of ACEnet, SHARCnet, WestGrid, and in part by the Chinese Academy of Sciences (CAS)/SAFEA International Partnership Program for Creative Research Teams. J.M. would like to thank the Wuhan Institute of Physics and Mathematics for its hospitality during his visits. The work of J.M was supported in part by the Australian Research Council Discovery Project DP-1092620. ITAMP is partially supported by a grant from the US National Science Foundation (NSF) to Harvard University and the Smithsonian Astrophysical Observatory. NR 58 TC 10 Z9 10 U1 3 U2 12 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 MAR 14 PY 2012 VL 136 IS 10 AR 104104 DI 10.1063/1.3691891 PG 8 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA 910TF UT WOS:000301664600005 PM 22423825 ER PT J AU Schwadron, NA Baker, T Blake, B Case, AW Cooper, JF Golightly, M Jordan, A Joyce, C Kasper, J Kozarev, K Mislinski, J Mazur, J Posner, A Rother, O Smith, S Spence, HE Townsend, LW Wilson, J Zeitlin, C AF Schwadron, N. A. Baker, T. Blake, B. Case, A. W. Cooper, J. F. Golightly, M. Jordan, A. Joyce, C. Kasper, J. Kozarev, K. Mislinski, J. Mazur, J. Posner, A. Rother, O. Smith, S. Spence, H. E. Townsend, L. W. Wilson, J. Zeitlin, C. TI Lunar radiation environment and space weathering from the Cosmic Ray Telescope for the Effects of Radiation (CRaTER) SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article ID INFRARED MAPPING SPECTROMETER; ICY GALILEAN SATELLITES; HYDRATED SALT MINERALS; MAGNETIC-FLUX; PROTON IRRADIATION; EUROPAS SURFACE; SULFURIC-ACID; SOLAR-SYSTEM; KUIPER-BELT; MODULATION AB The Cosmic Ray Telescope for the Effects of Radiation (CRaTER) measures linear energy transfer by Galactic Cosmic Rays (GCRs) and Solar Energetic Particles (SEPs) on the Lunar Reconnaissance Orbiter (LRO) Mission in a circular, polar lunar orbit. GCR fluxes remain at the highest levels ever observed during the space age. One of the largest SEP events observed by CRaTER during the LRO mission occurred on June 7, 2011. We compare model predictions by the Earth-Moon-Mars Radiation Environment Module (EMMREM) for both dose rates from GCRs and SEPs during this event with results from CRaTER. We find agreement between these models and the CRaTER dose rates, which together demonstrate the accuracy of EMMREM, and its suitability for a real-time space weather system. We utilize CRaTER to test forecasts made by the Relativistic Electron Alert System for Exploration (REleASE), which successfully predicts the June 7th event. At the maximum CRaTER-observed GCR dose rate (similar to 11.7 cGy/yr where Gy is a unit indicating energy deposition per unit mass, 1 Gy = 1 J/kg), GCRs deposit similar to 88 eV/molecule in water over 4 billion years, causing significant change in molecular composition and physical structure (e. g., density, color, crystallinity) of water ice, loss of molecular hydrogen, and production of more complex molecules linking carbon and other elements in the irradiated ice. This shows that space weathering by GCRs may be extremely important for chemical evolution of ice on the Moon. Thus, we show comprehensive observations from the CRaTER instrument on the Lunar Reconnaissance Orbiter that characterizes the radiation environment and space weathering on the Moon. C1 [Schwadron, N. A.; Baker, T.; Golightly, M.; Jordan, A.; Joyce, C.; Mislinski, J.; Smith, S.; Spence, H. E.; Wilson, J.] Univ New Hampshire, EOS Space Sci Ctr, Durham, NH 03824 USA. [Blake, B.] Aerosp Corp, Dept Space Sci, Los Angeles, CA 90245 USA. [Case, A. W.; Kasper, J.; Kozarev, K.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Cooper, J. F.] NASA, Goddard Space Flight Ctr, Heliospher Phys Lab, Greenbelt, MD 20771 USA. [Kozarev, K.] Boston Univ, Dept Astron, Boston, MA 02215 USA. [Mazur, J.] Aerosp Corp, Dept Space Sci, Chantilly, VA 20151 USA. [Posner, A.] NASA Headquarters, Washington, DC 20546 USA. [Rother, O.] Univ Kiel, Inst Expt & Angew Phys, D-24118 Kiel, Germany. [Townsend, L. W.] Univ Tennessee, Dept Nucl Engn, Knoxville, TN 37996 USA. [Zeitlin, C.] SW Res Inst, Space Sci & Engn Div, Boulder, CO 80302 USA. [Schwadron, N. A.; Baker, T.; Golightly, M.; Jordan, A.; Mislinski, J.; Smith, S.; Spence, H. E.; Wilson, J.] Univ New Hampshire, Inst Study Earth Oceans & Space, Durham, NH 03824 USA. [Rother, O.] Sci Data Proc, Kiel, Germany. RP Schwadron, NA (reprint author), Univ New Hampshire, EOS Space Sci Ctr, 8 Coll Rd, Durham, NH 03824 USA. EM n.schwadron@unh.edu RI Cooper, John/D-4709-2012; Spence, Harlan/A-1942-2011; Kasper, Justin/D-1152-2010; OI Kasper, Justin/0000-0002-7077-930X; Spence, Harlan/0000-0002-2526-2205 FU NASA CRaTER [NNG11PA03C]; EMMREM; NASA FX This work is supported by the NASA CRaTER contract NNG11PA03C and the EMMREM project, and for J.F.C. by the NASA Lunar Advanced Science and Exploration Research and Outer Planets Research programs. NR 73 TC 27 Z9 27 U1 3 U2 22 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9097 EI 2169-9100 J9 J GEOPHYS RES-PLANET JI J. Geophys. Res.-Planets PD MAR 13 PY 2012 VL 117 AR E00H13 DI 10.1029/2011JE003978 PG 13 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 910VU UT WOS:000301672200001 ER PT J AU Evans, AR Jones, D Boyer, AG Brown, JH Costa, DP Ernest, SKM Fitzgerald, EMG Fortelius, M Gittleman, JL Hamilton, MJ Harding, LE Lintulaakso, K Lyons, SK Okie, JG Saarinen, JJ Sibly, RM Smith, FA Stephens, PR Theodor, JM Uhen, MD AF Evans, Alistair R. Jones, David Boyer, Alison G. Brown, James H. Costa, Daniel P. Ernest, S. K. Morgan Fitzgerald, Erich M. G. Fortelius, Mikael Gittleman, John L. Hamilton, Marcus J. Harding, Larisa E. Lintulaakso, Kari Lyons, S. Kathleen Okie, Jordan G. Saarinen, Juha J. Sibly, Richard M. Smith, Felisa A. Stephens, Patrick R. Theodor, Jessica M. Uhen, Mark D. TI The maximum rate of mammal evolution SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA LA English DT Article DE haldanes; biological time; scaling; pedomorphosis ID BODY-SIZE; COPES RULE; SELECTION; LINEAGES; STASIS; TIME AB How fast can a mammal evolve from the size of a mouse to the size of an elephant? Achieving such a large transformation calls for major biological reorganization. Thus, the speed at which this occurs has important implications for extensive faunal changes, including adaptive radiations and recovery from mass extinctions. To quantify the pace of large-scale evolution we developed a metric, clade maximum rate, which represents the maximum evolutionary rate of a trait within a clade. We applied this metric to body mass evolution in mammals over the last 70 million years, during which multiple large evolutionary transitions occurred in oceans and on continents and islands. Our computations suggest that it took a minimum of 1.6, 5.1, and 10 million generations for terrestrial mammal mass to increase 100-, and 1,000-, and 5,000-fold, respectively. Values for whales were down to half the length (i.e., 1.1, 3, and 5 million generations), perhaps due to the reduced mechanical constraints of living in an aquatic environment. When differences in generation time are considered, we find an exponential increase in maximum mammal body mass during the 35 million years following the Cretaceous-Paleogene (K-Pg) extinction event. Our results also indicate a basic asymmetry in macroevolution: very large decreases (such as extreme insular dwarfism) can happen at more than 10 times the rate of increases. Our findings allow more rigorous comparisons of microevolutionary and macroevolutionary patterns and processes. C1 [Evans, Alistair R.; Jones, David] Monash Univ, Sch Biol Sci, Clayton, Vic 3800, Australia. [Jones, David] Univ Bristol, Sch Earth Sci, Bristol BS8 1RJ, Avon, England. [Boyer, Alison G.] Univ Tennessee, Dept Ecol & Evolutionary Biol, Knoxville, TN 37996 USA. [Brown, James H.; Hamilton, Marcus J.; Okie, Jordan G.; Smith, Felisa A.] Univ New Mexico, Dept Biol, Albuquerque, NM 87131 USA. [Brown, James H.; Hamilton, Marcus J.] Santa Fe Inst, Santa Fe, NM 87501 USA. [Costa, Daniel P.] Univ Calif Santa Cruz, Dept Ecol & Evolutionary Biol, Santa Cruz, CA 95060 USA. [Ernest, S. K. Morgan] Utah State Univ, Dept Biol, Logan, UT 84322 USA. [Ernest, S. K. Morgan] Utah State Univ, Ctr Ecol, Logan, UT 84322 USA. [Fitzgerald, Erich M. G.] Museum Victoria, Melbourne, Vic 3001, Australia. [Fortelius, Mikael] Univ Helsinki, Finnish Museum Nat Hist, FIN-00014 Helsinki, Finland. [Fortelius, Mikael] Univ Helsinki, Dept Geosci & Geog, FIN-00014 Helsinki, Finland. [Gittleman, John L.; Stephens, Patrick R.] Univ Georgia, Odum Sch Ecol, Athens, GA 30602 USA. [Hamilton, Marcus J.] Univ New Mexico, Dept Anthropol, Albuquerque, NM 87131 USA. [Harding, Larisa E.; Lintulaakso, Kari; Saarinen, Juha J.] Umea Univ, Dept Ecol & Environm Sci, SE-90187 Umea, Sweden. [Lyons, S. Kathleen] Smithsonian Inst, Washington, DC 20013 USA. [Okie, Jordan G.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA. [Sibly, Richard M.] Univ Reading, Sch Biol Sci, Reading RG6 6AH, Berks, England. [Theodor, Jessica M.] Univ Calgary, Dept Biol Sci, Calgary, AB T2N 1N4, Canada. [Uhen, Mark D.] George Mason Univ, Dept Atmospher Ocean & Earth Sci, Fairfax, VA 22030 USA. RP Evans, AR (reprint author), Monash Univ, Sch Biol Sci, Clayton, Vic 3800, Australia. EM arevans@fastmail.fm; jhbrown@unm.edu RI Evans, Alistair/D-4239-2011; Ernest, SK Morgan/O-2532-2015; OI Evans, Alistair/0000-0002-4078-4693; Ernest, SK Morgan/0000-0002-6026-8530; Sibly, Richard/0000-0001-6828-3543; Lintulaakso, Kari/0000-0001-9627-8821; Fortelius, Mikael/0000-0002-4851-783X FU Australian Research Council; Monash University; National Science Foundation [DEB 0541625]; European Union [PIOF-GA-2009-235868]; Harold Mitchell Foundation FX We thank G. Evans, M. Burd, D. Dowling, Evolutionary Biology at Monash, P. Smits, G. Sanson, J. Jernvall, F. Whiteman, M. Balk, B. Van Valkenburgh, J. Damuth, A. Lister, and P. D. Polly for discussions and comments on earlier manuscripts. This study was supported by an Australian Research Council Australian Research Fellowship (to A.R.E.), Monash University Monash Research Fellowship (to A.R.E.), National Science Foundation Grant Integrating Macroecological Pattern and Processes across Scales Research Coordination Network (IMPPS RCN) DEB 0541625 (to F.A.S., S.K.L., and S.K.M.E., principal investigators), European Union Marie Curie Grant PIOF-GA-2009-235868 (to D.J.), and a Harold Mitchell Foundation Harold Mitchell Fellowship (to E.M.G.F.). This paper is IMPPS RCN publication no. 18. NR 29 TC 37 Z9 38 U1 2 U2 84 PU NATL ACAD SCIENCES PI WASHINGTON PA 2101 CONSTITUTION AVE NW, WASHINGTON, DC 20418 USA SN 0027-8424 J9 P NATL ACAD SCI USA JI Proc. Natl. Acad. Sci. U. S. A. PD MAR 13 PY 2012 VL 109 IS 11 BP 4187 EP 4190 DI 10.1073/pnas.1120774109 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 907OH UT WOS:000301426700037 PM 22308461 ER PT J AU Engel, MC Heinke, CO Sivakoff, GR Elshamouty, KG Edmonds, PD AF Engel, M. C. Heinke, C. O. Sivakoff, G. R. Elshamouty, K. G. Edmonds, P. D. TI A 2.15 hr ORBITAL PERIOD FOR THE LOW-MASS X-RAY BINARY XB 1832-330 IN THE GLOBULAR CLUSTER NGC 6652 SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; globular clusters: individual (NGC 6652); stars: neutron; X-rays: binaries ID IMAGE SUBTRACTION; OPTICAL COUNTERPART; ELLIPTIC GALAXIES; TIME-SERIES; SPACED DATA; FIELD; NGC-6652; CHANDRA; VARIABILITY; PHOTOMETRY AB We present a candidate orbital period for the low-mass X-ray binary (LMXB) XB 1832-330 in the globular cluster NGC 6652 using a 6.5 hr Gemini South observation of the optical counterpart of the system. Light curves in g' and r' for two LMXBs in the cluster, sources A and B in previous literature, were extracted and analyzed for periodicity using the ISIS image subtraction package. A clear sinusoidal modulation is evident in both of A's curves, of amplitude similar to 0.11 mag in g' and similar to 0.065 mag in r', while B's curves exhibit rapid flickering, of amplitude similar to 1 mag in g' and similar to 0.5 mag in r'. A Lomb-Scargle test revealed a 2.15 hr periodic variation in the magnitude of A with a false alarm probability less than 10(-11), and no significant periodicity in the light curve for B. Though it is possible that saturated stars in the vicinity of our sources partially contaminated our signal, the identification of A's binary period is nonetheless robust. C1 [Engel, M. C.; Heinke, C. O.; Sivakoff, G. R.; Elshamouty, K. G.] Univ Alberta, Dept Phys, Edmonton, AB T6G 2E1, Canada. [Edmonds, P. D.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Engel, MC (reprint author), Univ Alberta, Dept Phys, 4-183 CCIS, Edmonton, AB T6G 2E1, Canada. EM mcengel@ualberta.ca; heinke@ualberta.ca RI Sivakoff, Gregory/G-9602-2011; OI Sivakoff, Gregory/0000-0001-6682-916X; Heinke, Craig/0000-0003-3944-6109 FU NSERC; Alberta Ingenuity New Faculty FX We acknowledge support by NSERC and an Alberta Ingenuity New Faculty Award, and useful conversations with C. Deloye. These results are based on observations obtained at the Gemini South Observatory (Proposal ID GN-2011A-Q-20). The Gemini Observatory is operated by the Association of Universities for Research in Astronomy, Inc., under a cooperative agreement with the NSF on behalf of the Gemini partnership: the National Science Foundation (United States), the Science and Technology Facilities Council (United Kingdom), the National Research Council (Canada), CONICYT (Chile), the Australian Research Council (Australia), CNPq (Brazil), and CONICET (Argentina). We thank R. Wijnands for drawing our attention to the decline in the bulge scan light curve of NGC 6652. NR 44 TC 7 Z9 7 U1 0 U2 6 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAR 10 PY 2012 VL 747 IS 2 AR 119 DI 10.1088/0004-637X/747/2/119 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 926UC UT WOS:000302856400035 ER PT J AU Espaillat, C Ingleby, L Hernandez, J Furlan, E D'Alessio, P Calvet, N Andrews, S Muzerolle, J Qi, C Wilner, D AF Espaillat, C. Ingleby, L. Hernandez, J. Furlan, E. D'Alessio, P. Calvet, N. Andrews, S. Muzerolle, J. Qi, C. Wilner, D. TI ON THE TRANSITIONAL DISK CLASS: LINKING OBSERVATIONS OF T TAURI STARS AND PHYSICAL DISK MODELS SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; circumstellar matter; protoplanetary disks; stars: formation; stars: pre-main sequence ID SPITZER-SPACE-TELESCOPE; LOW-MASS STARS; ORION OB1 ASSOCIATION; MAIN-SEQUENCE STARS; PROTOPLANETARY DISKS; INFRARED SPECTROGRAPH; CIRCUMSTELLAR DISKS; ACCRETION DISKS; YOUNG OBJECTS; PRETRANSITIONAL DISKS AB Two decades ago "transitional disks" (TDs) described spectral energy distributions (SEDs) of T Tauri stars with small near-IR excesses, but significant mid-and far-IR excesses. Many inferred this indicated dust-free holes in disks possibly cleared by planets. Recently, this term has been applied disparately to objects whose Spitzer SEDs diverge from the expectations for a typical full disk (FD). Here, we use irradiated accretion disk models to fit the SEDs of 15 such disks in NGC 2068 and IC 348. One group has a "dip" in infrared emission while the others' continuum emission decreases steadily at all wavelengths. We find that the former have an inner disk hole or gap at intermediate radii in the disk and we call these objects "transitional disks" and "pre-transitional disks" (PTDs), respectively. For the latter group, we can fit these SEDs with FD models and find that millimeter data are necessary to break the degeneracy between dust settling and disk mass. We suggest that the term "transitional" only be applied to objects that display evidence for a radical change in the disk's radial structure. Using this definition, we find that TDs and PTDs tend to have lower mass accretion rates than FDs and that TDs have lower accretion rates than PTDs. These reduced accretion rates onto the star could be linked to forming planets. Future observations of TDs and PTDs will allow us to better quantify the signatures of planet formation in young disks. C1 [Espaillat, C.; Andrews, S.; Qi, C.; Wilner, D.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Ingleby, L.; Calvet, N.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Hernandez, J.] Ctr Invest Astron CIDA, Merida 5101A, Venezuela. [Furlan, E.] Natl Opt Astron Observ, Tucson, AZ 85719 USA. [D'Alessio, P.] Univ Nacl Autonoma Mexico, Ctr Radioastron & Astrofis, Morelia 58089, Michoacan, Mexico. [Muzerolle, J.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. RP Espaillat, C (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS-78, Cambridge, MA 02138 USA. EM cespaillat@cfa.harvard.edu; lingleby@umich.edu; jesush@cida.ve; Elise.Furlan@jpl.nasa.gov; p.dalessio@crya.unam.mx; ncalvet@umich.edu; sandrews@cfa.harvard.edu; muzerol@stsci.edu; cqi@cfa.harvard.edu; dwilner@cfa.harvard.edu OI Furlan, Elise/0000-0001-9800-6248 FU National Science Foundation [0901947]; PAPIIT-DGAPA UNAM; NASA [NNX08AFM 5154G] FX We thank Lee Hartmann for helpful discussions and the referee for a careful review of the manuscript. C. E. was supported by the National Science Foundation under Award No. 0901947. P. D. acknowledges a grant from PAPIIT-DGAPA UNAM. N.C. acknowledges support from NASA Origins Grant NNX08AFM 5154G. NR 113 TC 62 Z9 62 U1 0 U2 6 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAR 10 PY 2012 VL 747 IS 2 AR 103 DI 10.1088/0004-637X/747/2/103 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 926UC UT WOS:000302856400019 ER PT J AU Hsieh, PY Ho, PTP Kohno, K Hwang, CY Matsushita, S AF Hsieh, Pei-Ying Ho, Paul T. P. Kohno, Kotaro Hwang, Chorng-Yuan Matsushita, Satoki TI PROBING CIRCUMNUCLEAR ENVIRONMENTS WITH THE HCN(J=3-2) AND HCO+(J=3-2) LINES: CASE OF NGC 1097 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: individual (NGC 1097); galaxies: ISM; galaxies: Seyfert; ISM: molecules; radio lines: ISM; submillimeter: ISM ID MOLECULAR GAS; ACTIVE GALAXIES; NEARBY GALAXIES; DENSE GAS; INFRARED GALAXIES; CENTRAL REGION; STARBURST; NGC-1097; NUCLEUS; HCN AB We present the first interferometric HCN(J = 3-2) and HCO+(J = 3-2) maps in the circumnuclear region of NGC 1097, obtained with the Submillimeter Array. The goal is to study the characteristics of the dense gas associated with the starburst ring/Seyfert nucleus. With these transitions, we suppress the diffuse low density emission in the nuclear region. We detect and resolve the individual compact giant molecular cloud associations (GMAs) in the 1.4 kpc circumnuclear starburst ring and within the 350 pc nuclear region. The nucleus is brighter than the ring in both lines, and contributes similar to 20% and similar to 30% to the total detected HCO+(J = 3-2) and HCN(J = 3-2) flux, within the central 1.4 kpc. The intensity ratios of HCN(J = 3-2)/HCO+(J = 3-2) are roughly unity in the GMAs of the starburst ring. However, this ratio is up to similar to 2 in the nuclear region. From the HCN(J= 3-2)/HCN(J= 1-0) ratio of <= 0.2 in the nucleus, we infer that the nuclear HCN(J = 3-2) emission might be optically thin. The HCO+(J = 3-2) and HCN(J = 3-2) show correlations with (CO)-C-12(J = 3-2) and the 24 mu m emission. The tight correlations of HCN(J = 3-2), HCO+(J = 3-2), and 24 mu m emission in the starburst ring suggest that the dense molecular gas and the dust are from the same origins of star-forming regions. On the other hand, the HCN(J = 3-2) emission of the nucleus is significantly enhanced, indicating mechanisms other than star formation, such as active galactic nucleus activities. A self-consistent check of the fractional abundance enhanced by X-ray ionization chemistry of the nucleus is possible with our observations. C1 [Hsieh, Pei-Ying; Ho, Paul T. P.; Matsushita, Satoki] Acad Sinica, Inst Astron & Astrophys, Taipei 10617, Taiwan. [Hsieh, Pei-Ying; Hwang, Chorng-Yuan] Natl Cent Univ, Inst Astron, Jhongli 32001, Taoyuan County, Taiwan. [Ho, Paul T. P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Kohno, Kotaro] Univ Tokyo, Inst Astron, Mitaka, Tokyo 1810015, Japan. [Kohno, Kotaro] Univ Tokyo, Res Ctr Early Universe, Bunkyo Ku, Tokyo 1130033, Japan. [Matsushita, Satoki] Joint ALMA Off, Santiago 7630355, Chile. RP Hsieh, PY (reprint author), Acad Sinica, Inst Astron & Astrophys, POB 23-141, Taipei 10617, Taiwan. EM pyhsieh@asiaa.sinica.edu.tw FU NSC [100-2119-M-008-011-MY3, NSC 99-2112-M-008-014-MY3, NSC-97-2112-M-001-007-MY3, NSC 100-2112-M-001-006-MY3] FX We thank for the SMA staffs for the SMA operations for this project. We acknowledge the anonymous referee for stimulating comments to improve the manuscript. P.-Y. Hsieh acknowledges Dr. Tatsuhiko Hasegawa to complete this project. This project is funded by NSC 100-2119-M-008-011-MY3, NSC 99-2112-M-008-014-MY3, NSC-97-2112-M-001-007-MY3, and NSC 100-2112-M-001-006-MY3. NR 45 TC 11 Z9 11 U1 0 U2 7 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAR 10 PY 2012 VL 747 IS 2 AR 90 DI 10.1088/0004-637X/747/2/90 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 926UC UT WOS:000302856400006 ER PT J AU Kim, DW Protopapas, P Trichas, M Rowan-Robinson, M Khardon, R Alcock, C Byun, YI AF Kim, Dae-Won Protopapas, Pavlos Trichas, Markos Rowan-Robinson, Michael Khardon, Roni Alcock, Charles Byun, Yong-Ik TI A REFINED QSO SELECTION METHOD USING DIAGNOSTICS TESTS: 663 QSO CANDIDATES IN THE LARGE MAGELLANIC CLOUD SO ASTROPHYSICAL JOURNAL LA English DT Article DE Magellanic Clouds; methods: data analysis; quasars: general ID ACTIVE GALACTIC NUCLEI; DIGITAL SKY SURVEY; ENERGY-DISTRIBUTIONS; TIME VARIABILITY; SOURCE CATALOG; QUASARS; STARBURSTS; DISCOVERY; GALAXIES; MODELS AB We present 663 QSO candidates in the Large Magellanic Cloud (LMC) selected using multiple diagnostics. We started with a set of 2566 QSO candidates selected using the methodology presented in our previous work based on time variability of the MACHO LMC light curves. We then obtained additional information for the candidates by crossmatching them with the Spitzer SAGE, the Two Micron All Sky Survey, the Chandra, the XMM, and an LMC UBVI catalog. Using this information, we specified six diagnostic features based on mid-IR colors, photometric redshifts using spectral energy distribution template fitting, and X-ray luminosities in order to further discriminate high-confidence QSO candidates in the absence of spectra information. We then trained a one-class Support Vector Machine model using the diagnostics features of the confirmed 58 MACHO QSOs. We applied the trained model to the original candidates and finally selected 663 high-confidence QSO candidates. Furthermore, we crossmatched these 663 QSO candidates with the newly confirmed 151 QSOs and 275 non-QSOs in the LMC fields. On the basis of the counterpart analysis, we found that the false positive rate is less than 1%. C1 [Kim, Dae-Won; Protopapas, Pavlos; Trichas, Markos; Alcock, Charles] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Kim, Dae-Won; Byun, Yong-Ik] Yonsei Univ, Dept Astron, Seoul 120749, South Korea. [Kim, Dae-Won; Protopapas, Pavlos] Harvard Univ, Inst Appl Computat Sci, Cambridge, MA 02138 USA. [Rowan-Robinson, Michael] Univ London Imperial Coll Sci Technol & Med, Astrophys Grp, London, England. [Khardon, Roni] Tufts Univ, Dept Comp Sci, Medford, MA 02155 USA. [Byun, Yong-Ik] Yonsei Univ, Yonsei Univ Observ, Seoul 120749, South Korea. RP Kim, DW (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. FU FAS Research Computing Group at Harvard; NSF [IIS-0803409] FX We thank L. Mylonadis for helpful comments. The analysis in this paper has been done using the Odyssey cluster supported by the FAS Research Computing Group at Harvard. This work has been supported by NSF grant IIS-0803409. This research has made use of the SIMBAD database, operated at CDS, Strasbourg, France. NR 46 TC 16 Z9 16 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAR 10 PY 2012 VL 747 IS 2 AR 107 DI 10.1088/0004-637X/747/2/107 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 926UC UT WOS:000302856400023 ER PT J AU Matranga, M Drake, JJ Kashyap, V Steeghs, D AF Matranga, Marco Drake, Jeremy J. Kashyap, Vinay Steeghs, Danny TI DETECTION OF ACCRETION X-RAYS FROM QS Vir: CATACLYSMIC OR A LOT OF HOT AIR? SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; binaries: close; binaries: eclipsing; novae, cataclysmic variables; stars: winds, outflows; X-rays: binaries ID PHOTON IMAGING CAMERA; MAGNETIC BRAKING; XMM-NEWTON; WHITE-DWARFS; MASS-LOSS; ANGULAR-MOMENTUM; SOLAR-WIND; VARIABLES; STARS; EVOLUTION AB An XMM-Newton observation of the nearby "pre-cataclysmic" short-period (P-orb = 3.62 hr) binary QS Vir (EC 13471-1258) revealed regular narrow X-ray eclipses when the white dwarf passed behind its M2-4 dwarf companion. The X-ray emission provides a clear signature of mass transfer and accretion onto the white dwarf. The low-resolution XMM-Newton EPIC spectra are consistent with a cooling flow model and indicate an accretion rate of (M) over dot = 1.7 x 10(-13) M-circle dot yr(-1). At 48 pc distant, QS Vir is then the second nearest accreting cataclysmic variable known, with one of the lowest accretion rates found to date for a non-magnetic system. To feed this accretion through a wind would require a wind mass-loss rate of (M) over dot similar to 2 x 10(-12) M-circle dot yr(-1) if the accretion efficiency is of the order of 10%. Consideration of likely mass-loss rates for M dwarfs suggests this is improbably high and pure wind accretion unlikely. A lack of accretion disk signatures also presents some difficulties for direct Roche lobe overflow. We speculate that QS Vir is on the verge of Roche lobe overflow, and that the observed mass transfer could be supplemented by upward chromospheric flows on the M dwarf, analogous to spicules and mottles on the Sun, that escape the Roche surface to be subsequently swept up into the white dwarf Roche lobe. If so, QS Vir would be in a rare evolutionary phase lasting only a million years. The X-ray luminosity of the M dwarf estimated during primary eclipse is L-X = 3 x 10(28) erg s(-1), which is consistent with that of rapidly rotating "saturated" K and M dwarfs. C1 [Matranga, Marco; Drake, Jeremy J.; Kashyap, Vinay] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Steeghs, Danny] Univ Warwick, Dept Phys, Coventry CV4 7AL, W Midlands, England. RP Matranga, M (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM mmatranga@cfa.harvard.edu RI Steeghs, Danny/C-5468-2009 OI Steeghs, Danny/0000-0003-0771-4746 FU NASA [NNG06GD34, GNAS8-39073]; CXC science team; Harvey Tananbaum FX We are indebted to Boris Gansicke for very useful comments and discussion of low accretion rate CV-like systems. M.M. was supported by NASA grant NNG06GD34G during the course of this work. J.J.D. and V.K. were funded by NASA contract NAS8-39073 to the Chandra X-ray Center (CXC) and thank the CXC director, Harvey Tananbaum, and the CXC science team for advice and support. NR 60 TC 8 Z9 8 U1 0 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAR 10 PY 2012 VL 747 IS 2 AR 132 DI 10.1088/0004-637X/747/2/132 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 926UC UT WOS:000302856400048 ER PT J AU Muirhead, PS Johnson, JA Apps, K Carter, JA Morton, TD Fabrycky, DC Pineda, JS Bottom, M Rojas-Ayala, B Schlawin, E Hamren, K Covey, KR Crepp, JR Stassun, KG Pepper, J Hebb, L Kirby, EN Howard, AW Isaacson, HT Marcy, GW Levitan, D Diaz-Santos, T Armus, L Lloyd, JP AF Muirhead, Philip S. Johnson, John Asher Apps, Kevin Carter, Joshua A. Morton, Timothy D. Fabrycky, Daniel C. Pineda, John Sebastian Bottom, Michael Rojas-Ayala, Barbara Schlawin, Everett Hamren, Katherine Covey, Kevin R. Crepp, Justin R. Stassun, Keivan G. Pepper, Joshua Hebb, Leslie Kirby, Evan N. Howard, Andrew W. Isaacson, Howard T. Marcy, Geoffrey W. Levitan, David Diaz-Santos, Tanio Armus, Lee Lloyd, James P. TI CHARACTERIZING THE COOL KOIs. III. KOI 961: A SMALL STAR WITH LARGE PROPER MOTION AND THREE SMALL PLANETS SO ASTROPHYSICAL JOURNAL LA English DT Article DE planetary systems; stars: fundamental parameters; stars: individual (Barnard's Star, KOI 961); stars: late-type; stars: low-mass ID LOW-MASS STARS; KEPLER INPUT CATALOG; TRANSIT LIGHT-CURVE; BINARY CM DRACONIS; DIGITAL SKY SURVEY; SOLAR-TYPE STARS; M-DWARFS; RADIAL-VELOCITIES; METAL-RICH; PHOTOMETRIC CALIBRATION AB We characterize the star KOI 961, an M dwarf with transit signals indicative of three short-period exoplanets discovered by the Kepler mission. We proceed by comparing KOI 961 to Barnard's Star, a nearby, well-characterized mid-M dwarf. We compare colors, optical and near-infrared spectra, and find remarkable agreement between the two, implying similar effective temperatures and metallicities. Both are metal-poor compared to the Solar neighborhood, have low projected rotational velocity, high absolute radial velocity, large proper motion, and no quiescent Ha emission-all of which are consistent with being old M dwarfs. We combine empirical measurements of Barnard's Star and expectations from evolutionary isochrones to estimate KOI 961's mass (0.13 +/- 0.05 M-circle dot), radius (0.17 +/- 0.04 R-circle dot), and luminosity (2.40 x 10(-3.0 perpendicular to 0.3) L-circle dot). We calculate KOI 961's distance (38.7 +/- 6.3 pc) and space motions, which, like Barnard's Star, are consistent with a high scale-height population in the Milky Way. We perform an independent multi-transit fit to the public Kepler light curve and significantly revise the transit parameters for the three planets. We calculate the false-positive probability for each planet candidate, and find a less than 1% chance that any one of the transiting signals is due to a background or hierarchical eclipsing binary, validating the planetary nature of the transits. The best-fitting radii for all three planets are less than 1 R., with KOI 961.03 being Mars-sized (R-P = 0.57 +/- 0.18 R-circle plus), and they represent some of the smallest exoplanets detected to date. C1 [Muirhead, Philip S.; Johnson, John Asher; Morton, Timothy D.; Pineda, John Sebastian; Bottom, Michael; Crepp, Justin R.; Kirby, Evan N.; Levitan, David] CALTECH, Dept Astron, Pasadena, CA 91125 USA. [Johnson, John Asher] NASA Exoplanet Sci Inst NExScI, Pasadena, CA 91125 USA. [Carter, Joshua A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Fabrycky, Daniel C.; Hamren, Katherine] Univ Calif Santa Cruz, UCO Lick, Santa Cruz, CA 95064 USA. [Rojas-Ayala, Barbara] Amer Museum Nat Hist, Dept Astrophys, New York, NY 10024 USA. [Schlawin, Everett; Covey, Kevin R.; Lloyd, James P.] Cornell Univ, Dept Astron, Ithaca, NY 14583 USA. [Stassun, Keivan G.; Pepper, Joshua; Hebb, Leslie] Vanderbilt Univ, Dept Phys & Astron, Nashville, TN 37235 USA. [Stassun, Keivan G.] Fisk Univ, Dept Phys, Nashville, TN 37208 USA. [Stassun, Keivan G.] MIT, Dept Phys, Cambridge, MA 02139 USA. [Howard, Andrew W.; Isaacson, Howard T.; Marcy, Geoffrey W.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Diaz-Santos, Tanio; Armus, Lee] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. RP Muirhead, PS (reprint author), CALTECH, Dept Astron, 1200 E Calif Blvd,MC 249-17, Pasadena, CA 91125 USA. EM philm@astro.caltech.edu RI Carter, Joshua/A-8280-2013; Lloyd, James/B-3769-2011; Muirhead, Philip/H-2273-2014; Howard, Andrew/D-4148-2015; Rojas-Ayala, Barbara/G-4382-2015; OI Covey, Kevin/0000-0001-6914-7797; Pepper, Joshua/0000-0002-3827-8417; Muirhead, Philip/0000-0002-0638-8822; Howard, Andrew/0000-0001-8638-0320; Rojas-Ayala, Barbara/0000-0002-0149-1302; Kirby, Evan/0000-0001-6196-5162; Fabrycky, Daniel/0000-0003-3750-0183 FU Hubble Fellowship Program; NASA [HF-51267.01-A, HST-HF-51253.01-A, HF-51272.01-A, HST-HF-51256.01-A, NAS 5-26555]; Space Telescope Science Institute; Vanderbilt Initiative in Data-intensive Astrophysics; NSF [AST-0849736, AST-1009810]; NASA Science Mission directorate; NASA Office of Space Science [NNX09AF08G]; U.S. Government [NAG W-2166]; National Geographic Society; Sloan Foundation; Samuel Oschin Foundation; Samuel Oschin Foundation, and the Eastman Kodak Corporation FX J.A.C, K. R. C., D. C. F., and E.N.K. acknowledge support for this work from the Hubble Fellowship Program, provided by NASA through Hubble Fellowship grants HF-51267.01-A, HST-HF-51253.01-A, HF-51272.01-A, and HST-HF-51256.01-A, awarded by the Space Telescope Science Institute, which is operated by the AURA, Inc., for NASA, under contract NAS 5-26555. K. G. S., J.P., and L. H. acknowledge support through the Vanderbilt Initiative in Data-intensive Astrophysics and NSF grants AST-0849736 and AST-1009810.; This paper includes data collected by the Kepler mission. Funding for the Kepler mission is provided by the NASA Science Mission directorate. Some of the data presented in this paper were obtained from the Multimission Archive at the Space Telescope Science Institute (MAST). STScI is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555. Support for MAST for non-HST data is provided by the NASA Office of Space Science via grant NNX09AF08G and by other grants and contracts.; The United Kingdom Infrared Telescope (UKIRT) is operated by the Joint Astronomy Centre on behalf of the Science and Technology Facilities Council of the U.K.; The Digitized Sky Surveys were produced at the Space Telescope Science Institute under U.S. Government grant NAG W-2166. The images of these surveys are based on photographic data obtained using the Oschin Schmidt Telescope on Palomar Mountain and the U. K. Schmidt Telescope. The plates were processed into the present compressed digital form with the permission of these institutions.; The National Geographic Society-Palomar Observatory Sky Atlas (POSS-I) was made by the California Institute of Technology with grants from the National Geographic Society. The Second Palomar Observatory Sky Survey (POSS-II) was made by the California Institute of Technology with funds from the National Science Foundation, the National Geographic Society, the Sloan Foundation, the Samuel Oschin Foundation, and the Eastman Kodak Corporation. The Oschin Schmidt Telescope is operated by the California Institute of Technology and Palomar Observatory. NR 100 TC 121 Z9 121 U1 2 U2 9 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAR 10 PY 2012 VL 747 IS 2 AR 144 DI 10.1088/0004-637X/747/2/144 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 926UC UT WOS:000302856400060 ER PT J AU Nagel, E Espaillat, C D'Alessio, P Calvet, N AF Nagel, Erick Espaillat, Catherine D'Alessio, Paola Calvet, Nuria TI MID-INFRARED VARIABILITY OF THE BINARY SYSTEM CS Cha SO ASTROPHYSICAL JOURNAL LA English DT Article DE circumstellar matter; infrared: stars; stars: pre-main sequence ID T-TAURI STARS; PRE-MAIN-SEQUENCE; SPECTRAL ENERGY-DISTRIBUTIONS; CHAMELEON-I; PRETRANSITIONAL DISKS; PROTOPLANETARY DISKS; TRANSITIONAL DISKS; ACCRETION DISKS; CIRCUMSTELLAR DISKS; CIRCUMBINARY DISKS AB CS Cha is a binary system surrounded by a circumbinary disk. We construct a model for the inner disk regions and compare the resulting synthetic spectral energy distribution (SED) with Infrared Spectrograph spectra of CS Cha taken at two different epochs. For our model, we adopt a non-axisymmetric mass distribution from results of published numerical simulations of the interaction between a circumbinary disk and a binary system, where each star is surrounded by a disk. In particular, we approximate the streams of mass from which the inner circumstellar disks accrete from the circumbinary disk. This structure is due to the gravitational interaction of the stars with the disk, in which an array of disks and streams is formed in an inner hole. We calculate the temperature distribution of the optically thin dust in these inner regions considering the variable impinging radiation from both stars and use the observations to estimate the mass variations in the streams. We find that the SEDs for both epochs can be explained with emission from an optically thick inner edge of the circumbinary disk and from the optically thin streams that connect the circumbinary disk with the two smaller circumstellar disks. To the best of our knowledge, this is the first time that the emission from the optically thin material in the hole, suggested by the theory, is tested against observations of a binary system. C1 [Nagel, Erick] Univ Guanajuato, Dept Astron, Guanajuato 36240, Gto, Mexico. [Espaillat, Catherine] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [D'Alessio, Paola] UNAM, Ctr Radioastron & Astrofis, Morelia 58089, Michoacan, Mexico. [Calvet, Nuria] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. RP Nagel, E (reprint author), Univ Guanajuato, Dept Astron, Guanajuato 36240, Gto, Mexico. EM erick@astro.ugto.mx FU National Science Foundation [0901947]; NASA [NNX08AH94G]; PAPITT-DGAPA-UNAM [IN11209]; CONACYT FX E.N. thanks the hospitality of the Department of Astronomy of the University of Michigan during a research stay, where part of this work was done. C.E. was supported by the National Science Foundation under Award No. 0901947. N.C. acknowledges support from NASA Origins Grant NNX08AH94G. P.D. acknowledges the grant IN11209 from PAPITT-DGAPA-UNAM and CONACYT. NR 58 TC 11 Z9 11 U1 0 U2 8 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAR 10 PY 2012 VL 747 IS 2 AR 139 DI 10.1088/0004-637X/747/2/139 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 926UC UT WOS:000302856400055 ER PT J AU Prestwich, AH Galache, JL Linden, T Kalogera, V Zezas, A Roberts, TP Kilgard, R Wolter, A Trinchieri, G AF Prestwich, A. H. Galache, J. L. Linden, T. Kalogera, V. Zezas, A. Roberts, T. P. Kilgard, R. Wolter, A. Trinchieri, G. TI CHANDRA OBSERVATIONS OF THE COLLISIONAL RING GALAXY NGC 922 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: individual (NGC 922); X-rays: galaxies ID X-RAY SOURCES; CARTWHEEL RING; STAR-FORMATION; ANTENNAE GALAXIES; SOURCE POPULATION; BLACK-HOLES; METALLICITY; NGC-922 AB In this paper, we report on Chandra observations of the starburst galaxy NGC 922. NGC 922 is a drop-through ring galaxy with an expanding ring of star formation, similar in many respects to the Cartwheel galaxy. The Cartwheel galaxy is famous for hosting 12 ultraluminous X-ray sources (ULXs), most of which are in the star-forming ring. This is the largest number of ULXs seen in a single system and has led to speculation that the low metallicity of the Cartwheel (0.3 Z(circle dot)) may optimize the conditions for ULX formation. In contrast, NGC 922 has metallicity near solar. The Chandra observations reveal a population of bright X-ray sources, including seven ULXs. The number of ULXs in NGC 922 and the Cartwheel scales with the star formation rate: we do not find any evidence for an excess of sources in the Cartwheel. Simulations of the binary population in these galaxies suggest that the ULX population in both systems is dominated by systems with strong wind accretion from supergiant donors onto direct-collapse black holes. The simulations correctly predict the ratio of the number of sources in NGC 922 and the Cartwheel. Thus, it would appear that the metallicity of the Cartwheel is not low enough to see a difference in the ULX population compared to NGC 922. C1 [Prestwich, A. H.; Galache, J. L.; Zezas, A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Linden, T.] Univ Calif Santa Cruz, Dept Phys, Santa Cruz, CA 95064 USA. [Kalogera, V.] Northwestern Univ, Dept Phys & Astron, Evanston, IL 60208 USA. [Kalogera, V.] Northwestern Univ, CIERA, Evanston, IL 60208 USA. [Zezas, A.] Univ Crete, Dept Phys, Iraklion 71003, Crete, Greece. [Zezas, A.] Fdn Res & Technol Hellas, Iraklion 71110, Crete, Greece. [Roberts, T. P.] Univ Durham, Dept Phys, Durham DH1 3LE, England. [Kilgard, R.] Wesleyan Univ, Van Vleck Observ, Middletown, CT 06459 USA. [Wolter, A.; Trinchieri, G.] Osserv Astron Brera, INAF, IT-20121 Milan, Italy. RP Prestwich, AH (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Zezas, Andreas/C-7543-2011; OI Zezas, Andreas/0000-0001-8952-676X; Wolter, Anna/0000-0001-5840-9835; Trinchieri, Ginevra/0000-0002-0227-502X FU National Aeronautics and Space Administration [GO9-0097A, NAS8-03060]; ASI-INAF [I/009/10/0] FX We thank the referee for comments which improved this paper. Support for this work was provided by the National Aeronautics and Space Administration through Chandra Award Number GO9-0097A issued by the Chandra X-ray Observatory Center, which is operated by the Smithsonian Astrophysical Observatory for and on behalf of the National Aeronautics Space Administration under contract NAS8-03060. This research has made use of the NASA/IPAC Extragalactic Database (NED) which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. G. T. and A. W. acknowledge partial financial contribution from the ASI-INAF agreement I/009/10/0. NR 34 TC 3 Z9 3 U1 0 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAR 10 PY 2012 VL 747 IS 2 AR 150 DI 10.1088/0004-637X/747/2/150 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 926UC UT WOS:000302856400066 ER PT J AU Wong, TW Valsecchi, F Fragos, T Kalogera, V AF Wong, Tsing-Wai Valsecchi, Francesca Fragos, Tassos Kalogera, Vassiliki TI UNDERSTANDING COMPACT OBJECT FORMATION AND NATAL KICKS. III. THE CASE OF CYGNUS X-1 SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries: close; X-rays: binaries; X-rays: individual (Cygnus X-1) ID BROAD-BAND SPECTRUM; X-RAY BINARIES; BLACK-HOLE; HDE 226868; OB-ASSOCIATIONS; OPTICAL-SPECTRUM; TRIGONOMETRIC PARALLAXES; FUNDAMENTAL PARAMETERS; STELLAR EVOLUTION; TIDAL-EVOLUTION AB In recent years, accurate observational constraints have become available for an increasing number of Galactic X-ray binaries (XRBs). Together with proper-motion measurements, we could reconstruct the full evolutionary history of XRBs back to the time of compact object formation. In this paper, we present the first study of the persistent X-ray source Cygnus X-1 that takes into account all available observational constraints. Our analysis accounts for three evolutionary phases: orbital evolution and motion through the Galactic potential after the formation of a black hole (BH), and binary orbital dynamics at the time of core collapse. We find that the mass of the BH immediate progenitor is 15.0-20.0 M-circle dot, and at the time of core collapse, the BH has potentially received a small kick velocity of <= 77 km s(-1) at 95% confidence. If the BH progenitor mass is less than similar to 17 M-circle dot, a non-zero natal kick velocity is required to explain the currently observed properties of Cygnus X-1. Since the BH has only accreted mass from its companion's stellar wind, the negligible amount of accreted mass does not explain the observationally inferred BH spin of a(*) > 0.95, and the origin of this extreme BH spin must be connected to the BH formation itself. Right after the BH formation, we find that the BH companion is a 19.8-22.6 M-circle dot main-sequence star, orbiting the BH at a period of 4.7-5.2 days. Furthermore, recent observations show that the BH companion is currently super-synchronized. This super-synchronism indicates that the strength of tides exerted on the BH companion should be weaker by a factor of at least two compared to the usually adopted strength. C1 [Wong, Tsing-Wai; Valsecchi, Francesca; Kalogera, Vassiliki] Northwestern Univ, CIERA, Evanston, IL 60208 USA. [Wong, Tsing-Wai; Valsecchi, Francesca; Kalogera, Vassiliki] Northwestern Univ, Dept Phys & Astron, Evanston, IL 60208 USA. [Fragos, Tassos] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Wong, TW (reprint author), Northwestern Univ, CIERA, 2145 Sheridan Rd, Evanston, IL 60208 USA. EM tsingwong2012@u.northwestern.edu; francesca@u.northwestern.edu; tfragos@cfa.harvard.edu; vicky@northwestern.edu RI Fragos, Tassos/A-3581-2016 OI Fragos, Tassos/0000-0003-1474-1523 FU NSF [AST-0908930, PHY-1066293]; Harvard-Smithsonian Center for Astrophysics; Harvard Institute for Theory and Computation FX This work has been primarily supported by the NSF Grant AST-0908930; V.K. also acknowledges partial support through the NSF Grant PHY-1066293 and the hospitality of the Aspen Center for Physics; T.F. acknowledges Fellowship support by the Harvard-Smithsonian Center for Astrophysics and the Harvard Institute for Theory and Computation. NR 67 TC 24 Z9 24 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAR 10 PY 2012 VL 747 IS 2 AR 111 DI 10.1088/0004-637X/747/2/111 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 926UC UT WOS:000302856400027 ER PT J AU Chen, XP Arce, HG Dunham, MM Zhang, QZ AF Chen, Xuepeng Arce, Hector G. Dunham, Michael M. Zhang, Qizhou TI DISCOVERY OF A BINARY SYSTEM IN IRAM 04191+1522 SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE binaries: general; ISM: clouds; ISM: individual objects (IRAM 04191+1522); stars: formation ID MOLECULAR LINE; PROTOSTAR IRAM-04191; DENSE CORES; HH 211; COLLAPSE; OUTFLOW; CLOUDS; FRAGMENTATION; ROTATION; ENVELOPE AB We present high angular resolution observations of the Class 0 protostar IRAM 04191+1522 using the Submillimeter Array (SMA). The SMA 1.3 mm continuum images reveal within IRAM 04191+1522 two distinct sources with an angular separation of 7 ''.8 +/- 0 ''.2. The two continuum sources are located in the southeast-northwest direction, with total gas masses of similar to 0.011 M-circle dot and similar to 0.005 M-circle dot, respectively. The southeastern source, associated with an infrared source seen in the Spitzer images, is the well-known Class 0 protostar with a bolometric luminosity of similar to 0.08 L-circle dot. The newly discovered northwestern continuum source is not visible in the Spitzer images at wavelengths from 3.6 to 70 mu m and has an extremely low bolometric luminosity (<0.03L(circle dot)). Complementary IRAM N2H+ (1-0) data that probe the dense gas in the common envelope suggest that the two sources were formed through the rotational fragmentation of an elongated dense core. Furthermore, comparisons between IRAM 04191+1522 and other protostars suggest that most cores with binary systems formed therein have ratios of rotational energy to gravitational energy beta(rot) > 1%. This is consistent with theoretical simulations and indicates that the level of rotational energy in a dense core plays an important role in the fragmentation process. C1 [Chen, Xuepeng; Arce, Hector G.; Dunham, Michael M.] Yale Univ, Dept Astron, New Haven, CT 06520 USA. [Zhang, Qizhou] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Chen, XP (reprint author), Yale Univ, Dept Astron, Box 208101, New Haven, CT 06520 USA. EM xuepeng.chen@yale.edu OI Zhang, Qizhou/0000-0003-2384-6589 FU NSF [AST-0845619] FX We thank the anonymous referee for many insightful comments and suggestions. We thank A. Belloche and P. Andre for providing their N2H+ (1-0) data of IRAM 04191+1522. This material is based on work supported by NSF grant AST-0845619 to HGA. NR 31 TC 11 Z9 11 U1 1 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD MAR 10 PY 2012 VL 747 IS 2 AR L43 DI 10.1088/2041-8205/747/2/L43 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 902SQ UT WOS:000301060900026 ER PT J AU Savage, SL McKenzie, DE Reeves, KK AF Savage, Sabrina L. McKenzie, David E. Reeves, Katharine K. TI RE-INTERPRETATION OF SUPRA-ARCADE DOWNFLOWS IN SOLAR FLARES SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE magnetic reconnection; Sun: corona; Sun: coronal mass ejections (CMEs); Sun: flares; Sun: magnetic topology; Sun: UV radiation ID QUANTITATIVE EXAMINATION; RECONNECTION; MODEL; EMISSIONS; MOTIONS; EVENTS AB Following the eruption of a filament from a flaring active region, sunward-flowing voids are often seen above developing post-eruption arcades. First discovered using the soft X-ray telescope aboard Yohkoh, these supra-arcade downflows (SADs) are now an expected observation of extreme ultra-violet and soft X-ray coronal imagers and spectrographs (e.g, TRACE, SOHO/SUMER, Hinode/XRT, SDO/AIA). Observations made prior to the operation of AIA suggested that these plasma voids (which are seen in contrast to bright, high-temperature plasma associated with current sheets) are the cross-sections of evacuated flux tubes retracting from reconnection sites high in the corona. The high temperature imaging afforded by AIA's 131, 94, and 193 angstrom channels coupled with the fast temporal cadence allows for unprecedented scrutiny of the voids. For a flare occurring on 2011 October 22, we provide evidence suggesting that SADs, instead of being the cross-sections of relatively large, evacuated flux tubes, are actually wakes (i.e., trailing regions of low density) created by the retraction of much thinner tubes. This re-interpretation is a significant shift in the fundamental understanding of SADs, as the features once thought to be identifiable as the shrinking loops themselves now appear to be "side effects" of the passage of the loops through the supra-arcade plasma. In light of the fact that previous measurements have attributed to the shrinking loops characteristics that may instead belong to their wakes, we discuss the implications of this new interpretation on previous parameter estimations and on reconnection theory. C1 [Savage, Sabrina L.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [McKenzie, David E.] Montana State Univ, Dept Phys, Bozeman, MT 59717 USA. [Reeves, Katharine K.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Savage, SL (reprint author), NASA, Goddard Space Flight Ctr, 8800 Greenbelt Rd,Code 671, Greenbelt, MD 20771 USA. RI Reeves, Katharine/P-9163-2014 FU NASA; Lockheed-Martin [SP02H3901R, SP02H1701R] FX S.L. Savage is supported by an appointment to the NASA Postdoctoral Program at Goddard Space Flight Center administered by Oakridge Associated Universities through a contract with NASA and under the mentorship of G. Holman. D. E. McKenzie is supported under contract SP02H3901R from Lockheed-Martin to MSU. K.K. Reeves is supported under contract SP02H1701R from Lockheed-Martin to SAO. NR 26 TC 38 Z9 38 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD MAR 10 PY 2012 VL 747 IS 2 AR L40 DI 10.1088/2041-8205/747/2/L40 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 902SQ UT WOS:000301060900023 ER PT J AU Hagedorn, M Carter, V Martorana, K Paresa, MK Acker, J Baums, IB Borneman, E Brittsan, M Byers, M Henley, M Laterveer, M Leong, JA McCarthy, M Meyers, S Nelson, BD Petersen, D Tiersch, T Uribe, RC Woods, E Wildt, D AF Hagedorn, Mary Carter, Virginia Martorana, Kelly Paresa, Malia K. Acker, Jason Baums, Iliana B. Borneman, Eric Brittsan, Michael Byers, Michael Henley, Michael Laterveer, Michael Leong, Jo-Ann McCarthy, Megan Meyers, Stuart Nelson, Brian D. Petersen, Dirk Tiersch, Terrence Uribe, Rafael Cuevas Woods, Erik Wildt, David TI Preserving and Using Germplasm and Dissociated Embryonic Cells for Conserving Caribbean and Pacific Coral SO PLOS ONE LA English DT Article ID IN-VITRO FERTILIZATION; REGION-WIDE DECLINES; ACROPORA-PALMATA; CLIMATE-CHANGE; POCILLOPORA-DAMICORNIS; SPERM CRYOPRESERVATION; CRASSOSTREA-GIGAS; FUNGIA-SCUTARIA; RESOURCE BANKS; PHASE-SHIFTS AB Coral reefs are experiencing unprecedented degradation due to human activities, and protecting specific reef habitats may not stop this decline, because the most serious threats are global (i.e., climate change), not local. However, ex situ preservation practices can provide safeguards for coral reef conservation. Specifically, modern advances in cryobiology and genome banking could secure existing species and genetic diversity until genotypes can be introduced into rehabilitated habitats. We assessed the feasibility of recovering viable sperm and embryonic cells post-thaw from two coral species, Acropora palmata and Fungia scutaria that have diffferent evolutionary histories, ecological niches and reproductive strategies. In vitro fertilization (IVF) of conspecific eggs using fresh (control) spermatozoa revealed high levels of fertilization (> 90% in A. palmata;> 84% in F. scutaria; P > 0.05) that were unaffected by tested sperm concentrations. A solution of 10% dimethyl sulfoxide (DMSO) at cooling rates of 20 to 30 degrees C/min most successfully cryopreserved both A. palmata and F. scutaria spermatozoa and allowed producing developing larvae in vitro. IVF success under these conditions was 65% in A. palmata and 53% in F. scutaria on particular nights; however, on subsequent nights, the same process resulted in little or no IVF success. Thus, the window for optimal freezing of high quality spermatozoa was short (similar to 5 h for one night each spawning cycle). Additionally, cryopreserved F. scutaria embryonic cells had, 50% post-thaw viability as measured by intact membranes. Thus, despite some differences between species, coral spermatozoa and embryonic cells are viable after low temperature (-196 degrees C) storage, preservation and thawing. Based on these results, we have begun systematically banking coral spermatozoa and embryonic cells on a large-scale as a support approach for preserving existing bio- and genetic diversity found in reef systems. C1 [Hagedorn, Mary; Carter, Virginia; Martorana, Kelly; Paresa, Malia K.; Wildt, David] Smithsonian Conservat Biol Inst, Dept Reprod Sci, Front Royal, VA USA. [Hagedorn, Mary; Carter, Virginia; Martorana, Kelly; Paresa, Malia K.; Leong, Jo-Ann] Univ Hawaii, Hawaii Inst Marine Biol, Kaneohe, HI USA. [Acker, Jason] Univ Alberta, Lab Med & Pathol, Edmonton, AB, Canada. [Baums, Iliana B.] Penn State Univ, Dept Biol, University Pk, PA 16802 USA. [Borneman, Eric] Univ Houston, Dept Biol & Biochem, Houston, TX USA. [Brittsan, Michael] Columbus Zoo & Aquarium, Powell, OH USA. [Byers, Michael; Woods, Erik] Gen BioTechnol, Indianapolis, IN USA. [Henley, Michael] Smithsonian Natl Zool Pk, Invertebrate Exhibit, Washington, DC USA. [Laterveer, Michael; Petersen, Dirk] Rotterdam Zoo, Rotterdam, Netherlands. [McCarthy, Megan; Meyers, Stuart] Univ Calif Davis, Dept Anat Physiol & Cell Biol, Davis, CA 95616 USA. [Nelson, Brian D.] Cent Wharf, New England Aquarium, Dept Fishes, Boston, MA USA. [Tiersch, Terrence; Uribe, Rafael Cuevas] Louisiana State Univ, Ctr Agr, Aquaculture Res Stn, Baton Rouge, LA 70803 USA. RP Hagedorn, M (reprint author), Smithsonian Conservat Biol Inst, Dept Reprod Sci, Front Royal, VA USA. EM hagedornm@si.edu RI Baums, Iliana/G-6435-2010 OI Baums, Iliana/0000-0001-6463-7308 FU National Oceanic and Atmospheric Administration [NA07NMF4630109, NA NA08NMF4630462]; National Science Foundation [OCE - 0825979]; Morris Animal Foundation [D07ZO-053]; Columbus Zoo and Aquarium Conservation Fund; Rotterdam Zoo, Green Foundation; Clyde and Connie Woodburn Foundation; Smithsonian Institution; Louisiana State University Agricultural Center; University of California Davis; Canadian Natural Sciences and Engineering Research Council (NSERC); Hawaii Institute of Marine Biology FX This work was supported by: National Oceanic and Atmospheric Administration (grant # NA07NMF4630109 to MH; grant # NA NA08NMF4630462 to IB); National Science Foundation (OCE - 0825979 to IB); Morris Animal Foundation (grant # D07ZO-053 to MH); Columbus Zoo and Aquarium Conservation Fund (to MH); Rotterdam Zoo, Green Foundation, Clyde and Connie Woodburn Foundation (to SECORE); Smithsonian Institution, Louisiana State University Agricultural Center, University of California Davis and Hawaii Institute of Marine Biology and the Canadian Natural Sciences and Engineering Research Council (NSERC). The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 64 TC 17 Z9 17 U1 1 U2 32 PU PUBLIC LIBRARY SCIENCE PI SAN FRANCISCO PA 1160 BATTERY STREET, STE 100, SAN FRANCISCO, CA 94111 USA SN 1932-6203 J9 PLOS ONE JI PLoS One PD MAR 8 PY 2012 VL 7 IS 3 AR e33354 DI 10.1371/journal.pone.0033354 PG 13 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 929KT UT WOS:000303062000044 PM 22413020 ER PT J AU Banks, ME Watters, TR Robinson, MS Tornabene, LL Tran, T Ojha, L Williams, NR AF Banks, M. E. Watters, T. R. Robinson, M. S. Tornabene, L. L. Tran, T. Ojha, L. Williams, N. R. TI Morphometric analysis of small-scale lobate scarps on the Moon using data from the Lunar Reconnaissance Orbiter SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article ID PLANETARY WRINKLE RIDGES; TOTALLY MOLTEN MOON; THRUST FAULTS; TERRESTRIAL PLANETS; CRUSTAL DICHOTOMY; ASTEROID 433-EROS; THERMAL HISTORY; MARS; MERCURY; TECTONICS AB Prior to Lunar Reconnaissance Orbiter (LRO), the morphology and dimensions of only a limited number of lobate scarps, all located near the equator (within 21 degrees), had been characterized. Topography derived from LRO Camera stereo images and Lunar Orbiter Laser Altimeter (LOLA) ranging is used to measure the relief and analyze the morphology of previously known and newly detected low and high latitude lobate scarps. The asymmetric profiles and maximum slopes on scarp faces (similar to 5 degrees to 29 degrees) of lunar lobate scarps are similar to those of lobate scarps observed on Mars and Mercury. Scarp lengths range from similar to 0.6 to 21.6 km (mean = similar to 6.0 km, median = similar to 4.4 km, n = 79), and measured relief ranges from similar to 5 to 150 m (mean = similar to 35 m, median = similar to 20 m, n = 26). Assuming a range of 20 degrees to 40 degrees for the fault plane dip, estimated lower limits for the horizontal shortening (S) expressed by the lobate scarp thrust faults range from similar to 10 to 410 m. The range in S estimated for the lunar scarps is roughly an order of magnitude lower than estimates of S for lobate scarp thrust faults on Mars and Mercury. The relatively small range of S estimated for the growing number of well-characterized lunar scarps is consistent with a small amount of global contraction. C1 [Banks, M. E.; Watters, T. R.; Tornabene, L. L.] Smithsonian Inst, Ctr Earth & Planetary Studies, Natl Air & Space Museum, Washington, DC 20560 USA. [Ojha, L.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA. [Robinson, M. S.; Tran, T.; Williams, N. R.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA. RP Banks, ME (reprint author), Smithsonian Inst, Ctr Earth & Planetary Studies, Natl Air & Space Museum, Washington, DC 20560 USA. EM banksme@si.edu RI Ojha, Lujendra/B-2805-2013 FU NASA [NNX08AM73G] FX We gratefully acknowledge the LRO and LROC engineers and technical support personnel. This work benefited from thoughtful reviews by Ernst Hauber, Matthew Golombek, and Laurent Montesi. This work was supported by NASA Grant NNX08AM73G. NR 64 TC 11 Z9 12 U1 0 U2 10 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0148-0227 J9 J GEOPHYS RES-PLANET JI J. Geophys. Res.-Planets PD MAR 7 PY 2012 VL 117 AR E00H11 DI 10.1029/2011JE003907 PG 11 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 908OH UT WOS:000301499200001 ER PT J AU Weimer, H Yao, NY Laumann, CR Lukin, MD AF Weimer, Hendrik Yao, Norman Y. Laumann, Chris R. Lukin, Mikhail D. TI Long-Range Quantum Gates using Dipolar Crystals SO PHYSICAL REVIEW LETTERS LA English DT Article ID NUCLEAR-SPIN QUBITS; SOLID-STATE SPIN; COUPLED ELECTRON; RYDBERG BLOCKADE; ATOMS; ENTANGLEMENT; DIAMOND; RESOLUTION AB We propose the use of dipolar spin chains to enable long-range quantum logic between distant qubits. In our approach, an effective interaction between remote qubits is achieved by adiabatically following the ground state of the dipolar chain across the paramagnet to crystal phase transition. We demonstrate that the proposed quantum gate is particularly robust against disorder and derive scaling relations, showing that high-fidelity qubit coupling is possible in the presence of realistic imperfections. Possible experimental implementations in systems ranging from ultracold Rydberg atoms to arrays of nitrogen vacancy defect centers in diamond are discussed. C1 [Weimer, Hendrik; Yao, Norman Y.; Laumann, Chris R.; Lukin, Mikhail D.] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. [Weimer, Hendrik; Laumann, Chris R.] Harvard Smithsonian Ctr Astrophys, ITAMP, Cambridge, MA 02138 USA. RP Weimer, H (reprint author), Harvard Univ, Dept Phys, 17 Oxford St, Cambridge, MA 02138 USA. EM hweimer@cfa.harvard.edu RI Yao, Norman/A-3929-2009 OI Yao, Norman/0000-0003-0194-7266 FU National Science Foundation; DOE [FG02-97ER25308]; Lawrence Golub Fellowship; CUA; NSF; DARPA; AFOSR MURI; Packard Foundation; German Academic Exchange Service (DAAD) FX We acknowledge fruitful discussions with P. Zoller, L. Huijse, and A. Chandran. This work was supported by the National Science Foundation through a grant for the Institute for Theoretical Atomic, Molecular and Optical Physics at Harvard University and Smithsonian Astrophysical Observatory, a fellowship within the Postdoc Program of the German Academic Exchange Service (DAAD), the DOE (FG02-97ER25308), the Lawrence Golub Fellowship, CUA, NSF, DARPA, AFOSR MURI, and the Packard Foundation. NR 45 TC 12 Z9 12 U1 1 U2 12 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 0031-9007 J9 PHYS REV LETT JI Phys. Rev. Lett. PD MAR 7 PY 2012 VL 108 IS 10 AR 100501 DI 10.1103/PhysRevLett.108.100501 PG 5 WC Physics, Multidisciplinary SC Physics GA 904FT UT WOS:000301180200001 PM 22463396 ER PT J AU Johnson, GD Ida, H Sakaue, J Sado, T Asahida, T Miya, M AF Johnson, G. David Ida, Hitoshi Sakaue, Jiro Sado, Tetsuya Asahida, Takashi Miya, Masaki TI A 'living fossil' eel (Anguilliformes: Protanguillidae, fam. nov.) from an undersea cave in Palau SO PROCEEDINGS OF THE ROYAL SOCIETY B-BIOLOGICAL SCIENCES LA English DT Article DE eel; morphology; phylogeny; new species; genus and family; divergence time ID PHYLOGENETIC TREE SELECTION; 1ST ANGUILLIFORMES; MAXIMUM-LIKELIHOOD; FISHES; TELEOSTEI; ORIGIN; GENERA AB We report the discovery of an enigmatic, small eel-like fish from a 35 m-deep fringing-reef cave in the western Pacific Ocean Republic of Palau that exhibits an unusual suite of morphological characters. Many of these uniquely characterize the Recent members of the 19 families comprising the elopomorph order Anguilliformes, the true eels. Others are found among anguilliforms only in the Cretaceous fossils, and still others are primitive with respect to both Recent and fossil eels. Thus, morphological evidence explicitly places it as the most basal lineage (i.e. the sister group of extant anguilliforms). Phylogenetic analysis and divergence time estimation based on whole mitogenome sequences from various actinopterygians, including representatives of all eel families, demonstrate that this fish represents one of the most basal, independent lineages of the true eels, with a long evolutionary history comparable to that of the entire Anguilliformes (approx. 200 Myr). Such a long, independent evolutionary history dating back to the early Mesozoic and a retention of primitive morphological features (e.g. the presence of a premaxilla, metapterygoid, free symplectic, gill rakers, pseudobranch and distinct caudal fin rays) warrant recognition of this species as a 'living fossil' of the true eels, herein described as Protanguilla palau genus et species nov. in the new family Protanguillidae. C1 [Sado, Tetsuya; Miya, Masaki] Nat Hist Museum & Inst, Chuo Ku, Chiba 2608682, Japan. [Johnson, G. David] Smithsonian Inst, Natl Museum Nat Hist, Div Fishes, Washington, DC 20560 USA. [Ida, Hitoshi; Asahida, Takashi] Kitasato Univ, Sch Marine Biosci, Ofunato, Iwate 0220101, Japan. [Sakaue, Jiro] So Marine Lab, Koror 96940, Palau. RP Miya, M (reprint author), Nat Hist Museum & Inst, Chuo Ku, Chiba 2608682, Japan. EM miya@chiba-muse.or.jp FU Ministry of Education, Culture, Sports, Science, and Technology, Japan [17207007, 22580229]; Herb and Evelyn Axelrod Chair in Systematic Ichthyology FX We sincerely thank H. Rebelkuul, A. Bukurrou and K. Kamiishi for their cooperation with our collection of the specimens. We also thank J. G. Inoue for his help in preliminary phylogenetic analysis, Z. Yang for his advice on the selection of appropriate priors in MCMCTREE analysis, and V. G. Springer, G. D. Smith, L. Ruber and G. Nelson for their useful comments on the manuscript. Ai Nonaka and Sandra Raredon provided technical assistance. Portions of this study were supported by grants-in-aid from the Ministry of Education, Culture, Sports, Science, and Technology, Japan to M.M. (17207007 and 22580229), and from the Herb and Evelyn Axelrod Chair in Systematic Ichthyology. NR 51 TC 18 Z9 19 U1 0 U2 17 PU ROYAL SOC PI LONDON PA 6-9 CARLTON HOUSE TERRACE, LONDON SW1Y 5AG, ENGLAND SN 0962-8452 J9 P ROY SOC B-BIOL SCI JI Proc. R. Soc. B-Biol. Sci. PD MAR 7 PY 2012 VL 279 IS 1730 BP 934 EP 943 DI 10.1098/rspb.2011.1289 PG 10 WC Biology; Ecology; Evolutionary Biology SC Life Sciences & Biomedicine - Other Topics; Environmental Sciences & Ecology; Evolutionary Biology GA 887ET UT WOS:000299910400014 PM 21849321 ER PT J AU Luiz, OJ Madin, JS Robertson, DR Rocha, LA Wirtz, P Floeter, SR AF Luiz, Osmar J. Madin, Joshua S. Ross Robertson, D. Rocha, Luiz A. Wirtz, Peter Floeter, Sergio R. TI Ecological traits influencing range expansion across large oceanic dispersal barriers: insights from tropical Atlantic reef fishes SO PROCEEDINGS OF THE ROYAL SOCIETY B-BIOLOGICAL SCIENCES LA English DT Article DE macroecology; biogeographic barriers; Amazon-Orinoco Plume; rafting; larval-development mode; body size ID PELAGIC LARVAL DURATION; INDO-PACIFIC; BODY-SIZE; COMPARATIVE PHYLOGEOGRAPHY; LIFE-HISTORY; CORAL-REEFS; PATTERNS; SPECIATION; DISTANCE; CONSERVATION AB How do biogeographically different provinces arise in response to oceanic barriers to dispersal? Here, we analyse how traits related to the pelagic dispersal and adult biology of 985 tropical reef fish species correlate with their establishing populations on both sides of two Atlantic marine barriers: the Mid-Atlantic Barrier (MAB) and the Amazon-Orinoco Plume (AOP). Generalized linear mixed-effects models indicate that predictors for successful barrier crossing are the ability to raft with flotsam for the deep-water MAB, non-reef habitat usage for the freshwater and sediment-rich AOP, and large adult-size and large latitudinal-range for both barriers. Variation in larval-development mode, often thought to be broadly related to larval-dispersal potential, is not a significant predictor in either case. Many more species of greater taxonomic diversity cross the AOP than the MAB. Rafters readily cross both barriers but represent a much smaller proportion of AOP crossers than MAB crossers. Successful establishment after crossing both barriers may be facilitated by broad environmental tolerance associated with large body size and wide latitudinal-range. These results highlight the need to look beyond larval-dispersal potential and assess adult-biology traits when assessing determinants of successful movements across marine barriers. C1 [Luiz, Osmar J.; Madin, Joshua S.] Macquarie Univ, Dept Biol Sci, Sydney, NSW 2109, Australia. [Ross Robertson, D.] Smithsonian Trop Res Inst, Balboa, Panama. [Rocha, Luiz A.] Calif Acad Sci, Sect Ichthyol, San Francisco, CA 94118 USA. [Wirtz, Peter] Univ Algarve, Ctr Ciencias Mar, P-8005139 Faro, Portugal. [Floeter, Sergio R.] Univ Fed Santa Catarina, Dept Ecol & Zool, BR-88010970 Florianopolis, SC, Brazil. RP Luiz, OJ (reprint author), Macquarie Univ, Dept Biol Sci, Sydney, NSW 2109, Australia. EM osmarluizjr@gmail.com RI Rocha, Luiz/C-5107-2011; Floeter, Sergio/B-1438-2012; Luiz, Osmar/D-9202-2011; OI Luiz, Osmar/0000-0002-6995-6524; Madin, Joshua/0000-0002-5005-6227 FU International Macquarie University; Australian Research Council; Smithsonian Tropical Research Institute; National Geographic Society [7937-05]; CNPq; NSF [DEB-0072909]; University of California FX Financial support was provided by an International Macquarie University Research Excellence Scholarship (O.J.L.), the Australian Research Council (J.S.M), the Smithsonian Tropical Research Institute (D.R.R.; STV grant to S.R.F.), the National Geographic Society (grant 7937-05 to S.R.F) and the CNPq (S.R.F.). This work benefited from informal meetings at the National Centre for Ecological Analysis and Synthesis, a centre funded by the NSF (grant DEB-0072909) and the University of California, Santa Barbara. We thank Michel Kulbicki and five anonymous reviewers for suggestions on the manuscript. NR 56 TC 51 Z9 53 U1 2 U2 52 PU ROYAL SOC PI LONDON PA 6-9 CARLTON HOUSE TERRACE, LONDON SW1Y 5AG, ENGLAND SN 0962-8452 J9 P ROY SOC B-BIOL SCI JI Proc. R. Soc. B-Biol. Sci. PD MAR 7 PY 2012 VL 279 IS 1730 BP 1033 EP 1040 DI 10.1098/rspb.2011.1525 PG 8 WC Biology; Ecology; Evolutionary Biology SC Life Sciences & Biomedicine - Other Topics; Environmental Sciences & Ecology; Evolutionary Biology GA 887ET UT WOS:000299910400026 PM 21920979 ER PT J AU Graham, AM Aiken, GR Gilmour, CC AF Graham, Andrew M. Aiken, George R. Gilmour, Cynthia C. TI Dissolved Organic Matter Enhances Microbial Mercury Methylation Under Sulfidic Conditions SO ENVIRONMENTAL SCIENCE & TECHNOLOGY LA English DT Article ID DESULFOVIBRIO-DESULFURICANS ND132; SEDIMENT PORE WATERS; METHYLMERCURY PRODUCTION; HUMIC SUBSTANCES; BIOAVAILABILITY; BACTERIA; NANOPARTICLES; CARBON; HG(II); PRECIPITATION AB Dissolved organic matter (DOM) is generally thought to lower metal bioavailability in aquatic systems due to the formation of metal DOM complexes that reduce free metal ion concentrations. However, this model may not be pertinent for metal nanoparticles, which are now understood to be ubiquitous, sometimes dominant, metal species in the environment. The influence of DOM on Hg bioavailability to microorganisms was examined under conditions (0.5-5.0 nM Hg and 2-10 mu M sulfide) that favor the formation of beta-HgS(s) (metacinnabar) nanoparticles. We used the methylation of stable-isotope enriched (HgCl2)-Hg-201 by Desulfovibrio desulfuricans ND132 in short-term washed cell assays as a sensitive, environmentally significant proxy for Hg uptake. Suwannee River humic acid (SRHA) and Williams Lake hydrophobic acid (WLHPoA) substantially enhanced (2- to 38-fold) the bioavailability of Hg to ND132 over a wide range of Hg/DOM ratios (9.4 pmol/mg DOM to 9.4 nmol/mg DOM), including environmentally relevant ratios. Methylmercury (MeHg) production by ND132 increased linearly with either SRHA or WLHPoA concentration, but SRHA, a terrestrially derived DOM, was far more effective at enhancing Hg-methylation than WLHPoA, an aquatic DOM dominated by autochthonous sources. No DOM-dependent enhancement in Hg methylation was observed in Hg-DOM-sulfide solutions amended with sufficient L-cysteine to prevent beta-HgS(s) formation. We hypothesize that small HgS particles, stabilized against aggregation by DOM, are bioavailable to Hg-methylating bacteria. Our laboratory experiments provide a mechanism for the positive correlations between DOC and MeHg production observed in many aquatic sediments and wetland soils. C1 [Graham, Andrew M.; Gilmour, Cynthia C.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. [Aiken, George R.] US Geol Survey, Boulder, CO 80303 USA. RP Graham, AM (reprint author), Smithsonian Environm Res Ctr, 647 Contees Wharf Rd, Edgewater, MD 21037 USA. EM grahaman@si.edu RI Gilmour, Cynthia/G-1784-2010 OI Gilmour, Cynthia/0000-0002-1720-9498 FU U.S. Department of Energy; Office of Biological and Environmental Research, Office of Science, through Oak Ridge National Laboratory; U.S. National Science Foundation [DEB0351050]; Smithsonian Institution FX We thank A. Bullock, A. Maizel, G. Riedel, T. Bell, K. Butler, and B. Poulin for laboratory assistance and C. Gerbig for his comments on the manuscript. This work was supported by the U.S. Department of Energy under the Subsurface Biogeochemical Research Program, Office of Biological and Environmental Research, Office of Science, through the Mercury Science Focus Area Program at Oak Ridge National Laboratory, by U.S. National Science Foundation grant DEB0351050 to A. Heyes and C. Gilmour, and by the U.S. Geological Survey Priority Ecosystems and Toxics Substances Hydrology Programs. A.M.G. acknowledges support from the Smithsonian Institution Postdoctoral Fellowship Program. Any use of trade, firm, or product names is for descriptive purposes only and does not imply endorsement by the U.S. government. NR 43 TC 79 Z9 87 U1 24 U2 181 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0013-936X J9 ENVIRON SCI TECHNOL JI Environ. Sci. Technol. PD MAR 6 PY 2012 VL 46 IS 5 BP 2715 EP 2723 DI 10.1021/es203658f PG 9 WC Engineering, Environmental; Environmental Sciences SC Engineering; Environmental Sciences & Ecology GA 902FJ UT WOS:000301023700033 PM 22309093 ER PT J AU Aliu, E Archambault, S Arlen, T Aune, T Beilicke, M Benbow, W Bouvier, A Bradbury, SM Buckley, JH Bugaev, V Byrum, K Cannon, A Cesarini, A Christiansen, JL Ciupik, L Collins-Hughes, E Connolly, MP Cui, W Decerprit, G Dickherber, R Dumm, J Errando, M Falcone, A Feng, Q Ferrer, F Finley, JP Finnegan, G Fortson, L Furniss, A Galante, N Gall, D Godambe, S Griffin, S Grube, J Gyuk, G Hanna, D Holder, J Huan, H Hughes, G Humensky, TB Kaaret, P Karlsson, N Kertzman, M Khassen, Y Kieda, D Krawczynski, H Krennrich, F Lee, K Madhavan, AS Maier, G Majumdar, P McArthur, S McCann, A Moriarty, P Mukherjee, R Ong, RA Orr, M Otte, AN Park, N Perkins, JS Pohl, M Prokoph, H Quinn, J Ragan, K Reyes, LC Reynolds, PT Roache, E Rose, HJ Ruppel, J Saxon, DB Schroedter, M Sembroski, GH Senturk, GD Skole, C Smith, AW Staszak, D Telezhinsky, I Tesic, G Theiling, M Thibadeau, S Tsurusaki, K Varlotta, A Vassiliev, VV Vincent, S Vivier, M Wagner, RG Wakely, SP Ward, JE Weekes, TC Weinstein, A Weisgarber, T Williams, DA Zitzer, B AF Aliu, E. Archambault, S. Arlen, T. Aune, T. Beilicke, M. Benbow, W. Bouvier, A. Bradbury, S. M. Buckley, J. H. Bugaev, V. Byrum, K. Cannon, A. Cesarini, A. Christiansen, J. L. Ciupik, L. Collins-Hughes, E. Connolly, M. P. Cui, W. Decerprit, G. Dickherber, R. Dumm, J. Errando, M. Falcone, A. Feng, Q. Ferrer, F. Finley, J. P. Finnegan, G. Fortson, L. Furniss, A. Galante, N. Gall, D. Godambe, S. Griffin, S. Grube, J. Gyuk, G. Hanna, D. Holder, J. Huan, H. Hughes, G. Humensky, T. B. Kaaret, P. Karlsson, N. Kertzman, M. Khassen, Y. Kieda, D. Krawczynski, H. Krennrich, F. Lee, K. Madhavan, A. S. Maier, G. Majumdar, P. McArthur, S. McCann, A. Moriarty, P. Mukherjee, R. Ong, R. A. Orr, M. Otte, A. N. Park, N. Perkins, J. S. Pohl, M. Prokoph, H. Quinn, J. Ragan, K. Reyes, L. C. Reynolds, P. T. Roache, E. Rose, H. J. Ruppel, J. Saxon, D. B. Schroedter, M. Sembroski, G. H. Sentuerk, G. D. Skole, C. Smith, A. W. Staszak, D. Telezhinsky, I. Tesic, G. Theiling, M. Thibadeau, S. Tsurusaki, K. Varlotta, A. Vassiliev, V. V. Vincent, S. Vivier, M. Wagner, R. G. Wakely, S. P. Ward, J. E. Weekes, T. C. Weinstein, A. Weisgarber, T. Williams, D. A. Zitzer, B. TI VERITAS deep observations of the dwarf spheroidal galaxy Segue 1 SO PHYSICAL REVIEW D LA English DT Article ID DARK-MATTER ANNIHILATION; LARGE-AREA TELESCOPE; GAMMA-RAY EMISSION; GALACTIC-CENTER; LOCAL GROUP; CHERENKOV TELESCOPES; EMPIRICAL-MODELS; MAGIC TELESCOPE; UPPER LIMITS; COSMIC-RAYS AB The VERITAS array of Cherenkov telescopes has carried out a deep observational program on the nearby dwarf spheroidal galaxy Segue 1. We report on the results of nearly 48 hours of good quality selected data, taken between January 2010 and May 2011. No significant gamma-ray emission is detected at the nominal position of Segue 1, and upper limits on the integrated flux are derived. According to recent studies, Segue 1 is the most dark matter-dominated dwarf spheroidal galaxy currently known. We derive stringent bounds on various annihilating and decaying dark matter particle models. The upper limits on the velocity-weighted annihilation cross-section are (95%) (CL) less than or similar to 10(-23) cm(3) s(-1), improving our limits from previous observations of dwarf spheroidal galaxies by at least a factor of 2 for dark matter particle masses m(chi) greater than or similar to 300 GeV. The lower limits on the decay lifetime are at the level of tau(95%) (CL) greater than or similar to 10(24) s. Finally, we address the interpretation of the cosmic ray lepton anomalies measured by ATIC and PAMELA in terms of dark matter annihilation, and show that the VERITAS observations of Segue 1 disfavor such a scenario. C1 [Holder, J.; Saxon, D. B.; Vivier, M.] Univ Delaware, Dept Phys & Astron, Newark, DE 19716 USA. [Holder, J.; Saxon, D. B.; Vivier, M.] Univ Delaware, Bartol Res Inst, Newark, DE 19716 USA. [Aliu, E.; Errando, M.; Mukherjee, R.] Columbia Univ, Dept Phys & Astron, Barnard Coll, New York, NY 10027 USA. [Archambault, S.; Griffin, S.; Hanna, D.; McCann, A.; Ragan, K.; Staszak, D.; Tesic, G.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada. [Arlen, T.; Majumdar, P.; Ong, R. A.; Vassiliev, V. V.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. [Aune, T.; Bouvier, A.; Furniss, A.; Otte, A. N.; Williams, D. A.] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Santa Cruz, CA 95064 USA. [Aune, T.; Bouvier, A.; Furniss, A.; Otte, A. N.; Williams, D. A.] Univ Calif Santa Cruz, Dept Phys, Santa Cruz, CA 95064 USA. [Beilicke, M.; Buckley, J. H.; Bugaev, V.; Dickherber, R.; Ferrer, F.; Krawczynski, H.; Lee, K.; McArthur, S.; Thibadeau, S.] Washington Univ, Dept Phys, St Louis, MO 63130 USA. [Benbow, W.; Galante, N.; Roache, E.; Schroedter, M.; Weekes, T. C.] Harvard Smithsonian Ctr Astrophys, Fred Lawrence Whipple Observ, Amado, AZ 85645 USA. [Bradbury, S. M.; Rose, H. J.] Univ Leeds, Sch Phys & Astron, Leeds LS2 9JT, W Yorkshire, England. [Byrum, K.; Wagner, R. G.] Argonne Natl Lab, Argonne, IL 60439 USA. [Cannon, A.; Collins-Hughes, E.; Khassen, Y.; Quinn, J.; Ward, J. E.] Natl Univ Ireland Univ Coll Dublin, Sch Phys, Dublin 4, Ireland. [Cesarini, A.; Connolly, M. P.] Natl Univ Ireland Univ Coll Galway, Sch Phys, Galway, Ireland. [Christiansen, J. L.; Reyes, L. C.] Calif Polytech State Univ San Luis Obispo, Dept Phys, San Luis Obispo, CA 94307 USA. [Ciupik, L.; Grube, J.; Gyuk, G.] Adler Planetarium & Astron Museum, Dept Astron, Chicago, IL 60605 USA. [Cui, W.; Feng, Q.; Finley, J. P.; Sembroski, G. H.; Theiling, M.; Varlotta, A.; Zitzer, B.] Purdue Univ, Dept Phys, W Lafayette, IN 47907 USA. [Decerprit, G.; Hughes, G.; Maier, G.; Pohl, M.; Prokoph, H.; Ruppel, J.; Skole, C.; Telezhinsky, I.] DESY, D-15738 Zeuthen, Germany. [Dumm, J.; Fortson, L.; Karlsson, N.] Univ Minnesota, Sch Phys & Astron, Minneapolis, MN 55455 USA. [Falcone, A.] Penn State Univ, Dept Astron & Astrophys, Davey Lab 525, University Pk, PA 16802 USA. [Finnegan, G.; Godambe, S.; Kieda, D.; Smith, A. W.; Vincent, S.] Univ Utah, Dept Phys & Astron, Salt Lake City, UT 84112 USA. [Gall, D.; Tsurusaki, K.] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA. [Huan, H.; Park, N.; Wakely, S. P.; Weisgarber, T.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA. [Humensky, T. B.; Sentuerk, G. D.] Columbia Univ, Dept Phys, New York, NY 10027 USA. [Kertzman, M.] DePauw Univ, Dept Phys & Astron, Greencastle, IN 46135 USA. [Krennrich, F.; Madhavan, A. S.; Orr, M.; Weinstein, A.] Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA. [Moriarty, P.] Galway Mayo Inst Technol, Dept Life & Phys Sci, Galway, Ireland. [Perkins, J. S.] NASA, Goddard Space Flight Ctr, Astroparticle Phys Lab, Greenbelt, MD 20771 USA. [Perkins, J. S.] CRESST, Greenbelt, MD 20771 USA. [Perkins, J. S.] Univ Maryland, Baltimore, MD 21250 USA. [Pohl, M.; Ruppel, J.; Telezhinsky, I.] Univ Potsdam, Inst Phys & Astron, D-14476 Potsdam, Germany. [Reynolds, P. T.] Cork Inst Technol, Dept Appl Phys & Instrumentat, Bishopstown, Cork, Ireland. RP Vivier, M (reprint author), Univ Delaware, Dept Phys & Astron, Newark, DE 19716 USA. EM mvivier@bartol.udel.edu RI Khassen, Yerbol/I-3806-2015; OI Khassen, Yerbol/0000-0002-7296-3100; Cui, Wei/0000-0002-6324-5772; Cesarini, Andrea/0000-0002-8611-8610; Ward, John E/0000-0003-1973-0794 FU US Department of Energy Office of Science; US National Science Foundation; Smithsonian Institution; NSERC in Canada; Science Foundation Ireland [SFI 10/RFP/AST2748]; STFC in the United Kingdom FX We thank Rouven Essig, Neelima Sehgal, and Louis E. Strigari for useful discussions about the Segue 1 dark matter distribution profile. VERITAS is supported by grants from the US Department of Energy Office of Science, the US National Science Foundation, and the Smithsonian Institution, by NSERC in Canada, by Science Foundation Ireland (Grant No. SFI 10/RFP/AST2748), and by STFC in the United Kingdom. We acknowledge the excellent work of the technical support staff at the Fred Lawrence Whipple Observatory and at the collaborating institutions in the construction and operation of the instrument. NR 99 TC 55 Z9 56 U1 0 U2 2 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 2470-0010 EI 2470-0029 J9 PHYS REV D JI Phys. Rev. D PD MAR 5 PY 2012 VL 85 IS 6 AR 062001 DI 10.1103/PhysRevD.85.062001 PG 12 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA 903LC UT WOS:000301117000003 ER PT J AU McCosker, JE Long, DJ Baldwin, CC AF McCosker, John E. Long, Douglas J. Baldwin, Carole C. TI Description of a new species of deepwater catshark, Bythaelurus giddingsi sp nov., from the Galapagos Islands (Chondrichthyes: Carcharhiniformes: Scyliorhinidae) SO ZOOTAXA LA English DT Article DE Ichthyology; systematics; Scyliorhinidae; Bythaelurus; new species; endemism; Galapagos AB We describe Bythaelurus giddingsi sp. nov. based on 7 specimens collected using the submersible Johnson Sea-Link from deepwater (428-562 m depth) areas of the Galapagos Islands. It is presumed to be endemic to the archipelago. The new species differs from its congeners in its coloration, the length of its anal-fin base, and in other morphological characters. The disjunct distribution of species of the widely-distributed Indo-Pacific genus Bythaelurus is discussed. C1 [McCosker, John E.; Long, Douglas J.] Calif Acad Sci, Dept Aquat Biol, San Francisco, CA 94118 USA. [Long, Douglas J.] Oakland Museum Calif, Dept Nat Sci, Oakland, CA 94607 USA. [Baldwin, Carole C.] Smithsonian Inst, Natl Museum Nat Hist, Divisi Fishes, Washington, DC 20560 USA. RP McCosker, JE (reprint author), Calif Acad Sci, Dept Aquat Biol, 55 Mus Concourse Dr, San Francisco, CA 94118 USA. EM jmccosker@calacademy.org; dlong@museumca.org; baldwinc@si.edu FU David and Lucile Packard Foundation; Griffith Family Foundation FX We thank Eliecer Cruz, Arturo Izurieta Valery, Eduardo Amador, and Mario Piu of the Galapagos National Park for permission to perform research in the GNP; Alex Hearn of CDRS for sharing information and a photograph of a Galapagos specimen; Robert Bensted-Smith and the CDRS for general assistance in the Galapagos; Leonard Compagno for his help with an earlier draft of this manuscript; the staff of the Harbor Branch Oceanographic Institution and the crews of the R/V Seward Johnson and its submersible, the Johnson Sea-Link, and in particular its ace sub pilot Don Libertore; Alison E. Schroeer for preparing Figure 2; Christina Fidler and Lauren Scheinberg (CAS) for their assistance with shark teeth photographs; Al Giddings of Images Unlimited, David Clark, David Pawson, Julie Piraino, the Discovery Channel, IMAX, and the Smithsonian Institution Discovery Center Project for their support during the expeditions; and the David and Lucile Packard Foundation and the Griffith Family Foundation for financial assistance to JM in support of this and other Galapagos projects. We also thank the staffs of the following institutions for the assistance that they provided us: the California Academy of Sciences (CAS), San Francisco; the Museum National d'Histoire Naturelle, Paris; the National Museum of Natural History (USNM), Washington D. C.; the Natural History Museum (BMNH), London; the South African Museum (SAM), Cape Town; and the Scripps Institution of Oceanography (SIO), San Diego. NR 33 TC 4 Z9 4 U1 0 U2 3 PU MAGNOLIA PRESS PI AUCKLAND PA PO BOX 41383, AUCKLAND, ST LUKES 1030, NEW ZEALAND SN 1175-5326 EI 1175-5334 J9 ZOOTAXA JI Zootaxa PD MAR 5 PY 2012 IS 3221 BP 48 EP 59 PG 12 WC Zoology SC Zoology GA 903ML UT WOS:000301120600004 ER PT J AU Mcgowan, R AF Mcgowan, Robert TI AN ACCOUNT INTENDED TO ESTABLISH FOR THE PAINTER BRADEN NESS HIS RIGHTFUL PLACE IN HISTORY SO DALHOUSIE REVIEW LA English DT Fiction, Creative Prose C1 [Mcgowan, Robert] Smithsonian Inst, Washington, DC 20560 USA. NR 0 TC 0 Z9 0 U1 1 U2 1 PU DALHOUSIE UNIV PRESS LTD PI HALIFAX NS PA DALHOUSIE UNIV SIR JAMES DUNN SCI BLDG 314, HALIFAX NS, B3H 3J5, CANADA SN 0011-5827 J9 DALHOUSIE REV JI Dalhous. Rev. PD SPR-SUM PY 2012 VL 92 IS 1-2 BP 149 EP 159 PG 11 WC Literary Reviews SC Literature GA 068YP UT WOS:000313402400024 ER PT J AU Dekar, MP King, RS Back, JA Whigham, DF Walker, CM AF Dekar, Matthew P. King, Ryan S. Back, Jeffrey A. Whigham, Dennis F. Walker, Coowe M. TI Allochthonous inputs from grass-dominated wetlands support juvenile salmonids in headwater streams: evidence from stable isotopes of carbon, hydrogen, and nitrogen SO FRESHWATER SCIENCE LA English DT Article DE deuterium; food webs; Oncorhynchus kisutch; Salvelinus malma; trophic structure ID FOOD WEBS; SOUTHEASTERN ALASKA; AQUATIC CONSUMERS; ENERGY-FLOW; COHO SALMON; RIVER; ECOSYSTEMS; PATHWAYS; WATER; BREAKDOWN AB We used dual-isotope mixing models (delta C-13/delta N-15 and delta H-2/delta N-15) in a Bayesian framework to partition allochthonous and autochthonous energy sources for salmonids in 2 headwater streams in the Kenai Lowlands, Alaska (USA). Our 1st objective was to estimate the production base for juvenile coho salmon (Oncorhynchus kisutch) and Dolly Varden (Salvelinus malma). We hypothesized that consumers would be reliant on both autochthonous (filamentous algae and periphyton) and allochthonous sources, but that autochthonous sources would dominate because of the open canopy and lower-quality litter inputs provided by the riparian wetland vegetation, primarily bluejoint grass (Calamagrostis canadensis). Our 2nd objective was to evaluate the utility of stable H isotopes for tracing energy pathways in a northern-latitude ecosystem. We hypothesized that delta H-2-based models would provide more precise estimates of source partitioning than delta C-13-based models because of greater source separation. Allochthonous source contributions consistently exceeded autochthonous sources for all fish species and size classes at both study sites. However, diet shifted during ontogeny, and larger Dolly Varden relied more on autochthonous sources than did smaller individuals of both species. Last, we found good correspondence and similar levels of precision between the delta C-13-and delta H-2-based models despite greater source separation by delta H-2. Our results highlight the importance of allochthonous sources in headwater streams, and we suggest that litter inputs from grasses may be an under-appreciated subsidy to salmon production. Stable H isotopes can be an effective foodweb tracer in northern-latitude streams, but source partitioning results were not sufficiently different from stable C isotope models for us to recommend unequivocally using them to replace or enhance delta C-13 in similar studies. C1 [Dekar, Matthew P.; King, Ryan S.; Back, Jeffrey A.] Baylor Univ, Dept Biol, Ctr Reservoir & Aquat Syst Res, Waco, TX 76798 USA. [Whigham, Dennis F.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. [Walker, Coowe M.] Kachemak Bay Res Reserve, Homer, AK 99603 USA. RP Dekar, MP (reprint author), Baylor Univ, Dept Biol, Ctr Reservoir & Aquat Syst Res, 1 Bear Pl 97178, Waco, TX 76798 USA. EM matthew_dekar@baylor.edu; ryan_s_king@baylor.edu; jeff_back@baylor.edu; whighamd@si.edu; coowe.walker@alaska.gov OI Whigham, Dennis/0000-0003-1488-820X FU US Environmental Protection Agency [CD-96011801-0]; Baylor University; University Research Committee [0301533EY]; Vice Provost for Research Postdoctoral Fellowship FX This project was funded by grants from the US Environmental Protection Agency (CD-96011801-0) and from Baylor University, including a University Research Committee grant to RSK (0301533EY) and a Vice Provost for Research Postdoctoral Fellowship to MPD. Additional support was provided by the Kachemak Bay Research Reserve (KBRR) and the Smithsonian Environmental Research Center. We thank Amy Alderfer, Steve Baird, Kim Cooney, Scott Pegau, Angela Doroff, and Terry Thompson for logistical and field support at KBRR. Richard Doucett from the Colorado Plateau Stable Isotope Laboratory at Northern Arizona University processed samples for stable-isotope analysis. Additional support for stable-isotope analysis was provided by Steve Dworkin and Ren Zhang at Baylor University. Jesse Ray, Rebecca Shaftel, Jason Taylor, and 2 anonymous referees provided helpful comments on an earlier draft of this manuscript. NR 39 TC 8 Z9 8 U1 7 U2 69 PU SOC FRESWATER SCIENCE PI WACO PA 5400 BOSQUE BLVD, STE 680, WACO, TX 76710 USA SN 2161-9565 J9 FRESHW SCI JI Freshw. Sci. PD MAR PY 2012 VL 31 IS 1 BP 121 EP 132 DI 10.1899/11-016.1 PG 12 WC Ecology; Marine & Freshwater Biology SC Environmental Sciences & Ecology; Marine & Freshwater Biology GA 021RY UT WOS:000309904300011 ER PT J AU Gowda, V Temeles, EJ Kress, WJ AF Gowda, Vinita Temeles, Ethan J. Kress, W. John TI TERRITORIAL FIDELITY TO NECTAR SOURCES BY PURPLE-THROATED CARIBS, EULAMPIS JUGULARIS SO WILSON JOURNAL OF ORNITHOLOGY LA English DT Article ID GOLDEN-WINGED SUNBIRD; TROPICAL HUMMINGBIRD; FEEDING TERRITORIALITY; SEXUAL-DIMORPHISM; HELICONIA; ECONOMICS; COMPETITION; BEHAVIOR; SIZE; INFLORESCENCES AB We present the first record of territorial site-fidelity across multiple years by Purple-throated Caribs (Eulatnpis jugularis) on three different islands in the eastern Caribbean: St. Kitts, Dominica, and St. Vincent. Marked male Purple-throated Caribs were monitored throughout the flowering season of their main nectar resources, Heliconia caribaea (St. Kitts and Dominica) and H. bihai (St. Vincent), both native perennial herbs. Individual males were observed defending the same Heliconia patches for 3 years (St. Vincent), 4 years (St. Kitts), and 5 years (Dominica), and remained near these patches even when they were not in flower. The territorial behavior and resource dependence of Purple-throated Caribs on native heliconias likely have a key role in the coevolution of this specialized plant-pollinator interaction. Received 17 March 2011. Accepted 2 August 2011. C1 [Gowda, Vinita] George Washington Univ, Dept Biol Sci, Washington, DC 20052 USA. [Temeles, Ethan J.] Amherst Coll, Dept Biol, Amherst, MA 01002 USA. RP Gowda, V (reprint author), Smithsonian Inst, Dept Bot, MRC-166,POB 37012, Washington, DC 20013 USA. EM vinitagowda@gmail.com FU Weintraub Graduate Fellowship from Department of Biological Sciences, The George Washington University; Cosmos Club; Sigma-Xi; Smithsonian Institution; National Science Foundation [DEB-0614218] FX We thank the Ministry of Agriculture and the Environment; Forestry, Wildlife, and Parks Division; Commonwealth of Dominica, Government of St. Christopher and Nevis, and Forestry Department, Ministry of Agriculture and Fisheries, St. Vincent and the Grenadines for facilitating this study. We also thank Arlington James, Eric Hypo lite, Ida Lopez, Anne Jno Baptiste, and Gregory Pereira for logistic help and discussion. We thank C. E. Braun and two anonymous reviewers for helpful comments and assistance on this manuscript. This work was supported by a Weintraub Graduate Fellowship from the Department of Biological Sciences, The George Washington University to VG and also by the Cosmos Club, Sigma-Xi, and the Smithsonian Institution. Field work for this study was supported by grants from National Science Foundation (DEB-0614218) to E. J. Temeles and W. J. Kress. NR 40 TC 4 Z9 4 U1 5 U2 29 PU WILSON ORNITHOLOGICAL SOC PI WACO PA 5400 BOSQUE BLVD, STE 680, WACO, TX 76710 USA SN 1559-4491 EI 1938-5447 J9 WILSON J ORNITHOL JI Wilson J. Ornithol. PD MAR PY 2012 VL 124 IS 1 BP 81 EP 86 PG 6 WC Ornithology SC Zoology GA 005YN UT WOS:000308786100011 ER PT J AU Deutsch, J AF Deutsch, James TI Spirits of Just Men: Mountaineers, Liquor Bosses, and Lawmen in the Moonshine Capital of the World SO WESTERN FOLKLORE LA English DT Book Review C1 [Deutsch, James] Smithsonian Inst, Washington, DC 20560 USA. RP Deutsch, J (reprint author), Smithsonian Inst, Washington, DC 20560 USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU CALIFORNIA FOLKLORE SOC PI POMONA PA WESTERN FOLKLORE DEPT OF ENGL/FOREIGN LANGUAGES 3801 W.TEMPLE AVENUE, POMONA, CA 91768-4010 USA SN 0043-373X J9 WESTERN FOLKLORE JI West. Folk. PD SPR PY 2012 VL 71 IS 2 BP 186 EP 187 PG 2 WC Folklore SC Arts & Humanities - Other Topics GA 998VA UT WOS:000308267300011 ER PT J AU Ferrari, FD Grygier, MJ AF Ferrari, Frank D. Grygier, Mark J. TI VARIABILITY OF TRUNK LIMBS ALONG THE ANTERIOR/POSTERIOR BODY AXIS OF JUVENILE AND ADULT LYNCEUS BIFORMIS (ISHIKAWA, 1895) (BRANCHIOPODA, LAEVICAUDATA, LYNCEIDAE) SO CRUSTACEANA LA English DT Article ID LARVAL DEVELOPMENT; JAPANESE CONCHOSTRACANS; PHYLLOPODOUS LIMBS; CRUSTACEA; SPINICAUDATA; MORPHOLOGY; REDESCRIPTION; HOMOLOGIES; PHYLOGENY AB Morphology of trunk limbs of the laevicaudatan branchiopod Lynceus biformis (Ishikawa, 1895) varies along the anterior/posterior axis of the body. On anterior limbs, the praecoxal endite is elongate and strongly flexed, endites of the coxa and basis are broad, and lobes of the endopod are elongate. On more posterior limbs protopodal endites and endopodal lobes are more similar to each other and none is particularly long or broad. In addition, an exite fails to form on more posterior limbs, and the exopod becomes progressively reduced in males or modified in females. Sexual dimorphism is expressed by fewer trunk limbs, 10, and a transformed trunk limb 1 of males, as well as by a modified exopod of posterior trunk limbs 8-12 of females. Development of all limbs includes an asetose step and several setose steps; some limb pairs may begin as a transverse bilobate flap. Developmental changes include the progressive addition of limbs posteriorly, addition of endites and lobes to some limbs, addition of an exite and proximal rod-like structure during the transformation to a setose limb, and the transformation of sexually dimorphic limbs during the molt to the adult. Naupliar asetose limbs 1-5 have fewer endites and lobes than the more posterior asetose limbs of juveniles have. The male clasper of L. biformis is a subchela formed from the basis and the distal segment of the endopod; the proximal and middle endopodal segments are closely associated with the subchela. In contrast, the clasper of male spinicaudatans is a subchela formed from the distal endopodal segment and the proximal of two middle segments of the endopod. The distal of the two middle endopodal segments and the palp it bears (together, the so-called "articulated palp") are absent in the clasper of L. biformis. The modified exopod on trunk limbs biformis of females of L. biformis has no similarly transformed counterpart on limbs of female spinicaudatans. There is no discoid endite on the trunk limb of L. biformis as there is on trunk limbs of spinicaudatans, and no setose attenuate endite either, although the asetose rod-like structure may be homologous to the latter. C1 [Ferrari, Frank D.] Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, Suitland, MD 20746 USA. [Grygier, Mark J.] Lake Biwa Museum, Kusatsu, Shiga 5250001, Japan. RP Ferrari, FD (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, MRC 534,4210 Silver Hill Rd, Suitland, MD 20746 USA. EM ferrarif@si.edu NR 33 TC 6 Z9 6 U1 0 U2 3 PU BRILL ACADEMIC PUBLISHERS PI LEIDEN PA PLANTIJNSTRAAT 2, P O BOX 9000, 2300 PA LEIDEN, NETHERLANDS SN 0011-216X J9 CRUSTACEANA JI Crustaceana PD MAR PY 2012 VL 85 IS 3 BP 359 EP 377 DI 10.1163/156854012X624655 PG 19 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA 944XI UT WOS:000304236700008 ER PT J AU Bernardini, MG Margutti, R Mao, J Zaninoni, E Chincarini, G AF Bernardini, M. G. Margutti, R. Mao, J. Zaninoni, E. Chincarini, G. TI The X-ray light curve of gamma-ray bursts: clues to the central engine SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE radiation mechanisms: non-thermal; X-rays: general; gamma rays: general ID SWIFT XRT DATA; COMPREHENSIVE ANALYSIS; ENERGY INJECTION; MILLISECOND PULSARS; AFTERGLOW EMISSION; FLARING ACTIVITY; PROMPT EMISSION; FLARES; LONG; GRBS AB Aims. We present the analysis of a large sample of gamma-ray burst (GRB) X-ray light curves in the rest frame to characterise their intrinsic properties in the context of different theoretical scenarios. Methods. We determine the morphology, timescales, and energetics of 64 long GRBs observed by Swift/XRT without flaring activity. We furthermore provide a one-to-one comparison to the properties of GRBs with X-ray flares. Results. We find that the steep decay morphology and its connection with X-ray flares favour a scenario in which a central engine origin. We show that this scenario can also account for the shallow decay phase, provided that the GRB progenitor star has a self-similar structure with a constant envelope-to-core mass ratio similar to 0.02-0.03. However, difficulties arise for very long duration (t(p) greater than or similar to 10(4) s) shallow phases. Alternatively, a spinning-down magnetar whose emitted power refreshes the forward shock can quantitatively account for the shallow decay properties. In particular we demonstrate that this model can account for the plateau luminosity vs. end time anticorrelation. C1 [Bernardini, M. G.; Margutti, R.; Zaninoni, E.; Chincarini, G.] INAF Osservatorio Astron Brera, I-23807 Merate, LC, Italy. [Bernardini, M. G.] ICRANet, I-65100 Pescara, Italy. [Margutti, R.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Mao, J.] Chinese Acad Sci, Yunnan Observ, Kunming 650011, Yunnan Province, Peoples R China. [Mao, J.] Chinese Acad Sci, Key Lab Struct & Evolut Celestial Objects, Kunming 650011, Yunnan Province, Peoples R China. [Mao, J.] Korean Astron & Space Sci Inst, Int Ctr Astrophys, Taejon, South Korea. [Zaninoni, E.] Univ Padua, Dept Astron, I-35122 Padua, Italy. [Chincarini, G.] Univ Milano Bicocca, Dept Phys, I-20126 Milan, Italy. RP Bernardini, MG (reprint author), INAF Osservatorio Astron Brera, Via Bianchi 46, I-23807 Merate, LC, Italy. EM grazia.bernardini@brera.inaf.it FU ASI [SWIFT I/011/07/0]; Ministry of University and Research of Italy [MIUR 2007TNYZXL]; MAE; University of Milano Bicocca (Italy) FX We thank the referee for her/his very useful comments and suggestions. This work is supported by ASI grant SWIFT I/011/07/0, by the Ministry of University and Research of Italy (PRIN MIUR 2007TNYZXL), by MAE, and by the University of Milano Bicocca (Italy). NR 58 TC 20 Z9 20 U1 0 U2 2 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD MAR PY 2012 VL 539 AR A3 DI 10.1051/0004-6361/201117895 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 932AS UT WOS:000303262000010 ER PT J AU Caramazza, M Micela, G Prisinzano, L Sciortino, S Damiani, F Favata, F Stauffer, JR Vallenari, A Wolk, SJ AF Caramazza, M. Micela, G. Prisinzano, L. Sciortino, S. Damiani, F. Favata, F. Stauffer, J. R. Vallenari, A. Wolk, S. J. TI Star formation in the outer Galaxy: coronal properties of NGC 1893 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE stars: pre-main sequence; stars: luminosity function, mass function; X-rays: stars; stars: coronae; stars: flare; open clusters and associations: individual: NGC 1893 ID ORION NEBULA CLUSTER; MAIN-SEQUENCE STARS; X-RAY-PROPERTIES; COUNTING DETECTOR IMAGES; TAURUS MOLECULAR CLOUD; YOUNG STARS; FORMING COMPLEX; SPECTRAL CLASSIFICATION; WAVELET TRANSFORMS; STELLAR POPULATION AB Context. The outer Galaxy, where the environmental conditions are different from the solar neighborhood, is a laboratory in which it is possible to investigate the dependence of star formation process on the environmental parameters. Aims. We investigate the X-ray properties of NGC 1893, a young cluster (similar to 1-2 Myr) in the outer part of the Galaxy (galactic radius >= 11 kpc) where we expect differences in the disk evolution and in the mass distribution of the stars, to explore the X-ray emission of its members and compare it with that of young stars in star-forming regions near to the Sun. Methods. We analyze 5 deep Chandra ACIS-I observations with a total exposure time of 450 ks. Source events of the 1021 X-ray sources have been extracted with the IDL-based routine ACIS-Extract. Using spectral fitting and quantile analysis of X-ray spectra, we derive X-ray luminosities and compare the respective properties of Class II and Class III members. We also evaluate the variability of sources using the Kolmogorov-Smirnov test and identify flares in the lightcurves. Results. The X-ray luminosity of NGC 1893 X-ray members is in the range 10(29.5)-10(31.5) erg s(-1). Diskless stars are brighter in X-rays than disk-bearing stars, given the same bolometric luminosity. We found that 34% of the 1021 lightcurves appear variable and that they show 0.16 flare per source, on average. Comparing our results with those relative to the Orion Nebula Cluster, we find that, by accounting for observational biases, the X-ray properties of NGC 1893 and the Orion ones are very similar. Conclusions. The X-ray properties in NGC 1893 are not affected by the environment and the stellar population in the outer Galaxy may have the same coronal properties of nearby star-forming regions. The X-ray luminosity properties and the X-ray luminosity function appear to be universal and can therefore be used for estimating distances and for determining stellar properties. C1 [Caramazza, M.; Micela, G.; Prisinzano, L.; Sciortino, S.; Damiani, F.] INAF Osservatorio Astron Palermo, I-90134 Palermo, Italy. [Favata, F.] European Space Agcy, F-75015 Paris, France. [Stauffer, J. R.] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. [Vallenari, A.] Osserv Astron Padova, INAF, I-35122 Padua, Italy. [Wolk, S. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Caramazza, M (reprint author), INAF Osservatorio Astron Palermo, Piazza Parlamento 1, I-90134 Palermo, Italy. EM mcarama@astropa.unipa.it OI Prisinzano, Loredana/0000-0002-8893-2210; Vallenari, Antonella/0000-0003-0014-519X; Micela, Giuseppina/0000-0002-9900-4751; Wolk, Scott/0000-0002-0826-9261; Damiani, Francesco/0000-0002-7065-3061 FU ASI-INAF [I/009/10/0]; European Commission [N. MRTN-CT-2006-035890]; PRIN-INAF; NASA [NAS8-03060] FX This research made use of data obtained from the Chandra X-ray Observatory and software provided by the Chandra X-ray Center (CXC) in the application packages CIAO, ChIPS, and Sherpa. We acknowledge financial contributions from ASI-INAF agreement I/009/10/0, from the European Commission (contract N. MRTN-CT-2006-035890) and PRIN-INAF (P. I. Lanza). S.J.W. is supported by NASA contract NAS8-03060 (Chandra). We thank the referee for helpful suggestions and comments that improved this work. NR 74 TC 5 Z9 5 U1 0 U2 3 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD MAR PY 2012 VL 539 AR A74 DI 10.1051/0004-6361/201117256 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 932AS UT WOS:000303262000081 ER PT J AU Chies-Santos, AL Larsen, SS Cantiello, M Strader, J Kuntschner, H Wehner, EM Brodie, JP AF Chies-Santos, A. L. Larsen, S. S. Cantiello, M. Strader, J. Kuntschner, H. Wehner, E. M. Brodie, J. P. TI An optical/NIR survey of globular clusters in early-type galaxies III. On the colour bimodality of globular cluster systems SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE galaxies: evolution; galaxies: star clusters: general; galaxies: elliptical and lenticular, cD ID ELLIPTIC GALAXIES; METALLICITY RELATIONS; STELLAR POPULATIONS; STAR-CLUSTERS; BRANCH STARS; AGES; DISTRIBUTIONS; PHOTOMETRY; M87; MODELS AB Context. The interpretation that bimodal colour distributions of globular clusters (GCs) reflect bimodal metallicity distributions has been challenged. Non-linearities in the colour to metallicity conversions caused for example by the horizontal branch (HB) stars may be responsible for transforming a unimodal metallicity distribution into a bimodal (optical) colour distribution. Aims. We study optical/near-infrared (NIR) colour distributions of the GC systems in 14 E/S0 galaxies. Methods. We test whether the bimodal feature, generally present in optical colour distributions, remains in the optical/NIR ones. The latter colour combination is a better metallicity proxy than the former. We use KMM and GMM tests to quantify the probability that different colour distributions are better described by a bimodal, as opposed to a unimodal distribution. Results. We find that double-peaked colour distributions are more commonly seen in optical than in optical/NIR colours. For some of the galaxies where the optical (g-z) distribution is clearly bimodal, a bimodal distribution is not preferred over a unimodal one at a statistically significant level for the (g-K) and (z-K) distributions. The two most cluster-rich galaxies in our sample, NGC4486 and NGC4649, show some interesting differences. The (g-K) distribution of NGC4649 is better described by a bimodal distribution, while this is true for the (g-K) distribution of NGC4486 GCs only if restricted to a brighter sub-sample with small K-band errors (<0.05 mag). Formally, the K-band photometric errors cannot be responsible for blurring bimodal metallicity distributions to unimodal (g-K) colour distributions. However, simulations including the extra scatter in the colour-colour diagrams (not fully accounted for in the photometric errors) show that such scatter may contribute to the disappearance of bimodality in (g-K) for the full NGC4486 sample. For the less cluster-rich galaxies results are inconclusive due to poorer statistics. Conclusions. A bimodal optical colour distribution is not necessarily an indication of an underlying bimodal metallicity distribution. Horizontal branch morphology may play an important role in shaping some of the optical GC colour distributions. However, we find tentative evidence that the (g-K) colour distributions remain bimodal in the two cluster-rich galaxies in our sample (NGC4486 and NGC4649) when restricted to clusters with small K-band photometric errors. This bimodality becomes less pronounced when including objects with larger errors, or for the (z-K) colour distributions. Deeper observations of large numbers of GCs will be required to reach more secure conclusions. C1 [Chies-Santos, A. L.] Univ Nottingham, Sch Phys & Astron, Nottingham NG7 2RD, England. [Chies-Santos, A. L.; Larsen, S. S.] Univ Utrecht, Astron Inst, NL-3584 Utrecht, Netherlands. [Cantiello, M.] INAF Osservatorio Astron Teramo, I-64100 Teramo, Italy. [Strader, J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Kuntschner, H.] European So Observ, D-85748 Garching, Germany. [Wehner, E. M.] Haverford Coll, Dept Phys & Astron, Haverford, PA 19041 USA. [Brodie, J. P.] Univ Calif Santa Cruz, UCO Lick Observ, Santa Cruz, CA 95064 USA. RP Chies-Santos, AL (reprint author), Univ Nottingham, Sch Phys & Astron, Univ Pk, Nottingham NG7 2RD, England. EM Ana.Chies_Santos@nottingham.ac.uk RI Chies-Santos, Ana/A-2570-2015; OI Kuntschner, Harald/0000-0002-2768-1198; Cantiello, Michele/0000-0003-2072-384X NR 52 TC 27 Z9 27 U1 0 U2 0 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD MAR PY 2012 VL 539 AR A54 DI 10.1051/0004-6361/201117169 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 932AS UT WOS:000303262000061 ER PT J AU Magnelli, B Lutz, D Santini, P Saintonge, A Berta, S Albrecht, M Altieri, B Andreani, P Aussel, H Bertoldi, F Bethermin, M Bongiovanni, A Capak, P Chapman, S Cepa, J Cimatti, A Cooray, A Daddi, E Danielson, ALR Dannerbauer, H Dunlop, JS Elbaz, D Farrah, D Schreiber, NMF Genzel, R Hwang, HS Ibar, E Ivison, RJ Le Floc'h, E Magdis, G Maiolino, R Nordon, R Oliver, SJ Garcia, AP Poglitsch, A Popesso, P Pozzi, F Riguccini, L Rodighiero, G Rosario, D Roseboom, I Salvato, M Sanchez-Portal, M Scott, D Smail, I Sturm, E Swinbank, AM Tacconi, LJ Valtchanov, I Wang, L Wuyts, S AF Magnelli, B. Lutz, D. Santini, P. Saintonge, A. Berta, S. Albrecht, M. Altieri, B. Andreani, P. Aussel, H. Bertoldi, F. Bethermin, M. Bongiovanni, A. Capak, P. Chapman, S. Cepa, J. Cimatti, A. Cooray, A. Daddi, E. Danielson, A. L. R. Dannerbauer, H. Dunlop, J. S. Elbaz, D. Farrah, D. Schreiber, N. M. Foerster Genzel, R. Hwang, H. S. Ibar, E. Ivison, R. J. Le Floc'h, E. Magdis, G. Maiolino, R. Nordon, R. Oliver, S. J. Perez Garcia, A. Poglitsch, A. Popesso, P. Pozzi, F. Riguccini, L. Rodighiero, G. Rosario, D. Roseboom, I. Salvato, M. Sanchez-Portal, M. Scott, D. Smail, I. Sturm, E. Swinbank, A. M. Tacconi, L. J. Valtchanov, I. Wang, L. Wuyts, S. TI A Herschel view of the far-infrared properties of submillimetre galaxies SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE galaxies: evolution; infrared: galaxies; galaxies: starburst; submillimeter: galaxies ID STAR-FORMING GALAXIES; DEEP-FIELD-SOUTH; SPECTRAL ENERGY-DISTRIBUTIONS; DEGREE EXTRAGALACTIC SURVEY; ACTIVE GALACTIC NUCLEI; HIGH-REDSHIFT GALAXIES; SCUBA SUPER-MAP; GOODS-N FIELD; HUBBLE-SPACE-TELESCOPE; 1200-MU-M MAMBO SURVEY AB We study a sample of 61 submillimetre galaxies (SMGs) selected from ground-based surveys, with known spectroscopic redshifts and observed with the Herschel Space Observatory as part of the PACS Evolutionary Probe (PEP) and the Herschel Multi-tiered Extragalactic Survey (HerMES) guaranteed time key programmes. Our study makes use of the broad far-infrared and submillimetre wavelength coverage (100-600 mu m) only made possible by the combination of observations from the PACS and SPIRE instruments aboard the Herschel Space Observatory. Using a power-law temperature distribution model to derive infrared luminosities and dust temperatures, we measure a dust emissivity spectral index for SMGs of beta = 2.0 +/- 0.2. Our results unambiguously unveil the diversity of the SMG population. Some SMGs exhibit extreme infrared luminosities of similar to 10(13)L(circle dot) and relatively warm dust components, while others are fainter (a few times 10(12) L-circle dot) and are biased towards cold dust temperatures. Although at z similar to 2 classical SMGs (>5 mJy at 850 mu m) have large infrared luminosities (similar to 10(13) L-circle dot), objects only selected on their submm flux densities (without any redshift informations) probe a large range in dust temperatures and infrared luminosities. The extreme infrared luminosities of some SMGs (L-IR greater than or similar to 10(12.7) L-circle dot, 26/ 61 systems) imply star formation rates (SFRs) of >500 M-circle dot yr(-1) (assuming a Chabrier IMF and no dominant AGN contribution to the FIR luminosity). Such high SFRs are difficult to reconcile with a secular mode of star formation, and may instead correspond to a merger-driven stage in the evolution of these galaxies. Another observational argument in favour of this scenario is the presence of dust temperatures warmer than that of SMGs of lower luminosities (similar to 40 K as opposed to similar to 25 K), consistent with observations of local ultra-luminous infrared galaxies triggered by major mergers and with results from hydrodynamic simulations of major mergers combined with radiative transfer calculations. Moreover, we find that luminous SMGs are systematically offset from normal star-forming galaxies in the stellar mass-SFR plane, suggesting that they are undergoing starburst events with short duty cycles, compatible with the major merger scenario. On the other hand, a significant fraction of the low infrared luminosity SMGs have cold dust temperatures, are located close to the main sequence of star formation, and therefore might be evolving through a secular mode of star formation. However, the properties of this latter population, especially their dust temperature, should be treated with caution because at these luminosities SMGs are not a representative sample of the entire star-forming galaxy population. C1 [Magnelli, B.; Lutz, D.; Saintonge, A.; Berta, S.; Schreiber, N. M. Foerster; Genzel, R.; Nordon, R.; Poglitsch, A.; Popesso, P.; Rosario, D.; Sturm, E.; Tacconi, L. J.; Wuyts, S.] Max Planck Inst Extraterr Phys, D-85741 Garching, Germany. [Santini, P.; Maiolino, R.] Osserv Astron Roma, INAF, I-00040 Monte Porzio Catone, Italy. [Albrecht, M.; Bertoldi, F.] Argelander Inst Astron, D-53121 Bonn, Germany. [Altieri, B.; Sanchez-Portal, M.; Valtchanov, I.] ESAC, Herschel Sci Ctr, Madrid 28691, Spain. [Andreani, P.] ESO, D-85748 Garching, Germany. [Andreani, P.] Osserv Astron Trieste, INAF, I-34143 Trieste, Italy. [Aussel, H.; Bethermin, M.; Daddi, E.; Dannerbauer, H.; Elbaz, D.; Hwang, H. S.; Le Floc'h, E.; Riguccini, L.] Univ Paris Diderot, CEA, DSM, CNRS,Lab AIM,IRFU,Serv Astrophys,CEA Saclay, F-91191 Gif Sur Yvette, France. [Bongiovanni, A.; Cepa, J.; Perez Garcia, A.] Inst Astrofis Canarias, E-38200 San Cristobal la Laguna, Spain. [Bongiovanni, A.; Cepa, J.; Perez Garcia, A.] Univ La Laguna, Dept Astrofis, E-38207 San Cristobal la Laguna, Spain. [Capak, P.] CALTECH, Pasadena, CA 91125 USA. [Chapman, S.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Cimatti, A.; Pozzi, F.] Univ Bologna, Dipartimento Astron, I-40127 Bologna, Italy. [Cooray, A.] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA. [Danielson, A. L. R.; Smail, I.; Swinbank, A. M.] Univ Durham, Dept Phys, Inst Computat Cosmol, Durham DH1 3LE, England. [Dannerbauer, H.] Univ Vienna, Inst Astron, A-1180 Vienna, Austria. [Dunlop, J. S.; Ivison, R. J.; Roseboom, I.] Univ Edinburgh, Inst Astron, SUPA, Edinburgh EH9 3HJ, Midlothian, Scotland. [Farrah, D.; Oliver, S. J.; Roseboom, I.; Wang, L.] Univ Sussex, Dept Phys & Astron, Ctr Astron, Brighton BN1 9QH, E Sussex, England. [Hwang, H. S.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. [Ibar, E.; Ivison, R. J.] Royal Observ, UK Astron Technol Ctr, Edinburgh EH9 3HJ, Midlothian, Scotland. [Magdis, G.] Univ Oxford, Dept Phys, Oxford OX1 3RH, England. [Rodighiero, G.] Univ Padua, Dipartimento Astron, I-35122 Padua, Italy. [Salvato, M.] Max Planck Inst Plasma Phys, D-85748 Garching, Germany. [Salvato, M.] TUM, Excellence Cluster Universe, D-85748 Garching, Germany. [Scott, D.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada. RP Magnelli, B (reprint author), Max Planck Inst Extraterr Phys, Postfach 1312,Giessenbachstr 1, D-85741 Garching, Germany. EM magnelli@mpe.mpg.de RI Magdis, Georgios/C-7295-2014; Daddi, Emanuele/D-1649-2012; Smail, Ian/M-5161-2013; Bongiovanni, Angel/J-6176-2012; Ivison, R./G-4450-2011; OI Altieri, Bruno/0000-0003-3936-0284; Magdis, Georgios/0000-0002-4872-2294; Daddi, Emanuele/0000-0002-3331-9590; Smail, Ian/0000-0003-3037-257X; Ivison, R./0000-0001-5118-1313; Scott, Douglas/0000-0002-6878-9840; Bethermin, Matthieu/0000-0002-3915-2015; Santini, Paola/0000-0002-9334-8705; Rodighiero, Giulia/0000-0002-9415-2296 FU BMVIT (Austria); ESA-PRODEX (Belgium); CEA/CNES (France); DLR (Germany); ASI/INAF (Italy); CICYT/MCYT (Spain); CSA (Canada); NAOC (China); CEA (France); CNES (France); CNRS (France); ASI (Italy); MCINN (Spain); SNSB (Sweden); STFC (UK); UKSA (UK); NASA (USA); Science and Technology Facilities Council [ST/F002858/1, ST/I000976/1] FX We thank the anonymous referee for suggestions which greatly enhanced this work. We thank C. Hayward for providing us with his simulated SEDs. 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 University of Lethbridge (Canada), NAOC (China), CEA, LAM (France), IFSI, University of Padua (Italy), IAC (Spain), Stockholm Observatory (Sweden), Imperial College London, RAL, UCL-MSSL, UKATC, University of Sussex (UK), Caltech, JPL, NHSC, University of 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). The SPIRE data presented in this paper will be released through the Herschel Database in Marseille HeDaM (hedam.oamp.fr/HerMES). We acknowledge support from the Science and Technology Facilities Council [grant number ST/F002858/1] and [grant number ST/I000976/1]. This study is based on observations made with ESO telescopes at the Paranal and Atacama Observatories under programme numbers: 171.A-3045, 168.A-0485, 082.A-0890 and 183.A-0666. NR 174 TC 103 Z9 103 U1 0 U2 2 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD MAR PY 2012 VL 539 AR A155 DI 10.1051/0004-6361/201118312 PG 35 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 932AS UT WOS:000303262000162 ER PT J AU Martin, S Martin-Pintado, J Montero-Castano, M Ho, PTP Blundell, R AF Martin, S. Martin-Pintado, J. Montero-Castano, M. Ho, P. T. P. Blundell, R. TI Surviving the hole I. Spatially resolved chemistry around Sagittarius A SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE ISM: molecules; ISM: clouds; radio lines: ISM; Galaxy: center; ISM: kinematics and dynamics ID GALACTIC-CENTER REGION; PHOTON-DOMINATED REGIONS; CIRCUMNUCLEAR DISK; SIO EMISSION; IONIZED-GAS; SGR-A; INTERSTELLAR-MEDIUM; MOLECULAR CLOUDS; INFALLING GAS; X-RAY AB Context. The interstellar region within the few central parsecs around the super-massive black hole, Sgr A*, at the very Galactic center is composed of a number of overlapping molecular structures that are subject to one of the most hostile physical environments in the Galaxy. Aims. Through the study of the morphology and kinematics of the emission from different molecular species as well as the variation of their line ratios we can attain a deeper understanding of the distribution and interaction between different gas structures and the energetic phenomena taking place in the surroundings of Sgr A* and of the physical processes responsible for the heating in this region. Methods. We performed high-resolution (4 '' x 3 '' similar to 0.16 x 0.11 pc) interferometric observations of CN, (CN)-C-13, H2CO, SiO, c-C3H2 and HC3N emission at 1.3 mm toward the central similar to 4 pc of the Galactic center region. Results. Strong differences are observed in the distribution of the different molecules. The UV resistant species CN, the only species tracing all previously identified circumnuclear disk (CND) structures, is mostly concentrated in optically thick clumps in the rotating filaments around Sgr A*. H2CO emission traces a shell-like structure that we interpret as the expansion of Sgr A East against the 50 km s(-1) and 20 km s(-1) giant molecular clouds (GMCs). We derive isotopic ratios C-12/C-13 similar to 15-45 across most of the CND region, except for the northeast arm, where the peak of H2CO is observed and ratios < 10 are found. The densest molecular material, traced by SiO and HC3N, is located in the southern CND, likely because of shocked gas infalling from the 20 km s(-1) GMC streamers, and the northeast arm, as a result of the expansion of SgrA East or a connecting point of the 50 km s(-1) streamer east of the CND. The observed c-C3H2/HC3N ratio observed in the region is more than an order of magnitude lower than in Galactic PDRs. Toward the central region only CN was detected in absorption. In addition to the known narrow line-of-sight absorptions, a 90 kms-1 wide optically thick spectral feature is observed. We found evidence of an even wider (> 100 km s(-1)) absorption feature. About 70-75% of the gas mass, concentrated in just the 27% densest molecular clumps, is associated with rotating structures and show evidence of an association with each of the arcs of ionized gas in the mini-spiral structure. Conclusions. These observations provide a combined chemical and kinematical picture of the very central region around Sgr A*. Chemical differentiation has been proven to be a powerful tool to distinguish the many overlapping molecular components in this crowded and heavily obscured region. C1 [Martin, S.] European So Observ, Santiago 19, Chile. [Martin, S.; Ho, P. T. P.; Blundell, R.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Martin-Pintado, J.] Ctr Astrobiol CSIC INTA, Madrid 28850, Spain. [Montero-Castano, M.] Columbia Univ, Dept Astron, New York, NY 10027 USA. [Ho, P. T. P.] Acad Sinica, Inst Astron & Astrophys, Taipei 106, Taiwan. RP Martin, S (reprint author), European So Observ, Alonso de Cordova 3107,Casilla 19001, Santiago 19, Chile. EM smartin@eso.org RI Martin-Pintado, Jesus/H-6107-2015 OI Martin-Pintado, Jesus/0000-0003-4561-3508 FU MICINN [ESP2007-65812-C02-C01, AYA2010-21697-C05-01]; AstroMadrid [CAM S2009/ESP-1496] FX J.M.-P. and S.M. have been supported MICINN through grants ESP2007-65812-C02-C01 and AYA2010-21697-C05-01, and AstroMadrid (CAM S2009/ESP-1496). The authors would like to thank the referee, whose comments helped to significantly improve the paper. NR 58 TC 22 Z9 22 U1 0 U2 0 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD MAR PY 2012 VL 539 AR A29 DI 10.1051/0004-6361/201117268 PG 25 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 932AS UT WOS:000303262000036 ER PT J AU Orellana, M Cieza, LA Schreiber, MR Merin, B Brown, JM Pellizza, LJ Romero, GA AF Orellana, M. Cieza, L. A. Schreiber, M. R. Merin, B. Brown, J. M. Pellizza, L. J. Romero, G. A. TI Transition disks: four candidates for ongoing giant planet formation in Ophiuchus (Research Note) SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE stars: pre-main sequence; protoplanetary disks; submillimeter: planetary systems ID T-TAURI STARS; SPECTRAL ENERGY-DISTRIBUTIONS; CIRCUMSTELLAR DUST DISKS; INNER HOLE; EVOLUTION; OBJECTS; VIEW; SEDS AB Among the large set of Spitzer-selected transitional disks that we have examined in the Ophiuchus molecular, four disks have been identified as (giant) planet-forming candidates based on the morphology of their spectral energy distributions (SEDs), their apparent lack of stellar companions, and evidence of accretion. Here we characterize the structures of these disks modeling their optical, infrared, and (sub) millimeter SEDs. We use the Monte Carlo radiative transfer package RADMC to construct a parametric model of the dust distribution in a flared disk with an inner cavity and calculate the temperature structure that is consistent with the density profile, when the disk is in thermal equilibrium with the irradiating star. For each object, we conducted a Bayesian exploration of the parameter space generating Monte Carlo Markov chains (MCMC) that allow the identification of the best-fit model parameters and to constrain their range of statistical confidence. Our calculations imply that evacuated cavities with radii similar to 2-8 AU are present that appear to have been carved by embedded giant planets. We found parameter values that are consistent with those previously given in the literature, indicating that there has been a mild degree of grain growth and dust settling, which deserves to be investigated with further modeling and follow-up observations. Resolved images with (sub) millimeter interferometers would be required to break some of the degeneracies of the models and more tightly constrain the physical properties of these fascinating disks. C1 [Orellana, M.; Pellizza, L. J.] Consejo Nacl Invest Cient & Tecn, RA-1033 Buenos Aires, DF, Argentina. [Orellana, M.; Schreiber, M. R.; Romero, G. A.] Univ Valparaiso, Dept Fis & Astron, Valparaiso, Chile. [Cieza, L. A.] Univ Hawaii Manoa, Inst Astron, Honolulu, HI 96822 USA. [Merin, B.] European Space Astron Ctr ESA, Herschel Sci Ctr, Villanueva De La Canada 28691, Madrid, Spain. [Brown, J. M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Pellizza, L. J.] Inst Astron & Fis Espacio, RA-1428 Buenos Aires, DF, Argentina. RP Orellana, M (reprint author), Consejo Nacl Invest Cient & Tecn, RA-1033 Buenos Aires, DF, Argentina. EM morellana@fcaglp.unlp.edu.ar OI Merin, Bruno/0000-0002-8555-3012 FU ALMA-CONICYT [31070021]; ANPCyT PICT [2007 00848/Prestamo BID]; Millennium Science Initiative, Chilean ministry of Economy [P10-022-F] FX We acknowledge useful discussions with C. Dullemond and S. Andrews. We thank H. Bouy for explanations. M. O. was supported by ALMA-CONICYT (31070021) and ANPCyT PICT 2007 00848/Prestamo BID. M. R. S. acknowledges support from Millennium Science Initiative, Chilean ministry of Economy: Nucleus P10-022-F. NR 34 TC 4 Z9 4 U1 0 U2 1 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD MAR PY 2012 VL 539 AR A41 DI 10.1051/0004-6361/201117659 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 932AS UT WOS:000303262000048 ER PT J AU Ricci, L Testi, L Maddison, ST Wilner, DJ AF Ricci, L. Testi, L. Maddison, S. T. Wilner, D. J. TI Fomalhaut debris disk emission at 7 millimeters: constraints on the collisional models of planetesimals SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE submillimeter: planetary systems; circumstellar matter ID PROTOPLANETARY DISKS; GRAIN-GROWTH; DUST; EVOLUTION; STARS; BELT; IMAGES; RING AB We present new spatially resolved observations of the dust thermal emission at 7 mm from the Fomalhaut debris disk obtained with the Australia Telescope Compact Array. These observations provide the longest wavelength detection of the Fomalhaut debris disk to date. We combined the new data to literature sub-mm data to investigate the spectral index of the dust thermal emission in the sub-millimeter and constrained the q-slope of the power-law grain size distribution. We derived a value for q = 3.48 +/- 0.14 for grains with sizes around 1 mm. This is consistent with the classical prediction for a collisional cascade at the steady-state. The same value cannot be explained by more recent collisional models of planetesimals in which either the velocity distribution of the large bodies or their tensile strength is a strong function of the body size. C1 [Ricci, L.] CALTECH, Div Phys Math & Astron, Pasadena, CA 91125 USA. [Ricci, L.; Testi, L.] European So Observ, D-85748 Garching, Germany. [Testi, L.] INAF Osservatorio Astrofis Arcetri, I-50125 Florence, Italy. [Maddison, S. T.] Swinburne Univ Technol, Ctr Astrophys & Supercomp, Hawthorn, Vic 3122, Australia. [Wilner, D. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Ricci, L (reprint author), CALTECH, Div Phys Math & Astron, MC 249-17, Pasadena, CA 91125 USA. EM lricci@astro.caltech.edu NR 28 TC 13 Z9 13 U1 1 U2 1 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD MAR PY 2012 VL 539 AR L6 DI 10.1051/0004-6361/201118524 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 932AS UT WOS:000303262000007 ER PT J AU Rygl, KLJ Brunthaler, A Sanna, A Menten, KM Reid, MJ van Langevelde, HJ Honma, M Torstensson, KJE Fujisawa, K AF Rygl, K. L. J. Brunthaler, A. Sanna, A. Menten, K. M. Reid, M. J. van Langevelde, H. J. Honma, M. Torstensson, K. J. E. Fujisawa, K. TI Parallaxes and proper motions of interstellar masers toward the Cygnus X star-forming complex I. Membership of the Cygnus X region SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE stars: formation; astrometry; techniques: interferometric; ISM: general; masers; ISM: kinematics and dynamics ID MASS PROTOSTELLAR CANDIDATES; YOUNG STELLAR OBJECTS; GHZ METHANOL MASERS; TRIGONOMETRIC PARALLAXES; H2O MASERS; MILKY-WAY; GALACTIC ROTATION; VERA ESTIMATION; IRAS SURVEY; DISTANCE AB Context. Whether the Cygnus X complex consists of one physically connected region of star formation or of multiple independent regions projected close together on the sky has been debated for decades. The main reason for this puzzling scenario is the lack of trustworthy distance measurements. Aims. We aim to understand the structure and dynamics of the star-forming regions toward Cygnus X by accurate distance and proper motion measurements. Methods. To measure trigonometric parallaxes, we observed 6.7 GHz methanol and 22 GHz water masers with the European VLBI Network and the Very Long Baseline Array. Results. We measured the trigonometric parallaxes and proper motions of five massive star-forming regions toward the Cygnus X complex and report the following distances within a 10% accuracy: 1.30(-0.07)(+0.07) kpc for W 75N, 1.46(-0.08)(+0.09) kpc for DR 20, 1.50(-0.07)(+0.08) kpc for DR 21, 1.36(-0.11)(+0.12) kpc for IRAS 20290+4052, and 3.33(-0.11)(+0.11) kpc for AFGL 2591. While the distances of W 75N, DR 20, DR 21, and IRAS 20290+4052 are consistent with a single distance of 1.40 +/- 0.08 kpc for the Cygnus X complex, AFGL 2591 is located at a much greater distance than previously assumed. The space velocities of the four star-forming regions in the Cygnus X complex do not suggest an expanding Stromgren sphere. C1 [Rygl, K. L. J.] Ist Fis Spazio Interplanetario INAF IFSI, I-00133 Rome, Italy. [Rygl, K. L. J.; Brunthaler, A.; Sanna, A.; Menten, K. M.] Max Planck Inst Radioastron MPIfR, D-53121 Bonn, Germany. [Brunthaler, A.] Natl Radio Astron Observ, Socorro, NM 87801 USA. [Reid, M. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [van Langevelde, H. J.; Torstensson, K. J. E.] Joint Inst VLBI Europe, NL-7990 AA Dwingeloo, Netherlands. [van Langevelde, H. J.; Torstensson, K. J. E.] Leiden Univ, Sterrewacht Leiden, NL-2300 RA Leiden, Netherlands. [Honma, M.] Natl Inst Nat Sci, Natl Astron Observ Japan, Mizusawa VLBI Observ, Mitaka, Tokyo 1818588, Japan. [Fujisawa, K.] Yamaguchi Univ, Fac Sci, Yamaguchi 7538512, Japan. RP Rygl, KLJ (reprint author), Ist Fis Spazio Interplanetario INAF IFSI, Via Fosso dell Cavaliere 100, I-00133 Rome, Italy. EM kazi.rygl@ifsi-roma.inaf.it; brunthal@mpifr-bonn.mpg.de; asanna@mpifr-bonn.mpg.de; kmenten@mpifr-bonn.mpg.de; reid@cfa.harvard.edu; langevelde@jive.nl; mareki.honma@nao.ac.jp; kalle@strw.leidenuniv.nl; kenta@yamaguchi-u.ac.jp OI van Langevelde, Huib Jan/0000-0002-0230-5946 FU ASI [I/005/07/1]; European Union [275596]; European Research Council [ERC-2009-AdG, 247078] FX We thank Dr. S. Bontemps for his constructive comments, which have greatly improved this manuscript. We are grateful to the staff at JIVE, the EVN antennas, the Japanese VERA network, the Yamaguchi telescope, and the NRAO's VLBA and VLA for carrying out the observations and the correlation of the data. We thank Dr. L. Moscadelli for his maser-plotting scripts. K.L.J.R is funded by an ASI fellowship under contract number I/005/07/1. A. B. was supported by a Marie Curie Outgoing International Fellowship (FP7) of the European Union (project number 275596). Financial support by the European Research Council for the ERC Advanced Grant GLOSTAR (ERC-2009-AdG, Grant Agreement No. 247078) is gratefully acknowledged. NR 68 TC 74 Z9 74 U1 1 U2 3 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD MAR PY 2012 VL 539 AR A79 DI 10.1051/0004-6361/201118211 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 932AS UT WOS:000303262000086 ER PT J AU Sommariva, V Mannucci, F Cresci, G Maiolino, R Marconi, A Nagao, T Baroni, A Grazian, A AF Sommariva, V. Mannucci, F. Cresci, G. Maiolino, R. Marconi, A. Nagao, T. Baroni, A. Grazian, A. TI Stellar metallicity of star-forming galaxies at z similar to 3 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE galaxies: evolution; galaxies: high-redshift ID LYMAN-BREAK GALAXIES; GRAVITATIONALLY LENSED GALAXY; HIGH-REDSHIFT GALAXIES; FRAME OPTICAL-SPECTRA; 8 OCLOCK ARC; MASS-METALLICITY; CHEMICAL ENRICHMENT; ULTRAVIOLET-SPECTRUM; PHYSICAL CONDITIONS; MS 1512-CB58 AB The stellar metallicity is a direct measure of the amount of metals present in a galaxy, since a large part of the metals lie in its stars. In this paper, we investigate new stellar metallicity indicators suitable for high-z galaxies by studying the stellar photospheric absorption lines in the rest-frame ultraviolet, hence sampling predominantly young hot stars. We defined these new indicators based on the equivalent widths (EW) of selected features using theoretical spectra created with the evolutionary population synthesis code Starburst99. We used them to compute the stellar metallicity for a sample of ultraviolet-selected galaxies at z > 3 from the AMAZE (Assessing the Mass-Abundance redshift Evolution) survey using very deep (37 h per object) VLT/FORS spectra. Moreover, we applied these new metallicity indicators to eight additional high redshift galaxies studied in literature. We then compared stellar and gas-phase metallicities measured from the emission lines for all these galaxies, finding that within the errors the two estimates are in good agreement, with possible tendency for stellar metallicities to be lower than the gas phase ones. For the first time, we study the stellar mass-stellar metallicity relation at z > 3. We find that the metallicity of young, hot stars in galaxies at z similar to 3 have similar values of the aged stars in local SDSS galaxies, in contrast to findings for the gas phase metallicity. C1 [Sommariva, V.; Mannucci, F.; Cresci, G.] INAF Osservatorio Astrofis Arcetri, Florence, Italy. [Mannucci, F.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Maiolino, R.; Grazian, A.] INAF Osservatorio Astronom Roma, Monte Porzio Catone, Italy. [Marconi, A.; Baroni, A.] Univ Florence, Dipartimento Astron, Florence, Italy. [Nagao, T.] Kyoto Univ, Kyoto 6068501, Japan. RP Sommariva, V (reprint author), INAF Osservatorio Astrofis Arcetri, Florence, Italy. EM veronica@arcetri.astro.it RI Marconi, Alessandro/C-5880-2009; OI Marconi, Alessandro/0000-0002-9889-4238; mannucci, filippo/0000-0002-4803-2381; Cresci, Giovanni/0000-0002-5281-1417 FU ASI-INAF [I/009/10/0] FX G.C. acknowledges financial support from ASI-INAF grant I/009/10/0. We would like to thank Chuck Steidel for kindly providing his spectrum of MS1512-cB58, and Alice Shapley for her spectra of some lensed galaxies. We thank Max Pettini, Claus Litherer and Federico Biondi for useful comments and suggestions. We are grateful to Niv Drory for providing the masses of the FDF galaxies. NR 90 TC 23 Z9 23 U1 0 U2 0 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD MAR PY 2012 VL 539 AR A136 DI 10.1051/0004-6361/201118134 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 932AS UT WOS:000303262000143 ER PT J AU Toscano, MA Macintyre, IG Lundberg, J AF Toscano, M. A. Macintyre, I. G. Lundberg, J. TI Last interglacial reef limestones, northeastern St. Croix, US Virgin Islands-evidence of tectonic tilting and subsidence since MIS 5.5 SO CORAL REEFS LA English DT Article DE St. Croix-USVI; MIS 5.5; Fossil coral reefs; U-Th dating; Platform tilting ID BRITISH-WEST-INDIES; HOMOTREMA RUBRUM LAMARCK; SEA-LEVEL HIGHSTANDS; CORAL-REEFS; IRONSHORE FORMATION; FLORIDA-KEYS; GRAND-CAYMAN; NETHERLANDS-ANTILLES; FALMOUTH FORMATION; PLEISTOCENE CORAL AB Most last interglacial (MIS 5.5) coral reef deposits in the Caribbean are emergent. However, in St. Croix, these are found mainly at depth, underneath Holocene material and confirmed by TIMS U-Th dated corals from eight cores through Holocene reefs. The only emergent MIS 5.5 marine deposit peaks at +1.5 m MSL at the northwestern end of the island. The Late Pleistocene surface decreases at least 9.25 m (based on reef crest elevations) in elevation over 15 km along a 0.62 m/km eastward (alongshore) slope. Neither differential erosion nor a naturally sloping deposit is likely, thus the directional elevation decrease requires the influence of tectonic processes. Platform tilting or differential subsidence increasing in rate to the east probably operated both during and since the last interglacial and created progressively greater accommodation space for increasingly thicker overlying Holocene reefs in an eastward direction. Rates of subsidence since MIS 5.5 increase from west to east, from 0.02 mm/year to 0.1 mm/year, assuming a MIS 5.5 +6-m sea level and +4 m initial reef elevation. St. Croix's association with extensional shelf faulting from the northern part of the Virgin Islands Basin, the Anegada Fault to the east and the Puerto Rico Trench to the north may be significant in terms of identifying mechanisms for, or past events resulting in, directional tilting. Identification of differential elevations of MIS 5.5 reefs adds substantially to the information on Late Quaternary tectonism of the area. C1 [Toscano, M. A.; Macintyre, I. G.] Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20013 USA. [Lundberg, J.] Carleton Univ, Dept Geog & Environm Studies, Ottawa, ON K1S 5B6, Canada. RP Toscano, MA (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, POB 37012,MRC 121, Washington, DC 20013 USA. EM toscanom@si.edu NR 99 TC 4 Z9 4 U1 1 U2 17 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0722-4028 J9 CORAL REEFS JI Coral Reefs PD MAR PY 2012 VL 31 IS 1 BP 27 EP 38 DI 10.1007/s00338-011-0822-7 PG 12 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA 934NB UT WOS:000303449900003 ER PT J AU Klaus, JS McNeill, DF Budd, AF Coates, AG AF Klaus, J. S. McNeill, D. F. Budd, A. F. Coates, A. G. TI Neogene reef coral assemblages of the Bocas del Toro region, Panama: the rise of Acropora palmata SO CORAL REEFS LA English DT Article DE Neogene; Caribbean; Coral reefs; Panama ID CARIBBEAN REEFS; NETHERLANDS-ANTILLES; COMMUNITY STRUCTURE; OCEAN CIRCULATION; SPECIES TURNOVER; EXTINCTION DEBT; AMERICAN SEAWAY; WESTERN PANAMA; MARINE RECORD; COSTA-RICA AB Temporal patterns are evaluated in Neogene reef coral assemblages from the Bocas del Toro Basin of Panama in order to understand how reef ecosystems respond to long-term environmental change. Analyses are based on a total of 1,702 zooxanthellate coral specimens collected from six coral-bearing units ranging in age from the earliest Late Miocene to the Early Pleistocene: (1) Valiente Formation (12-11 Ma), (2) Fish Hole Member of the Old Bank Formation (5.8-5.6 Ma), (3) La Gruta Member of the Isla Colon Formation (2.2-1.4 Ma), (4) Ground Creek Member of the Isla Colon Formation (2.2-1.4 Ma), (5) Mimitimbi Member of the Urraca Formation (1.2-0.8 Ma), and (6) Hill Point Member of the Urraca Formation (1.2-0.8 Ma). Over 100 coral species occur in the six units, with faunal assemblages ranging from less than 10% extant taxa (Valiente Formation) to over 85% extant taxa (Ground Creek Member). The collections provide new temporal constraints on the emergence of modern Caribbean reefs, with the La Gruta Member containing the earliest occurrence of large monospecific stands of the dominant Caribbean reef coral Acropora palmata, and the Urraca Formation containing the last fossil occurrences of 15 regionally extinct taxa. Canonical correspondence analysis of 41 Late Miocene to Recent reef coral assemblages from the Caribbean region suggests changes in community structure coincident with effective oceanic closure of the Central American Seaway (similar to 3.5 Ma). These changes, including increased Acropora dominance, may have contributed to a protracted period of elevated extinction debt prior to the major peak in regional coral extinctions (similar to 2-1 Ma). C1 [Klaus, J. S.] Univ Miami, Dept Geol Sci, Coral Gables, FL 33124 USA. [McNeill, D. F.] Univ Miami, Rosenstiel Sch Marine & Atmospher Sci, Miami, FL 33149 USA. [Budd, A. F.] Univ Iowa, Dept Geosci, Iowa City, IA 52242 USA. [Coates, A. G.] Smithsonian Trop Res Inst, Balboa, Panama. RP Klaus, JS (reprint author), Univ Miami, Dept Geol Sci, Coral Gables, FL 33124 USA. EM jklaus@rsmas.miami.edu FU ConocoPhillips; Industrial Associates of the Center for Carbonate Research (CSC); National Science Foundation [EAR-0445789] FX Support was provided by ConocoPhillips, the Industrial Associates of the Center for Carbonate Research (CSC), and the National Science Foundation (EAR-0445789). We are grateful to Laura Gillespie and Tiffany Adrain for help with coral collections and the Smithsonian Tropical Research Institute for logistical support. We thank the Government of Panama for permission to collect samples. NR 76 TC 7 Z9 8 U1 1 U2 18 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0722-4028 EI 1432-0975 J9 CORAL REEFS JI Coral Reefs PD MAR PY 2012 VL 31 IS 1 BP 191 EP 203 DI 10.1007/s00338-011-0835-2 PG 13 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA 934NB UT WOS:000303449900020 ER PT J AU Zordan, M Deem, SL Sanchez, CR AF Zordan, Martyn Deem, Sharon L. Sanchez, Carlos R. TI Focal Palatine Erosion in Captive and Free-Living Cheetahs (Acinonyx jubatus) and Other Felid Species SO ZOO BIOLOGY LA English DT Article DE dental disease; molars; palatine disorder; palatine perforation; nondomestic cats AB We examined 1,092 skulls of captive and free-living individuals, representing 33 felid species, to determine the prevalence of focal palatine erosion (FPE). FPE was detected in 3.2% of cats evaluated, including cheetah (Acinonyx jubatus) and 14 other felid species. The prevalence of FPE between cheetah (9.4%; n = 64) and non-cheetah species (2.8%; n = 1,028) (X-2 test; P = 0.004) and between captive (5.7%; n = 246) and free-living (2.4%; n = 824) individuals (X-2 test; P = 0.010) were significantly different, with prevalence between captive (19%; n = 21) and free-living (2.9%; n = 34) cheetahs approaching significance (Fisher's exact test; P = 0.064). FPE was diagnosed with equal prevalence in skulls from individuals in which the lower molars did not meet the palatine bone (60.6%) and individuals in which it did (39.4%; n = 33) (X-2 test; P = 0.139). In cheetahs with FPE, one was a captive animal in Germany, one a free-living cheetah from Mali, one captive cheetah from Kenya, and three captive cheetahs of unknown origin. Additionally, we evaluated the medical records of 49 captive cheetahs in Namibia. Of these cheetahs, 48 (98.0%) had clinical signs consistent with FPE, although only 16 of these 48 (39.6%) had perforation of the palatine bone. Based on physical examinations, FPE was diagnosed in two caracals (Caracal caracal) and one fishing cat (Prionailurus viverrinus) from a North American Zoo. Results from this study confirm FPE in cheetahs outside of Namibia, in a minimum of 15 felid species, and a higher FPE prevalence in captive individuals than free-living ones. Clinical implications of these findings and recommendations for future studies are provided. Zoo Biol 31: 181-188, 2012. (c) 2011 Wiley Periodicals, Inc. C1 [Zordan, Martyn] Univ Chile, Fac Ciencias Vet & Pecuarias, Dept Ciencias Biol Anim, Santiago, Chile. [Deem, Sharon L.] St Louis Zoo, St Louis, MO USA. [Sanchez, Carlos R.] Smithsonian Natl Zool Pk, Washington, DC USA. RP Zordan, M (reprint author), Nuestra Sra Rosario 165, Santiago, Chile. EM mzordan@gmail.com NR 7 TC 1 Z9 1 U1 1 U2 21 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0733-3188 J9 ZOO BIOL JI Zoo Biol. PD MAR-APR PY 2012 VL 31 IS 2 BP 181 EP 188 DI 10.1002/zoo.20392 PG 8 WC Veterinary Sciences; Zoology SC Veterinary Sciences; Zoology GA 931DV UT WOS:000303196300005 PM 21541986 ER PT J AU Pe'er, A Loeb, A AF Pe'er, Asaf Loeb, Abraham TI Constraining sources of ultra high energy cosmic rays using high energy observations with the Fermi satellite SO JOURNAL OF COSMOLOGY AND ASTROPARTICLE PHYSICS LA English DT Article DE ultra high energy cosmic rays; cosmic ray theory; active galactic nuclei ID ACTIVE GALACTIC NUCLEI; NEARBY EXTRAGALACTIC OBJECTS; RADIO GALAXY; PARTICLE-ACCELERATION; POSSIBLE ASSOCIATION; RELATIVISTIC JETS; CENTAURUS-A; SPECTRUM; BURSTS; ORIGIN AB We analyze the conditions that enable acceleration of particles to ultra-high energies, similar to 10(20) eV (UHECRs). We show that broad band photon data recently provided by WMAP, ISOCAM, Swift and Fermi satellites, yield constraints on the ability of active galacticnuclei (AGN) to produce UHECRs. The high energy (MeV-GeV) photons are produced by Compton scattering of the emitted low energy photons and the cosmic microwave background or extra-galactic background light. The ratio of the luminosities at high and low photon energies can therefore be used as a probe of the physical conditions in the acceleration site. We find that existing data excludes core regions of nearby radio-loud AGN as possible acceleration sites of UHECR protons. However, we show that giant radio lobes are not excluded. We apply our method to Cen A, and show that acceleration of protons to similar to 10(20) eV can only occur at distances greater than or similar to 100kpc from the core. C1 [Pe'er, Asaf; Loeb, Abraham] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Pe'er, A (reprint author), Harvard Smithsonian Ctr Astrophys, MS-51,60 Garden St, Cambridge, MA 02138 USA. EM apeer@cfa.harvard.edu; aloeb@cfa.harvard.edu FU NSF [AST-0907890]; NASA [NNX08AL43G, NNA09DB30A] FX We would like to thank Shmulik Balberg, Ramesh Narayan, Uri Keshet, Peter Meszaros and Colin Norman for useful discussions. This work was supported in part by NSF grant AST-0907890 and NASA grants NNX08AL43G and NNA09DB30A. NR 56 TC 9 Z9 9 U1 0 U2 2 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 MAR PY 2012 IS 3 AR 007 DI 10.1088/1475-7516/2012/03/007 PG 10 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA 927ZQ UT WOS:000302949600007 ER PT J AU Watson, CR Li, ZY Polley, NK AF Watson, Casey R. Li, Zhiyuan Polley, Nicholas K. TI Constraining sterile neutrino warm dark matter with Chandra observations of the Andromeda galaxy SO JOURNAL OF COSMOLOGY AND ASTROPARTICLE PHYSICS LA English DT Article DE dark matter theory; X-rays; dark matter experiments ID DWARF SPHEROIDAL GALAXY; X-RAY; MILKY-WAY; SPECTRAL FEATURE; URSA-MINOR; M31; COSMOLOGY; REIONIZATION; ASTROPHYSICS; OSCILLATIONS AB We use the Chandra unresolved X-ray emission spectrum from a 12'-28' (2.8-6.4 kpc) annular region of the Andromeda galaxy to constrain the radiative decay of sterile neutrino warm dark matter. By excising the most baryon-dominated, central 2.8 kpc of the galaxy, we reduce the uncertainties in our estimate of the dark matter mass within the field of view and improve the signal-to-noise ratio of prospective sterile neutrino decay signatures relative to hot gas and unresolved stellar emission. Our findings impose the most stringent limit on the sterile neutrino mass to date in the context of the Dodelson-Widrow model, m(s) < 2.2 keV (95% C.L.). Our results also constrain alternative sterile neutrino production scenarios at very small active-sterile neutrino mixing angles. C1 [Watson, Casey R.; Polley, Nicholas K.] Millikin Univ, Dept Phys & Astron, Decatur, IL 62522 USA. [Li, Zhiyuan] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Watson, CR (reprint author), Millikin Univ, Dept Phys & Astron, Decatur, IL 62522 USA. EM crwatson@millikin.edu; zyli@astro.ucla.edu; npolley@millikin.edu FU Millikin University Department of Physics and Astronomy; SAO [GO0-11098B] FX We thank M. Garcia, S. Murray, and Q.D. Wang, the principal investigators responsible for conducting the Chandra observations of M31 used in this work. We also thank John Beacom and Hasan Yuksel for extensive and very helpful discussions. CRW and NP acknowledge support from the Millikin University Department of Physics and Astronomy. ZL acknowledges support from SAO grant GO0-11098B. NR 114 TC 36 Z9 36 U1 2 U2 2 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 MAR PY 2012 IS 3 AR 018 DI 10.1088/1475-7516/2012/03/018 PG 18 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA 927ZQ UT WOS:000302949600018 ER PT J AU Hollins, H AF Hollins, Hunter TI Atomic Frontier Days HANFORD AND THE AMERICAN WEST SO MONTANA-THE MAGAZINE OF WESTERN HISTORY LA English DT Book Review C1 [Hollins, Hunter] Smithsonian Inst, Natl Air & Space Museum, Washington, DC 20560 USA. RP Hollins, H (reprint author), Smithsonian Inst, Natl Air & Space Museum, Washington, DC 20560 USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU MONTANA HISTORICAL SOC PI HELENA PA 225 N ROBERTS ST, HELENA, MT 59601 USA SN 0026-9891 J9 MONTANA JI Mont.-Mag. West. Hist. PD SPR PY 2012 VL 62 IS 1 BP 76 EP 77 PG 2 WC History SC History GA 930WN UT WOS:000303175500014 ER PT J AU Swenson, NG Stegen, JC Davies, SJ Erickson, DL Forero-Montana, J Hurlbert, AH Kress, WJ Thompson, J Uriarte, M Wright, SJ Zimmerman, JK AF Swenson, Nathan G. Stegen, James C. Davies, Stuart J. Erickson, David L. Forero-Montana, Jimena Hurlbert, Allen H. Kress, W. John Thompson, Jill Uriarte, Maria Wright, S. Joseph Zimmerman, Jess K. TI Temporal turnover in the composition of tropical tree communities: functional determinism and phylogenetic stochasticity SO ECOLOGY LA English DT Article DE beta diversity; community dynamics; community phylogenetics; functional ecology; functional traits; neutral theory; Panama; Puerto Rico; tropical forest ID NEOTROPICAL FOREST; LAND-USE; DIVERSITY; PATTERNS; TRAITS; MAINTENANCE; MECHANISMS; WORLDWIDE; ALIGNMENT; DYNAMICS AB The degree to which turnover in biological communities is structured by deterministic or stochastic factors and the identities of influential deterministic factors are fundamental, yet unresolved, questions in ecology. Answers to these questions are particularly important for projecting the fate of forests with diverse disturbance histories worldwide. To uncover the processes governing turnover we use species-level molecular phylogenies and functional trait data sets for two long-term tropical forest plots with contrasting disturbance histories: one forest is older-growth, and one was recently disturbed. Having both phylogenetic and functional information further allows us to parse out the deterministic influences of different ecological filters. With the use of null models we find that compositional turnover was random with respect to phylogeny on average, but highly nonrandom with respect to measured functional traits. Furthermore, as predicted by a deterministic assembly process, the older-growth and disturbed forests were characterized by less than and greater than expected functional turnover, respectively. These results suggest that the abiotic environment, which changes due to succession in the disturbed forest, strongly governs the temporal dynamics of disturbed and undisturbed tropical forests. Predicting future changes in the composition of disturbed and undisturbed forests may therefore be tractable when using a functional-trait-based approach. C1 [Swenson, Nathan G.] Michigan State Univ, Dept Plant Biol, E Lansing, MI 48824 USA. [Stegen, James C.; Hurlbert, Allen H.] Univ N Carolina, Dept Biol, Chapel Hill, NC 27599 USA. [Stegen, James C.] Pacific NW Natl Lab, Fundamental & Computat Sci Directorate, Div Biol Sci, Richland, WA 99352 USA. [Davies, Stuart J.] Harvard Univ, Ctr Trop Forest Sci, Cambridge, MA 02138 USA. [Davies, Stuart J.; Wright, S. Joseph] Smithsonian Trop Res Inst, Balboa Ancon, Panama. [Erickson, David L.; Kress, W. John] Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, Washington, DC 20013 USA. [Forero-Montana, Jimena; Thompson, Jill; Zimmerman, Jess K.] Univ Puerto Rico, Inst Trop Ecosyst Studies, Rio Piedras, PR 00931 USA. [Thompson, Jill] Ctr Ecol & Hydrol, Penicuik EH26 0QB, Midlothian, Scotland. [Uriarte, Maria] Columbia Univ, Dept Ecol Evolut & Environm Biol, New York, NY 10027 USA. RP Swenson, NG (reprint author), Michigan State Univ, Dept Plant Biol, E Lansing, MI 48824 USA. EM swensonn@msu.edu RI Thompson, Jill/K-2200-2012; Swenson, Nathan/A-3514-2012; Uriarte, Maria/L-8944-2013; Wright, Stuart/M-3311-2013; Stegen, James/Q-3078-2016 OI Thompson, Jill/0000-0002-4370-2593; Swenson, Nathan/0000-0003-3819-9767; Wright, Stuart/0000-0003-4260-5676; Stegen, James/0000-0001-9135-7424 FU F. H. Levinson Fund; Center for Tropical Forest Science; Smithsonian Institution; National Science Foundation [BSR-9015961, DEB-0516066, BSR-88111902, DEB-9411973, DEB-008538]; Mellon Foundation; Smithsonian Tropical Research Institute; John D. and Catherine T. MacArthur Foundation; Celera Foundation; National Science Foundation. [DEB-0218039, DEB-0620910, DEB-0640386, DEB-0425651, DEB-0346488, DEB-0129874, DEB-00753102, DEB-9909347, DEB-9615226, DEB-9405933, DEB-9221033, DEB-9100058, DEB-8906869, DEB-8605042, DEB-8206992, DEB-7922197, DBI-0906005] FX N. G. Swenson and J. C. Stegen contributed equally to this paper. We thank R. Condit for discussions regarding the dynamics of the BCI forest dynamics plot. The collection of plant material for DNA sequencing and trait quantification was funded by the F. H. Levinson Fund for BCI and a Center for Tropical Forest Science research grant awarded to N. G. Swenson for Luquillo. DNA barcode sequencing and analyses were supported by funds from the Smithsonian Institution Global Earth Observatories project. The Luquillo forest plot has been supported by National Science Foundation grants (BSR-9015961 and DEB-0516066) and from the Mellon Foundation. National Science Foundation funds to the Luquillo Long-Term Ecology Research Site (BSR-88111902, DEB-9411973, DEB-008538, DEB-0218039, and DEB-0620910) also supported this work. The BCI forest dynamics research project was made possible by National Science Foundation grants to Stephen P. Hubbell: DEB-0640386, DEB-0425651, DEB-0346488, DEB-0129874, DEB-00753102, DEB-9909347, DEB-9615226, DEB-9615226, DEB-9405933, DEB-9221033, DEB-9100058, DEB-8906869, DEB-8605042, DEB-8206992, DEB-7922197, support from the Center for Tropical Forest Science, the Smithsonian Tropical Research Institute, the John D. and Catherine T. MacArthur Foundation, the Mellon Foundation, the Celera Foundation, numerous private individuals, and through the hard work of over 100 people from 10 countries over the past two decades. Both forest plots are part of the Center for Tropical Forest Science, a global network of large-scale demographic tree plots. J. C. Stegen was supported by an NSF Postdoctoral Fellowship in Bioinformatics (DBI-0906005). NR 39 TC 50 Z9 53 U1 8 U2 112 PU ECOLOGICAL SOC AMER PI WASHINGTON PA 1990 M STREET NW, STE 700, WASHINGTON, DC 20036 USA SN 0012-9658 J9 ECOLOGY JI Ecology PD MAR PY 2012 VL 93 IS 3 BP 490 EP 499 PG 10 WC Ecology SC Environmental Sciences & Ecology GA 928CJ UT WOS:000302957300007 PM 22624204 ER PT J AU Harlow, GE Tsujimori, T Sorensen, SS AF Harlow, George E. Tsujimori, Tatsuki Sorensen, Sorena S. TI Introduction SO EUROPEAN JOURNAL OF MINERALOGY LA English DT Editorial Material C1 [Harlow, George E.] Amer Museum Nat Hist, New York, NY 10024 USA. [Tsujimori, Tatsuki] Okayama Univ, Misasa, Tottori, Japan. [Sorensen, Sorena S.] Smithsonian Inst, Washington, DC 20560 USA. RP Harlow, GE (reprint author), Amer Museum Nat Hist, New York, NY 10024 USA. RI Tsujimori, Tatsuki/D-2677-2009 OI Tsujimori, Tatsuki/0000-0001-9202-7312 NR 11 TC 4 Z9 4 U1 1 U2 3 PU E SCHWEIZERBARTSCHE VERLAGS PI STUTTGART PA NAEGELE U OBERMILLER, SCIENCE PUBLISHERS, JOHANNESSTRASSE 3A, D 70176 STUTTGART, GERMANY SN 0935-1221 J9 EUR J MINERAL JI Eur. J. Mineral. PD MAR PY 2012 VL 24 IS 2 BP 197 EP 198 DI 10.1127/0935-1221/2012/0024-2196 PG 2 WC Mineralogy SC Mineralogy GA 926EO UT WOS:000302814300001 ER PT J AU Neilsen, J Petschek, AJ Lee, JC AF Neilsen, Joseph Petschek, Andrew J. Lee, Julia C. TI Accretion disc wind variability in the states of the microquasar GRS 1915+105 SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE accretion, accretion discs; black hole physics; instabilities; stars: winds, outflows; X-rays: binaries; X-rays: individual: GRS 1915+105 ID TRANSMISSION GRATING SPECTROMETER; ABSORPTION-LINE FEATURES; COMPTON-HEATED WINDS; X-RAY; JET INTERACTION; RADIO-EMISSION; UNIFIED MODEL; CIRCINUS X-1; GRS-1915+105; CHANDRA AB Continuing our study of the role and evolution of accretion disc winds in the microquasar GRS 1915+105, we present high-resolution spectral variability analysis of the beta and gamma states with the Chandra High-Energy Transmission Grating Spectrometer. By tracking changes in the absorption lines from the accretion disc wind, we find new evidence that radiation links the inner and outer accretion discs on a range of time-scales. As the central X-ray flux rises during the high-luminosity gamma state, we observe the progressive overionization of the wind. In the beta state, we argue that changes in the inner disc leading to the ejection of a transient 'baby jet' also quench the highly ionized wind from the outer disc. Our analysis reveals how the state, structure and X-ray luminosity of the inner accretion disc all conspire to drive the formation and variability of highly ionized accretion disc winds. C1 [Neilsen, Joseph] MIT Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Neilsen, Joseph; Petschek, Andrew J.; Lee, Julia C.] Harvard Univ, Dept Astron, Cambridge, MA 02138 USA. [Neilsen, Joseph; Lee, Julia C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Neilsen, J (reprint author), MIT Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. EM jneilsen@space.mit.edu RI Lee, Julia/G-2381-2015; OI Lee, Julia/0000-0002-7336-3588; Neilsen, Joseph/0000-0002-8247-786X FU Chandra grant [AR0-11004X]; Harvard University Graduate School of Arts and Sciences; Harvard University Faculty of Arts and Sciences; National Aeronautics and Space Administration [SV3-73016]; National Aeronautics Space Administration [NAS8-03060] FX We thank the referee for comments that improved the clarity of our presentation. We thank Ron Remillard and Claude Canizares for helpful discussions of spectral variability. JN and JCL gratefully acknowledge funding support from Chandra grant AR0-11004X, the Harvard University Graduate School of Arts and Sciences, and the Harvard University Faculty of Arts and Sciences. JN acknowledges additional support from the National Aeronautics and Space Administration through the Smithsonian Astrophysical Observatory contract SV3-73016 to MIT for support of the Chandra Xray Center, which is operated by the Smithsonian Astrophysical Observatory for and on behalf of the National Aeronautics Space Administration under contract NAS8-03060. This research made use of data obtained from the High Energy Astrophysics Science Archive Research Center (HEASARC), provided by NASA's Goddard Space Flight Center. NR 61 TC 16 Z9 16 U1 0 U2 0 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD MAR PY 2012 VL 421 IS 1 BP 502 EP 511 DI 10.1111/j.1365-2966.2011.20329.x PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 924LQ UT WOS:000302693600072 ER PT J AU Pandge, MB Vagshette, ND David, LP Patil, MK AF Pandge, M. B. Vagshette, N. D. David, L. P. Patil, M. K. TI Systematic study of X-ray cavities in the brightest galaxy in the Draco constellation NGC 6338 SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies: active; galaxies: clusters: individual: NGC 6338; galaxies: general; intergalactic medium; X-rays: galaxies: clusters ID CENTRAL CLUSTER GALAXIES; COOLING FLOWS; STAR-FORMATION; CHANDRA OBSERVATION; RADIO-SOURCES; COLD FRONTS; HOT GAS; FEEDBACK; NUCLEUS; BUBBLES AB We present results based on the systematic analysis of currently available Chandra archive data on the brightest galaxy in the Draco constellation, NGC 6338, in order to investigate the properties of the X-ray cavities. In the central similar to 6 kpc, at least two, possibly three, X-ray cavities are evident. All these cavities are roughly of ellipsoidal shape and show a decrement in surface brightness of several tens of per cent. In addition to these cavities, a set of X-ray bright filaments are also noticed which are spatially coincident with the H alpha filaments over an extent of 15 kpc. The H alpha emission-line filaments are perpendicular to the X-ray cavities. Spectroscopic analysis of the hot gas in the filaments and cavities reveals that the X-ray filaments are cooler than the gas contained in the cavities. The emission-line ratios and the extended, asymmetric nature of the H alpha emission-line filaments seen in this system require a harder ionizing source than that produced by star formation and/or young, massive stars. Radio emission maps derived from the analysis of 1.4-GHz Very Large Array Faint Images of the Radio Sky at Twenty-Centimeters survey data failed to show any association of these X-ray cavities with radio jets; however, the cavities are filled by radio emission. The total power of the cavities is 17 x 10(42) erg s(-1) and the ratio of radio luminosity to cavity power is similar to 10(-4), implying that most of the jet power is mechanical. C1 [Pandge, M. B.; Vagshette, N. D.; Patil, M. K.] Swami Ramanand Teerth Marathwada Univ, Sch Phys Sci, Nanded 431606, India. [David, L. P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Pandge, MB (reprint author), Swami Ramanand Teerth Marathwada Univ, Sch Phys Sci, Nanded 431606, India. EM patil@iucaa.ernet.in FU Indian Space Research Organisation, Bangalore, through RESPOND, Department of Space, Government of India [9/211/2005-II] FX We thank Dr Joydeep Bagchi for providing the radio emission map from the analysis of FIRST survey radio data on NGC 6338. NDV gratefully acknowledges support by the Indian Space Research Organisation, Bangalore, through RESPOND scheme file No. 9/211/2005-II, Department of Space, Government of India. MBP, NDV and MKP acknowledge the use of computing and library facilities of the Inter-University Centre for Astronomy and Astrophysics, Pune, India. This work has made use of data from the Chandra archive, SDSS, GALEX, NASA's Astrophysics Data System, NASA/IPAC Extragalactic Database, and software provided by CXC. Optical images used in this work are obtained from the Hubble Legacy Archive, which is a collaboration between the Space Telescope Science Institute (NASA), Space Telescope European Coordinating Facility (ESA) and Canadian Astronomy Data Centre (NRC/CSA). NR 43 TC 14 Z9 14 U1 0 U2 3 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD MAR PY 2012 VL 421 IS 1 BP 808 EP 817 DI 10.1111/j.1365-2966.2011.20358.x PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 924LQ UT WOS:000302693600095 ER PT J AU Cacciato, M Dekel, A Genel, S AF Cacciato, Marcello Dekel, Avishai Genel, Shy TI Evolution of violent gravitational disc instability in galaxies: late stabilization by transition from gas to stellar dominance SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE methods: analytical; galaxies: evolution; galaxies: formation; galaxies: haloes; galaxies: spiral; galaxies: star formation ID SIMILAR-TO 2; STAR-FORMATION LAW; INTEGRAL FIELD SPECTROSCOPY; N-BODY SIMULATIONS; LY-ALPHA EMISSION; HIGH-REDSHIFT; COLD STREAMS; SINS SURVEY; COSMOLOGICAL SIMULATIONS; MILLENNIUM SIMULATION AB We address the cosmological evolution of violent gravitational instability in high-redshift, massive, star-forming galactic discs. To this aim, we integrate in time the equations of mass and energy conservation under self-regulated instability of a two-component disc of gas and stars. The disc is assumed to be continuously fed by cold gas at the average cosmological rate. The gas forms stars and is partly driven away by stellar feedback. The gas and stars flow inward through the disc to a central bulge due to torques that drive angular momentum outwards. The gravitational energy released by the mass inflow down the gravitational potential gradient drives the disc turbulence that maintains the disc unstable with a Toomre instability parameter Q similar to 1, compensating for the dissipative losses of the gas turbulence and raising the stellar velocity dispersion. We follow the velocity dispersion of stars and gas as they heat and cool, respectively, and search for disc 'stabilization', to be marked by a low gas velocity dispersion comparable to the speed of sound similar to 10 km s(-1). We vary the model parameters that characterize the accreted gas fraction, turbulence dissipation rate, star formation rate and stellar feedback. We find that as long as the gas input roughly follows the average cosmological rate, the disc instability is a robust phenomenon at high redshift till z similar to 1, driven by the high surface density and high gas fraction due to the intense cosmological accretion. For a broad range of model parameter values, the discs tend to 'stabilize' at z similar to 0-0.5 as they become dominated by hot stars. When the model parameters are pushed to extreme values, the discs may stabilize as early as z similar to 2, with the gas loss by strong outflows serving as the dominant stabilizing factor. C1 [Cacciato, Marcello; Dekel, Avishai] Hebrew Univ Jerusalem, Racah Inst Phys, IL-91904 Jerusalem, Israel. [Genel, Shy] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Genel, Shy] Tel Aviv Univ, Sch Phys & Astron, IL-69978 Tel Aviv, Israel. [Genel, Shy] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. RP Cacciato, M (reprint author), Hebrew Univ Jerusalem, Racah Inst Phys, IL-91904 Jerusalem, Israel. EM cacciato@phys.huji.ac.il OI Genel, Shy/0000-0002-3185-1540 FU ISF [6/08]; GIF [G-1052-104.7/2009]; DIP; NSF at UCSC [AST-1010033]; Max-Planck Gesellschaft FX We acknowledge stimulating discussions with Frederic Bournaud, Andi Burkert, Daniel Ceverino, John Forbes and Mark Krumholz. This work has been supported by the ISF through grant 6/08, by GIF through grant G-1052-104.7/2009, by a DIP grant and by an NSF grant AST-1010033 at UCSC. MC has been supported at HU by a Minerva fellowship (Max-Planck Gesellschaft). MC acknowledges the hospitality of the Dublin Institute for Advanced Studies and, together with AD, that of the Astronomy Department at UCSC. NR 70 TC 53 Z9 53 U1 0 U2 1 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD MAR PY 2012 VL 421 IS 1 BP 818 EP 831 DI 10.1111/j.1365-2966.2011.20359.x PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 924LQ UT WOS:000302693600096 ER PT J AU Tirsch, D Craddock, RA Platz, T Maturilli, A Helbert, J Jaumann, R AF Tirsch, Daniela Craddock, Robert Anthony Platz, Thomas Maturilli, Alessandro Helbert, Joern Jaumann, Ralf TI Spectral and petrologic analyses of basaltic sands in Ka'u Desert (Hawaii) - implications for the dark dunes on Mars SO EARTH SURFACE PROCESSES AND LANDFORMS LA English DT Article DE Mars; dunes; aeolian processes; terrestrial analogs; spectroscopy ID EMISSION SPECTROMETER DATA; SOIL ANALOG MATERIALS; KILAUEA VOLCANO; REFLECTANCE SPECTROSCOPY; SURFACE COMPOSITIONS; MERIDIANI-PLANUM; MARTIAN SURFACE; PARTICLE-SIZE; LANDING SITE; GUSEV CRATER AB Dark aeolian deposits on Mars are thought to consist of volcanic materials due to their mineral assemblages, which are common to basalts. However, the sediment source is still debated. Basaltic dunes on Earth are promising analogs for providing further insights into the assumed basaltic sand dunes on Mars. In our study we characterize basaltic dunes from the Ka'u Desert in Hawaii using optical microscopes, electron microprobe, and spectral analyses. We compare the spectra of terrestrial and Martian dune sands to determine possible origins of the Martian dark sediments. Our results show that the terrestrial sands consist primarily of medium to coarse sand-sized volcanic glass and rock fragments as well as olivine, pyroxene, and plagioclase minerals. Grain shapes range from angular to subrounded. The sample composition indicates that the material was derived from phreatomagmatic eruptions partially with additional proportions of rock fragments from local lava flows. Grain shape and size indicate the materials were transported by aeolian processes rather than by fluvial processes. Spectral analyses reveal an initial hydration of all terrestrial samples. A spectral mineralogical correlation between the terrestrial and Martian aeolian sands shows a similarity consistent with an origin from volcanic ash and lava. We suggest that the Martian deposits may contain similar abundances of volcanic glass, which has not yet been distinguished in Martian spectral data. Copyright (C) 2011 John Wiley & Sons, Ltd. C1 [Tirsch, Daniela; Maturilli, Alessandro; Helbert, Joern; Jaumann, Ralf] German Aerosp Ctr DLR, Inst Planetary Res, D-12489 Berlin, Germany. [Craddock, Robert Anthony] Smithsonian Inst, Natl Air & Space Museum, Ctr Earth & Planetary Studies, Washington, DC 20560 USA. [Platz, Thomas; Jaumann, Ralf] Freie Univ, Dept Geol Sci, Berlin, Germany. RP Tirsch, D (reprint author), German Aerosp Ctr DLR, Inst Planetary Res, Rutherfordstr 2, D-12489 Berlin, Germany. EM daniela.tirsch@dlr.de RI Tirsch, Daniela/I-7916-2012; Craddock, Robert/B-3884-2013; Platz, Thomas/F-7539-2013; OI Platz, Thomas/0000-0002-1253-2034; Helbert, Jorn/0000-0001-5346-9505; Tirsch, Daniela/0000-0001-5905-5426 FU NASA [NNX09AC27G]; George F. Becker Endowment at the Smithsonian Institution; Helmholtz Association FX This research and fieldwork has been supported by NASA's Mars Fundamental Research Program, Grant NNX09AC27G, funds from the George F. Becker Endowment at the Smithsonian Institution, and by the Helmholtz Association through the research alliance 'Planetary Evolution and Life'. The authors thank Daniel Spengler (Helmholtz Centre Potsdam GFZ German Research Center for Geosciences, Potsdam) for valuable assistance with the ASD spectral measurements and Mirjam Langhans (DLR Berlin/INAF-IASF Rome) for priceless field support. The authors acknowledge the reviews of Janice Bishop and Vincenzo Orofino that significantly improved this paper. NR 95 TC 10 Z9 10 U1 3 U2 25 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0197-9337 EI 1096-9837 J9 EARTH SURF PROC LAND JI Earth Surf. Process. Landf. PD MAR PY 2012 VL 37 IS 4 BP 434 EP 448 DI 10.1002/esp.2266 PG 15 WC Geography, Physical; Geosciences, Multidisciplinary SC Physical Geography; Geology GA 909RE UT WOS:000301581100007 ER PT J AU Pekar, S Coddington, JA Blackledge, TA AF Pekar, Stano Coddington, Jonathan A. Blackledge, Todd A. TI EVOLUTION OF STENOPHAGY IN SPIDERS (ARANEAE): EVIDENCE BASED ON THE COMPARATIVE ANALYSIS OF SPIDER DIETS SO EVOLUTION LA English DT Review DE Polyphagy; predator; prey; prey specificity; trophic niche ID ORB-WEAVING SPIDERS; PREY-CAPTURE TECHNIQUES; WEB-BUILDING SPIDERS; TETRAGNATHA-LABORIOSA ARANEAE; MYRMECOPHAGIC JUMPING SPIDER; WINTER-WHEAT FIELDS; ANT-EATING SPIDERS; IMPORTED FIRE ANT; PREDATORY BEHAVIOR; NATURAL-HISTORY AB Stenophagy (narrow diet breadth) represents an extreme of trophic specialization in carnivores, but little is known about the forces driving its evolution. We used spiders, the most diversified group of terrestrial predators, to investigate whether stenophagy (1) promoted diversification; (2) was phylogenetically conserved and evolutionarily derived state; and (3) was determined either by geographical distribution and foraging guild. We used published data on the prey of almost 600 species. Six categories of stenophagy were found: myrmecophagy, araneophagy, lepidopterophagy, termitophagy, dipterophagy, and crustaceophagy. We found that the species diversity of euryphagous genera and families was similar to stenophagous genera and families. At the family level, stenophagy evolved repeatedly and independently. Within families, the basal condition was oligophagy or euryphagy. Most types of stenophagy were clearly derived: myrmecophagy in Zodariidae; lepidopterophagy in Araneidae; dipterophagy in Theridiidae. In contrast, araneophagy was confined to basal and intermediate lineages, suggesting its ancestral condition. The diet breadth of species from the tropics and subtropics was less diverse than species from the temperate zone. Diet breadth was lower in cursorial spiders compared to web-building species. Thus, the evolution of stenophagy in spiders appears to be complex and governed by phylogeny as well as by ecological determinants. C1 [Pekar, Stano] Masaryk Univ, Fac Sci, Dept Bot & Zool, Brno 61137, Czech Republic. [Coddington, Jonathan A.] Smithsonian Natl Museum Nat Hist, Washington, DC 20013 USA. [Blackledge, Todd A.] Univ Akron, Dept Biol, Akron, OH 44325 USA. [Blackledge, Todd A.] Univ Akron, Integrated Biosci Program, Akron, OH 44325 USA. RP Pekar, S (reprint author), Masaryk Univ, Fac Sci, Dept Bot & Zool, Kotlarska 2, Brno 61137, Czech Republic. EM pekar@sci.muni.cz OI Pekar, Stano/0000-0002-0197-5040 FU Ministry of Education, Youth and Sports of the Czech Republic [MSM0021622416]; NSF [IOS-0745379] FX We thank the following colleagues for providing us their unpublished data or rare literature on the diet of spiders: L. Fernandez Garcia, D. Logunov, S. Korenko, and K. Rehakova. J. Bosselaers, W. P. Maddison, I. Agnarsson, N. Scharff, and B. Suresh are thanked for very valuable advice on the position of unresolved genera and the phylogeny of particular families. At last but not least, we thank two anonymous reviewers and the editor for useful comments. The study was supported by the grant no. MSM0021622416 provided by the Ministry of Education, Youth and Sports of the Czech Republic to S. Pekar and NSF IOS-0745379 to T. Blackledge. NR 474 TC 22 Z9 23 U1 2 U2 53 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0014-3820 EI 1558-5646 J9 EVOLUTION JI Evolution PD MAR PY 2012 VL 66 IS 3 BP 776 EP 806 DI 10.1111/j.1558-5646.2011.01471.x PG 31 WC Ecology; Evolutionary Biology; Genetics & Heredity SC Environmental Sciences & Ecology; Evolutionary Biology; Genetics & Heredity GA 900ZN UT WOS:000300931400014 PM 22380440 ER PT J AU Ortner, DJ Ponce, P Ogden, A Buckberry, J AF Ortner, Donald J. Ponce, Paola Ogden, Alan Buckberry, Jo TI Multicentric osteosarcoma associated with DISH, in a 19th century burial from England SO INTERNATIONAL JOURNAL OF OSTEOARCHAEOLOGY LA English DT Article DE osteosarcoma; paleopathology; England; DISH ID SKELETAL AGE; DEATH AB Osteosarcoma is a rare type of malignant neoplasm that is most frequent in adolescents and young adults although it can develop at any age. It can metastasize from a primary site in bone to other bones and soft tissues. Usually the disorder causes a single bone-forming lesion (unicentric) but some cases have multicentric, bone-forming lesions. Some of these lesions develop at different sites at different times. In a second variant of multicentric osteosarcoma, synchronous bone-forming lesions develop at multiple sites. Distinguishing between these two types of multicentric osteosarcoma is challenging in a clinical context and the criteria for doing so are unlikely to be met in an archaeological burial. Wolverhampton burial HB 39 was excavated from an early-nineteenth century cemetery site in England. It consists of the incomplete skeleton of an adult male of at least 45 years of age with multicentric osteosarcoma. The individual represented by this burial also had diffuse idiopathic skeletal hyperostosis (DISH). Three of the bone-forming lesions associated with osteosarcoma developed on the bony outgrowths related to DISH. Copyright (c) 2010 John Wiley & Sons, Ltd. C1 [Ortner, Donald J.] Smithsonian Inst, Natl Museum Nat Hist, Dept Anthropol, Washington, DC 20560 USA. [Ortner, Donald J.; Ogden, Alan; Buckberry, Jo] Univ Bradford, Biol Anthropol Res Ctr, Bradford BD7 1DP, W Yorkshire, England. [Ponce, Paola] Univ Durham, Dept Archaeol, Durham DH1 3LE, England. RP Ortner, DJ (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Anthropol, Washington, DC 20560 USA. EM ortner@si.edu NR 25 TC 3 Z9 3 U1 9 U2 16 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 1047-482X J9 INT J OSTEOARCHAEOL JI Int. J. Osteoarchaeol. PD MAR-APR PY 2012 VL 22 IS 2 BP 245 EP 252 DI 10.1002/oa.1196 PG 8 WC Anthropology; Archaeology SC Anthropology; Archaeology GA 923KQ UT WOS:000302618600011 ER PT J AU Zona, S Davis, P Gunathilake, LAAH Prince, J Horn, JW AF Zona, Scott Davis, Philip Gunathilake, L. A. A. H. Prince, Jeffery Horn, James W. TI Seeds of Eriocaulaceae of the United States and Canada SO CASTANEA LA English DT Article DE Eriocaulaceae; Eriocaulon; Lachnocaulon; seed; scanning electron microscopy; Syngonanthus ID RUHLAND ERIOCAULACEAE; COAT MORPHOLOGY; EMBRYOLOGY AB A study of seed coat micromorphology, using both light microscopy and scanning electron microscopy, revealed characters of taxonomic significance and utility among the species of Eriocaulaceae of the United States and Canada. Our survey of nine native species of Eriocaulon, five Lachnocaulon, and one Syngonanthus revealed diversity in the shape and size of the cells of the seed coat, the degree and pattern of ornamentation, and appendage shape. In the context of world Eriocaulaceae, the species of the United States and Canada exhibit no morphologies that are unique. C1 [Zona, Scott] Florida Int Univ, Dept Biol Sci OE 167, Miami, FL 33199 USA. [Davis, Philip; Gunathilake, L. A. A. H.; Prince, Jeffery] Univ Miami, Dept Biol, Dauer Elect Microscopy Lab, Coral Gables, FL 33124 USA. [Horn, James W.] Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, Washington, DC 20013 USA. RP Zona, S (reprint author), Florida Int Univ, Dept Biol Sci OE 167, 11200 SW 8 St, Miami, FL 33199 USA. EM zonas@fiu.edu NR 25 TC 4 Z9 4 U1 0 U2 4 PU SOUTHERN APPALACHIAN BOTANICAL SOC, NEWBERRY COLL PI NEWBERRY PA DEPT BIOLOGY, C/O CHARLES N HORN, SECRETARY-TREASURER, 2100 COLLEGE ST, NEWBERRY, SC 29108 USA SN 0008-7475 J9 CASTANEA JI Castanea PD MAR PY 2012 VL 77 IS 1 BP 37 EP 45 DI 10.2179/11-032 PG 9 WC Plant Sciences SC Plant Sciences GA 918VJ UT WOS:000302279100005 ER PT J AU Alexander, SN Hayek, LAC Weeks, A AF Alexander, Sara N. Hayek, Lee-Ann C. Weeks, Andrea TI A Subspecific Revision of North American Saltmarsh Mallow Kosteletzkya pentacarpos (L.) Ledeb. (Malvaceae) SO CASTANEA LA English DT Article DE Discriminant analysis; infraspecific; Kosteletzkya pentacarpos; lectotype; morphometric; revision; smilacifolia ID HIBISCEAE AB Kosteletzkya pentacarpos (L.) Ledeb. (syn. = Kosteletzkya virginica (L.) C. Presl ex A. Gray) has been treated as a single variable species or as a species including four varieties: K. virginica var. althaeifolia, var. aquilonia, var. smilacifolia, and var. virginica. The aim of this study was to test the validity of formally recognizing these putative infraspecific taxa with a statistical analysis of morphological data. Loans were received from 15 herbaria, for 1,114 specimens; 224 were selected. Measurements were taken from these 224 specimens for 42 characters and analyzed by canonical discriminant analysis, which recognized two dimensions. Var. smilacifolia and var. aquilonia were separated from the other two groupings and correctly predicted at 100%. Var. smilacifolia is morphologically distinct from the other taxa in having linear hastate leaves with reflexed linear lobes, an unbranched inflorescence, a slender stem, and a mostly entire leaf margin. A new combination is proposed: Kosteletzkya pentacarpos (L.) Ledeb. var. smilacifolia (Chapm.) S.N. Alexander. All other former putative infraspecific taxa are synonymous with Kosteletzkya pentacarpos var. pentacarpos. C1 [Alexander, Sara N.; Weeks, Andrea] George Mason Univ, Dept Environm Sci & Policy, Fairfax, VA 22030 USA. [Hayek, Lee-Ann C.] Smithsonian Inst Stat & Math, Washington, DC 20013 USA. RP Alexander, SN (reprint author), George Mason Univ, Dept Environm Sci & Policy, Fairfax, VA 22030 USA. EM Nazanin114@gmail.com OI Weeks, Andrea/0000-0002-0000-4541 NR 34 TC 3 Z9 3 U1 0 U2 2 PU SOUTHERN APPALACHIAN BOTANICAL SOC, NEWBERRY COLL PI NEWBERRY PA DEPT BIOLOGY, C/O CHARLES N HORN, SECRETARY-TREASURER, 2100 COLLEGE ST, NEWBERRY, SC 29108 USA SN 0008-7475 EI 1938-4386 J9 CASTANEA JI Castanea PD MAR PY 2012 VL 77 IS 1 BP 106 EP 122 DI 10.2179/11-022 PG 17 WC Plant Sciences SC Plant Sciences GA 918VJ UT WOS:000302279100010 ER PT J AU Chisholm, RA Wintle, BA AF Chisholm, Ryan A. Wintle, Brendan A. TI Choosing ecosystem service investments that are robust to uncertainty across multiple parameters SO ECOLOGICAL APPLICATIONS LA English DT Article DE asymmetric uncertainty; carbon price; Fynbos conservation; info-gap decision theory; Jonkershoek Valley, South Africa ID RESERVE NETWORKS; SOUTH-AFRICA; MANAGEMENT; WATER; CONSERVATION; DECISIONS; BIODIVERSITY; KNOWLEDGE; SELECTION; WORKING AB Info-gap decision theory facilitates decision making for problems in which uncertainty is large and probability distributions of uncertain variables are unknown. The info-gap framework allows the decision maker to maximize robustness to failure in the presence of uncertainty, where uncertainty is in the parameters of the model and failure is defined as the model output falling below some minimally acceptable performance threshold. Info-gap theory has found particular application to problems in conservation biology and ecological economics. In this study, we applied info-gap theory to an ecosystem services trade-off case study in which a decision maker aiming to maximize ecosystem service investment returns must choose between two alternative land uses: native vegetation conservation or the establishment of an exotic timber plantation. The uncertain variables are the carbon price and the water price. With a "no-information" uncertainty model that assumes equal relative uncertainty across both variables, info-gap theory identifies a minimally acceptable reward threshold above which conservation is preferred, but below which plantation establishment is preferred. However, with an uncertainty model that allows the carbon price to be substantially more uncertain than the water price, conservation of native vegetation becomes an economically more robust investment option than establishing alien pine plantations. We explored the sensitivity of the results to the use of alternative uncertainty models, including asymmetric uncertainty in individual variables. We emphasize the general finding that the results of info-gap analyses can be sensitive to the choice of uncertainty model and that, therefore, future applications to ecological problems should be careful to incorporate all available qualitative and quantitative information relating to uncertainties or should at least justify the no-information uncertainty model. C1 [Chisholm, Ryan A.] Smithsonian Trop Res Inst, Dpo, AA 34002 USA. [Chisholm, Ryan A.] Princeton Univ, Dept Ecol & Evolutionary Biol, Princeton, NJ 08544 USA. [Wintle, Brendan A.] Univ Melbourne, Sch Bot, Melbourne, Vic 3010, Australia. RP Chisholm, RA (reprint author), Smithsonian Trop Res Inst, Dpo, AA 34002 USA. EM ryan.chis@gmail.com RI Chisholm, Ryan/H-8033-2012 FU David A. Gardner '69 Magic Grant; High Meadows Foundation; Smithsonian Institution Global Earth Observatories; HSBC; Australian Research Council FX We thank Yakov Ben-Haim for advice on our analysis. We thank an anonymous reviewer for comments that improved the manuscript. R. Chisholm gratefully acknowledges the financial support of the David A. Gardner '69 Magic Grant, the High Meadows Foundation through the Africa Grand Challenge program, the Smithsonian Institution Global Earth Observatories, and the HSBC Climate Partnership. B. Wintle is supported by an Australian Research Council Future Fellowship. NR 27 TC 2 Z9 3 U1 1 U2 23 PU ECOLOGICAL SOC AMER PI WASHINGTON PA 1990 M STREET NW, STE 700, WASHINGTON, DC 20036 USA SN 1051-0761 J9 ECOL APPL JI Ecol. Appl. PD MAR PY 2012 VL 22 IS 2 BP 697 EP 704 PG 8 WC Ecology; Environmental Sciences SC Environmental Sciences & Ecology GA 921ZP UT WOS:000302516900025 PM 22611865 ER PT J AU Carvalho, JC Cardoso, P Crespo, LC Henriques, S Carvalho, R Gomes, P AF Carvalho, Jose C. Cardoso, Pedro Crespo, Luis C. Henriques, Sergio Carvalho, Rui Gomes, Pedro TI Determinants of spider species richness in coastal dunes along a gradient of mediterraneity SO INSECT CONSERVATION AND DIVERSITY LA English DT Article DE Araneae; grey dunes; habitat stability; latitudinal gradient; scale dependence; spatial analysis ID BETA DIVERSITY; ASSEMBLAGE STRUCTURE; NEIGHBOR MATRICES; IBERIAN PENINSULA; ECOLOGICAL DATA; GREY DUNES; NORTH-SEA; SCALE; PATTERNS; ARANEAE AB . 1. The Iberian Peninsula is one of the most relevant areas in terms of species richness, rarity and endemism in the Mediterranean Basin. Using spiders as a model, we studied the relative importance of environmental and non-environmental spatial variation along a gradient of mediterraneity on the western coast of the Iberian Peninsula. 2. We performed a spatially explicit analysis to evaluate the contribution of pure environmental and pure spatial effects and their shared influence on spider species richness by variation partitioning and principal coordinates of neighbour matrices (PCNM). We dissect the spatial variation of species richness into additive scale-specific models through PCNM analysis and estimate the relative importance of environmental variables for each model. 3. Variation partitioning revealed that 72.8% of species richness variation could be explained by the environmental (climate and dune stability) and spatial variables. Most of this variation (51.3%) corresponds to the environmental spatially structured component. 4. The influence of environmental variables was scale-dependent. At the broadest scales, the latitudinal-climatic gradient was the dominant factor that influenced spider species richness variation. At the finest scale, stability of the dune system was the most important component. 5. In conclusion, spider species richness patterns were determined mostly by spatially structured environmental variation. More importantly, this study shows that different environmental factors act at multiple scales. Hence, our results reinforce the importance of the incorporation of both local and broad-scale factors when examining species richness patterns. C1 [Carvalho, Jose C.; Gomes, Pedro] Univ Minho, Dept Biol, CBMA Mol & Environm Biol Ctr, P-4710057 Braga, Portugal. [Cardoso, Pedro] Natl Museum Nat Hist, Smithsonian Inst, Washington, DC 20560 USA. [Cardoso, Pedro; Crespo, Luis C.] Univ Azores, Azorean Biodivers Grp CITA A, Angra Do Heroismo, Portugal. [Henriques, Sergio; Carvalho, Rui] Univ Evora, Dept Biol, Evora, Portugal. RP Carvalho, JC (reprint author), Univ Minho, Dept Biol, CBMA Mol & Environm Biol Ctr, Campus Gualtar, P-4710057 Braga, Portugal. EM josecarvalho@bio.uminho.pt RI Cardoso, Pedro/A-8820-2008; Gomes, Pedro/I-8348-2015; CBMA, CBMA/J-1937-2016 OI Cardoso, Pedro/0000-0001-8119-9960; Gomes, Pedro/0000-0002-5595-6988; CBMA, CBMA/0000-0002-2841-2678 FU Luso-American Foundation; Portuguese Foundation for Science and Technology [SFRH/BPD/40688/2007] FX J.C.C. expresses his gratitude to the Luso-American Foundation for its support (FLAD C & T Links 2010 grant). P.C. is supported by the Portuguese Foundation for Science and Technology (SFRH/BPD/40688/2007). NR 69 TC 5 Z9 5 U1 1 U2 25 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 1752-458X J9 INSECT CONSERV DIVER JI Insect. Conserv. Divers. PD MAR PY 2012 VL 5 IS 2 BP 127 EP 137 DI 10.1111/j.1752-4598.2011.00139.x PG 11 WC Biodiversity Conservation; Entomology SC Biodiversity & Conservation; Entomology GA 907UC UT WOS:000301443200005 ER PT J AU Cardoso, P AF Cardoso, Pedro TI Habitats Directive species lists: urgent need of revision SO INSECT CONSERVATION AND DIVERSITY LA English DT Article DE Arthropods; conservation priority; endangered species lists; environmental policy; European Union; insects; LIFE programme; red lists; spiders ID BIODIVERSITY CONSERVATION; TOP PREDATORS; SURROGATES; DIVERSITY AB . 1. The European Habitats Directive is the main legislative work regarding Europes nature conservation policy. It lists the protected habitats and species in the European Union. The species lists include 122 arthropods. 2. The current lists of arthropods (Annexes II and IV) present, possibly among other, five obvious biases: taxonomic, geographic, range, size and aesthetic biases. Species of selected taxa (Lepidoptera, Coleoptera, Odonata and Orthoptera), from Northern or Central Europe, relatively widespread, of a large body size and attractive are favoured over species of other taxa, from southern and Mediterranean Europe, endemic or relatively small or inconspicuous. Such biases are obstacles to the effective protection of the European fauna. 3. Two main strategies should be followed to avoid these problems and therefore increase the effectiveness of conservation policies: (i) the adoption of objective and transparent criteria for the listing of protected species, and (ii) implement regular updates and amendments to the lists based on such criteria. C1 [Cardoso, Pedro] Natl Museum Nat Hist, Smithsonian Inst, Washington, DC 20013 USA. [Cardoso, Pedro] Univ Acores, Azorean Biodivers Grp CITA A, Angra Do Heroismo, Portugal. RP Cardoso, P (reprint author), Natl Museum Nat Hist, Smithsonian Inst, POB 37012,MRC 105,Room E-510, Washington, DC 20013 USA. EM pcardoso@ennor.org RI Cardoso, Pedro/A-8820-2008 OI Cardoso, Pedro/0000-0001-8119-9960 FU Portuguese Foundation for Science and Technology [SFRH/BPD/40688/2007] FX The author thank Jose Luis Martin, Clara Gaspar and Sergio Henriques for helpful discussion and comments on a previous version of the manuscript. This work was supported by the Portuguese Foundation for Science and Technology (SFRH/BPD/40688/2007). NR 31 TC 21 Z9 23 U1 2 U2 32 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1752-458X EI 1752-4598 J9 INSECT CONSERV DIVER JI Insect. Conserv. Divers. PD MAR PY 2012 VL 5 IS 2 BP 169 EP 174 DI 10.1111/j.1752-4598.2011.00140.x PG 6 WC Biodiversity Conservation; Entomology SC Biodiversity & Conservation; Entomology GA 907UC UT WOS:000301443200009 ER PT J AU McCormick, MK Taylor, DL Juhaszova, K Burnett, RK Whigham, DF O'Neill, JP AF McCormick, Melissa K. Taylor, D. Lee Juhaszova, Katarina Burnett, Robert K., Jr. Whigham, Dennis F. O'Neill, John P. TI Limitations on orchid recruitment: not a simple picture SO MOLECULAR ECOLOGY LA English DT Article DE fungal distribution; Goodyera pubescens; Liparis liliifolia; mycorrhizae; Orchid; Orchidaceae; Tipularia discolor; Tulasnella ID ARBUSCULAR MYCORRHIZAL FUNGI; MYCO-HETEROTROPHIC PLANTS; TERRESTRIAL ORCHIDS; IN-SITU; SYMBIOTIC GERMINATION; ECTOMYCORRHIZAL FUNGI; COMMUNITY STRUCTURE; SOIL PATHOGENS; HOST PLANTS; DIVERSITY AB Mycorrhizal fungi have substantial potential to influence plant distribution, especially in specialized orchids and mycoheterotrophic plants. However, little is known about environmental factors that influence the distribution of mycorrhizal fungi. Previous studies using seed packets have been unable to distinguish whether germination patterns resulted from the distribution of appropriate edaphic conditions or the distribution of host fungi, as these cannot be separated using seed packets alone. We used a combination of organic amendments, seed packets and molecular assessment of soil fungi required by three terrestrial orchid species to separate direct and indirect effects of fungi and environmental conditions on both seed germination and subsequent protocorm development. We found that locations with abundant mycorrhizal fungi were most likely to support seed germination and greater growth for all three orchids. Organic amendments affected germination primarily by affecting the abundance of appropriate mycorrhizal fungi. However, fungi associated with the three orchid species were affected differently by the organic amendments and by forest successional stage. The results of this study help contextualize the importance of fungal distribution and abundance to the population dynamics of plants with specific mycorrhizal requirements. Such phenomena may also be important for plants with more general mycorrhizal associations. C1 [McCormick, Melissa K.; Juhaszova, Katarina; Burnett, Robert K., Jr.; Whigham, Dennis F.; O'Neill, John P.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. [Taylor, D. Lee] Univ Alaska, Inst Arctic Biol, Fairbanks, AK 99775 USA. RP McCormick, MK (reprint author), Smithsonian Environm Res Ctr, POB 28, Edgewater, MD 21037 USA. EM mccormickm@si.edu OI Taylor, Donald/0000-0002-5985-9210; Whigham, Dennis/0000-0003-1488-820X FU NSF [DEB-0316523, REU-0353759]; Frank Bertrum Sherry Endowment at the Smithsonian Institution FX This work, M.K.M., and K.J. were funded by NSF grant DEB-0316523. Microsatellite development was funded by a grant from the Frank Bertrum Sherry Endowment at the Smithsonian Institution to D.F.W. and M.K.M. R.K.B. was funded by NSF grant REU-0353759. Hanne Rasmussen helped to establish the wood amendment plots. Timothy Filley and David Gambill helped to establish the amendment plots. NR 59 TC 37 Z9 39 U1 4 U2 94 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0962-1083 J9 MOL ECOL JI Mol. Ecol. PD MAR PY 2012 VL 21 IS 6 BP 1511 EP 1523 DI 10.1111/j.1365-294X.2012.05468.x PG 13 WC Biochemistry & Molecular Biology; Ecology; Evolutionary Biology SC Biochemistry & Molecular Biology; Environmental Sciences & Ecology; Evolutionary Biology GA 903KS UT WOS:000301116000016 PM 22272942 ER PT J AU Canning, REA Russell, HR Hatch, NA Fabian, AC Zabludoff, AI Crawford, CS King, LJ McNamara, BR Okamoto, S Raimundo, SI AF Canning, R. E. A. Russell, H. R. Hatch, N. A. Fabian, A. C. Zabludoff, A. I. Crawford, C. S. King, L. J. McNamara, B. R. Okamoto, S. Raimundo, S. I. TI Riding the wake of a merging galaxy cluster SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE ISM: kinematics and dynamics; galaxies: clusters: individual: Abell 2146; galaxies: clusters: intracluster medium; galaxies: kinematics and dynamics ID INTEGRAL FIELD SPECTROSCOPY; ACTIVE GALACTIC NUCLEI; X-RAY SPECTROSCOPY; MOLECULAR GAS; COLD FRONTS; CHANDRA OBSERVATION; ABELL 2146; BOW SHOCK; EMISSION; CORES AB Using William Herschel Telescope (WHT) Optically Adaptive System for Imaging Spectroscopy (OASIS) integral field unit observations, we report the discovery of a thin plume of ionized gas extending from the brightest cluster galaxy (BCG) in Abell 2146 to the subcluster X-ray cool core which is offset from the BCG by similar to 37 kpc. The plume is greater than 15 kpc long and less than 3 kpc wide. This plume is unique in that the cluster it is situated in is currently undergoing a major galaxy cluster merger. The BCG is unusually located behind the X-ray shock front and in the wake of the ram-pressure-stripped X-ray cool core, and evidence for recent disruption to the BCG is observed. We examine the gas and stellar morphology, the gas kinematics of the BCG and their relation to the X-ray gas. We propose that a causal link between the ionized gas plume and the offset X-ray cool core provides the simplest explanation for the formation of the plume. An interaction or merger between the BCG and another cluster galaxy is probably the cause of the offset. C1 [Canning, R. E. A.; Fabian, A. C.; Crawford, C. S.; King, L. J.; Raimundo, S. I.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Russell, H. R.; McNamara, B. R.] Univ Waterloo, Dept Phys & Astron, Waterloo, ON N2L 3G1, Canada. [Hatch, N. A.] Univ Nottingham, Sch Phys & Astron, Nottingham NG7 2RD, England. [Zabludoff, A. I.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [McNamara, B. R.] Perimeter Inst Theoret Phys, Waterloo, ON N2L 2Y5, Canada. [McNamara, B. R.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Okamoto, S.] Peking Univ, Kavli Inst Astron & Astrophys, Beijing 100871, Peoples R China. RP Canning, REA (reprint author), Univ Cambridge, Inst Astron, Madingley Rd, Cambridge CB3 0HA, England. EM bcanning@ast.cam.ac.uk OI Hatch, Nina/0000-0001-5600-0534 FU STFC; Canadian Space Agency; FCT - Fundacao para a Ciencia e a Tecnologia (Portugal); National Aeronautics and Space Administration FX REAC acknowledges STFC for financial support. HRR acknowledges generous financial support from the Canadian Space Agency Space Science Enhancement Program. ACF and LJK thank the Royal Society. SIR acknowledges financial support from FCT - Fundacao para a Ciencia e a Tecnologia (Portugal). REAC thanks S. Rix, J. Hlavacek-Larrondo, D. Zaritsky and R. Kennicutt for helpful discussions which greatly improved this work and N. Hatch for hosting REAC at Nottingham University while the data reduction was completed.; This research has made use of the NASA/IPAC Extragalactic Database (NED), which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. NR 47 TC 6 Z9 6 U1 0 U2 1 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD MAR PY 2012 VL 420 IS 4 BP 2956 EP 2968 DI 10.1111/j.1365-2966.2011.20116.x PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 901AW UT WOS:000300935100017 ER PT J AU Oguri, M Bayliss, MB Dahle, H Sharon, K Gladders, MD Natarajan, P Hennawi, JF Koester, BP AF Oguri, Masamune Bayliss, Matthew B. Dahle, Hakon Sharon, Keren Gladders, Michael D. Natarajan, Priyamvada Hennawi, Joseph F. Koester, Benjamin P. TI Combined strong and weak lensing analysis of 28 clusters from the Sloan Giant Arcs Survey SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Review DE gravitational lensing: strong; gravitational lensing: weak; galaxies: clusters: general; dark matter ID DARK-MATTER HALOS; DIGITAL SKY SURVEY; SEPARATION GRAVITATIONAL LENSES; LYMAN BREAK GALAXIES; STEEP MASS PROFILE; 3RD DATA RELEASE; X-RAY; RADIAL-DISTRIBUTION; DENSITY PROFILES; LAMBDA-CDM AB We study the mass distribution of a sample of 28 galaxy clusters using strong and weak lensing observations. The clusters are selected via their strong lensing properties as part of the Sloan Giant Arcs Survey (SGAS) from the Sloan Digital Sky Survey (SDSS). Mass modelling of the strong lensing information from the giant arcs is combined with weak lensing measurements from deep Subaru/Suprime-cam images to primarily obtain robust constraints on the concentration parameter and the shape of the mass distribution. We find that the concentration c(vir) is a steep function of the mass, c(vir) alpha M-vir(-0.59 +/- 0.12), with the value roughly consistent with the lensing-bias-corrected theoretical expectation for high-mass (similar to 10(15) h(-1) M circle dot) clusters. However, the observationally inferred concentration parameters appear to be much higher at lower masses (similar to 10(14) h(-1) M circle dot), possibly a consequence of the modification to the inner density profiles provided by baryon cooling. The steep massconcentration relation is also supported from direct stacking analysis of the tangential shear profiles. In addition, we explore the 2D shape of the projected mass distribution by stacking weak lensing shear maps of individual clusters with prior information on the position angle from strong lens modelling, and find significant evidence for a large mean ellipticity with the best-fitting value of < e >= 0.47 +/- 0.06 for the mass distribution of the stacked sample. We find that the luminous cluster member galaxy distribution traces the overall mass distribution very well, although the distribution of fainter cluster galaxies appears to be more extended than the total mass. C1 [Oguri, Masamune] Univ Tokyo, Inst Phys & Math Universe, Chiba 2778583, Japan. [Oguri, Masamune] Natl Astron Observ Japan, Div Theoret Astron, Tokyo 1818588, Japan. [Bayliss, Matthew B.] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. [Bayliss, Matthew B.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Bayliss, Matthew B.; Gladders, Michael D.; Koester, Benjamin P.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. [Bayliss, Matthew B.; Sharon, Keren; Gladders, Michael D.; Koester, Benjamin P.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Dahle, Hakon] Univ Oslo, Inst Theoret Astrophys, N-0315 Oslo, Norway. [Natarajan, Priyamvada] Yale Univ, Dept Astron, New Haven, CT 06511 USA. [Natarajan, Priyamvada] Yale Univ, Dept Phys, New Haven, CT 06520 USA. [Hennawi, Joseph F.] Max Planck Inst Astron, D-69117 Heidelberg, Germany. RP Oguri, M (reprint author), Univ Tokyo, Inst Phys & Math Universe, 5-1-5 Kashiwanoha, Chiba 2778583, Japan. EM oguri@ipmu.jp RI Oguri, Masamune/C-6230-2011 FU FIRST; World Premier International Research Center Initiative (WPI Initiative); MEXT, Japan; JSPS [23740161]; National Science Foundation [AST10-44455] FX We thank T. Hamana, E. Komatsu, Y.-T. Lin, S. Miyazaki, D. Nagai, N. Okabe, J. Schaye, M. Takada and K. Umetsu for useful discussions. We also thank an anonymous referee for useful comments and suggestions. This work was supported in part by the FIRST programme 'Subaru Measurements of Images and Redshifts (SuMIRe)', World Premier International Research Center Initiative (WPI Initiative), MEXT, Japan, and Grant-in-Aid for Scientific Research from the JSPS (23740161). PN acknowledges support from the National Science Foundation's Theory Programme via the grant AST10-44455. NR 140 TC 117 Z9 119 U1 2 U2 14 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD MAR PY 2012 VL 420 IS 4 BP 3213 EP 3239 DI 10.1111/j.1365-2966.2011.20248.x PG 27 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 901AW UT WOS:000300935100036 ER PT J AU Roediger, E Lovisari, L Dupke, R Ghizzardi, S Bruggen, M Kraft, RP Machacek, ME AF Roediger, E. Lovisari, L. Dupke, R. Ghizzardi, S. Brueggen, M. Kraft, R. P. Machacek, M. E. TI Gas sloshing, cold fronts, Kelvin-Helmholtz instabilities and the merger history of the cluster of galaxies Abell 496 SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE methods: numerical; galaxies: clusters: individual: A496; galaxies: clusters: intracluster medium; X-rays: galaxies: clusters ID XMM-NEWTON; INTRACLUSTER MEDIUM; INTERGALACTIC MEDIUM; CHANDRA OBSERVATION; VIRGO CLUSTER; CORES; SIMULATIONS; PROFILES; DYNAMICS; SAMPLE AB We investigate the origin and nature of the multiple sloshing cold fronts in the core of Abell 496 by direct comparison between observations and dedicated hydrodynamical simulations. Our simulations model a minor merger with a 4 x 1013 M? subcluster crossing A496 from the south-west to the northnorth-east, passing the cluster core in the south-east at a pericentre distance of 100 to a few x 100 kpc about 0.60.8 Gyr ago. The gas sloshing triggered by the merger can reproduce almost all observed features, e.g. the characteristic spiral-like brightness residual distribution in the cluster centre and its asymmetry out to 500 kpc, also the positions of and contrasts across the cold fronts. If the subcluster passes close (100 kpc) to the cluster core, the resulting shear flows are strong enough to trigger KelvinHelmholtz instabilities that in projection resemble the peculiar kinks in the cold fronts of Abell 496. Finally, we show that sloshing does not lead to a significant modification of the global intracluster medium profiles but a mild oscillation around the initial profiles. C1 [Roediger, E.; Brueggen, M.] Jacobs Univ Bremen, D-28725 Bremen, Germany. [Lovisari, L.] Univ Bonn, Argelander Inst Astron, D-53121 Bonn, Germany. [Lovisari, L.] Univ Innsbruck, Inst Astro & Teilchenphys, A-6020 Innsbruck, Austria. [Dupke, R.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Dupke, R.] Eureka Sci Inc, Oakland, CA 94602 USA. [Dupke, R.] Observ Nacl, BR-20921400 Rio De Janeiro, Brazil. [Dupke, R.] Univ Alabama, Tuscaloosa, AL 35487 USA. [Ghizzardi, S.] Ist Astrofis Spaziale & Fis Cosm, INAF, I-20133 Milan, Italy. [Kraft, R. P.; Machacek, M. E.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Roediger, E (reprint author), Jacobs Univ Bremen, POB 750 561, D-28725 Bremen, Germany. EM e.roediger@jacobs-university.de RI 7, INCT/H-6207-2013; Astrofisica, Inct/H-9455-2013; OI Ghizzardi, Simona/0000-0003-0879-7328 FU DFG (German Research Foundation) [RE 1462/6]; John-Neumann Institut at the Forschungszentrum Julich [NIC 3711, 4368]; Smithsonian Astrophysical Observatory (DLR); German Aerospace Agency from the Ministry of Economy and Technology (BMWi) [50 OR 1102E]; Austrian Science Foundation (FWF) [P19300-N16]; NASA [NNH10CD19C]; DFG Research Unit; DOE ASC/Alliances FX ER acknowledges the support of the Priority Programme Witnesses of Cosmic History of the DFG (German Research Foundation), the supercomputing grants NIC 3711 and 4368 at the John-Neumann Institut at the Forschungszentrum Julich, a visiting scientist fellowship of the Smithsonian Astrophysical Observatory and the hospitality of the Center for Astrophysics in Cambridge. LL acknowledges support by the DFG through Heisenberg grant RE 1462/6, by the German Aerospace Agency (DLR) with funds from the Ministry of Economy and Technology (BMWi) through grant 50 OR 1102E and the Austrian Science Foundation (FWF) through grant P19300-N16. RD acknowledges support from NASA Grant NNH10CD19C. MB acknowledges support by the DFG Research Unit 'Magnetisation of Interstellar and Intergalactic Media: The Prospects of Low-Frequency Radio Observations'. We thank Suresh Sivanandam for providing us with observational data and Georgiana Ogrean, Annalisa Bonafede and Paul Nulsen for helpful discussions. The results presented were produced using the FLASH code, a product of the DOE ASC/Alliances-funded Center for Astrophysical Thermonuclear Flashes at the University of Chicago. This research has made use of Aladin. It has also made use of the NASA/IPAC Extragalactic Database (NED) which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. NR 41 TC 29 Z9 29 U1 0 U2 1 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD MAR PY 2012 VL 420 IS 4 BP 3632 EP 3648 DI 10.1111/j.1365-2966.2011.20287.x PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 901AW UT WOS:000300935100067 ER PT J AU Sessa, JA Bralower, TJ Patzkowsky, ME Handley, JC Ivany, LC AF Sessa, Jocelyn A. Bralower, Timothy J. Patzkowsky, Mark E. Handley, John C. Ivany, Linda C. TI Environmental and biological controls on the diversity and ecology of Late Cretaceous through early Paleogene marine ecosystems in the U.S. Gulf Coastal Plain SO PALEOBIOLOGY LA English DT Article ID FOSSIL RECORD; TERTIARY BOUNDARY; MOLLUSCAN RECOVERY; VENEROID BIVALVES; SHELF COMMUNITIES; MASS EXTINCTION; EAST TEXAS; PATTERNS; EVOLUTION; BIODIVERSITY AB The late Mesozoic through early Cenozoic is an interval of significant biologic turnover and ecologic reorganization within marine assemblages, but the timing and causes of these changes remain poorly understood. Here, we quantify the pattern and timing of shifts in the diversity (richness and evenness) and ecology of local (i.e., sample level) mollusk-dominated assemblages during this critical interval using field-collected and published data sets from the U.S. Gulf Coastal Plain. We test whether the biologic and ecologic patterns observed primarily at the global level during this time are also expressed at the local level, and whether the end-Cretaceous (K/Pg) mass extinction and recovery moderated these trends. To explore whether environment had any effect on these patterns, we examine data from shallow subtidal and offshore settings. Assemblages from both settings recovered to pre-extinction diversity levels rapidly, in less than 7 million years. Following initial recovery, diversity remained unchanged in both settings. The trajectory of ecological restructuring was distinct for each setting in the wake of the K/Pg extinction. In offshore assemblages, the abundance and number of predatory carnivorous taxa dramatically increased, and surficial sessile suspension feeders were replaced by more active suspension feeders. In contrast, shallow subtidal assemblages did not experience ecological reorganization following the K/Pg extinction. The distinct ecological patterns displayed in each environment follow onshore-offshore patterns of innovation, whereby evolutionary novelties first appear in onshore settings relative to offshore habitats. Increased predation pressure may explain the significant ecological restructuring of offshore assemblages, whereby the explosive radiation of predators drove changes in their prey. Habitat-specific ecological restructuring, and its occurrence solely during the recovery interval, implies that disturbance and incumbency were also key in mediating these ecological changes. C1 [Sessa, Jocelyn A.; Bralower, Timothy J.; Patzkowsky, Mark E.] Penn State Univ, Dept Geosci, University Pk, PA 16802 USA. [Handley, John C.] Xerox Corp, Webster, NY 14580 USA. [Ivany, Linda C.] Syracuse Univ, Dept Earth Sci, Syracuse, NY 13244 USA. RP Sessa, JA (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, MRC 121, Washington, DC 20013 USA. EM SessaJ@si.edu FU American Museum of Natural History; Geological Society of America; Pennsylvania Space Grant Consortium; Paleontological Society; National Science Foundation [EAR-0318584, EAR-0120727, EAR-0719645]; NASA [NNX07AK62G, NNX07AK64G]; Director's Office of the Smithsonian Natural History Museum FX We are grateful to the researchers who originally collected and published the data we derived from the literature, and to those who entered these data into the PaleoDB. W. Allmon, S. Butts, G. Dietl, C. Garvie, A. Molineux, and J. Nagel-Myers are thanked for access to specimens. We appreciate that M. Kosnik provided a data set of his samples that contained individuals greater than 2 mm in size, and that C. Garvie made available unpublished faunal data. G. Hunt is thanked for elucidating time series analysis. J. Sessa enjoyed thought-provoking discussion about this work with R. Bambach, A. Bush, A. Z. Krug, P. Wagner, and especially A. Hendy and E. Currano. We thank M. Arthur, A. Hendy, E. Post, and P. Wilf for insightful comments on an earlier version of this manuscript. We are grateful to J. Stilwell and especially A. Miller and M. Kowalewski for thoughtful and detailed reviews of this manuscript. This research was supported by several funding sources: the American Museum of Natural History Theodore Roosevelt Grant (to Sessa); the Geological Society of America Graduate Student Research Grant program (to Sessa); the Pennsylvania Space Grant Consortium Fellowship (to Sessa); the Paleontological Society Student Research Grant program (to Sessa); National Science Foundation Grants EAR-0318584 (to Bra lower), EAR-0120727 (to Bra lower), and EAR-0719645 (to Ivany); NASA Grants NNX07AK62G (to Bra lower) and NNX07AK64G (to Patzkowsky). We acknowledge the Director's Office of the Smithsonian Natural History Museum for providing funding for page costs. Fieldwork is only as pleasant as your field companions make it, and J. Sessa is especially grateful for enjoyable fieldtrips with D. Dockery, R. Fluegeman, H. Ford, P. Harnik, L. Ivany, R. Lockwood, H. Wall, P. Wall, and L. B. Ward. This is Paleobiology Database contribution 145. NR 99 TC 17 Z9 17 U1 1 U2 14 PU CAMBRIDGE UNIV PRESS PI NEW YORK PA 32 AVENUE OF THE AMERICAS, NEW YORK, NY 10013-2473 USA SN 0094-8373 EI 1938-5331 J9 PALEOBIOLOGY JI Paleobiology PD SPR PY 2012 VL 38 IS 2 BP 218 EP 239 DI 10.1666/10042.1 PG 22 WC Biodiversity Conservation; Ecology; Evolutionary Biology; Paleontology SC Biodiversity & Conservation; Environmental Sciences & Ecology; Evolutionary Biology; Paleontology GA 921QK UT WOS:000302492000003 ER PT J AU Melian, CJ Alonso, D Allesina, S Condit, RS Etienne, RS AF Melian, Carlos J. Alonso, David Allesina, Stefano Condit, Richard S. Etienne, Rampal S. TI Does Sex Speed Up Evolutionary Rate and Increase Biodiversity? SO PLOS COMPUTATIONAL BIOLOGY LA English DT Article ID NEUTRAL THEORY; ADAPTIVE RADIATION; NATURAL-SELECTION; SPECIES FORMATION; SPECIATION; DIVERSITY; MODEL; INCOMPATIBILITIES; CONSEQUENCES; POPULATION AB Most empirical and theoretical studies have shown that sex increases the rate of evolution, although evidence of sex constraining genomic and epigenetic variation and slowing down evolution also exists. Faster rates with sex have been attributed to new gene combinations, removal of deleterious mutations, and adaptation to heterogeneous environments. Slower rates with sex have been attributed to removal of major genetic rearrangements, the cost of finding a mate, vulnerability to predation, and exposure to sexually transmitted diseases. Whether sex speeds or slows evolution, the connection between reproductive mode, the evolutionary rate, and species diversity remains largely unexplored. Here we present a spatially explicit model of ecological and evolutionary dynamics based on DNA sequence change to study the connection between mutation, speciation, and the resulting biodiversity in sexual and asexual populations. We show that faster speciation can decrease the abundance of newly formed species and thus decrease long-term biodiversity. In this way, sex can reduce diversity relative to asexual populations, because it leads to a higher rate of production of new species, but with lower abundances. Our results show that reproductive mode and the mechanisms underlying it can alter the link between mutation, evolutionary rate, speciation and biodiversity and we suggest that a high rate of evolution may not be required to yield high biodiversity. C1 [Melian, Carlos J.; Allesina, Stefano] Univ Calif Santa Barbara, Natl Ctr Ecol Anal & Synth, Santa Barbara, CA 93106 USA. [Melian, Carlos J.] Swiss Fed Inst Aquat Sci & Technol, Ctr Ecol Evolut & Biogeochem, Kastanienbaum, Switzerland. [Alonso, David; Etienne, Rampal S.] Univ Groningen, Community & Conservat Ecol Grp, Groningen, Netherlands. [Allesina, Stefano] Univ Chicago, Dept Ecol & Evolut, Chicago, IL 60637 USA. [Condit, Richard S.] Smithsonian Trop Res Inst, Ctr Trop Forest Sci, Balboa, Ancon, Panama. RP Melian, CJ (reprint author), Univ Calif Santa Barbara, Natl Ctr Ecol Anal & Synth, Santa Barbara, CA 93106 USA. EM carlos.melian@eawag.ch RI Etienne, Rampal/F-5835-2012; alonso, david/A-5406-2008; Melian, Carlos/C-2146-2008 OI Etienne, Rampal/0000-0003-2142-7612; alonso, david/0000-0002-8888-1644; Melian, Carlos/0000-0003-3974-6515 FU National Center for Ecological Analysis and Synthesis; NSF [DEB-0553768]; University of California, Santa Barbara; State of California; Microsoft Research Ltd., Cambridge, United Kingdom; Netherlands Organization for Scientific Research (NWO) FX CJM, SA, and RSC were supported by fellowships from the National Center for Ecological Analysis and Synthesis, a Center funded by NSF (Grant \#DEB-0553768), the University of California, Santa Barbara, and the State of California. CJM also acknowledges the support by Microsoft Research Ltd., Cambridge, United Kingdom. DA and RSE acknowledge the support of the Netherlands Organization for Scientific Research (NWO). The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 77 TC 7 Z9 7 U1 0 U2 44 PU PUBLIC LIBRARY SCIENCE PI SAN FRANCISCO PA 1160 BATTERY STREET, STE 100, SAN FRANCISCO, CA 94111 USA SN 1553-734X EI 1553-7358 J9 PLOS COMPUT BIOL JI PLoS Comput. Biol. PD MAR PY 2012 VL 8 IS 3 AR e1002414 DI 10.1371/journal.pcbi.1002414 PG 9 WC Biochemical Research Methods; Mathematical & Computational Biology SC Biochemistry & Molecular Biology; Mathematical & Computational Biology GA 918IY UT WOS:000302244000022 PM 22412362 ER PT J AU Dillehay, TD Bonavia, D Goodbred, S Pino, M Vasquez, V Tham, TR Conklin, W Splitstoser, J Piperno, D Iriarte, J Grobman, A Levi-Lazzaris, G Moreira, D Lopez, M Tung, T Titelbaum, A Verano, J Adovasio, J Cummings, LS Bearez, P Dufour, E Tombret, O Ramirez, M Beavins, R DeSantis, L Rey, I Mink, P Maggard, G Franco, T AF Dillehay, Tom D. Bonavia, Duccio Goodbred, Steven Pino, Mario Vasquez, Victor Rosales Tham, Teresa Conklin, William Splitstoser, Jeff Piperno, Dolores Iriarte, Jose Grobman, Alexander Levi-Lazzaris, Gerson Moreira, Daniel Lopez, Marilaura Tung, Tiffiny Titelbaum, Anne Verano, John Adovasio, James Cummings, Linda Scott Bearez, Phillipe Dufour, Elise Tombret, Olivier Ramirez, Michael Beavins, Rachel DeSantis, Larisa Rey, Isabel Mink, Philip Maggard, Greg Franco, Teresa TI Chronology, mound-building and environment at Huaca Prieta, coastal Peru, from 13 700 to 4000 years ago SO ANTIQUITY LA English DT Article DE Peru; Holocene; ritual mound; horticulture AB Renewed in-depth multi-disciplinary investigation of a large coastal mound settlement in Peru has extended the occupation back more than 7000 years to a first human exploitation similar to 13 720 BR Research by the authors has chronicled the prehistoric sequence from the activities of the first maritime foragers to the construction of the black mound and the introduction of horticulture and monumentality. The community of Huaca Prieta emerges as innovative, complex and ritualised, as yet with no antecedents. C1 [Dillehay, Tom D.; Levi-Lazzaris, Gerson; Tung, Tiffiny; Franco, Teresa] Vanderbilt Univ, Dept Anthropol, Coll Arts & Sci, Nashville, TN 37235 USA. [Dillehay, Tom D.] Univ Catolica Temuco, Escuela Antropol, Fac Ciensias Sociales, Manuel Montt 056, Temuco, Chile. [Bonavia, Duccio] Acad Nacl Hist, Lima 1, Peru. [Goodbred, Steven; Beavins, Rachel; DeSantis, Larisa] Vanderbilt Univ, Dept Earth & Environm Sci, Coll Arts & Sci, Nashville, TN 37240 USA. [Pino, Mario] Univ Austral Chile, Inst Ciencias Geol, Fac Ciencias, Valdivia, Chile. [Vasquez, Victor; Rosales Tham, Teresa] Univ Nacl Trujillo, Lab Bioarqueol, Trujillo, Peru. [Conklin, William] Field Museum, Dept Anthropol, Chicago, IL 60605 USA. [Splitstoser, Jeff] Boundary End Archaeol Res Ctr, Barnardsville, NC 28709 USA. [Piperno, Dolores] Smithsonian Inst, Archaeobiol Program, Dept Anthropol, Natl Museum Nat Hist, Washington, DC 20013 USA. [Piperno, Dolores] Smithsonian Trop Res Inst, Balboa, Panama. [Iriarte, Jose] Univ Exeter, Dept Archaeol, Exeter EX4 4QE, Devon, England. [Grobman, Alexander] Univ Nacl Agr La Molina, Fac Ciencias, Lima 12, Peru. [Moreira, Daniel] Univ Fed Rondonia, Dept Arqueol, BR-78900500 Porto Velho, Brazil. [Lopez, Marilaura] Univ Nacl Trujillo, Escuela Arqueol, Trujillo, La Libertad, Peru. [Titelbaum, Anne; Verano, John] Tulane Univ, Dept Anthropol, New Orleans, LA 70118 USA. [Adovasio, James] Mercyhurst Coll, Dept Anthropol, Mercyhurst Archaeol Inst, Erie, PA 16546 USA. [Cummings, Linda Scott] Paleo Res Inst, Golden, CO 80401 USA. [Bearez, Phillipe; Dufour, Elise; Tombret, Olivier] Museum Natl Hist Nat, F-75005 Paris, France. [Tombret, Olivier] Univ Picardie Jules Verne, F-80025 Amiens, France. [Ramirez, Michael] Univ Texas Austin, Dept Geol Sci, Austin, TX 78705 USA. [Rey, Isabel] CSIC, Museo Nacl Ciencias Nat, E-28006 Madrid, Spain. [Mink, Philip; Maggard, Greg] Univ Kentucky, Kentucky Archaeol Survey, Dept Anthropol, Lexington, KY 40506 USA. RP Dillehay, TD (reprint author), Vanderbilt Univ, Dept Anthropol, Coll Arts & Sci, 124 Garland Hall, Nashville, TN 37235 USA. RI Goodbred, Steven/A-1737-2011; Iriarte, Jose /A-1141-2010; PINO, MARIO/A-2709-2008; Rey, I/K-8136-2014; OI Goodbred, Steven/0000-0001-7626-9864; PINO, MARIO/0000-0001-6181-353X; Rey, I/0000-0002-2122-5124; Iriarte, Jose/0000-0002-8155-5360 NR 28 TC 14 Z9 15 U1 0 U2 17 PU ANTIQUITY PI YORK PA KINGS MANOR, YORK YO1 7EP, ENGLAND SN 0003-598X J9 ANTIQUITY JI Antiquity PD MAR PY 2012 VL 86 IS 331 BP 48 EP 70 PG 23 WC Anthropology; Archaeology SC Anthropology; Archaeology GA 912RU UT WOS:000301818200004 ER PT J AU Petersen, JJ Parker, IM Potter, D AF Petersen, Jennifer J. Parker, Ingrid M. Potter, Daniel TI ORIGINS AND CLOSE RELATIVES OF A SEMI-DOMESTICATED NEOTROPICAL FRUIT TREE: CHRYSOPHYLLUM CAINITO (SAPOTACEAE) SO AMERICAN JOURNAL OF BOTANY LA English DT Article DE caimito; Chrysophylloideae; domestication; geographic origins; lineage sorting; phylogeography; star apple ID CHLOROPLAST DNA; PHYLOGENETIC INFERENCE; HISTORICAL BIOGEOGRAPHY; VITELLARIA-PARADOXA; SPONDIAS-PURPUREA; GENE GENEALOGIES; MANILKARA-ZAPOTA; TROPICAL TREES; SEQUENCE DATA; L. AB Premise of the study: Understanding patterns and processes associated with domestication has implications for crop development and agricultural biodiversity conservation. Semi-domesticated crops provide excellent opportunities to examine the interplay of natural and anthropogenic influences on plant evolution. The domestication process has not been thoroughly examined in many tropical perennial crop species. Chrysophyllum cainito (Sapotaceae), the star apple or caimito, is a semi-domesticated species widely cultivated for its edible fruits. It is known to be native to the neotropics, but the precise geographic origins of wild and cultivated forms are unresolved. _ Methods: We used nuclear ribosomal ITS sequences to infer phylogenetic relationships among C. cainito and close relatives (section Chrysophyllum). We employed phylogeographic approaches using ITS and plastid sequence data to determine geographic origins and center(s) of domestication of caimito. Key results: ITS data suggest a close relationship between C. cainito and C. argenteum. Plastid haplotype networks reveal several haplotypes unique to individual taxa but fail to resolve distinct lineages for either C. cainito or C. argenteum. Caimito populations from northern Mesoamerica and the Antilles exhibit a subset of the genetic diversity found in southern Mesoamerica. In Panama, cultivated caimito retains high levels of the diversity seen in wild populations. Conclusions: Chrysophyllum cainito is most closely related to a clade containing Central and South American C. argenteum, including subsp. panamense. We hypothesize that caimito is native to southern Mesoamerica and was domesticated from multiple wild populations in Panama. Subsequent migration into northern Mesoamerica and the Antilles was mediated by human cultivation. C1 [Petersen, Jennifer J.; Potter, Daniel] Univ Calif Davis, Dept Plant Sci, Davis, CA 95616 USA. [Parker, Ingrid M.] Univ Calif Santa Cruz, Dept Ecol & Evolutionary Biol, Santa Cruz, CA 95064 USA. [Parker, Ingrid M.] Smithsonian Trop Res Inst, Balboa, Panama. RP Petersen, JJ (reprint author), Univ Calif Davis, Dept Plant Sci, Mail Stop 2,1 Shields Ave, Davis, CA 95616 USA. EM jjpetersen@ucdavis.edu RI perumal, murugiah/D-1565-2012 FU Davis Botanical Society; UC Davis Center for Biosystematics; U.C. Davis Academic Senate Committee on Research; University Outreach; UC MEXUS; Fulbright-Garcia Robles Scholarship FX Manuscript received 5 July 2011; revision accepted 16 December 2011. The authors thank R. Aguilar, G. Carnevali, T. Clase, T. Commack, A. Estrada, E. Gibley, S. Krosnick, P. Lash, I. Lopez, H. Membache, G. Proctor, and A. Veloz for their assistance during fieldwork; C. Jones, C. Perez, The Fairchild Tropical Garden, Montgomery Botanical Garden, and the Royal Botanical Garden, Kew for providing additional leaf material; A. McNally who made the maps; A. Kleist; the editors of AJB; and two anonymous reviewers for valuable comments on earlier versions of the manuscript. The authors thank the Smithsonian Tropical Research Institute for the logistical support and ANAM and ACP for granting us permission to conduct research in the Republic of Panama. Financial awards made to J.J.P. by the Davis Botanical Society, UC Davis Center for Biosystematics, Henry A. Jastro and Peter J. Shields Research Scholarships, and those made to D. P. from the U.C. Davis Academic Senate Committee on Research and University Outreach and International Programs all supported this work. J. J. P. made additional collections while working on a UC MEXUS Dissertation Research Grant and a Fulbright-Garcia Robles Scholarship. NR 62 TC 7 Z9 8 U1 4 U2 34 PU BOTANICAL SOC AMER INC PI ST LOUIS PA PO BOX 299, ST LOUIS, MO 63166-0299 USA SN 0002-9122 J9 AM J BOT JI Am. J. Bot. PD MAR PY 2012 VL 99 IS 3 BP 585 EP 604 DI 10.3732/ajb.1100326 PG 20 WC Plant Sciences SC Plant Sciences GA 905EI UT WOS:000301254600027 PM 22396333 ER PT J AU Guan, TP Ge, BM Powell, DM Mcshea, WJ Li, S Song, YL AF Guan, Tian Pei Ge, Bao Ming Powell, David M. Mcshea, William J. Li, Sheng Song, Yan Ling TI Does a temperate ungulate that breeds in summer exhibit rut-induced hypophagia? Analysis of time budgets of male takin (Budorcas taxicolor) in Sichuan, China SO BEHAVIOURAL PROCESSES LA English DT Article DE Foraging; Rutting; Constraints; Hypophagia; Temperate ungulate; Takin; Capital breeder ID ACTIVITY PATTERNS; QINLING MOUNTAINS; LARGE HERBIVORES; PLANT PHENOLOGY; GOLDEN TAKIN; DAMA-DAMA; BEHAVIOR; DEER; PREDATION; MIGRATION AB Mammals maximize fitness by optimizing time and energy allocation between reproduction and survival. Describing time budgets is a way to understand a species' constraints in energy allocation. We describe a time budget for male takin (Budorcas taxi color) in Tangjiahe Nature Reserve, China, to better understand rut-induced hypophagia, which is frequently observed in temperate ungulates that breed in autumn or in winter. Observations generally occurred at two elevations (1200-1600 m and 2600-3200 m). using 20-min focal animal scan sampling from 2007 to 2009. Feeding behaviors accounted for the majority in takin's time budget (61.1%) during daylight hours, relative to the other observed behaviors, such as rest (14.1%), alert behavior (10.2%) and locomotion (6.8%). We found a negative correlation between feeding behavior and rutting behavior during the rutting season. A ratio of feeding time to resting time increased from pre-rut to rut, while resting behavior did not change significantly across seasons. These results suggest the "energy saving" hypothesis could explain reduced foraging in male takin during the rut, but aspects of the species biology suggest that hypotheses for rut-induced hypophagia developed for other temperate ungulates do not apply to takin. We suggest that the unusual summer rutting season of takin releases males from the energy constraints encountered by temperate ungulates that breed in the autumn and has other benefits for offspring survival. Further research should be conducted on ungulates that exhibit rut during the summer and tropical ungulates that might not experience limited food availability following the mating season to improve our understanding on rut-induced hypophagia. (C) 2012 Elsevier B.V. All rights reserved. C1 [Song, Yan Ling] Chinese Acad Sci, Inst Zool, Key Lab Anim Ecol & Conservat Biol, Beijing 100101, Peoples R China. [Guan, Tian Pei; Song, Yan Ling] Beijing Normal Univ, Minist Educ, Key Lab Biodivers Sci & Ecol Engn, Coll Life Sci, Beijing 100875, Peoples R China. [Ge, Bao Ming] Jiangsu Prov Key Lab Coastal Wetland Bioresources, Yancheng 224002, Jiangsu, Peoples R China. [Powell, David M.] Wildlife Conservat Soc, Bronx, NY 10460 USA. [Mcshea, William J.; Li, Sheng] Smithsonian Conservat Biol Inst, Front Royal, VA 22630 USA. RP Song, YL (reprint author), Chinese Acad Sci, Inst Zool, Key Lab Anim Ecol & Conservat Biol, 1 Beichen W Rd, Beijing 100101, Peoples R China. EM songyl@ioz.ac.cn FU Hong Kong Ocean Park Conservation Foundation; National Geographic Society; Smithsonian National Zoological Park; Wilds and Friends of the National Zoo FX We thank the Hong Kong Ocean Park Conservation Foundation, National Geographic Society, Smithsonian National Zoological Park, The Wilds and Friends of the National Zoo for funding. We appreciate Sichuan Forestry Department and Administration of Tangjiahe Nature Reserve for research permissions and management support; We thank Ma Wenhu, Yang Jun, Sun Yubin, Zhang Zhonghuai and all other Tangjiahe staff for providing great help in the observation and logistic support. We also thank San Diego Zoo Global for access to takin weight data. We thanks two anonymous reviewers for helpful suggestions which improved the manuscript. NR 44 TC 4 Z9 5 U1 1 U2 30 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0376-6357 J9 BEHAV PROCESS JI Behav. Processes PD MAR PY 2012 VL 89 IS 3 BP 286 EP 291 DI 10.1016/j.beproc.2011.12.008 PG 6 WC Psychology, Biological; Behavioral Sciences; Zoology SC Psychology; Behavioral Sciences; Zoology GA 913NZ UT WOS:000301886000013 PM 22248568 ER PT J AU Cuk, M AF Cuk, Matija TI Chronology and sources of lunar impact bombardment SO ICARUS LA English DT Article DE Moon; Moon, Surface; Cratering; Asteroids, Dynamics; Meteorites ID LATE HEAVY BOMBARDMENT; CRUSTAL MAGNETIC-ANOMALIES; INNER SOLAR-SYSTEM; ASTEROID BELT; MELT BRECCIAS; TERRESTRIAL PLANETS; CATACLYSM IMPACTORS; AR-39-AR-40 AGES; IRON-METEORITES; THERMAL HISTORY AB The Moon has suffered intense impact bombardment ending at 3.9 Gyr ago, and this bombardment probably affected all of the inner Solar System. Basin magnetization signatures and lunar crater size-distributions indicate that the last episode of bombardment at about 3.85 Gyr ago was less extensive than previously thought. We explore the contribution of the primordial Mars-crosser population to early lunar bombardment. We find that Mars-crosser population initially decays with a 80-Myr half-life, with the long tail of survivors clustering on temporarily non-Mars-crossing orbits between 1.8 and 2 AU. These survivors decay with half-life of about 600 Myr and are progenitors of the extant Hungaria asteroid group in the same region. We estimate the primordial Mars-crosser population contained about 0.01-0.02 Earth masses. Such initial population is consistent with no lunar basins forming after 3.8 Gya and the amount of mass in the Hungaria group. As they survive longer and in greater numbers than other primordial populations, Mars-crossers are the best candidate for forming the majority of lunar craters and basins, including most of the Nectarian system. However, this remnant population cannot produce Imbrium and Orientale basins, which formed too late and are too large to be part of a smooth bombardment. We propose that the Imbrian basins and craters formed in a discrete event, consistent with the basin magnetization signatures and crater size-distributions. This late "impactor shower" would be triggered by a collisional disruption of a Vesta-sized body from this primordial Mars-crossing population (Wetherill, G.W. [1975]. Proc. Lunar Sci. Conf. 6, 1539-1561) that was still comparable to the present-day asteroid belt a 3.9 Gya. This tidal disruption lead to a short-lived spike in bombardment by non-chondritic impactors with a non-asteroidal size-frequency distribution, in agreement with available evidence. This body ("Wetherill's object") also uniquely matches the constraints for the parent body of mesosiderite meteorites. We propose that the present-day sources of mesosiderites are multi-km-sized asteroids residing in the Hungaria group, that have been implanted there soon after the original disruption of their parent 3.9 Gyr ago. (C) 2011 Elsevier Inc. All rights reserved. C1 [Cuk, Matija] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. [Cuk, Matija] Harvard Univ, Dept Earth & Planetary Sci, Cambridge, MA 02138 USA. RP Cuk, M (reprint author), SETI Inst, 189 N Bernardo Ave, Mountain View, CA 94043 USA. EM cuk@eps.harvard.edu NR 92 TC 13 Z9 13 U1 1 U2 11 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 J9 ICARUS JI Icarus PD MAR PY 2012 VL 218 IS 1 BP 69 EP 79 DI 10.1016/j.icarus.2011.11.031 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 910LH UT WOS:000301637700006 ER PT J AU Tulchinsky, AY Norenburg, JL Turbeville, JM AF Tulchinsky, Alexander Y. Norenburg, Jon L. Turbeville, James M. TI Phylogeography of the marine interstitial nemertean Ototyphlonemertes parmula (Nemertea, Hoplonemertea) reveals cryptic diversity and high dispersal potential SO MARINE BIOLOGY LA English DT Article ID POPULATION GENETIC-STRUCTURE; MITOCHONDRIAL-DNA SEQUENCES; MULTILOCUS GENOTYPE DATA; PLATYHELMINTHES PROSERIATA; PAIRWISE COMPARISONS; MOLECULAR DIVERSITY; PELLIODITIS-MARINA; NORTHEAST ATLANTIC; STATISTICAL TESTS; SOFTWARE PACKAGE AB We conducted a phylogeographic study of the meiofaunal nemertean Ototyphlonemertes parmula, an apparent species complex from the littoral zone of coarse-grained beaches, using a 494-bp fragment of the mitochondrial cytochrome oxidase 3 gene (cox3). Six populations from the Gulf and Atlantic coasts of Florida, two from New England, and one from the Caribbean were sampled in March and August 2005. Three major lineages were identified, separated by cox3 sequence divergence of 16-18%, with partially overlapping ranges. Tests for hybridization using ISSR markers detected nuclear gene exchange within but not between the major mitochondrial lineages, indicating the presence of cryptic species. One lineage dominating the Atlantic coast of Florida shows no evidence of geographic structuring. Another lineage shows a phylogenetic break between the Atlantic and Gulf coasts, suggesting that unsuitable habitat may act as a barrier to dispersal. Long-distance migration is evidenced by shared haplotypes between Florida and the eastern Caribbean. Overall, the widespread distribution of individual haplotypes and lack of structuring within geographic regions contrast with O. parmula's strongly sediment-bound lifestyle. We speculate that dispersal of adults by storms and/or sediment transport may be more important than few and potentially short-lived planktonic larvae to explain geographic diversity in O. parmula and may be important for meiofauna in general. C1 [Tulchinsky, Alexander Y.] Univ Massachusetts, Grad Program Organism & Evolutionary Biol, Amherst, MA 01003 USA. [Norenburg, Jon L.] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20013 USA. [Turbeville, James M.] Virginia Commonwealth Univ, Dept Biol, Richmond, VA 23284 USA. RP Tulchinsky, AY (reprint author), Univ Massachusetts, Grad Program Organism & Evolutionary Biol, 611 N Pleasant St, Amherst, MA 01003 USA. EM atulchin@cns.umass.edu RI Norenburg, Jon/K-3481-2015 OI Norenburg, Jon/0000-0001-7776-1527 FU Smithsonian Institution; National Science Foundation [DEB-0089654] FX Travel funding was provided by the Smithsonian Institution. We thank the staff at the Smithsonian Marine Station at Fort Pierce, Florida, where collections were processed. We thank D. Smith, A. Nicolas, and B. Brown for assistance with laboratory methods. A. Porter and N. Johnson provided valuable feedback on the manuscript. Thanks also to J. Woodruff, who provided useful information about storm-driven sediment transport, and to anonymous reviewers whose helpful and detailed comments improved this manuscript. This research was supported by National Science Foundation Grant DEB-0089654. This publication represents contribution 871 of the Smithsonian Marine Station at Fort Pierce. NR 92 TC 11 Z9 11 U1 1 U2 10 PU SPRINGER HEIDELBERG PI HEIDELBERG PA TIERGARTENSTRASSE 17, D-69121 HEIDELBERG, GERMANY SN 0025-3162 EI 1432-1793 J9 MAR BIOL JI Mar. Biol. PD MAR PY 2012 VL 159 IS 3 BP 661 EP 674 DI 10.1007/s00227-011-1844-y PG 14 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA 913BN UT WOS:000301846400017 ER PT J AU Werner, VR Laughinghouse, HD Fiore, MF Sant'Anna, CL Hoff, C Santos, KRD Neuhaus, EB Molica, RJR Honda, RY Echenique, RO AF Werner, Vera Regina Laughinghouse, Haywood Dail Fiore, Marli Fatima Sant'Anna, Celia Leite Hoff, Caroline de Souza Santos, Kleber Renan Neuhaus, Emanuel Bruno Reis Molica, Renato Jose Honda, Ricardo Yukio Omar Echenique, Ricardo TI Morphological and molecular studies of Sphaerospermopsis torques-reginae (Cyanobacteria, Nostocales) from South American water blooms SO PHYCOLOGIA LA English DT Article DE 16S rRNA gene; Anabaena torques-reginae; Cyanobacteria; Dolichospermum; Ecology; Geographic distribution; Morphology; Phylogeny; Toxicity ID MAXIMUM-LIKELIHOOD; ANABAENA; DOLICHOSPERMUM; APHANIZOMENON AB Sphaerospermopsis torques-reginae (Komarek) Werner, Laughinghouse IV, Fiore & Sant'Anna comb. nov. was originally described as Anabaena torques-reginae Komarek from planktonic populations of Cuban eutrophic environments, characterized by twisted trichomes with spherical akinetes adjacent to the heterocytes. Recently, using molecular analyses, all planktonic Anabaena Bory ex Bornet & Flahault morphospecies were transferred into the genus Dolichospermum (Ralfs ex Bornet & Flahault) Wacklin el al., including Dolichospermum torques-reginae (Komarek) Wacklin et al. However, by a polyphasic characterization of strains of Anabaena reniformis Lemmermann and Aphanizomenon aphanizomenoides (Forti) Horecka & Komarek (=Anabaena aphanizomenoides Forti), these planktonic species were reclassified into Sphaerospermopsis Zapomelova et al. Our study's main objective was to characterize morphologically and molecularly cyanobacterial populations identified as Dolichospermum torques-reginae, observed in different aquatic ecosystems in South America. The 16S rRNA gene of two Dolichospermum torques-reginae strains (ITEP-024 and ITEP-026) was sequenced and phylogenetically analyzed for the first time. The morphological and phylogenetic analyses demonstrated the affiliation of the studied populations with the genus Sphaerospermopsis and, consequently, were denominated as Sphaerospermopsis torques-reginae. Furthermore, geographic distribution, ecology, and toxicity of the species are discussed. It was observed in different aquatic environments, natural and artificial, tropical and subtropical in Brazil, temperate in Argentina, and tropical in Colombia, suggesting a wide distribution in South America. It normally occurred in dense freshwater blooms, although it was also found in water with low salinity. Sphaerospermopsis torques-reginae toxic blooms have been reported in tropical water bodies in northeastern Brazil. C1 [Werner, Vera Regina; Neuhaus, Emanuel Bruno] Zoobot Fdn Rio Grande do Sul, Museum Nat Sci, Porto Alegre, RS, Brazil. [Laughinghouse, Haywood Dail] Natl Museum Nat Hist, Smithsonian Inst, Dept Bot, Washington, DC 20560 USA. [Laughinghouse, Haywood Dail] Univ Maryland, Coll Comp Math & Nat Sci, MEES Program, College Pk, MD 20742 USA. [Fiore, Marli Fatima; Hoff, Caroline; Honda, Ricardo Yukio] Univ Sao Paulo, Ctr Nucl Energy Agr, Piracicaba, SP, Brazil. [Sant'Anna, Celia Leite; de Souza Santos, Kleber Renan] Inst Bot, Sect Phycol, Sao Paulo, Brazil. [Reis Molica, Renato Jose] Univ Fed Rural Pernambuco, Garanhuns, PE, Brazil. [Omar Echenique, Ricardo] UNLP, Coll Nat Sci & Museum, Phycol Sci Dept, La Plata, Argentina. [Omar Echenique, Ricardo] Sci Res Commiss Buenos Aires Prov, La Plata, Argentina. RP Werner, VR (reprint author), Zoobot Fdn Rio Grande do Sul, Museum Nat Sci, Porto Alegre, RS, Brazil. EM vera-werner@fzb.rs.gov.br RI SantAnna, Celia/G-2420-2012; Molica, Renato /J-2630-2012; Hoff Risseti, Caroline/K-6138-2012; Sant' Anna, Celia/D-3735-2015; Fiore, Marli/C-1436-2012; Laughinghouse, Haywood/M-5836-2016 OI Fiore, Marli/0000-0003-2555-7967; Laughinghouse, Haywood/0000-0003-1018-6948 FU CNPq (PIBIC - MCN/FZBRS) [142749/2009-5, 308299/2009-4]; FAPESP [2007/07075-5]; Ministry of Education Agency (CAPES) FX We especially thank Dr Jiri Komarek and Dr Masayuki Watanabe (in memoriam) for their valuable comments; to CNPq (PIBIC - MCN/FZBRS) for financial support to H.D. Laughinghouse IV and E.B. Neuhaus, graduate scholarship to C. Hoff (142749/2009-5), and research fellowship to M.F. Fiore (308299/2009-4); to FAPESP for financial support to M.F. Fiore (2007/07075-5); to the Ministry of Education Agency (CAPES) for the graduate scholarship to R.Y. Honda; to Dr Clarisse Odebrecht and Dr Marli Bergesch (FURG - Rio Grande, Brazil), and to Dr Juan Pablo Alvarez Silva (National University of Colombia) for providing some of the studied samples; to Rejane Rosa and to Arlete leda Pasqualetto and Everton Luis Luz de Quadros from MCN/FZBRS, for passing Indian ink on the line drawings for final print and for designing the maps, respectively; to Felipe Secco Richter for his technical help. NR 36 TC 10 Z9 11 U1 1 U2 11 PU INT PHYCOLOGICAL SOC PI LAWRENCE PA NEW BUSINESS OFFICE, PO BOX 1897, LAWRENCE, KS 66044-8897 USA SN 0031-8884 J9 PHYCOLOGIA JI Phycologia PD MAR PY 2012 VL 51 IS 2 BP 228 EP 238 DI 10.2216/11-32.1 PG 11 WC Plant Sciences; Marine & Freshwater Biology SC Plant Sciences; Marine & Freshwater Biology GA 913RN UT WOS:000301895200009 ER PT J AU Oftedal, OT AF Oftedal, O. T. TI The evolution of milk secretion and its ancient origins SO ANIMAL LA English DT Article DE evolution; lactation; milk composition; casein; milk fat globule ID WHEY ACIDIC PROTEIN; LACTATING MAMMARY-GLAND; INNATE IMMUNE-SYSTEM; XANTHINE-OXIDOREDUCTASE; ALPHA-LACTALBUMIN; BETA-LACTOGLOBULIN; TRICHOSURUS-VULPECULA; SKIN SECRETIONS; CHEMICAL-CHARACTERIZATION; ARCTOCEPHALUS-GAZELLA AB Lactation represents an important element of the life history strategies of all mammals, whether monotreme, marsupial, or eutherian. Milk originated as a glandular skin secretion in synapsids (the lineage ancestral to mammals), perhaps as early as the Pennsylvanian period, that is, approximately 310 million years ago (mya). Early synapsids laid eggs with parchment-like shells intolerant of desiccation and apparently dependent on glandular skin secretions for moisture. Mammary glands probably evolved from apocrine-like glands that combined multiple modes of secretion and developed in association with hair follicles. Comparative analyses of the evolutionary origin of milk constituents support a scenario in which these secretions evolved into a nutrient-rich milk long before mammals arose. A variety of antimicrobial and secretory constituents were co-opted into novel roles related to nutrition of the young. Secretory calcium-binding phosphoproteins may originally have had a role in calcium delivery to eggs; however, by evolving into large, complex casein micelles, they took on an important role in transport of amino acids, calcium and phosphorus. Several proteins involved in immunity, including an ancestral butyrophilin and xanthine oxidoreductase, were incorporated into a novel membrane-bound lipid droplet (the milk fat globule) that became a primary mode of energy transfer. An ancestral c-lysozyme lost its lytic functions in favor of a role as alpha-lactalbumin, which modifies a galactosyltransferase to recognize glucose as an acceptor, leading to the synthesis of novel milk sugars, of which free oligosaccharides may have predated free lactose. An ancestral lipocalin and an ancestral whey acidic protein four-disulphide core protein apparently lost their original transport and antimicrobial functions when they became the whey proteins beta-lactoglobulin and whey acidic protein, which with alpha-lactalbumin provide limiting sulfur amino acids to the young. By the late Triassic period (ca 210 mya), mammaliaforms (mammalian ancestors) were endothermic (requiring fluid to replace incubatory water losses of eggs), very small in size (making large eggs impossible), and had rapid growth and limited tooth replacement (indicating delayed onset of feeding and reliance on milk). Thus, milk had already supplanted egg yolk as the primary nutrient source, and by the Jurassic period (ca 170 mya) vitellogenin genes were being lost. All primary milk constituents evolved before the appearance of mammals, and some constituents may have origins that predate the split of the synapsids from sauropsids (the lineage leading to 'reptiles' and birds). Thus, the modern dairy industry is built upon a very old foundation, the cornerstones of which were laid even before dinosaurs ruled the earth in the Jurassic and Cretaceous periods. C1 Smithsonian Environm Res Ctr, Smithsonian Inst, Edgewater, MD 21037 USA. RP Oftedal, OT (reprint author), Smithsonian Environm Res Ctr, Smithsonian Inst, POB 28, Edgewater, MD 21037 USA. EM oftedalo@si.edu NR 151 TC 42 Z9 42 U1 8 U2 118 PU CAMBRIDGE UNIV PRESS PI CAMBRIDGE PA EDINBURGH BLDG, SHAFTESBURY RD, CB2 8RU CAMBRIDGE, ENGLAND SN 1751-7311 EI 1751-732X J9 ANIMAL JI Animal PD MAR PY 2012 VL 6 IS 3 BP 355 EP 368 DI 10.1017/S1751731111001935 PG 14 WC Agriculture, Dairy & Animal Science; Veterinary Sciences SC Agriculture; Veterinary Sciences GA 896AK UT WOS:000300537600002 PM 22436214 ER PT J AU Kruse, I Hare, MP Hines, AH AF Kruse, Inken Hare, Matthew P. Hines, Anson H. TI Genetic relationships of the marine invasive crab parasite Loxothylacus panopaei: an analysis of DNA sequence variation, host specificity, and distributional range SO BIOLOGICAL INVASIONS LA English DT Article DE Phylogeography; Mitochondrial introgression; Nuclear DNA; Rhizocephala; Sacculinidae ID MUD CRABS; CIRRIPEDIA RHIZOCEPHALA; MITOCHONDRIAL; CASTRATOR; TREES; PREVALENCE; DIVERSITY; XANTHIDAE; ABUNDANCE; BRACHYURA AB Host specificity is a key variable of the niche breath of parasites that can be an important determinant of a parasite's ability to invade new areas. There is increasing evidence that many parasite species may comprise a variety of genetically variable lineages, which differ in host specificity and geographic range. In this study, we (1) explored the extent of diversity in the invasive parasitic barnacle Loxothylacus panopaei (Rhizocephala) infecting mud crabs (2) examined the geographic origin for the invasive lineage and (3) assessed if further southward spread of the parasite may be impeded. Along the US Atlantic coast, L. panopaei infects different hosts in its invaded range (Chesapeake Bay to north of Cape Canaveral) compared to one portion of the native range in Southeast Florida. This difference was reflected in genetic lineages on two independent loci, mitochondrial cytochrome oxidase I and nuclear cytochrome c. Both loci were concordant in that they showed one lineage infecting crabs of the genus Panopeus in the native range and one lineage infecting Eurypanopeus depressus and Rhithropanopeus harrisii hosts in the invaded range and in the Gulf of Mexico, thus indicating Gulf of Mexico populations as the most likely source of introduction into Chesapeake Bay. Interestingly, the nuclear marker resolved an additional lineage of parasites infecting panopeid hosts in the native range. All three parasite lineages were well supported, but a decision about species status must await further analyses. Since its introduction in the 1960s, the invasive L. panopaei lineage has expanded its range southward along the US Atlantic coast, now almost reaching the northern limit of native Panopeus-infecting lineages at Cape Canaveral, Florida. We hypothesized that parasite-free E. depressus in Southeast Florida, living in sympatry with infected panopeid populations, might be resistant to infection by the invasive lineage. Our infection experiments rejected this hypothesis, suggesting that any impediment to further southward range expansion might be expected from temperature regimes of the subtropical zoogeographic region south of Cape Canaveral. C1 [Kruse, Inken] Smithsonian Marine Stn, Ft Pierce, FL 34949 USA. [Hare, Matthew P.] Cornell Univ, Dept Nat Resources, Ithaca, NY 14853 USA. [Hines, Anson H.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. RP Kruse, I (reprint author), IFM GEOMAR, Leibniz Inst Meereswissensch, Dusternbrooker Weg 20, D-24105 Kiel, Germany. EM ikruse@ifm-geomar.de RI Kruse, Inken/G-2624-2013; Kruse, Inken/E-4207-2014; Kruse, Inken/B-5949-2016 FU Smithsonian Institution; Smithsonian Marine Science Network FX We wish to thank S. Reed, T. and E.-G. Kruse, D. Beissel, S. Altman, P. Rodgers and J. O'Brien for help on field trips and the rest of the staff at SMS at Fort Pierce for general support. Specimens of L. panopaei from Fort Myers were kindly provided by G. Tolley. We are grateful to D. Felder for species identifications of panopaeid crabs and to W. Herrnkind for sampling advice for the Florida panhandle. Christoph Bleidorn, associate editor Carol A. Stepien and three anonymous reviewers provided valuable comments to drafts of the manuscript. This work was supported by a 'Postdoctoral Fellowship at the Smithsonian Marine Station at Fort Pierce' from the Smithsonian Institution to I. K. and by Smithsonian Marine Science Network funds to A. H. H. NR 48 TC 8 Z9 8 U1 0 U2 25 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 1387-3547 J9 BIOL INVASIONS JI Biol. Invasions PD MAR PY 2012 VL 14 IS 3 BP 701 EP 715 DI 10.1007/s10530-011-0111-y PG 15 WC Biodiversity Conservation; Ecology SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 907UT UT WOS:000301445100019 ER PT J AU Lu, JM Wen, J Lutz, S Wang, YP Li, DZ AF Lu, Jin-Mei Wen, Jun Lutz, Sue Wang, Yi-Ping Li, De-Zhu TI Phylogenetic relationships of Chinese Adiantum based on five plastid markers SO JOURNAL OF PLANT RESEARCH LA English DT Article DE Adiantum; China; Diversification; Molecular phylogeny; Plastid markers; Pteridaceae ID RBCL NUCLEOTIDE-SEQUENCES; CHEILANTHOID FERNS; EXTANT FERNS; PTERIDACEAE; DNA; DRYOPTERIDACEAE; GENERA; MODEL AB Adiantum consists of about 150-200 species mostly with a pantropical distribution, yet the classifications of Adiantum have been based primarily on regional studies. Confounding the clarity of reconstructing the evolutionary history of Adiantum is that previous molecular phylogenetic studies suggest that a separate and distinctive clade, the vittarioids, may be derived from within Adiantum. Five plastid markers (atpA, atpB, rbcL, trnL-F and rps4-trnS) are employed to assess the monophyly of Adiantum, and construct the molecular phylogeny of Chinese Adiantum. Our analyses support the monophyly of Adiantum. All temperate Adiantum species form a clade nested within the pantropical grade, suggesting a tropical origin of Adiantum. Six main clades are supported within Chinese Adiantum, which are only partially consistent with Lin's classification of the genus. Series Caudata is polyphyletic with series Gravesiana nested within one subgroup of series Caudata. The prolonged whip-like stolon at the apex of the fronds is the defining character for series Caudata, but it may have evolved multiple times. Adiantum reniforme with the simple fronds is sister to series Venusta, which has a decompound lamina with many flabellate to cuneate segments. Series Veneri-capilliformia is not monophyletic, with A. capillus-veneris sister to series Flabellulata except for A. diaphanum, and A. edentulum sister to series Pedata. Series Flabellulata is biphyletic with A. diaphanum nested within the pantropical grade. The phylogeny suggests that convergent evolution in frond architecture has occurred in Adiantum. C1 [Wen, Jun; Lutz, Sue] Natl Museum Nat Hist, Dept Bot, Smithsonian Inst, Washington, DC 20013 USA. [Lu, Jin-Mei] Chinese Acad Sci, Kunming Inst Bot, Lab Plant Biodivers & Biogeog, Kunming 650204, Yunnan, Peoples R China. [Wang, Yi-Ping] Jiangxi Agr Univ, Coll Agr, Nanchang 330045, Jiangxi, Peoples R China. [Li, De-Zhu] Chinese Acad Sci, Plant Germplasm & Genom Ctr, Germplasm Bank Wild Species, Kunming Inst Bot, Kunming 650204, Yunnan, Peoples R China. RP Wen, J (reprint author), Natl Museum Nat Hist, Dept Bot, Smithsonian Inst, MRC 166, Washington, DC 20013 USA. EM lujinmei@mail.kib.ac.cn; WENJ@si.edu; LUTZS@si.edu; wangyp1123@gmail.com; DZL@mail.kib.ac.cn OI li, de zhu/0000-0002-4990-724X FU National Natural Science Foundation of China [31070199, 30800063]; Chinese Academy of Sciences [2010KIBA02, 2009-LSF-GBOWS-01]; John D. and Catherine T. MacArthur Foundation FX We thank Xiao Cheng, Yu-xiao Zhang, Li-Yaung Kuo, Akiko Soejima and Tom Heutte for sample collection, and Elizabeth Zimmer for providing primers. The study was supported by the National Natural Science Foundation of China (Grant no. 31070199, 30800063), the Project of Knowledge Innovation Program of the Chinese Academy of Sciences (Grant no.: 2010KIBA02), the Research Fund for the Large-scale Scientific Facilities of the Chinese Academy of Sciences (Grant no. 2009-LSF-GBOWS-01), and the John D. and Catherine T. MacArthur Foundation (to J. Wen, R. Ree and G. Mueller). NR 49 TC 19 Z9 23 U1 1 U2 14 PU SPRINGER JAPAN KK PI TOKYO PA CHIYODA FIRST BLDG EAST, 3-8-1 NISHI-KANDA, CHIYODA-KU, TOKYO, 101-0065, JAPAN SN 0918-9440 J9 J PLANT RES JI J. Plant Res. PD MAR PY 2012 VL 125 IS 2 BP 237 EP 249 DI 10.1007/s10265-011-0441-y PG 13 WC Plant Sciences SC Plant Sciences GA 907XJ UT WOS:000301452900004 PM 21809178 ER PT J AU Selvans, MM Clayton, RW Stock, JM Granot, R AF Selvans, M. M. Clayton, R. W. Stock, J. M. Granot, R. TI Using overlapping sonobuoy data from the Ross Sea to construct a 2D deep crustal velocity model SO MARINE GEOPHYSICAL RESEARCH LA English DT Article DE Sonobuoy; Multi-channel seismic; Ross Sea; Finite-difference; 2D velocity model; Crustal structure ID CONTINENTAL-MARGIN; WAVE-FIELD; ANTARCTICA; INVERSION; TRANSECT; SVALBARD; LAND AB Sonobuoys provide an alternative to using long streamers while conducting multi-channel seismic (MCS) studies, in order to provide deeper velocity control. We present analysis and modeling techniques for interpreting the sonobuoy data and illustrate the method with ten overlapping sonobuoys collected in the Ross Sea, offshore from Antarctica. We demonstrate the importance of using the MCS data to correct for ocean currents and changes in ship navigation, which is required before using standard methods for obtaining a 1D velocity profile from each sonobuoy. We verify our 1D velocity models using acoustic finite-difference (FD) modeling and by performing depth migration on the data, and demonstrate the usefulness of FD modeling for tying interval velocities to the shallow crust imaged using MCS data. Finally, we show how overlapping sonobuoys along an MCS line can be used to construct a 2D velocity model of the crust. The velocity model reveals a thin crust (5.5 +/- A 0.4 km) at the boundary between the Adare and Northern Basins, and implies that the crustal structure of the Northern Basin may be more similar to that of the oceanic crust in the Adare Basin than to the stretched continental crust further south in the Ross Sea. C1 [Selvans, M. M.] Smithsonian Inst, Natl Air & Space Museum, Ctr Earth & Planetary Studies, Washington, DC 20560 USA. [Selvans, M. M.; Clayton, R. W.; Stock, J. M.] CALTECH, Seismol Lab, Pasadena, CA 91125 USA. [Granot, R.] Ben Gurion Univ Negev, Dept Geol & Environm Sci, IL-84105 Beer Sheva, Israel. RP Selvans, MM (reprint author), Smithsonian Inst, Natl Air & Space Museum, Ctr Earth & Planetary Studies, MRC 315, Washington, DC 20560 USA. EM selvans@gps.caltech.edu RI Granot, Roi /F-4555-2012; OI Stock, Joann Miriam/0000-0003-4816-7865 FU National Science Foundation [OPP04-40959, OPP-0440923, OPP-0944711] FX We would like to thank Captain Mike Watson, the crew, and the Raytheon Polar Services Corporation technical staff on board the Nathaniel B. Palmer. This study was supported by National Science Foundation grants OPP04-40959 (S. Cande) and OPP-0440923 and OPP-0944711 (J. Stock and R. Clayton). NR 22 TC 2 Z9 2 U1 0 U2 2 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0025-3235 J9 MAR GEOPHYS RES JI Mar. Geophys. Res. PD MAR PY 2012 VL 33 IS 1 BP 17 EP 32 DI 10.1007/s11001-011-9143-z PG 16 WC Geochemistry & Geophysics; Oceanography SC Geochemistry & Geophysics; Oceanography GA 909RA UT WOS:000301580700002 ER PT J AU Aebil, A Vaissiere, BE vanEngelsdorp, D Delaplane, KS Roubik, DW Neumann, P AF Aebil, Alexandre Vaissiere, Bernard E. vanEngelsdorp, Dennis Delaplane, Keith S. Roubik, David W. Neumann, Peter TI Back to the future: Apis versus non-Apis pollination-a response to Ollerton et al. SO TRENDS IN ECOLOGY & EVOLUTION LA English DT Letter ID AFRICANIZED HONEY-BEE; BUMBLE BEES; DECLINE; IMPACT C1 [Neumann, Peter] Agroscope Liebefeld Posieux, Swiss Bee Res Ctr, Res Stn ALP, CH-3003 Bern, Switzerland. [Neumann, Peter] Rhodes Univ, Dept Zool & Entomol, ZA-6140 Grahamstown, South Africa. [Aebil, Alexandre] Agroscope Reckenholz Tanikon, Res Stn ART, CH-8046 Zurich, Switzerland. [Vaissiere, Bernard E.] INRA, UMR Abeilles & Environm INRA UAPV 406, F-84914 Avignon 9, France. [vanEngelsdorp, Dennis] Univ Maryland, Dept Entomol, College Pk, MD 20742 USA. [Delaplane, Keith S.] Univ Georgia, Dept Entomol, Athens, GA 30602 USA. [Roubik, David W.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. RP Neumann, P (reprint author), Agroscope Liebefeld Posieux, Swiss Bee Res Ctr, Res Stn ALP, Schwarzenburgstr 161, CH-3003 Bern, Switzerland. EM peter.neumann@alp.admin.ch RI Aebi, Alexandre/B-7482-2013; vanEngelsdorp, Dennis/E-7934-2010 NR 12 TC 22 Z9 22 U1 1 U2 75 PU ELSEVIER SCIENCE LONDON PI LONDON PA 84 THEOBALDS RD, LONDON WC1X 8RR, ENGLAND SN 0169-5347 J9 TRENDS ECOL EVOL JI Trends Ecol. Evol. PD MAR PY 2012 VL 27 IS 3 BP 142 EP 143 DI 10.1016/j.tree.2011.11.017 PG 2 WC Ecology; Evolutionary Biology; Genetics & Heredity SC Environmental Sciences & Ecology; Evolutionary Biology; Genetics & Heredity GA 910KM UT WOS:000301635600004 ER PT J AU Stine, JK AF Stine, Jeffrey K. TI The Fall and Rise of the Wetlands of California's Great Central Valley. SO WESTERN HISTORICAL QUARTERLY LA English DT Book Review C1 [Stine, Jeffrey K.] Smithsonian Inst, Washington, DC 20560 USA. RP Stine, JK (reprint author), Smithsonian Inst, Washington, DC 20560 USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU OXFORD UNIV PRESS INC PI CARY PA JOURNALS DEPT, 2001 EVANS RD, CARY, NC 27513 USA SN 0043-3810 EI 1939-8603 J9 WESTERN HIST QUART JI West. Hist. Q. PD SPR PY 2012 VL 43 IS 1 BP 103 EP 104 PG 2 WC History SC History GA 905XC UT WOS:000301308500033 ER PT J AU Power, ML Ross, CN Schulkin, J Tardif, SD AF Power, Michael L. Ross, Corinna N. Schulkin, Jay Tardif, Suzette D. TI The Development of Obesity Begins at an Early Age in Captive Common Marmosets (Callithrix jacchus) SO AMERICAN JOURNAL OF PRIMATOLOGY LA English DT Article DE primates; body composition; adiposity; childhood obesity ID BODY COMPOSITION ANALYSIS; NONHUMAN PRIMATE; PRESCHOOL-CHILDREN; DIABETES-MELLITUS; ADIPOSE-TISSUE; MONKEYS; PREVALENCE; CHILDHOOD; ASSOCIATION; OVERWEIGHT AB Animal models to study the causes and consequences of obesity during infancy in humans would be valuable. In this study, we examine the patterns of fat mass gain from birth to 12 months in common marmosets (Callithrix jacchus). Lean and fat mass was measured by quantitative magnetic resonance at 1, 2, 6, and 12 months for 31 marmosets, 15 considered Normal and 16 considered Fat (>14% body fat) at 12 months. Animals were fed either the regular colony diet mix or a high-fat variation. Subjects classified as Fat at 12 months already had greater lean mass (198.4 +/- 6.2 g vs. 174.0 +/- 6.8 g, P = 0.013) and fat mass (45.5 +/- 5.0 g vs. 24.9 +/- 3.4 g, P = .002) by 6 months. Body mass did not differ between groups prior to 6 months, however, by 1 month, Fat infants had greater percent body fat. Percent body fat decreased between 1 and 12 months in Normal subjects; in Fat subjects, it increased. The high-fat diet was associated with body fat >14% at 6 months (P = 0.049), but not at 12 months. This shift was due to three subjects on the normal diet changing from Normal to Fat between 6 and 12 months. Although maternal prepregnancy adiposity did not differ, overall, between Normal and Fat subjects, the subjects Normal at 6 and Fat at 12 months all had Fat mothers. Therefore, diet and maternal obesity appear to have potentially independent effects that may also vary with developmental age. Although birth weight did not differ between groups, it was associated with fat mass gain from 1 to 6 months in animals with >14% body fat at 6 months of age (r = 0.612, P = 0.026); but not in 6-month-old animals with <14% body fat (r = -0.012, P = 0.964). Excess adiposity in captive marmosets develops by 1 month. Birth weight is associated with adiposity in animals vulnerable to obesity. Am. J. Primatol. 74: 261-269, 2012. (C) 2012 Wiley Periodicals, Inc. C1 [Power, Michael L.] Smithsonian Conservat Biol Inst, Nutr Lab, Conservat Ecol Ctr, Washington, DC 20013 USA. [Power, Michael L.; Schulkin, Jay] Amer Coll Obstetricians & Gynecologists, Res Dept, Washington, DC 20024 USA. [Ross, Corinna N.; Tardif, Suzette D.] Univ Texas Hlth Sci Ctr San Antonio, Barshop Inst Longev & Aging Studies, San Antonio, TX 78229 USA. [Schulkin, Jay] Georgetown Univ, Dept Neurosci, Washington, DC USA. RP Power, ML (reprint author), Smithsonian Conservat Biol Inst, Nutr Lab, Conservat Ecol Ctr, Natl Zool Pk,POB 37012,MRC 5503, Washington, DC 20013 USA. EM mpower@acog.org OI Power, Michael/0000-0002-6120-3528 FU PHS [R01 DK077639] FX Contract grant sponsor: PHS; contract grant number: R01 DK077639. NR 25 TC 8 Z9 8 U1 0 U2 17 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0275-2565 J9 AM J PRIMATOL JI Am. J. Primatol. PD MAR PY 2012 VL 74 IS 3 BP 261 EP 269 DI 10.1002/ajp.21995 PG 9 WC Zoology SC Zoology GA 904YO UT WOS:000301236000009 PM 24006544 ER PT J AU Kenyon, SJ Bromley, BC AF Kenyon, Scott J. Bromley, Benjamin C. TI COAGULATION CALCULATIONS OF ICY PLANET FORMATION AT 15-150 AU: A CORRELATION BETWEEN THE MAXIMUM RADIUS AND THE SLOPE OF THE SIZE DISTRIBUTION FOR TRANS-NEPTUNIAN OBJECTS SO ASTRONOMICAL JOURNAL LA English DT Article DE Kuiper Belt: general; planetary systems; planets and satellites: formation; planets and satellites: physical evolution ID KUIPER-BELT OBJECTS; OUTER SOLAR-SYSTEM; LATE HEAVY BOMBARDMENT; GAS GIANT PLANETS; LUMINOSITY FUNCTION; RUNAWAY GROWTH; DEBRIS DISKS; TRANSNEPTUNIAN BINARIES; COLLISIONAL EVOLUTION; ACCRETIONAL EVOLUTION AB We investigate whether coagulation models of planet formation can explain the observed size distributions of trans-Neptunian objects (TNOs). Analyzing published and new calculations, we demonstrate robust relations between the size of the largest object and the slope of the size distribution for sizes 0.1 km and larger. These relations yield clear, testable predictions for TNOs and other icy objects throughout the solar system. Applying our results to existing observations, we show that a broad range of initial disk masses, planetesimal sizes, and fragmentation parameters can explain the data. Adding dynamical constraints on the initial semimajor axis of "hot" Kuiper Belt objects along with probable TNO formation times of 10-700 Myr restricts the viable models to those with a massive disk composed of relatively small (1-10 km) planetesimals. C1 [Kenyon, Scott J.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. [Bromley, Benjamin C.] Univ Utah, Dept Phys, Salt Lake City, UT 84112 USA. RP Kenyon, SJ (reprint author), Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA. EM skenyon@cfa.harvard.edu; bromley@physics.utah.edu OI Kenyon, Scott/0000-0003-0214-609X FU NASA [NNX10AF35G, NNX11AM37G]; NASA TPF Foundation [NNG06GH25G]; Spitzer Guest Observer Program [20132]; Smithsonian Institution FX We acknowledge generous allotments of computer time on the NASA "discover" cluster, the SI "hydra" cluster, and the "cosmos" cluster at the Jet Propulsion Laboratory. We thank S. Weidenschilling for a careful and timely review. Advice and comments from W. Fraser, M. Geller, M. Holman, and A. Youdin also greatly improved our presentation. Portions of this project were supported by the NASA Astrophysics Theory and Origins of Solar Systems programs through grant NNX10AF35G, the NASA TPF Foundation Science Program through grant NNG06GH25G, the NASA Outer Planets Program through grant NNX11AM37G, the Spitzer Guest Observer Program through grant 20132, and grants from the endowment and scholarly studies programs of the Smithsonian Institution. NR 141 TC 26 Z9 26 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 J9 ASTRON J JI Astron. J. PD MAR PY 2012 VL 143 IS 3 AR 63 DI 10.1088/0004-6256/143/3/63 PG 21 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 898IK UT WOS:000300735600009 ER PT J AU Shin, MS Yi, H Kim, DW Chang, SW Byun, YI AF Shin, Min-Su Yi, Hahn Kim, Dae-Won Chang, Seo-Won Byun, Yong-Ik TI DETECTING VARIABILITY IN MASSIVE ASTRONOMICAL TIME-SERIES DATA. II. VARIABLE CANDIDATES IN THE NORTHERN SKY VARIABILITY SURVEY SO ASTRONOMICAL JOURNAL LA English DT Article DE astronomical databases: miscellaneous; methods: data analysis; methods: statistical; stars: variables: general ID RR LYRAE STARS; ASYMPTOTIC GIANT BRANCH; SQUARE SUCCESSIVE DIFFERENCE; IMAGE-SUBTRACTION PHOTOMETRY; GAUSSIAN MIXTURE MODEL; LARGE-MAGELLANIC-CLOUD; YOUNG STELLAR OBJECTS; POST-AGB OBJECTS; ALL-SKY; AUTOMATED SURVEY AB We present variability analysis of data from the Northern Sky Variability Survey (NSVS). Using the clustering method, which defines variable candidates as outliers from large clusters, we cluster 16,189,040 light curves having data points at more than 15 epochs as variable and non-variable candidates in 638 NSVS fields. Variable candidates are selected depending on how strongly they are separated from the largest cluster and how rarely they are grouped together in eight-dimensional space spanned by variability indices. All NSVS light curves are also cross-correlated with IRAS, AKARI, Two Micron All Sky Survey, Sloan Digital Sky Survey (SDSS), and GALEX objects, as well as known objects in the SIMBAD database. The variability analysis and cross-correlation results are provided in a public online database, which can be used to select interesting objects for further investigation. Adopting conservative selection criteria for variable candidates, we find about 1.8 million light curves as possible variable candidates in the NSVS data, corresponding to about 10% of our entire NSVS sample. Multi-wavelength colors help us find specific types of variability among the variable candidates. Moreover, we also use morphological classification from other surveys such as SDSS to suppress spurious cases caused by blending objects or extended sources due to the low angular resolution of the NSVS. C1 [Shin, Min-Su] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Yi, Hahn; Kim, Dae-Won; Chang, Seo-Won] Yonsei Univ, Dept Astron, Seoul 120749, South Korea. [Byun, Yong-Ik] Yonsei Univ, Dept Astron & Univ Observ, Seoul 120749, South Korea. [Kim, Dae-Won] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 01238 USA. RP Shin, MS (reprint author), Univ Michigan, Dept Astron, 500 Church St, Ann Arbor, MI 48109 USA. EM msshin@umich.edu; yihahn@galaxy.yonsei.ac.kr; dakim@cfa.harvard.edu; seowony@galaxy.yonsei.ac.kr; ybyun@yonsei.ac.kr FU National Research Foundation of Korea [2011-0030875]; Department of Energy; National Aeronautics and Space Administration; National Science Foundation; Alfred P. Sloan Foundation; U.S. Department of Energy; Japanese Monbukagakusho; Max Planck Society; Higher Education Funding Council for England FX We thank Bernie Shao and Przemek Wozniak for helping us access the GALEX data and the NSVS light curves, respectively. We also thank Michael Sekora, Charles Cowley, Mark Reynolds, and Stefan Kraus for useful discussions and careful reading. We are grateful to the anonymous referee for comments that improved this manuscript. Y.I.B. acknowledges the support of the National Research Foundation of Korea through grant 2011-0030875.; This publication makes use of data from the Northern Sky Variability Survey created jointly by the Los Alamos National Laboratory and the University of Michigan. The NSVS was funded by the Department of Energy, the National Aeronautics and Space Administration, and the National Science Foundation. This research has made use of the SIMBAD database, operated at CDS, Strasbourg, France. This research is based on observations with AKARI, a JAXA project with the participation of ESA. This publication also 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. Funding for the SDSS and SDSS-II has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, the U.S. Department of Energy, the National Aeronautics and Space Administration, the Japanese Monbukagakusho, the Max Planck Society, and the Higher Education Funding Council for England. The SDSS Web site is http://www.sdss.org/. The SDSS is managed by the Astrophysical Research Consortium for the Participating Institutions. The Participating Institutions are the American Museum of Natural History, Astrophysical Institute Potsdam, University of Basel, University of Cambridge, Case Western Reserve University, University of Chicago, Drexel University, Fermilab, the Institute for Advanced Study, the Japan Participation Group, Johns Hopkins University, the Joint Institute for Nuclear Astrophysics, the Kavli Institute for Particle Astrophysics and Cosmology, the Korean Scientist Group, the Chinese Academy of Sciences (LAMOST), Los Alamos National Laboratory, the Max-Planck-Institute for Astronomy (MPIA), the Max-Planck-Institute for Astrophysics (MPA), New Mexico State University, Ohio State University, University of Pittsburgh, University of Portsmouth, Princeton University, the United States Naval Observatory, and the University of Washington. The Galaxy Evolution Explorer (GALEX) is a NASA Small Explorer, launched in 2003 April. We gratefully acknowledge NASA's support for construction, operation, and science analysis for the GALEX mission, developed in cooperation with the Centre National d'Etudes Spatiales (CNES) of France and the Korean Ministry of Science and Technology. NR 121 TC 3 Z9 3 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 EI 1538-3881 J9 ASTRON J JI Astron. J. PD MAR PY 2012 VL 143 IS 3 AR 65 DI 10.1088/0004-6256/143/3/65 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 898IK UT WOS:000300735600011 ER PT J AU Farrell, SA Servillat, M Pforr, J Maccarone, TJ Knigge, C Godet, O Maraston, C Webb, NA Barret, D Gosling, AJ Belmont, R Wiersema, K AF Farrell, S. A. Servillat, M. Pforr, J. Maccarone, T. J. Knigge, C. Godet, O. Maraston, C. Webb, N. A. Barret, D. Gosling, A. J. Belmont, R. Wiersema, K. TI A YOUNG MASSIVE STELLAR POPULATION AROUND THE INTERMEDIATE-MASS BLACK HOLE ESO 243-49 HLX-1 SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE accretion, accretion disks; galaxies: interactions; galaxies: star clusters: general; globular clusters: general; X-rays: binaries; X-rays: individual (ESO 243-49 HLX-1) ID X-RAY SOURCE; GLOBULAR-CLUSTERS; STAR-CLUSTERS; MILKY-WAY; ACCRETION; GALAXY; MODELS; CATALOG; DISC AB We present Hubble Space Telescope and simultaneous Swift X-ray Telescope observations of the strongest candidate intermediate-mass black hole (IMBH) ESO 243-49 HLX-1. Fitting the spectral energy distribution from X-ray to near-infrared wavelengths showed that the broadband spectrum is not consistent with simple and irradiated disk models, but is well described by a model comprised of an irradiated accretion disk plus a similar to 10(6) M-circle dot stellar population. The age of the population cannot be uniquely constrained, with both young and old stellar populations allowed. However, the old solution requires excessive disk reprocessing and an extremely small disk, so we favor the young solution (similar to 13 Myr). In addition, the presence of dust lanes and the lack of any nuclear activity from X-ray observations of the host galaxy suggest that a gas-rich minor merger may have taken place less than similar to 200 Myr ago. Such a merger event would explain the presence of the IMBH and the young stellar population. C1 [Farrell, S. A.] Univ Sydney, Sch Phys, Sydney Inst Astron SIfA, Sydney, NSW 2006, Australia. [Farrell, S. A.; Wiersema, K.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. [Servillat, M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Pforr, J.; Maraston, C.] Univ Portsmouth, Inst Cosmol & Gravitat, Portsmouth PO1 3FX, Hants, England. [Maccarone, T. J.; Knigge, C.] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England. [Godet, O.; Webb, N. A.; Barret, D.; Belmont, R.] Univ Toulouse, UPS OMP, IRAP, Toulouse, France. [Godet, O.; Webb, N. A.; Barret, D.; Belmont, R.] IRAP, CNRS, F-31028 Toulouse 4, France. [Gosling, A. J.] Univ Oxford, Dept Phys, Oxford OX1 3RH, England. RP Farrell, SA (reprint author), Univ Sydney, Sch Phys, Sydney Inst Astron SIfA, Sydney, NSW 2006, Australia. EM sean.farrell@sydney.edu.au RI Pforr, Janine/J-3967-2015 OI Pforr, Janine/0000-0002-3414-8391 FU ARC; UK STFC; NASA [DD0-11050X, GO 12256, NAS 5-26555]; Marie-Curie Excellence Team grant Unimass [MEXT-CT-2006-042754]; European Community; [DP110102889] FX We thank the referee for useful comments and J.-P. Lasota, T. Alexander, C. Done, S. Shabala, F. Grise, K. Arnaud, and R. Starling for helpful discussions. S. A. F. is the recipient of an ARC Postdoctoral Fellowship, funded by grant DP110102889. S. A. F., T.J.M., A.J.G., and K. W. acknowledge funding from the UK STFC. M. S. acknowledges support from NASA grants DD0-11050X and GO 12256. J.P. and C. M. acknowledge the Marie-Curie Excellence Team grant Unimass, ref. MEXT-CT-2006-042754 of the TMR program financed by the European Community. N.A.W., D. B., and O.G. thank the CNES. Based on observations made with the NASA/ESA HST, obtained at the STScI, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-26555. These observations are associated with program 12256. Also based on observations with Swift. NR 42 TC 35 Z9 35 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 MAR 1 PY 2012 VL 747 IS 1 AR L13 DI 10.1088/2041-8205/747/1/L13 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 904KB UT WOS:000301192800013 ER PT J AU Wakelam, V Herbst, E Loison, JC Smith, IWM Chandrasekaran, V Pavone, B Adams, NG Bacchus-Montabonel, MC Bergeat, A Beroff, K Bierbaum, VM Chabot, M Dalgarno, A van Dishoeck, EF Faure, A Geppert, WD Gerlich, D Galli, D Hebrard, E Hersant, F Hickson, KM Honvault, P Klippenstein, SJ Le Picard, S Nyman, G Pernot, P Schlemmer, S Selsis, F Sims, IR Talbi, D Tennyson, J Troe, J Wester, R Wiesenfeld, L AF Wakelam, V. Herbst, E. Loison, J. -C. Smith, I. W. M. Chandrasekaran, V. Pavone, B. Adams, N. G. Bacchus-Montabonel, M. -C. Bergeat, A. Beroff, K. Bierbaum, V. M. Chabot, M. Dalgarno, A. van Dishoeck, E. F. Faure, A. Geppert, W. D. Gerlich, D. Galli, D. Hebrard, E. Hersant, F. Hickson, K. M. Honvault, P. Klippenstein, S. J. Le Picard, S. Nyman, G. Pernot, P. Schlemmer, S. Selsis, F. Sims, I. R. Talbi, D. Tennyson, J. Troe, J. Wester, R. Wiesenfeld, L. TI A KINETIC DATABASE FOR ASTROCHEMISTRY (KIDA) SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE astrochemistry; astronomical databases: miscellaneous; ISM: abundances; ISM: molecules ID DENSE INTERSTELLAR CLOUDS; GAS-PHASE REACTIONS; ION-MOLECULE REACTIONS; ASSOCIATION RATE COEFFICIENTS; NEUTRAL-NEUTRAL REACTIONS; MONTE-CARLO SIMULATIONS; CARBON-CHAIN ANIONS; DISSOCIATIVE RECOMBINATION; RATE CONSTANTS; AB-INITIO AB We present a novel chemical database for gas-phase astrochemistry. Named the KInetic Database for Astrochemistry (KIDA), this database consists of gas-phase reactions with rate coefficients and uncertainties that will be vetted to the greatest extent possible. Submissions of measured and calculated rate coefficients are welcome, and will be studied by experts before inclusion into the database. Besides providing kinetic information for the interstellar medium, KIDA is planned to contain such data for planetary atmospheres and for circumstellar envelopes. Each year, a subset of the reactions in the database (kida.uva) will be provided as a network for the simulation of the chemistry of dense interstellar clouds with temperatures between 10 K and 300 K. We also provide a code, named Nahoon, to study the time-dependent gas-phase chemistry of zero-dimensional and one-dimensional interstellar sources. C1 [Wakelam, V.; Pavone, B.; Hebrard, E.; Hersant, F.; Selsis, F.] Univ Bordeaux, LAB, UMR 5804, F-33270 Floirac, France. [Wakelam, V.; Pavone, B.; Hebrard, E.; Hersant, F.; Selsis, F.] CNRS, LAB, UMR 5804, F-33270 Floirac, France. [Herbst, E.] Ohio State Univ, Dept Phys, Columbus, OH 43210 USA. [Herbst, E.] Univ Virginia, Dept Chem, Charlottesville, VA 22904 USA. [Herbst, E.] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA. [Herbst, E.] Univ Virginia, Dept Phys, Charlottesville, VA 22904 USA. [Loison, J. -C.; Chandrasekaran, V.; Bergeat, A.; Hickson, K. M.] Univ Bordeaux, CNRS, ISM, UMR 5255, F-33400 Talence, France. [Smith, I. W. M.] Univ Cambridge, Chem Lab, Cambridge CB2 1EW, England. [Adams, N. G.] Univ Georgia, Dept Chem, Athens, GA 30602 USA. [Bacchus-Montabonel, M. -C.] Univ Lyon 1, CNRS, LASIM, UMR5579, F-69622 Villeurbanne, France. [Beroff, K.] CNRS, Inst Sci Mol Orsay, F-91405 Orsay, France. [Pernot, P.] Univ Paris 11, Chim Phys Lab, CNRS, UMR 8000, F-91405 Orsay, France. [Herbst, E.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. [Herbst, E.] Ohio State Univ, Dept Chem, Columbus, OH 43210 USA. [Bierbaum, V. M.] Univ Colorado, Dept Chem & Biochem, Ctr Astrophys & Space Astron, Boulder, CO 80309 USA. [Chabot, M.] IN2P3 CNRS, Intitut Phys Nucl Orsay, F-91406 Orsay, France. [Chabot, M.] Univ Paris 11, F-91406 Orsay, France. [Dalgarno, A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [van Dishoeck, E. F.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [Faure, A.; Wiesenfeld, L.] UJF Grenoble 1 CNRS, IPAG, UMR 5274, F-38041 Grenoble, France. [Geppert, W. D.] Univ Stockholm, Dept Phys, S-10691 Stockholm, Sweden. [Gerlich, D.] Tech Univ Chemnitz, Dept Phys, D-09107 Chemnitz, Germany. [Galli, D.] INAF Osservatorio Astrofis Arcetri, I-50125 Florence, Italy. [Honvault, P.] Univ Bourgogne, CNRS, Lab Interdisciplinaire Carnot Bourgogne, UMR 5209, F-21078 Dijon, France. [Honvault, P.] Univ Franche Compte, UFR Sci & Tech, F-25030 Besancon, France. [Klippenstein, S. J.] Argonne Natl Lab, Chem Sci & Engn Div, Argonne, IL 60439 USA. [Le Picard, S.; Sims, I. R.] Univ Rennes 1, Equipe Astrochim Expt, Inst Phys Rennes, CNRS,UMR 6251, F-35042 Rennes, France. [Nyman, G.] Univ Gothenburg, Dept Chem, S-41296 Gothenburg, Sweden. [Schlemmer, S.] Univ Cologne, Inst Phys 1, D-50937 Cologne, Germany. [Talbi, D.] Univ Montpellier 2, CNRS, GRAAL, UMR 5024, F-34095 Montpellier, France. [Tennyson, J.] UCL, Dept Phys & Astron, London WC1E 6BT, England. [Troe, J.] Univ Gottingen, Inst Phys Chem, D-37077 Gottingen, Germany. [Troe, J.] Max Planck Inst Biophys Chem, D-37077 Gottingen, Germany. [Wester, R.] Univ Innsbruck, Inst Ionenphys & Angew Phys, A-6020 Innsbruck, Austria. RP Wakelam, V (reprint author), Univ Bordeaux, LAB, UMR 5804, F-33270 Floirac, France. RI Hickson, Kevin/A-2443-2012; Nyman, Gunnar/B-1705-2009; bacchus, marie christine/F-4020-2010; PERNOT, Pascal/C-2643-2008; Sims, Ian/F-8989-2014; LE PICARD, Sebastien/N-1668-2014; Schlemmer, Stephan/E-2903-2015; Bergeat, Astrid/K-6780-2016; Tennyson, Jonathan/I-2222-2012; Wester, Roland/J-6293-2012; HONVAULT, Pascal/B-2993-2010; Chandrasekaran, Vijayanand/E-7341-2011; HEBRARD, Eric/E-9257-2014; OI Hickson, Kevin/0000-0001-8317-2606; bacchus, marie christine/0000-0002-0958-2380; PERNOT, Pascal/0000-0001-8586-6222; Sims, Ian/0000-0001-7870-1585; Schlemmer, Stephan/0000-0002-1421-7281; Tennyson, Jonathan/0000-0002-4994-5238; Wester, Roland/0000-0001-7935-6066; HONVAULT, Pascal/0000-0001-6857-5511; Chandrasekaran, Vijayanand/0000-0002-8314-8611; HEBRARD, Eric/0000-0003-0770-7271; Klippenstein, Stephen/0000-0001-6297-9187; Galli, Daniele/0000-0001-7706-6049; Wakelam, Valentine/0000-0001-9676-2605; Bergeat, Astrid/0000-0002-3961-5710 FU European Research Council (ERC) [209622: E3ARTHs]; Agence Nationale de la Recherche [ANR-JC08_311018: EMA:INC]; European program Astronet (CATS); VAMDC and EUROPLANET; Combination of Collaborative Projects and Coordination; Support Actions Funding Scheme of The Seventh Framework Program [Call topic: INFRA-2008-1.2.2, 239108]; EUROPLANET RI [228319]; NASA-PATM [NNH09AK24I] FX The KIDA team acknowledges various sources of funding, which have allowed us to develop this database. These sources include The University of Bordeaux, The "Institut de Physique Fondamentale de Bordeaux," the CNRS/INSU (PCMI, PNP, and ASOV), and The Observatoire Aquitain des Sciences de l'Univers. We acknowledge support from the European Research Council (ERC Grant 209622: E3ARTHs), the Agence Nationale de la Recherche (ANR-JC08_311018: EMA:INC), the European program Astronet (CATS project), and the European Seventh Framework Programme (FP7: VAMDC and EUROPLANET projects). VAMDC is funded under the Combination of Collaborative Projects and Coordination and Support Actions Funding Scheme of The Seventh Framework Program (Call topic: INFRA-2008-1.2.2, Grant Agreement number: 239108). The EUROPLANET RI (Research Infrastructure) is funded under the Grant Agreement number: 228319. The International Space Science Institute provided some of the KIDA team members with the opportunity to start this project in the context of the international team with the title " New generation of databases for interstellar chemical modeling in preparation for HSO and ALMA." V.W. and I.W.M.S. thank the Royal Society for its financial support of their collaboration. V.W. is grateful to all the participants of the project who helped design the data model of the database. V. W. also thanks Franck Le Petit for helpful discussions on the rate coefficients for photodissociation induced by cosmic rays. E.H. thanks the National Science Foundation (US) for his program in astrochemistry and NASA for the study of pre-planetary matter. N.G.A. thanks NASA for support of his experimental program. S.J.K. acknowledges support through NASA-PATM grant number NNH09AK24I. The anonymous referee is thanked for his/her useful comments, which helped to improve the quality of the paper. NR 146 TC 161 Z9 161 U1 6 U2 88 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0067-0049 J9 ASTROPHYS J SUPPL S JI Astrophys. J. Suppl. Ser. PD MAR PY 2012 VL 199 IS 1 AR 21 DI 10.1088/0067-0049/199/1/21 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 903ME UT WOS:000301119800021 ER PT J AU Lachniet, MS Bernal, JP Asmerom, Y Polyak, V Piperno, D AF Lachniet, Matthew S. Pablo Bernal, Juan Asmerom, Yemane Polyak, Victor Piperno, Dolores TI A 2400 yr Mesoamerican rainfall reconstruction links climate and cultural change SO GEOLOGY LA English DT Article ID CENTRAL MEXICO; MAYA LOWLANDS; TEOTIHUACAN; DROUGHT; POPOCATEPETL AB Droughts are a recurring feature of Mexican climate, but few high-resolution data are available to test for climate-change forcing of Mesoamerican civilizations. We present a quantitative 2400 yr rainfall reconstruction for the Basin of Mexico, from a precisely dated and highly resolved speleothern, that documents highly variable rainfall over the past 2400 yr. Dry conditions peaked during a 150-yr-long late Classic (ca. 600-900 CE) (Common Era) megadrought that culminated at 770 CE which followed centuries of climatic drying that spanned the fall of the city of Teotihuacan ca. 550 CE. The wettest conditions in the 1450s CE were associated with flooding in the Basin of Mexico. Our data suggest that rainfall variability was likely forced by the El Nino-Southern Oscillation, and impacts on spring-fed irrigation agriculture may have been a stressor on Mesoamerican civilizations. C1 [Lachniet, Matthew S.] Univ Nevada, Dept Geosci, Las Vegas, NV 89154 USA. [Pablo Bernal, Juan] Ctr Geociencias, Juriquilla 76230, Queretaro, Mexico. [Asmerom, Yemane; Polyak, Victor] Univ New Mexico, Dept Earth & Planetary Sci, Albuquerque, NM 87131 USA. [Piperno, Dolores] Smithsonian Natl Museum Nat Hist, Dept Anthropol, Program Human Ecol & Archaeobiol, Washington, DC 20004 USA. [Piperno, Dolores] Smithsonian Trop Res Inst, Balboa, Panama. RP Lachniet, MS (reprint author), Univ Nevada, Dept Geosci, 4505 Maryland Pkwy, Las Vegas, NV 89154 USA. EM matthew.lachniet@unlv.edu; jpbemal@geociencias.unam.mx; asmerom@unm.edu OI Lachniet, Matthew/0000-0001-5250-0144; Bernal, Juan Pablo/0000-0001-8363-572X FU U.S. National Science Foundation [ATM-0710707, ATM-1003558, EAR-0521196]; National Geographic Society [8828-10]; Consejo Nacional de Ciencia y Tecnologia [44016, 78828]; Universidad Nacional Autonoma de Mexico (UNAM) [IN112008] FX We thank Adrian Ortega of Colotlipa for support, O. Cervantes Sanchez (Comision Nacional del Agua, CONAGUA, Mexico) for Tacubaya data, E. Cienfuegos, P. Morales, and J. Baker for laboratory analyses, and K. Christenson and L. Rosales Lagarde for field support. This work was supported by U.S. National Science Foundation grants ATM-0710707, ATM-1003558, and EAR-0521196, National Geographic Society grant 8828-10, Consejo Nacional de Ciencia y Tecnologia grants 44016 and 78828, and Programa de Apoyo a Proyectos de Investigacion e Innovacion Tecnologica-Universidad Nacional Autonoma de Mexico (PAPIIT UNAM) grant IN112008. NR 40 TC 25 Z9 28 U1 1 U2 30 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 MAR PY 2012 VL 40 IS 3 BP 259 EP 262 DI 10.1130/G32471.1 PG 4 WC Geology SC Geology GA 904CL UT WOS:000301171200019 ER PT J AU Reitzel, K Ahlgren, J Rydin, E Egemose, S Turner, BL Hupfer, M AF Reitzel, Kasper Ahlgren, Joakim Rydin, Emil Egemose, Sara Turner, Benjamin L. Hupfer, Michael TI Diagenesis of settling seston: identity and transformations of organic phosphorus SO JOURNAL OF ENVIRONMENTAL MONITORING LA English DT Article ID NUCLEAR-MAGNETIC-RESONANCE; P-31 NMR-SPECTROSCOPY; LAKE-SEDIMENTS; FRESH-WATER; INORGANIC PHOSPHORUS; BIOGENIC PHOSPHORUS; ALUMINUM TREATMENT; MOBILE PHOSPHORUS; POLYPHOSPHATE; ERKEN AB Solution (31)phosphorus NMR spectroscopy and sequential fractionation were used to follow diagenetic changes in phosphorus forms during decomposition of settling seston in Lake Nordborg, a shallow eutrophic lake in Denmark. In a decomposition experiment, seston released >60% of their total phosphorus during similar to 50 days incubation, although seston collected during summer contained more phosphorus and released it over a longer period compared to seston collected during spring. Seston decomposition increased concentrations of potentially bioavailable polyphosphate and phosphodiesters, but also promoted the formation of refractory phosphorus forms that might be buried permanently in the sediment. Combining these results with in situ measurements of phosphorus concentrations in lake water and sediment traps revealed that the release from settling seston plays only a minor role in the accumulation of phosphorus in the hypolimnion of Lake Nordborg. C1 [Reitzel, Kasper; Egemose, Sara] Univ So Denmark, Inst Biol, DK-5230 Odense M, Denmark. [Ahlgren, Joakim] Swedish Univ Agr Sci, Dept Aquat Sci & Assessment, SE-75007 Uppsala, Sweden. [Rydin, Emil] Uppsala Univ, Dept Ecol & Genet, SE-75236 Uppsala, Sweden. [Turner, Benjamin L.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. [Hupfer, Michael] Leibniz Inst Freshwater Ecol & Inland Fisheries, D-12587 Berlin, Germany. RP Reitzel, K (reprint author), Univ So Denmark, Inst Biol, Campusvej 55, DK-5230 Odense M, Denmark. EM reitzel@biology.sdu.dk RI Turner, Benjamin/E-5940-2011 OI Turner, Benjamin/0000-0002-6585-0722 FU Villum Kann Rasmussen Centre of Excellence: Centre for Lake Restoration (CLEAR); Carlsberg foundation; The Danish Council for Independent Research\Natural Sciences [1637604] FX Kasper Reitzel and Sara Egemose were supported by the Villum Kann Rasmussen Centre of Excellence: Centre for Lake Restoration (CLEAR). In addition Kasper Reitzel was supported by the Carlsberg foundation and by The Danish Council for Independent Research vertical bar Natural Sciences by grant # 1637604. NR 34 TC 13 Z9 13 U1 1 U2 24 PU ROYAL SOC CHEMISTRY PI CAMBRIDGE PA THOMAS GRAHAM HOUSE, SCIENCE PARK, MILTON RD, CAMBRIDGE CB4 0WF, CAMBS, ENGLAND SN 1464-0325 J9 J ENVIRON MONITOR JI J. Environ. Monit. PD MAR PY 2012 VL 14 IS 3 BP 1098 EP 1106 DI 10.1039/c2em10883f PG 9 WC Chemistry, Analytical; Environmental Sciences SC Chemistry; Environmental Sciences & Ecology GA 900GP UT WOS:000300875100040 PM 22344567 ER PT J AU Melott, AL Bambach, RK Petersen, KD McArthur, JM AF Melott, Adrian L. Bambach, Richard K. Petersen, Kenni D. McArthur, John M. TI An similar to 60-Million-Year Periodicity Is Common to Marine Sr-87/Sr-86, Fossil Biodiversity, and Large-Scale Sedimentation: What Does the Periodicity Reflect? SO JOURNAL OF GEOLOGY LA English DT Article ID LARGE IGNEOUS PROVINCES; STRONTIUM-ISOTOPE STRATIGRAPHY; TIME-SERIES ANALYSIS; MANTLE PLUMES; SEA-LEVEL; MASS EXTINCTION; COSMIC-RAYS; ICE-AGE; DIVERSITY; CYCLES AB We find that the marine Sr-87/Sr-86 record shows a significant periodicity of 59.3 +/- 3 m.yr. The Sr-87/Sr-86 record is 171 degrees +/- 12 degrees out of phase with a 62 (+/- 3)-m.yr. periodicity previously reported in the record of marine animal diversity. These periodicities are close to 58 (+/- 4)-m.yr. cycles found for the number of gap-bounded sedimentary carbonate packages of North America. We propose that these periodicities reflect the operation of a periodic "pulse of the earth" in large-scale earth processes. These may be linked to mantle or plate-tectonic events, possibly uplift, which affects the earth's climate and oceans and, thus, the geochemistry, sedimentation, and biodiversity of the marine realm. C1 [Melott, Adrian L.] Univ Kansas, Dept Phys & Astron, Lawrence, KS 66045 USA. [Bambach, Richard K.] Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20013 USA. [Petersen, Kenni D.] Aarhus Univ, Dept Earth Sci, DK-8000 Aarhus C, Denmark. [McArthur, John M.] UCL, Dept Earth Sci, London WC1E 6BT, England. RP Melott, AL (reprint author), Univ Kansas, Dept Phys & Astron, Lawrence, KS 66045 USA. EM melott@ku.edu RI Petersen, Kenni Dinesen/A-3232-2012; McArthur, John/C-2705-2008 OI McArthur, John/0000-0003-1461-7805 FU American Astronomical Society FX We thank J. Alroy, P. Flemings, J. Ogg, and S. Peters for providing some of the data analyzed here. T. Hallam made useful comments. An anonymous reviewer and M. Foote provided extremely helpful feedback in review. We are grateful to the American Astronomical Society for the sponsorship of the 2007 Honolulu multidisciplinary Splinter Meeting at which discussions leading to this project took place. This is Paleobiology Database publication 150. NR 62 TC 16 Z9 16 U1 3 U2 15 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0022-1376 J9 J GEOL JI J. Geol. PD MAR PY 2012 VL 120 IS 2 BP 217 EP 226 DI 10.1086/663877 PG 10 WC Geology SC Geology GA 906GK UT WOS:000301332700007 ER PT J AU Songsasen, N Wesselowski, S Carpenter, JW Wildt, DE AF Songsasen, Nucharin Wesselowski, Sonya Carpenter, James W. Wildt, David E. TI The ability to achieve meiotic maturation in the dog oocyte is linked to glycolysis and glutamine oxidation SO MOLECULAR REPRODUCTION AND DEVELOPMENT LA English DT Article ID IN-VITRO MATURATION; DOMESTIC DOG; DEVELOPMENTAL COMPETENCE; PREIMPLANTATION EMBRYOS; NUCLEAR MATURATION; GLUCOSE-METABOLISM; SPERM PENETRATION; PORCINE OOCYTES; CANINE OOCYTES; BOVINE OOCYTES AB We tested the hypothesis that meiotic competence of dog oocytes is tightly linked with donor follicle size and energy metabolism. Oocytes were recovered from small (<1?mm diameter, n?=?327), medium (1<2?mm, n?=?292) or large (=2?mm, n?=?102) follicles, cultured for 0, 24, or 48?hr, and then assessed for glycolysis, glucose oxidation, pyruvate uptake, glutamine oxidation, and nuclear status. More oocytes (P??0.05). Glycolytic rate increased (P? l > -60 degrees and b < +/-1 degrees.5) in submillimeter (submm) continuum emission tracing the cold dust of dense and young star-forming regions. Here, we present the overall distribution of sources within our Galactic disk. The submm continuum emission is confined to a narrow range around the Galactic plane, but shifted on average by similar to 0.07 deg below the plane. Source number counts show strong enhancements toward the Galactic center, the spiral arms, and toward prominent star-forming regions. Comparing the distribution of ATLASGAL dust continuum emission to that of young intermediate-to high-mass young stellar objects (YSOs) derived from Spitzer data, we find similarities as well as differences. In particular, the distribution of submm dust continuum emission is significantly more confined to the plane than the YSO distribution (FWHM of 0.7 and 1.1 deg, corresponding to mean physical scale heights of approximately 46 and 80 pc, respectively). While this difference may partly be caused by the large extinction from the dense submm cores, gradual dispersal of stellar distributions after their birth could also contribute to this effect. Compared to other tracers of Galactic structure, the ATLASGAL data are strongly confined to a narrow latitude strip around the Galactic plane. C1 [Beuther, H.; Tackenberg, J.; Linz, H.; Henning, Th.] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Schuller, F.; Schilke, P.] Univ Cologne, Inst Phys 1, D-50937 Cologne, Germany. [Wyrowski, F.; Menten, K.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Robitaille, T. P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Walmsley, C. M.] Osserv Astrofis Arcetri, I-50125 Florence, Italy. [Walmsley, C. M.] Dublin Inst Adv Studies, Dublin 2, Ireland. [Bronfman, L.] Univ Chile, Dept Astron, Santiago, Chile. [Motte, F.; Nguyen-Luong, Q.] Univ Paris Diderot, CEA Saclay, CNRS INSU, CEA IRFU,Lab AIM, F-91191 Gif Sur Yvette, France. [Bontemps, S.] Univ Bordeaux, OASU, F-33271 Floirac, France. RP Beuther, H (reprint author), Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany. EM beuther@mpia.de RI Bronfman, Leonardo/H-9544-2013 OI Bronfman, Leonardo/0000-0002-9574-8454 FU CONICYT [15010003, PFB-06] FX We thank the referee for a careful review improving the paper significantly. H. B. thanks Sarah Kendrew for discussions about Galactic distributions. L. B. acknowledges support from CONICYT through projects FONDAP No. 15010003 and BASAL PFB-06. NR 48 TC 29 Z9 29 U1 0 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAR 1 PY 2012 VL 747 IS 1 AR 43 DI 10.1088/0004-637X/747/1/43 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 897EK UT WOS:000300627300043 ER PT J AU Boden, AF Torres, G Duchene, G Konopacky, Q Ghez, AM Torres, RM Loinard, L AF Boden, Andrew F. Torres, Guillermo Duchene, Gaspard Konopacky, Quinn Ghez, A. M. Torres, Rosa M. Loinard, Laurent TI A SURPRISING DYNAMICAL MASS FOR V773 Tau B SO ASTROPHYSICAL JOURNAL LA English DT Article DE stars fundamental parameters; stars individual (V773 Tau); stars pre-main sequence ID MAIN-SEQUENCE STARS; ECCENTRIC STELLAR BINARIES; PRELIMINARY PHYSICAL ORBIT; SOLAR-TYPE STARS; CIRCUMBINARY DISCS; SPECTRAL LIBRARY; V-773 TAURI; COOL STARS; SYSTEM; MULTIPLICITY AB We report on new high-resolution imaging and spectroscopy on the multiple T Tauri star system V773 Tau over the 2003-2009 period. With these data we derive relative astrometry, photometry between the A and B components, and radial velocity (RV) of the A-subsystem components. Combining these new data with previously published astrometry and RVs, we update the relative A-B orbit model. This updated orbit model, the known system distance, and A-subsystem parameters yield a dynamical mass for the B component for the first time. Remarkably, the derived B dynamical mass is in the range 1.7-3.0 M-circle dot. This is much higher than previous estimates and suggests that like A, B is also a multiple stellar system. Among these data, spatially resolved spectroscopy provides new insight into the nature of the B component. Similar to A, these near-IR spectra indicate that the dominant source in B is of mid-K spectral type. If B is in fact a multiple star system as suggested by the dynamical mass estimate, the simplest assumption is that B is composed of similar similar to 1.2 M-circle dot pre-main-sequence stars in a close (< 1 AU) binary system. This inference is supported by line-shape changes in near-IR spectroscopy of B, tentatively interpreted as changing RV among components in V773 Tau B. Relative photometry indicates that B is highly variable in the near-IR. The most likely explanation for this variability is circum-B material resulting in variable line-of-sight extinction. The distribution of this material must be significantly affected by both the putative B multiplicity and the A-B orbit. C1 [Boden, Andrew F.] CALTECH, Div Phys Math & Astron, Pasadena, CA 91125 USA. [Torres, Guillermo] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Duchene, Gaspard] Univ Calif Berkeley, Div Astron & Astrophys, Berkeley, CA 94720 USA. [Duchene, Gaspard] UJF Grenoble 1 CNRS INSU, IPAG, UMR 5274, F-38041 Grenoble, France. [Konopacky, Quinn] Lawrence Livermore Natl Lab, Livermore, CA 94550 USA. [Konopacky, Quinn; Ghez, A. M.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. [Torres, Rosa M.] Univ Bonn, Argelander Inst Astron, D-53121 Bonn, Germany. [Torres, Rosa M.; Loinard, Laurent] Univ Nacl Autonoma Mexico, Ctr Radiostron & Astrofis, Morelia 58089, Michoacan, Mexico. [Loinard, Laurent] Max Planck Inst Radioastron, D-53121 Bonn, Germany. RP Boden, AF (reprint author), CALTECH, Div Phys Math & Astron, MS 11-17, Pasadena, CA 91125 USA. FU W.M. Keck Foundation; National Science Foundation; California Institute of Technology, Harvard University; University of California; DGAPA; UNAM; CONACyT, Mexico; NSF [AST-1007992, AST-0908822]; Deutsche Forschungsgemeinschaft (DFG) [VL 61/3-1]; Guggenheim Foundation; von Humboldt Stiftung; U.S. Department of Energy by Lawrence Livermore National Laboratory [DE-AC52-07NA27344] FX Some of the data presented here were obtained at the W.M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California, the University of Hawaii, and NASA. The Observatory was made possible by the generous financial support of the W.M. Keck Foundation. We gratefully acknowledge personnel from the W.M. Keck Observatory in supporting observations of V773 Tau. The authors 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.; The authors gratefully acknowledge research support provided by the National Science Foundation, the California Institute of Technology, Harvard University, the University of California, DGAPA, UNAM, and CONACyT, Mexico. In particular: A.F.B. acknowledges support from NSF grant AST-0908822, G.T. acknowledges support from NSF grant AST-1007992, R.M.T. acknowledges support by the Deutsche Forschungsgemeinschaft (DFG) through the Emmy Noether Research grant VL 61/3-1. L.L. acknowledges the financial support of the Guggenheim Foundation and the von Humboldt Stiftung. Portions of this work were performed under the auspices of the U.S. Department of Energy by Lawrence Livermore National Laboratory under Contract DE-AC52-07NA27344. NR 48 TC 6 Z9 6 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAR 1 PY 2012 VL 747 IS 1 AR 17 DI 10.1088/0004-637X/747/1/17 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 897EK UT WOS:000300627300017 ER PT J AU Bulbul, GE Smith, RK Foster, A Cottam, J Loewenstein, M Mushotzky, R Shafer, R AF Bulbul, G. Esra Smith, Randall K. Foster, Adam Cottam, Jean Loewenstein, Michael Mushotzky, Richard Shafer, Richard TI HIGH-RESOLUTION XMM-NEWTON SPECTROSCOPY OF THE COOLING FLOW CLUSTER A3112 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: individual (A3112); X-rays: galaxies: clusters ID WIND CHARGE-EXCHANGE; RAY EXCESS EMISSION; MASSIVE GALAXY CLUSTERS; INTRACLUSTER MEDIUM; EMITTING GAS; SUZAKU OBSERVATIONS; TURBULENT VELOCITY; CENTAURUS CLUSTER; ELLIPTIC GALAXIES; CONSTRAINTS AB We examine high signal-to-noise XMM-Newton European Photon Imaging Camera (EPIC) and Reflection Grating Spectrometer (RGS) observations to determine the physical characteristics of the gas in the cool core and outskirts of the nearby rich cluster A3112. The XMM-Newton Extended Source Analysis Software data reduction and background modeling methods were used to analyze the XMM-Newton EPIC data. From the EPIC data, we find that the iron and silicon abundance gradients show significant increase toward the center of the cluster while the oxygen abundance profile is centrally peaked but has a shallower distribution than that of iron. The X-ray mass modeling is based on the temperature and deprojected density distributions of the intracluster medium determined from EPIC observations. The total mass of A3112 obeys the M-T scaling relations found using XMM-Newton and Chandra observations of massive clusters at r(500). The gas mass fraction f(gas) = 0.149(-0.032)(+0.036) at r(500) is consistent with the seven-year Wilkinson Microwave Anisotropy Probe results. The comparisons of line fluxes and flux limits on the Fe XVII and Fe XVIII lines obtained from high-resolution RGS spectra indicate that there is no spectral evidence for cooler gas associated with the cluster with temperature below 1.0 keV in the central <38 '' (similar to 52 kpc) region of A3112. High-resolution RGS spectra also yield an upper limit to the turbulent motions in the compact core of A3112 (206 km s(-1)). We find that the contribution of turbulence to total energy is less than 6%. This upper limit is consistent with the energy contribution measured in recent high-resolution simulations of relaxed galaxy clusters. C1 [Bulbul, G. Esra; Smith, Randall K.; Foster, Adam] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Cottam, Jean; Loewenstein, Michael; Mushotzky, Richard; Shafer, Richard] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Bulbul, GE (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM ebulbul@cfa.harvard.edu FU NASA XMM [NNX09AP92G]; NASA ROSES-ADP [NNX09AC71G] FX The authors thank Steve Snowden and Helen Russell for kindly providing help on the ESAS software and deprojection methods. We also thank the anonymous referee, Maxim Markevitch, Paul Nulsen, Max Bonamente, and Jelle de Plaa for providing useful suggestions and comments on the manuscript. We gratefully acknowledge support for this research from NASA XMM-Newton grant NNX09AP92G and NASA ROSES-ADP grant NNX09AC71G. NR 59 TC 23 Z9 23 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAR 1 PY 2012 VL 747 IS 1 AR 32 DI 10.1088/0004-637X/747/1/32 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 897EK UT WOS:000300627300032 ER PT J AU Conroy, C van Dokkum, P AF Conroy, Charlie van Dokkum, Pieter TI COUNTING LOW-MASS STARS IN INTEGRATED LIGHT SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: abundances; galaxies: stellar content; stars: abundances; stars: fundamental parameters ID EARLY-TYPE GALAXIES; STELLAR POPULATION-MODELS; EFFECTIVE TEMPERATURE SCALE; INFRARED CAII TRIPLET; SURFACE BRIGHTNESS FLUCTUATIONS; NEWTON-TELESCOPE LIBRARY; WING-FORD BAND; ELLIPTIC GALAXIES; GLOBULAR-CLUSTERS; EMPIRICAL CALIBRATION AB Low-mass stars (M less than or similar to 0.4 M-circle dot) are thought to comprise the bulk of the stellar mass of galaxies but they constitute only of order 1 percent of the bolometric luminosity of an old stellar population. Directly estimating the number of low-mass stars from integrated flux measurements of old stellar systems is therefore possible but very challenging, given the numerous variables that can affect the light at the percent level. Here we present a new population synthesis model created specifically for the purpose of measuring the low-mass initial mass function (IMF) down to similar to 0.1M(circle dot) for metal-rich stellar populations with ages in the range 3-13.5 Gyr. Our fiducial model is based on the synthesis of three separate isochrones, and a combination of optical and near-IR empirical stellar libraries in order to produce integrated light spectra over the wavelength interval 0.35 mu m < lambda < 2.4 mu m at a resolving power of R approximate to 2000. New synthetic stellar atmospheres and spectra have been computed in order to model the spectral variations due to changes in individual elemental abundances including C, N, Na, Mg, Si, Ca, Ti, Fe, and generic alpha elements. We demonstrate the power of combining blue spectral features with surface gravity-sensitive near-IR features in order to simultaneously constrain the low-mass IMF, stellar population age, metallicity, and abundance pattern from integrated light measurements. Finally, we show that the shape of the low-mass IMF can also be directly constrained by employing a suite of surface gravity-sensitive spectral features, each of which is most sensitive to a particular mass interval. C1 [Conroy, Charlie] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [van Dokkum, Pieter] Yale Univ, Dept Astrophys Sci, New Haven, CT USA. RP Conroy, C (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. FU FAS Science Division Research Computing Group at Harvard University FX We acknowledge fruitful conversations with Aaron Dotter, Marijn Franx, Bob Kurucz, and Ricardo Schiavon. We also thank Bob Kurucz for his expert advice regarding synthetic stellar spectra and for compiling the FeH linelist specifically for this project. Nelson Caldwell is thanked for providing his blue M31 GC spectra. We thank the referee for constructive comments. The synthetic spectral libraries were computed on the Odyssey cluster supported by the FAS Science Division Research Computing Group at Harvard University. NR 101 TC 84 Z9 84 U1 0 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAR 1 PY 2012 VL 747 IS 1 AR 69 DI 10.1088/0004-637X/747/1/69 PG 22 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 897EK UT WOS:000300627300069 ER PT J AU Cowan, NB Machalek, P Croll, B Shekhtman, LM Burrows, A Deming, D Greene, T Hora, JL AF Cowan, Nicolas B. Machalek, Pavel Croll, Bryce Shekhtman, Louis M. Burrows, Adam Deming, Drake Greene, Tom Hora, Joseph L. TI THERMAL PHASE VARIATIONS OF WASP-12b: DEFYING PREDICTIONS SO ASTROPHYSICAL JOURNAL LA English DT Article DE infrared: planetary systems; planets and satellites: atmospheres; planets and satellites: composition; planets and satellites: individual (WASP-12b); planet-star interactions; techniques: photometric ID SPITZER-SPACE-TELESCOPE; TRANSIT LIGHT CURVES; HD 189733B; EXTRASOLAR PLANET; HOT JUPITERS; SECONDARY ECLIPSE; MU-M; TRANSMISSION SPECTRUM; EXOPLANET WASP-12B; MODEL ATMOSPHERES AB We report Warm Spitzer full-orbit phase observations of WASP-12b at 3.6 and 4.5 mu m. This extremely inflated hot Jupiter is thought to be overflowing its Roche lobe, undergoing mass loss and accretion onto its host star, and has been claimed to have a C/O ratio in excess of unity. We are able to measure the transit depths, eclipse depths, thermal and ellipsoidal phase variations at both wavelengths. The large-amplitude phase variations, combined with the planet's previously measured dayside spectral energy distribution, are indicative of non-zero Bond albedo and very poor day-night heat redistribution. The transit depths in the mid-infrared-(R-p/R-*)(2) = 0.0123(3) and 0.0111(3) at 3.6 and 4.5 mu m, respectively-indicate that the atmospheric opacity is greater at 3.6 than at 4.5 mu m, in disagreement with model predictions, irrespective of C/O ratio. The secondary eclipse depths are consistent with previous studies: F-day/F-* = 0.0038(4) and 0.0039(3) at 3.6 and 4.5 mu m, respectively. We do not detect ellipsoidal variations at 3.6 mu m, but our parameter uncertainties-estimated via prayer-bead Monte Carlo-keep this non-detection consistent with model predictions. At 4.5 mu m, on the other hand, we detect ellipsoidal variations that are much stronger than predicted. If interpreted as a geometric effect due to the planet's elongated shape, these variations imply a 3: 2 ratio for the planet's longest: shortest axes and a relatively bright day-night terminator. If we instead presume that the 4.5 mu m ellipsoidal variations are due to uncorrected systematic noise and we fix the amplitude of the variations to zero, the best-fit 4.5 mu m transit depth becomes commensurate with the 3.6 mu m depth, within the uncertainties. The relative transit depths are then consistent with a solar composition and short scale height at the terminator. Assuming zero ellipsoidal variations also yields a much deeper 4.5 mu m eclipse depth, consistent with a solar composition and modest temperature inversion. We suggest future observations that could distinguish between these two scenarios. C1 [Cowan, Nicolas B.; Shekhtman, Louis M.] Northwestern Univ, CIERA, Evanston, IL 60208 USA. [Cowan, Nicolas B.; Shekhtman, Louis M.] Northwestern Univ, Dept Phys & Astron, Evanston, IL 60208 USA. [Machalek, Pavel] SETI Inst, Mountain View, CA 94043 USA. [Machalek, Pavel; Greene, Tom] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Croll, Bryce] Univ Toronto, Dept Astron & Astrophys, Toronto, ON M5S 3H4, Canada. [Croll, Bryce] MIT, Dept Phys, Cambridge, MA 02139 USA. [Burrows, Adam] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. [Deming, Drake] NASA, Goddard Space Flight Ctr, Planetary Syst Lab, Greenbelt, MD 20771 USA. [Deming, Drake] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Hora, Joseph L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Cowan, NB (reprint author), Northwestern Univ, CIERA, 2131 Tech Dr, Evanston, IL 60208 USA. EM n-cowan@northwestern.edu OI Hora, Joseph/0000-0002-5599-4650 FU NASA; NASA through JPL/Caltech FX Much of this work was completed while N.B.C. was at the Aspen Center for Physics. N.B.C. acknowledges useful conversations with F. A. Rasio, W. M. Farr, H. A. Knutson, N. Lewis, and J. Budaj, as well as countless fruitful discussions at the Future of Astronomy, Extreme Solar Systems II, and joint EPSC/DPS meetings. 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. NR 77 TC 74 Z9 74 U1 3 U2 7 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAR 1 PY 2012 VL 747 IS 1 AR 82 DI 10.1088/0004-637X/747/1/82 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 897EK UT WOS:000300627300082 ER PT J AU Koch, PM Tang, YW Ho, PTP AF Koch, Patrick M. Tang, Ya-Wen Ho, Paul T. P. TI QUANTIFYING THE SIGNIFICANCE OF THE MAGNETIC FIELD FROM LARGE-SCALE CLOUD TO COLLAPSING CORE: SELF-SIMILARITY, MASS-TO-FLUX RATIO, AND STAR FORMATION EFFICIENCY SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM: clouds; ISM: individual objects (W51, W51 e2); ISM: magnetic fields; polarization ID FORMING REGION; INTERSTELLAR GRAINS; DYNAMICAL COLLAPSE; RADIATIVE TORQUES; MOLECULAR CORES; W51; EVOLUTION; TURBULENCE; ALIGNMENT; OUTFLOW AB Dust polarization observational results are analyzed for the high-mass star formation region W51 from the largest parent cloud (similar to 2 pc, James Clerk Maxwell Telescope) to the large-scale envelope (similar to 0.5 pc, BIMA array) down to the collapsing core e2 (similar to 60 mpc, Submillimeter Array). Magnetic field and dust emission gradient orientations reveal a correlation which becomes increasingly more tight with higher resolution. The previously developed polarization-intensity-gradient method is applied in order to quantify the magnetic field significance. This technique provides a way to estimate the local magnetic field force compared to gravity without the need of any mass or field strength measurements, solely making use of measured angles which reflect the geometrical imprint of the various forces. All three data sets clearly show regions with distinct features in the field-to-gravity force ratio. Azimuthally averaged radial profiles of this force ratio reveal a transition from a field dominance at larger distances to a gravity dominance closer to the emission peaks. Normalizing these profiles to a characteristic core scale points toward self-similarity. Furthermore, the polarization-intensity-gradient method is linked to the mass-to-flux ratio, providing a new approach to estimate the latter one without mass and field strength inputs. A transition from a magnetically supercritical to a subcritical state as a function of distance from the emission peak is found for the e2 core. Finally, based on the measured radius-dependent field-to-gravity force ratio we derive a modified star formation efficiency with a diluted gravity force. Compared to a standard (free-fall) efficiency, the observed field is capable of reducing the efficiency down to 10% or less. C1 [Koch, Patrick M.; Ho, Paul T. P.] Acad Sinica, Inst Astron & Astrophys, Taipei 115, Taiwan. [Tang, Ya-Wen] Univ Bordeaux, Observ Aquitain Sci Univers, F-33271 Floirac, France. [Tang, Ya-Wen] CNRS, UMR 5804, Lab Astrophys Bordeaux, F-33271 Floirac, France. [Ho, Paul T. P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Koch, PM (reprint author), Acad Sinica, Inst Astron & Astrophys, Taipei 115, Taiwan. EM pmkoch@asiaa.sinica.edu.tw OI Tang, Ya-Wen/0000-0002-0675-276X FU NSC [NSC97-2112-M-001-007-MY3] FX The authors thank the referee for valuable comments which led to further important insight in this work. P.T.P.H. is supported by the NSC grant NSC97-2112-M-001-007-MY3. NR 43 TC 9 Z9 9 U1 0 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAR 1 PY 2012 VL 747 IS 1 AR 80 DI 10.1088/0004-637X/747/1/80 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 897EK UT WOS:000300627300080 ER PT J AU Koch, PM Tang, YW Ho, PTP AF Koch, Patrick M. Tang, Ya-Wen Ho, Paul T. P. TI MAGNETIC FIELD STRENGTH MAPS FOR MOLECULAR CLOUDS: A NEW METHOD BASED ON A POLARIZATION-INTENSITY GRADIENT RELATION SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM: clouds; ISM: individual objects (W51 e2); ISM: magnetic fields; polarization ID FAR-INFRARED POLARIMETRY; STAR-FORMING REGION; W51 MASSIVE CORES; RADIATIVE TORQUES; GRAIN ALIGNMENT; SUBMILLIMETER POLARIZATION; INTERSTELLAR GRAINS; DYNAMICAL COLLAPSE; PROPER MOTIONS; DISPERSION AB Dust polarization orientations in molecular clouds often tend to be close to tangential to the Stokes I dust continuum emission contours. The magnetic field and the emission gradient orientations, therefore, show some correlation. A method is proposed, which-in the framework of ideal magnetohydrodynamics (MHD)-connects the measured angle between magnetic field and emission gradient orientations to the total field strength. The approach is based on the assumption that a change in emission intensity (gradient) is a measure for the resulting direction of motion in the MHD force equation. In particular, this new method leads to maps of position-dependent magnetic field strength estimates. When evaluating the field curvature and the gravity direction locally on a map, the method can be generalized to arbitrary cloud shapes. The technique is applied to high-resolution (similar to 0 ''.7) Submillimeter Array polarization data of the collapsing core W51 e2. A tentative similar to 7.7 mG field strength is found when averaging over the entire core. The analysis further reveals some structures and an azimuthally averaged radial profile similar to r(-1/2) for the field strength. Maximum values close to the center are around 19 mG. The currently available observations lack higher resolution data to probe the innermost part of the core where the largest field strength is expected from the method. Application regime and limitations of the method are discussed. As a further important outcome of this technique, the local significance of the magnetic field force compared to the other forces can be quantified in a model-independent way, from measured angles only. Finally, the method can potentially also be expanded and applied to other objects (besides molecular clouds) with measurements that reveal the field morphology, as, e. g., Faraday rotation measurements in galaxies. C1 [Koch, Patrick M.; Tang, Ya-Wen; Ho, Paul T. P.] Acad Sinica, Inst Astron & Astrophys, Taipei 115, Taiwan. [Tang, Ya-Wen] Univ Bordeaux, Observ Aquitain Sci Univers, F-33271 Floirac, France. [Tang, Ya-Wen] CNRS, UMR 5804, Lab Astrophys Bordeaux, F-33271 Floirac, France. [Ho, Paul T. P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Koch, PM (reprint author), Acad Sinica, Inst Astron & Astrophys, Taipei 115, Taiwan. EM pmkoch@asiaa.sinica.edu.tw OI Tang, Ya-Wen/0000-0002-0675-276X FU NSC [NSC97-2112-M-001-007-MY3] FX The authors thank the referee for valuable comments which led to further significant insight in this work. P.T.P.H. is supported by NSC Grant NSC97-2112-M-001-007-MY3. NR 47 TC 14 Z9 15 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAR 1 PY 2012 VL 747 IS 1 AR 79 DI 10.1088/0004-637X/747/1/79 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 897EK UT WOS:000300627300079 ER PT J AU Privon, GC Baum, SA O'Dea, CP Gallimore, J Noel-Storr, J Axon, DJ Robinson, A AF Privon, G. C. Baum, S. A. O'Dea, C. P. Gallimore, J. Noel-Storr, J. Axon, D. J. Robinson, A. TI MODELING THE INFRARED EMISSION IN CYGNUS A SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: active; galaxies: individual (Cygnus A); galaxies: jets ID SPITZER-SPACE-TELESCOPE; STAR-FORMING GALAXIES; NARROW-LINE REGION; RADIO GALAXIES; NUCLEAR REGIONS; MARKARIAN 231; PKS 0637-752; BLACK-HOLE; X-RAY; A II AB We present new Spitzer IRS spectroscopy of Cygnus A, one of the most luminous radio sources in the local universe. Data on the inner 20 '' are combined with new reductions of MIPS and IRAC photometry as well as data from the literature to form a radio through mid-infrared spectral energy distribution (SED). This SED is then modeled as a combination of torus reprocessed active galactic nucleus (AGN) radiation, dust enshrouded starburst, and a synchrotron jet. This combination of physically motivated components successfully reproduces the observed emission over almost 5 dex in frequency. The bolometric AGN luminosity is found to be 10(12) L-circle dot (90% of L-IR), with a clumpy AGN-heated dust medium extending to similar to 130 pc from the supermassive black hole. Evidence is seen for a break or cutoff in the core synchrotron emission. The associated population of relativistic electrons could in principle be responsible for some of the observed X-ray emission though the synchrotron self-Compton mechanism. The SED requires a cool dust component, consistent with dust-reprocessed radiation from ongoing star formation. Star formation contributes at least 6 x 10(10) L-circle dot to the bolometric output of Cygnus A, corresponding to a star formation rate of similar to 10 M-circle dot yr(-1). C1 [Privon, G. C.; Baum, S. A.; Noel-Storr, J.] Rochester Inst Technol, Chester F Carlson Ctr Imaging Sci, Rochester, NY 14623 USA. [Privon, G. C.] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA. [O'Dea, C. P.; Axon, D. J.; Robinson, A.] Rochester Inst Technol, Dept Phys, Rochester, NY 14623 USA. [Baum, S. A.] Radcliffe Inst Adv Study, Cambridge, MA 02138 USA. [O'Dea, C. P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Gallimore, J.] Bucknell Univ, Dept Phys, Lewisburg, PA 17837 USA. [Gallimore, J.] Natl Radio Astron Observ, Charlottesville, VA 22904 USA. [Axon, D. J.] Univ Sussex, Sch Math & Phys Sci, Brighton BN1 9RH, E Sussex, England. RP Privon, GC (reprint author), Rochester Inst Technol, Chester F Carlson Ctr Imaging Sci, Rochester, NY 14623 USA. OI Privon, George/0000-0003-3474-1125 FU NASA; NASA through JPL/Caltech; Radcliffe Institute for Advanced Study at Harvard University 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. Computing resources were provided in part by the Research Computing group of the Rochester Institute of Technology. This research has made use of the NASA/IPAC Extragalactic Database (NED) which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. This research has made use of NASA's Astrophysics Data System. This work is supported in part by the Radcliffe Institute for Advanced Study at Harvard University. NR 61 TC 10 Z9 10 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAR 1 PY 2012 VL 747 IS 1 AR 46 DI 10.1088/0004-637X/747/1/46 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 897EK UT WOS:000300627300046 ER PT J AU Vrinceanu, D Onofrio, R Sadeghpour, HR AF Vrinceanu, D. Onofrio, R. Sadeghpour, H. R. TI ANGULAR MOMENTUM CHANGING TRANSITIONS IN PROTON-RYDBERG HYDROGEN ATOM COLLISIONS SO ASTROPHYSICAL JOURNAL LA English DT Article DE atomic processes; cosmic background radiation; planetary nebulae: general; stars: atmospheres; stars: early-type ID CHARGED-PARTICLES; STATES; IONS; RECOMBINATION; EQUILIBRIUM; POPULATIONS; NEBULAE AB Collisions between electrically charged particles and neutral atoms are central for understanding the dynamics of neutral gases and plasmas in a variety of physical situations of terrestrial and astronomical interest. Specifically, redistribution of angular momentum states within the degenerate shell of highly excited Rydberg atoms occurs efficiently in distant collisions with ions. This process is crucial in establishing the validity of the local thermal equilibrium assumption and may also play a role in determining a precise ionization fraction in primordial recombination. We provide an accurate expression for the non-perturbative rate coefficient of collisions between protons and H(nl) ending in a final state H(nl'), with n being the principal quantum number and l, l' the initial and final angular momentum quantum numbers, respectively. The validity of this result is confirmed by results of classical trajectory Monte Carlo simulations. Previous results, obtained by Pengelly and Seaton only for dipole-allowed transitions l -> l +/- 1, overestimate the l-changing collisional rate coefficients approximately by a factor of six, and the physical origin of this overestimation is discussed. C1 [Vrinceanu, D.] Texas So Univ, Dept Phys, Houston, TX 77004 USA. [Onofrio, R.] Univ Padua, Dipartimento Fis & Astron Galileo Galilei, I-35131 Padua, Italy. [Onofrio, R.; Sadeghpour, H. R.] Harvard Smithsonian Ctr Astrophys, ITAMP, Cambridge, MA 02138 USA. RP Vrinceanu, D (reprint author), Texas So Univ, Dept Phys, Houston, TX 77004 USA. EM daniel.vrinceanu@gmail.com; onofrior@gmail.com; hrsadeghpour@gmail.com FU National Science Foundation; Harvard University; Smithsonian Astrophysical Laboratory FX D.V. is grateful to Texas Southern University High Performance Computing Center for making the necessary computational resources available. This work was partially supported by the National Science Foundation through a grant for the Institute for Theoretical Atomic, Molecular and Optical Physics at Harvard University, and the Smithsonian Astrophysical Laboratory. NR 34 TC 11 Z9 11 U1 0 U2 7 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAR 1 PY 2012 VL 747 IS 1 AR 56 DI 10.1088/0004-637X/747/1/56 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 897EK UT WOS:000300627300056 ER PT J AU Alonso, R Crawford, AJ Bermingham, E AF Alonso, Roberto Crawford, Andrew J. Bermingham, Eldredge TI Molecular phylogeny of an endemic radiation of Cuban toads (Bufonidae: Peltophryne) based on mitochondrial and nuclear genes SO JOURNAL OF BIOGEOGRAPHY LA English DT Review DE Caribbean biogeography; Cuba; divergence time; GAARlandia; phylogeography; relaxed molecular clock; vicariance; West Indies; within-island diversification ID INDIAN TERRESTRIAL VERTEBRATES; OCEANIC ISLAND BIOGEOGRAPHY; LIZARD AMEIVA-CHRYSOLAEMA; LENGTH DIFFERENCE TEST; HISTORICAL BIOGEOGRAPHY; CARIBBEAN REGION; CENOZOIC BIOGEOGRAPHY; EVOLUTIONARY TREES; ADAPTIVE RADIATION; SEXUAL SELECTION AB Aim In this study we present a molecular phylogenetic and phylogeographical analysis of Peltophryne (Anura: Bufonidae), an endemic genus of Antillean toads, to investigate the spatial and temporal origins of the genus, with particular focus on the eight Cuban species. Location Greater Antilles, with extensive sampling of the Cuban archipelago. Methods We obtained DNA sequence data from two mitochondrial genes, cytochrome c oxidase subunit I (COI) and ribosomal RNA (16S), for 124 toads representing all eight Cuban species, and combined this with published data from Hispaniola (one of three species) and Puerto Rico (one of one species) to establish a molecular phylogeny for Peltophryne. In addition, we explored the phylogeographical structure of widespread Cuban species. For a subset of 42 toads we also obtained DNA sequence data from two nuclear genes, recombination activator-1 (RAG-1) and chemokine receptor 4 (CXCR-4). We combined our molecular data with published DNA sequences from a global sample of bufonid toads to place the spatial and temporal origins of Peltophryne in the Caribbean within a fuller geographical and phylogenetic context. Results All phylogenetic analyses supported the monophyly of West Indian toads. The ancestor of Peltophyrne diverged from its mainland source around the Eocene-Oligocene boundary, with a subsequent radiation across the Caribbean islands taking place during the Miocene. Cuban species are monophyletic with a basal split in the early-middle Miocene that separates extant small-bodied from large-bodied species. Extensive mitochondrial DNA (mtDNA) sampling within widespread Cuban species revealed contrasting phylogeographical patterns. Peltophryne taladai and P. empusa showed deeply divergent lineages, whereas no geographical structure was observed in the widespread P. peltocephala. Main conclusions Our timeline for Peltophryne diversification is consistent with a biogeographical model requiring no long-distance overwater dispersal. Although confidence intervals on divergence time estimates are wide, the stem age of Peltophyrne coincides with the hypothesized GAARlandia landspan or archipelago, which may have connected South America briefly with the Antilles. The ages of Peltophryne for Puerto Rico, Hispaniola and Cuba are consistent with a recently proposed vicariance scenario for the region. Our molecular results support the recognition of all eight species in Cuba, and provide evidence of possible cryptic species. C1 [Alonso, Roberto] Univ La Habana, Museo Hist Nat Felipe Poey, Fac Biol, Havana, Cuba. [Crawford, Andrew J.; Bermingham, Eldredge] Smithsonian Trop Res Inst, Panama City 03092, Panama. [Crawford, Andrew J.] Univ Los Andes, Dept Ciencias Biol, Bogota 4976, Colombia. RP Alonso, R (reprint author), Calle 25 455 E JeI Vedado,Plaza Revoluc, Ciudad De La Habana 10400, Thailand. EM ralonso@fbio.uh.cu OI Crawford, Andrew J./0000-0003-3153-6898 FU Smithsonian Tropical Research Institution; Smithsonian Institution in Molecular Evolution FX We thank the Centro de Inspeccion y Control Ambiental (CICA) for permission to collect the samples in Cuba and export them to Panama. Collections in the Cuban archipelago were made possible by the project 'Creacion, Conservacion y Manejo de Colecciones Zoologicas' of the Institute of Ecology and Systematics. We thank A. Rodriguez, A. Hernandez, M. Hernandez, A. Fong, A. Daniel, I. Ramos, Y. Martinez, M. Canizares, Y. Garcia and the many others who supported us during fieldwork in Cuban Protected Areas. The Autoridad Nacional del Ambiente (ANAM) kindly granted import permits to Panama, obtained via O. Arosemena of the Smithsonian Tropical Research Institute. For their inestimable help and advice in the laboratory we thank G. Grajales, M. Gonzalez, I. Ceron, O. Sanjur, N. Gomez, G. Reina and M. Nunez. For comments on drafts of this paper we thank A. Rodriguez and M. Iturralde-Vinent. The authors are also grateful to L. R. Heaney and two anonymous referees for insightful comments that significantly improved this paper. This work was supported by a Smithsonian Tropical Research Institution Short-term Fellowship to R. A. B. and by a Smithsonian Institution Postdoctoral Fellowship in Molecular Evolution to A.J.C. NR 134 TC 25 Z9 26 U1 1 U2 28 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0305-0270 EI 1365-2699 J9 J BIOGEOGR JI J. Biogeogr. PD MAR PY 2012 VL 39 IS 3 BP 434 EP 451 DI 10.1111/j.1365-2699.2011.02594.x PG 18 WC Ecology; Geography, Physical SC Environmental Sciences & Ecology; Physical Geography GA 897PP UT WOS:000300665400002 ER PT J AU Almeida, EAB Pie, MR Brady, SG Danforth, BN AF Almeida, Eduardo A. B. Pie, Marcio R. Brady, Sean G. Danforth, Bryan N. TI Biogeography and diversification of colletid bees (Hymenoptera: Colletidae): emerging patterns from the southern end of the world SO JOURNAL OF BIOGEOGRAPHY LA English DT Review DE Antarctica; Apoidea; Australia; event-based methods; Gondwana; historical biogeography; macroevolution; palaeoclimatology; South America ID DISPERSAL-VICARIANCE ANALYSIS; EXONEURINE ALLODAPINE BEES; HISTORICAL BIOGEOGRAPHY; MOLECULAR PHYLOGENIES; CONTINENTAL-DRIFT; BREAK-UP; GENETIC DIFFERENTIATION; KERGUELEN PLATEAU; BAYESIAN-APPROACH; GEOGRAPHIC RANGE AB Aim The evolutionary history of bees is presumed to extend back in time to the Early Cretaceous. Among all major clades of bees, Colletidae has been a prime example of an ancient group whose Gondwanan origin probably precedes the complete break-up of Africa, Antarctica, Australia and South America, because modern lineages of this family occur primarily in southern continents. In this paper, we aim to study the temporal and spatial diversification of colletid bees to better understand the processes that have resulted in the present southern disjunctions. Location Southern continents. Methods We assembled a dataset comprising four nuclear genes of a broad sample of Colletidae. We used Bayesian inference analyses to estimate the phylogenetic tree topology and divergence times. Biogeographical relationships were investigated using event-based analytical methods: a Bayesian approach to dispersal-vicariance analysis, a likelihood-based dispersal-extinctioncladogenesis model and a Bayesian model. We also used lineage through time analyses to explore the tempo of radiations of Colletidae and their context in the biogeographical history of these bees. Results Initial diversification of Colletidae took place at the Late Cretaceous (70 Ma). Several (6-14) lineage exchanges between Australia and South America via Antarctica during the Late Cretaceous and Eocene epochs could explain the disjunctions observed between colletid lineages today. All biogeographical methods consistently indicated that there were multiple lineage exchanges between South America and Australia, and these approaches were valuable in exploring the degree of uncertainty inherent in the ancestral reconstructions. Biogeographical and dating results preclude an explanation of Scrapterinae in Africa as a result of vicariance, so one dispersal event is assumed to explain the disjunction in relation to Euryglossinae. The net diversification rate was found to be highest in the recent history of colletid evolution. Main conclusions The biogeography and macroevolutionary history of colletid bees can be explained by a combination of Cenozoic vicariance and palaeoclimatic changes during the Neogene. The austral connection and posterior break-up of South America, Antarctica and Australia resulted in a pattern of disjunct sister lineages. Increased biome aridification coupled with floristic diversification in the southern continents during the Neogene may have contributed to the high rates of cladogenesis in these bees in the last 25-30 million years. C1 [Almeida, Eduardo A. B.] Univ Sao Paulo, Dept Biol, Fac Filosofia Ciencias & Letras Ribeirao Preto, BR-14040901 Ribeirao Preto, SP, Brazil. [Almeida, Eduardo A. B.; Danforth, Bryan N.] Cornell Univ, Dept Entomol, Ithaca, NY 14853 USA. [Pie, Marcio R.] Univ Fed Parana, Dept Zool, BR-81531990 Curitiba, Parana, Brazil. [Brady, Sean G.] Smithsonian Inst, Dept Entomol, Natl Museum Nat Hist, Washington, DC 20560 USA. RP Almeida, EAB (reprint author), Univ Sao Paulo, Dept Biol, Fac Filosofia Ciencias & Letras Ribeirao Preto, Av Bandeirantes 3900, BR-14040901 Ribeirao Preto, SP, Brazil. EM eduardo@ffclrp.usp.br RI Almeida, Eduardo/C-5271-2012; Pie, Marcio/B-7684-2008; Almeida, Eduardo/B-6995-2008 OI Almeida, Eduardo/0000-0001-6017-6364; Almeida, Eduardo/0000-0001-6017-6364 FU National Science Foundation [DEB-0412176]; A. C. Rawlins Endowment; Grace Griswold Fund; Tinker Foundation Latin American; National Science Foundation Research [EF-0431330]; Fundacao de Coordenacao de Aperfeicoamento de Pessoal de Nivel Superior ('CAPES'; Brazilian Ministry of Education) [BEX-0967/01-7]; CNPq [PDJ-150626/2007-0]; CNPq/MCT [571334/2008-3] FX Our thanks for comments on the manuscript to Laurence Packer, Gabriel A. R. Melo, Thomas Buckley, James K. Liebherr and Richard G. Harrison. Discussions with John Ascher, Dalton Amorim, Connal Eardley, Alejandra Gandolfo, Katja Hoogendoorn, Terry Houston, Pelin Kayaalp, Remko Leijs, Ricardo Lopes, Melissa Luckow, Charles Michener, Richard Ree, Guilherme Ribeiro, Isabel Sanmartin and Michael Schwarz contributed to the development of this research. Connal Eardley generously participated in field trips to South Africa, and Kenneth Walker and Laurence Packer generously participated in field trips to Australia. Specimens obtained on these field trips provided important material for this study. The majority of funding for this research came from a National Science Foundation Research Grant in Systematic Biology to B.N.D. and E.A.B.A. (DEB-0412176). Additional funding was provided by the A. C. Rawlins Endowment, the Grace Griswold Fund and the Tinker Foundation & Latin American Studies Program (Cornell University). S. G. B. was supported by National Science Foundation Research Grant EF-0431330. E.A.B.A. is thankful to Fundacao de Coordenacao de Aperfeicoamento de Pessoal de Nivel Superior ('CAPES'; Brazilian Ministry of Education) for the scholarship BEX-0967/01-7 and to CNPq for the fellowship PDJ-150626/2007-0. M. R. P. was funded by CNPq/MCT (grant 571334/2008-3). NR 122 TC 38 Z9 38 U1 3 U2 52 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0305-0270 EI 1365-2699 J9 J BIOGEOGR JI J. Biogeogr. PD MAR PY 2012 VL 39 IS 3 BP 526 EP 544 DI 10.1111/j.1365-2699.2011.02624.x PG 19 WC Ecology; Geography, Physical SC Environmental Sciences & Ecology; Physical Geography GA 897PP UT WOS:000300665400009 ER PT J AU Blakeslee, AMH Altman, I Miller, AW Byers, JE Gregory, CEH AF Blakeslee, April M. H. Altman, Irit Miller, A. Whitman Byers, James E. Gregory, Caitlin E. Hamer TI Parasites and invasions: a biogeographic examination of parasites and hosts in native and introduced ranges SO JOURNAL OF BIOGEOGRAPHY LA English DT Article DE Biogeography; gastropods; Ilyanassa obsoleta; intertidal; introduction vector; invasion history; Littorina saxatilis; North America; parasite; prevalence ID LARVAL TREMATODE INFECTIONS; ENEMY RELEASE HYPOTHESIS; SNAIL INTERMEDIATE HOSTS; BIRD FINAL HOSTS; COMMUNITY STRUCTURE; SPATIAL HETEROGENEITY; SPECIES COEXISTENCE; ILYANASSA-OBSOLETA; GENETIC DIVERSITY; INTERTIDAL ZONE AB Aim To use a comparative approach to understand parasite demographic patterns in native versus introduced populations, evaluating the potential roles of host invasion history and parasite life history. Location North American east and west coasts with a focus on San Francisco Bay (SFB). Methods Species richness and prevalence of trematode parasites were examined in the native and introduced ranges of two gastropod host species, Ilyanassa obsoleta and Littorina saxatilis. We divided the native range into the putative source area for introduction and areas to the north and south; we also sampled the overlapping introduced range in SFB. We dissected 14,781 snails from 103 populations and recorded the prevalence and identity of trematode parasites. We compared trematode species richness and prevalence across the hosts' introduced and native ranges, and evaluated the influence of host availability on observed patterns. Results Relative to the native range, both I. obsoleta and L. saxatilis have escaped (lost) parasites in SFB, and L. saxatilis demonstrated a greater reduction of trematode diversity and infection prevalence than I. obsoleta. This was not due to sampling inequalities between the hosts. Instead, rarefaction curves suggested complete capture of trematode species in native source and SFB subregions, except for L. saxatilis in SFB, where infection was extremely rare. For I. obsoleta, infection prevalence of trematodes using fish definitive hosts was significantly lower in SFB compared to the native range, unlike those using bird hosts. Host availability partly explained the presence of introduced trematodes in SFB. Main conclusions Differential losses of parasite richness and prevalence for the two gastropod host species in their introduced range is probably the result of several mechanistic factors: time since introduction, propagule pressure, vector of introduction, and host availability. Moreover, the recent occurrence of L. saxatilis' invasion and its active introduction vector suggest that its parasite diversity and distribution will probably increase over time. Our study suggests that host invasion history and parasite life history play key roles in the extent and diversity of trematodes transferred to introduced populations. Our results also provide vital information for understanding community-level influences of parasite introductions, as well as for disease ecology in general. C1 [Blakeslee, April M. H.; Miller, A. Whitman; Gregory, Caitlin E. Hamer] Smithsonian Environm Res Ctr, Marine Invas Lab, Edgewater, MD 21037 USA. [Altman, Irit] Univ New Hampshire, CAMEO, Ocean Proc Anal Lab, Durham, NH 03824 USA. [Byers, James E.] Univ Georgia, Odum Sch Ecol, Athens, GA 30602 USA. [Gregory, Caitlin E. Hamer] Duke Univ, Nicholas Inst Environm Policy Solut, Durham, NC 27708 USA. RP Blakeslee, AMH (reprint author), Long Isl Univ, Dept Biol, CW Post,720 No Blvd, Brookville, NY 11548 USA. EM april.blakeslee@liu.edu OI Ruiz, Gregory/0000-0003-2499-441X; Miller, Whitman/0000-0003-0484-182X FU Smithsonian Institution; Marine Science Network; US Department of Commerce's National Oceanic and Atmospheric Administration [NA16RG1035] FX We thank the following for their assistance in the field and lab: G. Ashton, C. Brown, J. Canning Clode, J. Carlton, A. Chang, J. Dawson, A. Fowler, L. Haram, K. Maglies, D. Padilla and C. Yeager. A. M. H. Blakeslee was funded by a Smithsonian Institution postdoctoral fellowship and a Marine Science Network postdoctoral fellowship. I. Altman was funded by the National Sea Grant College Program of the US Department of Commerce's National Oceanic and Atmospheric Administration grant NA16RG1035 to the N.H. Sea Grant College Program. We also thank two anonymous referees for their comments and suggestions. NR 80 TC 18 Z9 18 U1 2 U2 62 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0305-0270 EI 1365-2699 J9 J BIOGEOGR JI J. Biogeogr. PD MAR PY 2012 VL 39 IS 3 BP 609 EP 622 DI 10.1111/j.1365-2699.2011.02631.x PG 14 WC Ecology; Geography, Physical SC Environmental Sciences & Ecology; Physical Geography GA 897PP UT WOS:000300665400015 ER PT J AU Lidman, C Hayes, M Jones, DH Schaerer, D Westra, E Tapken, C Meisenheimer, K Verhamme, A AF Lidman, C. Hayes, M. Jones, D. H. Schaerer, D. Westra, E. Tapken, C. Meisenheimer, K. Verhamme, A. TI The properties of the brightest Ly alpha emitters at z similar to 5.7 SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE ISM: general; galaxies: formation; galaxies: high-redshift; galaxies: individual: SGP 8884; galaxies: individual: S11 5236; galaxies: starburst ID STAR-FORMING GALAXIES; LYMAN-BREAK GALAXIES; HIGH-REDSHIFT GALAXIES; ULTRA-DEEP-FIELD; REST-FRAME ULTRAVIOLET; STELLAR POPULATIONS; COSMIC REIONIZATION; RADIATION TRANSFER; EMITTING GALAXIES; FORMATION HISTORY AB We use deep Very Large Telescope (VLT) optical and near-infrared spectroscopy and deep Spitzer/IRAC imaging to examine the properties of two of the most luminous Lya emitters at z = 5.7. The continuum redward of the Lya line is clearly detected in both objects, thus facilitating a relatively accurate measurement (1020 per cent uncertainties) of the observed rest-frame equivalent widths, which are around 160 angstrom for both objects. Through detailed modelling of the profile of the Lya line with a 3D Monte Carlo radiative transfer code, we estimate the intrinsic rest-frame equivalent width of Lya and find values that are around 300 angstrom, which is at the upper end of the range allowed for very young, moderately metal-poor star-forming galaxies. However, the uncertainties are large and values as high as 700 angstrom are permitted by the data. Both Lya emitters are detected at 3.6 m in deep images taken with the Spitzer Space Telescope. We use these measurements, the measurement of the continuum redward of Lya and other photometry to constrain the spectral energy distributions of these very luminous Lya emitters and to compare them with three similar Lya emitters from the literature. The contribution from nebular emission is included in our models: excluding it results in significantly higher masses. Four of the five Lya emitters have masses of the order of similar to 109 M and fairly high specific star formation rates (10-100 Gyr-1). While our two Lya emitters appear similar in terms of the observed Lya rest-frame equivalent width, they are quite distinct from each other in terms of age, mass and star formation history. Evidence for dust is found in all objects, and emission from nebular lines often makes a dominant contribution to the rest-frame 3.6 m flux. Rich in emission lines, these objects are prime targets for the next generation of extremely large telescopes, the James Webb Space Telescope (JWST) and the Atacama Large Millimeter Array (ALMA). C1 [Lidman, C.] Australian Astron Observ, Epping, NSW 1710, Australia. [Hayes, M.; Schaerer, D.] Univ Geneva, Observ Geneva, CH-1290 Versoix, Switzerland. [Hayes, M.; Schaerer, D.] CNRS, IRAP, F-31400 Toulouse, France. [Jones, D. H.] Monash Univ, Sch Phys, Clayton, Vic 3800, Australia. [Westra, E.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. [Tapken, C.] Inst Astrophys, D-14482 Potsdam, Germany. [Meisenheimer, K.] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Verhamme, A.] Univ Lyon 1, Observ Lyon, F-69230 St Genis Laval, France. [Verhamme, A.] Univ Lyon, F-69003 Lyon, France. [Verhamme, A.] Ecole Normale Super Lyon, CNRS, UMR 5574, Ctr Rech Astrophys Lyon, F-69007 Lyon, France. RP Lidman, C (reprint author), Australian Astron Observ, POB 296, Epping, NSW 1710, Australia. EM clidman@aao.gov.au RI Hayes, Matthew/D-6692-2014 OI Hayes, Matthew/0000-0001-8587-218X FU Oskar Klein Centre at the University of Stockholm; Australian Research Council (ARC); Swiss National Science Foundation FX CL wishes to acknowledge the support of the Oskar Klein Centre at the University of Stockholm and the support of the Australian Research Council (ARC) through the ARC Future Fellowship. DS and MH acknowledge support from the Swiss National Science Foundation. NR 70 TC 15 Z9 15 U1 0 U2 0 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD MAR PY 2012 VL 420 IS 3 BP 1946 EP 1958 DI 10.1111/j.1365-2966.2011.19994.x PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 897ZI UT WOS:000300702200008 ER PT J AU Salucci, P Wilkinson, MI Walker, MG Gilmore, GF Grebel, EK Koch, A Martins, C Wyse, RFG AF Salucci, Paolo Wilkinson, Mark I. Walker, Matthew G. Gilmore, Gerard F. Grebel, Eva K. Koch, Andreas Frigerio Martins, Christiane Wyse, Rosemary F. G. TI Dwarf spheroidal galaxy kinematics and spiral galaxy scaling laws SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies: dwarf; galaxies: kinematics and dynamics; Local Group; dark matter ID SURFACE BRIGHTNESS GALAXIES; RESOLUTION ROTATION CURVES; VELOCITY DISPERSION PROFILES; EXPLORING HALO SUBSTRUCTURE; DARK-MATTER DISTRIBUTION; COMMON MASS SCALE; MILKY-WAY; LEO-I; STELLAR-SYSTEMS; TIDAL TAILS AB Kinematic surveys of the dwarf spheroidal (dSph) satellites of the Milky Way are revealing tantalizing hints about the structure of dark matter (DM) haloes at the low-mass end of the galaxy luminosity function. At the bright end, modelling of spiral galaxies has shown that their rotation curves are consistent with the hypothesis of a universal rotation curve whose shape is supported by a cored dark matter halo. In this paper, we investigate whether the internal kinematics of the Milky Way dSphs are consistent with the particular cored DM distributions which reproduce the properties of spiral galaxies. Although the DM densities in dSphs are typically almost two orders of magnitude higher than those found in (larger) disc systems, we find consistency between dSph kinematics and Burkert DM haloes whose core radii r0 and central densities ?0 lie on the extrapolation of the scaling law seen in spiral galaxies: log ?0?a log r0+ const with 0.9 < a < 1.1. We similarly find that the dSph data are consistent with the relation between ?0 and baryon scalelength seen in spiral galaxies. While the origin of these scaling relations is unclear, the finding that a single DM halo profile is consistent with kinematic data in galaxies of widely varying size, luminosity and Hubble type is important for our understanding of observed galaxies and must be accounted for in models of galaxy formation. C1 [Salucci, Paolo] SISSA, Dept Astrophys, I-34014 Trieste, Italy. [Wilkinson, Mark I.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. [Walker, Matthew G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Gilmore, Gerard F.] Univ Cambridge, Inst Astron, Cambridge CB3 OHA, England. [Grebel, Eva K.] Univ Heidelberg, Astron Rechen Inst, Zentrum Astron, D-69120 Heidelberg, Germany. [Koch, Andreas] Univ Heidelberg, Zentrum Astron, D-69117 Heidelberg, Germany. [Frigerio Martins, Christiane] Univ Fed Fluminense, INFES, BR-28470 Rio De Janeiro, Brazil. [Wyse, Rosemary F. G.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. RP Salucci, P (reprint author), SISSA, Dept Astrophys, Via Beirut, I-34014 Trieste, Italy. EM cfrigerio@ufabc.edu.br RI Walker, Matthew/P-1777-2014; OI Walker, Matthew/0000-0003-2496-1925; Koch, Andreas/0000-0002-9859-4956; /0000-0002-1891-3794 FU Royal Society University; NASA [HST-HF-51283.01-A, NAS5-26555]; Space Telescope Science Institute; German Research Foundation (DFG) [Sonderforschungsbereich SFB 881]; Deutsche Forschungsgemeinschaft [Ko 4161/1] FX MIW acknowledges support from a Royal Society University Research Fellowship. MGW is supported by NASA through Hubble Fellowship grant HST-HF-51283.01-A, awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., for NASA, under contract NAS5-26555. EKG is supported by Sonderforschungsbereich SFB 881 'The Milky Way System' (subproject A2) of the German Research Foundation (DFG). AK thanks the Deutsche Forschungsgemeinschaft for funding from Emmy-Noether grant Ko 4161/1. NR 84 TC 62 Z9 62 U1 0 U2 1 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD MAR PY 2012 VL 420 IS 3 BP 2034 EP 2041 DI 10.1111/j.1365-2966.2011.20144.x PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 897ZI UT WOS:000300702200014 ER PT J AU Riaz, B Honda, M Campins, H Micela, G Guarcello, MG Gledhill, T Hough, J Martin, EL AF Riaz, B. Honda, M. Campins, H. Micela, G. Guarcello, M. G. Gledhill, T. Hough, J. Martin, E. L. TI The radial distribution of dust species in young brown dwarf discs SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE stars: abundances; brown dwarfs; circumstellar matter; stars: low-mass ID INTERSTELLAR SILICATE MINERALOGY; LOW-TEMPERATURE CRYSTALLIZATION; PROTOPLANETARY ACCRETION DISKS; SCORPIUS OB ASSOCIATION; AURIGA MOLECULAR CLOUD; STAR-FORMING REGION; LOW-MASS STAR; GRAIN-GROWTH; CIRCUMSTELLAR DISK; SIZE DISTRIBUTION AB We present a study of the radial distribution of dust species in young brown dwarf discs. Our work is based on a compositional analysis of the 10 and 20 mu m silicate emission features for brown dwarfs in the TaurusAuriga star-forming region. A fundamental finding of our work is that brown dwarfs exhibit stronger signs of dust processing in the cold component of the disc, compared to the higher mass T Tauri stars in Taurus. For nearly all of our targets, we find a flat disc structure, which is consistent with the stronger signs of dust processing observed in these discs. For the case of one brown dwarf, 2M04230607, we find the forsterite mass fraction to be a factor of similar to 3 higher in the outer disc compared to the inner disc region. Simple large-scale radial mixing cannot account for this gradient in the dust chemical composition, and some local crystalline formation mechanism may be effective in this disc. The relatively high abundance of crystalline silicates in the outer cold regions of brown dwarf discs provides an interesting analogy to comets. In this context, we have discussed the applicability of the various mechanisms that have been proposed for comets on the formation and the outward transport of high-temperature material. We also present Chandra X-ray observations for two Taurus brown dwarfs, 2M04414825 and CFHT-BD-Tau 9. We find 2M04414825, which has an similar to 12 per cent crystalline mass fraction, to be more than an order of magnitude brighter in X-ray than CFHT-BD-Tau 9, which has an similar to 35 per cent crystalline mass fraction. Combining with previous X-ray data, we find the inner disc crystalline mass fractions to be anti-correlated with the X-ray strength. C1 [Riaz, B.; Gledhill, T.; Hough, J.] Univ Hertfordshire, Sci & Technol Res Inst, Ctr Astrophys Res, Hatfield AL10 9AB, Herts, England. [Honda, M.] Kanagawa Univ, Dept Informat Sci, Hiratsuka, Kanagawa 2591293, Japan. [Campins, H.] Univ Cent Florida, Dept Phys, Orlando, FL 32816 USA. [Micela, G.] INAF Osservatorio Astron Palermo, I-90134 Palermo, Italy. [Guarcello, M. G.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. [Martin, E. L.] CSIC INTA, Ctr Astrophys, Madrid 28850, Spain. RP Riaz, B (reprint author), Univ Hertfordshire, Sci & Technol Res Inst, Ctr Astrophys Res, Hatfield AL10 9AB, Herts, England. EM b.riaz@herts.ac.uk OI Micela, Giuseppina/0000-0002-9900-4751 FU National Aeronautics and Space Administration [12200172, NAS8-03060]; National Science Foundation FX Support for this work was provided by the National Aeronautics and Space Administration through Chandra Award Number 12200172 issued by the Chandra X-ray Observatory Center, which is operated by the Smithsonian Astrophysical Observatory for and on behalf of the National Aeronautics Space Administration under contract NAS8-03060. HC acknowledges support from NASA and the National Science Foundation. 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 work has made use of the SIMBAD data base. NR 82 TC 13 Z9 13 U1 0 U2 3 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD MAR PY 2012 VL 420 IS 3 BP 2603 EP 2624 DI 10.1111/j.1365-2966.2011.20233.x PG 22 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 897ZI UT WOS:000300702200062 ER PT J AU Watters, TR Robinson, MS Banks, ME Tran, T Denevi, BW AF Watters, Thomas R. Robinson, Mark S. Banks, Maria E. Thanh Tran Denevi, Brett W. TI Recent extensional tectonics on the Moon revealed by the Lunar Reconnaissance Orbiter Camera SO NATURE GEOSCIENCE LA English DT Article ID FLOOR-FRACTURED CRATERS; VISCOUS RELAXATION; EMPLACEMENT; SURFACE; BASINS; AGES AB Large-scale expressions of lunar tectonics-contractional wrinkle ridges and extensional rilles or graben-are directly related to stresses induced by mare basalt-filled basins(1,2). Basin-related extensional tectonic activity ceased about 3.6Gyr ago, whereas contractional tectonics continued until about 1.2Gyr ago(2). In the lunar highlands, relatively young contractional lobate scarps, less than 1Gyr in age, were first identified in Apollo-era photographs(3). However, no evidence of extensional landforms was found beyond the influence of mare basalt-filled basins and floor-fractured craters. Here we identify previously undetected small-scale graben in the farside highlands and in the mare basalts in images from the Lunar Reconnaissance Orbiter Camera. Crosscut impact craters with diameters as small as about 10 m, a lack of superposed craters, and graben depths as shallow as similar to 1m suggest these pristine-appearing graben are less than 50 Myr old. Thus, the young graben indicate recent extensional tectonic activity on the Moon where extensional stresses locally exceeded compressional stresses. We propose that these findings may be inconsistent with a totally molten early Moon, given that thermal history models for this scenario predict a high level of late-stage compressional stress(4-6) that might be expected to completely suppress the formation of graben. C1 [Watters, Thomas R.; Banks, Maria E.] Smithsonian Inst, Ctr Earth & Planetary Studies, Washington, DC 20560 USA. [Robinson, Mark S.; Thanh Tran] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85251 USA. [Denevi, Brett W.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. RP Watters, TR (reprint author), Smithsonian Inst, Ctr Earth & Planetary Studies, Washington, DC 20560 USA. EM watterst@si.edu RI Denevi, Brett/I-6502-2012 OI Denevi, Brett/0000-0001-7837-6663 FU National Aeronautics and Space Administration (NASA) [NNX08AM73G] FX We thank H.J. Melosh for helpful comments that greatly improved the manuscript. We gratefully acknowledge the LRO and LROC engineers and technical support personnel. This work was supported by National Aeronautics and Space Administration (NASA) Grant NNX08AM73G. NR 29 TC 16 Z9 17 U1 1 U2 16 PU NATURE PUBLISHING GROUP PI NEW YORK PA 75 VARICK ST, 9TH FLR, NEW YORK, NY 10013-1917 USA SN 1752-0894 J9 NAT GEOSCI JI Nat. Geosci. PD MAR PY 2012 VL 5 IS 3 BP 181 EP 185 DI 10.1038/NGEO1387 PG 5 WC Geosciences, Multidisciplinary SC Geology GA 900HZ UT WOS:000300879000010 ER PT J AU Nagele, S Pazourek, R Feist, J Burgdorfer, J AF Nagele, S. Pazourek, R. Feist, J. Burgdoerfer, J. TI Time shifts in photoemission from a fully correlated two-electron model system SO PHYSICAL REVIEW A LA English DT Article ID DEPENDENT SCHRODINGER-EQUATION; PHASE-SHIFT; ATTOSECOND; COULOMB; SPECTROSCOPY; IONIZATION; PULSES; FIELDS AB We theoretically investigate time-resolved photoemission originating from two different shells (1s and 2p) of a fully correlated atomic two-electron model system ionized by an extreme-ultraviolet attosecond light pulse. The parameters of the model system are tuned such that the ionization potentials of the 1s and 2p electrons have values close to those of the 2s and 2p levels in a neon atom, for which a relative time delay has been measured in a recent attosecond streaking experiment by Schultze et al. [Science 328, 1658 (2010)]. Up to now theoretical efforts could account only for delays more than a factor of 2 shorter than the reported experimental value. By solving the time-dependent Schrodinger equation numerically exactly we explore the influence of correlations on the time delay previously implicated as one of the potential sources of discrepancies. We investigate the influence of the interplay between electron interactions and the probing streaking infrared field on the extracted relative delays between the two emission channels. We find that for our model system the inclusion of electronic correlation only slightly modifies the time shifts, as compared to a mean-field treatment. In particular, the correlation-induced time delay is contained in the Eisenbud-Wigner-Smith time delay for the photoionization process. C1 [Nagele, S.; Pazourek, R.; Burgdoerfer, J.] Vienna Univ Technol, Inst Theoret Phys, A-1040 Vienna, Austria. [Feist, J.] Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom & Mol Phys, Cambridge, MA 02138 USA. RP Nagele, S (reprint author), Vienna Univ Technol, Inst Theoret Phys, A-1040 Vienna, Austria. EM stefan.nagele@tuwien.ac.at; renate.pazourek@tuwien.ac.at RI Nagele, Stefan/E-6938-2011; Feist, Johannes/J-7394-2012 OI Nagele, Stefan/0000-0003-1213-0294; Feist, Johannes/0000-0002-7972-0646 FU FWF-Austria [SFB016, P21141-N16]; National Science Foundation [TG-PHY090031]; TU Vienna Doctoral Program "Functional Matter" FX This work was supported by the FWF-Austria, Grants No. SFB016 and No. P21141-N16, and in part by the National Science Foundation through TeraGrid resources provided by NICS and TACC under Grant No. TG-PHY090031. The computational results presented have also been achieved in part using the Vienna Scientific Cluster (VSC). R. P. acknowledges support by the TU Vienna Doctoral Program "Functional Matter" and J.F. by the NSF through a grant to ITAMP. NR 45 TC 42 Z9 42 U1 0 U2 13 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 1050-2947 J9 PHYS REV A JI Phys. Rev. A PD MAR 1 PY 2012 VL 85 IS 3 AR 033401 DI 10.1103/PhysRevA.85.033401 PG 7 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA 900ZM UT WOS:000300931300002 ER PT J AU Savin, DW Brickhouse, NS Cowan, JJ Drake, RP Federman, SR Ferland, GJ Frank, A Gudipati, MS Haxton, WC Herbst, E Profumo, S Salama, F Ziurys, LM Zweibel, EG AF Savin, D. W. Brickhouse, N. S. Cowan, J. J. Drake, R. P. Federman, S. R. Ferland, G. J. Frank, A. Gudipati, M. S. Haxton, W. C. Herbst, E. Profumo, S. Salama, F. Ziurys, L. M. Zweibel, E. G. TI The impact of recent advances in laboratory astrophysics on our understanding of the cosmos SO REPORTS ON PROGRESS IN PHYSICS LA English DT Review ID METAL-POOR STARS; ACTIVE GALACTIC NUCLEI; X-RAY-SPECTRUM; VY CANIS MAJORIS; ATOMIC TRANSITION-PROBABILITIES; DIFFUSE INTERSTELLAR CLOUDS; FINITE-DENSITY PLASMAS; R-PROCESS-RICH; T-TAURI STARS; EXPERIMENTAL OSCILLATOR-STRENGTHS AB An emerging theme in modern astrophysics is the connection between astronomical observations and the underlying physical phenomena that drive our cosmos. Both the mechanisms responsible for the observed astrophysical phenomena and the tools used to probe such phenomena-the radiation and particle spectra we observe-have their roots in atomic, molecular, condensed matter, plasma, nuclear and particle physics. Chemistry is implicitly included in both molecular and condensed matter physics. This connection is the theme of the present report, which provides a broad, though non-exhaustive, overview of progress in our understanding of the cosmos resulting from recent theoretical and experimental advances in what is commonly called laboratory astrophysics. This work, carried out by a diverse community of laboratory astrophysicists, is increasingly important as astrophysics transitions into an era of precise measurement and high fidelity modeling. C1 [Savin, D. W.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA. [Brickhouse, N. S.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Cowan, J. J.] Univ Oklahoma, Homer L Dodge Dept Phys & Astron, Norman, OK 73019 USA. [Drake, R. P.] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA. [Federman, S. R.] Univ Toledo, Dept Phys & Astron, Toledo, OH 43606 USA. [Ferland, G. J.] Univ Kentucky, Dept Phys, Lexington, KY 40506 USA. [Frank, A.] Univ Rochester, Dept Phys & Astron, Rochester, NY 14627 USA. [Gudipati, M. S.] CALTECH, Jet Prop Lab, Div Sci, Pasadena, CA 91109 USA. [Haxton, W. C.] Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA. [Haxton, W. C.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. [Herbst, E.] Univ Virginia, Dept Chem, Charlottesville, VA 22904 USA. [Profumo, S.] Univ Calif Santa Cruz, Dept Phys, Santa Cruz, CA 95064 USA. [Salama, F.] NASA, Ames Res Ctr, Div Space Sci, Moffett Field, CA 94035 USA. [Ziurys, L. M.] Univ Arizona, Arizona Radio Observ, Dept Chem, Tucson, AZ 85721 USA. [Ziurys, L. M.] Univ Arizona, Arizona Radio Observ, Dept Astron, Tucson, AZ 85721 USA. [Ziurys, L. M.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Zweibel, E. G.] Univ Wisconsin, Dept Astron, Madison, WI 53706 USA. [Zweibel, E. G.] Univ Wisconsin, Dept Phys, Madison, WI 53706 USA. [Herbst, E.] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA. [Herbst, E.] Univ Virginia, Dept Phys, Charlottesville, VA 22904 USA. RP Savin, DW (reprint author), Columbia Univ, Columbia Astrophys Lab, 538 W 120th St, New York, NY 10027 USA. RI Savin, Daniel/B-9576-2012; Gudipati, Murthy/F-7575-2011; Salama, Farid/A-8787-2009; Drake, R Paul/I-9218-2012; OI Savin, Daniel/0000-0002-1111-6610; Salama, Farid/0000-0002-6064-4401; Drake, R Paul/0000-0002-5450-9844; Brickhouse, Nancy/0000-0002-8704-4473; Ferland, Gary/0000-0003-4503-6333 FU NASA [NAS8-03060, 07-ATFP07-0124, 10-ATP10-0053, 10-ADAP10-0073]; National Science Foundation [AST 0707447, 0908877, PHY-0757911, PHY-0821899]; DOE/NNSA Defense Sciences and Advanced Scientific Computing from DOE/Science Office of Fusion Energy Sciences; Defense Threat Reduction Agency; STScI [HST-AR-12125.01, HST-GO-12309]; NASA Astrobiology Institute 'Icy Worlds'; Jet Propulsion Laboratory, California Institute of Technology under National Aeronautics and Space Administration; US Department of Energy [DE-SC00046548, DE-FG02-04ER41268]; NASA Science Mission Directorate; NSF Division of Astronomical Sciences Astronomy and Astrophysics FX The authors thank their many colleagues including J E Bailey, P Beiersdorfer, G V Brown, J R Crespo Lopez-Urrutia, H Ji, H Kreckel, J E Lawler, M Medvedev, T Plewa, D Sasselov, R K Smith, C Sneden, B J Wargelin and S Widicus Weaver for stimulating conversations. NSB was supported in part by the NASA contract NAS8-03060 to the Smithsonian Astrophysical Observatory for the Chandra X-ray Center. JJC is supported in part by the National Science Foundation through grant AST 0707447. RPD acknowledges support from DOE/NNSA Defense Sciences and Advanced Scientific Computing, from DOE/Science Office of Fusion Energy Sciences and from the Defense Threat Reduction Agency. GJF acknowledges support by NSF (0908877), NASA (07-ATFP07-0124, 10-ATP10-0053 and 10-ADAP10-0073) and STScI (HST-AR-12125.01 and HST-GO-12309). MSG acknowledges funding from NASA Astrobiology Institute 'Icy Worlds' and support from the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. WCH was supported in part by the US Department of Energy under grant DE-SC00046548 to the University of California at Berkeley. EH acknowledges the support of NASA through its program in laboratory astrophysics and through the Herschel program. SP is partly supported by the US Department of Energy with an Outstanding Junior Investigator Award and by Contract DE-FG02-04ER41268 and by NSF Grant PHY-0757911. FS acknowledges the support of the Astrophysics Research and Analysis Program of NASA Science Mission Directorate. DWS is supported in part by the NASA Astronomy and Physics Research and Analysis program, the NASA Solar Heliospheric Physics program and the NSF Division of Astronomical Sciences Astronomy and Astrophysics Grants program. EGZ was supported in part by the NSF grant PHY-0821899 to the University of Wisconsin. NR 673 TC 26 Z9 26 U1 4 U2 42 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0034-4885 EI 1361-6633 J9 REP PROG PHYS JI Rep. Prog. Phys. PD MAR PY 2012 VL 75 IS 3 AR 036901 DI 10.1088/0034-4885/75/3/036901 PG 36 WC Physics, Multidisciplinary SC Physics GA 898JC UT WOS:000300737700006 PM 22790424 ER PT J AU Clough, GW AF Clough, G. Wayne TI DREAM BUILDING SO SMITHSONIAN LA English DT Editorial Material C1 Smithsonian Inst, Washington, DC 20560 USA. RP Clough, GW (reprint author), Smithsonian Inst, Washington, DC 20560 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU SMITHSONIAN ASSOC PI WASHINGTON PA 900 JEFFERSON DR, WASHINGTON, DC 20560 USA SN 0037-7333 J9 SMITHSONIAN JI Smithsonian PD MAR PY 2012 VL 42 IS 11 BP 8 EP 8 PG 1 WC Humanities, Multidisciplinary SC Arts & Humanities - Other Topics GA 898SN UT WOS:000300762200006 ER PT J AU Wang, H Laughinghouse, HD Anderson, MA Chen, F Willliams, E Place, AR Zmora, O Zohar, Y Zheng, TL Hill, RT AF Wang, Hui Laughinghouse, Haywood D. Anderson, Matthew A. Chen, Feng Willliams, Ernest Place, Allen R. Zmora, Odi Zohar, Yonathan Zheng, Tianling Hill, Russell T. TI Novel Bacterial Isolate from Permian Groundwater, Capable of Aggregating Potential Biofuel-Producing Microalga Nannochloropsis oceanica IMET1 SO APPLIED AND ENVIRONMENTAL MICROBIOLOGY LA English DT Article ID HETEROTROPHIC BACTERIA; AZOSPIRILLUM-BRASILENSE; MICROCYSTIS-AERUGINOSA; ALGAL GROWTH; MARINE; PHOSPHORUS; BIODIESEL; IDENTIFICATION; AQUACULTURE; DYNAMICS AB Increasing petroleum costs and climate change have resulted in microalgae receiving attention as potential biofuel producers. Little information is available on the diversity and functions of bacterial communities associated with biofuel-producing algae. A potential biofuel-producing microalgal strain, Nannochloropsis oceanica IMET1, was grown in Permian groundwater. Changes in the bacterial community structure at three temperatures were monitored by two culture-independent methods, and culturable bacteria were characterized. After 9 days of incubation, N. oceanica IMET1 began to aggregate and precipitate in cultures grown at 30 degrees C, whereas cells remained uniformly distributed at 15 degrees C and 25 degrees C. The bacterial communities in cultures at 30 degrees C changed markedly. Some bacteria isolated only at 30 degrees C were tested for their potential for aggregating microalgae. A novel bacterium designated HW001 showed a remarkable ability to aggregate N. oceanica IMET I, causing microalgal cells to aggregate after 3 days of incubation, while the total lipid content of the microalgal cells was not affected. Direct interaction of HW001 and N. oceanica is necessary for aggregation. HW001 can also aggregate the microalgae N. oceanica CT-1, Tetraselmis suecica, and T. chuii as well as the cyanobacterium Synechococcus WH8007. 16S rRNA gene sequence comparisons indicated the great novelty of this strain, which exhibited only 89% sequence similarity with any previously cultured bacteria. Specific primers targeted to HW001 revealed that the strain originated from the Permian groundwater. This study of the bacterial communities associated with potential biofuel-producing microalgae addresses a little-investigated area of microalgal biofuel research and provides a novel approach to harvest biofuel-producing microalgae by using the novel bacterium strain HW001. C1 [Wang, Hui; Anderson, Matthew A.; Chen, Feng; Willliams, Ernest; Place, Allen R.; Hill, Russell T.] Univ Maryland, Ctr Environm Sci, Inst Marine & Environm Technol, Baltimore, MD 21201 USA. [Zmora, Odi; Zohar, Yonathan] Univ Maryland Baltimore Cty, Baltimore, MD 21228 USA. [Wang, Hui; Zheng, Tianling] Xiamen Univ, Key Lab, Minist Educ Coast & Wetland Ecosyst, Sch Life Sci, Xiamen, Fujian, Peoples R China. [Wang, Hui; Zheng, Tianling] Xiamen Univ, State Key Lab Marine Environm Sci, Xiamen, Fujian, Peoples R China. [Laughinghouse, Haywood D.] Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, Washington, DC 20560 USA. RP Hill, RT (reprint author), Univ Maryland, Ctr Environm Sci, Inst Marine & Environm Technol, Baltimore, MD 21201 USA. EM wshwzh@xmu.edu.cn; hill@umces.edu RI Zheng, TL/G-3974-2010; Place, Allen/F-9267-2013; Chen, Feng/P-3088-2014; Laughinghouse, Haywood/M-5836-2016 OI Laughinghouse, Haywood/0000-0003-1018-6948 FU National Oceanic and Atmospheric Administration [NA10NMF4570328]; China Scholarship Council; NSFC [40930847] FX Funding for this research was provided by the National Oceanic and Atmospheric Administration (NA10NMF4570328). Funding for H.W. was generously provided by the China Scholarship Council and NSFC (40930847). NR 42 TC 18 Z9 22 U1 7 U2 53 PU AMER SOC MICROBIOLOGY PI WASHINGTON PA 1752 N ST NW, WASHINGTON, DC 20036-2904 USA SN 0099-2240 J9 APPL ENVIRON MICROB JI Appl. Environ. Microbiol. PD MAR PY 2012 VL 78 IS 5 BP 1445 EP 1453 DI 10.1128/AEM.06474-11 PG 9 WC Biotechnology & Applied Microbiology; Microbiology SC Biotechnology & Applied Microbiology; Microbiology GA 896AI UT WOS:000300537400015 PM 22194289 ER PT J AU Robertson, BA Porter, C Landis, DA Schemske, DW AF Robertson, Bruce A. Porter, Cody Landis, Douglas A. Schemske, Douglas W. TI Agroenergy Crops Influence the Diversity, Biomass, and Guild Structure of Terrestrial Arthropod Communities SO BIOENERGY RESEARCH LA English DT Article DE Biodiversity; Ecosystem services; Landscape ecology; Agroecology ID AGRICULTURAL LANDSCAPES; INSECT COMMUNITIES; ECOSYSTEM SERVICES; BIOLOGICAL-CONTROL; UNITED-STATES; BIODIVERSITY; CONSERVATION; HERBIVORES; HABITAT; INTENSIFICATION AB Expanded production of contemporary bioenergy crops (e.g., corn) is considered a threat to the conservation of biodiversity, yet next-generation perennially based crops (switchgrass, mixed-grass-forb prairie) may represent an opportunity for enhancing biodiversity in agricultural landscapes. We employed a multi-scaled approach to investigate the relative importance of feedstock selection, forb content, patch size, and landscape-scale habitat structure and composition as factors shaping the diversity and abundance of terrestrial arthropod communities and the biomass of functional groups of arthropods associated with the provisioning of ecosystem services. Compared to intensively managed annual corn fields, switchgrass and mixed-grass-forb prairie plantings were associated with a 230% and 324% increase in arthropod family diversity and a 750% and 2,700% increase in arthropod biomass, respectively. Biomass of arthropod pollinators, herbivores, predators, and parasites were similarly the highest in mixed-grass-forb prairie, intermediate in switchgrass plantings, and the lowest in cornfields. Community-wide biomass and that of several functional arthropod groups were positively linked to increasing forest cover and land cover diversity surrounding biomass plantings, while pollinator and detritivore biomass was lower in smaller fields. Results not only suggest that the choice of biomass feedstock will play an important role in shaping within-field arthropod diversity but also indicate an important role for the composition of this surrounding landscape. Collectively, our results suggest that selection of perennially based biomass feedstocks along with careful attention to crop placement have important potential to enhance biodiversity conservation and the provisioning of ecologically and economically important arthropod-mediated ecosystem services in future agricultural landscapes. C1 [Robertson, Bruce A.] Smithsonian Conservat Biol Inst, Migratory Bird Ctr, Washington, DC 20013 USA. [Robertson, Bruce A.; Porter, Cody; Landis, Douglas A.; Schemske, Douglas W.] Michigan State Univ, DOE Great Lakes Bioenergy Res Ctr, E Lansing, MI 48824 USA. RP Robertson, BA (reprint author), Smithsonian Conservat Biol Inst, Migratory Bird Ctr, Natl Zool Pk, Washington, DC 20013 USA. EM RobertsonBr@si.edu FU DOE Great Lakes Bioenergy Research Center (DOE BER Office of Science) [DE-FC02-07ER64494]; DOE Great Lakes Bioenergy Research Center (DOE OBP Office of Energy Efficiency and Renewable Energy) [DE-AC05-76RL01830]; Smithsonian Conservation Biology Institute, National Zoological Park FX This work was funded by the DOE Great Lakes Bioenergy Research Center (DOE BER Office of Science DE-FC02-07ER64494 and DOE OBP Office of Energy Efficiency and Renewable Energy DE-AC05-76RL01830). BAR was supported by a fellowship from the Smithsonian Conservation Biology Institute, National Zoological Park. NR 67 TC 19 Z9 20 U1 4 U2 67 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 1939-1234 EI 1939-1242 J9 BIOENERG RES JI BioEnergy Res. PD MAR PY 2012 VL 5 IS 1 BP 179 EP 188 DI 10.1007/s12155-011-9161-3 PG 10 WC Energy & Fuels; Environmental Sciences SC Energy & Fuels; Environmental Sciences & Ecology GA 897NV UT WOS:000300658900018 ER PT J AU Jagadeeshan, S O'Dea, A AF Jagadeeshan, Santosh O'Dea, Aaron TI Integrating fossils and molecules to study cupuladriid evolution in an emerging Isthmus SO EVOLUTIONARY ECOLOGY LA English DT Article DE Cupuladria; Isthmus of Panama; Morphological divergence; Fossil; Molecules; Evolutionary ecology ID TROPICAL AMERICAN MOLLUSKS; PANAMA LAND-BRIDGE; BOCAS-DEL-TORO; NEOGENE CUPULADRIIDAE; RAPID SPECIATION; REEF DEVELOPMENT; FAUNAL TURNOVER; OPPOSITE SIDES; WESTERN PANAMA; SOUTH-AMERICA AB Fossils and genes represent two principal sources of data for studying evolutionary biology, but they are rarely unified. The aim of this paper is to integrate the fossil and molecular records of Tropical American cupuladriid bryozoans to elucidate their evolutionary history. Molecules and fossils broadly concur in determining the timing of species divergences, and point to seaway constriction associated with the emergence of the Isthmus of Panama as a driver of speciation. We discover that although cross-Isthmian isolation of taxa was important, strong isolating mechanisms also existed within the southwestern Caribbean (SWC), caused by increasing physical and environmental heterogeneity as inter-oceanic straits constricted in the Late Pliocene. During this time of rapid environmental change and instability, recently diverged species pairs existed in locally separated habitats for around 2 million years, only to co-exist after final closure of the seaway. This pattern is consistent with a model of allopatric speciation caused by local isolating mechanisms followed by secondary contact. Fossils also reveal the trajectories of reproductive life history and morphology during and after species divergences. In the SWC, all extant species started to shift from clonal to aclonal reproduction immediately in response to changing oceanographic conditions. However, it took another million years for colonies to gain skeletal strength, a trait that reduces cloning by fragmentation, suggesting that the appearance of advantageous traits was delayed by 1-2 million years and only arose after the process of allopatric speciation had run its course. Changes in colony shape, height and size also appear to lag 2 million years, but may reflect exploitation of the diverse sedimentary environments created as reefs proliferated at this time. C1 [Jagadeeshan, Santosh; O'Dea, Aaron] Smithsonian Trop Res Inst, Panama City 03092, Panama. RP O'Dea, A (reprint author), Smithsonian Trop Res Inst, Apartado 0843, Panama City 03092, Panama. EM odeaa@si.edu RI O'Dea, Aaron/D-4114-2011 FU NSF [EAR03-45471]; Smithsonian Marine Science Network; Smithsonian Tropical Research Institute; SENACYT; National Geographic Society FX We are indebted to Felix Rodriguez, Brigida Degracia, and Yadixa del Valle who worked tirelessly collecting morphological data. Anthony Coates, Carlos De Gracia, Javier Jara, Amalia Herrera and the crew of the R/V Urraca helped in the field. Ligia Calderon helped with sequencing. Paul Taylor produced the scanning electron micrographs. Adriana Bilgray, Harilaos Lessios and Eldredge Bermigham provided logistical support. We thank Simon Coppard, Osamu Miura, Scott Lidgard and Matthew Dick for stimulating discussion. The manuscript benefited from constructive criticism and suggestions from Matthew Dick and an anonymous reviewer. Recursos Minerales kindly gave permission to collect fossil material in Panama. This work was funded by the NSF (EAR03-45471), the Smithsonian Marine Science Network, the Smithsonian Tropical Research Institute's Tupper Fellowship and Scholarly Studies Programs, SENACYT and the National Geographic Society's Exploration Grants. This work is dedicated to Jeremy B. C. Jackson for his vision, guidance and support. NR 80 TC 5 Z9 6 U1 1 U2 7 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0269-7653 J9 EVOL ECOL JI Evol. Ecol. PD MAR PY 2012 VL 26 IS 2 SI SI BP 337 EP 355 DI 10.1007/s10682-011-9522-6 PG 19 WC Ecology; Evolutionary Biology; Genetics & Heredity SC Environmental Sciences & Ecology; Evolutionary Biology; Genetics & Heredity GA 896FC UT WOS:000300549800007 ER PT J AU Lowery, DL Wagner, DP AF Lowery, Darrin L. Wagner, Daniel P. TI Geochemical impacts to prehistoric iron-rich siliceous artifacts in the nearshore coastal zone SO JOURNAL OF ARCHAEOLOGICAL SCIENCE LA English DT Article DE Coastal geochemistry; Sulfidization; Sulfuricization; Tidal marsh environments; Marine transgression; Inundated archaeological sites; Prehistoric lithic artifacts AB In the Middle Atlantic region of the United States, landscapes drowned by sea level rise contain scores of prehistoric archaeological sites. These sites provide archaeologists with a rare opportunity to investigate various geologic processes. During the transition from a terrestrial to an offshore setting, the materials associated with an archaeological site are exposed to a series of geochemical processes inherent to the formation of tidal marsh. The duration of the geochemical exposure to tidal marsh is largely dependent on the rate of marine transgression. Here we describe the stages associated with the sulfidization and sulfuricization scheme and the impact to iron-rich lithic artifacts from naturally drowned archaeological sites. Sulfidization and sulfuricization should also impact buried archaeological materials as a result of anthropogenic dredge spoil dumping and the creation of man-made tidal marshes along modern coastlines. Our results indicate that the surfaces of an iron-rich artifact, as well as its interior are visually and geochemically altered by prolonged exposure to the anaerobic conditions of a tidal marsh. Not only should researchers be cautious about making lithic material identification on artifacts found within coastal tidal marsh areas, but museum curators should be aware of the damaging impact of long-term aerobic storage. The geochemical tidal marsh scheme that has altered or corroded iron-rich lithic artifacts in the nearshore zone is an expression of a process that has impacted numerous earlier prehistoric sites currently located on the continental shelf or beneath the coastal estuaries around the world. (C) 2011 Elsevier Ltd. All rights reserved. C1 [Lowery, Darrin L.] Smithsonian Inst, Natl Museum Nat Hist, Dept Anthropol, Washington, DC 20560 USA. [Lowery, Darrin L.] Univ Delaware, Dept Geog, Easton, MD 21601 USA. [Wagner, Daniel P.] Geosci Consultants LLC, University Pk, MD 20782 USA. RP Lowery, DL (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Anthropol, Washington, DC 20560 USA. EM darrinlowery@yahoo.com; danwagner@juno.com NR 19 TC 2 Z9 2 U1 1 U2 7 PU ACADEMIC PRESS LTD- ELSEVIER SCIENCE LTD PI LONDON PA 24-28 OVAL RD, LONDON NW1 7DX, ENGLAND SN 0305-4403 J9 J ARCHAEOL SCI JI J. Archaeol. Sci. PD MAR PY 2012 VL 39 IS 3 BP 690 EP 697 DI 10.1016/j.jas.2011.10.035 PG 8 WC Anthropology; Archaeology; Geosciences, Multidisciplinary SC Anthropology; Archaeology; Geology GA 892CS UT WOS:000300264900013 ER PT J AU Santiago, LS Wright, SJ Harms, KE Yavitt, JB Korine, C Garcia, MN Turner, BL AF Santiago, Louis S. Wright, S. Joseph Harms, Kyle E. Yavitt, Joseph B. Korine, Carmi Garcia, Milton N. Turner, Benjamin L. TI Tropical tree seedling growth responses to nitrogen, phosphorus and potassium addition SO JOURNAL OF ECOLOGY LA English DT Article DE Barro Colorado Nature Monument; fertilization; herbivory; Liebig's law of the minimum; multiple limiting resources hypothesis; nutrient limitation; Panama; plant-soil (below-ground) interactions; relative growth rate; tropical forest ID FINE-ROOT-GROWTH; RAIN-FOREST; NUTRIENT LIMITATION; MOIST FOREST; TERRESTRIAL ECOSYSTEMS; LIFE-HISTORY; DRY FORESTS; SOIL; PANAMA; DYNAMICS AB 1. Nutrients are a critical resource for plant growth, but the elements limiting growth in tropical forests have rarely been determined. 2. We investigated the influence of nitrogen (N), phosphorus (P), potassium(K) and micronutrients on seedling biomass and nutrient allocation in a factorial nutrient fertilization experiment in lowland tropical forest at the Barro Colorado Nature Monument, Panama. We also measured 8 years of herbivory and growth for 1800 seedlings. We sought to determine the identity of limiting elements and possible nutrient interactions. 3. The five study species were Alseis blackiana, Desmopsis panamensis, Heisteria concinna, Sorocea affinis and Tetragastris panamensis. Plants grew in deeply shaded understorey with a mean canopy openness of 4.9%(+/-0.7%; 1 SE). 4. Tissue N concentration increased by 11% with N addition. Tissue P concentration increased by 16% with P addition. Tissue K increased by 4% with K addition. K addition reduced root-to-shoot biomass ratio. There was no significant effect of fertilization on specific leaf area or leaf area ratio. 5. The proportion of leaves damaged and the mean level of damage by herbivory increased with P and K addition and showed a significant P x K interaction. 6. Across all species and years, relative growth rate of height increased with K addition and with N and P in combination. Relative growth rate of leaf count trended 8.5% higher with K addition (P = 0.076). 7. We also added micronutrients in a parallel experiment. There was no effect of micronutrient addition on any seedling parameter. 8. Synthesis. K addition affected seedlings by enhancing tissue nutrient concentration, increasing herbivory, reducing root-to-shoot biomass ratio and increasing height growth. Additional effects of N or P on tissue chemistry, herbivory and growth offer support for the multiple limiting resources hypothesis. Our results suggest that seedling growth is limited by nutrients, especially K, even under highly shaded conditions in this lowland tropical forest. C1 [Santiago, Louis S.] Univ Calif Riverside, Dept Bot & Plant Sci, Riverside, CA 92521 USA. [Wright, S. Joseph; Harms, Kyle E.; Garcia, Milton N.; Turner, Benjamin L.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. [Harms, Kyle E.] Louisiana State Univ, Dept Biol Sci, Baton Rouge, LA 70803 USA. [Yavitt, Joseph B.] Cornell Univ, Dept Nat Resources, Ithaca, NY 14853 USA. [Korine, Carmi] Ben Gurion Univ Negev, Jacob Blaustein Inst Desert Res, Mitrani Dept Desert Ecol, IL-84990 Midreshet Ben Gurion, Israel. RP Santiago, LS (reprint author), Univ Calif Riverside, Dept Bot & Plant Sci, 2150 Batchelor Hall, Riverside, CA 92521 USA. EM santiago@ucr.edu RI Turner, Benjamin/E-5940-2011; Korine, Carmi/F-4116-2012; Wright, Stuart/M-3311-2013; Santiago, Louis/E-3185-2016 OI Turner, Benjamin/0000-0002-6585-0722; Wright, Stuart/0000-0003-4260-5676; Santiago, Louis/0000-0001-5994-6122 FU Andrew W. Mellon Foundation; Smithsonian Scholarly Studies grant; University of California FX We gratefully acknowledge Omar Hernandez and Rufino Gonzalez for their diligent efforts in the field, Alex Barron, Walt Carson, Jennifer Powers, Jim Sickman and Klaus Winter for insightful discussions, and the Smithsonian Tropical Research Institute and the University of California, Riverside, for logistical support. This is paper number 750 of the Mitrani Department of Desert Ecology. Partial support for this study was provided by a grant from the Andrew W. Mellon Foundation to Wright, a Smithsonian Scholarly Studies grant to Wright, Harms and Yavitt, and a University of California Regent's Faculty Fellowship to Santiago. NR 63 TC 75 Z9 82 U1 6 U2 138 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0022-0477 J9 J ECOL JI J. Ecol. PD MAR PY 2012 VL 100 IS 2 BP 309 EP 316 DI 10.1111/j.1365-2745.2011.01904.x PG 8 WC Plant Sciences; Ecology SC Plant Sciences; Environmental Sciences & Ecology GA 895MR UT WOS:000300500800002 ER PT J AU Meijer, HJM Gill, A de Louw, PGB Ostende, LWVD Hume, JP Rijsdijk, KF AF Meijer, Hanneke J. M. Gill, Arike de Louw, Perry G. B. Ostende, Lars W. Van Den Hoek Hume, Julian P. Rijsdijk, Kenneth F. TI Dodo remains from an in situ context from Mare aux Songes, Mauritius SO NATURWISSENSCHAFTEN LA English DT Article DE Raphus cucullatus; Insular ecosystem; Mare aux Songes; Mauritius; Taphonomy ID NEW-ZEALAND; SOUTH ISLAND; AFRICAN; TROPICS; SWAMP AB Since 2005, excavations at Mare aux Songes, Mauritius, have revealed the presence of a very rich, similar to 4,200-year-old fossil bone bed including dodo (Raphus cucullatus) bones and bone fragments. The recently excavated dodo assemblage comprises at least 17 individuals and is characterised by the presence of small and fragile skeletal elements, a dominance of leg elements and an absence of juveniles. The hydrology of the area suggests that dodos, like many other species, were probably lured to Mare aux Songes by the presence of freshwater during times of drought. The most likely scenario for the origin of the fossil deposit is that animals became trapped in the sediment in repeated miring events, which would favour the conservation of hindlimbs. Such a scenario is fully in accordance with the taphonomic characteristics of the bone assemblage. C1 [Meijer, Hanneke J. M.] Smithsonian Inst, Natl Museum Nat Hist, Div Birds, Washington, DC 20560 USA. [Meijer, Hanneke J. M.; Gill, Arike; Ostende, Lars W. Van Den Hoek] Netherlands Ctr Biodivers Nat, Dept Geol, NL-2300 RA Leiden, Netherlands. [de Louw, Perry G. B.] Deltares, Dept Soil & Groundwater, NL-3508 AL Utrecht, Netherlands. [Hume, Julian P.] Nat Hist Museum Tring, Bird Grp, Dept Zool, Tring HP23 6AP, Herts, England. [Rijsdijk, Kenneth F.] Univ Amsterdam, Inst Biodivers & Ecosyst Dynam, NL-1098 XH Amsterdam, Netherlands. RP Meijer, HJM (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Div Birds, Washington, DC 20560 USA. EM meijerh@si.edu RI Meijer, Hanneke/A-1912-2013; OI Meijer, Hanneke/0000-0001-7066-6869; Rijsdijk, kenneth/0000-0002-0943-2577 FU Omnicane; TNO-the Geological Survey of the Netherland; Treub Foundation for Research in the Tropics; World Wildlife Fund-The Netherlands; Deltares; Mauritius Museums Council; Hollandia Archaeology; Taylor Smith Group (Mauritius); Air Mauritius; Mauritius Sugar Industry Research Institute; Netherlands Centre for Biodiversity Naturalis FX We are very grateful to C. Foo Kune, former CEO of Mon Tresor Mon Desert Sugar Estate (now Omnicane), and his staff for their hospitality and invaluable support in the field. The excavation would not have been possible without the technical supervision by R. Floore. We thank A. Janoo (National Heritage Fund), C. Baider, F. B. V. Florens, A. Grihault, J. de Vos and J. Brinkkemper for their support in the field and valuable discussions regarding the extinct and extant Mauritian ecosystem. I. Prins provided invaluable logistic support. Fieldwork and research was funded by Omnicane, TNO-the Geological Survey of the Netherland, the Treub Foundation for Research in the Tropics, World Wildlife Fund-The Netherlands, Deltares, Mauritius Museums Council, Hollandia Archaeology, Taylor Smith Group (Mauritius), Air Mauritius, Mauritius Sugar Industry Research Institute and the Netherlands Centre for Biodiversity Naturalis. The funders had no role in study design, data collection and analysis, decision to publish or preparation of the manuscript. We thank S. Olson for insightful comments on an earlier version of the manuscript, and A. Cheke for help on correct citation details. Four anonymous reviewers provided their constructive input. NR 31 TC 6 Z9 7 U1 0 U2 16 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0028-1042 J9 NATURWISSENSCHAFTEN JI Naturwissenschaften PD MAR PY 2012 VL 99 IS 3 BP 177 EP 184 DI 10.1007/s00114-012-0882-8 PG 8 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 897TQ UT WOS:000300680700002 PM 22282037 ER PT J AU Shik, JZ Flatt, D Kay, A Kaspari, M AF Shik, Jonathan Z. Flatt, Deana Kay, Adam Kaspari, Michael TI A life history continuum in the males of a Neotropical ant assemblage: refuting the sperm vessel hypothesis SO NATURWISSENSCHAFTEN LA English DT Article DE Lifespan; Mating system; Tropical rainforest; Metabolic scaling ID SOCIAL INSECTS; HYMENOPTERA-FORMICIDAE; IRIDOMYRMEX-HUMILIS; REPRODUCTIVE-SYSTEM; SOLENOPSIS-INVICTA; ATTA-COLOMBICA; BODY-SIZE; FIRE ANT; FLIGHT; EVOLUTION AB Animal lifespans range from a few days to many decades, and this life history diversity is especially pronounced in ants. Queens can live for decades. Males, in contrast, are often assumed to act as ephemeral sperm delivery vessels that die after a brief mating flight-a view developed from studies of lekking species in temperate habitats. In a tropical ant assemblage, we found that males can live days to months outside the nest, a trait hypothesized to be associated with female calling, another common mating system. We combined feeding experiments with respirometry to show that lifespan can be enhanced over 3 months by feeding outside the nest. In one focal female calling species, Ectatomma ruidum, feeding enhanced male lifespan, but not sperm content. Extended lifespans outside the nest suggest stronger than expected selection on premating traits of male ants, although the ways these traits shape male mating success remain poorly understood. C1 [Shik, Jonathan Z.] N Carolina State Univ, Dept Entomol, Raleigh, NC 27695 USA. [Flatt, Deana; Kaspari, Michael] Univ Oklahoma, Dept Zool, Norman, OK 73019 USA. [Kay, Adam] St Thomas Univ, Dept Biol, St Paul, MN 55105 USA. [Kaspari, Michael] Univ Oklahoma, Grad Program Ecol & Evolutionary Biol, Norman, OK 73019 USA. [Kaspari, Michael] Smithsonian Trop Res Inst, Balboa, Panama. RP Shik, JZ (reprint author), N Carolina State Univ, Dept Entomol, Raleigh, NC 27695 USA. EM jonathan.shik@gmail.com OI Kaspari, Michael/0000-0002-9717-5768 FU National Science Foundation [DEB-0842038]; NSF REU [DEB-0842038] FX This project was funded by the National Science Foundation under the grant DEB-0842038 to A. Kay and M. Kaspari. DF was supported by an NSF REU on the same grant. JZS thanks WR Tschinkel for the instruction on the finer points of male ant dissection and SPA den Boer for instruction in the DAPI sperm staining method. JJ Boomsma and three anonymous reviewers provided many excellent suggestions for improving this manuscript. DD Donoso helped verify the identification of males. NR 44 TC 5 Z9 5 U1 0 U2 13 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0028-1042 EI 1432-1904 J9 NATURWISSENSCHAFTEN JI Naturwissenschaften PD MAR PY 2012 VL 99 IS 3 BP 191 EP 197 DI 10.1007/s00114-012-0884-6 PG 7 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 897TQ UT WOS:000300680700004 PM 22274637 ER PT J AU Waurich, R Braun, BC Comizzoli, P Jewgenow, K AF Waurich, R. Braun, B. C. Comizzoli, P. Jewgenow, K. TI Oct4 expression in early cat embryos: Comparing results from semi-quantitative and quantitative measurements SO REPRODUCTION IN DOMESTIC ANIMALS LA English DT Meeting Abstract CT 45th Annual Conference of Physiology and Pathology of Reproduction/37th Joint Conference on Veterinary and Human Reproduction Medicine/1st Joint German-Polish Conference on Reproductive Medicine CY FEB 29-MAR 02, 2012 CL Berlin, GERMANY C1 [Waurich, R.; Braun, B. C.; Jewgenow, K.] Leibniz Inst Zoo & Wildlife Res IZW, D-10252 Berlin, Germany. [Comizzoli, P.] Smithsonian Conservat Biol Inst, Dept Reprod Sci, Washington, DC 20008 USA. RI Braun, Beate/J-8641-2016 NR 0 TC 0 Z9 0 U1 0 U2 0 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0936-6768 J9 REPROD DOMEST ANIM JI Reprod. Domest. Anim. PD MAR PY 2012 VL 47 SU 2 SI SI BP 55 EP 55 PG 1 WC Agriculture, Dairy & Animal Science; Reproductive Biology; Veterinary Sciences SC Agriculture; Reproductive Biology; Veterinary Sciences GA 895MO UT WOS:000300500500177 ER PT J AU Novotny, V Miller, SE Hrcek, J Baje, L Basset, Y Lewis, OT Stewart, AJA Weiblen, GD AF Novotny, Vojtech Miller, Scott E. Hrcek, Jan Baje, Leontine Basset, Yves Lewis, Owen T. Stewart, Alan J. A. Weiblen, George D. TI Insects on Plants: Explaining the Paradox of Low Diversity within Specialist Herbivore Guilds SO AMERICAN NATURALIST LA English DT Article DE rainforest; New Guinea; host specialization; niche theory; community saturation; species pool ID GUINEA RAIN-FOREST; HOST SPECIALIZATION; SPECIES RICHNESS; TROPICAL FORESTS; ECOLOGICAL COMMUNITIES; PHYTOPHAGOUS INSECTS; BODY-SIZE; LEPIDOPTERA; SPECIFICITY; SPECIATION AB Classical niche theory explains the coexistence of species through their exploitation of different resources. Assemblages of herbivores coexisting on a particular plant species are thus expected to be dominated by species from host-specific guilds with narrow, coexistence-facilitating niches rather than by species from generalist guilds. Exactly the opposite pattern is observed for folivores feeding on trees in New Guinea. The least specialized mobile chewers were the most species rich, followed by the moderately specialized semiconcealed and exposed chewers. The highly specialized miners and mesophyll suckers were the least species-rich guilds. The Poisson distribution of herbivore species richness among plant species in specialized guilds and the absence of a negative correlation between species richness in different guilds on the same plant species suggest that these guilds are not saturated with species. We show that herbivore assemblages are enriched with generalists because these are more completely sampled from regional species pools. Herbivore diversity increases as a power function of plant diversity, and the rate of increase is inversely related to host specificity. The relative species diversity among guilds is thus scale dependent, as the importance of specialized guilds increases with plant diversity. Specialized insect guilds may therefore comprise a larger component of overall diversity in the tropics (where they are also poorly known taxonomically) than in the temperate zone, which has lower plant diversity. C1 [Novotny, Vojtech; Hrcek, Jan] Univ S Bohemia, Czech Acad Sci, Ctr Biol, Ceske Budejovice 37005, Czech Republic. [Novotny, Vojtech; Hrcek, Jan] Univ S Bohemia, Fac Sci, Ceske Budejovice 37005, Czech Republic. [Baje, Leontine] New Guinea Binatang Res Ctr, Madang, Papua N Guinea. [Miller, Scott E.] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20008 USA. [Basset, Yves] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. [Lewis, Owen T.] Univ Oxford, Dept Zool, Oxford OX1 3PS, England. [Stewart, Alan J. A.] Univ Sussex, Sch Life Sci, Brighton BN1 9QG, E Sussex, England. [Weiblen, George D.] Univ Minnesota, Dept Plant Biol, St Paul, MN 55108 USA. RP Novotny, V (reprint author), Univ S Bohemia, Czech Acad Sci, Ctr Biol, Branisovska 31, Ceske Budejovice 37005, Czech Republic. EM novotny@entu.cas.cz RI Basset, Yves/B-6642-2014; Novotny, Vojtech/G-9434-2014; Hrcek, Jan/D-7335-2015; OI Miller, Scott/0000-0002-4138-1378; Novotny, Vojtech/0000-0001-7918-8023; Hrcek, Jan/0000-0003-0711-6447; Stewart, Alan/0000-0001-7878-8879; Lewis, Owen/0000-0001-7935-6111 FU National Science Foundation [DEB-9628840, DEB-9707928, DEB-0211591, DEB-0515678]; Grant Agencies of the Czech Republic [206/ 09/0115, 206/08/H044, P505/10/0673]; Czech Academy of Sciences [AA600960712, AV0Z50070508]; Czech Ministry of Education [LC06073, LH11008, ME9082, MSM6007665801]; Darwin Initiative for the Survival of Species (UK); Center for Tropical Forest Science/Smithsonian Institution Global Earth Observatory; David and Lucile Packard Fellowship in Science and Engineering; Genome Canada FX We thank J. Auga, D. Bito, W. Boen, E. Brus, C. Dahl, K. Darrow, P. Drozd, L. Helgen, S. Ibalim, B. Isua, M. Janda, M. Keltim, J. Kua, R. Kutil, R. Lilip, M. Manumbor, M. Mogia, K. Molem, M. Rimandai, S. Sau, G. Setliff, G. Sosanika, E. Tamtiai, and D. Wal for technical assistance; V. O. Becker, J. Brown, L. Craven, K. Damas, D. R. Davis, J. D. Holloway, M. Horak, T. Kumata, K. Maes, J. Miller, E. G. Munroe, I. Ohshima, J. Rota, M. Shaffer, M. A. Solis, W. Takeuchi, K. Tuck, and T. Whitfeld for taxonomic assistance; P. Hebert for DNA bar codes; and T. Lewinsohn and two anonymous reviewers for comments on the manuscript. This work was supported by the National Science Foundation (DEB-9628840, -9707928, -0211591, and -0515678), the Grant Agencies of the Czech Republic (206/ 09/0115, 206/08/H044, and P505/10/0673), the Czech Academy of Sciences (AA600960712 and AV0Z50070508), the Czech Ministry of Education (LC06073, LH11008, ME9082, and MSM6007665801), the Darwin Initiative for the Survival of Species (UK), the Center for Tropical Forest Science/Smithsonian Institution Global Earth Observatory, and the David and Lucile Packard Fellowship in Science and Engineering (to G. D. W.). DNA bar coding was provided by the Biodiversity Institute of Ontario, with the support of Genome Canada under the iBOL project. NR 53 TC 22 Z9 22 U1 2 U2 67 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0003-0147 J9 AM NAT JI Am. Nat. PD MAR PY 2012 VL 179 IS 3 BP 351 EP 362 DI 10.1086/664082 PG 12 WC Ecology; Evolutionary Biology SC Environmental Sciences & Ecology; Evolutionary Biology GA 894VD UT WOS:000300454400006 PM 22322223 ER PT J AU Pinto-Sanchez, NR Ibanez, R Madrinan, S Sanjur, OI Bermingham, E Crawford, AJ AF Rocio Pinto-Sanchez, Nelsy Ibanez, Roberto Madrinan, Santiago Sanjur, Oris I. Bermingham, Eldredge Crawford, Andrew J. TI The Great American Biotic Interchange in frogs: Multiple and early colonization of Central America by the South American genus Pristimantis (Anura: Craugastoridae) SO MOLECULAR PHYLOGENETICS AND EVOLUTION LA English DT Article DE Ancestral area reconstruction; DEC; Isthmus of Panama; Multi-locus molecular phylogenetics; Terrarana ID PHYLOGENETIC ANALYSIS; DIVERGENCE TIMES; CENOZOIC BIOGEOGRAPHY; EVOLUTIONARY HISTORY; GEOGRAPHIC RANGE; DARIEN PROVINCE; GLOBAL PATTERNS; MIXED MODELS; PHYLOGEOGRAPHY; PANAMA AB The completion of the land bridge between North and South America approximately 3.5-3.1 million years ago (Ma) initiated a tremendous biogeographic event called the Great American Biotic Interchange (GABI), described principally from the mammalian fossil record. The history of biotic interchange between continents for taxonomic groups with poor fossil records, however, is not well understood. Molecular and fossil data suggest that a number of plant and animal lineages crossed the Isthmus of Panama well before 3.5 Ma, leading biologists to speculate about trans-oceanic dispersal mechanisms. Here we present a molecular phylogenetic analysis of the frog genus Pristimantis based on 189 individuals of 137 species, including 71 individuals of 31 species from Panama and Colombia. DNA sequence data were obtained from three mitochondrial (COI, 12S, 16S) and two nuclear (RAG-1 and Tyr) genes, for a total of 4074 base pairs. The resulting phylogenetic hypothesis showed statistically significant conflict with most recognized taxonomic groups within Pristimantis, supporting only the rubicundus Species Series, and the Pristimantis myersi and Pristimantis pardalis Species Groups as monophyletic. Inference of ancestral areas based on a likelihood model of geographic range evolution via dispersal, local extinction, and cladogenesis (DEC) suggested that the colonization of Central America by South American Pristimantis involved at least 11 independent events. Relaxed-clock analyses of divergence times suggested that at least eight of these invasions into Central America took place prior to 4 Ma, mainly in the Miocene. These findings contribute to a growing list of molecular-based biogeographic studies presenting apparent temporal conflicts with the traditional GABI model. (C) 2011 Elsevier Inc. All rights reserved. C1 [Crawford, Andrew J.] Univ Los Andes, Dept Ciencias Biol, Inst Genet, Bogota 4976, Colombia. [Ibanez, Roberto; Sanjur, Oris I.; Bermingham, Eldredge; Crawford, Andrew J.] Smithsonian Trop Res Inst, Panama City, Panama. [Ibanez, Roberto; Crawford, Andrew J.] Circulo Herpetol Panama, Panama City, Panama. RP Crawford, AJ (reprint author), Univ Los Andes, Dept Ciencias Biol, Inst Genet, Edif M1-304,Carrera 1E 18A-10, Bogota 4976, Colombia. EM nr.pinto81@uniandes.edu.co; ibanezr@si.edu; samadrin@uniandes.edu.co; sanjuro@si.edu; bermingham@si.edu; andrew@dna.ac RI Madrinan, Santiago/A-1149-2010; OI Madrinan, Santiago/0000-0002-0807-6523; Crawford, Andrew J./0000-0003-3153-6898; Pinto-Sanchez, Nelsy Rocio/0000-0001-7561-2982 FU Colombia's Instituto Francisco Jose de Caldas for the Advancement of Science and Technology (Colciencias) [074]; Smithsonian Tropical Research Institute; Research Committee of the Faculty of Sciences at Universidad de los Andes FX This work was supported by grants from Colombia's Instituto Francisco Jose de Caldas for the Advancement of Science and Technology (Colciencias; Convenio No. 074 from 2006), an Adelante Fellowship from the Smithsonian Tropical Research Institute, and the Research Committee of the Faculty of Sciences at Universidad de los Andes. Valuable comments on the manuscript were provided by J. Daza, A. Larson and one anonymous reviewer. This research formed the basis of the masters' thesis of N.R.P.-S. presented to the Departamento de Ciencias Biologicas at the Universidad de los Andes. NR 101 TC 47 Z9 47 U1 0 U2 32 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 1055-7903 EI 1095-9513 J9 MOL PHYLOGENET EVOL JI Mol. Phylogenet. Evol. PD MAR PY 2012 VL 62 IS 3 BP 954 EP 972 DI 10.1016/j.ympev.2011.11.022 PG 19 WC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity SC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity GA 892GS UT WOS:000300275300016 PM 22178362 ER PT J AU Power, ML AF Power, Michael L. TI The human obesity epidemic, the mismatch paradigm, and our modern "captive" environment SO AMERICAN JOURNAL OF HUMAN BIOLOGY LA English DT Review ID 11-BETA-HYDROXYSTEROID DEHYDROGENASE TYPE-1; BREAST-MILK; ADIPOSE-TISSUE; CORTISOL METABOLISM; MATERNAL OBESITY; CALLITHRIX-JACCHUS; PLACENTAL WEIGHTS; LEPTIN LEVELS; BODY-MASS; IN-UTERO AB In the distant past obesity in humans was rare and likely caused by metabolic dysregulation due to genetic or disease-related pathology. External factors precluded the ability of most people to overeat or under exert. Socio-cultural obesity came about due to the rareness of obesity and its difficulty to achieve. What is rare becomes valuable and what is difficult to achieve becomes a badge of prestige. The modern human obesity epidemic would appear to represent a third class of obesity: environmental obesity. Much like the captive environments which humans construct for the captive/companion animals in our care, the modern human environment has greatly decreased the challenges of life that would restrict food intake and enforce exertion. And like us, our captive/companion animal populations are also experiencing obesity epidemics. A further concern is that maternal obesity alters maternal signaling to offspring, in utero through the placenta and after birth through breast milk, in ways that perpetuate an enhanced vulnerability to obesity. Molecules such as leptin, produced by adipose tissue and placenta, have significant developmental effects on brain areas associated with feeding behavior. Leptin and other cytokines and growth factors are found in breast milk. These molecules have positive effects on gut maturation; their effects on metabolism and brain development are unclear. Placenta and brain also are hotspots for epigenetic regulation, and epigenetic changes may play significant roles in the later vulnerability to obesity and to the development of a diverse array of diseases, including heart disease, hypertension, and noninsulin-dependent diabetes. Am. J. Hum. Biol., 2012. (C) 2012 Wiley Periodicals, Inc. C1 Smithsonian Conservat Biol Inst, Nutr Lab, Conservat Ecol Ctr, Washington, DC 20013 USA. RP Power, ML (reprint author), Smithsonian Conservat Biol Inst, Nutr Lab, Conservat Ecol Ctr, Natl Zool Pk,POB 37012,MRC 5503, Washington, DC 20013 USA. EM powerm@si.edu OI Power, Michael/0000-0002-6120-3528 FU PHS [R01 DK077639] FX Contract grant sponsor: PHS; Contract grant number: R01 DK077639. NR 56 TC 3 Z9 3 U1 0 U2 19 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1042-0533 J9 AM J HUM BIOL JI Am. J. Hum. Biol. PD MAR-APR PY 2012 VL 24 IS 2 BP 116 EP 122 DI 10.1002/ajhb.22236 PG 7 WC Anthropology; Biology SC Anthropology; Life Sciences & Biomedicine - Other Topics GA 888IQ UT WOS:000299997500004 PM 22287210 ER PT J AU Power, ML AF Power, M. L. TI Milk protein content and relative growth in early infancy in anthropoid primates SO AMERICAN JOURNAL OF HUMAN BIOLOGY LA English DT Meeting Abstract C1 [Power, M. L.] Smithsonian Conservat Biol Inst, Nutr Lab, Washington, DC USA. [Power, M. L.] Smithsonian Conservat Biol Inst, Conservat Ecol Ctr, Washington, DC USA. NR 0 TC 0 Z9 0 U1 0 U2 1 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 1042-0533 J9 AM J HUM BIOL JI Am. J. Hum. Biol. PD MAR-APR PY 2012 VL 24 IS 2 BP 240 EP 240 PG 1 WC Anthropology; Biology SC Anthropology; Life Sciences & Biomedicine - Other Topics GA 888IQ UT WOS:000299997500089 ER PT J AU Quinn, EA Power, ML AF Quinn, E. A. Power, M. L. TI Crawling, not age, predicts greater sIgA content of milk in Filipino women SO AMERICAN JOURNAL OF HUMAN BIOLOGY LA English DT Meeting Abstract C1 [Quinn, E. A.] Washington Univ, Dept Anthropol, St Louis, MO 63130 USA. [Power, M. L.] Smithsonian Conservat Biol Inst, Nutr Lab, Washington, DC USA. [Power, M. L.] Smithsonian Conservat Biol Inst, Conservat Ecol Ctr, Washington, DC USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 1042-0533 J9 AM J HUM BIOL JI Am. J. Hum. Biol. PD MAR-APR PY 2012 VL 24 IS 2 BP 240 EP 240 PG 1 WC Anthropology; Biology SC Anthropology; Life Sciences & Biomedicine - Other Topics GA 888IQ UT WOS:000299997500090 ER PT J AU Germain, RR Reudink, MW Marra, PP Boag, PT Ratcliffe, LM AF Germain, Ryan R. Reudink, Matthew W. Marra, Peter P. Boag, Peter T. Ratcliffe, Laurene M. TI Delayed maturation of multiple signals in a migratory songbird SO BEHAVIORAL ECOLOGY AND SOCIOBIOLOGY LA English DT Article DE Delayed song maturation; Delayed plumage maturation; Multiple signals; Mate choice; American redstart ID REDSTARTS SETOPHAGA-RUTICILLA; MALE AMERICAN REDSTARTS; NIGHTINGALES LUSCINIA-MEGARHYNCHOS; SEXUALLY SELECTED TRAITS; PLUMAGE MATURATION; REPRODUCTIVE SUCCESS; BREEDING-SEASON; TERRITORY QUALITY; INDIGO BUNTINGS; PASSERINE BIRDS AB Many animals use multiple signals in sexual communication, but our understanding of the interactions between multiple signals, particularly in inexperienced breeders, is limited. In birds, delayed plumage maturation (DPM) is well documented; young birds appear duller than adults, despite reaching sexual maturity. Age-related changes in song structure are also common in songbirds, though the extent to which songs of yearling males differ from those of adults (delayed song maturation, DSM) and its prevalence in species with DPM is unknown. We tested for DSM in the mate-attraction (repeat) song of a species with dramatic DPM, the American redstart (Setophaga ruticilla). Repeat song structure of territorial yearling and adult males differed significantly, based on discriminant analysis of nine non-collinear song features. Combined with previous evidence of delayed maturation in territorial (serial) song, we provide the first evidence for DSM in different song types used in different behavioral contexts during the breeding season of a migratory songbird. Within adults, variation in repeat song was associated with pairing, earlier onset of breeding, and number of offspring sired, suggesting a potential benefit for expressing more adult-like song. We found no relationship between the expression of adult-like repeat song and plumage in either age class. These results indicate that delayed maturation of repeat song in yearling redstarts is not due to a generalized delay in signal development, and suggest further work is needed to determine whether mate attraction (for both yearling and adult males) provides greater pressure to sound more "adult-like" than to look more "adult-like". C1 [Germain, Ryan R.; Reudink, Matthew W.; Boag, Peter T.; Ratcliffe, Laurene M.] Queens Univ, Dept Biol, Kingston, ON K7L 3N6, Canada. [Reudink, Matthew W.; Marra, Peter P.] Smithsonian Conservat Biol Inst, Migratory Bird Ctr, Washington, DC 20008 USA. RP Germain, RR (reprint author), Univ British Columbia, Ctr Appl Conservat Res, 2424 Main Mall, Vancouver, BC V6T 1Z4, Canada. EM r.germain@alumni.ubc.ca RI Boag, Peter/B-2907-2014 OI Boag, Peter/0000-0003-0050-2089 FU Queen's University; Natural Sciences and Engineering Research Council; National Science Foundation; Ontario Government (MTCU); American Ornithologists' Union; Society of Canadian Ornithologists; Sigma Xi; American Museum of Natural History FX We thank R. Montgomerie and T. Murphy for providing color-analysis equipment and support, C. Scott for paternity analysis, J. Foote for support in song analysis, and C. Toth, M. Osmond, and many capable assistants in the field. We thank K. Delmore, R. Robertson, P. Martin, W. Plaxton, and K. Munhall for useful discussion and helpful comments on this manuscript. Funding for this work was provided by Queen's University, Natural Sciences and Engineering Research Council, National Science Foundation, Ontario Government (MTCU), American Ornithologists' Union, Society of Canadian Ornithologists, Sigma Xi, and the American Museum of Natural History. NR 69 TC 4 Z9 4 U1 2 U2 25 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0340-5443 J9 BEHAV ECOL SOCIOBIOL JI Behav. Ecol. Sociobiol. PD MAR PY 2012 VL 66 IS 3 BP 419 EP 431 DI 10.1007/s00265-011-1288-x PG 13 WC Behavioral Sciences; Ecology; Zoology SC Behavioral Sciences; Environmental Sciences & Ecology; Zoology GA 891WU UT WOS:000300248300008 ER PT J AU Parrott, DL Brinks, JS Lhotka, JM AF Parrott, David L. Brinks, Joshua S. Lhotka, John M. TI Designing Nelder wheel plots for tree density experiments SO NEW FORESTS LA English DT Article DE Experimental design; Tree spacing; Stand density; Tree growth ID SPACING EXPERIMENTS; SYSTEMATIC DESIGNS; GROWTH; MORPHOLOGY; EUCALYPTUS; MODELS AB The Nelder (Biometrics 18:283-307, 1962) wheel design allows a researcher to test multiple tree densities in a single plot. Because spatial relationships among planted trees are fundamental to a Nelder wheel, a researcher needs a specific set of layout parameters to establish a Nelder plot. While Nelder (Biometrics 18:283-307, 1962) provides calculus-based equations for determining the required layout parameters, the presentation focuses on derivation of these equations and not their application to forestry research. Other authors have outlined the design of Nelder plots for forestry research, but have done so using trigonometry-based equations. Existence of two layout methodologies in the literature is a source of confusion. In this paper, we present a straightforward means to determine the design parameters critical to the establishment of Nelder plots used within tree density research. The layout equations presented are expressed in terms that allow applied forestry researchers to easily answer the following question. Given the number and range of tree densities I want to evaluate, what are the required Nelder wheel layout parameters? Finally, we provide a step-by-step example of the design and installation of a Nelder plot for a scenario familiar to tree density research and discuss analysis of Nelder wheel experiments. C1 [Parrott, David L.; Lhotka, John M.] Univ Kentucky, Dept Forestry, Lexington, KY 40546 USA. [Brinks, Joshua S.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. RP Lhotka, JM (reprint author), Univ Kentucky, Dept Forestry, 210 Thomas Poe Cooper Bldg, Lexington, KY 40546 USA. EM david.parrott2@gmail.com; jbrinks@gmail.com; john.lhotka@uky.edu NR 22 TC 1 Z9 3 U1 1 U2 7 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0169-4286 EI 1573-5095 J9 NEW FOREST JI New For. PD MAR PY 2012 VL 43 IS 2 BP 245 EP 254 DI 10.1007/s11056-011-9278-4 PG 10 WC Forestry SC Forestry GA 889OB UT WOS:000300081900009 ER PT J AU Shockley, FW AF Shockley, Floyd W. TI FIRST RECORDS OF MICROPSEPHODES LUNDGRENI LESCHEN AND CARLTON (COLEOPTERA: ENDOMYCHIDAE) IN ALABAMA AND TEXAS, U.S.A. SO COLEOPTERISTS BULLETIN LA English DT Editorial Material C1 Smithsonian Inst, Dept Entomol, Natl Museum Nat Hist, Washington, DC 20013 USA. RP Shockley, FW (reprint author), Smithsonian Inst, Dept Entomol, Natl Museum Nat Hist, POB 37012,MRC 165, Washington, DC 20013 USA. EM ShockleyF@si.edu NR 3 TC 0 Z9 0 U1 0 U2 1 PU COLEOPTERISTS SOC PI ATHENS PA UNIV GEORGIA, 413 BIOLOGICAL SCIENCES BUILDING, ATHENS, GA 30602-2603 USA SN 0010-065X J9 COLEOPTS BULL JI Coleopt. Bull. PD MAR PY 2012 VL 66 IS 1 BP 76 EP 78 PG 3 WC Entomology SC Entomology GA 142UE UT WOS:000318822300016 ER PT J AU Brown, DD Lapoint, S Kays, R Heidrich, W Kummeth, F Wikelski, M AF Brown, Danielle D. Lapoint, Scott Kays, Roland Heidrich, Wolfgang Kuemmeth, Franz Wikelski, Martin TI Accelerometer-Informed GPS Telemetry: Reducing the Trade-Off Between Resolution and Longevity SO WILDLIFE SOCIETY BULLETIN LA English DT Article DE accelerometry; activity; animal movement; anteater; fisher; fix success; Global Positioning System performance; location success; wildlife tracking AB Tracking animal movement using Global Positioning System (GPS) technology is an increasingly popular method for studying animal ecology, behavior, and conservation. To date, most GPS location schedules have been set at regular intervals. If intervals are too long, they undersample the details of movement paths, and if too short, they oversample resting sites and deplete the unit's battery without providing new information. We address this problem by creating a dynamic GPS schedule that is linked to the activity level of the animal via an accelerometer onboard the tracking tag. We deployed traditional and accelerometer-informed GPS tags on northern tamanduas anteater (Tamandua mexicana) in tropical forest in the Republic of Panama (2009-2010), and on fisher (Martes pennanti) in temperate forest in New York, USA (2009-2011). These species are medium-sized forest-dwellers that frequently use tree cavities, ground burrows, and thick vegetation for resting and foraging, all traits that make them particularly challenging for GPS tracking. The accelerometer-informed tags performed better than the traditional GPS tags: they attempted 73.6% more locations per day, achieved 61.7% higher location success rates, spent 28.2% less time searching for satellites, made 67.4% fewer redundant location attempts in places where animals were inactive, and ultimately provided more data for a given battery size. The resulting tracks of animal movement had high temporal resolution, revealing aspects of their behavior and ecology that would have been missed by traditional tags, especially for the fast-moving fisher. By dynamically linking the location schedule to animal movement rate, accelerometer-informed GPS tags reduce the trade-off between collecting detailed movement data and recording movement data for a longer period of time. (C) 2012 The Wildlife Society. C1 [Brown, Danielle D.] Univ Calif Davis, Anim Behav Grad Grp, Davis, CA 95616 USA. [Lapoint, Scott; Kays, Roland] New York State Museum & Sci Serv, Albany, NY 12230 USA. [Lapoint, Scott; Wikelski, Martin] Max Planck Inst Ornithol, Vogelwarte Radolfzell, D-78315 Radolfzell am Bodensee, Germany. [Kays, Roland; Wikelski, Martin] Smithsonian Trop Res Inst, Panama City, Panama. [Heidrich, Wolfgang; Kuemmeth, Franz] E Obs GmbH, D-82031 Grunwald, Germany. [Wikelski, Martin] Univ Konstanz, Chair Ornithol, D-78457 Constance, Germany. RP Brown, DD (reprint author), Middle Tennessee State Univ, Dept Biol, POB 60, Murfreesboro, TN 37132 USA. EM dabrown@mtsu.edu FU New York State Museum; Max Planck Institute for Ornithology; NSF [0756920]; Albany Pine Bush Preserve; Smithsonian Tropical Research Institute; University of California, Davis FX This project was supported by the New York State Museum; the Max Planck Institute for Ornithology; an NSF predoctoral fellowship (D. D. Brown) and research grant (no. 0756920 to R. Kays), the Albany Pine Bush Preserve; the Smithsonian Tropical Research Institute; and the University of California, Davis. We thank the Smithsonian Tropical Research Institute, New York State Museum, and Autoridad Nacional del Ambiente de Panama for administrative support. D. Brown wishes to thank R. Acosta, V. Jaramillo, F. Rodriguez, S. Escobar, J. A. Ramirez Silva, and J. Thoma's for assistance in the field. NR 38 TC 25 Z9 25 U1 4 U2 23 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1938-5463 J9 WILDLIFE SOC B JI Wildl. Soc. Bull. PD MAR PY 2012 VL 36 IS 1 BP 139 EP 146 DI 10.1002/wsb.111 PG 8 WC Biodiversity Conservation SC Biodiversity & Conservation GA V38GX UT WOS:000209333000021 ER PT J AU Harrison, BA Ruiz-Lopez, F Falero, GC Savage, HM Pecor, JE Wilkerson, RC AF Harrison, Bruce A. Ruiz-Lopez, Freddy Falero, Guillermo Calderon Savage, Harry M. Pecor, James E. Wilkerson, Richard C. TI Anopheles (Kerteszia) lepidotus (Diptera: Culicidae), not the malaria vector we thought it was: Revised male and female morphology; larva, pupa, and male genitalia characters; and molecular verification SO ZOOTAXA LA English DT Article DE Anopheles lepidotus; Anopheles pholidotus; redescription; key; morphology; ITS2; COI; malaria ID INTERNAL TRANSCRIBED SPACER; PLASMODIUM-KNOWLESI; SUBGENUS KERTESZIA; SPECIES COMPLEX; CRUZII; DNA; POPULATIONS; PHYLOGENY; SEQUENCES; AMAZON AB The name Anopheles (Kerteszia) lepidotus Zavortink, commonly used for an important malaria vector in the eastern cordillera of the Andes, is here corrected to An. pholidotus Zavortink. We discovered that An. (Ker.) specimens from Peru, and reared-associated specimens from Ecuador, had unambiguous habitus characters that matched those on the male holotype of An. lepidotus. However, the specimens do not exhibit characters of the female allotype and female paratypes of An. lepidotus, which are actually An. pholidotus. Our specimens are the first correctly associated females of An. lepidotus, which allow us to provide a new morphological interpretation for the adult habitus of this species. This finding is also corroborated by molecular data from a portion of the Cytochrome Oxidase I (COI) gene and ribosomal DNA Internal Transcribed Spacer 2 (rDNA ITS2). The pupal stage of An. lepidotus is described for the first time, and additional larval characters are also noted. Diagnostic morphological characters for the adult, pupal, and larval stages of An. pholidotus are provided to separate the two species. All stages of An. lepidotus are easily separated from other currently known species in subgenus Kerteszia and a new key to the females of An. (Kerteszia) is given. Previously published distribution, bionomics, and medical significance data are corrected and enhanced. C1 [Ruiz-Lopez, Freddy; Pecor, James E.; Wilkerson, Richard C.] Museum Support Ctr, Walter Reed Biosystemat Unit, Smithsonian Inst, Suitland, MD 20746 USA. [Savage, Harry M.] Ctr Dis Control & Prevent, Div Vector Borne Dis, Ft Collins, CO 80521 USA. [Pecor, James E.; Wilkerson, Richard C.] Walter Reed Army Inst Res, Entomol Branch, Silver Spring, MD 20910 USA. RP Wilkerson, RC (reprint author), Museum Support Ctr, Walter Reed Biosystemat Unit, Smithsonian Inst, 4210 Silver Hill Rd, Suitland, MD 20746 USA. EM skeeterdoc@gmail.com; ruizj@si.edu; calderon_entomol@hotmail.com; hms1@cdc.gov; pecorj@si.edu; wilkersonr@si.edu FU National Research Council, National Academy of Science, Washington, DC; BOSTID [MVR-PE-4-84-35]; Walter Reed Biosystematics Unit (WRBU); National Museum of Natural History; Smithsonian Institution, Washington, DC; National Institutes of Health [2R01AI054139] FX We gratefully acknowledge the National Research Council, National Academy of Science, Washington, DC, for support with BOSTID Grant No. MVR-PE-4-84-35, the Walter Reed Biosystematics Unit (WRBU), National Museum of Natural History, Smithsonian Institution, Washington, DC, National Institutes of Health grant 2R01AI054139 to Jan Conn, the Instituto Nacional de Salud, Ministerio de Salud, Lima, Peru, the Naval Medical Research Institute (NAMRID), Lima Detachment, Lima, Peru, and to Kelly Swing and the staff at the Tiputini Biodiversity Station, Universidad San Francisco de Quito, who made collections of crucial specimens for this study possible. We are very grateful to LCDR Chris H. Gardiner, for local assistance in Lima and in Junin Province. The hard field and laboratory work of Roberto Falcone and Victor Zambrano in Peru was of great value to the study. Special thanks are also due Taina Litwak for the beautiful illustrations, Judith Stoffer for the photomicrographs and their preparation for publication. We also appreciate the helpful and constructive edits and comments provided by Ralph Harbach, Anice Sallum, and Yvonne-Marie Linton. NR 59 TC 4 Z9 5 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 MAR 1 PY 2012 IS 3218 BP 1 EP 17 PG 17 WC Zoology SC Zoology GA 903LH UT WOS:000301117500001 ER PT J AU Baeza, JA Asorey, CM AF Baeza, J. Antonio Asorey, Cynthia M. TI Testing the role of male-male competition in the evolution of sexual dimorphism: a comparison between two species of porcelain crabs SO BIOLOGICAL JOURNAL OF THE LINNEAN SOCIETY LA English DT Article DE mating system; ontogenetic phase; Porcellanidae; selection; symbiosis ID ALLOPETROLISTHES-SPINIFRONS; MACROBRACHIUM-ROSENBERGII; HOST CHARACTERISTICS; AGONISTIC BEHAVIOR; PORCELLANID CRAB; SIZE DIMORPHISM; EASTERN PACIFIC; ANOLIS-LIZARDS; SELECTION; DECAPODA AB Theory predicts marked sexual dimorphism in terms of body size and body structures used as weapons (e.g. chelipeds) in gonochoric species with intense male sexual competition for receptive females and reduced or no sexual dimorphism in species where competition among males is trivial. We tested this hypothesis using a pair of closely-related species of symbiotic porcelain crabs as a model. In one species that inhabits sea anemones solitarily, competition among males for receptive females is unimportant. In a second species that dwells as dense aggregations on sea urchins, malemale competition for sexual partners is recurrent. We expected considerable sexual dimorphism in body size and weaponry in the urchin-dwelling crab and reduced sexual dimorphism in the anemone-dwelling crab. In agreement with expectations, in the urchin-dwelling crab, male body size was, on average, larger than that of females and males invested considerably more to cheliped length than females. Also supporting theoretical considerations, in the anemone-dwelling crab, sexual dimorphism in terms of body size was not detected and differences between the sexes in investment to cheliped length were minor. Interestingly, chelipeds were more developed both in males and females of the anemone-dwelling crab than in the urchin-dwelling crab as a result of the importance of these structures for monopolization of their naturally scarce anemone hosts. Another difference between the studied species was the existence of two clearly distinguishable ontogenetic phases in males of the urchin-dwelling crab but not in males of the anemone-dwelling crab. Whether the two different male morphs display different male reproductive strategies in the urchin-dwelling crab remains to be addressed. Other conditions that might additionally explain the observed differences in sexual dimorphism (e.g. female mate choice) between the studied species remain to be explored. (C) 2011 The Linnean Society of London, Biological Journal of the Linnean Society, 2012, 105, 548558. C1 [Baeza, J. Antonio] Old Dominion Univ, Dept Biol Sci, Norfolk, VA 23435 USA. [Baeza, J. Antonio] Smithsonian Marine Stn Ft Pierce, Ft Pierce, FL 34949 USA. [Baeza, J. Antonio; Asorey, Cynthia M.] Univ Catolica Norte, Dept Biol Marina, Fac Ciencias Mar, Larrondo 1281, Coquimbo, Chile. [Baeza, J. Antonio; Asorey, Cynthia M.] CEAZA, Larrondo 1281, Coquimbo, Chile. RP Baeza, JA (reprint author), Old Dominion Univ, Dept Biol Sci, Norfolk, VA 23435 USA. EM baezaa@si.edu OI Baeza, Juan Antonio/0000-0002-2573-6773 FU Smithsonian Marine Station (SMS); CEAZA; Universidad Catolica del Norte FX J.A.B. thanks the support from a Smithsonian Marine Station (SMS) Postdoctoral Fellowship. C. M. A. thanks the support from a CEAZA and Universidad Catolica del Norte Doctoral Fellowship. Bernardo Broitman facilitated the transportation of animals from the collection sites to the laboratory and Henrikas Urbonas, Emilio Figueroa, and Claudia Fernandez helped during collections. Mr Joshua Anderson kindly provided statistical support. Mrs Casey Boleman kindly reviewed the English. We appreciate the comments made by two anonymous reviewers that substantially improved the present manuscript. This is Smithsonian Marine Station at Fort Pierce Contribution No. 869. NR 59 TC 13 Z9 14 U1 3 U2 26 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0024-4066 J9 BIOL J LINN SOC JI Biol. J. Linnean Soc. PD MAR PY 2012 VL 105 IS 3 BP 548 EP 558 DI 10.1111/j.1095-8312.2011.01803.x PG 11 WC Evolutionary Biology SC Evolutionary Biology GA 884GV UT WOS:000299693800005 ER PT J AU Heinzel, P Avrett, EH AF Heinzel, P. Avrett, E. H. TI Optical-to-Radio Continua in Solar Flares SO SOLAR PHYSICS LA English DT Article DE Solar flares; Spectral continua; Diagnostics ID WHITE-LIGHT FLARES; 1982 JUNE 15; TRANSITION REGION; MODELS; CHROMOSPHERE; HYDROGEN; LINES; SUMER; BURST; GHZ AB Spectral continua observed during solar flares may contain information about both thermal and non-thermal heating mechanisms. Using two semi-empirical flare models F2 and FLA, we synthesize the thermal continua from optical to mm-radio domains and compare their intensities with quiet-Sun values computed from a recent model C7. In this way, the far-infrared and sub-mm/mm continua are studied for the first time, and we present our results as a benchmark for further modeling and for planning new observations, especially with the ALMA instrument. Finally, we demonstrate how these continua are formed and show a close correspondence between their brightness temperature and the kinetic-temperature structure of the flaring atmosphere. C1 [Heinzel, P.] Acad Sci Czech Republic, Inst Astron, CS-25165 Ondrejov, Czech Republic. [Avrett, E. H.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA USA. RP Heinzel, P (reprint author), Acad Sci Czech Republic, Inst Astron, CS-25165 Ondrejov, Czech Republic. EM pheinzel@asu.cas.cz; avrett@cfa.harvard.edu RI Heinzel, Petr/G-9014-2014 FU Grant Agency of the Czech Republic [P209/10/1680] FX The authors thank H. Hudson, G. Trottet, J.-P. Raulin, and an anonymous referee for useful comments. P.H. was the member of the Team 165 of L. Fletcher and J. Kasparova at ISSI - Bern, where the problems related to flare continua have been extensively discussed. He also acknowledges support from grant P209/10/1680 (Grant Agency of the Czech Republic) and appreciates the kind hospitality of the Center for Astrophysics, Cambridge (USA), where part of this work was done. NR 28 TC 10 Z9 10 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 MAR PY 2012 VL 277 IS 1 BP 31 EP 44 DI 10.1007/s11207-011-9823-5 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 885HT UT WOS:000299770300004 ER PT J AU Rosindell, J Jansen, PA Etienne, RS AF Rosindell, James Jansen, Patrick A. Etienne, Rampal S. TI Age structure in neutral theory resolves inconsistencies related to reproductive-size threshold SO JOURNAL OF PLANT ECOLOGY LA English DT Article DE neutral theory; age structure; sampling; DBH ID SPECIES-AREA RELATIONSHIPS; BIODIVERSITY; SPECIATION; MODEL; BIOGEOGRAPHY; LIMITATION; DISPERSAL; DIVERSITY; ABUNDANCE; FORESTS AB Neutral theory consists of a suite of models that assume ecological equivalence among individual organisms. They have been most commonly applied to tropical forest tree communities either as null models or as approximations. Neutral models typically only include reproductive adults; therefore, fitting to empirical tree community data requires defining a reproductive-size threshold, which for trees is usually set arbitrarily to a diameter at breast height (DBH) of 100 mm. The inevitable exclusion of some reproductive adults and inclusion of some saplings cause a non-random sampling bias in neutral model fits. Here, we investigate this problem and resolve it by introducing simple age structure into a neutral model. We compared the performance and sensitivity of DBH threshold of three variants of a spatially explicit neutral model: the traditional model, a model incorporating random sampling and a model with two distinct age classes-reproductive adults and saplings. In the age-structured model, saplings are offspring from adults that disperse according to a Gaussian dispersal kernel around the adults. The only extra parameter is the ratio of adults to saplings, which is not a free parameter but directly measurable. We used species-area relationships (SARs) to explore the predicted effect of saplings on the species richness at different scales in our model. We then evaluated the three model variations to find the parameters required to maintain the observed level of species richness in the 50-ha plot on Barro Colorado Island (BCI). We repeated our analysis filtering the data at different minimum tree-size thresholds in order to find the effect this threshold has on our results. Lastly, we used empirical species-individual relationships (SIRs) to test the pre-existing hypothesis that environmental filtering is the primary cause of differences between the assemblage of saplings and that of adults on BCI. Our age-structured neutral model was characterized by SARs that were insensitive to the presence of saplings at large scales and highly sensitive to them at small scales. Both models without age structure were highly sensitive to the DBH threshold chosen in a way that could not be explained based on random samplings alone. The age-structured neutral model, which allowed for non-random sampling based on life stage, was consistent with species richness observations. Our analysis of empirical SIRs did not support environmental filtering as a dominant force, but it did show evidence for other differences between age classes. Age can now be easily incorporated into future studies of neutral models whenever there is a concern that a sample is not entirely composed of reproductive adult individuals. More generally, we suggest that modeling studies using tree data subject to a minimum size threshold should consider the sensitivity of their results to that threshold. C1 [Rosindell, James] Univ Leeds, Inst Integrat & Comparat Biol, Fac Biol Sci, Leeds LS2 9JT, W Yorkshire, England. [Rosindell, James] Univ Idaho, Inst Bioinformat & Evolutionary Studies, Moscow, ID 83844 USA. [Jansen, Patrick A.] Smithsonian Trop Res Inst, Ctr Trop Forest Sci, Balboa, Ancon, Panama. [Jansen, Patrick A.] Wageningen Univ, Ctr Ecosyst Studies, NL-6700 AA Wageningen, Netherlands. [Jansen, Patrick A.; Etienne, Rampal S.] Univ Groningen, Ctr Ecol & Evolutionary Studies, NL-9700 CC Groningen, Netherlands. RP Rosindell, J (reprint author), Univ Leeds, Inst Integrat & Comparat Biol, Fac Biol Sci, Leeds LS2 9JT, W Yorkshire, England. EM james@rosindell.org RI Etienne, Rampal/F-5835-2012; Jansen, Patrick/G-2545-2015 OI Etienne, Rampal/0000-0003-2142-7612; Jansen, Patrick/0000-0002-4660-0314 FU Engineering and Physical Sciences Research Council [EP/F043112/1]; Netherlands Organization for Scientific Research (NWO-ALW) [864-07-007, 863-07-008]; National Science Foundation [DEB-0640386, DEB-0425651, DEB-0346488, DEB-0129874, DEB-00753102, DEB-9909347, DEB-9615226, DEB-9405933, DEB-9221033, DEB-9100058, DEB-8906869, DEB-8605042, DEB-8206992, DEB-7922197]; Center for Tropical Forest Science; Smithsonian Tropical Research Institute; John D. and Catherine T. MacArthur Foundation; Mellon Foundation; Small World Institute FX Engineering and Physical Sciences Research Council overseas postdoctoral research fellowship at the life sciences interface (EP/F043112/1 to J.R.); the Netherlands Organization for Scientific Research (NWO-ALW 864-07-007 to R. S. E., NWO-ALW 863-07-008 to P.A.J.).; We thank Stephen Cornell, Dominique Gravel, Bill Kunin, Alan Mckane and Steve Sait for very helpful comments on the manuscript. The BCI forest dynamics research project was made possible by National Science Foundation grants to Stephen P. Hubbell: DEB-0640386, DEB-0425651, DEB-0346488, DEB-0129874, DEB-00753102, DEB-9909347, DEB-9615226, DEB-9615226, DEB-9405933, DEB-9221033, DEB-9100058, DEB-8906869, DEB-8605042, DEB-8206992, DEB-7922197, support from the Center for Tropical Forest Science, the Smithsonian Tropical Research Institute, the John D. and Catherine T. MacArthur Foundation, the Mellon Foundation, the Small World Institute Fund and numerous private individuals and through the hard work of > 100 people from 10 countries over the past two decades. The plot project is part of the Center for Tropical Forest Science, a global network of large-scale demographic tree plots. NR 31 TC 1 Z9 1 U1 2 U2 12 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 1752-9921 J9 J PLANT ECOL-UK JI J. Plant Ecol. PD MAR PY 2012 VL 5 IS 1 SI SI BP 64 EP 71 DI 10.1093/jpe/rtr034 PG 8 WC Plant Sciences; Ecology SC Plant Sciences; Environmental Sciences & Ecology GA 876JK UT WOS:000299103600007 ER PT J AU Zhang, DY Zhang, BY Lin, K Jiang, XH Tao, Y Hubbell, S He, FL Ostling, A AF Zhang, Da-Yong Zhang, Bo-Yu Lin, Kui Jiang, Xinhua Tao, Yi Hubbell, Stephen He, Fangliang Ostling, Annette TI Demographic trade-offs determine species abundance and diversity SO JOURNAL OF PLANT ECOLOGY LA English DT Article DE birth-death trade-off; ecological drift; fitness equivalence; neutral theory; species coexistence ID NEUTRAL BIODIVERSITY THEORY; ZERO-SUM ASSUMPTION; COMMUNITY ECOLOGY; STOCHASTIC-THEORY; UNIFIED THEORY; RAIN-FORESTS; CORAL-REEFS; DRIFT MODEL; NUMBERS ADD; NICHE AB Much recent theory has focused on the role of neutral processes in assembling communities, but the basic assumption that all species are demographically identical has found little empirical support. Here, we show that the framework of the current neutral theory can easily be generalized to incorporate species differences so long as fitness equivalence among individuals is maintained through trade-offs between birth and death. Our theory development is based on a careful reformulation of the Moran model of metacommunity dynamics in terms of a non-linear one-step stochastic process, which is described by a master equation. We demonstrate how fitness equalization through demographic trade-offs can generate significant macroecological diversity patterns, leading to a very different interpretation of the relation between Fisher's alpha and Hubbell's fundamental biodiversity number. Our model shows that equal fitness (not equal demographics) significantly promotes species diversity through strong selective sieving of community membership against high-mortality species, resulting in a positive association between species abundance and per capita death rate. An important implication of demographic trade-off is that it can partly explain the excessively high speciation rates predicted by the neutral theory of the stronger symmetry. Fitness equalization through demographic trade-offs generalizes neutral theory by considering heterospecific demographic difference, thus representing a significant step toward integrating the neutral and niche paradigms of biodiversity. C1 [Zhang, Da-Yong] Beijing Normal Univ, Coll Life Sci, State Key Lab Earth Surface Proc & Resource Ecol, Beijing 100875, Peoples R China. [Zhang, Bo-Yu] Beijing Normal Univ, Sch Math Sci, Beijing 100875, Peoples R China. [Zhang, Bo-Yu; Tao, Yi] Chinese Acad Sci, Inst Zool, Key Lab Anim Ecol & Conservat Biol, Beijing 100101, Peoples R China. [Hubbell, Stephen] Univ Calif Los Angeles, Dept Ecol & Evolutionary Biol, Los Angeles, CA 90095 USA. [Hubbell, Stephen] Smithsonian Trop Res Inst, Ctr Trop Forest Sci, Panama City, Panama. [He, Fangliang] Univ Alberta, Dept Renewable Resources, Edmonton, AB T6G 2H1, Canada. [Ostling, Annette] Univ Michigan, Dept Ecol & Evolutionary Biol, Ann Arbor, MI 48109 USA. RP Zhang, DY (reprint author), Beijing Normal Univ, Coll Life Sci, State Key Lab Earth Surface Proc & Resource Ecol, Beijing 100875, Peoples R China. EM zhangdy@bnu.edu.cn RI Zhang, Da-Yong/B-3078-2011; Lin, Kui/P-4492-2015 OI Zhang, Da-Yong/0000-0003-1056-8735; Lin, Kui/0000-0002-5993-1972 FU National Natural Science Foundation of China [31030014, 31121003]; State Key Basic Research and Development Plan [2007CB106800, 2010CB434800]; Natural Sciences and Engineering Research Council (Canada); University of Alberta International FX National Natural Science Foundation of China (31030014, 31121003); State Key Basic Research and Development Plan (2007CB106800 and 2010CB434800); Natural Sciences and Engineering Research Council (Canada); University of Alberta International (the China-UofA Joint Research Lab program). NR 45 TC 8 Z9 8 U1 2 U2 40 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 1752-9921 J9 J PLANT ECOL JI J. Plant Ecol. PD MAR PY 2012 VL 5 IS 1 SI SI BP 82 EP 88 DI 10.1093/jpe/rtr039 PG 7 WC Plant Sciences; Ecology SC Plant Sciences; Environmental Sciences & Ecology GA 876JK UT WOS:000299103600009 ER PT J AU Vari, RP Hadiaty, RK AF Vari, Richard P. Hadiaty, Renny Kurnia TI THE ENDEMIC SULAWESI FISH GENUS LAGUSIA (TELEOSTEI: TERAPONTIDAE) SO RAFFLES BULLETIN OF ZOOLOGY LA English DT Article DE Datnia; Sulawesi; life history; redescription AB Lagusia micracanthus, originally described from three specimens collected in a river near Lagusi in southern Sulawesi, is redescribed in detail based on an extensive series of specimens ranging from small juveniles through adults, and its phylogenetic position is reevaluated. Information on life colouration, habitat, and ontogenetic transitions in dark pigmentation in small juveniles through adults is provided for the first time. Females of the species have ripe ovaries with large numbers of well-developed eggs by at least 56 mm SL and the species thus matures at one of the, if not the, smallest body sizes in the Terapontidae. C1 [Vari, Richard P.] Natl Museum Nat Hist, Div Fishes Smithsonian Inst, Washington, DC 20013 USA. [Hadiaty, Renny Kurnia] Indonesian Inst Sci LIPI, Biol Res Ctr, Div Zool, MZB,Ichthyol Lab, Cibinong 16911, Indonesia. RP Vari, RP (reprint author), Natl Museum Nat Hist, Div Fishes Smithsonian Inst, POB 37012,WG-14,MRC 159, Washington, DC 20013 USA. EM varir@si.edu; renny_hadiaty@yahoo.com FU Division of Fishes, National Museum of Natural History of the Smithsonian Institution FX The specimens that served as the basis for this paper were collected during the Research Center for Biology Karst Project in 2006 and 2007 and by the International Expedition of South and South East Sulawesi lead by Dr. Louis Deharveng. We thank the karst team of the Research Center for Biology led by Prof. Dr. Yayuk R Suhardjono, Ir. Ristiyanti R Marwoto MSi and other team members for their continued collaboration during the last five years, Thanks are due to the head and staffs of Bantimurung-Bulusaraung National Park for permission to collect and assistance during field trips. Abdul Mun'im, Harun and Rafi assisted in the field. Research associated with the project was support by the Herbert R. and Evelyn Axelrod Chair in Systematic Ichthyology in the Division of Fishes, National Museum of Natural History of the Smithsonian Institution. Fig. 1 was prepared by T. Britt Griswold and Figs. 2-4. by RKH. NR 15 TC 1 Z9 2 U1 0 U2 2 PU NATL UNIV SINGAPORE, SCHOOL BIOLOGICAL SCIENCES PI SINGAPORE PA DEPT ZOOLOGY, KENT RIDGE, SINGAPORE 0511, SINGAPORE SN 0217-2445 J9 RAFFLES B ZOOL JI Raffles Bull. Zool. PD FEB 29 PY 2012 VL 60 IS 1 BP 157 EP 162 PG 6 WC Zoology SC Zoology GA 908TU UT WOS:000301516200015 ER PT J AU Ferraris, CJ Vari, RP AF Ferraris, Carl J., Jr. Vari, Richard P. TI Review of the African catfish genus Andersonia (Teleostei: Siluriformes) SO ZOOTAXA LA English DT Article DE Amphiliidae; Doumeinae; Nilo-Sudan Bioregion ID AMPHILIIDAE; FISHES; NILE AB Fishes of the catfish genus Andersonia (Amphiliidae, Doumeinae) are distributed widely across the northern sub-Saharan portion of Africa that is called the Nilo-Sudan Bioregion. Recent literature indicated that either one or two species of Andersonia occur in the four drainage basins (upper Niger, upper Nile, Omo, and Lake Chad) in which the genus has been found. Our study failed to find any differences in the samples from those basins, as we therefore treat them as populations of a single species, A. leptura, which is redescribed based on extensive series of specimens from across its range. The genus Andersonia is retained as valid at this time, based on the lack of clear evidence of the phylogenetic position of A. leptura within the Doumeinae. However, a broader sampling of taxa, especially among species currently placed in the genus Phractura, may require a change to that assignment. C1 [Vari, Richard P.] Natl Museum Nat Hist, Smithsonian Inst, Div Fishes, Washington, DC 20013 USA. RP Ferraris, CJ (reprint author), 2944 NE Couch St, Portland, OR 97232 USA. EM carlferraris@comcast.net; varir@si.edu FU Herbert R. and Evelyn Axelrod Chair in Systematic Ichthyology, in the Division of Fishes, National Museum of Natural History of the Smithsonian Institution FX Support for this project was provided by the Herbert R. and Evelyn Axelrod Chair in Systematic Ichthyology, in the Division of Fishes, National Museum of Natural History of the Smithsonian Institution. We thank O. Crimmen and J. Maclaine (BMNH), D. Catania (CAS), J. Friel (CU), R. Causse (MNHN), S. Kullander (NRM), H. Wilkens (ZMH) and D. Neumann (ZSM) for the loan of specimens, and J. Friel for help in obtaining needed literature. Radiographs of specimens and other assistance during the study were provided by S. Raredon (NMNH). Figure 1 was prepared by T. Griswold. Figure 2 was prepared with the assistance of D. Cole and S. Raredon (NMNH). This manuscript was improved by careful readings by A. Thomson and an anonymous reviewer. NR 49 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 FEB 28 PY 2012 IS 3210 BP 39 EP 49 PG 11 WC Zoology SC Zoology GA 899UP UT WOS:000300842200003 ER PT J AU Oda, H Machida, M Nakamura, KE Matsumoto, R Narayan, R AF Oda, Hiroshi Machida, Mami Nakamura, Kenji E. Matsumoto, Ryoji Narayan, Ramesh TI Global Structure of Optically Thin, Magnetically Supported, Two-Temperature, Black Hole Accretion Disks SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN LA English DT Article DE accretion, accretion disks; black hole physics; magnetic fields; radiation mechanisms: non-thermal ID ADVECTION-DOMINATED ACCRETION; X-RAY BINARIES; SELF-SIMILAR SOLUTION; CYGNUS X-1; THERMAL EQUILIBRIA; MAGNETOHYDRODYNAMIC SIMULATIONS; SPECTRAL TRANSITIONS; GAS-PRESSURE; HARD STATE; FLOWS AB We present global solutions of optically thin, two-temperature black hole accretion disks incorporating magnetic fields. We assume that the (omega) over bar phi-component of the Maxwell stress is proportional to the total pressure, and prescribe the radial dependence of the magnetic flux advection rate in order to complete the set of basic equations. We obtained magnetically supported (low-beta) disk solutions, whose luminosity exceeds the maximum luminosity for an advection-dominated accretion flow (ADAF), L greater than or similar to 0.4 alpha L-2(Edd), where L-Edd is the Eddington luminosity. The accretion flow is composed of the outer ADAF, a luminous hot accretion flow (LHAF) inside the transition layer from the outer ADAF to the low-beta disk, the low-beta disk, and the inner ADAF. The low-beta disk region becomes wider as the mass-accretion rate increases further. In the low-beta disk, the magnetic heating balances the radiative cooling, and the electron temperature decreases from similar to 10(9.5) K to similar to 10(8) K as the luminosity increases. These results are consistent with the anti-correlation between the energy cutoff in X-ray spectra (hence the electron temperature) and the luminosity when L greater than or similar to 0.1 L-Edd, observed in the bright/hard state during the bright hard-to-soft transitions of transient outbursts in galactic black hole candidates. C1 [Oda, Hiroshi] Chinese Acad Sci, Shanghai Astron Observ, Shanghai 200030, Peoples R China. [Machida, Mami] Kyushu Univ, Dept Phys, Fac Sci, Higashi Ku, Fukuoka 8128581, Japan. [Nakamura, Kenji E.] Kyushu Sangyo Univ, Fac Engn, Dept Mech Engn, Higashi Ku, Fukuoka 8138503, Japan. [Matsumoto, Ryoji] Chiba Univ, Grad Sch Sci, Dept Phys, Inage Ku, Chiba 2638522, Japan. [Narayan, Ramesh] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Oda, H (reprint author), Chinese Acad Sci, Shanghai Astron Observ, 80 Nandan Rd, Shanghai 200030, Peoples R China. EM hoda@shoo.ac.cn OI Narayan, Ramesh/0000-0002-1919-2730 FU Ministry of Education, Culture, Sports, Science and Technology [20340040]; Natural Science Foundation of China [10833002, 10821302, 10825314, 1105110416]; National Basic Research Program of China (973 Program) [2009CB824800]; [20.1842] FX We would like to thank Feng Yuan for helpful discussions and comments. This work was supported in part by the Grant-in-Aid for Science Research of the Ministry of Education, Culture, Sports, Science and Technology (R.M.: 20340040), Grant-in-Aid for JSPS Fellows (20.1842), the Natural Science Foundation of China (grant 10833002, 10821302, 10825314, and 1105110416), and the National Basic Research Program of China (973 Program 2009CB824800). NR 61 TC 10 Z9 10 U1 0 U2 1 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0004-6264 EI 2053-051X J9 PUBL ASTRON SOC JPN JI Publ. Astron. Soc. Jpn. PD FEB 25 PY 2012 VL 64 IS 1 AR 15 DI 10.1093/pasj/64.1.15 PG 21 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 905WS UT WOS:000301307500015 ER PT J AU Parrish, MA AF Parrish, Mary A. TI Charles R. Knight The Artist Who Saw Through Time SO SCIENCE LA English DT Book Review C1 [Parrish, Mary A.] Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20013 USA. RP Parrish, MA (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20013 USA. EM parrishm@si.edu NR 1 TC 0 Z9 0 U1 0 U2 1 PU AMER ASSOC ADVANCEMENT SCIENCE PI WASHINGTON PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA SN 0036-8075 J9 SCIENCE JI Science PD FEB 24 PY 2012 VL 335 IS 6071 BP 921 EP 921 DI 10.1126/science.1220073 PG 1 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 900ZQ UT WOS:000300931800028 ER PT J AU Secord, R Bloch, JI Chester, SGB Boyer, DM Wood, AR Wing, SL Kraus, MJ McInerney, FA Krigbaum, J AF Secord, Ross Bloch, Jonathan I. Chester, Stephen G. B. Boyer, Doug M. Wood, Aaron R. Wing, Scott L. Kraus, Mary J. McInerney, Francesca A. Krigbaum, John TI Evolution of the Earliest Horses Driven by Climate Change in the Paleocene-Eocene Thermal Maximum SO SCIENCE LA English DT Article ID ISOTOPE FRACTIONATION; STABLE-ISOTOPES; BERGMANNS RULE; BIGHORN BASIN; BODY-SIZE; CARBON; MAMMALS; ENVIRONMENT; BOUNDARY; FUTURE AB Body size plays a critical role in mammalian ecology and physiology. Previous research has shown that many mammals became smaller during the Paleocene-Eocene Thermal Maximum (PETM), but the timing and magnitude of that change relative to climate change have been unclear. A high-resolution record of continental climate and equid body size change shows a directional size decrease of similar to 30% over the first similar to 130,000 years of the PETM, followed by a similar to 76% increase in the recovery phase of the PETM. These size changes are negatively correlated with temperature inferred from oxygen isotopes in mammal teeth and were probably driven by shifts in temperature and possibly high atmospheric CO2 concentrations. These findings could be important for understanding mammalian evolutionary responses to future global warming. C1 [Secord, Ross] Univ Nebraska, Dept Earth & Atmospher Sci, Lincoln, NE 68588 USA. [Secord, Ross; Bloch, Jonathan I.; Wood, Aaron R.] Univ Florida, Florida Museum Nat Hist, Gainesville, FL 32611 USA. [Chester, Stephen G. B.] Yale Univ, Dept Anthropol, New Haven, CT 06520 USA. [Boyer, Doug M.] CUNY Brooklyn Coll, Dept Anthropol & Archaeol, Brooklyn, NY 11210 USA. [Wood, Aaron R.] S Dakota Sch Mines & Technol, Dept Geol & Geol Engn, Rapid City, SD 57701 USA. [Wing, Scott L.] Smithsonian Museum Nat Hist, Dept Paleobiol, Washington, DC 20560 USA. [Kraus, Mary J.] Univ Colorado, Dept Geol Sci, Boulder, CO 80309 USA. [McInerney, Francesca A.] Northwestern Univ, Dept Earth & Planetary Sci, Evanston, IL 60208 USA. [Krigbaum, John] Univ Florida, Dept Anthropol, Gainesville, FL 32611 USA. RP Secord, R (reprint author), Univ Nebraska, Dept Earth & Atmospher Sci, Lincoln, NE 68588 USA. EM rsecord2@unl.edu RI Kraus, Mary/C-3323-2008; McInerney, Francesca/B-7894-2009; OI Kraus, Mary/0000-0002-1721-2566; McInerney, Francesca/0000-0002-2020-6650; Bloch, Jonathan/0000-0003-1484-6931; Wing, Scott/0000-0002-2954-8905 FU NSF [EAR-0640076, EAR-0719941, EAR-0717892, EAR-0718740, EAR-0720268] FX We thank T. Bown, P. Gingerich, B. MacFadden, K. Rose, E. Sargis, and S. Strait for helpful discussions and advice; J. Curtis, B. Tucker, and A. Baczynski for help with isotope lab work; J. Bourque and A. Hastings for specimen preparation; and P. Koch and two anonymous reviewers for helpful comments. Supported by NSF grants EAR-0640076 (J.I.B., J.K., R.S.), EAR-0719941 (J.I.B.), EAR-0717892 (S.L.W.), EAR-0718740 (M.J.K.), and EAR-0720268 (F.A.M.). Data used in this paper are available in the SOM. NR 30 TC 48 Z9 51 U1 10 U2 193 PU AMER ASSOC ADVANCEMENT SCIENCE PI WASHINGTON PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA SN 0036-8075 J9 SCIENCE JI Science PD FEB 24 PY 2012 VL 335 IS 6071 BP 959 EP 962 DI 10.1126/science.1213859 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 900ZQ UT WOS:000300931800044 PM 22363006 ER PT J AU He, FL Hubbell, SP AF He, Fangliang Hubbell, Stephen P. TI Extinction and climate change He and Hubbell reply SO NATURE LA English DT Letter C1 [He, Fangliang] Sun Yat Sen Univ, Sch Life Sci, State Key Lab Biocontrol, Guangzhou 510275, Guangdong, Peoples R China. [He, Fangliang] Sun Yat Sen Univ, Sch Life Sci, SYSU Alberta Joint Lab Biodivers Conservat, Guangzhou 510275, Guangdong, Peoples R China. [He, Fangliang] Univ Alberta, Dept Renewable Resources, Edmonton, AB T6G 2H1, Canada. [Hubbell, Stephen P.] Univ Calif Los Angeles, Dept Ecol & Evolutionary Biol, Los Angeles, CA 90095 USA. [Hubbell, Stephen P.] Smithsonian Trop Res Inst, Ctr Trop Forest Sci, Unit 0948, Panama City, Panama. RP He, FL (reprint author), Sun Yat Sen Univ, Sch Life Sci, State Key Lab Biocontrol, Guangzhou 510275, Guangdong, Peoples R China. EM fhe@ualberta.ca NR 5 TC 5 Z9 5 U1 5 U2 50 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 0028-0836 J9 NATURE JI Nature PD FEB 23 PY 2012 VL 482 IS 7386 BP E5 EP E6 DI 10.1038/nature10859 PG 2 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 898VM UT WOS:000300770500003 ER PT J AU Fitzgerald, EMG AF Fitzgerald, Erich M. G. TI Archaeocete-like jaws in a baleen whale SO BIOLOGY LETTERS LA English DT Article DE Cetacea; Mysticeti; Mammalodontidae; evolution; Australia; Oligocene ID TOOTHED MYSTICETE; EVOLUTION; AUSTRALIA; MORPHOLOGY; CETACEANS; OLIGOCENE; ANATOMY; HEAD AB The titanic baleen whales (Cetacea, Mysticeti) have a bizarre skull morphology, including an elastic mandibular symphysis, which permits dynamic oral cavity expansion during bulk feeding. How this key innovation evolved from the sutured symphysis of archaeocetes has remained unclear. Now, mandibles of the Oligocene toothed mysticete Janjucetus hunderi show that basal mysticetes had an archaeocete-like sutured symphysis. This archaic morphology was paired with a wide rostrum typical of later-diverging baleen whales. This demonstrates that increased oral capacity via rostral widening preceded the evolution of mandibular innovations for filter feeding. Thus, the initial evolution of the mysticetes' unique cranial form and huge mouths was perhaps not linked to filtering plankton, but to enhancing suction feeding on individual prey. C1 [Fitzgerald, Erich M. G.] Museum Victoria, Melbourne, Vic 3001, Australia. [Fitzgerald, Erich M. G.] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA. RP Fitzgerald, EMG (reprint author), Museum Victoria, GPO Box 666, Melbourne, Vic 3001, Australia. EM efitzgerald@museum.vic.gov.au FU Harold Mitchell Foundation; Museum Victoria; Smithsonian Institution FX I thank R. Benson, T. Holland, F. Marx, J. Mead and T. Rich for comments; D. Bohaska, B. Crichton, W. Longmore, R. O'Brien and C. Potter for access to collections; Museum Victoria Preparation staff for casting; T. Demere for the photograph in figure 2c; three anonymous referees and the editor for improvements to the manuscript; and C. Buell for permission to reproduce his artwork. This study was supported by the Harold Mitchell Foundation, Museum Victoria, and the Smithsonian Institution. NR 12 TC 16 Z9 16 U1 1 U2 32 PU ROYAL SOC PI LONDON PA 6-9 CARLTON HOUSE TERRACE, LONDON SW1Y 5AG, ENGLAND SN 1744-9561 J9 BIOL LETTERS JI Biol. Lett. PD FEB 23 PY 2012 VL 8 IS 1 BP 94 EP 96 DI 10.1098/rsbl.2011.0690 PG 3 WC Biology; Ecology; Evolutionary Biology SC Life Sciences & Biomedicine - Other Topics; Environmental Sciences & Ecology; Evolutionary Biology GA 879IF UT WOS:000299322200028 PM 21849306 ER PT J AU Wagner, PJ AF Wagner, Peter J. TI Modelling rate distributions using character compatibility: implications for morphological evolution among fossil invertebrates SO BIOLOGY LETTERS LA English DT Article DE character evolution; compatibility; lognormal distribution; gamma distribution; information theory ID LIKELIHOOD APPROACH; DNA-SEQUENCES; PHYLOGENY; SELECTION AB Rate distributions are important considerations when testing hypotheses aboutmorphological evolution or phylogeny. They also have implications about general processes underlying character evolution. Molecular systematists often assume that rates are Poisson processes with gamma distributions. However, morphological change is the product of multiple probabilistic processes and should theoretically be affected by hierarchical integration of characters. Both factors predict lognormal rate distributions. Here, a simple inverse modelling approach assesses the best single-rate, gamma and lognormal models given observed character compatibility for 115 invertebrate groups. Tests reject the single-rate model for nearly all cases. Moreover, the lognormal outperforms the gamma for character change rates and (especially) state derivation rates. The latter in particular is consistent with integration affecting morphological character evolution. C1 Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20013 USA. RP Wagner, PJ (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20013 USA. EM wagnerpj@si.edu RI Wagner, Peter/A-5514-2009 OI Wagner, Peter/0000-0002-9083-9787 NR 22 TC 20 Z9 20 U1 1 U2 3 PU ROYAL SOC PI LONDON PA 6-9 CARLTON HOUSE TERRACE, LONDON SW1Y 5AG, ENGLAND SN 1744-9561 J9 BIOL LETTERS JI Biol. Lett. PD FEB 23 PY 2012 VL 8 IS 1 BP 143 EP 146 DI 10.1098/rsbl.2011.0523 PG 4 WC Biology; Ecology; Evolutionary Biology SC Life Sciences & Biomedicine - Other Topics; Environmental Sciences & Ecology; Evolutionary Biology GA 879IF UT WOS:000299322200041 PM 21795266 ER PT J AU Bacon, CD McKenna, MJ Simmons, MP Wagner, WL AF Bacon, Christine D. McKenna, Miles J. Simmons, Mark P. Wagner, Warren L. TI Evaluating multiple criteria for species delimitation: an empirical example using Hawaiian palms (Arecaceae: Pritchardia) SO BMC EVOLUTIONARY BIOLOGY LA English DT Article DE Hawaii; Hybridization; Lineage sorting; Microsatellite; Pritchardia; Radiation ID POPULATION-STRUCTURE; PHYLOGENETIC NETWORKS; SILVERSWORD ALLIANCE; MAXIMUM-LIKELIHOOD; ADAPTIVE RADIATION; GENETIC-VARIATION; TREE ESTIMATION; DNA-SEQUENCES; ORIGIN; INFERENCE AB Background: Robust species delimitations are fundamental for conservation, evolutionary, and systematic studies, but they can be difficult to estimate, particularly in rapid and recent radiations. The consensus that species concepts aim to identify evolutionarily distinct lineages is clear, but the criteria used to distinguish evolutionary lineages differ based on the perceived importance of the various characteristics of evolving populations. We examined three different species-delimitation criteria (monophyly, absence of genetic intermediates, and diagnosability) to determine whether currently recognized species of Hawaiian Pritchardia are distinct lineages. Results: Data from plastid and nuclear genes, microsatellite loci, and morphological characters resulted in various levels of lineage subdivision that were likely caused by differing evolutionary rates between data sources. Additionally, taxonomic entities may be confounded because of the effects of incomplete lineage sorting and/or gene flow. A coalescent species tree was largely congruent with the simultaneous analysis, consistent with the idea that incomplete lineage sorting did not mislead our results. Furthermore, gene flow among populations of sympatric lineages likely explains the admixture and lack of resolution between those groups. Conclusions: Delimiting Hawaiian Pritchardia species remains difficult but the ability to understand the influence of the evolutionary processes of incomplete lineage sorting and hybridization allow for mechanisms driving species diversity to be inferred. These processes likely extend to speciation in other Hawaiian angiosperm groups and the biota in general and must be explicitly accounted for in species delimitation. C1 [Bacon, Christine D.; McKenna, Miles J.; Simmons, Mark P.] Colorado State Univ, Dept Biol, Ft Collins, CO 80523 USA. [Wagner, Warren L.] Smithsonian Inst, Dept Bot, Washington, DC 20013 USA. [Bacon, Christine D.] Smithsonian Trop Res, Balboa, Ancon, Panama. RP Bacon, CD (reprint author), Colorado State Univ, Dept Biol, Ft Collins, CO 80523 USA. EM christinedbacon@gmail.edu RI Simmons, Mark/F-7157-2013 OI Simmons, Mark/0000-0003-3896-4633 FU National Tropical Botanical Garden McBryde Graduate Student Fellowship; NSF-DDIG [DEB-1010731]; Smithsonian Pre-Doctoral Fellowship; Montgomery Botanical Center Research Associateship; Hunt Institute; Bruno Klinger Memorial Scholarship FX The authors thank Ane Bakutis, Susan Ching, Don Hodel, Leland Miyano, Hank Oppenheimer, Steve Perlman, Geovanni Romero, Natalia Tangalin, Clay Trauernicht, Dick Watling, and Ken Wood for assistance with fieldwork; Jean-Yves Meyer and Lauren Weisenberger for DNA samples; Don Hodel and David Lorence for insightful feedback and discussions; Don Hodel for the use of the Pritchardia hillebrandii image; and Gabriel Johnson (Smithsonian) and Arwen Milroy (Colorado State University) for lab assistance. This research was supported by a National Tropical Botanical Garden McBryde Graduate Student Fellowship, an NSF-DDIG (DEB-1010731) award, a Smithsonian Pre-Doctoral Fellowship, a Montgomery Botanical Center Research Associateship, the Hunt Institute Lawrence Memorial Award, and the Bruno Klinger Memorial Scholarship to C.D.B. NR 115 TC 16 Z9 17 U1 3 U2 35 PU BIOMED CENTRAL LTD PI LONDON PA 236 GRAYS INN RD, FLOOR 6, LONDON WC1X 8HL, ENGLAND SN 1471-2148 J9 BMC EVOL BIOL JI BMC Evol. Biol. PD FEB 22 PY 2012 VL 12 AR 23 DI 10.1186/1471-2148-12-23 PG 17 WC Evolutionary Biology; Genetics & Heredity SC Evolutionary Biology; Genetics & Heredity GA 945IJ UT WOS:000304266000001 PM 22353848 ER PT J AU Finkbeiner, DP Galli, S Lin, T Slatyer, TR AF Finkbeiner, Douglas P. Galli, Silvia Lin, Tongyan Slatyer, Tracy R. TI Searching for dark matter in the CMB: A compact parametrization of energy injection from new physics SO PHYSICAL REVIEW D LA English DT Article ID PROBE WMAP OBSERVATIONS; POWER SPECTRUM; DATA SET; MICROWAVE; COSMOLOGY; TELESCOPE; MAPS AB High-precision measurements of the temperature and polarization anisotropies of the cosmic microwave background radiation have been employed to set robust constraints on dark matter annihilation during recombination. In this work we improve and generalize these constraints to apply to energy deposition during the recombination era with arbitrary redshift dependence. Our approach also provides more rigorous and model-independent bounds on dark matter annihilation and decay scenarios. We employ principal component analysis to identify a basis of weighting functions for the energy deposition. The coefficients of these weighting functions parameterize any energy deposition model and can be constrained directly by experiment. For generic energy deposition histories that are currently allowed by WMAP 7 data, up to 3 principal component coefficients are measurable by Planck and up to 5 coefficients are measurable by an ideal cosmic variance limited experiment. For WIMP dark matter, our analysis demonstrates that the effect on the CMB is described well by a single (normalization) parameter and a universal redshift dependence for the energy deposition history. We give WMAP 7 constraints on both generic energy deposition histories and the universal WIMP case. C1 [Finkbeiner, Douglas P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Finkbeiner, Douglas P.; Lin, Tongyan] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. [Galli, Silvia] Univ Paris Diderot, Lab Astroparticule & Cosmol APC, F-75205 Paris 13, France. [Galli, Silvia] Univ Roma La Sapienza, Dept Phys, I-00185 Rome, Italy. [Galli, Silvia] Univ Roma La Sapienza, INFN, I-00185 Rome, Italy. [Slatyer, Tracy R.] Inst Adv Study, Sch Nat Sci, Princeton, NJ 08540 USA. RP Finkbeiner, DP (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM dfinkbeiner@cfa.harvard.edu; galli@apc.univ-paris7.fr; tongyan@physics.harvard.edu; tslatyer@ias.edu FU NASA [NNX10AD85G]; NSF [NSF AST-0807444]; DOE [DE-FG02-90ER40542] FX We wish to acknowledge helpful conversations with Jens Chluba, Joanna Dunkley, Fabio Iocco, Eric Linder, Alessandro Melchiorri, Nikhil Padmanabhan and Joshua Ruderman. We are grateful to Antony Lewis for his advice on increasing the numerical accuracy of CAMB. DPF and TL are partially supported by NASA Theory grant NNX10AD85G. T. R. S is supported by the NSF under grant NSF AST-0807444 and the DOE under grant DE-FG02-90ER40542. This research made use of the NASA Astrophysics Data System (ADS) and the IDL Astronomy User's Library at Goddard.13 NR 60 TC 75 Z9 75 U1 1 U2 2 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 2470-0010 EI 2470-0029 J9 PHYS REV D JI Phys. Rev. D PD FEB 22 PY 2012 VL 85 IS 4 AR 043522 DI 10.1103/PhysRevD.85.043522 PG 28 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA 896MQ UT WOS:000300571500004 ER PT J AU Duda, TF Terbio, M Chen, G Phillips, S Olenzek, AM Chang, D Morris, DW AF Duda, Thomas F., Jr. Terbio, Marielle Chen, Gang Phillips, Semoya Olenzek, Amy M. Chang, Dan Morris, David W. TI Patterns of population structure and historical demography of Conus species in the tropical Pacific SO AMERICAN MALACOLOGICAL BULLETIN LA English DT Article; Proceedings Paper CT Symposium on Molluscan Biogeography - Perspectives from the Pacific Ocean/Joint Annual Meeting of the Western-Society-of-Malacologists/76th Annual Meeting of the American-Malacological-Society CY JUN 29, 2010 CL San Diego, CA SP Amer Malacolog Soc, Western Soc Malacolog DE Conidae; phylogeography; genetic differentiation; population expansion; cytochrome oxidase subunit 1 ID INDO-WEST PACIFIC; HIGH-DISPERSAL STARFISH; CORAL-REEF FISH; GENETIC-STRUCTURE; MITOCHONDRIAL-DNA; MARINE GASTROPOD; EVOLUTIONARY HISTORY; OCEAN CURRENTS; CONTROL REGION; CHANOS-CHANOS AB We compared patterns of genetic population structure and historical demography of several tropical Pacific Conus species that have similar though not completely overlapping distributions. Although these species possess similar life histories with planktonic larval durations of at least three weeks and exhibit genetic homogeneity across broad expanses of their distributions, they show distinct patterns of genetic population structure that are largely associated with genetic differentiation of geographically isolated populations. While previous analyses of C. ebraeus (Linnaeus, 1758) and C. miliaris (Hwass in Bruguiere, 1792) detected high levels of genetic differentiation among isolated locations in the eastern Pacific and at Easter Island for each species, respectively, C. chaldaeus (Roding, 1798) does not show robust evidence of population differentiation across the East Pacific Barrier, albeit the sample size from the eastern Pacific is small. In addition, unlike C. chaldaeus and C. ebraeus, C. sanguinolentus (Quoy and Gaimard, 1834) exhibits a strong genetic break at Hawaii. Analyses of mismatch distributions suggest recent population expansion of C. chaldaeus and C. sanguinolent us as well as the Hawaiian endemic species C. abbreviatus (Reeve, 1843) during the past one million years as was observed previously for tropical Pacific populations of C. ebraeus and C. miliaris. Taken together, these results show that although high dispersal rates appear to genetically homogenize broadly distributed species in the tropical Pacific, stochasticity in long-distance dispersal likely instigates genetic differentiation of geographically isolated and peripheral populations and results in discordant phylogeographic patterns among even closely related species. Thus, population divergence and speciation in the tropical Pacific likely occur among populations at isolated locations though gene flow tends to prevent differentiation at broad geographic scales in species with high potentials for dispersal. C1 [Duda, Thomas F., Jr.; Terbio, Marielle; Chen, Gang; Phillips, Semoya; Olenzek, Amy M.; Chang, Dan; Morris, David W.] Univ Michigan, Museum Zool, Ann Arbor, MI 48109 USA. [Duda, Thomas F., Jr.; Terbio, Marielle; Chen, Gang; Phillips, Semoya; Olenzek, Amy M.; Chang, Dan; Morris, David W.] Univ Michigan, Dept Ecol & Evolutionary Biol, Ann Arbor, MI 48109 USA. [Duda, Thomas F., Jr.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. RP Duda, TF (reprint author), Univ Michigan, Museum Zool, 1109 Geddes Ave, Ann Arbor, MI 48109 USA. EM tfduda@umich.edu NR 55 TC 6 Z9 6 U1 0 U2 15 PU AMER MALACOLOGICAL SOC, INC PI WILMINGTON PA DELAWARE MUSEUM NATURAL HISTORY, BOX 3937, WILMINGTON, DE 19807-0937 USA SN 0740-2783 J9 AM MALACOL BULL JI Am. Malacol. Bull. PD FEB 22 PY 2012 VL 30 IS 1 BP 175 EP 187 PG 13 WC Marine & Freshwater Biology; Zoology SC Marine & Freshwater Biology; Zoology GA 904OI UT WOS:000301207400016 ER PT J AU Molinar, E Rios, N Spadafora, C Arnold, AE Coley, PD Kursar, TA Gerwick, WH Cubilla-Rios, L AF Molinar, Eunice Rios, Nivia Spadafora, Carmenza Arnold, A. Elizabeth Coley, Phyllis D. Kursar, Thomas A. Gerwick, William H. Cubilla-Rios, Luis TI Coibanoles, a new class of meroterpenoids produced by Pycnoporus sanguineus SO TETRAHEDRON LETTERS LA English DT Article DE Pycnoporus; Trypanosoma; Leishmania; Meroterpenoids; Coibanoles ID ALTERNARIA-ALTERNATA; FUNGAL ENDOPHYTES; CONSERVATION AB Three new terpenoids of mixed biosynthetic origin were isolated from the culture filtrate of the endophytic fungus Pycnoporus sanguineus. Their structures were determined by extensive spectroscopic analyses. We have named these tricyclic and tetracyclic metabolites 'coibanoles A-C' in reference to Coiba Island and Coiba National Park, Panama, from which the plant and endophyte were collected. The extract was inactive to the human parasites Trypanosoma cruzi, Leishmania donovani, and Plasmodium falciparum at a test concentration of 10 mu g/mL. (C) 2011 Elsevier Ltd. All rights reserved. C1 [Molinar, Eunice; Rios, Nivia; Cubilla-Rios, Luis] Univ Panama, Fac Nat Exact Sci & Technol, Lab Trop Bioorgan Chem, Panama City, Panama. [Spadafora, Carmenza] Natl Secretariat Sci Technol & Innovat, Inst Adv Sci Invest & High Technol Serv, City Of Knowledge, Panama. [Arnold, A. Elizabeth] Univ Arizona, Sch Plant Sci, Tucson, AZ 85721 USA. [Coley, Phyllis D.; Kursar, Thomas A.] Univ Utah, Dept Biol, Salt Lake City, UT 84112 USA. [Coley, Phyllis D.; Kursar, Thomas A.; Cubilla-Rios, Luis] Smithsonian Trop Res Inst, Unit 0948, Apo Aa 340020948, Panama. [Gerwick, William H.] Univ Calif San Diego, Skaggs Sch Pharm & Pharmaceut Sci, La Jolla, CA 92093 USA. [Gerwick, William H.] Univ Calif San Diego, Scripps Inst Oceanog, Ctr Marine Biotechnol & Biomed, La Jolla, CA 92093 USA. RP Cubilla-Rios, L (reprint author), Univ Panama, Fac Nat Exact Sci & Technol, Lab Trop Bioorgan Chem, Panama City, Panama. EM lucr@ancon.up.ac.pa OI Spadafora, Carmenza/0000-0002-3002-9467 FU US NIH [2 U01 TW006634-06]; College of Agriculture and Life Sciences at the University of Arizona FX This work was supported by US NIH Grant for the International Cooperative Biodiversity Groups program (ICBG-Panama; 2 U01 TW006634-06). We thank M. Gunatilaka and D. Mahana for assistance with DNA sequencing, and the College of Agriculture and Life Sciences at the University of Arizona for logistical and financial support. We also give our thanks to the personnel of Panama's Autoridad Nacional del Ambiente for their assistance in conducting this research project. NR 26 TC 6 Z9 6 U1 0 U2 31 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0040-4039 J9 TETRAHEDRON LETT JI Tetrahedron Lett. PD FEB 22 PY 2012 VL 53 IS 8 BP 919 EP 922 DI 10.1016/j.tetlet.2011.12.021 PG 4 WC Chemistry, Organic SC Chemistry GA 891IL UT WOS:000300210300005 PM 25177062 ER PT J AU Tierney, SM Sanjur, O Grajales, GG Santos, LM Bermingham, E Wcislo, WT AF Tierney, Simon M. Sanjur, Oris Grajales, Grethel G. Santos, Leandro M. Bermingham, Eldredge Wcislo, William T. TI Photic niche invasions: phylogenetic history of the dim-light foraging augochlorine bees (Halictidae) SO PROCEEDINGS OF THE ROYAL SOCIETY B-BIOLOGICAL SCIENCES LA English DT Article DE opsin; dim-light; Augochlorini; adaptive radiation; relictual taxa ID NOCTURNAL BEE; HYMENOPTERA-HALICTIDAE; ACHROMATIC VISION; GENUS MEGALOPTA; SOCIAL-BEHAVIOR; NUCLEAR GENES; COLOR-VISION; MAJOR OPSIN; EVOLUTION; INSECTS AB Most bees rely on flowering plants and hence are diurnal foragers. From this ancestral state, dim-light foraging in bees requires significant adaptations to a new photic environment. We used DNA sequences to evaluate the phylogenetic history of the most diverse clade of Apoidea that is adapted to dim-light environments (Augochlorini: Megalopta, Megaloptidia and Megommation). The most speciose lineage, Megalopta, is distal to the remaining dim-light genera, and its closest diurnal relative (Xenochlora) is recovered as a lineage that has secondarily reverted to diurnal foraging. Tests for adaptive protein evolution indicate that long-wavelength opsin shows strong evidence of stabilizing selection, with no more than five codons (2%) under positive selection, depending on analytical procedure. In the branch leading to Megalopta, the amino acid of the single positively selected codon is conserved among ancestral Halictidae examined, and is homologous to codons known to influence molecular structure at the chromophore-binding pocket. Theoretically, such mutations can shift photopigment lambda(max) sensitivity and enable visual transduction in alternate photic environments. Results are discussed in light of the available evidence on photopigment structure, morphological specialization and biogeographic distributions over geological time. C1 [Tierney, Simon M.; Sanjur, Oris; Grajales, Grethel G.; Bermingham, Eldredge; Wcislo, William T.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. [Santos, Leandro M.] Univ Fed Parana, Dept Zool, Lab Biol Comparada Hymenoptera, BR-81531980 Curitiba, Parana, Brazil. RP Tierney, SM (reprint author), Smithsonian Trop Res Inst, Apartado Postal 0843-03092, Balboa, Ancon, Panama. EM tierneys@si.edu; wcislow@si.edu RI Santos, Leandro/H-4364-2012; Tierney, Simon/H-2410-2015 OI Tierney, Simon/0000-0002-8812-6753 FU Earl S. Tupper Post-doctoral Fellowship; STRI; Royal Entomological Society; National Geographic Society FX For assistance in the field and associated logistics, we would like to thank Eduardo Almeida, Ricardo Ayala, Carlos Espinosa, Paola Galgani, Therany Gonzales-Ojeda, Emmet Gowin, Gabriel Jacome, Karen Kapheim, Fatima Knoll, Gabriel Melo, Nigel Pitman, Adam Smith, Elicio Tapia, Jelle Van Sweden, Don Windsor and the Smithsonian Tropical Research Institute (STRI) support staff. We are grateful to Maribel Gonzalez and Nimiadina Herrera for laboratory assistance and Matt Kweskin for bioinformatic assistance. For constructive comments, we thank Karen Kapheim, Oscar Puebla, Sandra Rehan and two anonymous referees. Research was supported by an Earl S. Tupper Post-doctoral Fellowship (S. M. T.), general funds from STRI (W. T. W. and S. M. T.), a Royal Entomological Society Outreach Expedition Grant (S. M. T.) and a National Geographic Society Research and Exploration Grant (W. T. W. and S. M. T.). NR 72 TC 12 Z9 12 U1 1 U2 20 PU ROYAL SOC PI LONDON PA 6-9 CARLTON HOUSE TERRACE, LONDON SW1Y 5AG, ENGLAND SN 0962-8452 EI 1471-2954 J9 P ROY SOC B-BIOL SCI JI Proc. R. Soc. B-Biol. Sci. PD FEB 22 PY 2012 VL 279 IS 1729 BP 794 EP 803 DI 10.1098/rspb.2011.1355 PG 10 WC Biology; Ecology; Evolutionary Biology SC Life Sciences & Biomedicine - Other Topics; Environmental Sciences & Ecology; Evolutionary Biology GA 876NK UT WOS:000299114100023 PM 21795273 ER PT J AU Stutter, MI Shand, CA George, TS Blackwell, MSA Bol, R MacKay, RL Richardson, AE Condron, LM Turner, BL Haygarth, PM AF Stutter, Marc I. Shand, Charles A. George, Timothy S. Blackwell, Martin S. A. Bol, Roland MacKay, Regina L. Richardson, Alan E. Condron, Leo M. Turner, Benjamin L. Haygarth, Philip M. TI Recovering Phosphorus from Soil: A Root Solution? SO ENVIRONMENTAL SCIENCE & TECHNOLOGY LA English DT Editorial Material C1 [Stutter, Marc I.; Shand, Charles A.; George, Timothy S.] James Hutton Inst, Aberdeen AB15 8QH, Scotland. [Stutter, Marc I.; Shand, Charles A.; George, Timothy S.] James Hutton Inst, Dundee DD2 5DA, Scotland. [Blackwell, Martin S. A.; Bol, Roland] Rothamstead Res N Wyke, Okehampton EX20 2SB, Devon, England. [MacKay, Regina L.] Univ Dundee, Coll Life Sci, Dundee DD1 5EH, Scotland. [Richardson, Alan E.] CSIRO Plant Ind, Canberra, ACT 2601, Australia. [Condron, Leo M.] Lincoln Univ, Fac Agr & Life Sci, Canterbury 7647, New Zealand. [Turner, Benjamin L.] Smithsonian Trop Res Inst, Balboa, Panama. [Haygarth, Philip M.] Univ Lancaster, Lancaster Environm Ctr, Lancaster LA1 4YQ, England. RP Stutter, MI (reprint author), James Hutton Inst, Aberdeen AB15 8QH, Scotland. EM marc.stutter@hutton.ac.uk RI Turner, Benjamin/E-5940-2011; Richardson, Alan/I-1903-2012; Condron, Leo/E-9458-2013; bol, roland/H-9324-2013; CSIRO, SAF/H-3134-2013; Blackwell, Martin/D-4081-2013; Haygarth, Philip/F-6790-2014; OI Turner, Benjamin/0000-0002-6585-0722; Stutter, Marc/0000-0003-1483-376X FU Biotechnology and Biological Sciences Research Council [BB/D011612/1, BB/D011612/2] NR 5 TC 31 Z9 35 U1 5 U2 92 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0013-936X J9 ENVIRON SCI TECHNOL JI Environ. Sci. Technol. PD FEB 21 PY 2012 VL 46 IS 4 BP 1977 EP 1978 DI 10.1021/es2044745 PG 2 WC Engineering, Environmental; Environmental Sciences SC Engineering; Environmental Sciences & Ecology GA 894ZL UT WOS:000300465900004 PM 22280364 ER PT J AU Abramowski, A Acero, F Aharonian, F Akhperjanian, AG Anton, G Balzer, A Barnacka, A de Almeida, UB Becherini, Y Becker, J Behera, B Bernlohr, K Birsin, E Biteau, J Bochow, A Boisson, C Bolmont, J Bordas, P Brucker, J Brun, F Brun, P Bulik, T Busching, I Carrigan, S Casanova, S Cerruti, M Chadwick, PM Charbonnier, A Chaves, RCG Cheesebrough, A Clapson, AC Coignet, G Cologna, G Conrad, J Dalton, M Daniel, MK Davids, ID Degrange, B Deil, C Dickinson, HJ Djannati-Atai, A Domainko, W Drury, LO Dubus, G Dutson, K Dyks, J Dyrda, M Egberts, K Eger, P Espigat, P Fallon, L Farnier, C Fegan, S Feinstein, F Fernandes, MV Fiasson, A Fontaine, G Forster, A Fussling, M Gallant, YA Gast, H Gerard, L Gerbig, D Giebels, B Glicenstein, JF Gluck, B Goret, P Goring, D Haffner, S Hague, JD Hampf, D Hauser, M Heinz, S Heinzelmann, G Henri, G Hermann, G Hinton, JA Hoffmann, A Hofmann, W Hofverberg, P Holler, M Horns, D Jacholkowska, A de Jager, OC Jahn, C Jamrozy, M Jung, I Kastendieck, MA Katarzynski, K Katz, U Kaufmann, S Keogh, D Khangulyan, D Khelifi, B Klochkov, D Kluzniak, W Kneiske, T Komin, N Kosack, K Kossakowski, R Laffon, H Lamanna, G Lennarz, D Lohse, T Lopatin, A Lu, CC Marandon, V Marcowith, A Masbou, J Maurin, D Maxted, N Mayer, M McComb, TJL Medina, MC Mehault, J Moderski, R Moulin, E Naumann, CL Naumann-Godo, M de Naurois, M Nedbal, D Nekrassov, D Nguyen, N Nicholas, B Niemiec, J Nolan, SJ Ohm, S Wilhelmi, ED Opitz, B Ostrowski, M Oya, I Panter, M Arribas, MP Pedaletti, G Pelletier, G Petrucci, PO Pita, S Puhlhofer, G Punch, M Quirrenbach, A Raue, M Rayner, SM Reimer, A Reimer, O Renaud, M de los Reyes, R Rieger, F Ripken, J Rob, L Rosier-Lees, S Rowell, G Rudak, B Rulten, CB Ruppel, J Sahakian, V Sanchez, DA Santangelo, A Schlickeiser, R Schock, FM Schulz, A Schwanke, U Schwarzburg, S Schwemmer, S Sheidaei, F Skilton, JL Sol, H Spengler, G Stawarz, L Steenkamp, R Stegmann, C Stinzing, F Stycz, K Sushch, I Szostek, A Tavernet, JP Terrier, R Tluczykont, M Valerius, K van Eldik, C Vasileiadis, G Venter, C Vialle, JP Viana, A Vincent, P Volk, HJ Volpe, F Vorobiov, S Vorster, M Wagner, SJ Ward, M White, R Wierzcholska, A Zacharias, M Zajczyk, A Zdziarski, AA Zech, A Zechlin, HS Aleksic, J Antonelli, LA Antoranz, P Backes, M Barrio, JA Bastieri, D Gonzalez, JB Bednarek, W Berdyugin, A Berger, K Bernardini, E Biland, A Blanch, O Bock, RK Boller, A Bonnoli, G Tridon, DB Braun, I Bretz, T Canellas, A Carmona, E Carosi, A Colin, P Colombo, E Contreras, JL Cortina, J Cossio, L Covino, S Dazzi, F De Angelis, A del Pozo, ED De Lotto, B Mendez, CD Ortega, AD Doert, M Dominguez, A Prester, DD Dorner, D Doro, M Elsaesser, D Ferenc, D Fonseca, MV Font, L Fruck, C Lopez, RJG Garczarczyk, M Garrido, D Giavitto, G Godinovic, N Hadasch, D Hafner, D Herrero, A Hildebrand, D Hohne-Monch, D Hose, J Hrupec, D Huber, B Jogler, T Klepser, S Krahenbuhl, T Krause, J La Barbera, A Lelas, D Leonardo, E Lindfors, E Lombardi, S Lopez, M Lorenz, E Makariev, M Maneva, G Mankuzhiyil, N Mannheim, K Maraschi, L Mariotti, M Martinez, M Mazin, D Meucci, M Miranda, JM Mirzoyan, R Miyamoto, H Moldon, J Moralejo, A Munar, P Nieto, D Nilsson, K Orito, R Oya, I Paneque, D Paoletti, R Pardo, S Paredes, JM Partini, S Pasanen, M Pauss, F Perez-Torres, MA Persic, M Peruzzo, L Pilia, M Pochon, J Prada, F Moroni, PGP Prandini, E Puljak, I Reichardt, I Reinthal, R Rhode, W Ribo, M Rico, J Rugamer, S Saggion, A Saito, K Saito, TY Salvati, M Satalecka, K Scalzotto, V Scapin, V Schultz, C Schweizer, T Shayduk, M Shore, SN Sillanpaa, A Sitarek, J Sobczynska, D Spanier, F Spiro, S Stamerra, A Steinke, B Storz, J Strah, N Suric, T Takalo, L Takami, H Tavecchio, F Temnikov, P Terzic, T Tescaro, D Teshima, M Thom, M Tibolla, O Torres, DF Treves, A Vankov, H Vogler, P Wagner, RM Weitzel, Q Zabalza, V Zandanel, F Zanin, R Arlen, T Aune, T Beilicke, M Benbow, W Bouvier, A Bradbury, SM Buckley, JH Bugaev, V Byrum, K Cannon, A Cesarini, A Ciupik, L Connolly, MP Cui, W Dickherber, R Duke, C Errando, M Falcone, A Finley, JP Finnegan, G Fortson, L Furniss, A Galante, N Gall, D Godambe, S Griffin, S Grube, J Gyuk, G Hanna, D Holder, J Huan, H Hui, CM Kaaret, P Karlsson, N Kertzman, M Khassen, Y Kieda, D Krawczynski, H Krennrich, F Lang, MJ LeBohec, S Maier, G McArthur, S McCann, A Moriarty, P Mukherjee, R Nunez, PD Ong, RA Orr, M Otte, AN Park, N Perkins, JS Pichel, A Pohl, M Prokoph, H Ragan, K Reyes, LC Reynolds, PT Roache, E Rose, HJ Ruppel, J Schroedter, M Sembroski, GH Senturk, GD Telezhinsky, I Tesic, G Theiling, M Thibadeau, S Varlotta, A Vassiliev, VV Vivier, M Wakely, SP Weekes, TC Williams, DA Zitzer, B de Almeida, UB Cara, M Casadio, C Cheung, CC McConville, W Davies, F Doi, A Giovannini, G Giroletti, M Hada, K Hardee, P Harris, DE Junor, W Kino, M Lee, NP Ly, C Madrid, J Massaro, F Mundell, CG Nagai, H Perlman, ES Steele, IA Walker, RC Wood, DL AF Abramowski, A. Acero, F. Aharonian, F. Akhperjanian, A. G. Anton, G. Balzer, A. Barnacka, A. de Almeida, U. Barres Becherini, Y. Becker, J. Behera, B. Bernloehr, K. Birsin, E. Biteau, J. Bochow, A. Boisson, C. Bolmont, J. Bordas, P. Brucker, J. Brun, F. Brun, P. Bulik, T. Buesching, I. Carrigan, S. Casanova, S. Cerruti, M. Chadwick, P. M. Charbonnier, A. Chaves, R. C. G. Cheesebrough, A. Clapson, A. C. Coignet, G. Cologna, G. Conrad, J. Dalton, M. Daniel, M. K. Davids, I. D. Degrange, B. Deil, C. Dickinson, H. J. Djannati-Atai, A. Domainko, W. Drury, L. O'C. Dubus, G. Dutson, K. Dyks, J. Dyrda, M. Egberts, K. Eger, P. Espigat, P. Fallon, L. Farnier, C. Fegan, S. Feinstein, F. Fernandes, M. V. Fiasson, A. Fontaine, G. Foerster, A. Fuessling, M. Gallant, Y. A. Gast, H. Gerard, L. Gerbig, D. Giebels, B. Glicenstein, J. F. Glueck, B. Goret, P. Goering, D. Haeffner, S. Hague, J. D. Hampf, D. Hauser, M. Heinz, S. Heinzelmann, G. Henri, G. Hermann, G. Hinton, J. A. Hoffmann, A. Hofmann, W. Hofverberg, P. 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CA HESS Collaboration MAGIC Collaboration VERITAS Collaboration TI THE 2010 VERY HIGH ENERGY gamma-RAY FLARE AND 10 YEARS OF MULTI-WAVELENGTH OBSERVATIONS OF M 87 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: active; galaxies: individual (M 87); galaxies: jets; galaxies: nuclei; gamma rays: galaxies; radiation mechanisms: non-thermal ID ACTIVE GALACTIC NUCLEI; LARGE-AREA TELESCOPE; SUPERMASSIVE BLACK-HOLE; RADIO GALAXY M87; BASE-LINE ARRAY; TEV EMISSION; CRAB-NEBULA; UNIFIED SCHEMES; SCALE JETS; INNER JET AB The giant radio galaxy M 87 with its proximity (16 Mpc), famous jet, and very massive black hole ((3-6) x 10(9) M-circle dot) provides a unique opportunity to investigate the origin of very high energy (VHE; E > 100 GeV) gamma-ray emission generated in relativistic outflows and the surroundings of supermassive black holes. M 87 has been established as a VHE gamma-ray emitter since 2006. The VHE gamma-ray emission displays strong variability on timescales as short as a day. In this paper, results from a joint VHE monitoring campaign on M 87 by the MAGIC and VERITAS instruments in 2010 are reported. During the campaign, a flare at VHE was detected triggering further observations at VHE (H.E.S.S.), X-rays (Chandra), and radio (43 GHz Very Long Baseline Array, VLBA). The excellent sampling of the VHE gamma-ray light curve enables one to derive a precise temporal characterization of the flare: the single, isolated flare is well described by a two-sided exponential function with significantly different flux rise and decay times of tau(rise)(d) = (1.69 +/- 0.30) days and tau(decay)(d) = (0.611 +/- 0.080) days, respectively. While the overall variability pattern of the 2010 flare appears somewhat different from that of previous VHE flares in 2005 and 2008, they share very similar timescales (similar to day), peak fluxes (Phi(>0.35 TeV) similar or equal to (1-3) x 10(-11) photons cm(-2) s(-1)), and VHE spectra. VLBA radio observations of 43 GHz of the inner jet regions indicate no enhanced flux in 2010 in contrast to observations in 2008, where an increase of the radio flux of the innermost core regions coincided with a VHE flare. On the other hand, Chandra X-ray observations taken similar to 3 days after the peak of the VHE gamma-ray emission reveal an enhanced flux from the core (flux increased by factor similar to 2; variability timescale <2 days). The long-term (2001-2010) multi-wavelength (MWL) light curve of M 87, spanning from radio to VHE and including data from Hubble Space Telescope, Liverpool Telescope, Very Large Array, and European VLBI Network, is used to further investigate the origin of the VHE gamma-ray emission. No unique, common MWL signature of the three VHE flares has been identified. In the outer kiloparsec jet region, in particular in HST-1, no enhanced MWL activity was detected in 2008 and 2010, disfavoring it as the origin of the VHE flares during these years. Shortly after two of the three flares (2008 and 2010), the X-ray core was observed to be at a higher flux level than its characteristic range (determined from more than 60 monitoring observations: 2002-2009). In 2005, the strong flux dominance of HST-1 could have suppressed the detection of such a feature. Published models for VHE gamma-ray emission from M 87 are reviewed in the light of the new data. C1 [Abramowski, A.; Fernandes, M. 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S.] Astroparticle Phys Lab NASA GSFC, Greenbelt, MD 20771 USA. [Perkins, J. S.] Univ Maryland Baltimore Cty, Baltimore, MD 21250 USA. [Pichel, A.] Inst Astron & Fis Espacio, RA-1428 Buenos Aires, DF, Argentina. [Pohl, M.; Ruppel, J.; Telezhinsky, I.] Univ Potsdam, Inst Phys & Astron, D-14476 Potsdam, Germany. [Reynolds, P. T.] Cork Inst Technol, Dept Appl Phys & Instrumentat, Cork, Ireland. [Cara, M.; Perlman, E. S.] Florida Inst Technol, Dept Phys & Space Sci, Melbourne, FL 32901 USA. [Casadio, C.; Giovannini, G.; Giroletti, M.] INAF Ist Radioastron, I-40129 Bologna, Italy. [Cheung, C. C.] Natl Acad Sci, Washington, DC 20001 USA. [McConville, W.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [McConville, W.] Univ Maryland, Dept Phys, College Pk, MD 20742 USA. [McConville, W.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Davies, F.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. [Doi, A.] Japan Aerosp Explorat Agcy, Inst Space & Astronaut Sci, Sagamihara, Kanagawa 2525210, Japan. [Giovannini, G.] Univ Bologna, Dipartimento Astron, I-40127 Bologna, Italy. [Hada, K.] Grad Univ Adv Studies SOKENDAI, Mitaka, Tokyo 1818588, Japan. [Hada, K.; Kino, M.; Nagai, H.] Natl Inst Nat Sci, Natl Astron Observ Japan, Mitaka, Tokyo 1818588, Japan. [Hardee, P.] Univ Alabama, Dept Phys & Astron, Tuscaloosa, AL 35487 USA. [Harris, D. E.; Lee, N. P.; Massaro, F.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. [Junor, W.] Los Alamos Natl Lab, Los Alamos, NM 87545 USA. [Ly, C.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Madrid, J.] Swinburne Univ Technol, Ctr Astrophys & Supercomp, Hawthorn, Vic 3122, Australia. [Mundell, C. G.; Steele, I. A.] Liverpool John Moores Univ, Astrophys Res Inst, Liverpool L3 5UX, Merseyside, England. [Walker, R. C.] Natl Radio Astron Observ NRAO, Socorro, NM 87801 USA. [Wood, D. L.] USN, Res Lab, Div Space Sci, Washington, DC 20375 USA. RP Abramowski, A (reprint author), Univ Hamburg, Inst Expt Phys, Luruper Chaussee 149, D-22761 Hamburg, Germany. EM martin.raue@desy.de; stawarz@astro.isas.jaxa.jp; colin@mppmu.mpg.de; mazin@ifae.es; beilicke@physics.wustl.edu; cmhui@physics.utah.edu RI Font, Lluis/L-4197-2014; Contreras Gonzalez, Jose Luis/K-7255-2014; Maneva, Galina/L-7120-2016; Temnikov, Petar/L-6999-2016; Massaro, Francesco/L-9102-2016; Makariev, Martin/M-2122-2016; Torres, Diego/O-9422-2016; Drury, Luke/B-1916-2017; Barrio, Juan/L-3227-2014; Moulin, Emmanuel/B-5959-2017; Martinez Rodriguez, Manel/C-2539-2017; Cortina, Juan/C-2783-2017; Lopez Moya, Marcos/L-2304-2014; Moralejo Olaizola, Abelardo/M-2916-2014; Ribo, Marc/B-3579-2015; Katarzynski, Krzysztof/G-4528-2014; Jamrozy, Marek/F-4507-2015; Casanova, Sabrina/J-8935-2013; Antoranz, Pedro/H-5095-2015; Anton, Gisela/C-4840-2013; Khassen, Yerbol/I-3806-2015; Delgado, Carlos/K-7587-2014; Nieto, Daniel/J-7250-2015; Miranda, Jose Miguel/F-2913-2013; Daniel, Michael/A-2903-2010; Braun, Isabel/C-9373-2012; Prada Moroni, Pier Giorgio/G-5565-2011; Mannheim, Karl/F-6705-2012; Reimer, Olaf/A-3117-2013; van Eldik, Christopher/C-3901-2013; Katz, Uli/E-1925-2013; Cara, Mihai/G-1023-2013; Tjus, Julia/G-8145-2012; Fontaine, Gerard/D-6420-2014; Venter, Christo/E-6884-2011; Rico, Javier/K-8004-2014; Fernandez, Ester/K-9734-2014; Komin, Nukri/J-6781-2015; Fonseca Gonzalez, Maria Victoria/I-2004-2015; Backes, Michael/N-5126-2016; Reichardt, Ignasi/P-7478-2016 OI Giovannini, Gabriele/0000-0003-4916-6362; Prada Moroni, Pier Giorgio/0000-0001-9712-9916; Chadwick, Paula/0000-0002-1468-2685; Kneiske, Tanja M./0000-0002-3210-6200; LA BARBERA, ANTONINO/0000-0002-5880-8913; Font, Lluis/0000-0003-2109-5961; Contreras Gonzalez, Jose Luis/0000-0001-7282-2394; Temnikov, Petar/0000-0002-9559-3384; Massaro, Francesco/0000-0002-1704-9850; Torres, Diego/0000-0002-1522-9065; Drury, Luke/0000-0002-9257-2270; Barrio, Juan/0000-0002-0965-0259; Moulin, Emmanuel/0000-0003-4007-0145; Cortina, Juan/0000-0003-4576-0452; Cui, Wei/0000-0002-6324-5772; Lopez Moya, Marcos/0000-0002-8791-7908; Moralejo Olaizola, Abelardo/0000-0002-1344-9080; Casanova, Sabrina/0000-0002-6144-9122; Antoranz, Pedro/0000-0002-3015-3601; Anton, Gisela/0000-0003-2039-4724; Khassen, Yerbol/0000-0002-7296-3100; Delgado, Carlos/0000-0002-7014-4101; Nieto, Daniel/0000-0003-3343-0755; Miranda, Jose Miguel/0000-0002-1472-9690; Daniel, Michael/0000-0002-8053-7910; Braun, Isabel/0000-0002-9389-0502; Reimer, Olaf/0000-0001-6953-1385; van Eldik, Christopher/0000-0001-9669-645X; Katz, Uli/0000-0002-7063-4418; Venter, Christo/0000-0002-2666-4812; Rico, Javier/0000-0003-4137-1134; Cesarini, Andrea/0000-0002-8611-8610; leonardo, elvira/0000-0003-0271-7673; de los Reyes Lopez, Raquel/0000-0003-0485-9552; Komin, Nukri/0000-0003-3280-0582; De Lotto, Barbara/0000-0003-3624-4480; Fonseca Gonzalez, Maria Victoria/0000-0003-2235-0725; Backes, Michael/0000-0002-9326-6400; Reichardt, Ignasi/0000-0003-3694-3820 FU Namibian authorities; German Ministry for Education and Research (BMBF); Max Planck Society; French Ministry for Research; CNRS-IN2P3; CNRS; U.K. Science and Technology Facilities Council (STFC); IPNP of the Charles University; Polish Ministry of Science and Higher Education; South African Department of Science and Technology; National Research Foundation; University of Namibia; German BMBF; German MPG; Italian INFN; Swiss National Fund SNF; Spanish MICINN; Bulgarian NSF [CSD2007-00042, CSD2009-00064, DO02-353]; Academy of Finland [127740]; YIP of the Helmholtz Gemeinschaft; DFG Cluster of Excellence "Origin and Structure of the Universe,"; DFG Collaborative Research Centers [SFB823/C4, SFB876/C3]; Polish MNiSzW [745/N-HESS-MAGIC/2010/0]; US Department of Energy Office of Science; US National Science Foundation; Smithsonian Institution; NSERC in Canada; Science Foundation Ireland (SFI) [10/RFP/AST2748]; STFC in the UK; Istituto Nazionale di Astrofisica in Italy; Centre National d'Etudes Spatiales in France; NASA [GO0-11120X]; Associated Universities, Inc.; European Community [227290] FX The H.E.S.S. Collaboration acknowledges support of the Namibian authorities and of the University of Namibia in facilitating the construction and operation of H.E.S.S., as is the support by the German Ministry for Education and Research (BMBF), the Max Planck Society, the French Ministry for Research, the CNRS-IN2P3 and the Astroparticle Interdisciplinary Programme of the CNRS, the U.K. Science and Technology Facilities Council (STFC), the IPNP of the Charles University, the Polish Ministry of Science and Higher Education, the South African Department of Science and Technology and National Research Foundation, and by the University of Namibia. We appreciate the excellent work of the technical support staff in Berlin, Durham, Hamburg, Heidelberg, Palaiseau, Paris, Saclay, and in Namibia in the construction and operation of the equipment.; The MAGIC Collaboration thank the Instituto de Astrofisica de Canarias for the excellent working conditions at the Observatorio del Roque de los Muchachos in La Palma. The support of the German BMBF and MPG, the Italian INFN, the Swiss National Fund SNF, and the Spanish MICINN is gratefully acknowledged. This work was also supported by the Marie Curie program, by the CPAN CSD2007-00042 and MultiDark CSD2009-00064 projects of the Spanish Consolider-Ingenio 2010 programme, by grant DO02-353 of the Bulgarian NSF, by grant 127740 of the Academy of Finland, by the YIP of the Helmholtz Gemeinschaft, by the DFG Cluster of Excellence "Origin and Structure of the Universe," by the DFG Collaborative Research Centers SFB823/C4 and SFB876/C3, and by the Polish MNiSzW grant 745/N-HESS-MAGIC/2010/0.; The VERITAS Collaboration acknowledges support from the US Department of Energy Office of Science, the US National Science Foundation, and the Smithsonian Institution, from NSERC in Canada, from Science Foundation Ireland (SFI 10/RFP/AST2748), and from STFC in the UK. We acknowledge the excellent work of the technical support staff at the FLWO and at the collaborating institutions in the construction and operation of the instrument.; The Fermi LAT Collaboration acknowledges generous ongoing support from a number of agencies and institutes that have supported both the development and the operation of the LAT as well as scientific data analysis. These include the National Aeronautics and Space Administration and the Department of Energy in the United States, the Commissariat a l'Energie Atomique and the Centre National de la Recherche Scientifique/Institut National de Physique Nucleaire et de Physique des Particules in France, the Agenzia Spaziale Italiana and the Istituto Nazionale di Fisica Nucleare in Italy, the Ministry of Education, Culture, Sports, Science and Technology (MEXT), High Energy Accelerator Research Organization (KEK) and Japan Aerospace Exploration Agency (JAXA) in Japan, and the K. A. Wallenberg Foundation, the Swedish Research Council and the Swedish National Space Board in Sweden. Additional support for science analysis during the operations phase is gratefully acknowledged from the Istituto Nazionale di Astrofisica in Italy and the Centre National d'Etudes Spatiales in France.; Analysis of the Chandra data was supported by NASA grant GO0-11120X.; The Very Long Baseline Array is operated by the National Radio Astronomy Observatory, a facility of the NSF, operated under cooperative agreement by Associated Universities, Inc.; The European VLBI Network is a joint facility of European, Chinese, South African, and other radio astronomy institutes funded by their national research councils. This effort is supported by the European Community Framework Programme 7, Advanced Radio Astronomy in Europe, grant agreement no. 227290. NR 107 TC 59 Z9 61 U1 3 U2 42 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD FEB 20 PY 2012 VL 746 IS 2 AR 151 DI 10.1088/0004-637X/746/2/151 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 894DD UT WOS:000300406300037 ER PT J AU Aliu, E Arlen, T Aune, T Beilicke, M Benbow, W Bouvier, A Bradbury, SM Buckley, JH Bugaev, V Byrum, K Cannon, A Cesarini, A Ciupik, L Collins-Hughes, E Connolly, MP Cui, W Dickherber, R Duke, C Errando, M Falcone, A Finley, JP Finnegan, G Fortson, L Furniss, A Galante, N Gall, D Godambe, S Griffin, S Grube, J Guenette, R Gyuk, G Hanna, D Holder, J Huan, H Hughes, G Hui, CM Humensky, TB Imran, A Kaaret, P Karlsson, N Kertzman, M Kieda, D Krawczynski, H Krennrich, F Lang, MJ LeBohec, S Madhavan, AS Maier, G Majumdar, P McArthur, S McCann, A Moriarty, P Mukherjee, R Nunez, PD Ong, RA Orr, M Otte, AN Park, N Perkins, JS Pichel, A Pohl, M Prokoph, H Quinn, J Ragan, K Reyes, LC Reynolds, PT Roache, E Rose, HJ Ruppel, J Saxon, DB Schroedter, M Sembroski, GH Senturk, GD Skole, C Staszak, D Tesic, G Theiling, M Thibadeau, S Tsurusaki, K Tyler, J Varlotta, A Vassiliev, VV Vincent, S Vivier, M Wakely, SP Ward, JE Weekes, TC Weinstein, A Weisgarber, T Williams, DA Zitzer, B AF Aliu, E. Arlen, T. Aune, T. Beilicke, M. Benbow, W. Bouvier, A. Bradbury, S. M. Buckley, J. H. Bugaev, V. Byrum, K. Cannon, A. Cesarini, A. Ciupik, L. Collins-Hughes, E. Connolly, M. P. Cui, W. Dickherber, R. Duke, C. Errando, M. Falcone, A. Finley, J. P. Finnegan, G. Fortson, L. Furniss, A. Galante, N. Gall, D. Godambe, S. Griffin, S. Grube, J. Guenette, R. Gyuk, G. Hanna, D. Holder, J. Huan, H. Hughes, G. Hui, C. M. Humensky, T. B. Imran, A. Kaaret, P. Karlsson, N. Kertzman, M. Kieda, D. Krawczynski, H. Krennrich, F. Lang, M. J. LeBohec, S. Madhavan, A. S. Maier, G. Majumdar, P. McArthur, S. McCann, A. Moriarty, P. Mukherjee, R. Nunez, P. D. Ong, R. A. Orr, M. Otte, A. N. Park, N. Perkins, J. S. Pichel, A. Pohl, M. Prokoph, H. Quinn, J. Ragan, K. Reyes, L. C. Reynolds, P. T. Roache, E. Rose, H. J. Ruppel, J. Saxon, D. B. Schroedter, M. Sembroski, G. H. Sentuerk, G. D. Skole, C. Staszak, D. Tesic, G. Theiling, M. Thibadeau, S. Tsurusaki, K. Tyler, J. Varlotta, A. Vassiliev, V. V. Vincent, S. Vivier, M. Wakely, S. P. Ward, J. E. Weekes, T. C. Weinstein, A. Weisgarber, T. Williams, D. A. Zitzer, B. TI VERITAS OBSERVATIONS OF DAY-SCALE FLARING OF M 87 IN 2010 APRIL SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: individual (M 87, VER J1230+123); gamma rays: galaxies ID GAMMA-RAY EMISSION; SUPERMASSIVE BLACK-HOLE; RADIO GALAXY M87; TEV EMISSION; JET; VARIABILITY; TELESCOPE; HST-1; BLAZAR; AGNS AB VERITAS has been monitoring the very-high-energy (VHE; > 100 GeV) gamma-ray activity of the radio galaxy M87 since 2007. During 2008, flaring activity on a timescale of a few days was observed with a peak flux of (0.70 +/- 0.16) x 10(-11) cm(-2) s(-1) at energies above 350 GeV. In 2010 April, VERITAS detected a flare from M 87 with peak flux of (2.71 +/- 0.68) x 10(-11) cm(-2) s(-1) for E > 350 GeV. The source was observed for six consecutive nights during the flare, resulting in a total of 21 hr of good-quality data. The most rapid flux variation occurred on the trailing edge of the flare with an exponential flux decay time of 0.90(-0.15)(+0.22) days. The shortest detected exponential rise time is three times as long, at 2.87(+1.65)(-0.99) days. The quality of the data sample is such that spectral analysis can be performed for three periods: rising flux, peak flux, and falling flux. The spectra obtained are consistent with power-law forms. The spectral index at the peak of the flare is equal to 2.19 +/- 0.07. There is some indication that the spectrum is softer in the falling phase of the flare than the peak phase, with a confidence level corresponding to 3.6 standard deviations. We discuss the implications of these results for the acceleration and cooling rates of VHE electrons in M 87 and the constraints they provide on the physical size of the emitting region. C1 [Aliu, E.; Errando, M.; Mukherjee, R.] Columbia Univ Barnard Coll, Dept Phys & Astron, New York, NY 10027 USA. [Arlen, T.; Majumdar, P.; Ong, R. A.; Vassiliev, V. V.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. [Aune, T.; Bouvier, A.; Furniss, A.; Williams, D. A.] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Santa Cruz, CA 95064 USA. [Aune, T.; Bouvier, A.; Furniss, A.; Williams, D. A.] Univ Calif Santa Cruz, Dept Phys, Santa Cruz, CA 95064 USA. [Beilicke, M.; Buckley, J. H.; Bugaev, V.; Dickherber, R.; Krawczynski, H.; McArthur, S.; Thibadeau, S.] Washington Univ, Dept Phys, St Louis, MO 63130 USA. [Benbow, W.; Galante, N.; Roache, E.; Schroedter, M.; Weekes, T. C.] Harvard Smithsonian Ctr Astrophys, Fred Lawrence Whipple Observ, Amado, AZ 85645 USA. [Bradbury, S. M.; Rose, H. J.] Univ Leeds, Sch Phys & Astron, Leeds LS2 9JT, W Yorkshire, England. [Byrum, K.] Argonne Natl Lab, Argonne, IL 60439 USA. [Cannon, A.; Collins-Hughes, E.; Quinn, J.; Ward, J. E.] Univ Coll Dublin, Sch Phys, Dublin 4, Ireland. [Cesarini, A.; Connolly, M. P.; Lang, M. J.] Natl Univ Ireland Galway, Sch Phys, Galway, Ireland. [Ciupik, L.; Grube, J.; Gyuk, G.] Adler Planetarium & Astron Museum, Dept Astron, Chicago, IL 60605 USA. [Cui, W.; Finley, J. P.; Sembroski, G. H.; Theiling, M.; Varlotta, A.; Zitzer, B.] Purdue Univ, Dept Phys, W Lafayette, IN 47907 USA. [Duke, C.] Grinnell Coll, Dept Phys, Grinnell, IA 50112 USA. [Falcone, A.] Penn State Univ, Dept Astron & Astrophys, Davey Lab 525, University Pk, PA 16802 USA. [Finnegan, G.; Godambe, S.; Hui, C. M.; Kieda, D.; LeBohec, S.; Nunez, P. D.; Vincent, S.] Univ Utah, Dept Phys & Astron, Salt Lake City, UT 84112 USA. [Fortson, L.; Karlsson, N.] Univ Minnesota, Sch Phys & Astron, Minneapolis, MN 55455 USA. [Gall, D.; Kaaret, P.; Tsurusaki, K.] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA. [Griffin, S.; Guenette, R.; Hanna, D.; McCann, A.; Ragan, K.; Staszak, D.; Tesic, G.; Tyler, J.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada. [Holder, J.; Saxon, D. B.; Vivier, M.] Univ Delaware, Dept Phys & Astron, Newark, DE 19716 USA. [Holder, J.; Saxon, D. B.; Vivier, M.] Univ Delaware, Bartol Res Inst, Newark, DE 19716 USA. [Huan, H.; Park, N.; Wakely, S. P.; Weisgarber, T.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA. [Hughes, G.; Maier, G.; Pohl, M.; Prokoph, H.; Ruppel, J.; Skole, C.] DESY, D-15738 Zeuthen, Germany. [Humensky, T. B.; Sentuerk, G. D.] Columbia Univ, Dept Phys, New York, NY 10027 USA. [Imran, A.; Krennrich, F.; Madhavan, A. S.; Orr, M.; Weinstein, A.] Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA. [Kertzman, M.] DePauw Univ, Dept Phys & Astron, Greencastle, IN 46135 USA. [Moriarty, P.] Galway Mayo Inst Technol, Dept Life & Phys Sci, Galway, Ireland. [Otte, A. N.] Georgia Inst Technol, Sch Phys, Atlanta, GA 30332 USA. [Otte, A. N.] Georgia Inst Technol, Ctr Relativist Astrophys, Atlanta, GA 30332 USA. [Perkins, J. S.] CRESST, Greenbelt, MD 20771 USA. [Perkins, J. S.] Astroparticle Phys Lab NASA GSFC, Greenbelt, MD 20771 USA. [Perkins, J. S.] Univ Maryland Baltimore Cty, Baltimore, MD 21250 USA. [Pichel, A.] Inst Astron & Fis Espacio, RA-1428 Buenos Aires, DF, Argentina. [Pohl, M.; Ruppel, J.] Univ Potsdam, Inst Phys & Astron, D-14476 Potsdam, Germany. [Reyes, L. C.] Calif Polytech State Univ San Luis Obispo, Dept Phys, San Luis Obispo, CA 94307 USA. [Reynolds, P. T.] Cork Inst Technol, Dept Appl Phys & Instrumentat, Cork, Ireland. RP Aliu, E (reprint author), Columbia Univ Barnard Coll, Dept Phys & Astron, New York, NY 10027 USA. EM cmhui@physics.utah.edu OI Cui, Wei/0000-0002-6324-5772; Cesarini, Andrea/0000-0002-8611-8610; Lang, Mark/0000-0003-4641-4201 FU U.S. Department of Energy Office of Science; U.S. National Science Foundation; Smithsonian Institution; NSERC in Canada; Science Foundation Ireland (SFI) [10/RFP/AST2748]; STFC in the UK FX This research is supported by grants from the U.S. Department of Energy Office of Science, the U.S. National Science Foundation and the Smithsonian Institution, by NSERC in Canada, by Science Foundation Ireland (SFI 10/RFP/AST2748), and by STFC in the UK. We acknowledge the excellent work of the technical support staff at the Fred Lawrence Whipple Observatory and at the collaborating institutions in the construction and operation of the instrument. NR 40 TC 13 Z9 13 U1 0 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 20 PY 2012 VL 746 IS 2 AR 141 DI 10.1088/0004-637X/746/2/141 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 894DD UT WOS:000300406300027 ER PT J AU Faigler, S Mazeh, T Quinn, SN Latham, DW Tal-Or, L AF Faigler, S. Mazeh, T. Quinn, S. N. Latham, D. W. Tal-Or, L. TI SEVEN NEW BINARIES DISCOVERED IN THE KEPLER LIGHT CURVES THROUGH THE BEER METHOD CONFIRMED BY RADIAL-VELOCITY OBSERVATIONS SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries: spectroscopic; brown dwarfs; methods: data analysis; planets and satellites: detection ID PROPER-MOTION STARS; COMPANIONS; PHOTOMETRY; PLANETS; CATALOG; SYSTEMS AB We present seven newly discovered non-eclipsing short-period binary systems with low-mass companions, identified by the recently introduced BEER algorithm, applied to the publicly available 138-day photometric light curves obtained by the Kepler mission. The detection is based on the beaming effect (sometimes called Doppler boosting), which increases (decreases) the brightness of any light source approaching (receding from) the observer, enabling a prediction of the stellar Doppler radial-velocity (RV) modulation from its precise photometry. The BEER algorithm identifies the BEaming periodic modulation, with a combination of the well-known Ellipsoidal and Reflection/heating periodic effects, induced by short-period companions. The seven detections were confirmed by spectroscopic RV follow-up observations, indicating minimum secondary masses in the range 0.07-0.4 M-circle dot. The binaries discovered establish for the first time the feasibility of the BEER algorithm as a new detection method for short-period non-eclipsing binaries, with the potential to detect in the near future non-transiting brown-dwarf secondaries, or even massive planets. C1 [Faigler, S.; Mazeh, T.; Tal-Or, L.] Tel Aviv Univ, Raymond & Beverly Sackler Fac Exact Sci, Sch Phys & Astron, IL-69978 Tel Aviv, Israel. [Quinn, S. N.; Latham, D. W.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Faigler, S (reprint author), Tel Aviv Univ, Raymond & Beverly Sackler Fac Exact Sci, Sch Phys & Astron, IL-69978 Tel Aviv, Israel. OI Faigler, Simchon/0000-0002-8368-5724 FU NASA [NAS5-26555, NNX11AB99A]; NASA Office of Space Science [NNX09AF08G]; Smithsonian Astrophysical Observatory; Israel Science Foundation [655/07] FX All the photometric data presented in this paper were obtained from the Multimission Archive at the Space Telescope Science Institute (MAST). STScI is operated by the Association of Universities for Research in Astronomy, Inc., under NASA Contract NAS5-26555. Support for MAST for non-HST data is provided by the NASA Office of Space Science via grant NNX09AF08G and by other grants and contracts.; We thank the Kepler mission for partial support of the spectroscopic observations under NASA Cooperative Agreement NNX11AB99A with the Smithsonian Astrophysical Observatory; PI: D. W. L.; This research was supported by the Israel Science Foundation (grant no. 655/07). NR 35 TC 20 Z9 20 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 20 PY 2012 VL 746 IS 2 AR 185 DI 10.1088/0004-637X/746/2/185 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 894DD UT WOS:000300406300071 ER PT J AU Hong, J van den Berg, M Grindlay, JE Servillat, M Zhao, P AF Hong, JaeSub van den Berg, Maureen Grindlay, Jonathan E. Servillat, Mathieu Zhao, Ping TI DISCOVERY OF A SIGNIFICANT MAGNETIC CATACLYSMIC VARIABLE POPULATION IN THE LIMITING WINDOW SO ASTROPHYSICAL JOURNAL LA English DT Article DE Galaxy: bulge; novae, cataclysmic variables; X-rays: binaries ID XMM-NEWTON OBSERVATIONS; X-RAY SOURCES; TIME-SERIES ANALYSIS; INTERMEDIATE POLAR; GALACTIC-CENTER; POINT SOURCES; SPIN PULSE; CHANDRA; ACCRETION; EMISSION AB We have discovered 10 periodic X-ray sources from the 1 Ms Chandra ACIS observation of the Limiting Window (LW), a low-extinction region (A(V) similar to 3.9) at 1 degrees.4 south of the Galactic center. The observed periods (similar to 1.3-3.4 hr) and the X-ray luminosities (10(31.8-32.9) erg s(-1) at 8 kpc) of the 10 periodic sources, combined with the lack of bright optical counterparts and thus high X-ray-to-optical flux ratios, suggest that they are likely accreting binaries, in particular, magnetic cataclysmic variables (MCVs). All of them exhibit a relatively hard X-ray spectrum (Gamma < 2 for a power-law model), and relatively high extinction observed in the X-ray spectra of at least five sources indicates some intrinsic absorption in the system, which is also a typical sign of MCVs. On close inspection, the period distribution of these sources resembles those of polars, whereas the relatively hard spectra suggest that they could be intermediate polars (IPs). These puzzling properties can be explained by unusual polars with buried magnetic fields or a rare sub-class of MCVs, nearly synchronous MCVs. These unusual MCVs may provide important clues in the evolutionary path of MCVs from IPs to polars. The completeness simulation indicates that greater than or similar to 40% of the hard X-ray sources in the LW are periodic. Therefore, this discovery provides a first direct evidence of a large MCV population in the bulge and further supports the current view that MCVs constitute the majority of low-luminosity hard X-ray sources (similar to 10(30-33) erg s(-1)) in the bulge. C1 [Hong, JaeSub; Grindlay, Jonathan E.; Servillat, Mathieu; Zhao, Ping] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [van den Berg, Maureen] Univ Utrecht, Astron Inst, NL-3508 TA Utrecht, Netherlands. RP Hong, J (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM jaesub@head.cfa.harvard.edu FU NASA/Chandra [GO6-7088X, GO7-8090X, GO8-9093X] FX We thank Dr. Silas Laycock for the Magellan/IMACS observation and the initial data processing of the LW. We also thank Dr. Brandon Kelly for suggesting negative binomial distribution. This work is supported in part by NASA/Chandra grants GO6-7088X, GO7-8090X, and GO8-9093X. We also thank Chandra X-ray Center (CXC) for their support in publication. Finally, we thank the anonymous referee for useful comments. NR 71 TC 13 Z9 13 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 20 PY 2012 VL 746 IS 2 AR 165 DI 10.1088/0004-637X/746/2/165 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 894DD UT WOS:000300406300051 ER PT J AU Howell, SB Rowe, JF Bryson, ST Quinn, SN Marcy, GW Isaacson, H Ciardi, DR Chaplin, WJ Metcalfe, TS Monteiro, MJPFG Appourchaux, T Basu, S Creevey, OL Gilliland, RL Quirion, PO Stello, D Kjeldsen, H Christensen-Dalsgaard, J Elsworth, Y Garcia, RA Houdek, G Karoff, C Molenda-Zakowicz, J Thompson, MJ Verner, GA Torres, G Fressin, F Crepp, JR Adams, E Dupree, A Sasselov, DD Dressing, CD Borucki, WJ Koch, DG Lissauer, JJ Latham, DW Buchhave, LA Gautier, TN Everett, M Horch, E Batalha, NM Dunham, EW Szkody, P Silva, DR Mighell, K Holberg, J Ballot, J Bedding, TR Bruntt, H Campante, TL Handberg, R Hekker, S Huber, D Mathur, S Mosser, B Regulo, C White, TR Christiansen, JL Middour, CK Haas, MR Hall, JR Jenkins, JM McCaulif, S Fanelli, MN Kulesa, C McCarthy, D Henze, CE AF Howell, Steve B. Rowe, Jason F. Bryson, Stephen T. Quinn, Samuel N. Marcy, Geoffrey W. Isaacson, Howard Ciardi, David R. Chaplin, William J. Metcalfe, Travis S. Monteiro, Mario J. P. F. G. Appourchaux, Thierry Basu, Sarbani Creevey, Orlagh L. Gilliland, Ronald L. Quirion, Pierre-Olivier Stello, Denis Kjeldsen, Hans Christensen-Dalsgaard, Jorgen Elsworth, Yvonne Garcia, Rafael A. Houdek, Guenter Karoff, Christoffer Molenda-Zakowicz, Joanna Thompson, Michael J. Verner, Graham A. Torres, Guillermo Fressin, Francois Crepp, Justin R. Adams, Elisabeth Dupree, Andrea Sasselov, Dimitar D. Dressing, Courtney D. Borucki, William J. Koch, David G. Lissauer, Jack J. Latham, David W. Buchhave, Lars A. Gautier, Thomas N., III Everett, Mark Horch, Elliott Batalha, Natalie M. Dunham, Edward W. Szkody, Paula Silva, David R. Mighell, Ken Holberg, Jay Ballot, Jerome Bedding, Timothy R. Bruntt, Hans Campante, Tiago L. Handberg, Rasmus Hekker, Saskia Huber, Daniel Mathur, Savita Mosser, Benoit Regulo, Clara White, Timothy R. Christiansen, Jessie L. Middour, Christopher K. Haas, Michael R. Hall, Jennifer R. Jenkins, Jon M. McCaulif, Sean Fanelli, Michael N. Kulesa, Craig McCarthy, Don Henze, Christopher E. TI KEPLER-21b: A 1.6 R-Earth PLANET TRANSITING THE BRIGHT OSCILLATING F SUBGIANT STAR HD 179070 SO ASTROPHYSICAL JOURNAL LA English DT Article DE planetary systems; stars: activity; stars: individual (HD 179070: KIC 3632418); stars: interiors; stars: late-type; stars: magnetic field; stars: oscillations (including pulsations); techniques: photometric ID SOLAR-TYPE STARS; SUN-LIKE STAR; TIMING VARIATIONS; INITIAL CHARACTERISTICS; ASTEROSEISMIC DATA; BLEND SCENARIOS; MULTIPLE SYSTEM; LIGHT CURVES; SUPER-EARTHS; CADENCE DATA AB We present Kepler observations of the bright (V = 8.3), oscillating star HD 179070. The observations show transit-like events which reveal that the star is orbited every 2.8 days by a small, 1.6 R-Earth object. Seismic studies of HD 179070 using short cadence Kepler observations show that HD 179070 has a frequency-power spectrum consistent with solar-like oscillations that are acoustic p-modes. Asteroseismic analysis provides robust values for the mass and radius of HD 179070, 1.34 +/- 0.06 M-circle dot and 1.86 +/- 0.04 R-circle dot, respectively, as well as yielding an age of 2.84 +/- 0.34 Gyr for this F5 subgiant. Together with ground-based follow-up observations, analysis of the Kepler light curves and image data, and blend scenario models, we conservatively show at the >99.7% confidence level (3 sigma) that the transit event is caused by a 1.64 +/- 0.04 R-Earth exoplanet in a 2.785755 +/- 0.000032 day orbit. The exoplanet is only 0.04 AU away from the star and our spectroscopic observations provide an upper limit to its mass of similar to 10 M-Earth (2 sigma). HD 179070 is the brightest exoplanet host star yet discovered by Kepler. C1 [Howell, Steve B.; Everett, Mark; Silva, David R.; Mighell, Ken] Natl Opt Astron Observ, Tucson, AZ 85719 USA. [Middour, Christopher K.; Hall, Jennifer R.; McCaulif, Sean] NASA, Ames Res Ctr, Orbital Sci Corp, Moffett Field, CA 94035 USA. [Fanelli, Michael N.] NASA, Ames Res Ctr, Bay Area Environm Res Inst, Moffett Field, CA 94035 USA. [Rowe, Jason F.; Christiansen, Jessie L.; Jenkins, Jon M.] SETI Inst, Mountain View, CA 94043 USA. [Quinn, Samuel N.; Torres, Guillermo; Fressin, Francois; Adams, Elisabeth; Dupree, Andrea; Sasselov, Dimitar D.; Dressing, Courtney D.; Latham, David W.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Marcy, Geoffrey W.; Isaacson, Howard] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Ciardi, David R.] CALTECH, NASA, Exoplanet Sci Inst, Pasadena, CA 91125 USA. [Chaplin, William J.; Elsworth, Yvonne; Karoff, Christoffer; Verner, Graham A.; Hekker, Saskia] Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England. [Metcalfe, Travis S.; Thompson, Michael J.; Mathur, Savita] Natl Ctr Atmospher Res, High Altitude Observ, Boulder, CO 80307 USA. [Metcalfe, Travis S.; Thompson, Michael J.; Mathur, Savita] Natl Ctr Atmospher Res, Div Comp Sci, Boulder, CO 80307 USA. [Monteiro, Mario J. P. F. G.; Campante, Tiago L.] Univ Porto, Ctr Astrofis, P-4150762 Oporto, Portugal. [Appourchaux, Thierry] Univ Paris 11, CNRS, Inst Astrophys Spatiale, UMR8617, F-91405 Orsay, France. [Basu, Sarbani] Yale Univ, Dept Astron, New Haven, CT 06520 USA. [Creevey, Orlagh L.; Bruntt, Hans; Regulo, Clara] Univ La Laguna, Dept Astrofis, E-38206 Tenerife, Spain. [Creevey, Orlagh L.; Regulo, Clara] Inst Astrofis Canarias, E-38200 Tenerife, Spain. [Gilliland, Ronald L.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Quirion, Pierre-Olivier] Canadian Space Agcy, St Hubert, PQ J3Y 8Y9, Canada. [Stello, Denis; Bedding, Timothy R.; Huber, Daniel; White, Timothy R.] Univ Sydney, Sydney Inst Astron SIfA, Sch Phys, Sydney, NSW 2006, Australia. [Kjeldsen, Hans; Christensen-Dalsgaard, Jorgen; Campante, Tiago L.; Handberg, Rasmus] Aarhus Univ, Dept Phys & Astron, DK-8000 Aarhus C, Denmark. [Garcia, Rafael A.] Univ Paris Diderot, Lab AIM, CEA, DSM,CNRS,IRFU,SAp, F-91191 Gif Sur Yvette, France. [Houdek, Guenter] Univ Vienna, Inst Astron, A-1180 Vienna, Austria. [Molenda-Zakowicz, Joanna] Univ Wroclaw, Astron Inst, PL-51622 Wroclaw, Poland. [Verner, Graham A.] Univ London, Astron Unit, London E1 4NS, England. [Buchhave, Lars A.] Univ Copenhagen, Niels Bohr Inst, DK-2100 Copenhagen, Denmark. [Crepp, Justin R.] CALTECH, Dept Astrophys, Pasadena, CA 91125 USA. [Gautier, Thomas N., III] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Horch, Elliott] So Connecticut State Univ, Dept Phys, New Haven, CT 06515 USA. [Batalha, Natalie M.] San Jose State Univ, Dept Phys & Astron, San Jose, CA 95192 USA. [Dunham, Edward W.] Lowell Observ, Flagstaff, AZ 86001 USA. [Szkody, Paula] Univ Washington, Dept Astron, Seattle, WA USA. [Holberg, Jay] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85726 USA. [Ballot, Jerome] Univ Toulouse, Lab Astrophys Toulouse Tarbes, CNRS, F-31400 Toulouse, France. [Mosser, Benoit] Univ Paris 07, Univ Paris 06, LESIA, CNRS,Observ Paris, F-92195 Meudon, France. [Kulesa, Craig; McCarthy, Don] Univ Arizona, Steward Observ, Tucson, AZ 85726 USA. [Buchhave, Lars A.] Univ Copenhagen, Ctr Star & Planet Format, Nat Hist Museum Denmark, DK-1350 Copenhagen, Denmark. RP Howell, SB (reprint author), Natl Opt Astron Observ, Tucson, AZ 85719 USA. RI Ballot, Jerome/G-1019-2010; Monteiro, Mario J.P.F.G./B-4715-2008; Karoff, Christoffer/L-1007-2013; OI Monteiro, Mario J.P.F.G./0000-0003-0513-8116; Karoff, Christoffer/0000-0003-2009-7965; Buchhave, Lars A./0000-0003-1605-5666; Bedding, Timothy/0000-0001-5943-1460; Basu, Sarbani/0000-0002-6163-3472 FU National Aeronautics and Space Administration FX We thank John Johnson for use of some of his Keck Time. This research has made use of the NASA/IPAC/NExScI Star and Exoplanet Database, which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. The authors thank the Kepler Science Office and the Science Operations Center personal for their dedicated effort to the mission and for providing us access to the science office data products. The ground-based observations reported on herein were obtained at Kitt Peak National Observatory, 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. Kepler was selected as the 10th mission of the Discovery Program. Funding for this mission is provided by NASA. NR 90 TC 73 Z9 73 U1 1 U2 10 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 20 PY 2012 VL 746 IS 2 AR 123 DI 10.1088/0004-637X/746/2/123 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 894DD UT WOS:000300406300009 ER PT J AU Longmore, SN Rathborne, J Bastian, N Alves, J Ascenso, J Bally, J Testi, L Longmore, A Battersby, C Bressert, E Purcell, C Walsh, A Jackson, J Foster, J Molinari, S Meingast, S Amorim, A Lima, J Marques, R Moitinho, A Pinhao, J Rebordao, J Santos, FD AF Longmore, Steven N. Rathborne, Jill Bastian, Nate Alves, Joao Ascenso, Joana Bally, John Testi, Leonardo Longmore, Andy Battersby, Cara Bressert, Eli Purcell, Cormac Walsh, Andrew Jackson, James Foster, Jonathan Molinari, Sergio Meingast, Stefan Amorim, A. Lima, J. Marques, R. Moitinho, A. Pinhao, J. Rebordao, J. Santos, F. D. TI G0.253+0.016: A MOLECULAR CLOUD PROGENITOR OF AN ARCHES-LIKE CLUSTER SO ASTROPHYSICAL JOURNAL LA English DT Article DE evolution; Galaxy: center; open clusters and associations: general; stars: formation; stars: massive; stars: protostars ID GALACTIC PLANE SURVEY; INFRARED DARK CLOUDS; MASS PROTOSTELLAR CANDIDATES; SUPER-STAR-CLUSTERS; STELLAR CLUSTERS; INTERSTELLAR-MEDIUM; METHANOL MASERS; DUST CONTINUUM; YOUNG CLUSTERS; RING SURVEY AB Young massive clusters (YMCs) with stellar masses of 10(4)-10(5) M-circle dot and core stellar densities of 10(4)-10(5) stars per cubic pc are thought to be the "missing link" between open clusters and extreme extragalactic super star clusters and globular clusters. As such, studying the initial conditions of YMCs offers an opportunity to test cluster formation models across the full clustermass range. G0.253 + 0.016 is an excellent candidate YMC progenitor. We make use of existing multi-wavelength data including recently available far-IR continuum (Herschel/Herschel Infrared Galactic Plane Survey) and mm spectral line (H2O Southern Galactic Plane Survey and Millimetre Astronomy Legacy Team 90 GHz Survey) data and present new, deep, multiple-filter, near-IR (Very Large Telescope/NACO) observations to study G0.253 + 0.016. These data show that G0.253 + 0.016 is a high-mass (1.3 x 10(5) M-circle dot), low-temperature (T-dust similar to 20 K), high-volume, and column density (n similar to 8 x 10(4) cm(-3); N-H2 similar to 4 x 10(23) cm(-2)) molecular clump which is close to virial equilibrium (M-dust similar to M-virial) so is likely to be gravitationally bound. It is almost devoid of star formation and, thus, has exactly the properties expected for the initial conditions of a clump that may form an Arches-like massive cluster. We compare the properties of G0.253 + 0.016 to typical Galactic cluster-forming molecular clumps and find it is extreme, and possibly unique in the Galaxy. This uniqueness makes detailed studies of G0.253 + 0.016 extremely important for testing massive cluster formation models. C1 [Longmore, Steven N.; Ascenso, Joana; Testi, Leonardo; Bressert, Eli] European So Observ, D-85748 Garching, Germany. [Longmore, Steven N.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Rathborne, Jill] CSIRO Astron & Space Sci, Sydney, NSW, Australia. [Bastian, Nate] Excellence Cluster Universe, D-85748 Garching, Germany. [Alves, Joao; Meingast, Stefan] Univ Vienna, Inst Astron, A-1180 Vienna, Austria. [Bally, John; Battersby, Cara] Univ Colorado, Ctr Astrophys & Space Astron, Boulder, CO 80309 USA. [Longmore, Andy] Royal Observ, UK Astron Technol Ctr, Edinburgh EH9 3HJ, Midlothian, Scotland. [Bressert, Eli] Univ Exeter, Sch Phys, Exeter EX4 4QL, Devon, England. [Purcell, Cormac] Univ Leeds, Sch Phys & Astron, Leeds LS2 9JT, W Yorkshire, England. [Purcell, Cormac] Univ Sydney, Sch Phys, Sydney Inst Astron SiFA, Sydney, NSW 2006, Australia. [Walsh, Andrew] James Cook Univ, Dept Astron, Townesville, Australia. [Jackson, James; Foster, Jonathan] Boston Univ, Inst Astrophys Res, Boston, MA 02215 USA. [Molinari, Sergio] INAF Ist Fis Spazio Interplanetario, I-00133 Rome, Italy. [Amorim, A.; Lima, J.; Marques, R.; Moitinho, A.; Santos, F. D.] Univ Lisbon, SIM, Fac Ciencias, P-1749016 Lisbon, Portugal. [Pinhao, J.] Univ Coimbra, LIP Coimbra, Dept Phys, P-3004516 Coimbra, Portugal. [Rebordao, J.] CAAUL FCUL, P-1649038 Lisbon, Portugal. RP Longmore, SN (reprint author), European So Observ, Karl Schwarzschild Str 2, D-85748 Garching, Germany. EM slongmor@eso.org RI Walsh, Andrew/B-5627-2013; Santos, Filipe/M-7709-2013; Rebordao, Jose Manuel/M-3269-2013; Moitinho de Almeida, Andre/L-1624-2015; Molinari, Sergio/O-4095-2016 OI Purcell, Cormac/0000-0002-7491-7386; Amorim, Antonio/0000-0003-0638-2321; Meingast, Stefan/0000-0002-0568-5526; Alves, Joao/0000-0002-4355-0921; Walsh, Andrew/0000-0001-9506-0855; Bressert, Eli/0000-0002-6564-6182; Santos, Filipe/0000-0001-7316-1479; Rebordao, Jose Manuel/0000-0002-7418-0345; Moitinho de Almeida, Andre/0000-0003-0822-5995; Molinari, Sergio/0000-0002-9826-7525 NR 91 TC 65 Z9 65 U1 1 U2 7 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD FEB 20 PY 2012 VL 746 IS 2 AR 117 DI 10.1088/0004-637X/746/2/117 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 894DD UT WOS:000300406300003 ER PT J AU Ragan, SE Heitsch, F Bergin, EA Wilner, D AF Ragan, Sarah E. Heitsch, Fabian Bergin, Edwin A. Wilner, David TI VERY LARGE ARRAY OBSERVATIONS OF AMMONIA IN INFRARED-DARK CLOUDS. II. INTERNAL KINEMATICS SO ASTROPHYSICAL JOURNAL LA English DT Article DE Galaxy: structure; ISM: clouds; ISM: kinematics and dynamics; radio lines: ISM; stars: formation; techniques: interferometric; techniques: spectroscopic ID MASSIVE STAR-FORMATION; DENSE CORES; MOLECULAR CLOUDS; NH3 OBSERVATIONS; GRAVITATIONAL-INSTABILITY; INTERSTELLAR CLOUDS; PHYSICAL-PROPERTIES; INITIAL CONDITIONS; TURBULENT; PERSEUS AB Infrared-dark clouds (IRDCs) are believed to be the birthplaces of rich clusters and thus contain the earliest phases of high-mass star formation. We use the Green Bank Telescope and Very Large Array maps of ammonia (NH3) in six IRDCs to measure their column density and temperature structure (Paper 1), and here, we investigate the kinematic structure and energy content. We find that IRDCs overall display organized velocity fields, with only localized disruptions due to embedded star formation. The local effects seen in NH3 emission are not high-velocity outflows but rather moderate (few km s(-1)) increases in the linewidth that exhibit maxima near or coincident with the mid-infrared emission tracing protostars. These linewidth enhancements could be the result of infall or (hidden in NH3 emission) outflow. Not only is the kinetic energy content insufficient to support the IRDCs against collapse, but also the spatial energy distribution is inconsistent with a scenario of turbulent cloud support. We conclude that the velocity signatures of the IRDCs in our sample are due to active collapse and fragmentation, in some cases augmented by local feedback from stars. C1 [Ragan, Sarah E.; Bergin, Edwin A.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Ragan, Sarah E.] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Heitsch, Fabian] Univ N Carolina, Dept Phys & Astron, Chapel Hill, NC 27599 USA. [Wilner, David] Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Ragan, SE (reprint author), Univ Michigan, Dept Astron, 830 Dennison Bldg,500 Church St, Ann Arbor, MI 48109 USA. EM ragan@mpia.de OI Ragan, Sarah/0000-0003-4164-5588 FU National Science Foundation [0707777, AST-0807305] FX The authors thank the anonymous referee for comments which greatly improved the manuscript. S.R. is grateful to Lee Hartmann and Fred Adams for useful discussions. This work was supported by the National Science Foundation under Grant 0707777. F.H. acknowledges support by NSF grant AST-0807305. NR 51 TC 23 Z9 23 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 20 PY 2012 VL 746 IS 2 AR 174 DI 10.1088/0004-637X/746/2/174 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 894DD UT WOS:000300406300060 ER PT J AU Reeves, KK Gibson, SE Kucera, TA Hudson, HS Kano, R AF Reeves, Katharine K. Gibson, Sarah E. Kucera, Therese A. Hudson, Hugh S. Kano, Ryouhei TI THERMAL PROPERTIES OF A SOLAR CORONAL CAVITY OBSERVED WITH THE X-RAY TELESCOPE ON HINODE SO ASTROPHYSICAL JOURNAL LA English DT Article DE Sun: corona; Sun: filaments, prominences ID WHOLE SUN MONTH; PROMINENCES; DENSITIES; XRT; SPECTROMETER; TEMPERATURES; TOMOGRAPHY; MISSION; CORE AB Coronal cavities are voids in coronal emission often observed above high latitude filament channels. Sometimes, these cavities have areas of bright X-ray emission in their centers. In this study, we use data from the X-ray Telescope (XRT) on the Hinode satellite to examine the thermal emission properties of a cavity observed during 2008 July that contains bright X-ray emission in its center. Using ratios of XRT filters, we find evidence for elevated temperatures in the cavity center. The area of elevated temperature evolves from a ring-shaped structure at the beginning of the observation, to an elongated structure two days later, finally appearing as a compact round source four days after the initial observation. We use a morphological model to fit the cavity emission, and find that a uniform structure running through the cavity does not fit the observations well. Instead, the observations are reproduced by modeling several short cylindrical cavity "cores" with different parameters on different days. These changing core parameters may be due to some observed activity heating different parts of the cavity core at different times. We find that core temperatures of 1.75 MK, 1.7 MK, and 2.0 MK (for July 19, July 21, and July 23, respectively) in the model lead to structures that are consistent with the data, and that line-of-sight effects serve to lower the effective temperature derived from the filter ratio. C1 [Reeves, Katharine K.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Gibson, Sarah E.] HAO NCAR, Boulder, CO 80307 USA. [Kucera, Therese A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Hudson, Hugh S.] Univ Calif Berkeley, Space Sci Labs, Berkeley, CA 94720 USA. [Hudson, Hugh S.] Univ Glasgow, Sch Phys & Astron, Glasgow G12 8QQ, Lanark, Scotland. [Kano, Ryouhei] Natl Inst Nat Sci, Natl Astron Observ Japan, Mitaka, Tokyo 1818588, Japan. RP Reeves, KK (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS 58, Cambridge, MA 02138 USA. EM kreeves@cfa.harvard.edu RI Kucera, Therese/C-9558-2012; Reeves, Katharine/P-9163-2014; OI Kucera, Therese/0000-0001-9632-447X FU International Space Science Institute (ISSI); NASA [NNM07AB07C]; National Science Foundation FX The authors thank the anonymous referee, whose insightful comments helped improve the paper, and Yuhong Fan for useful discussions. The authors also thank the International Space Science Institute (ISSI) for funding a Working Group on Coronal Cavities, where this work began. K. K. Reeves is supported under contract NNM07AB07C from NASA to SAO. T. Kucera is supported by an award from the NASA SHP Program. The National Center for Atmospheric Research is sponsored by the National Science Foundation. Hinode is a Japanese mission developed and launched by ISAS/JAXA, with NAOJ as domestic partner and NASA and STFC (UK) as international partners. It is operated by these agencies in cooperation with ESA and NSC (Norway). SoHO is a project of international collaboration between ESA and NASA. The STEREO/SECCHI data used here are produced by an international consortium of the Naval Research Laboratory (USA), Lockheed Martin Solar and Astrophysics Lab (USA), NASA Goddard Space Flight Center (USA) Rutherford Appleton Laboratory (UK), University of Birmingham (UK), Max-Planck-Institut fur Sonnensystemforschung (Germany), Centre Spatiale de Liege (Belgium), Institut d'Optique Theorique et Appliquee (France), and Institut d'Astrophysique Spatiale (France). NR 31 TC 19 Z9 19 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 20 PY 2012 VL 746 IS 2 AR 146 DI 10.1088/0004-637X/746/2/146 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 894DD UT WOS:000300406300032 ER PT J AU Saglia, RP Tonry, JL Bender, R Greisel, N Seitz, S Senger, R Snigula, J Phleps, S Wilman, D Bailer-Jones, CAL Klement, RJ Rix, HW Smith, K Green, PJ Burgett, WS Chambers, KC Heasley, JN Kaiser, N Magnier, EA Morgan, JS Price, PA Stubbs, CW Wainscoat, RJ AF Saglia, R. P. Tonry, J. L. Bender, R. Greisel, N. Seitz, S. Senger, R. Snigula, J. Phleps, S. Wilman, D. Bailer-Jones, C. A. L. Klement, R. J. Rix, H. -W. Smith, K. Green, P. J. Burgett, W. S. Chambers, K. C. Heasley, J. N. Kaiser, N. Magnier, E. A. Morgan, J. S. Price, P. A. Stubbs, C. W. Wainscoat, R. J. TI THE PHOTOMETRIC CLASSIFICATION SERVER FOR Pan-STARRS1 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: active; galaxies: distances and redshifts; stars: general; surveys ID DIGITAL SKY SURVEY; VLT DEEP SURVEY; SPECTROSCOPIC TARGET SELECTION; SYNTHETIC GALAXY SPECTRA; SUPPORT VECTOR MACHINES; DATA RELEASE; UNRESOLVED GALAXIES; REDSHIFT SURVEY; COSMOS FIELD; QUASARS AB The Pan-STARRS1 survey is obtaining multi-epoch imaging in five bands (g(P1)r(P1)i(P1)z(P1)y(P1)) over the entire sky north of declination -30 deg. We describe here the implementation of the Photometric Classification Server (PCS) for Pan-STARRS1. PCS will allow the automatic classification of objects into star/galaxy/quasar classes based on colors and the measurement of photometric redshifts for extragalactic objects, and will constrain stellar parameters for stellar objects, working at the catalog level. We present tests of the system based on high signal-to-noise photometry derived from the Medium-Deep Fields of Pan-STARRS1, using available spectroscopic surveys as training and/or verification sets. We show that the Pan-STARRS1 photometry delivers classifications and photometric redshifts as good as the Sloan Digital Sky Survey (SDSS) photometry to the same magnitude limits. In particular, our preliminary results, based on this relatively limited data set down to the SDSS spectroscopic limits, and therefore potentially improvable, show that stars are correctly classified as such in 85% of cases, galaxies in 97%, and QSOs in 84%. False positives are less than 1% for galaxies, approximate to 19% for stars, and approximate to 28% for QSOs. Moreover, photometric redshifts for 1000 luminous red galaxies up to redshift 0.5 are determined to 2.4% precision (defined as 1.48 x Median vertical bar z(phot) - z(spec)vertical bar/(1 + z)) with just 0.4% catastrophic outliers and small (-0.5%) residual bias. For bluer galaxies up to the same redshift, the residual bias (on average -0.5%) trend, percentage of catastrophic failures (1.2%), and precision (4.2%) are higher, but still interestingly small for many science applications. Good photometric redshifts (to 5%) can be obtained for at most 60% of the QSOs of the sample. PCS will create a value-added catalog with classifications and photometric redshifts for eventually many millions of sources. C1 [Saglia, R. P.; Bender, R.; Seitz, S.; Senger, R.; Snigula, J.; Phleps, S.; Wilman, D.] Max Planck Inst Extraterr Phys, D-85741 Garching, Germany. [Saglia, R. P.; Bender, R.; Greisel, N.; Seitz, S.] Univ Munich, Univ Observ Munich, D-81679 Munich, Germany. [Tonry, J. L.; Burgett, W. S.; Chambers, K. C.; Heasley, J. N.; Kaiser, N.; Magnier, E. A.; Morgan, J. S.; Wainscoat, R. J.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Bailer-Jones, C. A. L.; Klement, R. J.; Rix, H. -W.; Smith, K.] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Klement, R. J.] Univ Wurzburg, Dept Radiat Oncol, D-97080 Wurzburg, Germany. [Green, P. J.; Stubbs, C. W.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Price, P. A.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. RP Saglia, RP (reprint author), Max Planck Inst Extraterr Phys, Giessenbachstr,Postfach 1312, D-85741 Garching, Germany. RI Stubbs, Christopher/C-2829-2012; OI Stubbs, Christopher/0000-0003-0347-1724; Klement, Rainer/0000-0003-1401-4270; Greisel, Natascha/0000-0002-4907-6247; Wilman, David/0000-0002-1822-4462; Chambers, Kenneth /0000-0001-6965-7789 FU National Aeronautics and Space Administration through the Planetary Science Division of the NASA Science Mission Directorate [NNX08AR22G]; National Science Foundation [AST-1009749] FX The Pan-STARRS1 survey has been made possible through contributions of the Institute for Astronomy; the University of Hawaii; the Pan-STARRS Project Office; the Max-Planck Society and its participating institutes; the Max Planck Institute for Astronomy, Heidelberg, and the Max Planck Institute for Extraterrestrial Physics, Garching; The Johns Hopkins University; Durham University; the University of Edinburgh; Queen's University Belfast; the Harvard-Smithsonian Center for Astrophysics; and the Las Cumbres Observatory Global Telescope Network, Incorporated; the National Central University of Taiwan; and the National Aeronautics and Space Administration under grant no. NNX08AR22G issued through the Planetary Science Division of the NASA Science Mission Directorate. Partial support for this work was provided by National Science Foundation grant AST-1009749. NR 62 TC 22 Z9 23 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 20 PY 2012 VL 746 IS 2 AR 128 DI 10.1088/0004-637X/746/2/128 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 894DD UT WOS:000300406300014 ER PT J AU Sand, DJ Graham, ML Bildfell, C Zaritsky, D Pritchet, C Hoekstra, H Just, DW Herbert-Fort, S Sivanandam, S Foley, RJ Mahdavi, A AF Sand, David J. Graham, Melissa L. Bildfell, Chris Zaritsky, Dennis Pritchet, Chris Hoekstra, Henk Just, Dennis W. Herbert-Fort, Stephane Sivanandam, Suresh Foley, Ryan J. Mahdavi, Andisheh TI THE MULTI-EPOCH NEARBY CLUSTER SURVEY: TYPE Ia SUPERNOVA RATE MEASUREMENT IN z similar to 0.1 CLUSTERS AND THE LATE-TIME DELAY TIME DISTRIBUTION SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: clusters: general; supernovae: general ID REDSHIFT GALAXY CLUSTERS; FRANCE-HAWAII-TELESCOPE; K-CORRECTIONS; STAR-FORMATION; LEGACY SURVEY; MASS; PROGENITORS; LUMINOSITY; EVOLUTION; SPECTROGRAPH AB We describe the Multi-Epoch Nearby Cluster Survey, designed to measure the cluster Type Ia supernova (SN Ia) rate in a sample of 57 X-ray selected galaxy clusters, with redshifts of 0.05 < z < 0.15. Utilizing our real-time analysis pipeline, we spectroscopically confirmed twenty-three cluster SNe Ia, four of which were intracluster events. Using our deep Canada-France-Hawaii Telescope/MegaCam imaging, we measured total stellar luminosities in each of our galaxy clusters, and we performed detailed supernova (SN) detection efficiency simulations. Bringing these ingredients together, we measure an overall cluster SN Ia rate within R-200 (1 Mpc) of 0.042(-0.010-0.008)(+0.012+0.010) SNuM (0.049(-0.014-0.004)(+0.016-0.005) SNuM) and an SN Ia rate within red-sequence galaxies of 0.041(-0.015-0.010)(+0.015+0.005) SNuM (0.041(-0.015-0.004)(+0.019+0.005) SNuM). The red-sequence SN Ia rate is consistent with published rates in early-type/elliptical galaxies in the "field." Using our red-sequence SN Ia rate, and other cluster SN measurements in early-type galaxies up to z similar to 1, we derive the late-time (> 2 Gyr) delay time distribution (DTD) of SN Ia assuming a cluster early-type galaxy star formation epoch of z(f) = 3. Assuming a power-law form for the DTD, Psi(t) proportional to t(s), we find s = -1.62 +/- 0.54. This result is consistent with predictions for the double degenerate SN Ia progenitor scenario (s similar to -1) and is also in line with recent calculations for the double detonation explosion mechanism (s similar to -2). The most recent calculations of the single degenerate scenario DTD predicts an order-of-magnitude drop-off in SN Ia rate similar to 6-7 Gyr after stellar formation, and the observed cluster rates cannot rule this out. C1 [Sand, David J.; Graham, Melissa L.] Las Cumbres Observ Global Telescope Network, Santa Barbara, CA 93117 USA. [Sand, David J.; Graham, Melissa L.] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA. [Bildfell, Chris; Pritchet, Chris] Univ Victoria, Dept Phys & Astron, STN CSC, Victoria, BC V8W 3P6, Canada. [Zaritsky, Dennis; Just, Dennis W.; Herbert-Fort, Stephane] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Hoekstra, Henk] Leiden Univ, Leiden Observ, NL-2333 CA Leiden, Netherlands. [Sivanandam, Suresh] Dunlap Inst Astron & Astrophys, Toronto, ON M5S 3H4, Canada. [Foley, Ryan J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Mahdavi, Andisheh] San Francisco State Univ, Dept Phys & Astron, San Francisco, CA 94132 USA. EM dsand@lcogt.net OI Hoekstra, Henk/0000-0002-0641-3231 FU National Aeronautics and Space Administration; NRC; CNRS; Canada-France-Hawaii Telescope (CFHT); NSF [GN-2009A-Q-10, GN-2008B-Q-3] FX We are extremely grateful to the operators of the CFHT queue without whom this project would not be possible. We thank Nelson Caldwell for managing the MMT/Hectospec queue. We are grateful to Stephenson Yang for his patience and diligence regarding computer and network maintenance. H. H. acknowledges support from a Marie Curie International Reintegration Grant. This research has made use of the VizieR catalog access tool, CDS, Strasbourg, France. This research has made use of the NASA/IPAC Extragalactic Database (NED) which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration.; This work is based in part on data products produced at the Canadian Astronomy Data Centre as part of the Canada-France-Hawaii Telescope Legacy Survey, a collaborative project of NRC and CNRS.; This work is based on observations obtained with MegaPrime/MegaCam, a joint project of CFHT and CEA/DAPNIA, at the Canada-France-Hawaii Telescope (CFHT) which is operated by the National Research Council (NRC) of Canada, the Institut National des Science de l'Univers of the Centre National de la Recherche Scientifique (CNRS) of France, and the University of Hawaii.; This work is based on observations obtained at the Gemini Observatory (under program IDs GN-2009A-Q-10 and GN-2008B-Q-3), which is operated by the Association of Universities for Research in Astronomy, Inc., under a cooperative agreement with the NSF on behalf of the Gemini partnership: the National Science Foundation (United States), the Science and Technology Facilities Council (United Kingdom), the National Research Council (Canada), CONICYT (Chile), the Australian Research Council (Australia), Ministerio da Ciencia e Tecnologia (Brazil), and Ministerio de Ciencia, Tecnologia e Innovacion Productiva (Argentina). NR 82 TC 25 Z9 25 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 20 PY 2012 VL 746 IS 2 AR 163 DI 10.1088/0004-637X/746/2/163 PG 22 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 894DD UT WOS:000300406300049 ER PT J AU Shen, Y Kelly, BC AF Shen, Yue Kelly, Brandon C. TI THE DEMOGRAPHICS OF BROAD-LINE QUASARS IN THE MASS-LUMINOSITY PLANE. I. TESTING FWHM-BASED VIRIAL BLACK HOLE MASSES SO ASTROPHYSICAL JOURNAL LA English DT Article DE black hole physics; galaxies: active; quasars: general; surveys ID ACTIVE GALACTIC NUCLEI; DIGITAL-SKY-SURVEY; HIGH-REDSHIFT QUASARS; REVERBERATION MAPPING DATA; AGN MONITORING PROJECT; FALL EQUATORIAL STRIPE; HOST-GALAXY STARLIGHT; SINGLE-EPOCH SPECTRA; MS SOURCE CATALOGS; SIMILAR-TO 4 AB We jointly constrain the luminosity function (LF) and black hole mass function (BHMF) of broad-line quasars with forward Bayesian modeling in the quasar mass-luminosity plane, based on a homogeneous sample of similar to 58,000 Sloan Digital Sky Survey (SDSS) Data Release 7 quasars at z similar to 0.3-5. We take into account the selection effect of the sample flux limit; more importantly, we deal with the statistical scatter between true BH masses and FWHM-based single-epoch virial mass estimates, as well as potential luminosity-dependent biases of these mass estimates. The LF is tightly constrained in the regime sampled by SDSS and makes reasonable predictions when extrapolated to similar to 3 mag fainter. Downsizing is seen in the model LF. On the other hand, we find it difficult to constrain the BHMF to within a factor of a few at z greater than or similar to 0.7 (with Mg II and C IV-based virial BH masses). This is mainly driven by the unknown luminosity-dependent bias of these mass estimators and its degeneracy with other model parameters, and secondly driven by the fact that SDSS quasars only sample the tip of the active BH population at high redshift. Nevertheless, the most likely models favor a positive luminosity-dependent bias for Mg II and possibly for C IV, such that at fixed true BH mass, objects with higher-than-average luminosities have overestimated FWHM-based virial masses. There is tentative evidence that downsizing also manifests itself in the active BHMF, and the BH mass density in broad-line quasars contributes an insignificant amount to the total BH mass density at all times. Within our model uncertainties, we do not find a strong BH mass dependence of the mean Eddington ratio, but there is evidence that the mean Eddington ratio (at fixed BH mass) increases with redshift. C1 [Shen, Yue; Kelly, Brandon C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Shen, Y (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. FU Alfred P. Sloan Foundation; National Science Foundation; U.S. Department of Energy; National Aeronautics and Space Administration [NAS 5-26555]; Japanese Monbukagakusho; Max Planck Society; Higher Education Funding Council for England; Smithsonian Astrophysical Observatory (SAO); NASA through Space Telescope Science Institute [HF-51243.01] FX Funding for SDSS and SDSS-II has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, the U.S. Department of Energy, the National Aeronautics and Space Administration, the Japanese Monbukagakusho, the Max Planck Society, and the Higher Education Funding Council for England. The SDSS Web Site is http://www.sdss.org/.; We thank the referee for suggestions that led to improvement of the manuscript, and Brad Peterson, Gordon Richards, Marianne Vestergaard, Youjun Lu, Qingjuan Yu, and Francesco Shankar for useful comments on the draft. We also acknowledge Michael Strauss, Xin Liu, Scott Tremaine, and Subo Dong for helpful discussions during early stages of this work. Y.S. acknowledges support from a Clay Postdoctoral Fellowship through the Smithsonian Astrophysical Observatory (SAO). B. K. acknowledges support by NASA through Hubble Fellowship Grant HF-51243.01 awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., for NASA, under contract NAS 5-26555. NR 140 TC 46 Z9 47 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 20 PY 2012 VL 746 IS 2 AR 169 DI 10.1088/0004-637X/746/2/169 PG 22 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 894DD UT WOS:000300406300055 ER PT J AU Tsai, MC Hwang, CY Matsushita, S Baker, AJ Espada, D AF Tsai, Mengchun Hwang, Chorng-Yuan Matsushita, Satoki Baker, Andrew J. Espada, Daniel TI INTERFEROMETRIC CO(3-2) OBSERVATIONS TOWARD THE CENTRAL REGION OF NGC 1068 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: active; galaxies: individual (NGC 1068); galaxies: ISM; galaxies: nuclei; galaxies: Seyfert ID SEYFERT 2 GALAXY; ACTIVE GALACTIC NUCLEUS; MOLECULAR GAS CHEMISTRY; STAR-FORMATION RATE; CO J=3-2 EMISSION; NEARBY GALAXIES; PHYSICAL CONDITIONS; DENSE GAS; LINE OBSERVATIONS; MILLIMETER ARRAY AB We present CO(3-2) interferometric observations of the central region of the Seyfert 2 galaxy NGC 1068 using the Submillimeter Array, together with CO(1-0) data taken with the Owens Valley Radio Observatory Millimeter Array. Both the CO(3-2) and CO(1-0) emission lines are mainly distributed within similar to 5 arcsec of the nucleus and along the spiral arms, but the intensity distributions show differences: the CO(3-2) map peaks in the nucleus, while the CO(1-0) emission is mainly located along the spiral arms. The CO(3-2)/CO(1-0) ratio is about 3.1 in the nucleus, which is four times as large as the average line ratio in the spiral arms, suggesting that the molecular gas there must be affected by the radiation arising from the active galactic nucleus. On the other hand, the line ratios in the spiral arms vary over a wide range from 0.24 to 2.34 with an average value around 0.75, which is similar to the line ratios of star formation regions, indicating that the molecular gas is affected by star formation. Besides, we see a tight correlation between CO(3-2)/(1-0) ratios in the spiral arms and star formation rate surface densities derived from Spitzer 8 mu m dust flux densities. We also compare the CO(3-2)/(1-0) ratio and the star formation rate at different positions within the spiral arms; both are found to decrease as the radius from the nucleus increases. C1 [Tsai, Mengchun; Hwang, Chorng-Yuan] Natl Cent Univ, Inst Astron, Chungli, Taiwan. [Matsushita, Satoki; Espada, Daniel] Acad Sinica, Inst Astron & Astrophys, Taipei 10617, Taiwan. [Matsushita, Satoki] Acad Sinica, Inst Astron & Astrophys, Joint ALMA Off, Santiago, Chile. [Baker, Andrew J.] Rutgers State Univ, Dept Phys & Astron, Piscataway, NJ 08854 USA. [Espada, Daniel] CSIC, Inst Astrofis Andalucia, E-18080 Granada, Spain. [Espada, Daniel] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Tsai, MC (reprint author), Natl Cent Univ, Inst Astron, Chungli, Taiwan. FU National Science Council (NSC) of Taiwan [NSC 100-2119-M-008-011-MY3, NSC 99-2112-M-008-014-MY3, NSC 97-2112-M-001-021-MY3]; European Community [MOIF-CT-2006-40298] FX The authors thank an anonymous referee for important suggestions. M. T. and C.Y.H. acknowledge support from the National Science Council (NSC) of Taiwan through grants NSC 100-2119-M-008-011-MY3 and NSC 99-2112-M-008-014-MY3. S. M. acknowledges support from the NSC of Taiwan through grant NSC 97-2112-M-001-021-MY3. D. E. was supported by a Marie Curie International Fellowship within the Sixth European Community Framework Programme (MOIF-CT-2006-40298). NR 95 TC 17 Z9 17 U1 0 U2 7 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 20 PY 2012 VL 746 IS 2 AR 129 DI 10.1088/0004-637X/746/2/129 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 894DD UT WOS:000300406300015 ER PT J AU Wolff, S Dawson, RI Murray-Clay, RA AF Wolff, Schuyler Dawson, Rebekah I. Murray-Clay, Ruth A. TI NEPTUNE ON TIPTOES: DYNAMICAL HISTORIES THAT PRESERVE THE COLD CLASSICAL KUIPER BELT SO ASTROPHYSICAL JOURNAL LA English DT Article DE celestial mechanics; Kuiper belt: general; planets and satellites: dynamical evolution and stability; planets and satellites: individual (Neptune) ID SOLAR-SYSTEM; INCLINATION DISTRIBUTION; PLANETARY MIGRATION; ORIGIN; URANUS; EVOLUTION; OBJECTS; BODIES; ACCRETION; ORBITS AB The current dynamical structure of the Kuiper Belt was shaped by the orbital evolution of the giant planets, especially Neptune, during the era following planet formation when the giant planets may have undergone planet-planet scattering and/or planetesimal-driven migration. Numerical simulations of this process, while reproducing many properties of the Belt, fail to generate the high inclinations and eccentricities observed for some objects while maintaining the observed dynamically "cold" population. We present the first of a three-part parameter study of how different dynamical histories of Neptune sculpt the planetesimal disk. Here we identify which dynamical histories allow an in situ planetesimal disk to remain dynamically cold, becoming today's cold Kuiper Belt population. We find that if Neptune undergoes a period of elevated eccentricity and/or inclination, it secularly excites the eccentricities and inclinations of the planetesimal disk. We demonstrate that there are several well-defined regimes for this secular excitation, depending on the relative timescales of Neptune's migration, the damping of Neptune's orbital inclination and/or eccentricity, and the secular evolution of the planetesimals. We model this secular excitation analytically in each regime, allowing for a thorough exploration of parameter space. Neptune's eccentricity and inclination can remain high for a limited amount of time without disrupting the cold classical belt. In the regime of slow damping and slow migration, if Neptune is located (for example) at 20 AU, then its eccentricity must stay below 0.18 and its inclination below 6 degrees. C1 [Wolff, Schuyler] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Wolff, Schuyler] Western Kentucky Univ, Dept Phys & Astron, Bowling Green, KY 42101 USA. [Dawson, Rebekah I.; Murray-Clay, Ruth A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Wolff, S (reprint author), Johns Hopkins Univ, Dept Phys & Astron, 3400 N Charles St, Baltimore, MD 21218 USA. EM swolff@pha.jhu.edu; rdawson@cfa.harvard.edu; rmurray-clay@cfa.harvard.edu FU National Science Foundation Research Experiences for Undergraduates (REU); Department of Defense [0754568]; National Science Foundation [DGE-1144152]; Smithsonian Institution; Harvard FAS Sciences Division Research Computing Group FX We thank an anonymous referee for helpful comments, including recommending the addition of Section 3.4. S.W. gratefully acknowledges funding by the National Science Foundation Research Experiences for Undergraduates (REU) and the Department of Defense Awards to Stimulate and Support Undergraduate Research Experiences (ASSURE) programs under grant no. 0754568. R.I.D. is supported by a National Science Foundation Graduate Research Fellowship under grant DGE-1144152 and R.M.C. by the Smithsonian Institution. The computations in this paper were run on the Odyssey cluster supported by the Harvard FAS Sciences Division Research Computing Group. NR 47 TC 12 Z9 12 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 20 PY 2012 VL 746 IS 2 AR 171 DI 10.1088/0004-637X/746/2/171 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 894DD UT WOS:000300406300057 ER PT J AU Wright, M Zhao, JH Sandell, G Corder, S Goss, WM Zhu, L AF Wright, Melvyn Zhao, Jun-Hui Sandell, Goeran Corder, Stuartt Goss, W. M. Zhu, Lei TI OBSERVATIONS OF A HIGH-MASS PROTOSTAR IN NGC 7538 S SO ASTROPHYSICAL JOURNAL LA English DT Article DE circumstellar matter; ISM: clouds; stars: formation; stars: pre-main sequence; submillimeter: ISM ID SUBMILLIMETER CONTINUUM OBSERVATIONS; STAR-FORMATION; CIRCUMSTELLAR DISKS; NGC-7538 REGION; ACCRETION DISK; DUST EMISSION; ORION-KL; CORES; OBJECTS; MASERS AB We present high angular resolution continuum observations of the high-mass protostar NGC 7538 S with BIMA and CARMA at 3 and 1.4 mm, Very Large Array (VLA) observations at 1.3, 2, 3.5, and 6 cm, and archive Infrared Array Camera (IRAC) observations from the Spitzer Space Observatory, which detect the star at 4.5, 5.8, and 8 mu m. The star looks rather unremarkable in the mid-IR. The excellent positional agreement of the IRAC source with the VLA free-free emission, the OH, CH3OH, H2O masers, and the dust continuum confirms that this is the most luminous object in the NGC 7538 S core. The continuum emission at millimeter wavelengths is dominated by dust emission from the dense cold cloud core surrounding the protostar. Including all array configurations, the emission is dominated by an elliptical source with a size of similar to 8 '' x 3 ''. If we filter out the extended emission we find three compact millimeter sources inside the elliptical core. The strongest one, S-A, coincides with the VLA/IRAC source and resolves into a double source at 1.4 mm, where we have subarcsecond resolution. The measured spectral index, a, between 3 and 1.4 mm is similar to 2.3, and steeper at longer wavelengths, suggesting a low dust emissivity or that the dust is optically thick. We argue that the dust in these accretion disks is optically thick and estimate a mass of an accretion disk or infalling envelope surrounding S-A to be similar to 60 M-circle dot. C1 [Wright, Melvyn] Univ Calif Berkeley, Radio Astron Lab, Berkeley, CA 94720 USA. [Zhao, Jun-Hui] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Sandell, Goeran] NASA, Ames Res Ctr, SOFIA USRA, Moffett Field, CA 94035 USA. [Corder, Stuartt] Natl Radio Astron Observ, Charlottesville, VA 22903 USA. [Goss, W. M.] Natl Radio Astron Observ, Socorro, NM 87801 USA. [Zhu, Lei] Peking Univ, Dept Astron, Beijing 100871, Peoples R China. RP Wright, M (reprint author), Univ Calif Berkeley, Radio Astron Lab, 601 Campbell Hall, Berkeley, CA 94720 USA. FU National Science Foundation; state of California; state of Illinois; state of Maryland; Gordon and Betty Moore Foundation; Kenneth T. and Eileen L. Norris Foundation; California Institute of Technology; CARMA partner universities FX The BIMA array was operated by the Universities of California (Berkeley), Illinois, and Maryland with support from the National Science Foundation. Support for CARMA construction was derived from the states of California, Illinois, and Maryland, the Gordon and Betty Moore Foundation, the Kenneth T. and Eileen L. Norris Foundation, the Associates of the California Institute of Technology, and the National Science Foundation. Ongoing CARMA development and operations are supported by the National Science Foundation under a cooperative agreement, and by the CARMA partner universities. NR 35 TC 5 Z9 5 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 20 PY 2012 VL 746 IS 2 AR 187 DI 10.1088/0004-637X/746/2/187 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 894DD UT WOS:000300406300073 ER PT J AU King, AL Miller, JM Raymond, J Fabian, AC Reynolds, CS Kallman, TR Maitra, D Cackett, EM Rupen, MP AF King, A. L. Miller, J. M. Raymond, J. Fabian, A. C. Reynolds, C. S. Kallman, T. R. Maitra, D. Cackett, E. M. Rupen, M. P. TI AN EXTREME X-RAY DISK WIND IN THE BLACK HOLE CANDIDATE IGR J17091-3624 SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE accretion, accretion disks; black hole physics; X-rays: binaries ID GALAXY NGC 4051; ACCRETION DISKS; ABSORPTION-LINES; WARM ABSORBERS; GRO J1655-40; OUTBURST; CHANDRA; RADIO; SPECTROSCOPY; OUTFLOWS AB Chandra spectroscopy of transient stellar-mass black holes in outburst has clearly revealed accretion disk winds in soft, disk-dominated states, in apparent anti-correlation with relativistic jets in low/hard states. These disk winds are observed to be highly ionized, dense, and to have typical velocities of similar to 1000 km s(-1) or less projected along our line of sight. Here, we present an analysis of two Chandra High Energy Transmission Grating spectra of the Galactic black hole candidate IGR J17091-3624 and contemporaneous Expanded Very Large Array (EVLA) radio observations, obtained in 2011. The second Chandra observation reveals an absorption line at 6.91 +/- 0.01 keV; associating this line with He-like Fe XXV requires a blueshift of 9300(-400)(+500) km s(-1) (0.03c, or the escape velocity at 1000 R-Schw). This projected outflow velocity is an order of magnitude higher than has previously been observed in stellar-mass black holes, and is broadly consistent with some of the fastest winds detected in active galactic nuclei. A potential feature at 7.32 keV, if due to Fe XXVI, would imply a velocity of similar to 14,600 km s(-1) (0.05c), but this putative feature is marginal. Photoionization modeling suggests that the accretion disk wind in IGR J17091-3624 may originate within 43,300 Schwarzschild radii of the black hole and may be expelling more gas than it accretes. The contemporaneous EVLA observations strongly indicate that jet activity was indeed quenched at the time of our Chandra observations. We discuss the results in the context of disk winds, jets, and basic accretion disk physics in accreting black hole systems. C1 [King, A. L.; Miller, J. M.; Maitra, D.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Raymond, J.] Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Fabian, A. C.; Cackett, E. M.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Reynolds, C. S.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Kallman, T. R.] NASA, High Energy Astrophys Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Cackett, E. M.] Wayne State Univ, Dept Phys & Astron, Detroit, MI 48201 USA. [Rupen, M. P.] Natl Radio Astron Observ, Socorro, NM 87801 USA. RP King, AL (reprint author), Univ Michigan, Dept Astron, 500 Church St, Ann Arbor, MI 48109 USA. EM ashking@umich.edu FU NASA; Chandra Guest Observer program FX We thank the anonymous referee. We thank Michael Nowak for his instrumental help as well. A.L.K. gratefully acknowledges support through the NASA Earth and Space Sciences Fellowship. J.M.M. gratefully acknowledges support through the Chandra Guest Observer program. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. NR 38 TC 49 Z9 49 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 FEB 20 PY 2012 VL 746 IS 2 AR L20 DI 10.1088/2041-8205/746/2/L20 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 896ZT UT WOS:000300611100007 ER PT J AU Winebarger, AR Warren, HP Schmelz, JT Cirtain, J Mulu-Moore, F Golub, L Kobayashi, K AF Winebarger, Amy R. Warren, Harry P. Schmelz, Joan T. Cirtain, Jonathan Mulu-Moore, Fana Golub, Leon Kobayashi, Ken TI DEFINING THE "BLIND SPOT" OF HINODE EIS AND XRT TEMPERATURE MEASUREMENTS SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE Sun: corona ID X-RAY TELESCOPE; DIFFERENTIAL EMISSION MEASURE; ACTIVE-REGION; PLASMA; LINES; DIAGNOSTICS; LOOPS; FLARE AB Observing high-temperature, low emission measure plasma is key to unlocking the coronal heating problem. With current instrumentation, a combination of EUV spectral data from Hinode Extreme-ultraviolet Imaging Spectrometer (EIS; sensitive to temperatures up to 4 MK) and broadband filter data from Hinode X-ray Telescope (XRT; sensitive to higher temperatures) is typically used to diagnose the temperature structure of the observed plasma. In this Letter, we demonstrate that a "blind spot" exists in temperature-emission measure space for combined Hinode EIS and XRT observations. For a typical active region core with significant emission at 3-4 MK, Hinode EIS and XRT are insensitive to plasma with temperatures greater than similar to 6 MK and emission measures less than similar to 10(27) cm(-5). We then demonstrate that the temperature and emission measure limits of this blind spot depend upon the temperature distribution of the plasma along the line of sight by considering a hypothetical emission measure distribution sharply peaked at 1 MK. For this emission measure distribution, we find that EIS and XRT are insensitive to plasma with emission measures less than similar to 10(26) cm(-5). We suggest that a spatially and spectrally resolved 6-24 angstrom spectrum would improve the sensitivity to these high-temperature, low emission measure plasma. C1 [Winebarger, Amy R.; Cirtain, Jonathan; Mulu-Moore, Fana] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. [Warren, Harry P.] USN, Div Space Sci, Res Lab, Washington, DC 20375 USA. [Schmelz, Joan T.] Univ Memphis, Dept Phys, Memphis, TN 38152 USA. [Golub, Leon] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Kobayashi, Ken] Ctr Space Plasma & Aeron Res, Huntsville, AL 35805 USA. RP Winebarger, AR (reprint author), NASA, George C Marshall Space Flight Ctr, VP 62, Huntsville, AL 35812 USA. EM amy.r.winebarger@nasa.gov OI Golub, Leon/0000-0001-9638-3082 NR 23 TC 22 Z9 22 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD FEB 20 PY 2012 VL 746 IS 2 AR L17 DI 10.1088/2041-8205/746/2/L17 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 896ZT UT WOS:000300611100004 ER PT J AU Wright, NJ Drake, JJ Drew, JE Guarcello, MG Gutermuth, RA Hora, JL Kraemer, KE AF Wright, Nicholas J. Drake, Jeremy J. Drew, Janet E. Guarcello, Mario G. Gutermuth, Robert A. Hora, Joseph L. Kraemer, Kathleen E. TI PHOTOEVAPORATING PROPLYD-LIKE OBJECTS IN CYGNUS OB2 SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE ISM: individual objects (IRAS 20324+4057); ISM: jets and outflows; protoplanetary disks; stars: formation; stars: pre-main sequence; stars: protostars ID HUBBLE-SPACE-TELESCOPE; CANDIDATE PLANETARY-NEBULAE; NORTHERN GALACTIC PLANE; ORION-NEBULA; MASSIVE STARS; PROTOPLANETARY DISKS; CYG-OB2 ASSOCIATION; CIRCUMSTELLAR DISK; CARINA NEBULA; SPITZER MIPS AB We report the discovery of 10 proplyd-like objects in the vicinity of the massive OB association Cygnus OB2. They were discovered in IPHAS H alpha images and are clearly resolved in broadband Hubble Space Telescope/Advanced Camera for Surveys, near-IR, and Spitzer mid-IR images. All exhibit the familiar tadpole shape seen in photoevaporating objects such as the Orion proplyds, with a bright ionization front at the head facing the central cluster of massive stars and a tail stretching in the opposite direction. Many also show secondary ionization fronts, complex tail morphologies, or multiple heads. We consider the evidence that these are either proplyds or "evaporating gaseous globules" (EGGs) left over from a fragmenting molecular cloud, but find that neither scenario fully explains the observations. Typical sizes are 50,000-100,000 AU, larger than the Orion proplyds, but in agreement with the theoretical scaling of proplyd size with distance from the ionizing source. These objects are located at projected separations of similar to 6-14 pc from the OB association, compared to similar to 0.1 pc for the Orion proplyds, but are clearly being photoionized by the similar to 65 O-type stars in Cyg OB2. Central star candidates are identified in near- and mid-IR images, supporting the proplyd scenario, though their large sizes and notable asymmetries are more consistent with the EGG scenario. A third possibility is therefore considered that these are a unique class of photoevaporating partially embedded young stellar objects that have survived the destruction of their natal molecular cloud. This has implications for the properties of stars that form in the vicinity of massive stars. C1 [Wright, Nicholas J.; Drake, Jeremy J.; Guarcello, Mario G.; Hora, Joseph L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Drew, Janet E.] Univ Hertfordshire, Ctr Astron Res, Sci & Technol Res Inst, Hatfield AL10 9AB, Herts, England. [Gutermuth, Robert A.] Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA. [Kraemer, Kathleen E.] Boston Coll, Inst Sci Res, Chestnut Hill, MA 02467 USA. RP Wright, NJ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM nwright@cfa.harvard.edu OI Hora, Joseph/0000-0002-5599-4650; Drew, Janet/0000-0003-1192-7082; Kraemer, Kathleen/0000-0002-2626-7155 FU NASA [NAS8-39073] FX We thank Geert Barentsen, Robert Greimel, Roberto Raddi, and Jorick Vink for constructive discussions and thank the anonymous referee for a prompt report. This research used data obtained at the INT by the IPHAS project and processed by the Cambridge Astronomical Survey Unit. We acknowledge data products from the Spitzer Space Telescope, UKIDSS, and the NASA/ESA Hubble Space Telescope, and MONTAGE, funded by NASA. J.J.D. was supported by NASA contract NAS8-39073 to the Chandra X-ray Center (CXC). NR 44 TC 28 Z9 28 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD FEB 20 PY 2012 VL 746 IS 2 AR L21 DI 10.1088/2041-8205/746/2/L21 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 896ZT UT WOS:000300611100008 ER PT J AU Abraham, C Touwaide, A AF Abraham, Curtis Touwaide, Alain TI When Hippocrates had a headache ... SO NEW SCIENTIST LA English DT Editorial Material C1 [Touwaide, Alain] Smithsonian Inst, Inst Preservat Med Tradit, Washington, DC 20560 USA. NR 0 TC 0 Z9 0 U1 0 U2 1 PU REED BUSINESS INFORMATION LTD PI SUTTON PA QUADRANT HOUSE THE QUADRANT, SUTTON SM2 5AS, SURREY, ENGLAND SN 0262-4079 J9 NEW SCI JI New Sci. PD FEB 18 PY 2012 VL 213 IS 2852 BP 30 EP 31 PG 2 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 898OT UT WOS:000300752400015 ER PT J AU Dove, CJ Straker, LC AF Dove, Carla J. Straker, Lorian C. TI Comment on "A Diverse Assemblage of Late Cretaceous Dinosaur and Bird Feathers from Canadian Amber" SO SCIENCE LA English DT Editorial Material ID THEROPOD DINOSAUR; SINOSAUROPTERYX; CHINA C1 [Dove, Carla J.; Straker, Lorian C.] Smithsonian Inst, Natl Museum Nat Hist, Div Birds, Washington, DC 20013 USA. [Straker, Lorian C.] Univ Fed Rio de Janeiro, Inst Biofis Carlos Chagas Filho, Lab Ultraestrutura Celular Hertha Meyer, BR-21949900 Rio De Janeiro, Brazil. RP Dove, CJ (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Div Birds, MRC 116,POB 37102, Washington, DC 20013 USA. EM dovec@si.edu RI Straker, Lorian/J-5560-2016; Straker, Leon/B-2407-2013 OI Straker, Leon/0000-0002-7786-4128 NR 5 TC 3 Z9 3 U1 0 U2 13 PU AMER ASSOC ADVANCEMENT SCIENCE PI WASHINGTON PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA SN 0036-8075 J9 SCIENCE JI Science PD FEB 17 PY 2012 VL 335 IS 6070 DI 10.1126/science.1216208 PG 3 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 893LC UT WOS:000300356400020 PM 22344430 ER PT J AU Rest, A Prieto, JL Walborn, NR Smith, N Bianco, FB Chornock, R Welch, DL Howell, DA Huber, ME Foley, RJ Fong, W Sinnott, B Bond, HE Smith, RC Toledo, I Minniti, D Mandel, K AF Rest, A. Prieto, J. L. Walborn, N. R. Smith, N. Bianco, F. B. Chornock, R. Welch, D. L. Howell, D. A. Huber, M. E. Foley, R. J. Fong, W. Sinnott, B. Bond, H. E. Smith, R. C. Toledo, I. Minniti, D. Mandel, K. TI Light echoes reveal an unexpectedly cool eta Carinae during its nineteenth-century Great Eruption SO NATURE LA English DT Article ID LUMINOUS BLUE VARIABLES; HOMUNCULUS; SPECTRA; PROGENITORS; TRANSIENTS; SUPERNOVAE; DIVERSITY; NEBULA; ANALOG; MASS AB eta Carinae is one of the most massive binary stars in the Milky Way(1,2). It became the second-brightest star in our sky during its mid-nineteenth-century 'Great Eruption', but then faded from view (with only naked-eye estimates of brightness(3,4)). Its eruption is unique in that it exceeded the Eddington luminosity limit for ten years. Because it is only 2.3 kiloparsecs away, spatially resolved studies of the nebula have constrained the ejected mass and velocity, indicating that during its nineteenth-century eruption, eta Car ejected more than ten solar masses in an event that released ten per cent of the energy of a typical core-collapse supernova(5,6), without destroying the star. Here we report observations of light echoes of eta Carinae from the 1838-1858 Great Eruption. Spectra of these light echoes show only absorption lines, which are blueshifted by -210 km s(-1), in good agreement with predicted expansion speeds(6). The light-echo spectra correlate best with those of G2-to-G5 supergiants, which have effective temperatures of around 5,000 kelvin. In contrast to the class of extragalactic outbursts assumed to be analogues of the Great Eruption of eta Carinae(7-12), the effective temperature of its outburst is significantly lower than that allowed by standard opaque wind models(13). This indicates that other physical mechanisms such as an energetic blast wave may have triggered and influenced the eruption. C1 [Rest, A.; Walborn, N. R.; Bond, H. E.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Prieto, J. L.] Carnegie Observ, Pasadena, CA 91101 USA. [Prieto, J. L.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. [Smith, N.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Bianco, F. B.; Howell, D. A.] Las Cumbres Observ Global Telescope Network, Goleta, CA 93117 USA. [Bianco, F. B.; Howell, D. A.] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA. [Chornock, R.; Foley, R. J.; Fong, W.; Mandel, K.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Welch, D. L.; Sinnott, B.] McMaster Univ, Dept Phys & Astron, Hamilton, ON L8S 4M1, Canada. [Huber, M. E.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Smith, R. C.] Cerro Tololo Interamer Observ, Natl Opt Astron Observ, La Serena, Chile. [Toledo, I.] ALMA, San Pedro De Atacama, Ii Region, Chile. [Minniti, D.] Pontificia Univ Catolica Chile, Dept Astron & Astrophys, Santiago 22, Chile. [Mandel, K.] Univ London Imperial Coll Sci Technol & Med, Blackett Lab, London SW7 2AZ, England. RP Rest, A (reprint author), Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA. EM arest@stsci.edu FU National Science Foundation; LCOGT FX We thank R. Humphreys, K. Davidson and J. Vink for comments and discussions. We thank S. Blondin for help with the continuum subtraction. The Blanco 4-m telescope is a facility of the Cerro Tololo Inter-American Observatory, National Optical Astronomy Observatory, which is operated by the Association of Universities for Research in Astronomy, under contract with the National Science Foundation. We use data from the UVES Paranal Observatory Project. The computations in this paper were run on the Odyssey cluster supported by the FAS Science Division Research Computing Group at Harvard University. Observations were obtained at LCOGT, and F. B. B. and D. A. H. acknowledge support from LCOGT. J. L. P. is a Hubble Carnegie-Princeton Fellow. R. J. F. is a Clay Fellow. NR 28 TC 31 Z9 31 U1 0 U2 3 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 0028-0836 J9 NATURE JI Nature PD FEB 16 PY 2012 VL 482 IS 7385 BP 375 EP 378 DI 10.1038/nature10775 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 892LG UT WOS:000300287100040 PM 22337057 ER PT J AU Moser, WE Richardson, DJ Hammond, CI Lazo-Wasem, E AF Moser, William E. Richardson, Dennis J. Hammond, Charlotte I. Lazo-Wasem, Eric TI Molecular Characterization of Glossiphonia elegans (Verrill, 1872) (Glossiphoniidae: Hirudinida) from its type locality, West River, New Haven County, Connecticut, USA SO ZOOTAXA LA English DT Letter ID LEECH FAMILY GLOSSIPHONIIDAE C1 [Moser, William E.] Smithsonian Inst, Dept Invertebrate Zool, Museum Support Ctr MRC 534, Natl Museum Nat Hist, Suitland, MD 20746 USA. [Richardson, Dennis J.; Hammond, Charlotte I.] Quinnipiac Univ, Dept Biol Sci, Hamden, CT 06518 USA. [Lazo-Wasem, Eric] Yale Univ, Peabody Museum Nat Hist, Div Invertebrate Zool, New Haven, CT 06520 USA. RP Moser, WE (reprint author), Smithsonian Inst, Dept Invertebrate Zool, Museum Support Ctr MRC 534, Natl Museum Nat Hist, 4210 Silver Hill Rd, Suitland, MD 20746 USA. EM moserw@si.edu; Dennis.Richardson@quinnipiac.edu; Charlotte.Hammond@quinnipiac.edu; eric.lazo-wasem@yale.edu NR 11 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 FEB 16 PY 2012 IS 3195 BP 57 EP 60 PG 4 WC Zoology SC Zoology GA 895QM UT WOS:000300511300004 ER PT J AU Bravo, GA Chesser, RT Brumfield, RT AF Bravo, Gustavo A. Chesser, R. Terry Brumfield, Robb T. TI Isleria, a new genus of antwren (Aves: Passeriformes: Thamnophilidae) SO ZOOTAXA LA English DT Article DE Myrmotherula; Isleria; phylogeny; Thamnophilidae; antwrens ID TYPICAL ANTBIRDS THAMNOPHILIDAE; SPECIES LIMITS; COMPLEX; BIRDS; SPECIALIZATION; VOCALIZATIONS; FORMICARIIDAE; ANTSHRIKES AB A comprehensive molecular phylogenetic analysis of the family Thamnophilidae indicated that the genus Myrmotherula is not monophyletic. The clade composed of M. guttata and M. hauxwelli is only distantly related to other members of the genus and should be removed from Myrmotherula. The phenotypic distinctiveness of the clade argues against merging it with its sister group Thamnomanes and no generic name is available for the guttata-hauxwelli clade. Consequently, we describe the genus Isleria for these two species, and designate Myrmothera guttata as its type species. C1 [Bravo, Gustavo A.; Brumfield, Robb T.] Louisiana State Univ, Museum Nat Sci, Baton Rouge, LA 70803 USA. [Bravo, Gustavo A.; Brumfield, Robb T.] Louisiana State Univ, Dept Biol Sci, Baton Rouge, LA 70803 USA. [Chesser, R. Terry] US Geol Survey, Natl Museum Nat Hist, Patuxent Wildlife Res Ctr, Smithsonian Inst, Washington, DC 20013 USA. RP Bravo, GA (reprint author), Louisiana State Univ, Museum Nat Sci, Baton Rouge, LA 70803 USA. EM gbravo1@tigers.lsu.edu OI Brumfield, Robb/0000-0003-2307-0688 FU Frank Chapman Memorial Fund - AMNH; American Ornithologists' Union; LSUMNS; LSU Biograds; NSF [DEB-0841729, DBI-0400797, DEB-1011435] FX We are grateful to curators and collection managers of the Field Museum of Natural History (FMNH), the American Museum of Natural History (AMNH), University of Washington's Burke Museum (UWBM); Colecao de Aves, Instituto Nacional de Pesquisas de Amazonia (INPA), and Museu Paraense Emilio Goeldi (MPEG). N. Aristizabal and L. N. Naka assisted in obtaining sequences. N. David, M. L. Isler, P. R. Isler, and B. M. Whitney provided valuable comments regarding antbird taxonomy and nomenclature. This research was supported by grants from the Frank Chapman Memorial Fund - AMNH, the American Ornithologists' Union, the LSUMNS Big Day Fund, and LSU Biograds to GAB, NSF grants DEB-0841729 and DBI-0400797 to RTB, and DEB-1011435 to GAB. This manuscript was improved thanks to valuable comments from R. C. Banks, R. Belmonte-Lopes, S. Claramunt, A. M. Cuervo, L. P. Gonzaga, J. V. Remsen, R. P. Reynolds, and N. Woodman. Use of trade, product, or firm names does not imply endorsement by the US Government. NR 38 TC 9 Z9 9 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 FEB 16 PY 2012 IS 3195 BP 61 EP 67 PG 7 WC Zoology SC Zoology GA 895QM UT WOS:000300511300005 ER PT J AU Penniston-Dorland, SC Walker, RJ Pitcher, L Sorensen, SS AF Penniston-Dorland, Sarah C. Walker, Richard J. Pitcher, Lynnette Sorensen, Sorena S. TI Mantle-crust interactions in a paleosubduction zone: Evidence from highly siderophile element systematics of eclogite and related rocks SO EARTH AND PLANETARY SCIENCE LETTERS LA English DT Article DE highly siderophile elements; subduction zone; melange; metamorphism; osmium isotopes ID RE-OS ISOTOPES; FRANCISCAN SUBDUCTION COMPLEX; CONVERGENT PLATE MARGINS; PLATINUM-GROUP ELEMENTS; RHENIUM-OSMIUM ISOTOPE; PRIMITIVE UPPER-MANTLE; CIMA-DI-GAGNONE; P-T EVOLUTION; MELANGE FORMATION; ABYSSAL PERIDOTITES AB Substantial differences in Os-187/Os-188 and absolute and relative abundances of highly siderophile elements (HSE: Os, Ir, Ru, Pt, Pd, Re) in mantle peridotites compared to oceanic crust indicate that this suite of elements may prove useful in assessing mechanisms and pathways of mantle and slab mass transfer within the subduction channel. Currently, however, information regarding the mobility of the HSE in subduction zone environments is limited. To better understand the systematics of highly siderophile elements in subduction settings, we measured Os isotopic compositions and HSE abundances of cores and rinds of meter-scale blocks of eclogite, blueschist and garnet amphibolite from subduction-related melanges within 1) the Franciscan Complex, CA, and a related terrane in Oregon; 2) the Catalina Schist, CA; and 3) the Samana Metamorphic Complex, Samana Peninsula, Dominican Republic. Rinds composed of amphibole, chlorite, +/- phengite, talc, titanite and rutile partly enclose blocks at each location. Mineralogic, petrologic and geochemical data suggest that these rinds are metasomatic features that formed by fluid-mediated interaction between mafic blocks and an ultramafic matrix. The cores of high-grade blocks are characterized by high (Pt + Pd)/(Os + Ir + Ru), and variably radiogenic Os; initial Os-187/Os-188 ranges from 0.197 to 4.30. These characteristics are consistent with the HSE compositions of subducted basalts. In contrast, (Pt+Pd)/(Os + Ir + Ru) of rinds are generally much lower than cores, approaching values typical of mantle peridotites. The initial Os-187/Os-188 of most rinds are also typical of upper mantle peridotites; values for most rinds fall between 0.125 and 0.14. The similarities of the Os-187/Os-188 and HSE abundances between rinds and mantle peridotites indicate that the HSE contained within rinds reflect a contribution by mantle peridotite, whether by fluid-mediated transfer or through mechanical processes. If the HSE signatures of the rinds were generated by fluid-mediated metasomatic processes, these data require remarkably efficient and uniform transference of mantle HSE from peridotitic m lange matrix to the exteriors of m lange blocks during rind formation. More likely, the rinds are coatings of materials that contain HSE derived from peridotite precursors. These results suggest that centimeter-scale mass transfer by physical mechanisms may be important for some elements within the subduction channel. (C) 2011 Elsevier B.V. All rights reserved. C1 [Penniston-Dorland, Sarah C.; Walker, Richard J.; Pitcher, Lynnette] Univ Maryland, Dept Geol, College Pk, MD 20742 USA. [Sorensen, Sorena S.] Smithsonian Inst, Dept Mineral Sci, Natl Museum Nat Hist, Washington, DC 20560 USA. RP Penniston-Dorland, SC (reprint author), Univ Maryland, Dept Geol, College Pk, MD 20742 USA. EM sarahpd@umd.edu RI Walker, Richard/K-6869-2016 OI Walker, Richard/0000-0003-0348-2407 FU NSF [EAR-0911100, EAR-1119111] FX We thank the NSF for support to SP-D, grants EAR-0911100 and EAR-1119111. We thank Timm John, Chris Dale and Horst Marschall for their constructive reviews, and Rick Carlson for his editorial handling of the paper. Most specimens in this study were received from the Department of Mineral Sciences, Smithsonian Institution. The Santa Catalina Island Conservancy is acknowledged for support of sample collection logistics for samples of the Catalina Schist. NR 95 TC 7 Z9 8 U1 1 U2 33 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0012-821X J9 EARTH PLANET SC LETT JI Earth Planet. Sci. Lett. PD FEB 15 PY 2012 VL 319 BP 295 EP 306 DI 10.1016/j.epsl.2011.11.042 PG 12 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 913WW UT WOS:000301909100031 ER PT J AU Swanson, DA Rose, TR Fiske, RS McGeehin, JP AF Swanson, Donald A. Rose, Timothy R. Fiske, Richard S. McGeehin, John P. TI Keanakako'i Tephra produced by 300 years of explosive eruptions following collapse of Kilauea's caldera in about 1500 CE SO JOURNAL OF VOLCANOLOGY AND GEOTHERMAL RESEARCH LA English DT Article DE Kilauea; Keanakako'i Tephra; Hawaiian caldera; Kilauea explosive eruption; C-14 age ID VOLCANO; HAWAII; AD; CALIBRATION; INSIGHTS; ASH AB The Keanakako'i Tephra at Kilauea Volcano has previously been interpreted by some as the product of a caldera-forming eruption in 1790 CE. Our study, however, finds stratigraphic and C-14 evidence that the tephra instead results from numerous eruptions throughout a 300-year period between about 1500 and 1800. The stratigraphic evidence includes: (1) as many as six pure lithic ash beds interleaved in sand dunes made of earlier Keanakakoi vitric ash, (2) three lava flows from Kilauea and Mauna Loa interbedded with the tephra, (3) buried syneruptive cultural structures, (4) numerous intraformational water-cut gullies, and (5) abundant organic layers rich in charcoal within the tephra section. Interpretation of 97 new accelerator mass spectrometry (AMS) C-14 ages and 4 previous conventional ages suggests that explosive eruptions began in 1470-1510 CE, and that explosive activity continued episodically until the early 1800s, probably with two periods of quiescence lasting several decades. Kilauea's caldera, rather than forming in 1790, predates the first eruption of the Keanakakcri and collapsed in 1470-1510, immediately following, and perhaps causing, the end of the 60-year-long, 4-6 km(3) 'Aila'au eruption from the east side of Kilauea's summit area. The caldera was several hundred meters deep when the Keanakakoi began erupting, consistent with oral tradition, and probably had a volume of 4-6 km3. The caldera formed by collapse, but no eruption of lava coincided with its formation. A large volume of magma may have quickly drained from the summit reservoir and intruded into the east rift zone, perhaps in response to a major south-flank slip event, leading to summit collapse. Alternatively, magma may have slowly drained from the reservoir during the prolonged Aila'au eruption, causing episodic collapses before the final, largest downdrop took place. Two prolonged periods of episodic explosive eruptions are known at Kilauea, the Keanakakoi and the Uwekahuna Tephra (Fiske et al., 2009), and both occurred when a deep caldera existed, probably with a floor at or below the water table, and external water could readily interact with the magmatic system. The next period of intense explosive activity will probably have to await the drastic deepening of the present caldera (or Halema`uma`u Crater) or the formation of a new caldera. Published by Elsevier B.V. C1 [Swanson, Donald A.] US Geol Survey, Hawaiian Volcano Observ, Hawaii Natl Pk, HI 96718 USA. [Rose, Timothy R.; Fiske, Richard S.] Smithsonian Inst, Museum Nat Hist, Dept Mineral Sci, Washington, DC 20013 USA. [McGeehin, John P.] US Geol Survey, Reston, VA 20192 USA. RP Swanson, DA (reprint author), US Geol Survey, Hawaiian Volcano Observ, POB 51, Hawaii Natl Pk, HI 96718 USA. EM donswan@usgs.gov NR 55 TC 25 Z9 25 U1 3 U2 13 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0377-0273 EI 1872-6097 J9 J VOLCANOL GEOTH RES JI J. Volcanol. Geotherm. Res. PD FEB 15 PY 2012 VL 215 BP 8 EP 25 DI 10.1016/j.jvolgeores.2011.11.009 PG 18 WC Geosciences, Multidisciplinary SC Geology GA 905MQ UT WOS:000301276700002 ER PT J AU Hong, T AF Hong, Terry TI The Thief SO LIBRARY JOURNAL LA English DT Book Review C1 [Hong, Terry] Smithsonian Book Dragon, Washington, DC 20004 USA. RP Hong, T (reprint author), Smithsonian Book Dragon, Washington, DC 20004 USA. NR 1 TC 3 Z9 3 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 FEB 15 PY 2012 VL 137 IS 3 BP 98 EP 98 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA 892EB UT WOS:000300268400094 ER PT J AU Fogarty, ND Vollmer, SV Levitan, DR AF Fogarty, Nicole D. Vollmer, Steven V. Levitan, Don R. TI Weak Prezygotic Isolating Mechanisms in Threatened Caribbean Acropora Corals SO PLOS ONE LA English DT Article ID ANNULARIS SPECIES COMPLEX; REEF CORALS; REPRODUCTIVE ISOLATION; SCLERACTINIAN CORALS; GAMETE RECOGNITION; FERTILIZATION SUCCESS; CONSPECIFIC SPERM; GENETIC DIVERSITY; SPAWNING CORALS; SEA-URCHINS AB The Caribbean corals, Acropora palmata and A. cervicornis, recently have undergone drastic declines primarily as a result of disease. Previous molecular studies have demonstrated that these species form a hybrid (A. prolifera) that varies in abundance throughout the range of the parental distribution. There is variable unidirectional introgression across loci and sites of A. palmata genes flowing into A. cervicornis. Here we examine the efficacy of prezygotic reproductive isolating mechanisms within these corals including spawning times and choice and no-choice fertilization crosses. We show that these species have subtly different mean but overlapping spawning times, suggesting that temporal isolation is likely not an effective barrier to hybridization. We found species-specific differences in gametic incompatibilities. Acropora palmata eggs were relatively resistant to hybridization, especially when conspecific sperm are available to outcompete heterospecific sperm. Acropora cervicornis eggs demonstrated no evidence for gametic incompatibility and no evidence of reduced viability after aging four hours. This asymmetry in compatibility matches previous genetic data on unidirectional introgression. C1 [Fogarty, Nicole D.; Levitan, Don R.] Florida State Univ, Dept Biol Sci, Tallahassee, FL 32306 USA. [Vollmer, Steven V.] NE Univ, Ctr Marine Sci, Nahant, MA USA. RP Fogarty, ND (reprint author), Smithsonian Marine Stn, Ft Pierce, FL USA. EM fogartyn@si.edu FU Caribbean Coral Reef Ecosystems (CCRE) program [915]; Smithsonian Marine Science Network; PADI foundation; American Academy of Underwater Science; AWARE foundation; National Geographic Society [8230-07]; American Museum of Natural History; FSU; Marine Science Network; NSF [OCE-9911225] FX Funding was supplied by the Caribbean Coral Reef Ecosystems (CCRE) program (http://www.ccre.si.edu/) contribution #915, The Smithsonian Marine Science Network (http://www.sms.si.edu/), the PADI foundation (http://www.padifoundation.org/), the American Academy of Underwater Science (http://www.aaus.org), the Project AWARE foundation (http://www.projectaware.org/), the National Geographic Society (8230-07; http://www.nationalgeographic.com/), the Lerner-Gray Memorial Fund of the American Museum of Natural History (http://rggs.amnh.org/pages/academics_and_research/fellowship_and_grant_ opportunities), and FSU's International dissertation, Bennison, Gramling, and Short Fellowships to N.D. Fogarty. The Marine Science Network supplied funding to S.V. Vollmer, and NSF OCE-9911225 and the National Geographic Society (8230-07) supplied funding to D.R. Levitan. The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 82 TC 16 Z9 18 U1 0 U2 27 PU PUBLIC LIBRARY SCIENCE PI SAN FRANCISCO PA 185 BERRY ST, STE 1300, SAN FRANCISCO, CA 94107 USA SN 1932-6203 J9 PLOS ONE JI PLoS One PD FEB 14 PY 2012 VL 7 IS 2 AR e30486 DI 10.1371/journal.pone.0030486 PG 11 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 925CF UT WOS:000302737400001 PM 22348010 ER PT J AU Reisz, RR Evans, DC Roberts, EM Sues, HD Yates, AM AF Reisz, Robert R. Evans, David C. Roberts, Eric M. Sues, Hans-Dieter Yates, Adam M. TI Oldest known dinosaurian nesting site and reproductive biology of the Early Jurassic sauropodomorph Massospondylus SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA LA English DT Article ID SOUTH-AFRICA; ORNITHISCHIAN DINOSAUR; PARENTAL-CARE; EGGS; EVOLUTION; EMBRYOS; ELLIOT; SIZE AB The extensive Early Jurassic continental strata of southern Africa have yielded an exceptional record of dinosaurs that includes scores of partial to complete skeletons of the sauropodomorph Massospondylus, ranging from embryos to large adults. In 1976 an incomplete egg clutch including in ovo embryos of this dinosaur, the oldest known example in the fossil record, was collected from a road-cut talus, but its exact provenance was uncertain. An excavation program at the site started in 2006 has yielded multiple in situ egg clutches, documenting the oldest known dinosaurian nesting site, predating other similar sites by more than 100 million years. The presence of numerous clutches of eggs, some of which contain embryonic remains, in at least four distinct horizons within a small area, provides the earliest known evidence of complex reproductive behavior including site fidelity and colonial nesting in a terrestrial vertebrate. Thus, fossil and sedimentological evidence from this nesting site provides empirical data on reproductive strategies in early dinosaurs. A temporally calibrated optimization of dinosaurian reproductive biology not only demonstrates the primary significance of the Massospondylus nesting site, but also provides additional insights into the initial stages of the evolutionary history of dinosaurs, including evidence that deposition of eggs in a tightly organized single layer in a nest evolved independently from brooding. C1 [Reisz, Robert R.] Univ Toronto, Dept Biol, Mississauga, ON L5L 1C6, Canada. [Evans, David C.] Royal Ontario Museum, Toronto, ON M5S 2C6, Canada. [Roberts, Eric M.] James Cook Univ, Sch Earth & Environm Sci, Townsville, Qld 4811, Australia. [Sues, Hans-Dieter] Smithsonian Inst, Dept Paleobiol, Natl Museum Nat Hist, Washington, DC 20013 USA. [Yates, Adam M.] Univ Witwatersrand, Bernard Price Inst Palaeontol Res, ZA-2050 Johannesburg, South Africa. RP Reisz, RR (reprint author), Univ Toronto, Dept Biol, Mississauga, ON L5L 1C6, Canada. EM robert.reisz@utoronto.ca RI Roberts, Eric/J-1836-2014 OI Roberts, Eric/0000-0002-8583-7437 FU Golden Gate Highlands National Park; National Geographic Society; University of Toronto; Royal Ontario Museum; Natural Sciences and Engineering Research Council (Canada) FX The authors thank B. Rubidge, M. Raath, and B. Zipfel for ongoing support in South Africa; D. Scott for preparation and illustration of specimens; J. Hancox for advice on depositional environment of the fossil locality; and the staff of Golden Gate Highlands National Park for assistance and support during fieldwork. I. Morrison, H. Maddin, and N. Campione assisted in the field excavations. Fieldwork and research was supported by the National Geographic Society, University of Toronto, Royal Ontario Museum, and Natural Sciences and Engineering Research Council (Canada). NR 34 TC 18 Z9 20 U1 0 U2 34 PU NATL ACAD SCIENCES PI WASHINGTON PA 2101 CONSTITUTION AVE NW, WASHINGTON, DC 20418 USA SN 0027-8424 J9 P NATL ACAD SCI USA JI Proc. Natl. Acad. Sci. U. S. A. PD FEB 14 PY 2012 VL 109 IS 7 BP 2428 EP 2433 DI 10.1073/pnas.1109385109 PG 6 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 895IH UT WOS:000300489200056 PM 22308330 ER PT J AU Wang, XG Comita, LS Hao, ZQ Davies, SJ Ye, J Lin, F Yuan, ZQ AF Wang, Xugao Comita, Liza S. Hao, Zhanqing Davies, Stuart J. Ye, Ji Lin, Fei Yuan, Zuoqiang TI Local-Scale Drivers of Tree Survival in a Temperate Forest SO PLOS ONE LA English DT Article ID HEMLOCK-HARDWOOD FORESTS; TROPICAL TREE; DENSITY-DEPENDENCE; HABITAT ASSOCIATIONS; NORTHEASTERN CHINA; NEOTROPICAL FOREST; PLANT-POPULATIONS; SHADE TOLERANCE; RAIN-FOREST; SPATIAL DISTRIBUTIONS AB Tree survival plays a central role in forest ecosystems. Although many factors such as tree size, abiotic and biotic neighborhoods have been proposed as being important in explaining patterns of tree survival, their contributions are still subject to debate. We used generalized linear mixed models to examine the relative importance of tree size, local abiotic conditions and the density and identity of neighbors on tree survival in an old-growth temperate forest in northeastern China at three levels (community, guild and species). Tree size and both abiotic and biotic neighborhood variables influenced tree survival under current forest conditions, but their relative importance varied dramatically within and among the community, guild and species levels. Of the variables tested, tree size was typically the most important predictor of tree survival, followed by biotic and then abiotic variables. The effect of tree size on survival varied from strongly positive for small trees (1-20 cm dbh) and medium trees (20-40 cm dbh), to slightly negative for large trees (>40 cm dbh). Among the biotic factors, we found strong evidence for negative density and frequency dependence in this temperate forest, as indicated by negative effects of both total basal area of neighbors and the frequency of conspecific neighbors. Among the abiotic factors tested, soil nutrients tended to be more important in affecting tree survival than topographic variables. Abiotic factors generally influenced survival for species with relatively high abundance, for individuals in smaller size classes and for shade-tolerant species. Our study demonstrates that the relative importance of variables driving patterns of tree survival differs greatly among size classes, species guilds and abundance classes in temperate forest, which can further understanding of forest dynamics and offer important insights into forest management. C1 [Wang, Xugao; Hao, Zhanqing; Ye, Ji; Lin, Fei; Yuan, Zuoqiang] Chinese Acad Sci, Inst Appl Ecol, State Key Lab Forest & Soil Ecol, Shenyang, Liaoning Provin, Peoples R China. [Comita, Liza S.] Ohio State Univ, Dept Ecol Evolut & Organismal Biol, Columbus, OH 43210 USA. [Comita, Liza S.] Smithsonian Trop Res Inst, Balboa Ancon, Panama. [Davies, Stuart J.] Harvard Univ, Ctr Trop Forest Sci, Boston, MA 02115 USA. [Davies, Stuart J.] Smithsonian Trop Res Inst, Boston, MA USA. RP Wang, XG (reprint author), Chinese Acad Sci, Inst Appl Ecol, State Key Lab Forest & Soil Ecol, Shenyang, Liaoning Provin, Peoples R China. EM hzq@iae.ac.cn RI wang, xugao/B-1111-2015; OI wang, xugao/0000-0003-1207-8852; Comita, Liza/0000-0002-9169-1331 FU Chinese Academy of Sciences [KSCX2-EW-Z-5, KZCX2-YW-QN402]; National Natural Science Foundation of China [40971286, 31011120470, 31061160188]; Center for Tropical Forest Science of the Smithsonian Tropical Research Institute; HSBC Climate Partnership; National Center for Ecological Analysis and Synthesis; NSF [EF-0553768]; University of California, Santa Barbara; State of California FX This study was supported by the Knowledge Innovation Program of the Chinese Academy of Sciences (KSCX2-EW-Z-5 and KZCX2-YW-QN402) and the National Natural Science Foundation of China (40971286, 31011120470 and 31061160188). XW acknowledges the support of a fellowship from the Center for Tropical Forest Science of the Smithsonian Tropical Research Institute and the HSBC Climate Partnership. LSC acknowledges the support of a fellowship from the National Center for Ecological Analysis and Synthesis, a center funded by NSF (Grant #EF-0553768), the University of California, Santa Barbara, and the State of California. The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 83 TC 135 Z9 140 U1 12 U2 71 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 FEB 13 PY 2012 VL 7 IS 2 AR e29469 DI 10.1371/journal.pone.0029469 PG 10 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 925BB UT WOS:000302733900002 PM 22347996 ER PT J AU Versteirt, V Pecor, JE Fonseca, DM Coosemans, M Van Bortel, W AF Versteirt, Veerle Pecor, James E. Fonseca, Dina M. Coosemans, Marc Van Bortel, Wim TI Confirmation of Aedes koreicus (Diptera: Culicidae) in Belgium and description of morphological differences between Korean and Belgian specimens validated by molecular identification SO ZOOTAXA LA English DT Article DE Aedes koreicus; morphological comparison; egg structure; molecular identification; ND4; Republic of Korea; Belgium ID JAPONICUS DIPTERA; OCHLEROTATUS-JAPONICUS; MOSQUITOS DIPTERA; AEDINI DIPTERA; UNITED-STATES; LIFE STAGES; CLASSIFICATION; PHYLOGENY; DISEASE; COMPLEX AB In 2008, specimens resembling Aedes (Finlaya) koreicus (Edwards) (also Ochlerotatus koreicus or Hulecoeteomyia koreica) were found in Belgium during a national mosquito survey (MODIRISK). Small but consistent differences were, however, observed between the specimens described from Peninsula Korea and those found in Belgian. To achieve the correct identification a detailed morphological comparison was made between the Belgian specimens and reference material from Korean mainland and island populations housed at the Smithsonian Institution (Walter Reed Biosystematics Unit (WR-BU), Washington, USA). The identification was furthermore supported by molecular evidence based on the ND4 region (mtDNA) of available Korean and Belgian mosquito specimens. Morphological and molecular comparison confirmed the initial identification of Aedes koreicus. Based on morphological characteristics, the species collected in Belgium most likely originated from Jeju-do, an island south of the Korean Peninsula. The observed dissimilarities between Korean and Belgian specimens resembled a number of morphological differences mentioned previously between female adults collected on the Korean Peninsula and Jeju-do. This is the first report of Aedes koreicus outside its natural distribution range. A correct and rapid identification of new invading and spreading vector species is crucial for the implementation of effective control measurements. Hence a correct and easy accessible description of all possible variations of species arriving in new areas is highly recommended. Therefore, a comparative morphological study on the Smithsonian material of the species from Korean mainland, island population and from Belgium is given, pictures of the main aberrant characteristics and scanning electron microscope images of all stages of the species are included and molecular confirmation of the identification based on the mtDNA ND4 region is provided. C1 [Versteirt, Veerle; Coosemans, Marc; Van Bortel, Wim] Inst Trop Med, Dept Biomed Sci, Med Entomol Unit, Vector Biol Grp, B-2000 Antwerp, Belgium. [Pecor, James E.] Smithsonian Inst, Walter Reed Biosystemat Unit, Museum Support Ctr, Suitland, MD 20746 USA. [Fonseca, Dina M.] Rutgers State Univ, Ctr Vector Biol, New Brunswick, NJ 08901 USA. [Coosemans, Marc] Univ Antwerp, Dept Biomed Sci, Fac Pharmaceut Vet & Biomed Sci, B-2610 Antwerp, Belgium. RP Coosemans, M (reprint author), Inst Trop Med, Dept Biomed Sci, Med Entomol Unit, Vector Biol Grp, B-2000 Antwerp, Belgium. EM vversteirt@itg.be; pecorj@si.edu; dinafons@rci.rutgers.edu; mcoosemans@itg.be OI Fonseca, Dina/0000-0003-4726-7100 FU UA; NIH-NIAID [N01-AI-25490]; Belgium Science Policy (Belspo) [SD/BD/04A, SD/BD/04B] FX We would like to thank the conservator of the sample site Jos Gorissen and Agentschap voor Natuur en Bos for the authorisation of the many visits and Bram Wellekens and Patricia Roelants for technical support. We are very grateful to Ms. Judith Stoffer for the pictures, Julien Cillis (KBIN) for the SEM micrographs, and Drs Rick Wilkerson and Yiau-Min Huang for the verification of the identification and the use of the material at the Walter Reed Biosystematics Unit (Smithsonian Institute, Washington DC, USA). The opinions or assertions contained herein are the private views of the authors, and are not to be construed as official views of the supporting agencies. V.V. would like to acknowledge the UA for funding her stay at the WRBU. D.M.F. obtained funds to sequence the ND4 gene of Ae. koreicus and Ae. japonicus from NIH-NIAID under Contract No. N01-AI-25490. This work was funded by the Belgium Science Policy (Belspo; SD/BD/04A and SD/BD/04B). NR 29 TC 12 Z9 15 U1 1 U2 3 PU MAGNOLIA PRESS PI AUCKLAND PA PO BOX 41383, AUCKLAND, ST LUKES 1030, NEW ZEALAND SN 1175-5326 EI 1175-5334 J9 ZOOTAXA JI Zootaxa PD FEB 13 PY 2012 IS 3191 BP 21 EP 32 PG 12 WC Zoology SC Zoology GA 891XM UT WOS:000300250100002 ER PT J AU Asgari-Targhi, M van Ballegooijen, AA AF Asgari-Targhi, M. van Ballegooijen, A. A. TI MODEL FOR ALFVEN WAVE TURBULENCE IN SOLAR CORONAL LOOPS: HEATING RATE PROFILES AND TEMPERATURE FLUCTUATIONS SO ASTROPHYSICAL JOURNAL LA English DT Article DE magnetohydrodynamics (MHD); Sun: corona; Sun: surface magnetism; turbulence ID EMISSION MEASURE DISTRIBUTION; ACTIVE-REGION 10953; TRANSITION REGION; MAGNETIC-FIELDS; WIND; SUN; DYNAMICS; HINODE; PROMINENCES; ATMOSPHERE AB It has been suggested that the solar corona may be heated by dissipation of Alfven waves that propagate up from the solar photosphere. According to this theory, counterpropagating Alfven waves are subject to nonlinear interactions that lead to turbulent decay of the waves and heating of the chromospheric and coronal plasma. To test this theory, better models for the dynamics of Alfven waves in coronal loops are required. In this paper, we consider wave heating in an active region observed with the Solar Dynamics Observatory in 2010 May. First a three-dimensional (3D) magnetic model of the region is constructed, and ten magnetic field lines that match observed coronal loops are selected. For each loop we construct a 3D magnetohydrodynamic model of the Alfven waves near the selected field line. The waves are assumed to be generated by footpoint motions inside the kilogauss magnetic flux elements at the two ends of the loop. Based on such models, we predict the spatial and temporal profiles of the heating along the selected loops. We also estimate the temperature fluctuations resulting from such heating. We find that the Alfven wave turbulence model can reproduce the observed characteristics of the hotter loops in the active region core, but the loops at the periphery of the region have large expansion factors and are predicted to be thermally unstable. C1 [Asgari-Targhi, M.; van Ballegooijen, A. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Asgari-Targhi, M (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS-15, Cambridge, MA 02138 USA. OI van Ballegooijen, Adriaan/0000-0002-5622-3540 FU UK's Engineering and Physical Sciences Research Council [EP/I034327/1] FX We thank the referee for comments which helped to improve the description of the model assumptions. We are most grateful to Alex Voss from the School of Computer Science at the University of St. Andrews for his support with the computational work, which was funded by the UK's Engineering and Physical Sciences Research Council (EP/I034327/1). We also thank Steve Cranmer and Ed DeLuca for many interesting discussions about coronal heating and turbulence in the solar atmosphere. The HMI and AIA data have been used courtesy of NASA/SDO and the AIA, EVE, and HMI science teams. NR 57 TC 35 Z9 35 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 FEB 10 PY 2012 VL 746 IS 1 AR 81 DI 10.1088/0004-637X/746/1/81 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 926VZ UT WOS:000302861300081 ER PT J AU King, AL Miller, JM Raymond, J AF King, Ashley L. Miller, Jon M. Raymond, John TI WARM ABSORBERS AND OUTFLOWS IN THE SEYFERT-1 GALAXY NGC 4051 SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; galaxies: active; galaxies: individual (NGC 4051); galaxies: nuclei; galaxies: Seyfert ID ACTIVE GALACTIC NUCLEI; X-RAY-ABSORPTION; BLACK-HOLES; DISK WINDS; XMM-NEWTON; ACCRETION DISKS; IONIZED OUTFLOW; CHANDRA-LETGS; GRO J1655-40; SPECTRUM AB We present both phenomenological and more physical photoionization models of the Chandra/HETG spectra of the Seyfert-1 active galactic nucleus NGC 4051. We detect 40 absorption and emission lines, encompassing highly ionized charge states from O, Ne, Mg, Si, S, and the Fe L-shell and K-shell. Two independent photoionization packages, XSTAR and Cloudy, were both used to self-consistently model the continuum and line spectra. These fits detected three absorbing regions in this system with densities ranging from 10(10) to 10(11) cm(-3). In particular, our XSTAR models require three components that have ionization parameters of log(xi) = 4.5, 3.3, and 1.0, and are located within the broad-line region at 70, 300, and 13000 R-g, respectively, assuming a constant wind density. Larger radii are inferred for density profiles which decline with radius. The Cloudy models give a similar set of parameters with ionization parameters of log(xi) = 5.0, 3.6, and 2.2 located at 40, 200, and 3300 R-g. We demonstrate that these regions are outflowing from the system, and carry a small fraction of material out of the system relative to the implied mass accretion rate. The data suggest that magnetic fields may be an important driving mechanism. C1 [King, Ashley L.; Miller, Jon M.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Raymond, John] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP King, AL (reprint author), Univ Michigan, Dept Astron, 500 Church St, Ann Arbor, MI 48109 USA. EM ashking@umich.edu NR 49 TC 13 Z9 13 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 FEB 10 PY 2012 VL 746 IS 1 AR 2 DI 10.1088/0004-637X/746/1/2 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 926VZ UT WOS:000302861300002 ER PT J AU Leauthaud, A George, MR Behroozi, PS Bundy, K Tinker, J Wechsler, RH Conroy, C Finoguenov, A Tanaka, M AF Leauthaud, Alexie George, Matthew R. Behroozi, Peter S. Bundy, Kevin Tinker, Jeremy Wechsler, Risa H. Conroy, Charlie Finoguenov, Alexis Tanaka, Masayuki TI THE INTEGRATED STELLAR CONTENT OF DARK MATTER HALOS SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology : observations; diffuse radiation; galaxies : clusters: general; galaxies : stellar content; X-rays : galaxies: clusters ID DIGITAL SKY SURVEY; INITIAL MASS FUNCTION; WIDE-FIELD SURVEY; BRIGHTEST CLUSTER GALAXIES; STAR-FORMATION EFFICIENCY; K-BAND PROPERTIES; LESS-THAN 2; OCCUPATION DISTRIBUTION; POPULATION SYNTHESIS; COSMOS FIELD AB Measurements of the total amount of stars locked up in galaxies as a function of host halo mass contain key clues about the efficiency of processes that regulate star formation. We derive the total stellar mass fraction f(star) (excluding stars in the intracluster light) as a function of halo mass M-500c from z = 0.2 to z = 1 using two complementary methods. First, we derive f(star) using a statistical Halo Occupation Distribution model jointly constrained by data from lensing, clustering, and the stellar mass function. This method enables us to probe f(star) over a much wider halo mass range than with group or cluster catalogs. Second, we derive f(star) at group scales using a COSMOS X-ray group catalog and show that the two methods agree to within 30%. We quantify the systematic uncertainty on f(star) using abundance matching methods and show that the statistical uncertainty on f(star) (similar to 10%) is dwarfed by systematic uncertainties associated with stellar mass measurements (similar to 45% excluding initial mass function, IMF, uncertainties). Assuming a Chabrier IMF, we find 0.012 <= f(star) <= 0.025 at M-500c = 10(13) M-circle dot and 0.0057 <= f(star) <= 0.015 at M-500c = 10(14) M-circle dot. These values are significantly lower than previously published estimates. We investigate the cause of this difference and find that previous work has overestimated f(star) owing to a combination of inaccurate stellar mass estimators and/or because they have assumed that all galaxies in groups are early-type galaxies with a constant mass-to-light ratio. Contrary to previous claims, our results suggest that the mean value of f(star) is always significantly lower than f(gas) for halos above 1013M(circle dot). Combining our results with recently published gas mass fractions, we find a shortfall in f(star) + f(gas) at R-500c compared to the cosmic mean. This shortfall varies with halo mass and becomes larger toward lower halo masses. C1 [Leauthaud, Alexie; Bundy, Kevin; Tanaka, Masayuki] Univ Tokyo, Inst Phys & Math Universe, Chiba 2778582, Japan. [Leauthaud, Alexie] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA. [Leauthaud, Alexie] Univ Calif Berkeley, Berkeley Ctr Cosmol Phys, Berkeley, CA 94720 USA. [George, Matthew R.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Behroozi, Peter S.; Wechsler, Risa H.] Stanford Univ, Dept Phys, Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94305 USA. [Behroozi, Peter S.; Wechsler, Risa H.] SLAC Natl Accelerator Lab, Stanford, CA 94305 USA. [Tinker, Jeremy] NYU, Ctr Cosmol & Particle Phys, Dept Phys, New York, NY 10013 USA. [Conroy, Charlie] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Finoguenov, Alexis] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Finoguenov, Alexis] Univ Maryland Baltimore Cty, Ctr Space Sci Technol, Baltimore, MD 21250 USA. RP Leauthaud, A (reprint author), Univ Tokyo, Inst Phys & Math Universe, Chiba 2778582, Japan. EM alexie.leauthaud@ipmu.jp FU World Premier International Research Center Initiative (WPI Initiative), MEXT, Japan; NASA [HST-GO-09822]; NASA HST Theory [HST-AR-12159.01-A]; U.S. Department of Energy [DE-AC02-76SF00515] FX We thank Ian McCarthy, Andrey Kravtsov, Andrew Wetzel, and Stefania Giodini for insightful discussions. We are grateful to Anthony Gonzalez for useful comments on an early version of the manuscript and for providing data in electronic format. We thank Michele Cappellari and Claudia Maraston for providing details on IMF conversions and SPS models. We are grateful to Jack Bishop and Al Leon for inspiring conversations. A.L. acknowledges support from the Chamberlain Fellowship at LBNL and from the Berkeley Center for Cosmological Physics. This work was supported by World Premier International Research Center Initiative (WPI Initiative), MEXT, Japan. The HST COSMOS Treasury program was supported through NASA grant HST-GO-09822. We wish to thank Tony Roman, Denise Taylor, and David Soderblom for their assistance in planning and scheduling of the extensive COSMOS observations. R.H.W. and P.S.B. received support from a NASA HST Theory Grant HST-AR-12159.01-A and from the U.S. Department of Energy under contract number DE-AC02-76SF00515 and used computing resources at SLAC National Accelerator Laboratory. We gratefully acknowledge the contributions of the entire COSMOS collaboration, consisting of more than 70 scientists. More information on the COSMOS survey is available at http://cosmos.astro.caltech.edu/. It is a pleasure to acknowledge the excellent services provided by the NASA IPAC/IRSA staff (Anastasia Laity, Anastasia Alexov, Bruce Berriman, and John Good) in providing online archive and server capabilities for the COSMOS data sets. NR 111 TC 67 Z9 67 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 10 PY 2012 VL 746 IS 1 AR 95 DI 10.1088/0004-637X/746/1/95 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 926VZ UT WOS:000302861300095 ER PT J AU Lunnan, R Vogelsberger, M Frebel, A Hernquist, L Lidz, A Boylan-Kolchin, M AF Lunnan, Ragnhild Vogelsberger, Mark Frebel, Anna Hernquist, Lars Lidz, Adam Boylan-Kolchin, Michael TI THE EFFECTS OF PATCHY REIONIZATION ON SATELLITE GALAXIES OF THE MILKY WAY SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology: theory; early universe; galaxies: dwarf; methods: numerical ID METAL-POOR STARS; HIGH-RESOLUTION SPECTROSCOPY; DWARF SPHEROIDAL GALAXIES; PROBE WMAP OBSERVATIONS; DIGITAL SKY SURVEY; LUMINOSITY FUNCTION; MAGELLANIC CLOUDS; COSMIC REIONIZATION; STELLAR HALO; HII-REGIONS AB We combine the high-resolution Aquarius simulations with three-dimensional models of reionization based on the initial density field of the Aquarius parent simulation, Millennium-II, to study the impact of patchy reionization on the faint satellite population of Milky Way halos. Because the Aquarius suite consists of zoom-in simulations of halos in the Millennium-II volume, we follow the formation of substructure and the growth of reionization bubbles due to the larger environment simultaneously, and thereby determine the reionization redshifts of satellite candidates. We do this for four different reionization models and also compare results to instantaneous reionization. Using a simple procedure for selecting satellites and assigning luminosities in the simulations, we compare the resulting satellite populations. We find that the overall number of satellites depends sensitively on the reionization model, with a factor of 3-4 variation between the four models for a given host halo, although the difference is entirely in the population of faint satellites (M-V > -10). In addition, we find that for a given reionization model the total number of satellites differs by 10%-20% between the patchy and homogeneous scenarios, provided that the redshift is chosen appropriately for the instantaneous case. However, the halo-halo scatter from the six Aquarius halos is large, up to a factor of 2-3, and so is comparable to the difference between reionization scenarios. In order to use the population of faint dwarf galaxies around the Milky Way as a probe of the local reionization history, it is necessary to first better understand the general distribution of substructure around Milky Way-mass halos. C1 [Lunnan, Ragnhild; Vogelsberger, Mark; Frebel, Anna; Hernquist, Lars] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Lidz, Adam] Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA. [Boylan-Kolchin, Michael] Univ Calif Irvine, Ctr Galaxy Evolut, Irvine, CA 92697 USA. RP Lunnan, R (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM rlunnan@cfa.harvard.edu OI Lunnan, Ragnhild/0000-0001-9454-4639; Boylan-Kolchin, Michael/0000-0002-9604-343X FU Clay Fellowship FX We thank the Virgo Consortium for access to the Aquarius simulations for this project, and Matt Walker and Daniel Eisenstein for helpful discussions. We also thank the anonymous referee for helpful comments that improved the structure of the manuscript. A.F. acknowledges support of a Clay Fellowship administered by the Smithsonian Astrophysical Observatory. NR 72 TC 17 Z9 17 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 10 PY 2012 VL 746 IS 1 AR 109 DI 10.1088/0004-637X/746/1/109 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 926VZ UT WOS:000302861300109 ER PT J AU McLean, M Berger, E Reiners, A AF McLean, M. Berger, E. Reiners, A. TI THE RADIO ACTIVITY-ROTATION RELATION OF ULTRACOOL DWARFS SO ASTROPHYSICAL JOURNAL LA English DT Article DE brown dwarfs; radio continuum: stars; stars: activity; stars: low-mass; stars: magnetic field ID LOW-MASS STARS; H-ALPHA EMISSION; SIMULTANEOUS MULTIWAVELENGTH OBSERVATIONS; MAGNETIC-FIELD TOPOLOGY; X-RAY-EMISSION; MAIN-SEQUENCE; LARGE-SCALE; CHROMOSPHERIC ACTIVITY; BROWN DWARFS; FLARE STARS AB We present a new radio survey of about 100 late-M and L dwarfs undertaken with the Very Large Array. The sample was chosen to explore the role of rotation in the radio activity of ultracool dwarfs. As part of the survey we discovered radio emission from three new objects, 2MASS J 0518113-310153 (M6.5), 2MASS J 0952219-192431 (M7), and 2MASS J 1314203+132001 (M7), and made an additional detection of LP 349-25 (M8). Combining the new sample with results from our previous studies and from the literature, we compile the largest sample to date of ultracool dwarfs with radio observations and measured rotation velocities (167 objects). In the spectral type range M0-M6 we find a radio activity-rotation relation, with saturation at L-rad/L-bol approximate to 10(-7.5) above v sin i approximate to 5 km s(-1), similar to the relation in Ha and X-rays. However, at spectral types greater than or similar to M7 the ratio of radio to bolometric luminosity increases significantly regardless of rotation velocity, and the scatter in radio luminosity increases. In particular, while the most rapid rotators (v sin i greater than or similar to 20 km s(-1)) exhibit "super-saturation" in X-rays and Ha, this effect is not seen in the radio. We also find that ultracool dwarfs with v sin i greater than or similar to 20 km s(-1) have a higher radio detection fraction by about a factor of three compared to objects with v sin i less than or similar to 10 km s(-1). When measured in terms of the Rossby number (Ro), the radio activity-rotation relation follows a single trend and with no apparent saturation from G to L dwarfs and down to Ro similar to 10(-3); in X-rays and Ha there is clear saturation at Ro less than or similar to 0.1, with super-saturation beyond M7. A similar trend is observed for the radio surface flux (L-rad/R-*(2)) as a function of Ro. The continued role of rotation in the overall level of radio activity and in the fraction of active sources, and the single trend of L-rad/L-bol and L-rad/R-*(2) as a function of Ro from G to L dwarfs, indicates that rotation effects are important in regulating the topology or strength of magnetic fields in at least some fully convective dwarfs. The fact that not all rapid rotators are detected in the radio provides additional support to the idea of dual dynamo states proposed from spectropolarimetric observations. C1 [McLean, M.; Berger, E.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Reiners, A.] Univ Gottingen, Inst Astrophys, D-37077 Gottingen, Germany. RP McLean, M (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. FU National Science Foundation [AST-1008361]; DFG [RE 1664/4-1] FX E.B. acknowledges support for this work from the National Science Foundation through Grant AST-1008361. A. R. received research funding from the DFG as an Emmy Noether Fellow (RE 1664/4-1). This work has made use of the SIMBAD database, operated at CDS, Strasbourg, France. NR 59 TC 45 Z9 45 U1 0 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 10 PY 2012 VL 746 IS 1 AR 23 DI 10.1088/0004-637X/746/1/23 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 926VZ UT WOS:000302861300023 ER PT J AU Metzger, BD Berger, E AF Metzger, B. D. Berger, E. TI WHAT IS THE MOST PROMISING ELECTROMAGNETIC COUNTERPART OF A NEUTRON STAR BINARY MERGER? SO ASTROPHYSICAL JOURNAL LA English DT Article DE gamma-ray burst: general; gravitational waves; stars: neutron; surveys ID GAMMA-RAY BURSTS; COMPACT OBJECT MERGERS; GRAVITATIONAL-WAVE OBSERVATIONS; EXTENDED EMISSION; HOST GALAXY; R-PROCESS; OPTICAL AFTERGLOW; STANDARD SIRENS; LIGHT CURVES; SCIENCE RUN AB The final inspiral of double neutron star and neutron-star-black-hole binaries are likely to be detected by advanced networks of ground-based gravitational wave (GW) interferometers. Maximizing the science returns from such a discovery will require the identification of an electromagnetic counterpart. Here we critically evaluate and compare several possible counterparts, including short-duration gamma-ray bursts (SGRBs), "orphan" optical and radio afterglows, and day-long optical transients powered by the radioactive decay of heavy nuclei synthesized in the merger ejecta ("kilonovae"). We assess the promise of each counterpart in terms of four "Cardinal Virtues": detectability, high fraction, identifiability, and positional accuracy. Taking into account the search strategy for typical error regions of tens of square degrees, we conclude that SGRBs are the most useful to confirm the cosmic origin of a few GW events, and to test the association with neutron star mergers. However, for the more ambitious goal of localizing and obtaining redshifts for a large sample of GW events, kilonovae are instead preferred. Off-axis optical afterglows are detectable for at most tens of percent of events, while radio afterglows are promising only for energetic relativistic ejecta in a high-density medium. Our main recommendations are: (1) an all-sky gamma-ray satellite is essential for temporal coincidence detections, and for GW searches of gamma-ray-triggered events; (2) the Large Synoptic Survey Telescope should adopt a one-day cadence follow-up strategy, ideally with 0.5 hr per pointing to cover GW error regions; and (3) radio searches should focus on the relativistic case, which requires observations for a few months. C1 [Metzger, B. D.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. [Berger, E.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Metzger, BD (reprint author), NASA, Washington, DC 20546 USA. FU NASA [PF9-00065, NAS8-03060]; Chandra Xray Center; National Science Foundation [AST-1107973] FX We thank Hendrik van Eerten and Andrew MacFadyen for producing and maintaining their online library of afterglow light curves. We thank Ehud Nakar for providing theoretical light curves of supernova shock breakout. We thank S. Nissanke and R. O'Shaughnessy for helpful discussions and information. B. D. M. is supported by NASA through Einstein Postdoctoral Fellowship grant No. PF9-00065 awarded by the Chandra Xray Center, which is operated by the Smithsonian Astrophysical Observatory for NASA under contract NAS8-03060. E. B. acknowledges support for this work from the National Science Foundation through grant AST-1107973. NR 118 TC 211 Z9 212 U1 2 U2 7 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 10 PY 2012 VL 746 IS 1 DI 10.1088/0004-637X/746/1/48 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 926VZ UT WOS:000302861300048 ER PT J AU Rodney, SA Riess, AG Dahlen, T Strolger, LG Ferguson, HC Hjorth, J Frederiksen, TF Weiner, BJ Mobasher, B Casertano, S Jones, DO Challis, P Faber, SM Filippenko, AV Garnavich, P Graur, O Grogin, NA Hayden, B Jha, SW Kirshner, RP Kocevski, D Koekemoer, A McCully, C Patel, B Rajan, A Scarlata, C AF Rodney, Steven A. Riess, Adam G. Dahlen, Tomas Strolger, Louis-Gregory Ferguson, Henry C. Hjorth, Jens Frederiksen, Teddy F. Weiner, Benjamin J. Mobasher, Bahram Casertano, Stefano Jones, David O. Challis, Peter Faber, S. M. Filippenko, Alexei V. Garnavich, Peter Graur, Or Grogin, Norman A. Hayden, Brian Jha, Saurabh W. Kirshner, Robert P. Kocevski, Dale Koekemoer, Anton McCully, Curtis Patel, Brandon Rajan, Abhijith Scarlata, Claudia TI A TYPE Ia SUPERNOVA AT REDSHIFT 1.55 IN HUBBLE SPACE TELESCOPE INFRARED OBSERVATIONS FROM CANDELS SO ASTROPHYSICAL JOURNAL LA English DT Article DE supernovae: general ID EXTRAGALACTIC LEGACY SURVEY; EQUATION-OF-STATE; DARK ENERGY; LIGHT CURVES; ACCELERATING UNIVERSE; SNE-IA; CONSTRAINTS; DECELERATION; DISCOVERIES; FRACTIONS AB We report the discovery of a Type Ia supernova (SN Ia) at redshift z = 1.55 with the infrared detector of the Wide Field Camera 3 (WFC3-IR) on the Hubble Space Telescope (HST). This object was discovered in CANDELS imaging data of the Hubble Ultra Deep Field and followed as part of the CANDELS+CLASH Supernova project, comprising the SN search components from those two HST multi-cycle treasury programs. This is the highest redshift SN Ia with direct spectroscopic evidence for classification. It is also the first SN Ia at z > 1 found and followed in the infrared, providing a full light curve in rest-frame optical bands. The classification and redshift are securely defined from a combination of multi-band and multi-epoch photometry of the SN, ground-based spectroscopy of the host galaxy, and WFC3-IR grism spectroscopy of both the SN and host. This object is the first of a projected sample at z > 1.5 that will be discovered by the CANDELS and CLASH programs. The full CANDELS+CLASH SN Ia sample will enable unique tests for evolutionary effects that could arise due to differences in SN Ia progenitor systems as a function of redshift. This high-z sample will also allow measurement of the SN Ia rate out to z approximate to 2, providing a complementary constraint on SN Ia progenitor models. C1 [Rodney, Steven A.; Riess, Adam G.; Jones, David O.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Riess, Adam G.; Dahlen, Tomas; Ferguson, Henry C.; Casertano, Stefano; Grogin, Norman A.; Koekemoer, Anton; Rajan, Abhijith] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Strolger, Louis-Gregory] Western Kentucky Univ, Dept Phys, Bowling Green, KY 42101 USA. [Hjorth, Jens; Frederiksen, Teddy F.] Univ Copenhagen, Niels Bohr Inst, Dark Cosmol Ctr, DK-2100 Copenhagen, Denmark. [Weiner, Benjamin J.] Univ Arizona, Dept Astron, Tucson, AZ 85721 USA. [Mobasher, Bahram] Univ Calif Riverside, Dept Phys & Astron, Riverside, CA 92521 USA. [Challis, Peter; Kirshner, Robert P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Faber, S. M.; Kocevski, Dale] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 92064 USA. [Filippenko, Alexei V.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Garnavich, Peter; Hayden, Brian] Univ Notre Dame, Dept Phys, Notre Dame, IN 46556 USA. [Graur, Or] Tel Aviv Univ, Dept Astrophys, IL-69978 Tel Aviv, Israel. [Jha, Saurabh W.; McCully, Curtis; Patel, Brandon] Rutgers State Univ, Dept Phys & Astron, Piscataway, NJ 08854 USA. [Scarlata, Claudia] Univ Minnesota, Dept Astron, Minneapolis, MN 55455 USA. RP Rodney, SA (reprint author), Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. RI Hjorth, Jens/M-5787-2014; OI Hjorth, Jens/0000-0002-4571-2306; Graur, Or/0000-0002-4391-6137; Weiner, Benjamin/0000-0001-6065-7483; Koekemoer, Anton/0000-0002-6610-2048 FU NASA from the Space Telescope Science Institute [HST-GO-12060, HST-GO-12099]; NASA [NAS 5-26555]; NSF [AST-0847157]; Danish National Research Foundation FX Financial support for this work was provided by NASA through grants HST-GO-12060 and HST-GO-12099 from the Space Telescope Science Institute, which is operated by Associated Universities for Research in Astronomy, Inc., under NASA contract NAS 5-26555. Support for this research at Rutgers University was provided in part by NSF CAREER award AST-0847157 to S.W.J. The Dark Cosmology Centre is supported by the Danish National Research Foundation. NR 45 TC 27 Z9 27 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 FEB 10 PY 2012 VL 746 IS 1 AR 5 DI 10.1088/0004-637X/746/1/5 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 926VZ UT WOS:000302861300005 ER PT J AU Schindhelm, E France, K Burgh, EB Herczeg, GJ Green, JC Brown, A Brown, JM Valenti, JA AF Schindhelm, Eric France, Kevin Burgh, Eric B. Herczeg, Gregory J. Green, James C. Brown, Alexander Brown, Joanna M. Valenti, Jeff A. TI CHARACTERIZING CO FOURTH POSITIVE EMISSION IN YOUNG CIRCUMSTELLAR DISKS SO ASTROPHYSICAL JOURNAL LA English DT Article DE protoplanetary disks; stars : individual (RECX 15, DM Tau, DE Tau, HD 135344B, DR Tau, DK Tau, DF Tau, LkCa 15, GM Aur) ID T-TAURI STARS; ETA-CHAMAELEONTIS CLUSTER; FAR-ULTRAVIOLET CONTINUUM; FLUORESCENT H-2 EMISSION; PROTOPLANETARY DISKS; TRANSITIONAL DISKS; MOLECULAR-HYDROGEN; CARBON-MONOXIDE; ACCRETION RATES; BINARY STARS AB Carbon monoxide is a commonly used IR/submillimeter tracer of gas in protoplanetary disks. We present an analysis of ultraviolet CO emission in Hubble Space Telescope Cosmic Origins Spectrograph spectra for 12 Classical T Tauri stars (CTTSs). Several ro-vibrational bands of the CO A(1)Pi-X-1 Sigma(+) (Fourth Positive) electronic transition system are spectrally resolved from emission of other atoms and H-2. The CO A(1)Pi nu' = 14 state is populated by absorption of Ly alpha photons, created at the accretion column on the stellar surface. For targets with strong CO emission, we model the Lya radiation field as an input for a simple fluorescence model to estimate CO rotational excitation temperatures and column densities. Typical column densities range from N-CO = 10(18) to 10(19) cm(-2). Our measured excitation temperatures are mostly below T-CO = 600 K, cooler than typical M-band CO emission. These temperatures and the emission line widths imply that the UV emission originates in a different population of CO than that which is IR-emitting. We also find a significant correlation between CO emission and the disk accretion rate (M) over dot and age. Our analysis shows that ultraviolet CO emission can be a useful diagnostic of CTTS disk gas. C1 [Schindhelm, Eric; France, Kevin; Burgh, Eric B.; Green, James C.; Brown, Alexander] Univ Colorado, Ctr Astrophys & Space Astron, Boulder, CO 80309 USA. [Herczeg, Gregory J.] Max Planck Inst Extraterr Phys, D-85741 Garching, Germany. [Brown, Joanna M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Valenti, Jeff A.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. RP Schindhelm, E (reprint author), Univ Colorado, Ctr Astrophys & Space Astron, 389 UCB, Boulder, CO 80309 USA. OI Herczeg, Gregory/0000-0002-7154-6065 NR 70 TC 17 Z9 17 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 10 PY 2012 VL 746 IS 1 AR 97 DI 10.1088/0004-637X/746/1/97 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 926VZ UT WOS:000302861300097 ER PT J AU Suzuki, N Rubin, D Lidman, C Aldering, G Amanullah, R Barbary, K Barrientos, LF Botyanszki, J Brodwin, M Connolly, N Dawson, KS Dey, A Doi, M Donahue, M Deustua, S Eisenhardt, P Ellingson, E Faccioli, L Fadeyev, V Fakhouri, HK Fruchter, AS Gilbank, DG Gladders, MD Goldhaber, G Gonzalez, AH Goobar, A Gude, A Hattori, T Hoekstra, H Hsiao, E Huang, X Ihara, Y Jee, MJ Johnston, D Kashikawa, N Koester, B Konishi, K Kowalski, M Linder, EV Lubin, L Melbourne, J Meyers, J Morokuma, T Munshi, F Mullis, C Oda, T Panagia, N Perlmutter, S Postman, M Pritchard, T Rhodes, J Ripoche, P Rosati, P Schlegel, DJ Spadafora, A Stanford, SA Stanishev, V Stern, D Strovink, M Takanashi, N Tokita, K Wagner, M Wang, L Yasuda, N Yee, HKC AF Suzuki, N. Rubin, D. Lidman, C. Aldering, G. Amanullah, R. Barbary, K. Barrientos, L. F. Botyanszki, J. Brodwin, M. Connolly, N. Dawson, K. S. Dey, A. Doi, M. Donahue, M. Deustua, S. Eisenhardt, P. Ellingson, E. Faccioli, L. Fadeyev, V. Fakhouri, H. K. Fruchter, A. S. Gilbank, D. G. Gladders, M. D. Goldhaber, G. Gonzalez, A. H. Goobar, A. Gude, A. Hattori, T. Hoekstra, H. Hsiao, E. Huang, X. Ihara, Y. Jee, M. J. Johnston, D. Kashikawa, N. Koester, B. Konishi, K. Kowalski, M. Linder, E. V. Lubin, L. Melbourne, J. Meyers, J. Morokuma, T. Munshi, F. Mullis, C. Oda, T. Panagia, N. Perlmutter, S. Postman, M. Pritchard, T. Rhodes, J. Ripoche, P. Rosati, P. Schlegel, D. J. Spadafora, A. Stanford, S. A. Stanishev, V. Stern, D. Strovink, M. Takanashi, N. Tokita, K. Wagner, M. Wang, L. Yasuda, N. Yee, H. K. C. CA Supernova Cosmology Project TI THE HUBBLE SPACE TELESCOPE CLUSTER SUPERNOVA SURVEY. V. IMPROVING THE DARK- ENERGY CONSTRAINTS ABOVE z > 1 AND BUILDING AN EARLY-TYPE-HOSTED SUPERNOVA SAMPLE SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmological parameters; distance scale; supernovae: general ID DIGITAL SKY SURVEY; COLOR-MAGNITUDE RELATION; HIGH-REDSHIFT SUPERNOVAE; PROBE WMAP OBSERVATIONS; LASER ADAPTIVE OPTICS; IA LIGHT CURVES; ADVANCED CAMERA; GALAXY CLUSTERS; LEGACY SURVEY; COSMOLOGICAL CONSTRAINTS AB We present Advanced Camera for Surveys, NICMOS, and Keck adaptive-optics-assisted photometry of 20 Type Ia supernovae (SNe Ia) from the Hubble Space Telescope (HST) Cluster Supernova Survey. The SNe Ia were discovered over the redshift interval 0.623 < z < 1.415. Of these SNe Ia, 14 pass our strict selection cuts and are used in combination with the world's sample of SNe Ia to derive the best current constraints on dark energy. Of our new SNe Ia, 10 are beyond redshift z = 1, thereby nearly doubling the statistical weight of HST-discovered SNe Ia beyond this redshift. Our detailed analysis corrects for the recently identified correlation between SN Ia luminosity and host galaxy mass and corrects the NICMOS zero point at the count rates appropriate for very distant SNe Ia. Adding these SNe improves the best combined constraint on dark-energy density,rho(DE)(z), at redshifts 1.0 < z < 1.6 by 18% (including systematic errors). For a flat. CDM universe, we find Omega(A) = 0.729 +/- 0.014 (68% confidence level (CL) including systematic errors). For a flat wCDM model, we measure a constant dark-energy equation-of-state parameter w = -1.013(-0.073)(+0.068) (68% CL). Curvature is constrained to similar to 0.7% in the owCDM model and to similar to 2% in a model in which dark energy is allowed to vary with parameters w(0) and w(a). Further tightening the constraints on the time evolution of dark energy will require several improvements, including high-quality multi-passband photometry of a sample of several dozenz > 1 SNe Ia. We describe how such a sample could be efficiently obtained by targeting cluster fields with WFC3 on board HST. The updated supernova Union2.1 compilation of 580 SNe is available at http://supernova.lbl.gov/Union. C1 [Suzuki, N.; Rubin, D.; Aldering, G.; Barbary, K.; Faccioli, L.; Fakhouri, H. K.; Goldhaber, G.; Hsiao, E.; Huang, X.; Linder, E. V.; Meyers, J.; Perlmutter, S.; Ripoche, P.; Schlegel, D. J.; Spadafora, A.; Strovink, M.] EO Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA. [Suzuki, N.; Rubin, D.; Amanullah, R.; Barbary, K.; Botyanszki, J.; Faccioli, L.; Fakhouri, H. K.; Goldhaber, G.; Gude, A.; Hsiao, E.; Huang, X.; Linder, E. V.; Meyers, J.; Munshi, F.; Perlmutter, S.; Pritchard, T.; Ripoche, P.; Strovink, M.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. [Lidman, C.] Australian Astron Observ, Epping, NSW 1710, Australia. [Amanullah, R.; Goobar, A.] AlbaNova, Oskar Klein Ctr Cosmo Particle Phys, SE-10691 Stockholm, Sweden. [Barrientos, L. F.] Pontificia Univ Catolica Chile, Dept Astron & Astrofis, Santiago, Chile. [Brodwin, M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Connolly, N.] Hamilton Coll, Dept Phys, Clinton, NY 13323 USA. [Dawson, K. S.] Univ Utah, Dept Phys & Astron, Salt Lake City, UT 84112 USA. [Dey, A.] Natl Opt Astron Observ, Tucson, AZ 85726 USA. [Doi, M.; Ihara, Y.; Morokuma, T.; Tokita, K.] Univ Tokyo, Grad Sch Sci, Inst Astron, Mitaka, Tokyo 1810015, Japan. [Donahue, M.; Johnston, D.] Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA. [Deustua, S.; Fruchter, A. S.; Panagia, N.; Postman, M.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Eisenhardt, P.; Rhodes, J.; Stern, D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Ellingson, E.] Univ Colorado, Ctr Astrophys & Space Astron, Boulder, CO 80309 USA. [Fadeyev, V.] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Santa Cruz, CA 94064 USA. [Gilbank, D. G.] Univ Waterloo, Dept Phys & Astron, Waterloo, ON N2L 3G1, Canada. [Gladders, M. D.; Koester, B.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. [Gonzalez, A. H.] Univ Florida, Dept Astron, Gainesville, FL 32611 USA. [Goobar, A.; Stanishev, V.] Stockholm Univ, Albanova Univ Ctr, Dept Phys, SE-10691 Stockholm, Sweden. [Gude, A.] Univ Minnesota, Sch Phys & Astron, Minneapolis, MN 55455 USA. [Hattori, T.] Natl Astron Observ Japan, Subaru Telescope, Hilo, HI 96720 USA. [Hoekstra, H.] Leiden Univ, Leiden Observ, Leiden, Netherlands. [Jee, M. J.; Lubin, L.; Stanford, S. A.] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA. [Johnston, D.] Northwestern Univ, Dept Phys & Astron, Evanston, IL 60208 USA. [Kashikawa, N.; Morokuma, T.; Takanashi, N.] Natl Astron Observ Japan, Tokyo 1818588, Japan. [Koester, B.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Konishi, K.] Univ Tokyo, Inst Cosm Ray Res, Kashiwa, Chiba 2778582, Japan. [Kowalski, M.] Univ Bonn, Inst Phys, Bonn, Germany. [Melbourne, J.; Rhodes, J.] CALTECH, Div Phys Math & Astron, Caltech Opt Observ, Pasadena, CA 91125 USA. [Munshi, F.] Univ Washington, Dept Astron, Seattle, WA 98195 USA. [Mullis, C.] Wachovia Corp, Winston Salem, NC 27101 USA. [Oda, T.] Kyoto Univ, Dept Astron, Sakyo Ku, Kyoto 6068502, Japan. [Pritchard, T.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Rosati, P.] ESO, D-85748 Garching, Germany. [Stanford, S. A.] Lawrence Livermore Natl Lab, Inst Geophys & Planetary Phys, Livermore, CA 94550 USA. [Stanishev, V.] Inst Super Tecn, CENTRA Ctr Multidisciplinar Astrofis, P-1049001 Lisbon, Portugal. [Wagner, M.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Wang, L.] Texas A&M Univ, Dept Phys, College Stn, TX 77843 USA. [Yasuda, N.] Univ Tokyo, Inst Phys & Math Universe, Kashiwa, Chiba 2778583, Japan. [Yee, H. K. C.] Univ Toronto, Dept Astron & Astrophys, Toronto, ON M5S 3H4, Canada. RP Suzuki, N (reprint author), EO Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA. EM nsuzuki@lbl.gov; rubind@berkeley.edu; clidman@aao.gov.au RI Kowalski, Marek/G-5546-2012; Yasuda, Naoki/A-4355-2011; Stanishev, Vallery/M-8930-2013; Perlmutter, Saul/I-3505-2015; OI Stanishev, Vallery/0000-0002-7626-1181; Perlmutter, Saul/0000-0002-4436-4661; Strovink, Mark/0000-0001-7020-7769; Meyers, Joshua/0000-0002-2308-4230; Hoekstra, Henk/0000-0002-0641-3231 FU NASA from the Space Telescope Science Institute [GO-10496]; AURA, Inc., under NASA [NAS 5-26555]; Director, Office of Science, Office of High Energy and Nuclear Physics, of the U.S. Department of Energy [AC02-05CH11231]; JSPS [20040003]; U.S. Department of Energy by Lawrence Livermore National Laboratory [W-7405-Eng-48, DE-AC52-07NA27344]; Japan Society for the Promotion of Science; Netherlands Organization for Scientific Research (WO); Marie Curie International Reintegration Grant FX Financial support for this work was provided by NASA through program GO-10496 from the Space Telescope Science Institute, which is operated by AURA, Inc., under NASA contract NAS 5-26555. This work was also supported in part by the Director, Office of Science, Office of High Energy and Nuclear Physics, of the U.S. Department of Energy under contract No. AC02-05CH11231, as well as a JSPS core-to-core program "International Research Network for Dark Energy" and by JSPS research grant 20040003. Support for M.B. was provided by the W. M. Keck Foundation. The work of S.A.S. was performed under the auspices of the U.S. Department of Energy by Lawrence Livermore National Laboratory in part under Contract W-7405-Eng-48 and in part under contract DE-AC52-07NA27344. The work of P.E., J.R., and D.S. was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA. T.M. and Y.I. have been financially supported by the Japan Society for the Promotion of Science through its Research Fellowship. H.H. acknowledges support from a VIDI grant from the Netherlands Organization for Scientific Research (WO) and a Marie Curie International Reintegration Grant. N.S., C.L., and S.P. wish to thank the support and hospitality of the Aspen Center for Physics, where much of this paper was written. We thank Jay Anderson, L. E. Bergeron, Ralph Bohlin, Roelof de Jong, Anton Koekemoer, Jennifer Mack, Bahram Mobasher, Adam Riess, Kenneth Sembach, and ACS and NICMOS teams at the Space Telescope Science Institute for their advice on the HST data calibration. We also thank Alex Conley for calibration discussions. Finally, we thank our referee, who carefully read our paper and gave valuable feedback. NR 117 TC 673 Z9 678 U1 1 U2 38 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD FEB 10 PY 2012 VL 746 IS 1 AR 85 DI 10.1088/0004-637X/746/1/85 PG 24 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 926VZ UT WOS:000302861300085 ER PT J AU Teodoro, M Damineli, A Arias, JI de Araujo, FX Barba, RH Corcoran, MF Fernandes, MB Fernandez-Lajus, E Fraga, L Gamen, RC Gonzalez, JF Groh, JH Marshall, JL McGregor, PJ Morrell, N Nicholls, DC Parkin, ER Pereira, CB Phillips, MM Solivella, GR Steiner, JE Stritzinger, M Thompson, I Torres, CAO Torres, MAP Herencia, MIZ AF Teodoro, M. Damineli, A. Arias, J. I. de Araujo, F. X. Barba, R. H. Corcoran, M. F. Borges Fernandes, M. Fernandez-Lajus, E. Fraga, L. Gamen, R. C. Gonzalez, J. F. Groh, J. H. Marshall, J. L. McGregor, P. J. Morrell, N. Nicholls, D. C. Parkin, E. R. Pereira, C. B. Phillips, M. M. Solivella, G. R. Steiner, J. E. Stritzinger, M. Thompson, I. Torres, C. A. O. Torres, M. A. P. Zevallos Herencia, M. I. TI He II lambda 4686 IN eta CARINAE: COLLAPSE OF THE WIND-WIND COLLISION REGION DURING PERIASTRON PASSAGE SO ASTROPHYSICAL JOURNAL LA English DT Article DE line: profiles; stars: early-type; stars: individual (eta Carinae); stars: massive ID BINARY V444 CYGNI; X-RAY MINIMUM; COLLIDING-WINDS; SPECTROSCOPIC EVENT; EMISSION-LINES; HD 5980; RADIO-EMISSION; THETA-CARINAE; LIGHT-CURVE; SYSTEM AB The periodic spectroscopic events in eta Carinae are now well established and occur near the periastron passage of two massive stars in a very eccentric orbit. Several mechanisms have been proposed to explain the variations of different spectral features, such as an eclipse by the wind-wind collision (WWC) boundary, a shell ejection from the primary star or accretion of its wind onto the secondary. All of them have problems explaining all the observed phenomena. To better understand the nature of the cyclic events, we performed a dense monitoring of eta Carinae with five Southern telescopes during the 2009 low-excitation event, resulting in a set of data of unprecedented quality and sampling. The intrinsic luminosity of the He II lambda 4686 emission line (L similar to 310 L-circle dot) just before periastron reveals the presence of a very luminous transient source of extreme UV radiation emitted in the WWC region. Clumps in the primary's wind probably explain the flare-like behavior of both the X-ray and He II lambda 4686 light curves. After a short-lived minimum, He II lambda 4686 emission rises again to a new maximum, when X-rays are still absent or very weak. We interpret this as a collapse of the WWC onto the "surface" of the secondary star, switching off the hard X-ray source and diminishing the WWC shock cone. The recovery from this state is controlled by the momentum balance between the secondary's wind and the clumps in the primary's wind. C1 [Teodoro, M.; Damineli, A.; Steiner, J. E.] Univ Sao Paulo, Inst Astron Geofis & Ciencias Atmosfer, BR-05508900 Sao Paulo, Brazil. [Arias, J. I.] Univ La Serena, Dept Fis, La Serena, Chile. [de Araujo, F. X.; Borges Fernandes, M.; Pereira, C. B.; Zevallos Herencia, M. I.] Observ Nacl, BR-20921400 Rio De Janeiro, Brazil. [Barba, R. H.; Gonzalez, J. F.] Consejo Nacl Invest Cient & Tecn, ICATE, San Juan, Argentina. [Corcoran, M. F.] CRESST, Greenbelt, MD 20771 USA. [Corcoran, M. F.] NASA, Goddard Space Flight Ctr, Xray Astrophys Lab, Greenbelt, MD 20771 USA. [Fernandez-Lajus, E.; Gamen, R. C.; Solivella, G. R.] Univ Nacl La Plata, Fac Ciencias Astron & Geofis, La Plata, BA, Argentina. [Fraga, L.] So Observ Astrophys Res, La Serena, Chile. [Groh, J. H.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Marshall, J. L.] Texas A&M Univ, Dept Phys & Astron, College Stn, TX 77843 USA. [McGregor, P. J.; Nicholls, D. C.; Parkin, E. R.] RSAA, Mt Stromlo Observ, Weston, ACT 2611, Australia. [Morrell, N.; Phillips, M. M.] Observ Carnegie Inst Washington, Las Campanas Observ, La Serena, Chile. [Stritzinger, M.] Stockholm Univ, Dept Astron, Oskar Klein Ctr, S-10691 Stockholm, Sweden. [Thompson, I.] Observ Carnegie Inst, Pasadena, CA 91101 USA. [Torres, C. A. O.] Lab Nacl Astrofis, BR-37504364 Bairro Das Nacoes, Itajuba, Brazil. [Torres, M. A. P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Teodoro, M (reprint author), Univ Sao Paulo, Inst Astron Geofis & Ciencias Atmosfer, Rua Matao 1226,Cidade Univ, BR-05508900 Sao Paulo, Brazil. EM mairan@astro.iag.usp.br RI Borges Fernandes, Marcelo/K-6210-2016; Pereira, Claudio/L-3199-2016; Damineli, Augusto/D-8210-2012; 7, INCT/H-6207-2013; Teodoro, Mairan/H-9123-2013; Astrofisica, Inct/H-9455-2013; Damineli, Augusto/P-8829-2016; Barba, Rodolfo/P-4649-2014; Gamen, Roberto/A-1728-2015 OI Damineli, Augusto/0000-0002-7978-2994; Damineli, Augusto/0000-0002-7978-2994; Barba, Rodolfo/0000-0003-1086-1579; FU FAPESP [05/00190-8, 09/08013-9]; CNPq; Conselho Nacional de Desenvolvimento Cientifico e Tecnologico (CNPq-Brazil); NASA; Chandra [G07-8022A, G08-9018A, G09-0016A, GO0-11039A]; RXTE Guest Observer facility at NASA/GSFC FX We thank the referee for questions and suggestions that led to a clarification of the ideas discussed in this paper. M. T., A. D., and J.E.S. are grateful to the Brazilian agencies FAPESP and CNPq for continuous financial support. M. T. is supported through grants FAPESP 05/00190-8 and 09/08013-9. M. B. F. acknowledges Conselho Nacional de Desenvolvimento Cientifico e Tecnologico (CNPq-Brazil) for the post-doctoral grant. M. F. C. gratefully acknowledges support from NASA and Chandra via grants G07-8022A, G08-9018A, G09-0016A, and GO0-11039A, along with continued aid from the RXTE Guest Observer facility at NASA/GSFC. Calculations were performed with version 07.02 of Cloudy, last described by Ferland et al. (1998). This research has made use of NASA's Astrophysics Data System. In addition, this research has made use of data obtained from the High Energy Astrophysics Science Archive Research Center (HEASARC), provided by NASA's Goddard Space Flight Center. NR 86 TC 18 Z9 18 U1 1 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 10 PY 2012 VL 746 IS 1 AR 73 DI 10.1088/0004-637X/746/1/73 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 926VZ UT WOS:000302861300073 ER PT J AU Todorov, KO Deming, D Knutson, HA Burrows, A Sada, PV Cowan, NB Agol, E Desert, JM Fortney, JJ Charbonneau, D Laughlin, G Langton, J Showman, AP Lewis, NK AF Todorov, Kamen O. Deming, Drake Knutson, Heather A. Burrows, Adam Sada, Pedro V. Cowan, Nicolas B. Agol, Eric Desert, Jean-Michel Fortney, Jonathan J. Charbonneau, David Laughlin, Gregory Langton, Jonathan Showman, Adam P. Lewis, Nikole K. TI WARM SPITZER OBSERVATIONS OF THREE HOT EXOPLANETS: XO-4b, HAT-P-6b, AND HAT-P-8b SO ASTROPHYSICAL JOURNAL LA English DT Article DE eclipses; planetary systems; techniques: photometric ID INFRARED-EMISSION SPECTRUM; SECONDARY ECLIPSE PHOTOMETRY; EXTRASOLAR PLANET; THERMAL EMISSION; TEMPERATURE INVERSION; HD 189733B; TRANSITING PLANET; GIANT PLANETS; LIGHT CURVES; F-STAR AB We analyze Warm Spitzer/Infrared Array Camera observations of the secondary eclipses of three planets, XO-4b, HAT-P-6b, and HAT-P-8b. We measure secondary eclipse amplitudes at 3.6 mu m and 4.5 mu m for each target. XO-4b exhibits a stronger eclipse depth at 4.5 mu m than at 3.6 mu m, which is consistent with the presence of a temperature inversion. HAT-P-8b shows a stronger eclipse amplitude at 3.6 mu m and is best described by models without a temperature inversion. The eclipse depths of HAT-P-6b can be fitted with models with a small or no temperature inversion. We consider our results in the context of a postulated relationship between stellar activity and temperature inversion and a relationship between irradiation level and planet dayside temperature, as discussed by Knutson et al. and Cowan & Agol, respectively. Our results are consistent with these hypotheses, but do not significantly strengthen them. To measure accurate secondary eclipse central phases, we require accurate ephemerides. We obtain primary transit observations and supplement them with publicly available observations to update the orbital ephemerides of the three planets. Based on the secondary eclipse timing, we set upper boundaries for e cos(omega) for HAT-P-6b, HAT-P-8b, and XO-4b and find that the values are consistent with circular orbits. C1 [Todorov, Kamen O.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Deming, Drake] NASA, Goddard Space Flight Ctr, Planetary Syst Lab, Greenbelt, MD 20771 USA. [Knutson, Heather A.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. [Knutson, Heather A.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Burrows, Adam] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. [Sada, Pedro V.] Univ Monterrey, Dept Math & Phys, Monterrey, Mexico. [Cowan, Nicolas B.] Northwestern Univ, Dept Phys & Astron, Evanston, IL 60208 USA. [Agol, Eric] Univ Washington, Dept Astron, Seattle, WA 98195 USA. [Desert, Jean-Michel; Charbonneau, David] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Fortney, Jonathan J.; Laughlin, Gregory] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. [Langton, Jonathan] Principia Coll, Dept Phys, Elsah, IL 62028 USA. [Showman, Adam P.; Lewis, Nikole K.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA. [Todorov, Kamen O.] Penn State Univ, Ctr Exoplanets & Habitable Worlds, University Pk, PA 16802 USA. RP Todorov, KO (reprint author), Penn State Univ, Dept Astron & Astrophys, 525 Davey Lab, University Pk, PA 16802 USA. RI Agol, Eric/B-8775-2013; OI Agol, Eric/0000-0002-0802-9145; Fortney, Jonathan/0000-0002-9843-4354; Todorov, Kamen/0000-0002-9276-8118; Charbonneau, David/0000-0002-9003-484X FU NASA through JPL/Caltech; NASA; Pennsylvania State University; Eberly College of Science; Pennsylvania Space Grant Consortium 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. The Center for Exoplanets and Habitable Worlds is supported by the Pennsylvania State University, the Eberly College of Science, and the Pennsylvania Space Grant Consortium. We thank the anonymous referee for a careful review of this paper. NR 51 TC 29 Z9 30 U1 0 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 10 PY 2012 VL 746 IS 1 AR 111 DI 10.1088/0004-637X/746/1/111 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 926VZ UT WOS:000302861300111 ER PT J AU Torrey, P Cox, TJ Kewley, L Hernquist, L AF Torrey, Paul Cox, T. J. Kewley, Lisa Hernquist, Lars TI THE METALLICITY EVOLUTION OF INTERACTING GALAXIES SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: abundances; galaxies: evolution; galaxies: interactions; galaxies: ISM ID PARTICLE HYDRODYNAMICS SIMULATIONS; STAR-FORMING GALAXIES; DIGITAL SKY SURVEY; STELLAR MASS-LOSS; H-II REGIONS; COSMOLOGICAL SIMULATIONS; CHEMICAL ENRICHMENT; ELLIPTIC GALAXIES; MERGER REMNANTS; SPIRAL GALAXIES AB Nuclear inflows of metal-poor interstellar gas triggered by galaxy interactions can account for the systematically lower central oxygen abundances observed in local interacting galaxies. Here, we investigate the metallicity evolution of a large set of simulations of colliding galaxies. Our models include cooling, star formation, feedback, and a new stochastic method for tracking the mass recycled back to the interstellar medium from stellar winds and supernovae. We study the influence of merger-induced inflows, enrichment, gas consumption, and galactic winds in determining the nuclear metallicity. The central metallicity is primarily a competition between the inflow of low-metallicity gas and enrichment from star formation. An average depression in the nuclear metallicity of similar to 0.07 is found for gas-poor disk-disk interactions. Gas-rich disk-disk interactions, on the other hand, typically have an enhancement in the central metallicity that is positively correlated with the gas content. The simulations fare reasonably well when compared to the observed mass-metallicity and separation-metallicity relationships, but further study is warranted. C1 [Torrey, Paul; Hernquist, Lars] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Cox, T. J.] Observ Carnegie Inst Washington, Pasadena, CA 91101 USA. [Kewley, Lisa] Mt Stromlo & Siding Spring Observ, Res Sch Astron & Astrophys, Weston, ACT 2611, Australia. RP Torrey, P (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. OI Torrey, Paul/0000-0002-5653-0786 NR 84 TC 62 Z9 62 U1 1 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 10 PY 2012 VL 746 IS 1 AR 108 DI 10.1088/0004-637X/746/1/108 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 926VZ UT WOS:000302861300108 ER PT J AU Janiak, DS Whitlatch, RB AF Janiak, Dean S. Whitlatch, Robert B. TI Epifaunal and algal assemblages associated with the native Chondrus crispus (Stackhouse) and the non-native Grateloupia turuturu (Yamada) in eastern Long Island Sound SO JOURNAL OF EXPERIMENTAL MARINE BIOLOGY AND ECOLOGY LA English DT Article DE Chondrus crispus; Grateloupia turuturu; Invasive algae; Long Island Sound; Mesograzers ID FRAGILE SSP TOMENTOSOIDES; SARGASSUM-MUTICUM PHAEOPHYTA; LACUNA-VINCTA MONTAGU; HABITAT COMPLEXITY; DORYPHORA HALYMENIACEAE; INTRODUCED SEAWEEDS; UNDARIA-PINNATIFIDA; FEEDING PREFERENCE; NOVA-SCOTIA; GREEN-ALGA AB Although the spread of non-native algae is rapidly escalating, relatively few ecological studies have been done to gauge the impacts incurred to native flora and fauna. A reduction in the dominance of a native habitat-forming macroalga due to the replacement by an introduced species can have adverse effects on the community. The non-native red alga Grateloupia turuturu, first reported in Rhode Island, USA in 1994, has since extended its southern range into eastern Long Island Sound. This large alga has the potential to impact coastal communities by altering the floristic composition important to associated flora and fauna. A comparison of algal and epifaunal assemblages was made during 2006 and 2007 between native and non-native algal communities dominated by either G. turuturu or the native, Chondrus crispus at two sites in Long Island Sound. We found that within Grateloupia-dominated habitat, there was a large decrease in overall macrophyte biomass as compared to native habitat. We also found that habitat dominated by the non-native alga reduced species richness and total abundance of invertebrates relative to nearby habitats dominated by C. crispus. In addition, we found that the dominant mesofaunal species, important to higher trophic level consumers, had greatly reduced densities in communities dominated by the non-native alga. Published by Elsevier B.V. C1 [Janiak, Dean S.; Whitlatch, Robert B.] Univ Connecticut, Dept Marine Sci, Groton, CT 06340 USA. RP Janiak, DS (reprint author), Smithsonian Environm Res Ctr, POB 28,647 Contees Wharf Rd, Edgewater, MD 21037 USA. EM janiakd@si.edu; robert.whitlatch@uconn.edu FU Connecticut Sea Grant FX Funding was generously provided by the Connecticut Sea Grant made to R.B. Whitlatch. We greatly appreciate the field and lab assistance of all members of Team Benthos including L Stefaniak, J. Reinhardt, R. Patrylak, and N. Blaschik. The manuscript was greatly improved from comments by R.W. Osman and 2 anonymous reviewers. [ST] NR 56 TC 15 Z9 15 U1 2 U2 27 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0022-0981 EI 1879-1697 J9 J EXP MAR BIOL ECOL JI J. Exp. Mar. Biol. Ecol. PD FEB 10 PY 2012 VL 413 BP 38 EP 44 DI 10.1016/j.jembe.2011.11.016 PG 7 WC Ecology; Marine & Freshwater Biology SC Environmental Sciences & Ecology; Marine & Freshwater Biology GA 902IJ UT WOS:000301031500006 ER PT J AU Long, WC Hines, AH AF Long, William Christopher Hines, Anson H. TI Scale and the guild functional response: Density-dependent predation varies with plot size SO JOURNAL OF EXPERIMENTAL MARINE BIOLOGY AND ECOLOGY LA English DT Article DE Density-dependent effects; Functional response; Mercenaria mercenaria; Predation; Spatial scale ID CRABS CALLINECTES-SAPIDUS; BLUE CRABS; PATCH SIZE; SPATIAL-DISTRIBUTION; FISH POPULATIONS; PREY MORTALITY; INTERFERENCE; PATTERNS; BIVALVE; LANDSCAPE AB The predator functional response is an important mechanism determining the persistence of prey species; however, little is known about the effects of spatial scale on the functional response. We used a manipulative field experiment to quantify the effects of plot size on the guild functional response on the clam Mercenaria mercenaria, replicating the experiment in the summer in Chesapeake Bay, Virginia, and in the spring and fall in Indian River Lagoon, Florida, to examine the effects of predator and alternative prey abundance. In Virginia, the predation rate increased with both patch size and predator density, and was described by a modified sigmoid Type III functional response model that incorporated the effects of patch size. In Florida in the spring, the predator functional response was a Type III and did not vary with plot size, but in the fall it was a linear Type I at small plot sizes, and a Type III at a larger plot size. We hypothesize that the difference is primarily driven by changes in predator abundance and species between sites. In showing that the functional response can vary with plot size and season, our results indicate that small-scale experiments do not always scale up spatially or temporally. We suggest that the predictive power of such experiments may be limited by the complexity of the food web. Published by Elsevier B.V. C1 [Long, William Christopher; Hines, Anson H.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. RP Long, WC (reprint author), Natl Ocean & Atmospher Adm, Kodiak Lab, Resource Assessment & Conservat Engn Div, Alaska Fisheries Sci Ctr,Natl Marine Fisheries Se, 301 Res Court, Kodiak, AK 99615 USA. EM Chris.Long@noaa.gov RI Long, William/C-7074-2009 OI Long, William/0000-0002-7095-1245 FU PADI Foundation; Smithsonian Marine Science Network; NOAA Chesapeake Bay Program Office to the Blue Crab Advanced Research Consortium FX We thank J. Majoris, B. Tunberg, S. Reed, M. Jones, M. Stevens, E. Linley, J. Lin, H. Reichardt, M. Luckenbach and all the staff and scientists at the Smithsonian Marine Station at Fort Pierce, Florida, and the Virginia Institute of Marine Science's Eastern Shore Laboratory for help with planning, field work, and laboratory work. We thank Judge Northam for letting us use his property and boat ramp. We thank Cherrystone Aquafarms and Clams R Us for providing clams. Critical comments on earlier versions of this paper by J. Long, R. Foy, the AFSC publications office, and anonymous reviewers substantially improved the manuscript. Funding was provided by a grant from the PADI Foundation to WCL, a Smithsonian Marine Science Network Postdoctoral Fellowship to WCL, and from the NOAA Chesapeake Bay Program Office to the Blue Crab Advanced Research Consortium. The findings and conclusions in the paper are those of the authors and do not necessarily represent the views of the National Marine Fisheries Service, NOAA. [ST] NR 35 TC 5 Z9 5 U1 1 U2 22 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0022-0981 J9 J EXP MAR BIOL ECOL JI J. Exp. Mar. Biol. Ecol. PD FEB 10 PY 2012 VL 413 BP 50 EP 55 DI 10.1016/j.jembe.2011.11.015 PG 6 WC Ecology; Marine & Freshwater Biology SC Environmental Sciences & Ecology; Marine & Freshwater Biology GA 902IJ UT WOS:000301031500008 ER PT J AU Cohen, O Drake, JJ Kashyap, VL AF Cohen, O. Drake, J. J. Kashyap, V. L. TI THE ROLE OF WHITE DWARFS IN CATACLYSMIC VARIABLE SPIN-DOWN SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE binaries: close; stars: coronae; stars: magnetic field ID ANGULAR-MOMENTUM LOSS; HERCULIS TYPE SYSTEMS; X-RAY BINARIES; MAGNETIC BRAKING; SOLAR-WIND; SYNCHRONOUS ROTATION; PERIOD GAP; STARS; EVOLUTION AB We study the effect of a white dwarf on the spin-down of a cataclysmic variable (CV) system using a three-dimensional magnetohydrodynamic numerical model. The model includes the stellar corona, the stellar wind, and the WD mass and magnetic field. The existence of the WD modifies the system spin-down by physically blocking the stellar wind, restructuring the wind, channeling the wind toward the WD surface, and modifying the shape and size of the Alfven surface. The combination of these processes differs among a set of simple test cases, and the resulting angular momentum loss rates vary by factors of 2-3, and by factors of 2 relative to a test model with a single M dwarf. While the model employs some simplifications, the results suggest that angular momentum loss schemes currently employed in CV studies do not require drastic revision. Insights are also gained on wind accretion. We find that efficient accretion switches on quite rapidly with decreasing orbital separation. Accretion rates depend on magnetic field alignment and should be modulated by magnetic cycles on the M dwarf. For particular values of white dwarf magnetic field strength, an efficient syphoning of coronal plasma from the inward facing M dwarf hemisphere occurs. Wind accretion rates are expected to vary by factors of 10 or more between fairly similar close binaries, depending on magnetic field strengths and orbital separation. C1 [Cohen, O.; Drake, J. J.; Kashyap, V. L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Cohen, O (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. OI Cohen, Ofer/0000-0003-3721-0215 FU NASA-LWSTRT [NNG05GM44G]; NASA [NAS8-39073]; NASA-ESS; NASA-ESTO-CT; NSF-KDI; DoD-MURI FX We thank an anonymous referee for her/his report. O.C. is supported by NASA-LWSTRT Grant NNG05GM44G. J.D. and V. L. K. were funded by NASA contract NAS8-39073 to the Chandra X-ray Center. Simulation results were obtained using the Space-Weather-Modeling-Framework, developed by the CSEM, at the U. Michigan with funding support from NASA-ESS, NASA-ESTO-CT, NSF-KDI, and DoD-MURI. NR 34 TC 4 Z9 4 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD FEB 10 PY 2012 VL 746 IS 1 AR L3 DI 10.1088/2041-8205/746/1/L3 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 892ZD UT WOS:000300323500003 ER PT J AU Fu, RR Moullet, A Patel, NA Biersteker, J Derose, KL Young, KH AF Fu, Roger R. Moullet, Arielle Patel, Nimesh A. Biersteker, John Derose, Kimberly L. Young, Kenneth H. TI ARCSECOND RESOLUTION MAPPING OF SULFUR DIOXIDE EMISSION IN THE CIRCUMSTELLAR ENVELOPE OF VY CANIS MAJORIS SO ASTROPHYSICAL JOURNAL LA English DT Article DE astrochemistry; circumstellar matter; radio lines: stars; stars: individual (VY CMa); stars: late-type; supergiants ID LINE INTENSITY RATIOS; GIANT BRANCH STARS; MASS-LOSS RATES; APERTURE SYNTHESIS; RED SUPERGIANTS; SO2; CHEMISTRY; NEBULA; SPECTROSCOPY; DIAGNOSTICS AB We report Submillimeter Array observations of SO2 emission in the circumstellar envelope (CSE) of the red supergiant VY Canis Majoris, with an angular resolution of approximate to 1 ''. SO2 emission appears in three distinct outflow regions surrounding the central continuum peak emission that is spatially unresolved. No bipolar structure is noted in the sources. A fourth source of SO2 is identified as a spherical wind centered at the systemic velocity. We estimate the SO2 column density and rotational temperature assuming local thermal equilibrium (LTE) as well as perform non-LTE radiative transfer analysis using RADEX. Column densities of SO2 are found to be similar to 10(16) cm(-2) in the outflows and in the spherical wind. Comparison with existing maps of the two parent species OH and SO shows the SO2 distribution to be consistent with that of OH. The abundance ratio f(SO2)/fSO is greater than unity for all radii larger than 3 x 10(16) cm. SO2 is distributed in fragmented clumps compared to SO, PN, and SiS molecules. These observations lend support to specific models of circumstellar chemistry that predict f(SO2)/f(SO) > 1 and may suggest the role of localized effects such as shocks in the production of SO2 in the CSE. C1 [Fu, Roger R.; Moullet, Arielle; Patel, Nimesh A.; Biersteker, John; Derose, Kimberly L.; Young, Kenneth H.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Fu, Roger R.] MIT, Dept Earth Atmospher & Planetary Sci, Cambridge, MA USA. RP Fu, RR (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM npatel@cfa.harvard.edu NR 36 TC 9 Z9 9 U1 3 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 10 PY 2012 VL 746 IS 1 DI 10.1088/0004-637X/746/1/42 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 926VZ UT WOS:000302861300042 ER PT J AU Fressin, F Torres, G Rowe, JF Charbonneau, D Rogers, LA Ballard, S Batalha, NM Borucki, WJ Bryson, ST Buchhave, LA Ciardi, DR Desert, JM Dressing, CD Fabrycky, DC Ford, EB Gautier, TN Henze, CE Holman, MJ Howard, A Howell, SB Jenkins, JM Koch, DG Latham, DW Lissauer, JJ Marcy, GW Quinn, SN Ragozzine, D Sasselov, DD Seager, S Barclay, T Mullally, F Seader, SE Still, M Twicken, JD Thompson, SE Uddin, K AF Fressin, Francois Torres, Guillermo Rowe, Jason F. Charbonneau, David Rogers, Leslie A. Ballard, Sarah Batalha, Natalie M. Borucki, William J. Bryson, Stephen T. Buchhave, Lars A. Ciardi, David R. Desert, Jean-Michel Dressing, Courtney D. Fabrycky, Daniel C. Ford, Eric B. Gautier, Thomas N., III Henze, Christopher E. Holman, Matthew J. Howard, Andrew Howell, Steve B. Jenkins, Jon M. Koch, David G. Latham, David W. Lissauer, Jack J. Marcy, Geoffrey W. Quinn, Samuel N. Ragozzine, Darin Sasselov, Dimitar D. Seager, Sara Barclay, Thomas Mullally, Fergal Seader, Shawn E. Still, Martin Twicken, Joseph D. Thompson, Susan E. Uddin, Kamal TI Two Earth-sized planets orbiting Kepler-20 SO NATURE LA English DT Article ID TRANSITING PLANET; BLEND SCENARIOS; MULTIPLE SYSTEM; GIANT IMPACTS; CANDIDATES; VALIDATION; EXOPLANETS; COMPANION AB Since the discovery of the first extrasolar giant planets around Sun-like stars(1,2), evolving observational capabilities have brought us closer to the detection of true Earth analogues. The size of an exoplanet can be determined when it periodically passes in front of (transits) its parent star, causing a decrease in starlight proportional to its radius. The smallest exoplanet hitherto discovered(3) has a radius 1.42 times that of the Earth's radius (R-circle plus), and hence has 2.9 times its volume. Here we report the discovery of two planets, one Earth-sized (1.03 R-circle plus) and the other smaller than the Earth (0.87 R-circle plus), orbiting the star Kepler-20, which is already known to host three other, larger, transiting planets(4). The gravitational pull of the new planets on the parent star is too small to measure with current instrumentation. We apply a statistical method to show that the likelihood of the planetary interpretation of the transit signals is more than three orders of magnitude larger than that of the alternative hypothesis that the signals result from an eclipsing binary star. Theoretical considerations imply that these planets are rocky, with a composition of iron and silicate. The outer planet could have developed a thick water vapour atmosphere. C1 [Fressin, Francois; Torres, Guillermo; Charbonneau, David; Ballard, Sarah; Desert, Jean-Michel; Dressing, Courtney D.; Holman, Matthew J.; Latham, David W.; Quinn, Samuel N.; Ragozzine, Darin; Sasselov, Dimitar D.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Rowe, Jason F.; Borucki, William J.; Bryson, Stephen T.; Henze, Christopher E.; Howell, Steve B.; Koch, David G.; Lissauer, Jack J.; Barclay, Thomas; Still, Martin] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Rogers, Leslie A.; Seager, Sara] MIT, Dept Phys, Cambridge, MA 02139 USA. [Batalha, Natalie M.] San Jose State Univ, Dept Phys & Astron, San Jose, CA 95192 USA. [Buchhave, Lars A.] Univ Copenhagen, Niels Bohr Inst, DK-2100 Copenhagen, Denmark. [Buchhave, Lars A.] Univ Copenhagen, Ctr Star & Planet Format, DK-1350 Copenhagen, Denmark. [Ciardi, David R.] CALTECH, NASA Exoplanet Sci Inst, Pasadena, CA 91125 USA. [Fabrycky, Daniel C.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. [Ford, Eric B.] Univ Florida, Dept Astron, Gainesville, FL 32111 USA. [Gautier, Thomas N., III] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Howard, Andrew; Marcy, Geoffrey W.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Jenkins, Jon M.; Mullally, Fergal; Seader, Shawn E.; Twicken, Joseph D.; Thompson, Susan E.] NASA, Ames Res Ctr, SETI Inst, Moffett Field, CA 94035 USA. [Uddin, Kamal] NASA, Ames Res Ctr, Orbital Sci Corp, Moffett Field, CA 94035 USA. RP Fressin, F (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM ffressin@cfa.harvard.edu RI Ragozzine, Darin/C-4926-2013; OI Buchhave, Lars A./0000-0003-1605-5666; Ciardi, David/0000-0002-5741-3047; Charbonneau, David/0000-0002-9003-484X; Barclay, Thomas/0000-0001-7139-2724; Fabrycky, Daniel/0000-0003-3750-0183 FU NASA's Science Mission Directorate FX Kepler was competitively selected as the tenth Discovery mission. Funding for this mission is provided by NASA's Science Mission Directorate. NR 28 TC 93 Z9 93 U1 7 U2 53 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 0028-0836 J9 NATURE JI Nature PD FEB 9 PY 2012 VL 482 IS 7384 BP 195 EP 198 DI 10.1038/nature10780 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 888HI UT WOS:000299994100033 PM 22186831 ER PT J AU Nie, ZL Sun, H Manchester, SR Meng, Y Luke, Q Wen, J AF Nie, Ze-Long Sun, Hang Manchester, Steven R. Meng, Ying Luke, Quentin Wen, Jun TI Evolution of the intercontinental disjunctions in six continents in the Ampelopsis clade of the grape family (Vitaceae) SO BMC EVOLUTIONARY BIOLOGY LA English DT Article ID LONG-DISTANCE DISPERSAL; EASTERN NORTH-AMERICA; HISTORICAL BIOGEOGRAPHY; SOUTHERN-HEMISPHERE; DNA-SEQUENCES; TRANSOCEANIC DISPERSAL; ANEMONE RANUNCULACEAE; PHYLOGENETIC TREES; FLOWERING PLANTS; GEOGRAPHIC RANGE AB Background: The Ampelopsis clade (Ampelopsis and its close allies) of the grape family Vitaceae contains ca. 43 species disjunctly distributed in Asia, Europe, North America, South America, Africa, and Australia, and is a rare example to study both the Northern and the Southern Hemisphere intercontinental disjunctions. We reconstruct the temporal and spatial diversification of the Ampelopsis clade to explore the evolutionary processes that have resulted in their intercontinental disjunctions in six continents. Results: The Bayesian molecular clock dating and the likelihood ancestral area analyses suggest that the Ampelopsis clade most likely originated in North America with its crown group dated at 41.2 Ma (95% HPD 23.4 - 61.0 Ma) in the middle Eocene. Two independent Laurasian migrations into Eurasia are inferred to have occurred in the early Miocene via the North Atlantic land bridges. The ancestor of the Southern Hemisphere lineage migrated from North America to South America in the early Oligocene. The Gondwanan-like pattern of intercontinental disjunction is best explained by two long-distance dispersals: once from South America to Africa estimated at 30.5 Ma (95% HPD 16.9 - 45.9 Ma), and the other from South America to Australia dated to 19.2 Ma (95% HPD 6.7 - 22.3 Ma). Conclusions: The global disjunctions in the Ampelopsis clade are best explained by a diversification model of North American origin, two Laurasian migrations, one migration into South America, and two post-Gondwanan long-distance dispersals. These findings highlight the importance of both vicariance and long distance dispersal in shaping intercontinental disjunctions of flowering plants. C1 [Nie, Ze-Long; Wen, Jun] Natl Museum Nat Hist, Smithsonian Inst, Dept Bot, Washington, DC 20013 USA. [Nie, Ze-Long; Sun, Hang; Meng, Ying] Chinese Acad Sci, Kunming Inst Bot, Key Lab Biodivers & Biogeog, Kunming 650204, Yunnan, Peoples R China. [Manchester, Steven R.] Univ Florida, Florida Museum Nat Hist, Gainesville, FL 32611 USA. [Meng, Ying] Chinese Acad Sci, Kunming Inst Bot, Inst Tibetan Plateau Res Kunming, Kunming 650204, Yannan, Peoples R China. [Luke, Quentin] Natl Museums Kenya, E African Herbarium, Nairobi 00502, Kenya. RP Wen, J (reprint author), Natl Museum Nat Hist, Smithsonian Inst, Dept Bot, MRC 166, Washington, DC 20013 USA. EM wenj@si.edu FU National Science Foundation [DEB 0743474]; Natural Science Foundation of China (NSFC) [31061160184, 31129001]; NSFC-Yunnan [U1136601]; John D and Catherine T MacArthur Foundation; Laboratory of Analytical Biology of National Museum of Natural History; Smithsonian Institution; National Museum of Natural History FX This study was supported by grants from the National Science Foundation (DEB 0743474 to SR Manchester and J Wen), the Natural Science Foundation of China (NSFC 31061160184 to H Sun and 31129001 to J Wen), the NSFC-Yunnan Joint project (U1136601 to H Sun), and the John D and Catherine T MacArthur Foundation (to J Wen, R Ree, and G Mueller). Laboratory work was conducted in and partially supported by the Laboratory of Analytical Biology of the National Museum of Natural History, the Smithsonian Institution. Fieldwork in North America was supported by the Small Grants Program of the National Museum of Natural History, the Smithsonian Institution. Michael Nee, Maurizio Rossetto, Ihsan Al-Shehbaz, and Daigui Zhang kindly helped with the sample collection. NR 101 TC 23 Z9 23 U1 1 U2 30 PU BIOMED CENTRAL LTD PI LONDON PA 236 GRAYS INN RD, FLOOR 6, LONDON WC1X 8HL, ENGLAND SN 1471-2148 J9 BMC EVOL BIOL JI BMC Evol. Biol. PD FEB 8 PY 2012 VL 12 AR 17 DI 10.1186/1471-2148-12-17 PG 13 WC Evolutionary Biology; Genetics & Heredity SC Evolutionary Biology; Genetics & Heredity GA 907QE UT WOS:000301431600001 PM 22316163 ER PT J AU Ibanez, R Jaramillo, CA Solis, FA AF Ibanez D, Roberto Jaramillo A, Cesar A. Solis, Frank A. TI Description of the advertisement call of a species without vocal sac: Craugastor gollmeri (Amphibia: Craugastoridae) SO ZOOTAXA LA English DT Letter ID FROGS C1 [Ibanez D, Roberto; Jaramillo A, Cesar A.] Smithsonian Trop Res Inst, Panama City, Panama. [Ibanez D, Roberto; Jaramillo A, Cesar A.; Solis, Frank A.] Circulo Herpetol Panama, Panama City, Panama. [Ibanez D, Roberto; Solis, Frank A.] Univ Panama, Dept Zool, Panama City, Panama. [Jaramillo A, Cesar A.] Univ Panama, Dept Histol & Neuroanat Humana, Panama City, Panama. RP Ibanez, R (reprint author), Smithsonian Trop Res Inst, Apdo 0843-03092, Panama City, Panama. EM ibanezr@si.edu; jaramilc@si.edu; franksolisa@yahoo.es NR 10 TC 2 Z9 2 U1 0 U2 0 PU MAGNOLIA PRESS PI AUCKLAND PA PO BOX 41383, AUCKLAND, ST LUKES 1030, NEW ZEALAND SN 1175-5326 EI 1175-5334 J9 ZOOTAXA JI Zootaxa PD FEB 6 PY 2012 IS 3184 BP 67 EP 68 PG 2 WC Zoology SC Zoology GA 891VZ UT WOS:000300246200005 ER PT J AU Velez-Juarbe, J Domning, DP Pyenson, ND AF Velez-Juarbe, Jorge Domning, Daryl P. Pyenson, Nicholas D. TI Iterative Evolution of Sympatric Seacow (Dugongidae, Sirenia) Assemblages during the Past similar to 26 Million Years SO PLOS ONE LA English DT Article ID CETACEANS CENOZOIC DRIVERS; BODY-SIZE; ENVIRONMENTAL-CHANGE; ECOLOGICAL CHANGE; CARIBBEAN REGION; FOSSIL SIRENIA; WEST ATLANTIC; MODERN WHALES; MIOCENE; COMMUNITIES AB Extant sirenians show allopatric distributions throughout most of their range. However, their fossil record shows evidence of multispecies communities throughout most of the past similar to 26 million years, in different oceanic basins. Morphological differences among co-occurring sirenian taxa suggest that resource partitioning played a role in structuring these communities. We examined body size and ecomorphological differences (e.g., rostral deflection and tusk morphology) among sirenian assemblages from the late Oligocene of Florida, early Miocene of India and early Pliocene of Mexico; each with three species of the family Dugongidae. Although overlapping in several ecomorphological traits, each assemblage showed at least one dominant trait in which coexisting species differed. Fossil sirenian occurrences occasionally are monotypic, but the assemblages analyzed herein show iterative evolution of multispecies communities, a phenomenon unparalleled in extant sirenian ecology. As primary consumers of seagrasses, these communities likely had a strong impact on past seagrass ecology and diversity, although the sparse fossil record of seagrasses limits direct comparisons. Nonetheless, our results provide robust support for previous suggestions that some sirenians in these extinct assemblages served as keystone species, controlling the dominance of climax seagrass species, permitting more taxonomically diverse seagrass beds (and sirenian communities) than many of those observed today. C1 [Velez-Juarbe, Jorge; Domning, Daryl P.] Howard Univ, Dept Anat, Lab Evolutionary Biol, Washington, DC 20059 USA. [Velez-Juarbe, Jorge; Domning, Daryl P.; Pyenson, Nicholas D.] Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20560 USA. [Pyenson, Nicholas D.] Univ Washington, Burke Museum Nat Hist & Culture, Dept Mammal, Seattle, WA 98195 USA. [Pyenson, Nicholas D.] Univ Washington, Burke Museum Nat Hist & Culture, Dept Paleontol, Seattle, WA 98195 USA. RP Velez-Juarbe, J (reprint author), Howard Univ, Dept Anat, Lab Evolutionary Biol, Washington, DC 20059 USA. EM velezjuarbe@gmail.com FU Washington-Baltimore-Hampton-Roads Louis Stokes Alliance for Minority Participation Bridge; National Museum of Natural History, Smithsonian Institution; Smithsonian Institution; National Science Foundation [0929117] FX JVJ was partially supported by the Washington-Baltimore-Hampton-Roads Louis Stokes Alliance for Minority Participation Bridge to the Doctorate Program at Howard University and a predoctoral fellowship from the National Museum of Natural History, Smithsonian Institution. NDP was also supported by funding from the Smithsonian Institution. Ongoing work by DPD and JVJ is supported by National Science Foundation Earth Sciences grant no. 0929117. The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 64 TC 23 Z9 23 U1 1 U2 25 PU PUBLIC LIBRARY SCIENCE PI SAN FRANCISCO PA 185 BERRY ST, STE 1300, SAN FRANCISCO, CA 94107 USA SN 1932-6203 J9 PLOS ONE JI PLoS One PD FEB 3 PY 2012 VL 7 IS 2 AR e31294 DI 10.1371/journal.pone.0031294 PG 8 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 917LO UT WOS:000302178400034 PM 22319622 ER PT J AU Rando, JC Pieper, H Alcover, JA Olson, SL AF Carlos Rando, Juan Pieper, Harald Antoni Alcover, Josep Olson, Storrs L. TI A new species of extinct fossil scops owl (Aves: Strigiformes: Strigidae: Otus) from the Archipelago of Madeira (North Atlantic Ocean) SO ZOOTAXA LA English DT Article DE Extinction; evolution of island biotas; Madeiran Scops Owl; Otus mauli n. sp.; Macaronesia; Quaternary ID CANARY-ISLANDS; HAWAIIAN-ISLANDS; N-SP; PLEISTOCENE; BIRDS; GENUS; COLONIZATION; ATHENE; MOUSE AB The extinct Madeiran Scops Owl Otus mauli n. sp. is described from fossil bones found in Quaternary sites on Madeira Island (Madeira Archipelago, North Atlantic Ocean). It is the first extinct bird to be described from this archipelago and the first extinct species of Strigiformes known from anywhere in Macaronesia. The forelimb bones of the new taxon are similar in size to those of the Eurasian Scops Owl (Otus scops Linnaeus) but the hindlimb bones are longer, especially the tarsometatarsus, which is much longer and more slender than in O. scops. The estimated body weight and wing loading, together with the proportions of hindlimb bones (femur, tibiotarsus and tarsometatarsus) in relation to total length of leg bones (femur+tibiotarsus+tarsometatarsus), seem to indicate a ground-dwelling life-style. Human arrival and subsequent habitat alterations (introduction of alien taxa, burning, etc.) are the most probable causes of its extinction. The same species or a close relative is documented from dunes on the island of Porto Santo, but the quality of preservation of its bones precludes more certain identification. C1 [Antoni Alcover, Josep] Inst Mediterrani Estudis Avancats, Dept Diodiversitat & Conservacio, Mallorca 07190, Balearic Island, Spain. [Carlos Rando, Juan] Isl Ecol & Evolut Res Grp IPNA CSIC, Tenerife, Spain. [Carlos Rando, Juan] Univ La Laguna, Dept Biol Anim UDI Zool, E-38206 Tenerife, Spain. [Olson, Storrs L.] Smithsonian Inst, Div Birds, Natl Museum Nat Hist, Washington, DC 20013 USA. RP Alcover, JA (reprint author), Inst Mediterrani Estudis Avancats, Dept Diodiversitat & Conservacio, Cr Miquel Marques 21, Mallorca 07190, Balearic Island, Spain. EM canariomys@yahoo.es; orunzehpieper@condaservices.com; jaalcover@imedea.uib-csic.es; olsons@si.edu FU Spanish Ministerio de Ciencia e Innovacion [CGL2010-17889] FX H.P. wants to thank foremost his wife, Ortrud Runze, who eagerly assisted with collecting bird bones and helped with continual encouragement and in countless other ways. Dr. G.E. Maul was unstintingly helpful in all things to be organized in Madeira, especially by providing skeletons of recent birds from the island as comparative material and was ever a competent partner in scientific conversations. Klaus Groh of Hackenheim and Dr. Frank Zino of Funchal should be thanked for fossil collecting, especially in less-often-visited localities such as Deserta Grande and Bugio. We thank Dr. P. Oliveira, Dr. D. Meneses, M. Trias, Dr. J.C. Illera, and Dr. M. Biscoito for help during our last visits to Madeira. This paper is included in Research Project CGL2010-17889 of the Spanish Ministerio de Ciencia e Innovacion. We thank also Dr. Joanne Cooper, Dr. Cecile Mourer-Chauvire and Dr. Trevor Worthy for useful comments. NR 48 TC 4 Z9 4 U1 2 U2 3 PU MAGNOLIA PRESS PI AUCKLAND PA PO BOX 41383, AUCKLAND, ST LUKES 1030, NEW ZEALAND SN 1175-5326 EI 1175-5334 J9 ZOOTAXA JI Zootaxa PD FEB 3 PY 2012 IS 3182 BP 29 EP 42 PG 14 WC Zoology SC Zoology GA 891VO UT WOS:000300245000003 ER PT J AU Breedy, O Guzman, HM AF Breedy, Odalisca Guzman, Hector M. TI A new species of Leptogorgia (Cnidaria: Anthozoa: Octocorallia) from Golfo Dulce, Pacific, Costa Rica SO ZOOTAXA LA English DT Letter ID GORGONIIDAE C1 [Breedy, Odalisca] Univ Costa Rica, Ctr Invest Ciencias Mar & Limnol, San Jose, Costa Rica. [Breedy, Odalisca] Univ Costa Rica, Ctr Invest Estruct Microscop, San Jose, Costa Rica. [Guzman, Hector M.] Smithsonian Trop Res Inst, Panama City, Panama. RP Breedy, O (reprint author), Univ Costa Rica, Ctr Invest Ciencias Mar & Limnol, San Jose, Costa Rica. EM odalisca.breedy@ucr.ac.cr; guzmah@si.edu NR 7 TC 1 Z9 1 U1 1 U2 1 PU MAGNOLIA PRESS PI AUCKLAND PA PO BOX 41383, AUCKLAND, ST LUKES 1030, NEW ZEALAND SN 1175-5326 EI 1175-5334 J9 ZOOTAXA JI Zootaxa PD FEB 3 PY 2012 IS 3182 BP 65 EP 68 PG 4 WC Zoology SC Zoology GA 891VO UT WOS:000300245000007 ER PT J AU Lock, J Hauber, ME AF Lock, Justin Hauber, Mark E. TI A predation risk-and-avoidance model of nestling responses to parental vocalizations SO EVOLUTIONARY ECOLOGY RESEARCH LA English DT Article DE nestling begging; parental vocalizations; predation; predator avoidance ID ALARM CALLS; BEGGING BEHAVIOR; ADULT FOOD; EVOLUTION; COST; GROWTH; BIRDS; RECOGNITION; THRESHOLDS; HOSTS AB Question: How does the nest type of a bird species-cup versus cavity-affect the evolution of its nestlings' responses to parental vocalizations? Background: Nestling birds show distinct behavioural responses either to parental begging-solicitation calls (switch-on begging, lower-frequency sounds) or to parental alarm calls (switch-off begging, high-frequency sounds), but rarely to both. Previous theory suggested that differences in the vibrational conductance of cup versus cavity nests drive the evolution of divergent nestling responses to the different types of parental vocalizations. Many predators eavesdrop on begging displays of nestling birds, then locate the nest and prey on the brood. The risk of predation on broods in cup nests is consistently greater than on broods in cavity nests. New theory: Whether nestlings respond to parental begging-solicitation calls (switch-on) or to parental alarm calls (switch-off) is dependent on a trade-off influenced by predation risks. Although switch-on calls are more efficient at protecting the nestlings that perceive them, they are less efficient at delivering their signal to younger nestlings with poorer sensory and discriminatory abilities (compared with switch-off calls). Thus, where predation risk is high, 'off' calls are favoured; where predation risk is lower, 'on' calls are favoured. Hypotheses: Cup-nesting species, which have higher rates of predation, use 'off' signals, which their young are able to sense early in life before they can sense 'on' signals. Cavity-nesting species are the opposite in all particulars. In addition, cavity nestlings develop the ability to sense low-frequency 'on' sounds later than cup nestlings develop the ability to sense high-frequency 'off' signals. Method: We examined existing comparative data on predation rates at different nesting locations. Using auditory brainstem response studies, we also examined data on the development (ontogeny) of acoustic sensitivity in altricial avian species. Results: Nestlings of cup-nesting species suffer relatively higher predation rates than nestlings of cavity-nesting species. At first, nestlings can hear only a narrow range of sound frequencies. Nestlings gradually develop sensitivity to the full spectrum of vocalizations only after several weeks. The sparse data available on avian auditory ontogeny indicate that cup-nesting species develop early sensitivity to high-frequency sounds, and cavity nesters do so to lower-frequency sounds. Conclusion: The higher predation rates of cup nesters compared with cavity nesters, coupled with the post-hatching delay of all nestlings in achieving full sensitivity to the different types and frequency ranges of parental calls, provide a reasonable explanation for the evolutionary advantage of alarm calls to cup nesters and begging-solicitation calls to cavity nesters. C1 [Lock, Justin] Smithsonian Inst, Ctr Conservat & Evolutionary Genet, Washington, DC 20013 USA. [Lock, Justin; Hauber, Mark E.] Univ Auckland, Sch Biol Sci, Auckland 1, New Zealand. [Hauber, Mark E.] CUNY, Hunter Coll & Grad Ctr, Dept Psychol, New York, NY 10021 USA. RP Lock, J (reprint author), Smithsonian Inst, Ctr Conservat & Evolutionary Genet, Natl Zool Pk, Washington, DC 20013 USA. EM lock.justin.c@gmail.com FU Human Frontier Science Program; Center for Conservation and Evolutionary Genetics, Smithsonian Institution FX We thank the Human Frontier Science Program and the Center for Conservation and Evolutionary Genetics, Smithsonian Institution for funding. We thank Tomas Grim, Becky Kilner, Rob Magrath, and Bill Strausberger for discussion. We thank Teak and Dale Toweill, Michael Rosenzweig, and two anonymous reviewers for valuable comments. NR 36 TC 3 Z9 3 U1 0 U2 14 PU EVOLUTIONARY ECOLOGY LTD PI TUCSON PA UNIV ARIZONA, 321 BIOSCIENCES WEST, TUCSON, AZ 85721 USA SN 1522-0613 EI 1937-3791 J9 EVOL ECOL RES JI Evol. Ecol. Res. PD FEB PY 2012 VL 14 IS 2 BP 235 EP 245 PG 11 WC Ecology; Evolutionary Biology; Genetics & Heredity SC Environmental Sciences & Ecology; Evolutionary Biology; Genetics & Heredity GA 020BZ UT WOS:000309784900007 ER PT J AU Romaschenko, K Peterson, PM Soreng, RJ Garcia-Jacas, N Futorna, O Susanna, A AF Romaschenko, Konstantin Peterson, Paul M. Soreng, Robert J. Garcia-Jacas, Nuria Futorna, Oksana Susanna, Alfonso TI Systematics and evolution of the needle grasses (Poaceae: Pooideae: Stipeae) based on analysis of multiple chloroplast loci, ITS, and lemma micromorphology SO TAXON LA English DT Article DE biogeography; evolution; grasses; lemma micromorphology; molecular systematics; phylogeny; plastid DNA sequences; Poaceae; Stipeae ID MULTIGENE PHYLOGENETIC TREES; FAMILY POACEAE; NONCODING REGIONS; SEQUENCE DATA; DNA BARCODES; PIPTOCHAETIUM POACEAE; NOMENCLATURAL CHANGES; MOLECULAR PHYLOGENY; SMALL INVERSIONS; MATK SEQUENCES AB We conducted a molecular phylogenetic study of the tribe Stipeae using nine plastid DNA sequences (trnK-matK, matK, trnH-psbA, trnL-F, rps3, ndhF, rpl32-trnL, rpsI6-trnK, rps16 intron), the nuclear ITS DNA regions, and micromorphological characters from the lemma surface. Our large original dataset includes 156 accessions representing 139 species of Stipeae representing all genera currently placed in the tribe. The maximum likelihood and Bayesian analyses of DNA sequences provide strong support for the monophyly of Stipeae; including, in phylogenetic order, Macrochloa as remote sister lineage to all other Stipeae, then a primary stepwise divergence of three deep lineages with a saw-like (SL) lemma epidermal pattern (a plesiomorphic state). The next split is between a lineage (SL I) which bifurcates into separate Eurasian and American clades, and a lineage of three parts; a small Patis (SL2) clade, as sister to Piptathertun s.str. (SL3), and the achnatheroid clade (AC). The AC exhibits a maize-like lemma epidermal pattern throughout. AC consists of a core clade of Austral-Eurasian distribution and a "major American clade" of North and South American distribution. The base chromosome number for Stipeae is somewhat ambiguous but based on our survey it seems most likely to be x = 1 or 12. Our phylogenetic hypothesis supports the recognition of the following genera and groups (listed by region): Eurasia-Achnatherum,"Miliacea group", "Neotrinia" (monotypic), Orthoraphium (monotypic), Patis (also 1 from North America), Piptatherum s.str., Psammochloa (monotypic), Ptilagrostis, Stipa, "Timouria group", and Thikeraia; Mediterranean-Ampelodesmos (monotypic), Celtica (monotypic), Macrochloa (monotypic), and "Stipella-Inaequiglumes group"; Australasia-Anemanthele (monotypic), and Austrostipa; North America (NA)-"Eriocoma group", Hesperostipa, Oryzopsis (monotypic), Piptatheropsis, "Pseudoeriocoma group", and "Stillmania" (monotypic); South America-Aciachne, Amelichloa (also NA), Anatherostipa (s.str.), Jarava (polyphyletic), Lorenzochloa, Nassella (also NA), Ortachne, Pappostipa (also NA), and Piptochaetium (also NA). Monophyly of Phaenospermateae including Duthieinae is demonstrated, and its inclusion within or treatment as sister to Stipeae is rejected. C1 [Romaschenko, Konstantin; Peterson, Paul M.; Soreng, Robert J.] Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, Washington, DC 20013 USA. [Romaschenko, Konstantin; Garcia-Jacas, Nuria; Susanna, Alfonso] Bot Inst Barcelona CSIC ICUB, Lab Mol Systemat, Barcelona 08038, Spain. [Futorna, Oksana] Natl Acad Sci Ukraine, MG Kholodny Inst Bot, UA-01601 Kiev, Ukraine. RP Peterson, PM (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, Washington, DC 20013 USA. EM peterson@si.edu RI Susanna, Alfonso/C-1683-2013; Romaschenko, Konstantin/K-3096-2014 OI Susanna, Alfonso/0000-0003-4717-9063; Romaschenko, Konstantin/0000-0002-7248-4193 FU Smithsonian Institution's Restricted Endowment Fund; Scholarly Studies Program, Research Opportunities; Atherton Seidell Foundation; Biodiversity Surveys and Inventories Program; National Museum of Natural History-Small Grants; Laboratory of Analytical Biology (LAB); National Geographic Society Committee for Research and Exploration [808706] FX We thank the following organizations and people: the Smithsonian Institution's Restricted Endowment Fund, the Scholarly Studies Program, Research Opportunities, Atherton Seidell Foundation, Biodiversity Surveys and Inventories Program, National Museum of Natural History-Small Grants, and Laboratory of Analytical Biology (LAB) all for financial support; Lee Weigt, Gabriel Johnson, Jeffrey Hunt, David Erickson, Kenneth Wurdack, and Andrea Ormon for support and consultation while working at LAB; the National Geographic Society Committee for Research and Exploration (grant number 808706) for field and laboratory support; the Fulbright Scholar Program to KR for a research visit to the Smithsonian Institution; the Komarov Botanical Institute, Russian Academy of Sciences for the opportunity to work with herbarium collections, and Nikolai Czvelev and Dmitry Geltman for consultation and permitting us to sample Stipeae specimens; Asuncion Cano Echevarria, Oscar Tovar Serpa dagger, Dorita Susanibar Cruz, Maria Isabel La Torre Acuy, Jenny Vanessa Rojas Fox, Isidoro Sanchez Vega, Socorro Gonzalez Elizondo, Nancy Refulio-Rodriguez, Diego Leonel Salariato, Adela Maria Panizza, Fernando O. Zuloaga, and Stephan Beck for help with our field expeditions to Peru, Bolivia, and Argentina; Sun Hang for help doing fieldwork in China; Sabine Miehe for providing samples from China, Hidehisa Koba for providing samples from Japan, Samuel Pyke for providing samples from North Africa, and Jeffery M. Saarela for providing samples from North America; Michael Pine, Ana Maria Cialdella, Osvaldo Morrone dagger, and three anonymous reviewers for suggesting improvements to the manuscript. NR 156 TC 21 Z9 24 U1 2 U2 21 PU INT ASSOC PLANT TAXONOMY-IAPT PI BRATISLAVA PA C/O INST BOTANY, SLOVAK ACAD SCIENCES DUBRAVSKA CESTA 9, SK-845 23 BRATISLAVA, SLOVAKIA SN 0040-0262 J9 TAXON JI Taxon PD FEB PY 2012 VL 61 IS 1 BP 18 EP 44 PG 27 WC Plant Sciences; Evolutionary Biology SC Plant Sciences; Evolutionary Biology GA 959ZO UT WOS:000305357100002 ER PT J AU Bonifacino, JM Funk, VA AF Bonifacino, Jose M. Funk, Vicki A. TI Phylogenetics of the Chiliotrichum group (Compositae: Astereae): The story of the fascinating radiation in the paleate Astereae genera from southern South America SO TAXON LA English DT Article DE Astereae; Chiliotrichum group; Compositae; molecular systematics; South America ID EXTERNAL TRANSCRIBED SPACER; CHAIN MONTE-CARLO; NONCODING REGIONS; CHLOROPLAST DNA; MAXIMUM-LIKELIHOOD; ETS SEQUENCES; SUBSTITUTION; INFERENCE; TREES; SITES AB The Chiliotrichum group (Compositae: Astereae) is an informal taxonomic group consisting of shrubby daisies that grow mainly in the Andean and Patagonian regions of South America; it is composed of 31 species in 11 genera: Aylacophora, Cabreraea, Chiliotrichiopsis, Chiliophyllum, Chiliotrichum, Haroldia, Katinasia, Lepidophyllum, Llerasia, Nardophyllum, and Ocyroe. We analyzed phylogenetic relationships in the Chiliotrichum group using five DNA regions from two plant genomes: the plastid trnL-trnF and rpl32-trnL((UAG)) spacers, the rp116 intron, and the nuclear ribosomal internal and external transcribed spacers, ITS and ETS respectively. The dataset includes 21 ingroup species representing all the genera, and 10 outgroup species belonging to six genera. Maximum parsimony, maximum likelihood, and Bayesian inference analyses performed on the chloroplast and nuclear data support the monophyly of the group. The four major clades recovered on the basis of the combined nuclear evidence (ITS+ETS) are: (1)Llerasia clade, (2) Nardophyllum clade, (3) Chiliotrichum clade, and (4) a clade formed by Nardophyllum+Llerasia clades. As regards the status of the four non-monospecific genera, Chiliotrichum (2 spp.) and Llerasia (14 spp.) were recovered as monophyletic, whereas the other two, Nardophyllum (5 spp.) and Chiliotrichiopsis (3 spp.), were not recovered as monophyletic. These two are nonetheless recognized as distinct genera because of robust morphological support despite the lack of resolution in the phylogeny based solely on sequence data. The rest of the genera composing the group are monospecific, and they are scattered among the major clades in the group. The only genus with no clear position is Haroldia. An analysis of the morphological data shows that the presence of paleae, believed to function as a defensive structure for the protection of the achenes, is well correlated with other derived head and floret traits such as the number of florets per head and the type of pappus. C1 [Bonifacino, Jose M.] Univ Republica, Fac Agron, Lab Bot, Montevideo, Uruguay. [Funk, Vicki A.] Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, Washington, DC 20560 USA. RP Bonifacino, JM (reprint author), Univ Republica, Fac Agron, Lab Bot, Casilla Correos 1238, Montevideo, Uruguay. EM bonifacinoj@fagro.edu.uy FU Facultad de Agronomia UdelaR (Montevideo, Uruguay); Fundacion Myndel Pedersen; IAPT; Smithsonian Institution; National Geographic Society [7646-04] FX We are grateful to the curators of the following herbaria who provided herbarium material for loan, leaf material for DNA extraction or facilitated JMB's visits to their institutions: BA A, BAB, BAF, BM, BR I, CONC, CORD, E, F, G, K, LIL, LP, MO, MVFA, NY, P, SI, SGO, and US. We thank the Facultad de Agronomia UdelaR (Montevideo, Uruguay), Fundacion Myndel Pedersen, IAPT, Smithsonian Institution, and the National Geographic Society (grant no. 7646-04) for their financial support towards the completion of this work. We also acknowledge the Smithsonian Institution's support through a postdoctoral fellowship granted to JMB. NR 39 TC 3 Z9 4 U1 1 U2 3 PU INT ASSOC PLANT TAXONOMY-IAPT PI BRATISLAVA PA C/O INST BOTANY, SLOVAK ACAD SCIENCES DUBRAVSKA CESTA 9, SK-845 23 BRATISLAVA, SLOVAKIA SN 0040-0262 J9 TAXON JI Taxon PD FEB PY 2012 VL 61 IS 1 BP 180 EP 196 PG 17 WC Plant Sciences; Evolutionary Biology SC Plant Sciences; Evolutionary Biology GA 959ZO UT WOS:000305357100013 ER PT J AU Johnson, NA Smith, JJ Pobiner, B Schrein, C AF Johnson, Norman A. Smith, James J. Pobiner, Briana Schrein, Caitlin TI Why Are Chimps Still Chimps? SO AMERICAN BIOLOGY TEACHER LA English DT Article DE Anagenesis; bonobo; brain; chimpanzee; cladogenesis; evolution; human evolution ID POSITIVE SELECTION; HUMAN-EVOLUTION; CHIMPANZEE; BRAIN; HYPOTHESIS; HOMINOIDS; HUMANS; GENES AB Teachers may be posed with such questions as, "If we evolved from chimps, why are there still chimps?" We provide teachers with answers to this and related questions in the context of the latest genetic, fossil, and behavioral evidence. We also provide references they can use to further students' understanding of human evolution and evolution in general. In the process, we highlight recent discoveries in paleontology, molecular evolution, and comparative genomics. Modern chimps and humans shared a now extinct common ancestor that was neither a chimp nor a human - in other words, humans did not evolve from chimps - and, though chimps are humans' closest living relatives, we are characterized by distinct evolutionary histories. C1 [Johnson, Norman A.] Univ Massachusetts, Amherst, MA 01003 USA. [Smith, James J.] Michigan State Univ, Lyman Briggs Coll, E Lansing, MI 48825 USA. [Pobiner, Briana] Natl Museum Natl Hist, Human Origins Program, Smithsonian Inst, Washington, DC 20013 USA. [Schrein, Caitlin] Arizona State Univ, Sch Human Evolut & Social Change, Tempe, AZ 85281 USA. RP Johnson, NA (reprint author), Univ Massachusetts, Agr Engn Bldg, Amherst, MA 01003 USA. EM njohnson@ent.umass.edu; jimsmith@msu.edu; pobinerb@si.edu; caitlin.schrein@asu.edu NR 35 TC 2 Z9 2 U1 5 U2 23 PU NATL ASSOC BIOLOGY TEACHERS INC PI RESTON PA 12030 SUNRISE VALLEY DR, #110, RESTON, VA 20191 USA SN 0002-7685 J9 AM BIOL TEACH JI Am. Biol. Teach. PD FEB PY 2012 VL 74 IS 2 BP 74 EP 80 DI 10.1525/abt.2012.74.2.3 PG 7 WC Biology; Education, Scientific Disciplines SC Life Sciences & Biomedicine - Other Topics; Education & Educational Research GA 958AZ UT WOS:000305209600003 ER PT J AU Gowda, V Erickson, DL Kress, WJ AF Gowda, Vinita Erickson, David L. Kress, W. John TI DEVELOPMENT AND CHARACTERIZATION OF MICROSATELLITE LOCI FOR TWO CARIBBEAN HELICONIA (HELICONIACEAE: H. BIHAI AND H. CARIBAEA) SO AMERICAN JOURNAL OF BOTANY LA English DT Article DE Caribbean; coevolution; Heliconia bihai; Heliconia caribaea; Heliconiaceae; microsatellites AB Premise of the study: Microsatellite loci were developed to characterize genetic variation and population subdivision in Heliconia bihai and H. caribaea from the Caribbean Islands. Methods and Results: A total of 13 new microsatellite markers were developed and characterized in the two Caribbean heliconias. Di-, tri-, and tetranucleotide repeats were identified with one to 17 alleles per locus, and the observed heterozygosity ranged from 0.13 to 0.87. Additionally, cross-species amplification was successful in eight out of 13 loci. Conclusions: The microsatellite loci developed have discriminatory potential to be used in genetic characterizations of Caribbean Heliconia. Both H. bihai and H. caribaea are known to have adaptive interactions with their hummingbird pollinators, and the characterized microsatellite markers will be used to study mating system, genetic structure, and phylogeographic patterns in Caribbean Heliconia. C1 [Gowda, Vinita] George Washington Univ, Dept Biol Sci, Washington, DC 20052 USA. [Gowda, Vinita; Erickson, David L.; Kress, W. John] Smithsonian Inst, Dept Bot, Washington, DC 20013 USA. RP Gowda, V (reprint author), George Washington Univ, Dept Biol Sci, 2023 G St NW, Washington, DC 20052 USA. EM vinitagowda@gmail.com FU National Science Foundation [DEB-0614218]; George Washington University FX This work was supported by a National Science Foundation grant (DEB-0614218) to E. J. Temeles and W. J. Kress, and a Weintraub graduate fellowship (George Washington University) to V. Gowda. We thank the Ministry of Agriculture and the Environment, Forestry, Wildlife, and Parks Division, Commonwealth of Dominica, for research and collection permits. We also thank L. Weight, J. Hunt, I. Lopez, and S. Sonsthagen for assistance and technical advice. NR 9 TC 1 Z9 1 U1 2 U2 6 PU BOTANICAL SOC AMER INC PI ST LOUIS PA PO BOX 299, ST LOUIS, MO 63166-0299 USA SN 0002-9122 J9 AM J BOT JI Am. J. Bot. PD FEB PY 2012 VL 99 IS 2 BP E81 EP E83 DI 10.3732/ajb.1100386 PG 3 WC Plant Sciences SC Plant Sciences GA 952SM UT WOS:000304812600013 PM 22282112 ER PT J AU Liu, HP Hershler, R AF Liu, Hsiu-Ping Hershler, Robert TI Phylogeography of an endangered Western North American springsnail SO CONSERVATION GENETICS LA English DT Article DE Phylogeography; Gastropoda; Endangered species; Springs; Conservation ID MITOCHONDRIAL-DNA SEQUENCES; PYRGULOPSIS-BRUNEAUENSIS; NYMPHOPHILINE GASTROPODS; POPULATION-STRUCTURE; UNITED-STATES; GREAT-BASIN; GENE FLOW; HYDROBIIDAE; SNAIL; DIVERGENCE AB We provide the first genetic analysis of the Bruneau Hot Springsnail (Pyrgulopsis bruneauensis), a federally listed (endangered) hydrobiid gastropod that is distributed in spring-fed habitats along a short reach of the Bruneau River in southwestern Idaho and threatened with extinction by groundwater withdrawal. Partial sequences of mitochondrial cytochrome c oxidase subunit I (COI) and NADH dehydrogenase subunit I (NDI) were obtained from 51 specimens from six sites spanning the narrow geographic range of P. bruneauensis. A Bayesian analysis of the combined dataset resolved this species as a well supported clade which differed from other regional congeners by 4.66-10.62% sequence divergence (COI). The 11 observed COI haplotypes in P. bruneauensis formed two divergent (1.42 +/- 0.7%) subgroups that co-occurred at five of the six collecting sites. COI haplotype diversity was substantial (ranging up to 0.9111) in all but one sample, while nucleotide diversity was low (<0.01). AMOVA detected small but significant variation among sites, although only one sample was significantly differentiated by pairwise comparisons. Haplotype composition varied widely among the collecting localities and no obvious geographic pattern was detected. These findings suggest that translocation of snails, which was considered as a possible measure in the P. bruneauensis recovery plan, should be preceded by assays to ensure selection of appropriately genetically diverse source populations. C1 [Hershler, Robert] Smithsonian Inst, Dept Invertebrate Zool, Washington, DC 20013 USA. [Liu, Hsiu-Ping] Metropolitan State Coll Denver, Dept Biol, Denver, CO 80217 USA. RP Hershler, R (reprint author), Smithsonian Inst, Dept Invertebrate Zool, NHB W-305,MRC 163,POB 37012, Washington, DC 20013 USA. EM hershlerr@si.edu FU Idaho Fish and Wildlife Office FX We thank David Hopper and his IFWO colleagues for collecting the specimens of P. bruneauensis that were analyzed in this study. This study was supported, in part, by an award from the Idaho Fish and Wildlife Office. NR 35 TC 3 Z9 3 U1 2 U2 8 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 1566-0621 EI 1572-9737 J9 CONSERV GENET JI Conserv. Genet. PD FEB PY 2012 VL 13 IS 1 BP 299 EP 305 DI 10.1007/s10592-011-0288-8 PG 7 WC Biodiversity Conservation; Genetics & Heredity SC Biodiversity & Conservation; Genetics & Heredity GA 934VW UT WOS:000303475800025 ER PT J AU Marble, S AF Marble, Sanders TI Brigadier General James Stevens Simmons (1890-1954), Medical Corps, United States Army: a career in preventive medicine SO JOURNAL OF MEDICAL BIOGRAPHY LA English DT Article AB James Simmons began his career in the US Army as a laboratory officer and his assignments progressed into tropical medicine research. His interests and work evolved into preventive medicine (PM, as the Army termed public health), and he took both a PhD and a Doctorate in Public Health. As the Army's leading PM officer he was appointed head of PM in 1940 and guided the Army's PM effort through World War II. His responsibility ran from gas masks through healthy nutrition and occupational health to an enormous variety of diseases; by the war's end, the breadth and importance of PM was reflected in the Preventive Medicine Division, having fully one-sixth of all military personnel at the Surgeon General's Office. Simmons used his strong professional credentials to tap into civilian medicine for expertise the Army lacked and he established organizations that survive to this day. After retirement, he sought to expand the field of public health and raise another generation of public health physicians. C1 [Marble, Sanders] USA, Off Med Hist, Ft Sam Houston, TX 78234 USA. [Marble, Sanders] Walter Reed Army Med Ctr, Smithsonian Inst, Washington, DC USA. RP Marble, S (reprint author), USA, Off Med Hist, 2050 Worth Rd, Ft Sam Houston, TX 78234 USA. EM sanders.marble@us.army.mil NR 24 TC 0 Z9 0 U1 0 U2 0 PU ROYAL SOC MEDICINE PRESS LTD PI LONDON PA 1 WIMPOLE STREET, LONDON W1G 0AE, ENGLAND SN 0967-7720 J9 J MED BIOGR JI J. Med. Biogr. PD FEB PY 2012 VL 20 IS 1 BP 3 EP 10 DI 10.1258/jmb.2010.010054 PG 8 WC History & Philosophy Of Science SC History & Philosophy of Science GA 936ZD UT WOS:000303627900002 PM 22499600 ER PT J AU Breger, M Hareter, M Endl, M Kuschnig, R Weiss, WW Matthews, JM Guenther, DB Moffat, AFJ Rowe, JF Rucinski, SM Sasselov, D AF Breger, M. Hareter, M. Endl, M. Kuschnig, R. Weiss, W. W. Matthews, J. M. Guenther, D. B. Moffat, A. F. J. Rowe, J. F. Rucinski, S. M. Sasselov, D. TI Delta Scuti stars in the Praesepe cluster observed by the MOST satellite SO ASTRONOMISCHE NACHRICHTEN LA English DT Article DE delta Scuti stars; open clusters and associations: individual (Praesepe); stars: individual (BS Cnc, BT Cnc, EP Cnc, HD 73872); stars: oscillations; techniques: photometric ID STACC 1998 CAMPAIGN; BT CANCRI; F-STARS; PHOTOMETRY; SPACE; VARIABILITY; PULSATION AB The Praesepe cluster contains a number of delta Sct and gamma Dor pulsators. Asteroseismology of cluster stars is simplified by the common distance, age and stellar abundances. Since asteroseismology requires a large number of known frequencies, the small pulsation amplitudes of these stars require space satellite campaigns. The present study utilizes photometric MOST satellite measurements in order to determine the pulsation frequencies of two evolved (EP Cnc, BT Cnc) and two main-sequence (BS Cnc, HD 73872) delta Sct stars in the Praesepe cluster. The frequency analysis of the 2008 and 2009 data detected up to 34 frequencies per star with most amplitudes in the submillimag range. In BS Cnc, two modes showed strong amplitude variability between 2008 and 2009. The frequencies ranged from 0.76 to 41.7 cd(-1). After considering the different evolutionary states and mean stellar densities of these four stars, the differences and large ranges in frequency remain. (C) 2012 WILEY-VCH Verlag GmbH & Co. KGaA, Weinheim C1 [Breger, M.; Hareter, M.; Endl, M.; Kuschnig, R.; Weiss, W. W.] Univ Vienna, Inst Astron, A-1180 Vienna, Austria. [Breger, M.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA. [Matthews, J. M.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada. [Guenther, D. B.] St Marys Univ, Dept Phys & Astron, Halifax, NS B3H 3C3, Canada. [Moffat, A. F. J.] Univ Montreal, Dept Phys, Montreal, PQ H3C 3J7, Canada. [Rowe, J. F.] NASA Ames Res Pk, Moffett Field, CA 94035 USA. [Rucinski, S. M.] Univ Toronto, Dept Astron & Astrophys, Toronto, ON M5S 3H4, Canada. [Sasselov, D.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Breger, M (reprint author), Univ Vienna, Inst Astron, Turkenschanzstr 17, A-1180 Vienna, Austria. EM michel.breger@univie.ac.at FU Austrian Fonds zur Forderung der wissenschaftlichen Forschung [P 21830-N16, P 22691-N16] FX This investigation has been supported by the Austrian Fonds zur Forderung der wissenschaftlichen Forschung through projects P 21830-N16 and P 22691-N16. NR 31 TC 6 Z9 6 U1 0 U2 2 PU WILEY-V C H VERLAG GMBH PI WEINHEIM PA PO BOX 10 11 61, D-69451 WEINHEIM, GERMANY SN 0004-6337 J9 ASTRON NACHR JI Astro. Nachr. PD FEB PY 2012 VL 333 IS 2 BP 131 EP 137 DI 10.1002/asna.201111640 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 932TH UT WOS:000303312900005 ER PT J AU Cardone, VF Camera, S Diaferio, A AF Cardone, Vincenzo F. Camera, Stefano Diaferio, Antonaldo TI An updated analysis of two classes of f (R) theories of gravity SO JOURNAL OF COSMOLOGY AND ASTROPARTICLE PHYSICS LA English DT Article DE modified gravity; dark energy theory; supernova type Ia - standard candles; baryon acoustic oscillations ID EQUATION-OF-STATE; OBSERVATIONS COSMOLOGICAL INTERPRETATION; BARYON ACOUSTIC-OSCILLATIONS; MODIFIED NEWTONIAN DYNAMICS; PROBE WMAP OBSERVATIONS; HUBBLE-SPACE-TELESCOPE; GLOBULAR-CLUSTER AGES; GAMMA-RAY BURSTS; DARK-MATTER; OLD GALAXIES AB The observed accelerated cosmic expansion can be a signature of fourth-order gravity theories, where the acceleration of the Universe is a consequence!) of departures from Einstein General Relativity, rather than the sign of the existence of a fluid with negative pressure. In the fourth-order gravity theories, the gravity Lagrangian is described by an analytic function f(R) of the scalar curvature R subject to the demanding conditions that no detectable deviations from standard GR is observed on the Solar System scale. Here we consider two classes of f (R) theories able to pass Solar System tests and investigate their viability on cosmological scales. To this end, we fit the theories to a large dataset including the combined Hubble diagram of Type Ia Supernovae and Gamma Ray Bursts, the Hubble parameter H(z) data from passively evolving red galaxies, Baryon Acoustic Oscillations extracted from the seventh data release of the Sloan lAgital Sky Survey (SDSS) and the distance priors from the Wilkinson Microwave Anisotropy Probe seven years (WMAP7) data. We find that both classes of f(B) fit very well this large dataset with the present-day values of the matter density. Hubble constant and deceleration parameter in agreement with previous estimates; however, the strong degeneracy among the f(R) parameters prevents us from strongly constraining their values. We also derive the growth factor g = d In delta/d In a, with delta = delta pm/pm the matter density perturbation, and show that it can still be well approximated by g(z) alpha Omega(M)(z)(gamma). We finally constrain gamma (on some representative scales) and investigate its redshift dependence to see whether future data can discriminate between these classes of f (R) theories and standard dark energy models. C1 [Cardone, Vincenzo F.] INAF, Osservatorio Astronomico Roma, I-00040 Rome, Italy. [Camera, Stefano; Diaferio, Antonaldo] Univ Turin, Dipartimento Fis Gen A Avogadro, I-10125 Turin, Italy. [Camera, Stefano] Univ Turin, Dipartimento Fis Teor, I-10125 Turin, Italy. [Camera, Stefano; Diaferio, Antonaldo] Ist Nazl Fis Nucl, Sez Torino, I-10125 Turin, Italy. [Camera, Stefano] Univ Tecn Lisboa, Inst Super Tecn, CENTRA, P-1049001 Lisbon, Portugal. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Cardone, VF (reprint author), INAF, Osservatorio Astronomico Roma, V Frascati 33, I-00040 Rome, Italy. EM winnyenodrac@gmail.com; camera@ph.unito.it; diaferio@ph.unito.it RI Camera, Stefano/N-2456-2013 OI Camera, Stefano/0000-0003-3399-3574 FU Agenzia Spaziale Italiana (ASI); INFN [PD51]; PRIN-MIUR [2008NR3EBK_003] FX VFC warmly thanks S. Capozziello and M.G Dainotti for working together on GRBs. VFC is supported by Agenzia Spaziale Italiana (ASI). SC and AD gratefully acknowledge partial support from INFN grant PD51 and the PRIN-MIUR-2008 grant 2008NR3EBK_003 "Matter-antiniatter asymmetry, dark matter and dark energy in the LHC era". This research has made use of NASA's Astrophysics Data System. NR 97 TC 6 Z9 6 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 1475-7516 J9 J COSMOL ASTROPART P JI J. Cosmol. Astropart. Phys. PD FEB PY 2012 IS 2 AR 030 DI 10.1088/1475-7516/2012/02/030 PG 28 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA 904EE UT WOS:000301176000031 ER PT J AU Aronson, RB Precht, WF Macintyre, IG Toth, LT AF Aronson, Richard B. Precht, William F. Macintyre, Ian G. Toth, Lauren T. TI Catastrophe and the life span of coral reefs SO ECOLOGY LA English DT Article DE Belize; coral bleaching; coral disease; coral reef; earthquake; paleoecology; resilience; sponges; submarine avalanche; T-50 ID SELF-ORGANIZED CRITICALITY; COMMUNITY STRUCTURE; CLIMATE-CHANGE; PHASE-SHIFTS; BELIZE; ECOSYSTEMS; RESILIENCE; DISTURBANCE; RECOVERY; ISLANDS AB A strong earthquake in the western Caribbean in 2009 had a catastrophic impact on uncemented, unconsolidated coral reefs in the central sector of the shelf lagoon of the Belizean barrier reef. In a set of 21 reef sites that had been observed prior to the earthquake, the benthic assemblages of 10 were eradicated, and one was partially damaged, by avalanching of their slopes. Ecological dynamics that had played out over the previous 23 years, including the mass mortalities of two sequentially dominant coral species and a large increase in the cover of an encrusting sponge, were instantaneously rendered moot in the areas of catastrophic reef-slope failure. Because these prior dynamics also determined the benthic composition and resilience of adjacent sections of reef that remained intact, the history of disturbance prior to the earthquake will strongly influence decadal-scale recovery in the failed areas. Geological analysis of the reef framework yielded a minimum return time of 2000-4000 years for this type of high-amplitude event. Anthropogenic degradation of ecosystems must be viewed against the backdrop of long-period, natural catastrophes, such as the impact of strong earthquakes on uncemented, lagoonal reefs. C1 [Aronson, Richard B.; Toth, Lauren T.] Florida Inst Technol, Dept Biol Sci, Melbourne, FL 32901 USA. [Precht, William F.] NOAA, Florida Keys Natl Marine Sanctuary, Key Largo, FL 33037 USA. [Macintyre, Ian G.] Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20560 USA. RP Aronson, RB (reprint author), Florida Inst Technol, Dept Biol Sci, 150 W Univ Blvd, Melbourne, FL 32901 USA. EM raronson@fit.edu FU Smithsonian Marine Science Network FX We thank M. B. Bush, S. R. Dudgeon, L. Kaufman, R. M. Moody, B. R. Silliman, R. A. Tankersley, R. van Woesik, and J. L. Wulff for advice and discussion. Comments from two anonymous reviewers improved the manuscript. W. B. Goodwin and A. G. Macintyre assisted with the fieldwork. T. Rath and B. V. Shank kindly provided images and initial information on the impacts of the earthquake in Belize. Fieldwork was supported by a grant from the Smithsonian Marine Science Network and carried out under a permit from the Belize Department of Fisheries. This paper is Contribution No. 909 from the Smithsonian's Caribbean Coral Reef Ecosystems (CCRE) Program and Contribution No. 62 from the Institute for Research on Global Climate Change at the Florida Institute of Technology. The content of this paper does not reflect any position of the National Oceanic and Atmospheric Administration (NOAA) or the U.S. Government, unless otherwise specified. NR 71 TC 6 Z9 6 U1 3 U2 49 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 FEB PY 2012 VL 93 IS 2 BP 303 EP 313 PG 11 WC Ecology SC Environmental Sciences & Ecology GA 925WZ UT WOS:000302794100011 PM 22624312 ER PT J AU Wing, SL Stromberg, CAE Hickey, LJ Tiver, F Willis, B Burnham, RJ Behrensmeyer, AK AF Wing, Scott L. Stromberg, Caroline A. E. Hickey, Leo J. Tiver, Fleur Willis, Brian Burnham, Robyn J. Behrensmeyer, Anna K. TI Floral and environmental gradients on a Late Cretaceous landscape SO ECOLOGICAL MONOGRAPHS LA English DT Article DE angiosperms; Big Cedar Ridge, Wyoming, USA; disturbance; ferns; nutrient stress; paleoecology ID CANONICAL CORRESPONDENCE-ANALYSIS; FERN LYGODIUM-MICROPHYLLUM; EARLY ANGIOSPERM RADIATION; NEOTROPICAL RAIN-FOREST; LEAF VEIN EVOLUTION; SPECIES RICHNESS; PLANT DIVERSITY; DICRANOPTERIS-LINEARIS; SEED SIZE; PALEOLATITUDINAL GRADIENTS AB We describe an in situ fossil flora of Late Cretaceous age (similar to 73 Ma [megaannum or million years]) from Big Cedar Ridge in central Wyoming, USA, which we sampled using a modified line-intercept method to quantify the relative abundances of 122 taxa at 100 sites across 4 km of exposed sedimentary deposits. We also measured three physical variables at each site: paleotopographic level, grain size, and total organic content. Paleoenvironmental conditions and paleolloral composition at Big Cedar Ridge covary strongly and are highly heterogeneous on small spatial scales. The reconstructed vegetation has some similarities with extant topogenous fens, but also important differences. Non-monocot angiosperms were abundant only on wet, mineral substrates that had been disturbed shortly before preservation, consistent with the weedy life histories that are inferred for their Early Cretaceous ancestors. Many non-monocot angiosperms grew in small, dispersed populations, consistent with the hypothesis that they were biotically pollinated. Overall, non-monocot angiosperm abundance was low compared with many modern wetlands. A single species of coryphoid palm was the dominant on moist, stable, moderately organic-rich sites, a pattern seen in some subtropical to tropical wetlands in the present day. Fern thickets at Big Cedar Ridge occupied highly organic, possibly low-nutrient substrates, and were dominated by Dipteridaceae, Gleicheniaceae, Schizaeaceae, and Matoniaceae. The overall high diversity and abundance of pteridophytes is unusual in the context of modern vegetation, regardless of climate zone, and probably represents a late occurrence of pieridophyte-dominated vegetation that was common earlier in the Mesozoic. Plant distributions at Big Cedar Ridge combine aspects of pre-angiosperm and modern vegetation in a way that suggests both niche conservatism and niche evolution on geological time scales. C1 [Wing, Scott L.; Behrensmeyer, Anna K.] Smithsonian Inst, NHB121, Dept Paleobiol, Washington, DC 20013 USA. [Stromberg, Caroline A. E.] Univ Washington, Dept Biol, Seattle, WA 98195 USA. [Stromberg, Caroline A. E.] Univ Washington, Burke Museum Nat Hist & Culture, Seattle, WA 98195 USA. [Hickey, Leo J.] Yale Univ, Dept Geol & Geophys, New Haven, CT 06520 USA. [Tiver, Fleur] Univ S Australia, Sch Nat & Built Environm, Adelaide, SA 5095, Australia. [Willis, Brian] Chevron Energy Technol Co, Clast R&D, Houston, TX 77002 USA. [Burnham, Robyn J.] Univ Michigan, Museum Paleontol, Ann Arbor, MI 48109 USA. RP Wing, SL (reprint author), Smithsonian Inst, NHB121, Dept Paleobiol, Washington, DC 20013 USA. EM wings@si.edu OI Wing, Scott/0000-0002-2954-8905 FU National Geographic Society; Smithsonian Institution Scholarly Studies; Smithsonian Office of Fellowships; Department of Paleobiology, Smithsonian Institution FX We thank the BCR census crew: Jill McElderry, Ana Ruesink, Colin Shaw, Ashley Allen, Brett Balogh, Michele Capella, Tom Cotter, Alice Dustira, Megan Healy, Damian Hickey, Tom Jorstad, Bill Keyser, Peter Kroehler, Michelle Liven, Skip Lyles, Finnegan Marsh, Mary Parrish, and Craig Van Boskirk. Bill Keyser made the census frames. Nathan hid, Amy Morey, Julie Nicol, and James Super helped with additional collecting in 2007 and 2008, as well as with morphotype description. Jim McCrea made initial measurements of grain size and paleosol carbon content: the University of Colorado Quaternary Lab provided grain size analyses reported here, and Julie Nicol helped with remaining TOC measurements. Stephen Chester mapped locality positions. Amy Morey photographed fossils. Mike Bies, Doug Bleak, and others at the Bureau of Land Management District Office in Worland. Wyoming, provided logistical support on many occasions. This research was supported by grants from the National Geographic Society, Smithsonian Institution Scholarly Studies, Smithsonian Office of Fellowships, and the Roland W. Brown Fund of the Department of Paleobiology, Smithsonian Institution. This is Publication 255 of the Evolution of Terrestrial Ecosystems Program. NR 149 TC 8 Z9 8 U1 5 U2 41 PU ECOLOGICAL SOC AMER PI WASHINGTON PA 1990 M STREET NW, STE 700, WASHINGTON, DC 20036 USA SN 0012-9615 EI 1557-7015 J9 ECOL MONOGR JI Ecol. Monogr. PD FEB PY 2012 VL 82 IS 1 BP 23 EP 47 DI 10.1890/11-0870.1 PG 25 WC Ecology SC Environmental Sciences & Ecology GA 917SH UT WOS:000302198400003 ER PT J AU Launius, RD AF Launius, Roger D. TI Planning the post-Apollo space program: Are there lessons for the present? SO SPACE POLICY LA English DT Article ID INTERNATIONAL-COOPERATION; HUMAN SPACEFLIGHT; POLICY; SHUTTLE; VISION AB The current debate over the future of human spaceflight in the USA has been a fascinating, and troubling, exercise in futility for those inextricably committed to an expansive vision of human exploration and development of space. The retirement of the Space Shuttle, originally set for the end of 2010 but later extended into 2011, the technical and funding problems of the Constellation follow-on program that led to its cancellation in 2009, and the emergence of commercial vendors who might be able to offer human access to Earth orbit have all complicated the current environment. In view of this situation, the question may be legitimately asked: what might we learn from earlier efforts to develop a human spaceflight capability the last time such a transition took place? Using the post-Apollo transition from the ballistic capsule to a winged, reusable vehicle as a case study, this article seeks to illuminate the planning, decision-making, economic, and political issues that have arisen in this policy debate. It suggests that a web of interlocking issues-only one of which was technical-affected the course taken. Instead, politics, economics, social and cultural priorities, values, and institutional considerations all helped to frame the debate and shape the decision. Published by Elsevier Ltd. C1 Smithsonian Inst, Natl Air & Space Museum, Washington, DC 20013 USA. RP Launius, RD (reprint author), Smithsonian Inst, Natl Air & Space Museum, POB 37012,NASM Room 3556,MRC 311, Washington, DC 20013 USA. EM launiusr@si.edu OI Launius, Roger/0000-0003-1633-1253 NR 67 TC 1 Z9 1 U1 3 U2 7 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 0265-9646 J9 SPACE POLICY JI Space Policy PD FEB PY 2012 VL 28 IS 1 BP 38 EP 44 DI 10.1016/j.spacepol.2011.07.005 PG 7 WC International Relations; Social Sciences, Interdisciplinary SC International Relations; Social Sciences - Other Topics GA 912XD UT WOS:000301833800006 ER PT J AU Adams, RMM Jones, TH Jeter, AW Licht, HHD Schultz, TR Nash, DR AF Adams, Rachelle M. M. Jones, Tappey H. Jeter, Andrew W. Licht, Henrik H. De Fine Schultz, Ted R. Nash, David R. TI A comparative study of exocrine gland chemistry in Trachymyrmex and Sericomyrmex fungus-growing ants SO BIOCHEMICAL SYSTEMATICS AND ECOLOGY LA English DT Article DE Attini; Terpenes; Ketones; Farnesenes; alpha,alpha-Acariolide ID LEAF-CUTTING ANT; ATTA-SEXDENS-RUBROPILOSA; HYMENOPTERA-FORMICIDAE; ALARM PHEROMONES; TRAIL PHEROMONE; ACROMYRMEX-OCTOSPINOSUS; MYRMICA-SULCINODIS; METAPLEURAL GLAND; ATTINE ANTS; SECRETIONS AB Ants possess many exocrine glands that produce a variety of compounds important for chemical communication. Fungus-growing ants, a tribe of over 230 species within the subfamily Myrmicinae, are unique among ants because they cultivate fungus gardens inside their nests as food. Here the chemistry of the exocrine glands of the two genera most closely related to the conspicuous leaf-cutting ants are examined. Based on a recent phylogeny of the fungus-growing ants, these genera comprise three clades that together link the more basal species to the most derived, leaf-cutting species. The leaf-cutting ants possess many derived characteristics such as extensive leaf-cutting behavior and massive colony sizes, effectively making them major herbivores in many Neotropical habitats. This is the first comparison of the chemistry of eight Trachymyrmex and one Sericomyrmex species in a phylogenetic context. Most of the compounds found in the Trachymyrmex species examined were terpenes. In one species, the major component was alpha,alpha-acariolide, the first example of this compound, which was only previously reported in mites, from an insect. Additionally, 3-octanol, 3-octanone, and 4-methyl-3-heptanone were detected, well-known mandibular gland compounds from a number of ant genera, together with high levels of undecane, likely from the Dufour's gland, all generally thought to be used as alarm pheromones. Overall the combination of compounds discovered was unique for each species but biosynthetic similarities corroborate, at a very basic level, the phylogenetic relationships. (C) 2011 Elsevier Ltd. All rights reserved. C1 [Adams, Rachelle M. M.; Licht, Henrik H. De Fine; Nash, David R.] Univ Copenhagen, Ctr Social Evolut, Dept Biol, DK-2100 Copenhagen O, Denmark. [Adams, Rachelle M. M.; Schultz, Ted R.] Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol, Washington, DC 20560 USA. [Adams, Rachelle M. M.; Schultz, Ted R.] Smithsonian Inst, Natl Museum Nat Hist, Labs Analyt Biol, Washington, DC 20560 USA. [Jones, Tappey H.; Jeter, Andrew W.] Virginia Mil Inst, Dept Chem, Lexington, VA 24450 USA. RP Adams, RMM (reprint author), Univ Copenhagen, Ctr Social Evolut, Dept Biol, Univ Pk 15, DK-2100 Copenhagen O, Denmark. EM RAdams@bio.ku.dk; JonesTH@vmi.edu; Henrik.de_Fine_Licht@biol.lu.se; SCHULTZT@si.edu; drnash@bio.ku.dk RI Nash, David/H-4433-2012; Nash, David/B-2916-2009; Adams, Rachelle/J-8846-2013; De Fine Licht, Henrik/G-3307-2014 OI Nash, David/0000-0002-0462-6794; Nash, David/0000-0002-0462-6794; Adams, Rachelle/0000-0002-0918-9861; De Fine Licht, Henrik/0000-0003-3326-5729 FU Marie Curie International Incoming Fellowships [237266 - ANCEPS] FX This work was funded by a Marie Curie International Incoming Fellowships (237266 - ANCEPS) awarded to R. M. M. Adams. We would like to thank Hermogenes Fernandez-Marin and Steve Rehner for colony collection and one anonymous reviewer for comments on the manuscript. We also thank the Autoridad Nacional del Ambiente of the Republic of Panama and the Smithsonian Tropical Research Institute for research permits and help with logistics. NR 47 TC 7 Z9 7 U1 1 U2 19 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0305-1978 EI 1873-2925 J9 BIOCHEM SYST ECOL JI Biochem. Syst. Ecol. PD FEB PY 2012 VL 40 BP 91 EP 97 DI 10.1016/j.bse.2011.10.011 PG 7 WC Biochemistry & Molecular Biology; Ecology; Evolutionary Biology SC Biochemistry & Molecular Biology; Environmental Sciences & Ecology; Evolutionary Biology GA 884MR UT WOS:000299712700019 ER PT J AU Thompson, FC AF Thompson, F. Christian TI Fabulous flower flies for famous fly fanatics (Diptera: Syrphidae). A tribute to the dipterists of the Canadian National Collection SO CANADIAN ENTOMOLOGIST LA English DT Article AB Six new flower fly species are described: Blera chillcotti Thompson (Nepal), Sphiximorpha mcalpinei Thompson (Mexico), Psilota shewelli Thompson (Nepal), Rhopalosyrphus teskeyi Thompson (Argentina), Parasyrphus vockerothi Thompson (United States of America and Canada), and Lycopale woodi Thompson (Mexico). Keys are provided to the species of the genera Lycopale Hull and Rhopalosyrphus Giglio-Tos, the Nearctic species of Sphiximorpha Rondani, and the Oriental species of Blera Billberg and Psilota Meigen. C1 Smithsonian Inst, Dept Entomol, Washington, DC 20560 USA. RP Thompson, FC (reprint author), Smithsonian Inst, Dept Entomol, NHB 169, Washington, DC 20560 USA. EM thompsonf@si.edu NR 52 TC 1 Z9 1 U1 0 U2 1 PU CAMBRIDGE UNIV PRESS PI NEW YORK PA 32 AVENUE OF THE AMERICAS, NEW YORK, NY 10013-2473 USA SN 0008-347X EI 1918-3240 J9 CAN ENTOMOL JI Can. Entomol. PD FEB PY 2012 VL 144 IS 1 BP 1 EP 16 DI 10.4039/tce.2012.4 PG 16 WC Entomology SC Entomology GA 909OV UT WOS:000301575000002 ER PT J AU Mathis, WN Zatwarnicki, T AF Mathis, Wayne N. Zatwarnicki, Tadeusz TI Review of the shore-fly genus Oedenopiforma (Diptera: Ephydridae) SO CANADIAN ENTOMOLOGIST LA English DT Review AB The shore-fly genus Oedenopiforma Cogan is reviewed, including new information on Oedenopiforma argentea (distribution), Oedenopiforma javana (comb. nov. and O. orientalis syn. nov.), and Oedenopiforma vockerothi (sp. nov. from United Arab Emirates). Structures of the male terminalia of these three species, a diagnosis of the genus, and a key to the included genera of Dryxini and species of Oedenopiforma are presented. C1 [Mathis, Wayne N.] Smithsonian Inst, Dept Entomol, Washington, DC 20013 USA. [Zatwarnicki, Tadeusz] Univ Opole, Dept Biosystemat, PL-45052 Opole, Poland. RP Mathis, WN (reprint author), Smithsonian Inst, Dept Entomol, POB 37012,MRC 169, Washington, DC 20013 USA. EM mathisw@si.edu OI Zatwarnicki, Tadeusz/0000-0003-2163-0143 NR 21 TC 0 Z9 0 U1 0 U2 3 PU CAMBRIDGE UNIV PRESS PI NEW YORK PA 32 AVENUE OF THE AMERICAS, NEW YORK, NY 10013-2473 USA SN 0008-347X J9 CAN ENTOMOL JI Can. Entomol. PD FEB PY 2012 VL 144 IS 1 BP 81 EP 92 DI 10.4039/tce.2012.9 PG 12 WC Entomology SC Entomology GA 909OV UT WOS:000301575000007 ER PT J AU Norrbom, AL Korytkowski, CA AF Norrbom, Allen L. Korytkowski, Cheslavo A. TI A new species of Anastrepha (Diptera: Tephritidae) from Colombia, Costa Rica, and Panama SO CANADIAN ENTOMOLOGIST LA English DT Article AB Anastrepha woodi sp. nov. is described and illustrated based on specimens from Colombia, Costa Rica, and Panama. Anastrepha loewi Stone, the species most similar to A. woodi, is redescribed, and the two species are compared. C1 [Norrbom, Allen L.] ARS, Systemat Entomol Lab, USDA, Smithsonian Inst, Washington, DC 20013 USA. [Korytkowski, Cheslavo A.] Univ Panama, Programa Maestria Entomol Vice Rectoria Invest &, Panama City, Panama. RP Norrbom, AL (reprint author), ARS, Systemat Entomol Lab, USDA, Smithsonian Inst, POB 37012,MRC 168, Washington, DC 20013 USA. EM allen.norrbom@ars.usda.gov FU USDA; APHIS; CPHST FX We sincerely thank the curators and institutions who kindly loaned or provided specimens for study, particularly Jeff Cumming (CNC) and Manuel Zumbado (INBio). Jerrett McCormick, George Venable, and Lucrecia Rodriguez helped to produce some of the illustrations, and Terrence Walters (USDA, APHIS, CPHST) secured funding for some of the illustration work. We also thank Roberto Zucchi, Michael Gates, Norman Woodley, and Brad Sinclair for their comments on previous drafts of the manuscript. NR 12 TC 2 Z9 2 U1 0 U2 0 PU CAMBRIDGE UNIV PRESS PI NEW YORK PA 32 AVENUE OF THE AMERICAS, NEW YORK, NY 10013-2473 USA SN 0008-347X EI 1918-3240 J9 CAN ENTOMOL JI Can. Entomol. PD FEB PY 2012 VL 144 IS 1 BP 158 EP 168 DI 10.4039/tce.2012.13 PG 11 WC Entomology SC Entomology GA 909OV UT WOS:000301575000011 ER PT J AU Andersen, KM Endara, MJ Turner, BL Dalling, JW AF Andersen, Kelly M. Endara, Maria Jose Turner, Benjamin L. Dalling, James W. TI Trait-based community assembly of understory palms along a soil nutrient gradient in a lower montane tropical forest SO OECOLOGIA LA English DT Article DE Habitat filtering; Niche differentiation; Functional traits; Species turnover; Trait plasticity ID FUNCTIONAL TRAITS; HABITAT SPECIALIZATION; LEAF TRAITS; RESOURCE AVAILABILITY; COASTAL CALIFORNIA; AMAZONIAN FORESTS; MINERAL-NUTRITION; PLANT-COMMUNITIES; CLIMATE-CHANGE; WILD PLANTS AB Two opposing niche processes have been shown to shape the relationship between ecological traits and species distribution patterns: habitat filtering and competitive exclusion. Habitat filtering is expected to select for similar traits among coexisting species that share similar habitat conditions, whereas competitive exclusion is expected to limit the ecological similarity of coexisting species leading to trait differentiation. Here, we explore how functional traits vary among 19 understory palm species that differ in their distribution across a gradient of soil resource availability in lower montane forest in western Panama. We found evidence that habitat filtering influences species distribution patterns and shifts community-wide and intraspecific trait values. Differences in trait values among sites were more strongly related to soil nutrient availability than to variation in light or rainfall. Soil nutrient availability explained a significant amount of variation in site mean trait values for 4 of 15 functional traits. Site mean values of leaf nitrogen and phosphorus increased 37 and 64%, respectively, leaf carbon: nitrogen decreased 38%, and specific leaf area increased 29% with increasing soil nutrient availability. For Geonoma cuneata, the only species occurring at all sites, leaf phosphorus increased 34% and nitrogen: phosphorus decreased 42% with increasing soil nutrients. In addition to among-site variation, most morphological and leaf nutrient traits differed among coexisting species within sites, suggesting these traits may be important for niche differentiation. Hence, a combination of habitat filtering due to turnover in species composition and intraspecific variation along a soil nutrient gradient and site-specific niche differentiation among co-occurring species influences understory palm community structure in this lower montane forest. C1 [Andersen, Kelly M.] Univ Georgia, Odum Sch Ecol, Athens, GA 30605 USA. [Andersen, Kelly M.; Turner, Benjamin L.; Dalling, James W.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. [Andersen, Kelly M.; Dalling, James W.] Univ Illinois, Program Ecol & Evolutionary Biol, Urbana, IL 61801 USA. [Endara, Maria Jose] Univ Utah, Dept Biol, Salt Lake City, UT 84112 USA. RP Andersen, KM (reprint author), Univ Georgia, Odum Sch Ecol, 140 E Green St, Athens, GA 30605 USA. EM kanderse@life.illinois.edu RI Turner, Benjamin/E-5940-2011 OI Turner, Benjamin/0000-0002-6585-0722 FU Smithsonian Tropical Research Institute; National Science Foundation [DEB 0608198]; University of Illinois at Urbana-Champaign FX We thank the Smithsonian Tropical Research Institute, the National Science Foundation (DEB 0608198), and the University of Illinois at Urbana-Champaign for financial support. We are grateful to Edevelio "Bady" Garcia for field and Tania Romero and Dayana Agudo for laboratory assistance. We thank C. Augspurger, C. Baldeck, L. Cernusak, A. Corrales, J. Dawson, M. Dietz, K. Heineman, B. Steidinger and three anonymous reviewers for providing comments on earlier versions of this manuscript and V. Jung for advice on null models. This study complies with laws of the Government of Panama. NR 67 TC 24 Z9 26 U1 4 U2 38 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0029-8549 J9 OECOLOGIA JI Oecologia PD FEB PY 2012 VL 168 IS 2 BP 519 EP 531 DI 10.1007/s00442-011-2112-z PG 13 WC Ecology SC Environmental Sciences & Ecology GA 911GQ UT WOS:000301705700022 PM 21894517 ER PT J AU Zhou, Z Wen, J Li, GD Sun, H AF Zhou, Zhuo Wen, Jun Li, Guodong Sun, Hang TI Phylogenetic assessment and biogeographic analyses of tribe Peracarpeae (Campanulaceae) SO PLANT SYSTEMATICS AND EVOLUTION LA English DT Article DE Campanulaceae; Heterocodon; Homocodon; Peracarpa; Peracarpeae; Madrean-Tethyan disjunction ID WESTERN NORTH-AMERICA; EASTERN ASIA; MOLECULAR PHYLOGENY; GEOGRAPHIC RANGE; EVOLUTION; DNA; SEQUENCES; CHLOROPLAST; HEMISPHERE; INFERENCE AB Peracarpeae is a small tribe consisting of three genera: Homocodon, Heterocodon and Peracarpa, with a disjunct distribution between eastern Asia and western North America. Homocodon is endemic to southwestern China and was previously placed in the western North American genus Heterocodon. Our phylogenetic analysis using four plastid markers (matK, atpB, rbcL and trnL-F) suggests the polyphyly of Peracarpeae. Homocodon is sister to a clade consisting of the eastern Asian Adenophora, Hanabusaya and species of Campanula from the Mediterranean region and North America, rather than forming a clade with Heterocodon. Homocodon and its Eurasia relatives are estimated to have diverged in the early Miocene (16.84 mya, 95% HPD 13.35-21.45 mya). The eastern Asian Peracarpa constitutes a clade with the North American Heterocodon, Githopsis and three species of Campanula, supporting a disjunction between eastern Asia and North America in Campanulaceae. The Asian-North American disjunct lineages diverged in the early Miocene (16.17 mya, 95% HPD 13.12-20.9 mya). The biogeographic analyses suggest that Homocodon may be a relict of an early radiation in eastern Asia, and that Peracarpa and its closest North American relatives most likely originated from a Eurasian ancestor. C1 [Zhou, Zhuo; Wen, Jun; Li, Guodong; Sun, Hang] Chinese Acad Sci, Kunming Inst Bot, Key Lab Biodivers & Biogeog, Kunming 650204, Yunnan, Peoples R China. [Zhou, Zhuo; Li, Guodong] Chinese Acad Sci, Grad Univ, Beijing 100049, Peoples R China. [Wen, Jun] Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, Washington, DC 20013 USA. RP Sun, H (reprint author), Chinese Acad Sci, Kunming Inst Bot, Key Lab Biodivers & Biogeog, Kunming 650204, Yunnan, Peoples R China. EM hsun@mail.kib.ac.cn FU National Natural Science Foundation of China (NSFC) [31061160184, 40930209, 31000101]; Chinese Academy of Sciences [KSCX2-YW-Z-1019]; John D. and Catherine T. MacArthur Foundation; Laboratory of Analytical Biology of the National Museum of Natural History, Smithsonian Institution FX The study was supported by grants from the National Natural Science Foundation of China (NSFC, 31061160184, 40930209, 31000101), the Innovation Project of the Chinese Academy of Sciences (KSCX2-YW-Z-1019) and the John D. and Catherine T. MacArthur Foundation to J. Wen, R. Ree and G. Mueller. Laboratory work was done at and partially supported by the Laboratory of Analytical Biology of the National Museum of Natural History, Smithsonian Institution. Laboratory assistance was provided by Lee Weigt, Jeff Hunt and Gabe Johnson at the Museum Support Center of the Smithsonian Institution. We thank Lawrence Janeway, David Boufford, Zelong Nie, Bo Xu and Yumin Shui for collecting samples. NR 84 TC 8 Z9 9 U1 1 U2 12 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 FEB PY 2012 VL 298 IS 2 BP 323 EP 336 DI 10.1007/s00606-011-0547-7 PG 14 WC Plant Sciences; Evolutionary Biology SC Plant Sciences; Evolutionary Biology GA 912HJ UT WOS:000301786500006 ER PT J AU Pabst, S Zack, T Savoy, IP Ludwig, T Rost, D Tonarini, S Vicenzi, EP AF Pabst, Sonja Zack, Thomas Savoy, Ivan P. Ludwig, Thomas Rost, Detlef Tonarini, Sonia Vicenzi, Edward P. TI The fate of subducted oceanic slabs in the shallow mantle: Insights from boron isotopes and light element composition of metasomatized blueschists from the Mariana forearc SO LITHOS LA English DT Article DE Blueschist; Izu-Bonin-Marianas subduction zone; Secondary ion mass spectrometry (SIMS); Time-of-Flight (ToF)-SIMS; Boron isotopes; Melange ID YOUNG VOLCANIC-ROCKS; SITE SELECTION SURVEYS; FLUID-MOBILE ELEMENTS; ION MASS-SPECTROMETRY; IZU-BONIN-MARIANA; ZONE MELANGE; METAMORPHIC ROCKS; CATALINA-SCHIST; TRACE-ELEMENTS; SEAMOUNT SUBDUCTION AB Serpentine muds from South Chamorro Seamount (SCS), drilled during ODP Leg 195 at Site 1200 contain metamafic clasts that experienced blueschist-facies metamorphism (including the critical mineral assemblage pumpellyite - Na-amphibole - epidote). These schists represent fragments from the actual slab-mantle interface at similar to 27 km depth. Their heterogeneous lithology with a metasomatic character indicates significant mobility of major elements in the Mariana forearc, a region of melange formation as it can also be observed in onland exposures such as the Catalina Schist. As the Mariana forearc blueschists show no late stage alteration they permit the direct study of material transfer during the subduction processes at an active convergent margin. This study presents the first data of detailed B isotope (delta B-11) and light element variations in blueschist-facies minerals from the Mariana arc system. The primary foci are B and Li concentrations and delta(11) values analyzed by SIMS and ToF-SIMS techniques. Minerals such as (Na-rich) amphibole, phengite and chlorite are found to be strongly enriched in Li (up to 70 [gig), Be (up to 8 mu g/g) and B (up to 35 mu g/g) and with delta B-11 values of -6 +/- 4 parts per thousand.. These new data are consistent with isotopically heavy B being released into the Mariana forearc mantle wedge (serpentinization of dry mantle peridotite after interaction with B-rich slab-released high pH fluids) and confirm models of significant B-loss and B isotope fractionation during forearc (shallow) slab dehydration. The elevated Li, Be and B concentrations in minerals that comprise the bulk of the rocks, namely, amphibole, phengite, and chlorite bear a strong potential to further transport Li and B as well as the isotopically light component of B to greater depths in the mantle, where ongoing metamorphism is responsible for further isotope and elemental fractionation and the formation of distinct mantle reservoirs, e.g. volcanic arc and oceanic intra-plate (OIB) magmas. (C) 2011 Elsevier B.V. All rights reserved. C1 [Pabst, Sonja; Ludwig, Thomas] Univ Heidelberg, Inst Geowissensch, INF 234 236, D-69120 Heidelberg, Germany. [Zack, Thomas] Johannes Gutenberg Univ Mainz, Inst Geowissensch, D-55099 Mainz, Germany. [Savoy, Ivan P.] Univ Leeds, Sch Earth & Environm, Leeds LS2 9JT, W Yorkshire, England. [Rost, Detlef] Univ Manchester, Sch Earth Atmospher & Environm Sci, Manchester M13 9PL, Lancs, England. [Tonarini, Sonia] CNR, Ist Geosci, I-56100 Pisa, Italy. [Vicenzi, Edward P.] Natl Museum Nat Hist, Smithsonian Inst, Dept Mineral Sci, Washington, DC 20560 USA. RP Pabst, S (reprint author), BHP Billiton Iron Ore, Explorat, POB 655, Newman, WA 6753, Australia. EM sonja.pabst@gmx.de RI Zack, Thomas/C-6153-2009; Zack, Thomas/K-7228-2013 OI Zack, Thomas/0000-0003-4747-4134 FU Deutsche Forschungsgemeinschaft (DFG) [Za285/4]; U.S. National Science Foundation (NSF) FX This study is part of the PhD work of the first author, funded by grants from the Deutsche Forschungsgemeinschaft (DFG, #Za285/4). The samples were allocated to I. Savoy by the Ocean Drilling Program (ODP Leg 195, Site 1200). ODP is sponsored by the U.S. National Science Foundation (NSF) and participating countries under the management of Joint Oceanographic Institutions (JOI), Inc. We like to thank H.P. Meyer for support with the electron microprobe analyses. NR 151 TC 22 Z9 22 U1 2 U2 42 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0024-4937 J9 LITHOS JI Lithos PD FEB PY 2012 VL 132 BP 162 EP 179 DI 10.1016/j.lithos.2011.11.010 PG 18 WC Geochemistry & Geophysics; Mineralogy SC Geochemistry & Geophysics; Mineralogy GA 904TD UT WOS:000301219900011 ER PT J AU Ratti, EM Steeghs, DTH Jonker, PG Torres, MAP Bassa, CG Verbunt, F AF Ratti, E. M. Steeghs, D. T. H. Jonker, P. G. Torres, M. A. P. Bassa, C. G. Verbunt, F. TI Optical spectroscopy of the quiescent counterpart to EXO 0748-676: a black widow scenario? SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE accretion, accretion discs; binaries eclipsing; stars: individual (EXO 0748-676); X-rays: binaries; X-rays: individual: EXO 0748-676 ID RAY-TIMING-EXPLORER; NEUTRON-STAR; DOPPLER TOMOGRAPHY; ECLIPSE TIMINGS; MASS; EMISSION; BINARIES; HOLE; EXO-0748-676; TRANSIENTS AB We present phase-resolved optical spectroscopy of the counterpart to the neutron star (NS) low-mass X-ray binary EXO 0748-676, almost one year after it turned into quiescence. The spectra display prominent H beta and H gamma and weak Fe II lines in emission. An average of all the spectra (corrected for the orbitalmotion) also exhibits a very weak line from Mg I. Tomographic reconstructions show that the accretion disc is not contributing to the optical line emission, which is instead dominated by the irradiated hemisphere of the companion star facing the NS. We could not detect absorption features from the mass donor star in the spectra. The emission lines appear broad, with an intrinsic full width at half-maximum (FWHM) of 255 +/- 22 km s(-1). Under the assumption that the width of the Fe II emission lines is dominated by rotational broadening, we obtain a lower limit on the compact object mass which is inconsistent with an NS accretor. We discuss this incongruity and conclude that either the lines are blends of unresolved features (although this requires some fine-tuning) or they are broadened by additional effects such as bulk gas motion in an outflow. The fact that the Fe II lines slightly lag in phase with respect to the companion star can be understood as outflowing gas consistent with a black-widow-like scenario. Nevertheless, we cannot rule out the possibility that blends of various emission lines cause the apparent phase lag of the Fe II emission lines as well as their large width. C1 [Ratti, E. M.; Jonker, P. G.; Torres, M. A. P.; Verbunt, F.] SRON Netherlands Inst Space Res, SRON, NL-3584 CA Utrecht, Netherlands. [Steeghs, D. T. H.; Jonker, P. G.; Torres, M. A. P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Steeghs, D. T. H.] Univ Warwick, Dept Phys, Coventry CV4 7AL, W Midlands, England. [Jonker, P. G.] Radboud Univ Nijmegen, IMAPP, Dept Astrophys, NL-6525 AJ Nijmegen, Netherlands. [Bassa, C. G.] Univ Manchester, Jodrell Bank Ctr Astrophys, Manchester M13 9PL, Lancs, England. [Verbunt, F.] Univ Utrecht, Astron Inst, NL-3508 TA Utrecht, Netherlands. RP Ratti, EM (reprint author), SRON Netherlands Inst Space Res, SRON, Sorbonnelaan 2, NL-3584 CA Utrecht, Netherlands. EM e.m.ratti@sron.nl RI Steeghs, Danny/C-5468-2009 OI Steeghs, Danny/0000-0003-0771-4746 FU VIDI; Netherlands Organisation for Scientific Research FX PGJ acknowledges support from a VIDI grant from the Netherlands Organisation for Scientific Research. Tom Marsh is thanked for developing and sharing his packages PAMELA and MOLLY. NR 42 TC 8 Z9 8 U1 0 U2 0 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD FEB PY 2012 VL 420 IS 1 BP 75 EP 83 DI 10.1111/j.1365-2966.2011.19999.x PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 905PL UT WOS:000301284600018 ER PT J AU Gruber, D Saio, H Kuschnig, R Fossati, L Handler, G Zwintz, K Weiss, WW Matthews, JM Guenther, DB Moffat, AFJ Rucinski, SM Sasselov, D AF Gruber, D. Saio, H. Kuschnig, R. Fossati, L. Handler, G. Zwintz, K. Weiss, W. W. Matthews, J. M. Guenther, D. B. Moffat, A. F. J. Rucinski, S. M. Sasselov, D. TI New slowly pulsating B stars in the field of the young open cluster NGC2244 discovered by the MOST photometric satellite SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE stars: early-type; stars: individual: GSC 00154-00785; stars: individual: GSC 00154-01871; stars: oscillations; stars: pre-main-sequence; open clusters and associations: individual: NGC2244 ID UVBY-BETA-PHOTOMETRY; ROSETTE NEBULA; NGC 2244; NGC-2244; SPACE; MEMBERSHIP; EVOLUTION; AGE AB During two weeks of nearly continuous optical photometry of the young open cluster NGC2244 obtained by the Microvariability and Oscillations of STars (MOST) satellite, we discovered two new slowly pulsating B (SPB) stars, GSC 00154-00785 and GSC 00154-01871. We present frequency analyses of the MOST light curves of these stars, which reveal two oscillation frequencies (0.61 and 0.71 cycle d(-1)) in GSC 00154-00785 and two (0.40 and 0.51 cycle d(-1)) in GSC 00154-01871. These frequency ranges are consistent with g modes of l <= 2 excited in models of main-sequence or pre-main-sequence (PMS) stars of masses 4.5-5M(circle dot) and solar composition (X, Z) = (0.7, 0.02). Published proper motion measurements and radial velocities are insufficient to establish unambiguously cluster membership for these two stars. However, the PMS models which fit best their eigenspectra have ages consistent with NGC2244. If cluster membership can be confirmed, these would be the first known PMS SPB stars, and would open a new window on testing asteroseismically the interior structures of PMS stars. C1 [Gruber, D.; Kuschnig, R.; Zwintz, K.; Weiss, W. W.] Univ Vienna, Inst Astron, A-1180 Vienna, Austria. [Gruber, D.] Max Planck Inst Extraterr Phys, D-85748 Munich, Germany. [Saio, H.] Tohoku Univ, Grad Sch Sci, Astron Inst, Sendai, Miyagi 9808578, Japan. [Fossati, L.] Open Univ, Dept Phys & Astron, Milton Keynes MK7 6AA, Bucks, England. [Handler, G.] Nicolaus Copernicus Astron Ctr, PL-00716 Warsaw, Poland. [Matthews, J. M.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada. [Guenther, D. B.] St Marys Univ, Dept Astron & Phys, Halifax, NS B3H 3C3, Canada. [Moffat, A. F. J.] Univ Montreal, Dept Phys, Montreal, PQ H3C 3J7, Canada. [Rucinski, S. M.] Univ Toronto, David Dunlap Observ, Dept Astron & Astrophys, Richmond Hill, ON L4C 4Y6, Canada. [Sasselov, D.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Gruber, D (reprint author), Univ Vienna, Inst Astron, Turkenschanzstr 17, A-1180 Vienna, Austria. EM dgruber@mpe.mpg.de; saio@astr.tohoku.ac.jp OI Zwintz, Konstanze/0000-0001-9229-8315 FU STFC; Austrian Fonds zur Forderung der wissenschaftlichen Forschung [P20526-N16, P22691-N16]; Austrian Academy of Sciences at the Institute of Astronomy of the University Vienna; NSERC (Canada); Canadian Space Agency FX The authors are grateful to Ewa Niemczura for useful discussion and the analysis of the FEROS spectra. We dedicate this work to the memory of our dear friend and colleague Dr Piet Reegen, who will be greatly missed by us all. Astronomy research at the Open University is supported by an STFC rolling grant (LF). GH is partially supported by the Austrian Fonds zur Forderung der wissenschaftlichen Forschung under grant P20526-N16 and WWW by P22691-N16. KZ is recipient of an APART fellowship of the Austrian Academy of Sciences at the Institute of Astronomy of the University Vienna. JMM, AFJM and SMR are funded by NSERC (Canada), and some of RK's contributions were partially funded by the Canadian Space Agency. This research has made use of the WEBDA database, operated at the Institute for Astronomy of the University of Vienna. NR 38 TC 5 Z9 5 U1 0 U2 1 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD FEB PY 2012 VL 420 IS 1 BP 291 EP 298 DI 10.1111/j.1365-2966.2011.20033.x PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 905PL UT WOS:000301284600036 ER PT J AU Hopkins, PF Hayward, CC Narayanan, D Hernquist, L AF Hopkins, Philip F. Hayward, Christopher C. Narayanan, Desika Hernquist, Lars TI The origins of active galactic nuclei obscuration: the 'torus' as a dynamical, unstable driver of accretion SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies: active; galaxies: evolution; quasars: general; cosmology: theory ID SUPERMASSIVE BLACK-HOLES; ULTRALUMINOUS INFRARED GALAXIES; DIGITAL-SKY-SURVEY; QUASAR LUMINOSITY FUNCTION; HUBBLE-SPACE-TELESCOPE; PARTICLE HYDRODYNAMICS SIMULATIONS; NARROW-LINE REGION; X-RAY LUMINOSITY; INTEGRAL FIELD SPECTROSCOPY; ABSORBING COLUMN DENSITIES AB Recent multiscale simulations have made it possible to follow gas inflows responsible for high-Eddington ratio accretion on to massive black holes (BHs) from galactic scales to the BH accretion disc. When sufficient gas is driven towards a BH, gravitational instabilities generically form lopsided, eccentric discs that propagate inwards from larger radii. The lopsided stellar disc exerts a strong torque on the gas, driving inflows that fuel the growth of the BH. Here, we investigate the possibility that the same disc, in its gas-rich phase, is the putative 'torus' invoked to explain obscured active galactic nuclei (AGN) and the cosmic X-ray background. The disc is generically thick and has characteristic similar to 1-10 pc sizes and masses resembling those required of the torus. Interestingly, the scale heights and obscured fractions of the predicted torii are substantial even in the absence of strong stellar feedback providing the vertical support. Rather, they can be maintained by strong bending modes and warps/twists excited by the inflow-generating instabilities. A number of other observed properties commonly attributed to 'feedback' processesmay in fact be explained entirely by dynamical, gravitational effects: the lack of alignment between torus and host galaxy, correlations between local star formation rate (SFR) and turbulent gas velocities and the dependence of obscured fractions on AGN luminosity or SFR. We compare the predicted torus properties with observations of gas surface density profiles, kinematics, scale heights and SFR densities in AGN, and find that they are consistent in all cases. We argue that it is not possible to reproduce these observations and the observed column density distribution without a clumpy gas distribution, but allowing for simple clumping on small scales the predicted column density distribution is in good agreement with observations from N-H similar to 10(20)-10(27) cm(-2). We examine how the N-H distribution scales with galaxy and AGN properties. The dependence is generally simple, but AGN feedback may be necessary to explain certain trends in obscured fraction with luminosity and/or redshift. In our paradigm, the torus is not merely a bystander or passive fuel source for accretion, but is itself the mechanism driving accretion. Its generic properties are not coincidence, but requirements for efficient accretion. C1 [Hopkins, Philip F.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Hayward, Christopher C.; Hernquist, Lars] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Narayanan, Desika] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. RP Hopkins, PF (reprint author), Univ Calif Berkeley, Dept Astron, 601 Campbell Hall, Berkeley, CA 94720 USA. EM phopkins@astro.berkeley.edu RI Hayward, Christopher/I-4756-2012 OI Hayward, Christopher/0000-0003-4073-3236 FU NSF [AST-1009452]; Miller Institute for Basic Research in Science, University of California Berkeley FX We thank Eliot Quataert, Nadia Zakamska, Jenny Greene, Patrik Jonsson and Josh Younger for helpful discussions in the development of this work. Support for PFH was provided by the Miller Institute for Basic Research in Science, University of California Berkeley. DN and LH acknowledge support from the NSF via grant AST-1009452. NR 249 TC 32 Z9 32 U1 0 U2 0 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD FEB PY 2012 VL 420 IS 1 BP 320 EP 339 DI 10.1111/j.1365-2966.2011.20035.x PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 905PL UT WOS:000301284600039 ER PT J AU Turnbull, SJ Hudson, MJ Feldman, HA Hicken, M Kirshner, RP Watkins, R AF Turnbull, Stephen J. Hudson, Michael J. Feldman, Hume A. Hicken, Malcolm Kirshner, Robert P. Watkins, Richard TI Cosmic flows in the nearby universe from Type Ia supernovae SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE supernovae: general; cosmological parameters; cosmology: observations; dark matter; large-scale structure of Universe ID PECULIAR VELOCITY-FIELD; SKY REDSHIFT SURVEY; LIGHT-CURVE SHAPES; 100 H(-1) MPC; GRAVITY-FIELD; BULK FLOW; DIPOLE ANISOTROPY; LOCAL UNIVERSE; DATA RELEASE; PSCZ DIPOLE AB Peculiar velocities are one of the only probes of very large scale mass density fluctuations in the nearby Universe. We present new 'minimal variance' bulk flow measurements based upon the 'First Amendment' compilation of 245 Type Ia supernovae (SNe) peculiar velocities and find a bulk flow of 249 +/- 76 km s(-1) in the direction l = 319 degrees +/- 18 degrees, b = 7 degrees +/- 14 degrees. The SNe bulk flow is consistent with the expectations of Lambda cold dark matter (Lambda CDM). However, it is also marginally consistent with the bulk flow of a larger compilation of non-SNe peculiar velocities. By comparing the SNe peculiar velocities to predictions of the IRAS Point Source Catalogue Redshift Survey (PSCz) galaxy density field, we find Omega(0.55)(m) sigma(8,lin) = 0.40 +/- 0.07, which is in agreement with Lambda CDM. However, we also show that the PSCz density field fails to account for 150 +/- 43 km s(-1) of the SNe bulk motion. C1 [Turnbull, Stephen J.; Hudson, Michael J.] Univ Waterloo, Dept Phys & Astron, Waterloo, ON N2L 3G1, Canada. [Hudson, Michael J.] Perimeter Inst Theoret Phys, Waterloo, ON N2L 2Y5, Canada. [Feldman, Hume A.] Univ Kansas, Dept Phys & Astron, Lawrence, KS 66045 USA. [Hicken, Malcolm; Kirshner, Robert P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Watkins, Richard] Willamette Univ, Dept Phys, Salem, OR 97301 USA. RP Turnbull, SJ (reprint author), Univ Waterloo, Dept Phys & Astron, Waterloo, ON N2L 3G1, Canada. EM s4turnbu@uwaterloo.ca RI Hudson, Michael/H-3238-2012 OI Hudson, Michael/0000-0002-1437-3786 FU NSERC; NSF [AST0907903]; National Aeronautics and Space Administration FX We thank Alex Conley for helpful comparisons of SNe data and acknowledge useful discussions with John Lucey, Roya Mohayaee and Jacques Colin. SJT and MJH acknowledge the financial support of NSERC. RPK acknowledges support from the NSF grant AST0907903.; This research has made use of the NASA/IPAC Extragalactic Database (NED) which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. NR 47 TC 73 Z9 73 U1 0 U2 0 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD FEB PY 2012 VL 420 IS 1 BP 447 EP 454 DI 10.1111/j.1365-2966.2011.20050.x PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 905PL UT WOS:000301284600051 ER PT J AU Pe'er, A Zhang, BB Ryde, F McGlynn, S Zhang, B Preece, RD Kouveliotou, C AF Pe'er, Asaf Zhang, Bin-Bin Ryde, Felix McGlynn, Sinead Zhang, Bing Preece, Robert D. Kouveliotou, Chryssa TI The connection between thermal and non-thermal emission in gamma-ray bursts: general considerations and GRB090902B as a case study SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE plasmas; radiation mechanisms: thermal; radiative transfer; scattering; gamma-ray burst: general ID INTERNAL SHOCK MODEL; HIGH-ENERGY EMISSION; SELF-COMPTON EMISSION; SCALE MAGNETIC-FIELDS; PROMPT EMISSION; X-RAY; SYNCHROTRON EMISSION; PHOTOSPHERIC EMISSION; PHYSICAL PARAMETERS; SPECTRAL PROPERTIES AB Photospheric (thermal) emission is inherent to the gamma-ray burst (GRB) 'fireball' model. We show here that inclusion of this component in the analysis of the GRB prompt emission phase naturally explains some of the prompt GRB spectra seen by the Fermi satellite over its entire energy band. The sub-MeV peak is explained as multicolour blackbody emission, and the high-energy tail, extending up to the GeV band, results from roughly similar contributions of synchrotron emission, synchrotron self-Compton and Comptonization of the thermal photons by energetic electrons originating after dissipation of the kinetic energy above the photosphere. We show how this analysis method results in a complete, self-consistent picture of the physical conditions at both emission sites of the thermal and non-thermal radiation. We study the connection between the thermal and non-thermal parts of the spectrum, and show how the values of the free model parameters are deduced from the data. We demonstrate our analysis method on GRB090902B: we deduce a Lorentz factor in the range 920 <= eta <= 1070, photospheric radius r(ph) similar or equal to 7.2-8.4 x 10(11) cm and dissipation radius r(gamma) >= 3.5-4.1 x 10(15) cm. By comparison to afterglow data, we deduce that a large fraction epsilon(d) approximate to 85-95 per cent of the kinetic energy is dissipated, and that a large fraction, similar to equipartition of this energy, is carried by the electrons and the magnetic field. This high value of epsilon(d) questions the 'internal shock' scenario as the main energy dissipation mechanism for this GRB. C1 [Pe'er, Asaf] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Pe'er, Asaf] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Zhang, Bin-Bin; Zhang, Bing] Univ Nevada, Dept Phys & Astron, Las Vegas, NV 89154 USA. [Ryde, Felix; McGlynn, Sinead] Royal Inst Technol, Dept Phys, AlbaNova, SE-10691 Stockholm, Sweden. [Preece, Robert D.] Univ Alabama, CSPAR, Huntsville, AL 35899 USA. [Kouveliotou, Chryssa] NASA, George C Marshall Space Flight Ctr, Space Sci Off, Huntsville, AL 35812 USA. RP Pe'er, A (reprint author), Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA. EM apeer@cfa.harvard.edu RI Zhang, Binbin/C-9035-2013; OI Zhang, Binbin/0000-0003-2002-116X; Preece, Robert/0000-0003-1626-7335 FU Space Telescope Science Institute; Fermi grant [31014]; Swedish National Space Board FX This research was supported by the Riccardo Giacconi Fellowship award of the Space Telescope Science Institute, and Fermi grant award #31014. FR acknowledges financial support by the Swedish National Space Board. AP wishes to thank Dale Frail, Jeremy Schnittman, Andy Fruchter, Kuntal Misra, Zeljka Bosnjak, Mario Livio and Kailash Sahu for useful discussions. NR 98 TC 52 Z9 52 U1 0 U2 5 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD FEB PY 2012 VL 420 IS 1 BP 468 EP 482 DI 10.1111/j.1365-2966.2011.20052.x PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 905PL UT WOS:000301284600053 ER PT J AU Narayan, R Piran, T AF Narayan, Ramesh Piran, Tsvi TI Variability in blazars: clues from PKS 2155-304 SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE black hole physics; magnetic reconnection; relativistic processes; turbulence; BL Lacertae objects: individual: PKS 2155-304; galaxies: jets ID GAMMA-RAY BURSTS; FAST TEV VARIABILITY; RECONNECTION; MINIJETS; OBJECTS; MODEL; JETS AB Rapid variability on a time-scale much faster than the light-crossing time of the central supermassive black hole has been seen in TeV emission from the blazar PKS 2155-304. The most plausible explanation for this puzzling observation is that the radiating fluid in the relativistic jet is divided into a large number of subregions which move in random directions with relative Lorentz factors approximate to gamma(j)'. The random motions introduce new relativistic effects, over and above those due to the overall mean bulk Lorentz factor Gamma(b) of the jet. We consider two versions of this 'jets in a jet' model. In the first, the 'subjets' model, stationary regions in the mean jet frame emit relativistic subjets that produce the observed radiation. The variability time-scale is determined by the size of the subregions in the mean jet frame. This model, which is loosely based on magnetic reconnection, has great difficulty explaining the observations in PKS 2155-304. In the alternate 'turbulence' model, various subregions move relativistically in random directions and the variability time-scale is determined by the size of these regions in their own comoving frames. This model fits the data much more comfortably. Details such as what generates the turbulent motion, how particles are heated, and what the radiation process is, remain to be worked out. We consider collisions between TeV photons and soft photons and find that, in both the subjets and turbulence models, the mean bulk Lorentz factor Gamma(b) of the jet needs to be >25 to avoid the pair catastrophe. C1 [Narayan, Ramesh] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Piran, Tsvi] Hebrew Univ Jerusalem, Racah Inst Phys, IL-91904 Jerusalem, Israel. RP Narayan, R (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM rnarayan@cfa.harvard.edu; tsvi@phys.huji.ac.il OI Narayan, Ramesh/0000-0002-1919-2730 FU NSF [AST-1041590]; NASA [NNX11AE16G]; Israel Center for Excellence for High Energy Astrophysics; ERC FX We thank Yury Lyubarsky for useful discussions on the physics of relativistic reconnection, and the referee for helpful comments. This work was supported in part by NSF grant AST-1041590 and NASA grant NNX11AE16G (RN), and by the Israel Center for Excellence for High Energy Astrophysics and an ERC advanced research grant (TP). NR 25 TC 38 Z9 38 U1 1 U2 2 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD FEB PY 2012 VL 420 IS 1 BP 604 EP 612 DI 10.1111/j.1365-2966.2011.20069.x PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 905PL UT WOS:000301284600066 ER PT J AU Penna, RF Sadowski, A McKinney, JC AF Penna, Robert F. Sadowski, Aleksander McKinney, Jonathan C. TI Thin-disc theory with a non-zero-torque boundary condition and comparisons with simulations SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE accretion, accretion discs; black hole physics; gravitation; hydrodynamics; MHD ID BLACK-HOLE SPIN; CONTINUUM-FITTING METHOD; MARGINALLY STABLE ORBIT; X-RAY CONTINUUM; ACCRETION DISK; SLIM DISKS; STRESS; INSTABILITY; RADIATION; BINARIES AB We present an analytical solution for thin-disc accretion on to a Kerr black hole that extends the standard Novikov-Thorne alpha-disc in three ways: (i) it incorporates non-zero stresses at the inner edge of the disc; (ii) it extends into the plunging region; and (iii) it uses a corrected vertical gravity formula. The free parameters of the model are unchanged. Non-zero boundary stresses are included by replacing the Novikov-Thorne no-torque boundary condition with the less strict requirement that the fluid velocity at the innermost stable circular orbit is the sound speed, which numerical models show to be the correct behaviour for luminosities below similar to 30 per cent Eddington. We assume the disc is thin so we can ignore advection. Boundary stresses scale as alpha h and advection terms scale as h(2) [where h is the disc opening angle (h = H/r)], so the model is self-consistent when h < alpha. We compare our solution with slim-disc models and general relativistic magnetohydrodynamic disc simulations. The model may improve the accuracy of black hole spin measurements. C1 [Penna, Robert F.; Sadowski, Aleksander] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [McKinney, Jonathan C.] Stanford Univ, Dept Phys, Stanford, CA 94305 USA. [McKinney, Jonathan C.] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94305 USA. RP Penna, RF (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM rpenna@cfa.harvard.edu; asadowski@cfa.harvard.edu; jmckinne@stanford.edu FU NSF [AST-1041590]; NASA [NNX11AE16G]; NSF through TeraGrid resources [TG-AST080025N, TG-AST080026N] FX We thank Stephen Balbus, Ramesh Narayan and Alexander Tchekhovskoy for discussions. This work was supported by an NSF Graduate Research Fellowship (RFP), NSF grant AST-1041590, NASA grant NNX11AE16G, and by the NSF through TeraGrid resources provided by NCSA (Abe), LONI (QueenBee) and NICS (Kraken) under grant numbers TG-AST080025N and TG-AST080026N. NR 35 TC 16 Z9 16 U1 0 U2 0 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD FEB PY 2012 VL 420 IS 1 BP 684 EP 698 DI 10.1111/j.1365-2966.2011.20084.x PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 905PL UT WOS:000301284600073 ER PT J AU Offner, SSR Capodilupo, J Schnee, S Goodman, AA AF Offner, Stella S. R. Capodilupo, John Schnee, Scott Goodman, Alyssa A. TI Observing turbulent fragmentation in simulations: predictions for CARMA and ALMA SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE stars: protostars; stars: starless cores ID STARLESS CORES; GRAVITATIONAL INSTABILITIES; DISKS; MULTIPLICITY; ENVELOPE; PERSEUS; SYSTEMS; CLOUDS; DISCS AB Determining the initial stellar multiplicity is a challenging problem since protostars are faint and deeply embedded at early times; once formed, multiple protostellar systems may significantly dynamically evolve before they are optically revealed. Interferometers such as Combined Array for Research in Millimeter-wave Astronomy (CARMA) and Atacama Large Millimeter/submillimeter Array (ALMA) make it possible to probe the scales at which turbulent fragmentation occurs in dust continuum emission, potentially constraining early stellar multiplicity. In this Letter, we present synthetic observations of starless and protostellar cores undergoing fragmentation on scales of a few thousand astronomical units to produce wide binary systems. We show that interferometric observations of starless cores by CARMA should be predominantly featureless at early stages, although wide protostellar companions should be apparent. The enhanced capabilities of ALMA improve the detection of core morphology so that it may be possible to detect substructure at earlier times. In either case, spatial filtering from interferometry reduces the observed core substructure and often eradicates traces of existing filamentary morphology on scales down to 0.025 pc. However, some missing structure may be recaptured by combining data from the ALMA full science and Atacama compact arrays. C1 [Offner, Stella S. R.; Goodman, Alyssa A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Capodilupo, John] Harvard Univ, Cambridge, MA 02138 USA. [Schnee, Scott] Natl Radio Astron Observ, Charlottesville, VA 22903 USA. RP Offner, SSR (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM soffner@cfa.harvard.edu RI Goodman, Alyssa/A-6007-2010 OI Goodman, Alyssa/0000-0003-1312-0477 FU NSF [AST-0901055, AST-0908159]; Harvard College FX This research has been supported by the NSF through grants AST-0901055 (SSRO) and AST-0908159 (AAG) and the Harvard College Programme for Research in Science and Engineering (JC). NR 26 TC 13 Z9 13 U1 0 U2 0 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD FEB PY 2012 VL 420 IS 1 BP L53 EP L57 DI 10.1111/j.1745-3933.2011.01194.x PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 905PL UT WOS:000301284600012 ER PT J AU Vogt, J Skora, A Feller, IC Piou, C Coldren, G Berger, U AF Vogt, Juliane Skora, Annegret Feller, Ilka C. Piou, Cyril Coldren, Glenn Berger, Uta TI Investigating the role of impoundment and forest structure on the resistance and resilience of mangrove forests to hurricanes SO AQUATIC BOTANY LA English DT Article DE Succession; Disturbance; Mangrove forest dynamics; Hurricane; Impoundment; Florida; Neotropics ID DISTURBANCE; REGENERATION; VEGETATION; PATTERNS; DAMAGE; CONSEQUENCES; REDUCTION; DISPERSAL; DYNAMICS; RECOVERY AB The present study evaluates how a prolonged artificial flooding regime in impounded mangrove forests influences the regeneration after medium-sized forest destruction created by two hurricanes in 2004 in the Indian River Lagoon, Florida, USA. Disturbance patterns, forest structure, and regeneration were investigated. We found disturbed areas, characterized by uprooted and snapped trees, and intact forests in close proximity. The canopy turnover was greater in forests in higher succession stages with median tree diameter at breast height of 7.6 +/- 5.7 cm compared to the intact forest with 3.7 +/- 1.2 cm. Larger trees with lower densities were more susceptible to hurricane damage. We observed that regeneration of the open patches was dominated by the flood-tolerant species Rhizophora mangle (89.9%) instead of the faster-growing pioneer species Laguncularia racemosa (7.0%). Some of the disturbed areas created by the hurricanes were not recolonized. The regeneration rate of the disturbed areas expressed by vegetation closure >50% differed between almost zero to 100% in three different impoundments. We concluded that the artificial flooding regime imposed by impoundment is the predominant selective force in the successive process according to the species composition. However, we were not able to detect the driving factors that prevented mangrove establishment in disturbed areas. (C) 2011 Elsevier B.V. All rights reserved. C1 [Vogt, Juliane; Skora, Annegret; Berger, Uta] Tech Univ Dresden, Dept Forest Biometry & Syst Anal, Inst Forest Growth & Forest Comp Sci, D-01735 Tharandt, Germany. [Feller, Ilka C.] Smithsonian Environm Res Ctr, Anim Plant Interact Lab, Edgewater, MD 21037 USA. [Piou, Cyril] UPR Bioagresseurs Anal & Maitrise Risque, CIRAD, F-34398 Montpellier, France. [Coldren, Glenn] Florida Atlantic Univ, Dept Biol, Ft Pierce, FL 34946 USA. RP Vogt, J (reprint author), Tech Univ Dresden, Dept Forest Biometry & Syst Anal, Inst Forest Growth & Forest Comp Sci, Postfach 1117, D-01735 Tharandt, Germany. EM juliane.vogt@forst.tu-dresden.de; annegret.skora@gmx.net; felleri@si.edu; cyril.piou@cirad.fr; gcoldren@fau.edu; uta.berger@tu-dresden.de OI Feller, Ilka/0000-0002-6391-1608 FU DFG [BE 1960/6-1] FX We appreciated the valuable advices of the two anonymous reviewers and the editor-in-chief George Bowes very much. Further we would like to thank James David the head of the Mosquito Control in the St. Lucie County, who gave us valuable information about the impoundment strategies. The Smithsonian Marine Station in Fort Pierce provided the facilities and a fellowship for carrying out the field work. Further, the DFG (BE 1960/6-1) grant a scholarship for Juliane Vogt. NR 38 TC 5 Z9 5 U1 4 U2 29 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0304-3770 J9 AQUAT BOT JI Aquat. Bot. PD FEB PY 2012 VL 97 IS 1 BP 24 EP 29 DI 10.1016/j.aquabot.2011.10.006 PG 6 WC Plant Sciences; Marine & Freshwater Biology SC Plant Sciences; Marine & Freshwater Biology GA 904QV UT WOS:000301213900004 ER PT J AU Bulgarelli, A Tavani, M Chen, AW Evangelista, Y Trifoglio, M Gianotti, F Piano, G Sabatini, S Striani, E Pooley, G Trushkin, S Nizhelskij, NA McCollough, M Koljonen, KII Hannikainen, D Lahteenmaki, A Tammi, J Lavonen, N Steeghs, D Aboudan, A Argan, A Barbiellini, G Campana, R Caraveo, P Cattaneo, PW Cocco, V Contessi, T Costa, E D'Ammando, F Del Monte, E De Paris, G Di Cocco, G Donnarumma, I Feroci, M Fiorini, M Fuschino, F Galli, M Giuliani, A Giusti, M Labanti, C Lapshov, I Lazzarotto, F Lipari, P Longo, F Marisaldi, M Mereghetti, S Morelli, E Moretti, E Morselli, A Pacciani, L Pellizzoni, A Perotti, F Picozza, P Pilia, M Prest, M Pucella, G Rapisarda, M Rappoldi, A Rubini, A Soffitta, P Trois, A Vallazza, E Vercellone, S Vittorini, V Zambra, A Zanello, D Giommi, P Pittori, C Verrecchia, F Santolamazza, P Lucarelli, F Colafrancesco, S Salotti, L AF Bulgarelli, A. Tavani, M. Chen, A. W. Evangelista, Y. Trifoglio, M. Gianotti, F. Piano, G. Sabatini, S. Striani, E. Pooley, G. Trushkin, S. Nizhelskij, N. A. McCollough, M. Koljonen, K. I. I. Hannikainen, D. Lahteenmaki, A. Tammi, J. Lavonen, N. Steeghs, D. Aboudan, A. Argan, A. Barbiellini, G. Campana, R. Caraveo, P. Cattaneo, P. W. Cocco, V. Contessi, T. Costa, E. D'Ammando, F. Del Monte, E. De Paris, G. Di Cocco, G. Donnarumma, I. Feroci, M. Fiorini, M. Fuschino, F. Galli, M. Giuliani, A. Giusti, M. Labanti, C. Lapshov, I. Lazzarotto, F. Lipari, P. Longo, F. Marisaldi, M. Mereghetti, S. Morelli, E. Moretti, E. Morselli, A. Pacciani, L. Pellizzoni, A. Perotti, F. Picozza, P. Pilia, M. Prest, M. Pucella, G. Rapisarda, M. Rappoldi, A. Rubini, A. Soffitta, P. Trois, A. Vallazza, E. Vercellone, S. Vittorini, V. Zambra, A. Zanello, D. Giommi, P. Pittori, C. Verrecchia, F. Santolamazza, P. Lucarelli, F. Colafrancesco, S. Salotti, L. TI AGILE detection of Cygnus X-3 gamma-ray active states during the period mid-2009/mid-2010 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE gamma-rays: stars; stars: individual: Cygnus X-3 ID FALSE-DISCOVERY RATE; HARD X-RAY; SILICON TRACKER; EMISSION-LINES; VARIABILITY; PULSARS; MISSION; REGION; SPACE; LAT AB Context. Cygnus X-3 (Cyg X-3) is a well-known microquasar producing variable emission at all wavelengths. Cyg X-3 is a prominent X-ray binary producing relativistic jets, and studying its high energy emission is crucial for the understanding of the fundamental acceleration processes in accreting compact objects. Aims. Our goal is to study extreme particle acceleration and gamma-ray production above 100 MeV during special spectral states of Cyg X-3 usually characterized by a low hard X-ray flux and enhanced soft X-ray states. Methods. We observed Cyg X-3 with the AGILE satellite in extended time intervals from 2009 Jun.-Jul., and 2009 Nov.-2010 Jul. We report here the results of the AGILE gamma-ray monitoring of Cyg X-3 as well as the results from extensive multiwavelength campaigns involving radio (RATAN-600, AMI-LA and Metsahovi Radio Observatories) and X-ray monitoring data (XTE and Swift). Results. We detect a series of repeated gamma-ray flaring activity from Cyg X-3 that correlate with the soft X-ray states and episodes of decreasing or non-detectable hard X-ray emission. Furthermore, we detect gamma-ray enhanced emission that tends to be associated with radio flares greater than 1 Jy at 15 GHz, confirming a trend already detected in previous observations. The source remained active above 100 MeV for an extended period of time (almost 1.5 months in 2009 Jun.-Jul. and 1 month in 2010 May). We study in detail the short timescale gamma-ray flares that occurred before or near the radio peaks. Conclusions. Our results confirm the transient nature of the extreme particle acceleration from the microquasar Cyg X-3. A series of repeated gamma-ray flares shows correlations with radio and X-ray emission confirming a well established trend of emission. We compare our results with Fermi-LAT and MAGIC TeV observations of Cyg X-3. C1 [Bulgarelli, A.; Trifoglio, M.; Gianotti, F.; Costa, E.; Di Cocco, G.; Labanti, C.; Marisaldi, M.; Morelli, E.] INAF IASF Bologna, I-40129 Bologna, Italy. [Tavani, M.; Evangelista, Y.; Piano, G.; Argan, A.; Campana, R.; Cocco, V.; Del Monte, E.; De Paris, G.; Donnarumma, I.; Feroci, M.; Giusti, M.; Lapshov, I.; Lazzarotto, F.; Pacciani, L.; Rubini, A.; Soffitta, P.; Trois, A.; Vittorini, V.] INAF IASF Roma, I-00133 Rome, Italy. [Tavani, M.; Chen, A. W.; Contessi, T.; Fuschino, F.; Giusti, M.; Vittorini, V.] CIFS Torino, I-10133 Turin, Italy. [Chen, A. W.; Caraveo, P.; Contessi, T.; Fiorini, M.; Giuliani, A.; Mereghetti, S.; Perotti, F.; Zambra, A.] INAF IASF Milano, I-20133 Milan, Italy. [Tavani, M.; Sabatini, S.; Striani, E.; Picozza, P.] Univ Roma Tor Vergata, Dip Fis, I-00133 Rome, Italy. [Barbiellini, G.; Longo, F.; Moretti, E.; Vallazza, E.] Dip Fis, I-34127 Trieste, Italy. [Barbiellini, G.; Longo, F.; Moretti, E.; Vallazza, E.] Ist Nazl Fis Nucl, I-34127 Trieste, Italy. [Galli, M.] ENEA Bologna, I-40059 Medicica, BO, Italy. [Lipari, P.; Zanello, D.] INFN Roma La Sapienza, I-00185 Rome, Italy. [Cattaneo, P. W.; Rappoldi, A.] Ist Nazl Fis Nucl, I-27100 Pavia, Italy. [Tavani, M.; Piano, G.; Sabatini, S.; Striani, E.; Morselli, A.; Picozza, P.] INFN Roma Tor Vergata, I-00133 Rome, Italy. [Pilia, M.; Prest, M.; Salotti, L.] Univ Insubria, Dip Fis, I-22100 Como, Italy. [Pucella, G.; Rapisarda, M.] ENEA Frascati, I-00044 Rome, Italy. [Giommi, P.; Pittori, C.; Verrecchia, F.; Santolamazza, P.; Lucarelli, F.; Colafrancesco, S.] AS ASDC, I-00044 Rome, Italy. [Lipari, P.] Univ Roma La Sapienza, Dipartimento Fis, I-00185 Rome, Italy. [Pellizzoni, A.; Pilia, M.] INAF Osservatorio Astron Cagliari, I-09012 Cagliari, Italy. [Pooley, G.] Univ Cambridge, Cavendish Lab, Astrophys Grp, Cambridge CB3 0HE, England. [Trushkin, S.; Nizhelskij, N. A.] RAS, Special Astrophys Observ, Karachaevo Cherkassian R 36916, Nizhnij Arkhyz, Russia. [McCollough, M.] Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Hannikainen, D.] Univ Turku, Finnish Ctr Astron ESO FINCA, Piikkio 21500, Finland. [Koljonen, K. I. I.; Hannikainen, D.; Lahteenmaki, A.; Tammi, J.; Lavonen, N.] Aalto Univ, Metsahovi Radio Observ, Kylmala 02540, Finland. [D'Ammando, F.; Vercellone, S.] INAF IASF Palermo, I-90146 Palermo, Italy. [Steeghs, D.] Univ Warwick, Astron & Astrophys Dept Phys, Coventry CV4 7AL, W Midlands, England. [Aboudan, A.] Univ Padua, CISAS G Colombo, I-35131 Padua, Italy. [Hannikainen, D.] Florida Inst Technol, Dept Phys & Space Sci, Melbourne, FL 32901 USA. [Colafrancesco, S.] Osserv Astron Roma, INAF, I-00040 Monte Porzio Catone, Italy. [Colafrancesco, S.] Univ Witwatersrand, Sch Phys, ZA-2050 Johannesburg Wits, South Africa. RP Bulgarelli, A (reprint author), INAF IASF Bologna, Via Gobetti 101, I-40129 Bologna, Italy. EM bulgarelli@iasfbo.inaf.it RI Lazzarotto, Francesco/J-4670-2012; Morselli, Aldo/G-6769-2011; Steeghs, Danny/C-5468-2009; Lahteenmaki, Anne/L-5987-2013; Campana, Riccardo/F-5272-2015; Trifoglio, Massimo/F-5302-2015; Pittori, Carlotta/C-7710-2016; OI Bulgarelli, Andrea/0000-0001-6347-0649; Cattaneo, Paolo Walter/0000-0001-6877-6882; Donnarumma, Immacolata/0000-0002-4700-4549; Sabatini, Sabina/0000-0003-2076-5767; Morselli, Aldo/0000-0002-7704-9553; Steeghs, Danny/0000-0003-0771-4746; Gianotti, Fulvio/0000-0003-4666-119X; Fiorini, Mauro/0000-0001-8297-1983; Pellizzoni, Alberto Paolo/0000-0002-4590-0040; Campana, Riccardo/0000-0002-4794-5453; Trifoglio, Massimo/0000-0002-2505-3630; Pittori, Carlotta/0000-0001-6661-9779; trois, alessio/0000-0002-3180-6002; Verrecchia, Francesco/0000-0003-3455-5082 FU Italian Space Agency (ASI); Italian Institute of Nuclear Physics (INFN); ASI [I/089/06/2, I/042/10/0]; ASI-INAF [I/009/10/0]; Academy of Finland [212656, 210338]; Ministry of Education and Science of the Russian Federation FX The AGILE Mission is funded by the Italian Space Agency (ASI) with scientific and programmatic participation by the Italian Institute of Astrophysics (INAF) and the Italian Institute of Nuclear Physics (INFN). Research partially supported through the ASI grants no. I/089/06/2 and I/042/10/0. We acknowledge financial contribution from the agreement ASI-INAF I/009/10/0. The Metsahovi team acknowledges the support from the Academy of Finland for our observing projects (numbers 212656, 210338, and others). The RATAN-600 observations were carried out with the financial support of the Ministry of Education and Science of the Russian Federation. NR 53 TC 11 Z9 11 U1 1 U2 9 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD FEB PY 2012 VL 538 AR A63 DI 10.1051/0004-6361/201016129 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 897AX UT WOS:000300614100063 ER PT J AU Combes, F Rex, M Rawle, TD Egami, E Boone, F Smail, I Richard, J Ivison, RJ Gurwell, M Casey, CM Omont, A Alba, AB Dessauges-Zavadsky, M Edge, AC Fazio, GG Kneib, JP Okabe, N Pello, R Perez-Gonzalez, PG Schaerer, D Smith, GP Swinbank, AM van der Werf, P AF Combes, F. Rex, M. Rawle, T. D. Egami, E. Boone, F. Smail, I. Richard, J. Ivison, R. J. Gurwell, M. Casey, C. M. Omont, A. Alba, A. Berciano Dessauges-Zavadsky, M. Edge, A. C. Fazio, G. G. Kneib, J. -P. Okabe, N. Pello, R. Perez-Gonzalez, P. G. Schaerer, D. Smith, G. P. Swinbank, A. M. van der Werf, P. TI A bright z=5.2 lensed submillimeter galaxy in the field of Abell 773 HLSJ091828.6+514223 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE galaxies: evolution; galaxies: high-redshift; galaxies: ISM; infrared: galaxies; submillimeter: galaxies; galaxies: individual: HLSJ091828.6+514223 ID STAR-FORMATION HISTORY; ULTRALUMINOUS INFRARED GALAXIES; MOLECULAR GAS; HERSCHEL-ATLAS; APM 08279+5255; MARKARIAN 231; WATER-VAPOR; INTERSTELLAR-MEDIUM; MASSIVE GALAXY; DARK-MATTER AB During our Herschel Lensing Survey (HLS) of massive galaxy clusters, we have discovered an exceptionally bright source behind the z = 0.22 cluster Abell 773, which appears to be a strongly lensed submillimeter galaxy (SMG) at z = 5.2429. This source is unusual compared to most other lensed sources discovered by Herschel so far, because of its higher submm flux (similar to 200 mJy at 500 mu m) and its high redshift. The dominant lens is a foreground z = 0.63 galaxy, not the cluster itself. The source has a far-infrared ( FIR) luminosity of L-FIR = 1.1 x 10(14)/mu L-circle dot, where mu is the magnification factor, likely similar to 11. We report here the redshift identification through CO lines with the IRAM-30 m, and the analysis of the gas excitation, based on CO(7-6), CO(6-5), CO(5-4) detected at IRAM and the CO(2-1) at the EVLA. All lines decompose into a wide and strong red component, and a narrower and weaker blue component, 540 km s(-1) apart. Assuming the ultraluminous galaxy (ULIRG) CO-to-H-2 conversion ratio, the H-2 mass is 5.8 x 1011/mu M-circle dot, of which one third is in a cool component. From the CI(P-3(2)-P-3(1)) line we derive a CI/H-2 number abundance of 6 x 10(-5) similar to that in other ULIRGs. The H2Op( 2, 0, 2-1, 1, 1) line is strong only in the red velocity component, with an intensity ratio I(H2O)/I( CO) similar to 0.5, suggesting a strong local FIR radiation field, possibly from an active nucleus (AGN) component. We detect the [NII]205 mu m line for the first time at high-z. It shows comparable blue and red components, with a strikingly broad blue one, suggesting strong ionized gas flows. C1 [Combes, F.] CNRS, LERMA, Observ Paris, F-75014 Paris, France. [Rex, M.; Rawle, T. D.; Egami, E.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Boone, F.; Pello, R.; Schaerer, D.] Univ Toulouse, UPS OMP, CNRS, IRAP, F-31028 Toulouse 4, France. [Smail, I.; Edge, A. C.; Swinbank, A. M.] Univ Durham, Inst Computat Cosmol, Durham DH1 3LE, England. [Richard, J.] Univ Lyon 1, CRAL, F-69561 St Genis Laval, France. [Ivison, R. J.] Royal Observ, UK Astron Technol Ctr, Edinburgh EH9 3HJ, Midlothian, Scotland. [Gurwell, M.; Fazio, G. G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Casey, C. M.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Omont, A.] UPMC, Inst Astrophys Paris, F-75014 Paris, France. [Omont, A.] CNRS, F-75014 Paris, France. [Alba, A. Berciano] ASTRON, NL-2990 AA Dwingeloo, Netherlands. [Dessauges-Zavadsky, M.; Schaerer, D.] Univ Geneva, Observ Geneva, CH-1290 Versoix, Switzerland. [Kneib, J. -P.] Univ Aix Marseille, CNRS, LAM, F-13388 Marseille 13, France. [Okabe, N.] ASIAA, Taipei 10617, Taiwan. [Perez-Gonzalez, P. G.] Univ Complutense Madrid, Fac CC Fis, Dep Astrofis, E-28040 Madrid, Spain. [Smith, G. P.] Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England. [van der Werf, P.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. RP Combes, F (reprint author), CNRS, LERMA, Observ Paris, 61 Av Observ, F-75014 Paris, France. EM francoise.combes@obspm.fr RI Pello, Roser/G-4754-2010; Smail, Ian/M-5161-2013; Kneib, Jean-Paul/A-7919-2015; Perez-Gonzalez, Pablo/J-2871-2016; Ivison, R./G-4450-2011; OI Smail, Ian/0000-0003-3037-257X; Kneib, Jean-Paul/0000-0002-4616-4989; Perez-Gonzalez, Pablo/0000-0003-4528-5639; Ivison, R./0000-0001-5118-1313; Edge, Alastair/0000-0002-3398-6916; Casey, Caitlin/0000-0002-0930-6466; Combes, Francoise/0000-0003-2658-7893 FU INSU/CNRS (France); MPG (Germany); IGN (Spain); NASA; Smithsonian Institution; Academia Sinica; JPL/Caltech FX IRAM is supported by INSU/CNRS (France), MPG (Germany) and IGN (Spain). Herschel is an ESA space observatory with instruments provided by European-led PI consortia and with important participation from NASA. Support for this work was provided in part by NASA through an award issued by JPL/Caltech. The SMA is a joint project between the Smithsonian Astrophysical Observatory and the Academia Sinica Institute of Astronomy and Astrophysics and is funded by the Smithsonian Institution and the Academia Sinica. NRAO is operated by Associated Universities Inc., under a cooperative agreement with the National Science Foundation. The Keck observatory, made possible thanks to the generous support of W. M. Keck Foundation, is operated by Caltech, the University of California, and NASA. NR 57 TC 69 Z9 69 U1 0 U2 4 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD FEB PY 2012 VL 538 AR L4 DI 10.1051/0004-6361/201118750 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 897AX UT WOS:000300614100157 ER PT J AU Postigo, AD Lundgren, A Martin, S Garcia-Appadoo, D Monsalvo, IDG Peck, A Michalowski, MJ Thone, CC Campana, S Gorosabel, J Tanvir, NR Wiersema, K Castro-Tirado, AJ Schulze, S De Breuck, C Petitpas, G Hjorth, J Jakobsson, P Covino, S Fynbo, JPU Winters, JM Bremer, M Levan, AJ Llorente, A Sanchez-Ramirez, R Tello, JC Salvaterra, R AF de Ugarte Postigo, A. Lundgren, A. Martin, S. Garcia-Appadoo, D. de Gregorio Monsalvo, I. Peck, A. Michalowski, M. J. Thoene, C. C. Campana, S. Gorosabel, J. Tanvir, N. R. Wiersema, K. Castro-Tirado, A. J. Schulze, S. De Breuck, C. Petitpas, G. Hjorth, J. Jakobsson, P. Covino, S. Fynbo, J. P. U. Winters, J. M. Bremer, M. Levan, A. J. Llorente, A. Sanchez-Ramirez, R. Tello, J. C. Salvaterra, R. TI Pre-ALMA observations of GRBs in the mm/submm range SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE gamma-ray burst: general; submillimeter: general ID GAMMA-RAY BURST; SCUBA SUBMILLIMETER OBSERVATIONS; NOBEYAMA MILLIMETER ARRAY; AFTERGLOW LIGHT CURVES; STAR-FORMATION RATES; 28 FEBRUARY 1997; HOST GALAXY; ENERGY INJECTION; HIGH-REDSHIFT; RADIO AFTERGLOW AB Context. Gamma-ray bursts (GRBs) generate an afterglow emission that can be detected from radio to X-rays during days, or even weeks after the initial explosion. The peak of this emission crosses the millimeter and submillimeter range during the first hours to days, making their study in this range crucial for constraining the models. Observations have been limited until now due to the low sensitivity of the observatories in this range. This situation will be greatly improved with the start of scientific operations of the Atacama Large Millimeter/submillimeter Array (ALMA). Aims. In this work we do a statistical analysis of the complete sample of mm/submm observations of GRB afterglows obtained before the beginning of scientific operations at ALMA. Methods. We present observations of 11 GRB afterglows obtained from the Atacama Pathfinder Experiment (APEX) and the SubMillimeter Array (SMA), as well as the first detection of a GRB with ALMA, still in the commissioning phase, and put them into context with a catalogue of all the observations that have been published until now in the spectral range that is covered by ALMA. Results. The catalogue of mm/submm observations collected here is the largest to date and is composed of 102 GRBs, of which 88 have afterglow observations, whereas the rest are host galaxy searches. With our programmes, we contributed with data of 11 GRBs and the discovery of 2 submm counterparts. In total, the full sample, including data from the literature, has 22 afterglow detections with redshifts ranging from 0.168 to 8.2. GRBs have been detected in mm/submm wavelengths with peak luminosities spanning 2.5 orders of magnitude, the most luminous reaching 10(33) erg s(-1) Hz(-1). We observe a correlation between the X-ray brightness at 0.5 days and the mm/submm peak brightness. Finally we give a rough estimate of the distribution of peak flux densities of GRB afterglows, based on the current mm/submm sample. Conclusions. Observations in the mm/submm bands have been shown to be crucial for our understanding of the physics of GRBs, but have until now been limited by the sensitivity of the observatories. With the start of the operations at ALMA, the sensitivity has improved by more than an order of magnitude, opening a new era in the study of GRB afterglows and their host galaxies. Our estimates predict that, once completed, ALMA will detect up to similar to 98% of the afterglows if observed during the passage of the peak synchrotron emission. C1 [de Ugarte Postigo, A.; Hjorth, J.; Fynbo, J. P. U.] Niels Bohr Inst, Dark Cosmol Ctr, DK-2100 Copenhagen O, Denmark. [de Ugarte Postigo, A.; Thoene, C. C.; Gorosabel, J.; Castro-Tirado, A. J.; Sanchez-Ramirez, R.; Tello, J. C.] Inst Astrofis Andalucia IAA CSIC, Granada 18008, Spain. [Lundgren, A.; Martin, S.; Garcia-Appadoo, D.; de Gregorio Monsalvo, I.] European So Observ, Santiago 19, Chile. [Lundgren, A.; Garcia-Appadoo, D.; de Gregorio Monsalvo, I.; Peck, A.] Joint ALMA Observ, Vitacura Santiago, Chile. [Michalowski, M. J.] Univ Edinburgh, Royal Observ, Inst Astron, Scottish Univ Phys Alliance, Edinburgh EH9 3HJ, Midlothian, Scotland. [Campana, S.; Covino, S.] INAF Osservatorio Astron Brera, I-23807 Merate, LC, Italy. [Tanvir, N. R.; Wiersema, K.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. [Schulze, S.; Jakobsson, P.] Univ Iceland, Inst Sci, Ctr Astrophys & Cosmol, IS-107 Reykjavik, Iceland. [De Breuck, C.] European So Observ, D-85748 Garching, Germany. [Petitpas, G.] Harvard Smithsonian Ctr Astrophys, Hilo, HI 96720 USA. [Winters, J. M.; Bremer, M.] Inst Radioastron Millimetr IRAM, F-38406 St Martin Dheres, France. [Levan, A. J.] Univ Warwick, Dept Phys, Coventry CV4 7AL, W Midlands, England. [Llorente, A.] ESAC, INSA, Herschel Sci Operat Ctr, Madrid 28080, Spain. [Salvaterra, R.] INAF IASF Milano, I-20133 Milan, Italy. RP Postigo, AD (reprint author), Niels Bohr Inst, Dark Cosmol Ctr, Juliane Maries Vej 30, DK-2100 Copenhagen O, Denmark. EM adeugartepostigo@gmail.com RI Hjorth, Jens/M-5787-2014; Jakobsson, Pall/L-9950-2015; OI de Ugarte Postigo, Antonio/0000-0001-7717-5085; Covino, Stefano/0000-0001-9078-5507; Sanchez-Ramirez, Ruben/0000-0002-7158-5099; Hjorth, Jens/0000-0002-4571-2306; Jakobsson, Pall/0000-0002-9404-5650; Castro-Tirado, A. J./0000-0003-2999-3563; Campana, Sergio/0000-0001-6278-1576; Thone, Christina/0000-0002-7978-7648; De Breuck, Carlos/0000-0002-6637-3315; Schulze, Steve/0000-0001-6797-1889; Salvaterra, Ruben/0000-0002-9393-8078 FU Danish National Research Foundation; ESO in Chile; ALMA commissioning team; INSU/CNRS (France); MPG (Germany); IGN (Spain); Spanish Ministry of Science and Innovation [AYA20082008-03467/ESP, AYA2009-14000-C03-01]; Icelandic Research Fund; [082.F-9850]; [084.D-0732]; [086.D-0590]; [086.F-9303]; [087.F-9301]; [2009B-S015]; [2010A-S004]; [2010B-S026] FX This publication is partially based on data acquired with the Atacama Pathfinder Experiment (APEX) under programmes 082.F-9850, 084.D-0732, 086.D-0590, 086.F-9303(A) and 087.F-9301(A) and with the Submillimeter Array (SMA) under programmes 2009B-S015, 2010A-S004 and 2010B-S026. This paper makes use of the following ALMA Science Verification data: ADS/JAO.ALMA#2011.0.00006.SV.; A.d.U.P. acknowledges support from ESO's Scientific Visitor Programme in Chile, where a significant part of this work was done. The Dark Cosmology Centre is funded by the Danish National Research Foundation. The Atacama Large Millimeter/submillimeter Array (ALMA), an international astronomy facility, is a partnership of Europe, North America and East Asia in cooperation with the Republic of Chile. This paper makes use of the following ALMA Science Verification data: ADS/JAO.ALMA#2011.0.00006.SV. We are grateful for the support from the ALMA commissioning team. APEX is a collaboration between the Max-Planck-Institut fur Radioastronomie, the European Southern Observatory, and the Onsala Space Observatory. The Submillimeter Array is a joint project between the Smithsonian Astrophysical Observatory and the Academia Sinica Institute of Astronomy and Astrophysics and is funded by the Smithsonian Institution and the Academia Sinica. This paper made use of observations carried out with the IRAM Plateau de Bure Interferometer. IRAM is supported by INSU/CNRS (France), MPG (Germany) and IGN (Spain). This work made use of data supplied by the UK Swift Science Data Centre at the University of Leicester. We acknowledge partial support from the Spanish Ministry of Science and Innovation through programmes AYA20082008-03467/ESP and AYA2009-14000-C03-01. S. S. acknowledges support by a Grant of Excellence from the Icelandic Research Fund. NR 205 TC 23 Z9 23 U1 0 U2 6 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD FEB PY 2012 VL 538 AR A44 DI 10.1051/0004-6361/201117848 PG 23 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 897AX UT WOS:000300614100044 ER PT J AU Giroletti, M Hada, K Giovannini, G Casadio, C Beilicke, M Cesarini, A Cheung, CC Doi, A Krawczynski, H Kino, M Lee, NP Nagai, H AF Giroletti, M. Hada, K. Giovannini, G. Casadio, C. Beilicke, M. Cesarini, A. Cheung, C. C. Doi, A. Krawczynski, H. Kino, M. Lee, N. P. Nagai, H. TI The kinematic of HST-1 in the jet of M 87 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE galaxies: jets; radio continuum: galaxies; galaxies: nuclei ID RADIO GALAXY M87; GAMMA-RAY EMISSION; CENTRAL BLACK-HOLE; VARIABILITY; KNOT; SITE AB Aims. We aim to constrain the structural variations within the HST-1 region downstream of the radio jet of M 87, in general as well as in connection to the episodes of activity at very high energy (VHE). Methods. We analyzed and compared 26 VLBI observations of the M 87 jet, obtained between 2006 and 2011 with the Very Long Baseline Array (VLBA) at 1.7 GHz and the European VLBI Network (EVN) at 5 GHz. Results. HST-1 is detected at all epochs; we model-fitted its complex structure with two or more components, the two outermost of which display a significant proper motion with a superluminal velocity around similar to 4c. The motion of a third feature that is detected upstream is more difficult to characterize. The overall position angle of HST-1 has changed during the time of our observations from -65 degrees to -90 degrees, while the structure has moved by over 80 mas downstream. Our results on the component evolution suggest that structural changes at the upstream edge of HST-1 can be related to the VHE events. C1 [Giroletti, M.; Giovannini, G.] INAF Ist Radioastron, I-40129 Bologna, Italy. [Hada, K.] Grad Univ Adv Studies SOKENDAI, Mitaka, Tokyo 1818588, Japan. [Hada, K.; Kino, M.; Nagai, H.] Natl Inst Nat Sci, Natl Astron Observ Japan, Mitaka, Tokyo 1818588, Japan. [Giovannini, G.] Dipartimento Astron, I-40127 Bologna, Italy. [Casadio, C.] CSIC, Inst Astrofis Andalucia, E-18080 Granada, Spain. [Beilicke, M.; Krawczynski, H.] Washington Univ, Dept Phys, St Louis, MO 63130 USA. [Cesarini, A.] Natl Univ Ireland, Sch Phys, Galway, Ireland. [Cheung, C. C.] Natl Acad Sci, Natl Res Council, Washington, DC 20001 USA. [Cheung, C. C.] USN, Res Lab, Washington, DC 20375 USA. [Doi, A.] JAXA, Inst Space & Astronaut Sci, Sagamihara, Kanagawa 2298510, Japan. [Lee, N. P.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Giroletti, M (reprint author), INAF Ist Radioastron, Via Gobetti 101, I-40129 Bologna, Italy. EM giroletti@ira.inaf.it OI Cesarini, Andrea/0000-0002-8611-8610; Giovannini, Gabriele/0000-0003-4916-6362; Giroletti, Marcello/0000-0002-8657-8852 FU European Union [RI-261525]; national research councils FX We thank D. E. Harris for reading the manuscript. We acknowledge a contribution from the Italian Foreign Affair Minister under the bilateral scientific collaboration between Italy and Japan. e-VLBI research infrastructure in Europe is supported by the European Union's Seventh Framework Programme (FP7/2007-2013) under grant agreement no. RI-261525 NEXPReS. The European VLBI Network is a joint facility of European, Chinese, South African and other radio astronomy institutes funded by their national research councils. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by AUI. NR 25 TC 21 Z9 21 U1 0 U2 1 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD FEB PY 2012 VL 538 AR L10 DI 10.1051/0004-6361/201218794 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 897AX UT WOS:000300614100163 ER PT J AU Hwang, HS Park, C Elbaz, D Choi, YY AF Hwang, H. S. Park, C. Elbaz, D. Choi, Y. -Y. TI Activity in galactic nuclei of cluster and field galaxies in the local universe SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE galaxies: active; galaxies: clusters: general; galaxies: evolution; galaxies: formation; galaxies: general; galaxies: interactions ID DIGITAL SKY SURVEY; SUPERMASSIVE BLACK-HOLES; EMISSION-LINE GALAXIES; ULTRALUMINOUS INFRARED GALAXIES; LARGE-SCALE ENVIRONMENT; STAR-FORMING GALAXIES; MERGER-AGN CONNECTION; SIMILAR-TO 1; SEYFERT-GALAXIES; X-RAY AB Aims. We study the environmental effects on the activity in galactic nuclei by comparing galaxies in clusters and in the field. Methods. Using a spectroscopic sample of galaxies in Abell clusters from the Sloan Digital Sky Survey Data Release 7, we investigate the dependence of nuclear activity on the physical parameters of clusters as well as the nearest neighbor galaxy. We also compare galaxy properties between active galactic nuclei (AGNs) hosts and non-AGN galaxies. Results. We find that the AGN fraction of early-type galaxies starts to decrease around one virial radius of clusters (r(200,cl)) as decreasing clustercentric radius, while that of late types starts to decrease close to the cluster center (R similar to 0.1-0.5r(200,cl)). The AGN fractions of early-type cluster galaxies, on average, are found to be lower than those of early-type field galaxies by a factor similar to 3. However, the mean AGN fractions of late-type cluster galaxies are similar to those of late-type field galaxies. The AGN fraction of early-type brightest cluster galaxies lies between those of other early-type, cluster and field galaxies with similar luminosities. In the field, the AGN fraction is strongly dependent on the morphology of and the distance to the nearest neighbor galaxy. We find an anti-correlation between the AGN fraction and the velocity dispersion of clusters for all subsamples divided by morphology and luminosity of host galaxies. The AGN power indicated by L-[OIII]/M-BH is found to depend strongly on the mass of host galaxies rather than the clustercentric radius. The difference in physical parameters such as luminosity, (u-r) colors, star formation rates, and (g-i) color gradients between AGN hosts and non-AGN galaxies is seen for both early and late types at all clustercentric radii, while the difference in structure parameters between the two is significant only for late types. Conclusions. These results support the idea that the activity in galactic nuclei is triggered through galaxy-galaxy interactions and mergers when gas supply for AGN is available. C1 [Hwang, H. S.; Elbaz, D.] CEA Saclay, Serv Astrophys, F-91191 Gif Sur Yvette, France. [Hwang, H. S.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. [Park, C.] Korea Inst Adv Study, Sch Phys, Seoul 130722, South Korea. [Choi, Y. -Y.] Kyung Hee Univ, Dept Astron & Space Sci, Gyeonggi 446701, South Korea. RP Hwang, HS (reprint author), CEA Saclay, Serv Astrophys, F-91191 Gif Sur Yvette, France. EM hhwang@cfa.harvard.edu; cbp@kias.re.kr; delbaz@cea.fr; yy.choi@khu.ac.kr FU Centre National d'Etudes Spatiales (CNES); Smithsonian Institution; Alfred P. Sloan Foundation; National Science Foundation; US Department of Energy; National Aeronautics and Space Administration; Japanese Monbukagakusho; Max Planck Society; Higher Education Funding Council for England FX We would like to thank the anonymous referee for constructive comments that helped improving the paper, and R. Gobat, J. Mullaney, and G.-H. Lee for useful discussion. H.S.H. acknowledges the Centre National d'Etudes Spatiales (CNES) and the Smithsonian Institution for the support of his post-doctoral fellowship. D.E. acknowledges the support of the Centre National d'Etudes Spatiales (CNES). Funding for the SDSS and SDSS-II has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, the US Department of Energy, the National Aeronautics and Space Administration, the Japanese Monbukagakusho, the Max Planck Society, and the Higher Education Funding Council for England. The SDSS Web Site is http://www.sdss.org/. The SDSS is managed by the Astrophysical Research Consortium for the Participating Institutions. The Participating Institutions are the American Museum of Natural History, Astrophysical Institute Potsdam, University of Basel, Cambridge University, Case Western Reserve University, University of Chicago, Drexel University, Fermilab, the Institute for Advanced Study, the Japan Participation Group, Johns Hopkins University, the Joint Institute for Nuclear Astrophysics, the Kavli Institute for Particle Astrophysics and Cosmology, the Korean Scientist Group, the Chinese Academy of Sciences (LAMOST), Los Alamos National Laboratory, the Max-Planck-Institute for Astronomy (MPIA), the Max-Planck-Institute for Astrophysics (MPA), New Mexico State University, Ohio State University, University of Pittsburgh, University of Portsmouth, Princeton University, the United States Naval Observatory, and the University of Washington. This research has made use of the NASA/IPAC Extragalactic Database (NED) which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. NR 149 TC 17 Z9 17 U1 1 U2 1 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD FEB PY 2012 VL 538 AR A15 DI 10.1051/0004-6361/201117351 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 897AX UT WOS:000300614100015 ER PT J AU Landi, E Reale, F Testa, P AF Landi, E. Reale, F. Testa, P. TI Monte Carlo Markov chain DEM reconstruction of isothermal plasmas SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE methods: data analysis; techniques: spectroscopic; Sun: corona; Sun: UV radiation ID POLAR CORONAL HOLE; EUV IMAGING SPECTROMETER; EMISSION-LINES; ATOMIC DATABASE; THERMAL STRUCTURE; RATE COEFFICIENTS; QUIET-SUN; SOLAR; SPECTRA; CHIANTI AB Context. Recent studies carried out with SOHO and Hinode high-resolution spectrometers have shown that the plasma in the off-disk solar corona is close to isothermal. If confirmed, these findings may have significant consequences for theoretical models of coronal heating. However, these studies have been carried out with diagnostic techniques whose ability to reconstruct the plasma distribution with temperature has not been thoroughly tested. Aims. In this paper, we carry out tests on the Monte Carlo Markov chain (MCMC) technique with the aim of determining: 1) its ability to retrieve isothermal plasmas from a set of spectral line intensities, with and without random noise; 2) to what extent can it discriminate between an isothermal solution and a narrow multithermal distribution; and 3) how well it can detect multiple isothermal components along the line of sight. We also test the effects of 4) atomic data uncertainties on the results, and 5) the number of ions whose lines are available for the DEM reconstruction. Methods. We first use the CHIANTI database to calculate synthetic spectra from different thermal distributions: single isothermal plasmas, multithermal plasmas made of multiple isothermal components, and multithermal plasmas with a Gaussian DEM distribution with variable width. We then apply the MCMC technique on each of these synthetic spectra, so that the ability of the MCMC technique at reconstructing the original thermal distribution can be evaluated. Next, we add a random noise to the synthetic spectra, and repeat the exercise, in order to determine the effects of random errors on the results. We also we repeat the exercise using a different set of atomic data from those used to calculate synthetic line intensities, to understand the robustness of the results against atomic physics uncertainties. The size of the temperature bin of the MCMC reconstruction is varied in all cases, in order to determine the optimal width. Results. We find that the MCMC technique is unable to retrieve isothermal plasmas to better than Delta log T similar or equal to 0.05. Also, the DEM curves obtained using lines calculated with an isothermal plasma and with a Gaussian distribution with FWHM of log T similar or equal to 0.05 are very similar. Two near-isothermal components can be resolved if their temperature separation is. log T = 0.2 or larger. Thus, DEM diagnostics has an intrinsic resolving power of log T = 0.05. Atomic data uncertainties may significantly affect both temperature and peak DEM values, but do not alter our conclusions. The availability of small sets of lines also does not worsen the performance of the MCMC technique, provided these lines are formed in a wide temperature range. Conclusions. Our analysis shows the present limitations in our ability to identify the presence of strictly isothermal plasmas in stellar and solar coronal spectra. C1 [Landi, E.] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA. [Reale, F.] Univ Palermo, Dipartimento Sci Fis & Astron, Sez Astron, I-90134 Palermo, Italy. [Reale, F.] INAF Osservatorio Astron Palermo, I-90134 Palermo, Italy. [Testa, P.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Landi, E (reprint author), Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA. EM elandi@umich.edu RI Landi, Enrico/H-4493-2011; OI Reale, Fabio/0000-0002-1820-4824 FU NASA [NNX10AM17G, NNX11AC20G, NNM07AB07C]; Italian Ministero dell'Universita e Ricerca; Agenzia Spaziale Italiana (ASI) [I/015/07/0] FX The work of Enrico Landi is supported by NASA grants NNX10AM17G and NNX11AC20G. Fabio Reale acknowledges support from Italian Ministero dell'Universita e Ricerca and from Agenzia Spaziale Italiana (ASI), contract I/015/07/0. Paola Testa was supported by NASA contract NNM07AB07C to the Smithsonian Astrophysical Observatory. We thank the referee for valuable comments that helped us improve the manuscript. NR 31 TC 8 Z9 8 U1 0 U2 2 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD FEB PY 2012 VL 538 AR A111 DI 10.1051/0004-6361/201117424 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 897AX UT WOS:000300614100111 ER PT J AU Turner, SC AF Turner, Steven C. TI Changing Images of the Inclined Plane: A Case Study of a Revolution in American Science Education SO SCIENCE & EDUCATION LA English DT Article AB Between 1880 and 1920 the way science was taught in American High Schools changed dramatically. The old "lecture/demonstration" method, where information was presented to essentially passive students, was replaced by the "laboratory" method, where students performed their own experiments in specially constructed student laboratories. National leadership in education was generally weak during this period, and the new method required significant investments by the schools, but within a few decades American science education was rapidly and completely transformed. Previous studies of this fundamental change have concentrated on the activities of organizations like the NEA, the Bureau of Education and a few major universities, but the way in which these groups were able to effect actual changes in classroom practice is not completely clear. This article attempts to broaden the existing narrative by integrating the rich and largely ignored material culture of science education-such things as textbooks, lab manuals, student notebooks, science teaching instruments and scientific instrument catalogs. Surprisingly, much of this story can be seen in changes to the depiction of a single, venerable and otherwise unremarkable teaching instrument: the inclined plane. C1 Smithsonian Inst, Natl Museum Amer Hist, Washington, DC 20560 USA. RP Turner, SC (reprint author), Smithsonian Inst, Natl Museum Amer Hist, Washington, DC 20560 USA. EM turners@si.edu NR 84 TC 3 Z9 3 U1 2 U2 5 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0926-7220 J9 SCI EDUC-NETHERLANDS JI Sci. Educ. PD FEB PY 2012 VL 21 IS 2 SI SI BP 245 EP 270 DI 10.1007/s11191-010-9322-3 PG 26 WC Education & Educational Research; History & Philosophy Of Science SC Education & Educational Research; History & Philosophy of Science GA 898XW UT WOS:000300776700006 ER PT J AU Yamaguchi, H Ozawa, M Ohnishi, T AF Yamaguchi, Hiroya Ozawa, Midori Ohnishi, Takao TI New insights into SNR evolution revealed by the discovery of recombining plasmas SO ADVANCES IN SPACE RESEARCH LA English DT Article DE ISM: individual (IC 443, W49B, G359.1-0.5); Radiation mechanisms: thermal; Supernova remnants; X-rays: ISM ID X-RAY-EMISSION; SUPERNOVA REMNANT IC-443; XMM-NEWTON OBSERVATIONS; INTERSTELLAR-MEDIUM; OVERIONIZED PLASMA; METAL ABUNDANCES; IC 443; ASCA; W49B; SUZAKU AB We report the discovery of recombining plasmas in three supernova remnants (SNRs) with the Suzaku X-ray astronomy satellite. During SNR's evolution, the expanding supernova ejecta and the ambient matter are compressed and heated by the reverse and forward shocks to form an X-ray emitting hot plasma. Since ionization proceeds slowly compared to shock heating, most young or middle-aged SNRs have ionizing (underionized) plasmas. Owing to high sensitivity of Suzaku, however, we have detected radiative recombination continua (RRCs) from the SNRs IC 443, W49B, and G359.1-0.5. The presence of the strong RRC is the definitive evidence that the plasma is recombining (overionized). As a possible origin of the overionization, an interaction between the ejecta and dense circumstellar matter is proposed; the highly ionized gas was made at the initial phase of the SNR evolution in dense regions, and subsequent rapid adiabatic expansion caused sudden cooling of the electrons. The analysis on the full X-ray band spectrum of IC 443, which is newly presented in this paper, provides a consistent picture with this scenario. We also comment on the implications from the fact that all the SNRs having recombining plasmas are correlated with the mixed-morphology class. (C) 2011 COSPAR. Published by Elsevier Ltd. All rights reserved. C1 [Yamaguchi, Hiroya] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Yamaguchi, Hiroya] RIKEN Inst Phys & Chem Res, Saitama 3510198, Japan. [Ozawa, Midori; Ohnishi, Takao] Kyoto Univ, Kyoto 6068502, Japan. RP Yamaguchi, H (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM hyamaguchi@head.cfa.harvard.edu RI XRAY, SUZAKU/A-1808-2009 FU Japan Society for the Promotion of Science (JSPS) FX The authors appreciate a number of constructive suggestions from the anonymous referees. We also thank to Drs. Katsuji Koyama, Kuniaki Masai, Randall K. Smith, Patrick O. Slane, and Jelle Kaastra for helpful discussion. H.Y. is supported by Japan Society for the Promotion of Science (JSPS) Research Fellowship for Research Abroad. NR 43 TC 10 Z9 11 U1 0 U2 1 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 0273-1177 J9 ADV SPACE RES JI Adv. Space Res. PD FEB 1 PY 2012 VL 49 IS 3 BP 451 EP 457 DI 10.1016/j.asr.2011.11.002 PG 7 WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA 892DA UT WOS:000300265700002 ER PT J AU Borucki, WJ Koch, DG Batalha, N Bryson, ST Rowe, J Fressin, F Torres, G Caldwell, DA Christensen-Dalsgaard, J Cochran, WD DeVore, E Gautier, TN Geary, JC Gilliland, R Gould, A Howell, SB Jenkins, JM Latham, DW Lissauer, JJ Marcy, GW Sasselov, D Boss, A Charbonneau, D Ciardi, D Kaltenegger, L Doyle, L Dupree, AK Ford, EB Fortney, J Holman, MJ Steffen, JH Mullally, F Still, M Tarter, J Ballard, S Buchhave, LA Carter, J Christiansen, JL Demory, BO Desert, JM Dressing, C Endl, M Fabrycky, D Fischer, D Haas, MR Henze, C Horch, E Howard, AW Isaacson, H Kjeldsen, H Johnson, JA Klaus, T Kolodziejczak, J Barclay, T Li, J Meibom, S Prsa, A Quinn, SN Quintana, EV Robertson, P Sherry, W Shporer, A Tenenbaum, P Thompson, SE Twicken, JD Van Cleve, J Welsh, WF Basu, S Chaplin, W Miglio, A Kawaler, SD Arentoft, T Stello, D Metcalfe, TS Verner, GA Karoff, C Lundkvist, M Lund, MN Handberg, R Elsworth, Y Hekker, S Huber, D Bedding, TR Rapin, W AF Borucki, William J. Koch, David G. Batalha, Natalie Bryson, Stephen T. Rowe, Jason Fressin, Francois Torres, Guillermo Caldwell, Douglas A. Christensen-Dalsgaard, Jorgen Cochran, William D. DeVore, Edna Gautier, Thomas N., III Geary, John C. Gilliland, Ronald Gould, Alan Howell, Steve B. Jenkins, Jon M. Latham, David W. Lissauer, Jack J. Marcy, Geoffrey W. Sasselov, Dimitar Boss, Alan Charbonneau, David Ciardi, David Kaltenegger, Lisa Doyle, Laurance Dupree, Andrea K. Ford, Eric B. Fortney, Jonathan Holman, Matthew J. Steffen, Jason H. Mullally, Fergal Still, Martin Tarter, Jill Ballard, Sarah Buchhave, Lars A. Carter, Josh Christiansen, Jessie L. Demory, Brice-Olivier Desert, Jean-Michel Dressing, Courtney Endl, Michael Fabrycky, Daniel Fischer, Debra Haas, Michael R. Henze, Christopher Horch, Elliott Howard, Andrew W. Isaacson, Howard Kjeldsen, Hans Johnson, John Asher Klaus, Todd Kolodziejczak, Jeffery Barclay, Thomas Li, Jie Meibom, Soren Prsa, Andrej Quinn, Samuel N. Quintana, Elisa V. Robertson, Paul Sherry, William Shporer, Avi Tenenbaum, Peter Thompson, Susan E. Twicken, Joseph D. Van Cleve, Jeffrey Welsh, William F. Basu, Sarbani Chaplin, William Miglio, Andrea Kawaler, Steven D. Arentoft, Torben Stello, Dennis Metcalfe, Travis S. Verner, Graham A. Karoff, Christoffer Lundkvist, Mia Lund, Mikkel N. Handberg, Rasmus Elsworth, Yvonne Hekker, Saskia Huber, Daniel Bedding, Timothy R. Rapin, William TI Kepler-22b: A 2.4 EARTH-RADIUS PLANET IN THE HABITABLE ZONE OF A SUN-LIKE STAR SO ASTROPHYSICAL JOURNAL LA English DT Article DE planetary systems; stars: fundamental parameters; stars: individual (Kepler-22, KIC 10593626) ID MAIN-SEQUENCE STARS; TRANSIT TIMING VARIATIONS; INITIAL CHARACTERISTICS; TERRESTRIAL PLANETS; ASTEROSEISMIC DATA; FALSE POSITIVES; SPACE-TELESCOPE; BLEND SCENARIOS; MULTIPLE SYSTEM; CADENCE DATA AB A search of the time-series photometry from NASA's Kepler spacecraft reveals a transiting planet candidate orbiting the 11th magnitude G5 dwarf KIC 10593626 with a period of 290 days. The characteristics of the host star are well constrained by high-resolution spectroscopy combined with an asteroseismic analysis of the Kepler photometry, leading to an estimated mass and radius of 0.970 +/- 0.060 M-circle dot and 0.979 +/- 0.020 R-circle dot. The depth of 492 +/- 10 ppm for the three observed transits yields a radius of 2.38 +/- 0.13 Re for the planet. The system passes a battery of tests for false positives, including reconnaissance spectroscopy, high-resolution imaging, and centroid motion. A full BLENDER analysis provides further validation of the planet interpretation by showing that contamination of the target by an eclipsing system would rarely mimic the observed shape of the transits. The final validation of the planet is provided by 16 radial velocities (RVs) obtained with the High Resolution Echelle Spectrometer on Keck I over a one-year span. Although the velocities do not lead to a reliable orbit and mass determination, they are able to constrain the mass to a 3 sigma upper limit of 124 M-circle plus, safely in the regime of planetary masses, thus earning the designation Kepler-22b. The radiative equilibrium temperature is 262 K for a planet in Kepler-22b's orbit. Although there is no evidence that Kepler-22b is a rocky planet, it is the first confirmed planet with a measured radius to orbit in the habitable zone of any star other than the Sun. C1 [Borucki, William J.; Klaus, Todd] NASA, Ames Res Ctr, Orbital Sci Corp, Moffett Field, CA 94035 USA. [Batalha, Natalie] San Jose State Univ, Dept Phys & Astron, San Jose, CA 95192 USA. [Rowe, Jason; Caldwell, Douglas A.; DeVore, Edna; Jenkins, Jon M.; Doyle, Laurance; Mullally, Fergal; Tarter, Jill; Christiansen, Jessie L.; Li, Jie; Quintana, Elisa V.; Tenenbaum, Peter; Thompson, Susan E.; Twicken, Joseph D.; Van Cleve, Jeffrey] SETI Inst, Mountain View, CA 94043 USA. [Fressin, Francois; Torres, Guillermo; Geary, John C.; Latham, David W.; Sasselov, Dimitar; Charbonneau, David; Dupree, Andrea K.; Holman, Matthew J.; Ballard, Sarah; Desert, Jean-Michel; Dressing, Courtney; Meibom, Soren; Quinn, Samuel N.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Christensen-Dalsgaard, Jorgen; Kjeldsen, Hans; Arentoft, Torben; Karoff, Christoffer; Lundkvist, Mia; Lund, Mikkel N.; Handberg, Rasmus] Aarhus Univ, Dept Phys & Astron, DK-8000 Aarhus C, Denmark. [Christensen-Dalsgaard, Jorgen] Natl Ctr Atmospher Res, High Altitude Observ, Boulder, CO 80307 USA. [Cochran, William D.; Endl, Michael; Robertson, Paul] Univ Texas Austin, McDonald Observ, Austin, TX 78712 USA. [Gautier, Thomas N., III; Johnson, John Asher] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Gilliland, Ronald] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Marcy, Geoffrey W.; Howard, Andrew W.; Isaacson, Howard] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Boss, Alan] Carnegie Inst Sci, Dept Terr Magnetism, Washington, DC 20015 USA. [Ciardi, David] CALTECH, Exoplanet Sci Inst, Pasadena, CA 91125 USA. [Kaltenegger, Lisa] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Ford, Eric B.] Univ Florida, Dept Astron, Gainesville, FL 32611 USA. [Fortney, Jonathan; Fabrycky, Daniel] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. [Steffen, Jason H.] Fermilab Natl Accelerator Lab, Batavia, IL 60510 USA. [Still, Martin; Barclay, Thomas] Bay Area Environm Res Inst, Moffett Field, CA 94035 USA. [Buchhave, Lars A.] Univ Copenhagen, Niels Bohr Inst, DK-2100 Copenhagen, Denmark. [Buchhave, Lars A.] Univ Copenhagen, Ctr Star & Planet Format, Nat Hist Museum Denmark, DK-1350 Copenhagen, Denmark. [Carter, Josh; Demory, Brice-Olivier] MIT, Cambridge, MA 02139 USA. [Fischer, Debra; Basu, Sarbani] Yale Univ, Dept Astron, New Haven, CT 06520 USA. [Welsh, William F.] San Diego State Univ, Dept Astron, San Diego, CA 92182 USA. [Horch, Elliott] So Connecticut State Univ, Dept Phys, New Haven, CT 06515 USA. [Kolodziejczak, Jeffery] MSFC, Huntsville, AL 35805 USA. [Prsa, Andrej] Villanova Univ, Dept Astron & Astrophys, Villanova, PA 19085 USA. [Sherry, William] Natl Opt Astron Observ, Tucson, AZ 85719 USA. [Shporer, Avi] Las Cumbres Observ, Goleta, CA 93117 USA. [Chaplin, William; Miglio, Andrea; Verner, Graham A.; Elsworth, Yvonne; Hekker, Saskia] Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England. [Kawaler, Steven D.] Iowa State Univ, Dept Phys & Astron, Ames, IA 50014 USA. [Stello, Dennis; Huber, Daniel; Bedding, Timothy R.] Univ Sydney, Sydney Inst Astron, Sch Phys, Sydney, NSW 2006, Australia. [Metcalfe, Travis S.] White Dwarf Res Corp, Boulder, CO 80301 USA. [Hekker, Saskia] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 XH Amsterdam, Netherlands. [Rapin, William] Ctr Spatial Toulouse, Ctr Natl Etud Spatiales, F-31401 Toulouse, France. RP Borucki, WJ (reprint author), NASA, Ames Res Ctr, Orbital Sci Corp, Moffett Field, CA 94035 USA. EM William.J.Borucki@nasa.gov RI Caldwell, Douglas/L-7911-2014; Howard, Andrew/D-4148-2015; OI Caldwell, Douglas/0000-0003-1963-9616; Howard, Andrew/0000-0001-8638-0320; Fortney, Jonathan/0000-0002-9843-4354; Buchhave, Lars A./0000-0003-1605-5666; Bedding, Timothy/0000-0001-5943-1460; Metcalfe, Travis/0000-0003-4034-0416; Ciardi, David/0000-0002-5741-3047; Karoff, Christoffer/0000-0003-2009-7965; Demory, Brice-Olivier/0000-0002-9355-5165; Basu, Sarbani/0000-0002-6163-3472; /0000-0001-6545-639X; Lund, Mikkel Norup/0000-0001-9214-5642; Fischer, Debra/0000-0003-2221-0861; Handberg, Rasmus/0000-0001-8725-4502; Kawaler, Steven/0000-0002-6536-6367; Fabrycky, Daniel/0000-0003-3750-0183; Lundkvist, Mia Sloth/0000-0002-8661-2571; Bedding, Tim/0000-0001-5222-4661 FU NASA's Science Mission Directorate; W. M. Keck Foundation; NASA; NASA through JPL/Caltech; National Center for Atmospheric Research; National Science Foundation; Netherlands Organisation for Scientific Research (NWO) FX Kepler was competitively selected as the tenth Discovery mission. Funding for this mission is provided by NASA's Science Mission Directorate. Some of the data presented herein were obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California, and the National Aeronautics and Space Administration. The Keck Observatory was made possible by the generous financial support of the W. M. Keck Foundation. Some of the observations were 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. Additional support for this work was also received from National Center for Atmospheric Research which is sponsored by the National Science Foundation. The authors thank the many people who gave so generously of their time to make this Mission a success. S. H. acknowledges financial support from the Netherlands Organisation for Scientific Research (NWO). NR 83 TC 139 Z9 139 U1 13 U2 60 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 1 PY 2012 VL 745 IS 2 AR 120 DI 10.1088/0004-637X/745/2/120 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 893AI UT WOS:000300326800018 ER PT J AU Bourke, TL Myers, PC Caselli, P Di Francesco, J Belloche, A Plume, R Wilner, DJ AF Bourke, Tyler L. Myers, Philip C. Caselli, Paola Di Francesco, James Belloche, Arnaud Plume, Rene Wilner, David J. TI INITIAL CONDITIONS FOR STAR FORMATION IN CLUSTERS: PHYSICAL AND KINEMATICAL STRUCTURE OF THE STARLESS CORE Oph A-N6 SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM: individual objects (Oph A-N6); stars: formation; stars: low-mass ID OPHIUCHI MOLECULAR CLOUD; 1ST HYDROSTATIC CORE; C2D LEGACY CLOUDS; DUST CONTINUUM EMISSION; PRE-STELLAR CORES; DENSE CORES; DARK CLOUDS; PROTOSTELLAR CORES; MASS FUNCTION; SUBMILLIMETER CONTINUUM AB We present high spatial (<300 AU) and spectral (0.07 km s(-1)) resolution Submillimeter Array observations of the dense starless cluster core Oph A-N6 in the 1 mm dust continuum and the 3-2 line of N2H+ and N2D+. The dust continuum observations reveal a compact source not seen in single-dish observations, of size similar to 1000 AU and mass 0.005-0.01 M-circle dot. The combined line and single-dish observations reveal a core of size 3000 x 1400 AU elongated in a NW-SE direction, with almost no variation in either line width nor line center velocity across the map, and very small non-thermal motions. The deuterium fraction has a peak value of similar to 0.15 and is >0.05 over much of the core. The N2H+ column density profile across the major axis of Oph A-N6 is well represented by an isothermal cylinder, with temperature 20 K, peak density 7.1 x 10(6) cm(-3), and N2H+ abundance 2.7 x 10(-10). The mass of Oph A-N6 is estimated to be 0.29 M-circle dot, compared to a value of 0.18 M-circle dot from the isothermal cylinder analysis, and 0.63 M-circle dot for the critical mass for fragmentation of an isothermal cylinder. Compared to isolated low-mass cores, Oph A-N6 shows similar narrow line widths and small velocity variation, with a deuterium fraction similar to "evolved" dense cores. It is significantly smaller than isolated cores, with larger peak column and volume density. The available evidence suggests that Oph A-N6 has formed through the fragmentation of the Oph A filament and is the precursor to a low-mass star. The dust continuum emission suggests that it may already have begun to form a star. C1 [Bourke, Tyler L.; Myers, Philip C.; Wilner, David J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Caselli, Paola] Univ Leeds, Sch Phys & Astron, Leeds LS2 9JT, W Yorkshire, England. [Di Francesco, James] Natl Res Council Canada, Herzberg Inst Astrophys, Victoria, BC, Canada. [Belloche, Arnaud] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Plume, Rene] Univ Calgary, Dept Phys & Astron, Calgary, AB T2N 1N4, Canada. RP Bourke, TL (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM tbourke@cfa.harvard.edu FU National Science Foundation [0708158]; Smithsonian Institution; Academia Sinica; INSU/CNRS (France); MPG (Germany); IGN (Spain) FX This research is supported in part by the National Science Foundation under grant number 0708158 (T. L. B.). We thank Andy Pon and Rachel Friesen for sharing results in advance of publication, and Rachel Friesen and Chris de Vries for checking column density estimates for optically thick N2H+. We thank Mark Gurwell for his diligent maintenance of the "Submillimeter Calibrator List." The Submillimeter Array is a joint project between the Smithsonian Astrophysical Observatory and the Academia Sinica Institute of Astronomy and Astrophysics, and is funded by the Smithsonian Institution and the Academia Sinica. The James Clerk Maxwell Telescope is operated by The Joint Astronomy Centre on behalf of the Science and Technology Facilities Council of the United Kingdom, the Netherlands Organisation for Scientific Research, and the National Research Council of Canada. This work is based on observations carried out with the IRAM 30 m telescope. IRAM is supported by INSU/CNRS (France), MPG (Germany), and IGN (Spain). This research has made use of NASA's Astrophysics Data System Bibliographic Services. NR 128 TC 13 Z9 13 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 FEB 1 PY 2012 VL 745 IS 2 AR 117 DI 10.1088/0004-637X/745/2/117 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 893AI UT WOS:000300326800015 ER PT J AU Hall, N Bradac, M Gonzalez, AH Treu, T Clowe, D Jones, C Stiavelli, M Zaritsky, D Cuby, JG Clement, B AF Hall, Nicholas Bradac, Marusa Gonzalez, Anthony H. Treu, Tommaso Clowe, Douglas Jones, Christine Stiavelli, Massimo Zaritsky, Dennis Cuby, Jean-Gabriel Clement, Benjamin TI USING THE BULLET CLUSTER AS A GRAVITATIONAL TELESCOPE TO STUDY z greater than or similar to 7 LYMAN BREAK GALAXIES SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: high-redshift; gravitational lensing: strong; gravitational lensing: weak ID HUBBLE-SPACE-TELESCOPE; ULTRA DEEP FIELD; LY-ALPHA EMITTERS; ULTRAVIOLET LUMINOSITY DENSITY; HIGH-REDSHIFT GALAXIES; STAR-FORMING GALAXIES; SPECTROSCOPIC CONFIRMATION; LENSING CLUSTERS; COSMIC VARIANCE; LENSED GALAXIES AB We use imaging obtained with the Hubble Space Telescope Wide Field Camera 3 to search for z(850) dropouts at z similar to 7 and J(110) dropouts at z similar to 9 lensed by the Bullet Cluster. In total we find 10 z850 dropouts in our 8.27 arcmin(2) field. Using magnification maps from a combined weak-and strong-lensing mass reconstruction of the Bullet Cluster and correcting for estimated completeness levels, we calculate the surface density and luminosity function of our z850 dropouts as a function of intrinsic (accounting for magnification) magnitude. We find results consistent with published blank field surveys, despite using much shallower data, and demonstrate the effectiveness of cluster surveys in the search for z similar to 7 galaxies. C1 [Hall, Nicholas; Bradac, Marusa] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA. [Gonzalez, Anthony H.] Univ Florida, Dept Astron, Gainesville, FL 32611 USA. [Treu, Tommaso] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA. [Clowe, Douglas] Ohio Univ, Dept Phys & Astron, Clippinger Labs 251B, Athens, OH 45701 USA. [Jones, Christine] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Stiavelli, Massimo] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Zaritsky, Dennis] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Cuby, Jean-Gabriel; Clement, Benjamin] Univ Aix Marseille, Lab Astrophys Marseille, OAMP, F-13388 Marseille 13, France. [Cuby, Jean-Gabriel; Clement, Benjamin] CNRS, F-13388 Marseille 13, France. RP Hall, N (reprint author), Univ Calif Davis, Dept Phys, 1 Shields Ave, Davis, CA 95616 USA. EM nrhall@ucdavis.edu FU NASA from the Space Telescope Science Institute (STScI) [HST-GO-10200, HST-GO-10863, HST-GO-11099]; NASA [NAS 5-26555, NNX08AD79G]; NSF [NSF-0642621]; Sloan Foundation; Packard Foundation FX We thank Rychard Bouwens for helpful discussions as well as providing relevant data for comparison with our results. We also thank Adriano Fontana and Laura Pentericci for valuable discussions. Support for this work was provided by NASA through grant numbers HST-GO-10200, HST-GO-10863, and HST-GO-11099 from the Space Telescope Science Institute (STScI), which is operated by AURA, Inc., under NASA contract NAS 5-26555 and NNX08AD79G. Tommaso Treu acknowledges support from the NSF through CAREER award NSF-0642621, by the Sloan Foundation through a Sloan Research Fellowship, and by the Packard Foundation through a Packard Fellowship. NR 68 TC 23 Z9 23 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 1 PY 2012 VL 745 IS 2 AR 155 DI 10.1088/0004-637X/745/2/155 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 893AI UT WOS:000300326800053 ER PT J AU Kasper, JC Stevens, ML Korreck, KE Maruca, BA Kiefer, KK Schwadron, NA Lepri, ST AF Kasper, J. C. Stevens, M. L. Korreck, K. E. Maruca, B. A. Kiefer, K. K. Schwadron, N. A. Lepri, S. T. TI EVOLUTION OF THE RELATIONSHIPS BETWEEN HELIUM ABUNDANCE, MINOR ION CHARGE STATE, AND SOLAR WIND SPEED OVER THE SOLAR CYCLE SO ASTROPHYSICAL JOURNAL LA English DT Article DE acceleration of particles; interplanetary medium; plasmas; Sun: abundances; Sun: corona; Sun: fundamental parameters ID ADVANCED COMPOSITION EXPLORER; CORONAL ELECTRON-TEMPERATURE; MAGNETIC-FIELDS; SCALING LAW; FLUX; IONIZATION; RECONNECTION; MINIMUM; BALANCE; REGIONS AB The changing relationships between solar wind speed, helium abundance, and minor ion charge state are examined over solar cycle 23. Observations of the abundance of helium relative to hydrogen (A(He) equivalent to 100 x n(He)/n(H)) by the Wind spacecraft are used to examine the dependence of AHe on solar wind speed and solar activity between 1994 and 2010. This work updates an earlier study of AHe from 1994 to 2004 to include the recent extreme solar minimum and broadly confirms our previous result that AHe in slow wind is strongly correlated with sunspot number, reaching its lowest values in each solar minima. During the last minimum, as sunspot numbers reached their lowest levels in recent history, AHe continued to decrease, falling to half the levels observed in slow wind during the previous minimum and, for the first time observed, decreasing even in the fastest solar wind. We have also extended our previous analysis by adding measurements of the mean carbon and oxygen charge states observed with the Advanced Composition Explorer spacecraft since 1998. We find that as solar activity decreased, the mean charge states of oxygen and carbon for solar wind of a given speed also fell, implying that the wind was formed in cooler regions in the corona during the recent solar minimum. The physical processes in the coronal responsible for establishing the mean charge state and speed of the solar wind have evolved with solar activity and time. C1 [Kasper, J. C.; Stevens, M. L.; Korreck, K. E.; Maruca, B. A.; Kiefer, K. K.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Schwadron, N. A.] Univ New Hampshire, Inst Study Earth Oceans & Space, Durham, NH 03824 USA. [Lepri, S. T.] Univ Michigan, Dept Atmospher Ocean & Space Studies, Ann Arbor, MI 48109 USA. RP Kasper, JC (reprint author), Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RI Lepri, Susan/I-8611-2012; Kasper, Justin/D-1152-2010 OI Kasper, Justin/0000-0002-7077-930X FU NASA [NNX09AU35G] FX Analysis of Wind SWE observations is supported by NASA grant NNX09AU35G. We thank the ACE SWICS and SWIMS instrument teams, and the ACE Science Center for providing the ion composition data. The authors also thank S. Cranmer, A. W. Case, A. Zaslavsky, and our anonymous reviewer for very helpful suggestions. NR 42 TC 24 Z9 24 U1 0 U2 14 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD FEB 1 PY 2012 VL 745 IS 2 AR 162 DI 10.1088/0004-637X/745/2/162 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 893AI UT WOS:000300326800060 ER PT J AU Kirk, H Myers, PC AF Kirk, Helen Myers, Philip C. TI VARIATIONS IN THE MASS FUNCTIONS OF CLUSTERED AND ISOLATED YOUNG STELLAR OBJECTS SO ASTROPHYSICAL JOURNAL LA English DT Article DE stars: formation; stars: luminosity function, mass function; stars: statistics ID ORION NEBULA CLUSTER; STAR-FORMING REGION; BROWN DWARFS; O-STARS; EVOLUTIONARY MODELS; SOLAR NEIGHBORHOOD; DISK POPULATION; FIELD STARS; FRAGMENTATION; LUMINOSITY AB We analyze high-quality, complete stellar catalogs for four young (roughly 1 Myr) and nearby (within similar to 300 pc) star-forming regions: Taurus, Lupus3, ChaI, and IC348, which have been previously shown to have stellar groups whose properties are similar to those of larger clusters such as the Orion Nebula Cluster (ONC). We find that stars at higher stellar surface densities within a region or belonging to groups tend to have a relative excess of more massive stars, over a wide range of masses. We find statistically significant evidence for this result in Taurus and IC348 as well as in the ONC. These differences correspond to having typically a similar to 10%-20% higher mean mass in the more clustered environment. Stars in ChaI show no evidence for a trend with either surface density or grouped status, and there are too few stars in Lupus3 to make any definitive interpretation. Models of clustered star formation do not typically extend to sufficiently low masses or small group sizes in order for their predictions to be tested, but our results suggest that this regime is important to consider. C1 [Kirk, Helen; Myers, Philip C.] Harvard Smithsonian Ctr Astrophys, Radio & Geoastron Div, Cambridge, MA 02138 USA. RP Kirk, H (reprint author), Harvard Smithsonian Ctr Astrophys, Radio & Geoastron Div, MS-42, Cambridge, MA 02138 USA. EM hkirk@cfa.harvard.edu NR 44 TC 11 Z9 11 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD FEB 1 PY 2012 VL 745 IS 2 AR 131 DI 10.1088/0004-637X/745/2/131 PG 27 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 893AI UT WOS:000300326800029 ER PT J AU Lada, CJ Forbrich, J Lombardi, M Alves, JF AF Lada, Charles J. Forbrich, Jan Lombardi, Marco Alves, Joao F. TI STAR FORMATION RATES IN MOLECULAR CLOUDS AND THE NATURE OF THE EXTRAGALACTIC SCALING RELATIONS SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: star formation; stars: formation ID FORMATION LAW; MILKY-WAY; NEARBY GALAXIES; GAS TRACERS; STARBURSTS; DISKS AB In this paper, we investigate scaling relations between star formation rates and molecular gas masses for both local Galactic clouds and a sample of external galaxies. We specifically consider relations between the star formation rates and measurements of dense, as well as total, molecular gas masses. We argue that there is a fundamental empirical scaling relation that directly connects the local star formation process with that operating globally within galaxies. Specifically, the total star formation rate in a molecular cloud or galaxy is linearly proportional to the mass of dense gas within the cloud or galaxy. This simple relation, first documented in previous studies, holds over a span of mass covering nearly nine orders of magnitude and indicates that the rate of star formation is directly controlled by the amount of dense molecular gas that can be assembled within a star formation complex. We further show that the star formation rates and total molecular masses, characterizing both local clouds and galaxies, are correlated over similarly large scales of mass and can be described by a family of linear star formation scaling laws, parameterized by f(DG), the fraction of dense gas contained within the clouds or galaxies. That is, the underlying star formation scaling law is always linear for clouds and galaxies with the same dense gas fraction. These considerations provide a single unified framework for understanding the relation between the standard (nonlinear) extragalactic Schmidt-Kennicutt scaling law, that is typically derived from CO observations of the gas, and the linear star formation scaling law derived from HCN observations of the dense gas. C1 [Lada, Charles J.; Forbrich, Jan] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Lombardi, Marco] Univ Milan, Dept Phys, I-20133 Milan, Italy. [Alves, Joao F.] Univ Vienna, Inst Astron, A-1180 Vienna, Austria. RP Lada, CJ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM clada@cfa.harvard.edu; jforbrich@cfa.harvard.edu; marco.lombardi@gmail.com; joao.alves@univie.ac.at OI LOMBARDI, MARCO/0000-0002-3336-4965; Alves, Joao/0000-0002-4355-0921 NR 26 TC 85 Z9 86 U1 1 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 1 PY 2012 VL 745 IS 2 AR 190 DI 10.1088/0004-637X/745/2/190 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 893AI UT WOS:000300326800088 ER PT J AU Mao, SA Gaensler, BM Stanimirovic, S Haverkorn, M McClure-Griffiths, NM Staveley-Smith, L Dickey, JM AF Mao, S. A. Gaensler, B. M. Stanimirovic, S. Haverkorn, M. McClure-Griffiths, N. M. Staveley-Smith, L. Dickey, J. M. TI A RADIO AND OPTICAL POLARIZATION STUDY OF THE MAGNETIC FIELD IN THE SMALL MAGELLANIC CLOUD (vol 688, pg 1029, 2008) SO ASTROPHYSICAL JOURNAL LA English DT Correction C1 [Mao, S. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Gaensler, B. M.] Univ Sydney, Sch Phys, Sydney, NSW 2006, Australia. [Stanimirovic, S.] Univ Wisconsin, Dept Astron, Madison, WI 53706 USA. [Haverkorn, M.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [McClure-Griffiths, N. M.] CSIRO, Australia Telescope Natl Facil, Epping, NSW 1710, Australia. [Staveley-Smith, L.] Univ Western Australia, Sch Phys, Crawley, WA 6009, Australia. [Dickey, J. M.] Univ Tasmania, Dept Phys, Hobart, Tas 7001, Australia. [Gaensler, B. M.] Australian Res Council Federat, Canberra, ACT, Australia. RP Mao, SA (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM samao@cfa.harvard.edu RI Dickey, John/C-6156-2013; Gaensler, Bryan/F-8655-2010 NR 3 TC 1 Z9 1 U1 1 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 1 PY 2012 VL 745 IS 2 AR 199 DI 10.1088/0004-637X/745/2/199 PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 893AI UT WOS:000300326800097 ER PT J AU Munoz, DJ Marrone, DP Moran, JM Rao, R AF Munoz, D. J. Marrone, D. P. Moran, J. M. Rao, R. TI THE CIRCULAR POLARIZATION OF SAGITTARIUS A* AT SUBMILLIMETER WAVELENGTHS SO ASTROPHYSICAL JOURNAL LA English DT Article DE black hole physics; Galaxy: center; plasmas; polarization; submillimeter: general; techniques: interferometric ID ADVECTION-DOMINATED ACCRETION; SUPERMASSIVE BLACK-HOLE; SGR-A; LINEAR-POLARIZATION; GALACTIC-CENTER; SYNCHROTRON SOURCES; X-RAY; FARADAY-ROTATION; STELLAR ORBITS; MILKY-WAY AB We report the first detections of circularly polarized emission at submillimeter wavelengths from the compact radio source and supermassive black hole candidate Sgr A* at a level of 1.2% +/- 0.3% at 1.3 mm wavelength (230 GHz) and 1.6% +/- 0.3% at 860 mu m (345 GHz) with the same handedness, left circular polarization (LCP), as observed at all lower frequencies (1.4-15 GHz). The observations, taken with the Submillimeter Array in multiple epochs, also show simultaneous linear polarization (LP) at both wavelengths of about 6%. These properties differ sharply from those at wavelengths longer than 1 cm (frequencies below 30 GHz), where weak circular polarization (CP) (similar to 0.5%) dominates over LP, which is not detected at similar fractional limits. We describe an extensive set of tests to ensure the accuracy of our measurements. We find no CP in any other source, including the bright quasar 1924-292, which traces the same path on the sky as Sgr A* and therefore should be subject to identical systematic errors originating in the instrument frame. Since a relativistic synchrotron plasma is expected to produce little CP, the observed CP is probably generated close to the event horizon by the Faraday conversion process. We use a simple approximation to show that the phase shift associated with Faraday conversion can be nearly independent of frequency, a sufficient condition to make the handedness of CP independent of frequency. Because the size of the tau = 1 surface changes by more than an order of magnitude between 1.4 and 345 GHz, the magnetic field must be coherent over such scales to consistently produce LCP. To improve our understanding of the environment of SgrA* critical future measurements includes determining whether the Faraday rotation deviates from a lambda(2) dependence in wavelength and whether the circular and linear components of the flux density are correlated. C1 [Munoz, D. J.; Moran, J. M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Marrone, D. P.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Marrone, D. P.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Rao, R.] Acad Sinica, Inst Astron & Astrophys, Hilo, HI 96720 USA. RP Munoz, DJ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM dmunoz@cfa.harvard.edu OI Marrone, Daniel/0000-0002-2367-1080; Moran, James/0000-0002-3882-4414 FU NASA [HST-HF-51259.01, NAS 5-26555]; Space Telescope Science Institute FX We thank Avery Broderick, Siming Liu, and Roman Shcherbakov for helpful comments and discussions. Support for D.P.M. was provided by NASA through Hubble Fellowship grant HST-HF-51259.01 awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., for NASA, under contract NAS 5-26555. NR 75 TC 12 Z9 11 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 FEB 1 PY 2012 VL 745 IS 2 AR 115 DI 10.1088/0004-637X/745/2/115 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 893AI UT WOS:000300326800013 ER PT J AU Sanna, A Reid, MJ Carrasco-Gonzalez, C Menten, KM Brunthaler, A Moscadelli, L Rygl, KLJ AF Sanna, A. Reid, M. J. Carrasco-Gonzalez, C. Menten, K. M. Brunthaler, A. Moscadelli, L. Rygl, K. L. J. TI CLUSTERED STAR FORMATION AND OUTFLOWS IN AFGL 2591 SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM: kinematics and dynamics; masers; stars: formation; stars: individual: AFGL 2591; techniques: high angular resolution ID YOUNG STELLAR OBJECTS; FORMING REGIONS; MASER OBSERVATIONS; MOLECULAR OUTFLOW; RADIO-CONTINUUM; JET-DRIVEN; AFGL-2591; KINEMATICS; EVOLUTION; GL-2591 AB We report on a detailed study of the water maser kinematics and radio continuum emission toward the most massive and young object in the star-forming region AFGL 2591. Our analysis shows at least two spatial scales of multiple star formation, one projected across 0.1 pc on the sky and another one at about 2000 AU from a ZAMS star of about 38 M-circle dot. This young stellar object drives a powerful jet-and wind-driven outflow system with the water masers associated to the outflow walls, previously detected as a limb-brightened cavity in the NIR band. At about 1300 AU to the north of this object a younger protostar drives two bow shocks, outlined by arc-like water maser emission, at 200 AU either side of the source. We have traced the velocity profile of the gas that expands along these arc-like maser structures and compared it with the jet-driven outflow model. This analysis suggests that the ambient medium around the northern protostar is swept up by a jet-driven shock (>66 km s(-1)) and perhaps a lower-velocity (similar to 10 km s(-1)) wind with an opening angle of about 20 degrees from the jet axis. C1 [Sanna, A.; Carrasco-Gonzalez, C.; Menten, K. M.; Brunthaler, A.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Reid, M. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Moscadelli, L.] Osserv Astrofis Arcetri, INAF, I-50125 Florence, Italy. [Rygl, K. L. J.] Ist Fis Spazio Interplanetario, IFSI INAF, I-00133 Rome, Italy. RP Sanna, A (reprint author), Max Planck Inst Radioastron, Hugel 69, D-53121 Bonn, Germany. EM asanna@mpifr-bonn.mpg.de RI Sanna, Andrea/A-2865-2015; OI Sanna, Andrea/0000-0002-0118-2649; Moscadelli, Luca/0000-0002-8517-8881 FU ERC [247078]; ASI [I/005/07/1] FX We thank J. M. Torrelles and A. P. Lobanov for helpful discussions in preparation. This work was partially funded by the ERC Advanced Investigator Grant GLOSTAR (247078). K. L. J. R. is funded by an ASI fellowship under contract number I/005/07/1. NR 38 TC 18 Z9 18 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 1 PY 2012 VL 745 IS 2 AR 191 DI 10.1088/0004-637X/745/2/191 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 893AI UT WOS:000300326800089 ER PT J AU Steiner, JF McClintock, JE AF Steiner, James F. McClintock, Jeffrey E. TI MODELING THE JET KINEMATICS OF THE BLACK HOLE MICROQUASAR XTE J1550-564: A CONSTRAINT ON SPIN-ORBIT ALIGNMENT SO ASTROPHYSICAL JOURNAL LA English DT Article DE black hole physics; stars: individual (XTE J1550-564); X-rays: binaries ID X-RAY BINARIES; RELATIVISTIC JETS; DYNAMICAL MODEL; LARGE-SCALE; ACCRETION DISCS; GRO J1655-40; J1819.3-2525; MISALIGNMENT; PHOTOMETRY; EVOLUTION AB Measurements of black hole spin made using the continuum-fitting method rely on the assumption that the inclination of the black hole's spin axis to our line of sight is the same as the orbital inclination angle i of the host binary system. The X-ray and radio jet data available for the microquasar XTE J1550-564 offer a rare opportunity to test this assumption. Following the work of others, we have modeled these data and thereby determined the inclination angle theta of the jet axis, which is presumed to be aligned with the black hole's spin axis. We find theta approximate to 71 degrees and place an upper limit on the difference between the spin and orbital inclinations of |theta - i| < 12 degrees (90% confidence). Our measurement tests for misalignment along the line of sight while providing no constraint perpendicular to this plane. Our constraint on the misalignment angle supports the prediction that the spinning black hole in XTE J1550-564 has aligned itself with the orbital plane and provides support for the measurement of its spin via the continuum-fitting method. Our conclusions are based on a simple and reasonable model of a pair of symmetric jets propagating into a low-density cavity whose western wall is approximate to 20% closer to XTE J1550-564 than its eastern wall. C1 [Steiner, James F.; McClintock, Jeffrey E.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Steiner, JF (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM jsteiner@cfa.harvard.edu FU Smithsonian Institution; NASA [NNX11AD08G]; FAS Science Division Research Computing Group at Harvard University FX J.F.S. was supported by the Smithsonian Institution Endowment Funds and J.E.M. acknowledges support from NASA grant NNX11AD08G. We thank Bob Penna, Sasha Tchekovskoy, and Ramesh Narayan for constructive ideas which helped in shaping the direction of this work, and both Joey Neilsen and Lijun Gou for their comments on the manuscript. We thank an anonymous referee for helpful feedback which has improved this paper. The MCMC analyses were run using the Odyssey cluster supported by the FAS Science Division Research Computing Group at Harvard University. NR 37 TC 35 Z9 35 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 1 PY 2012 VL 745 IS 2 AR 136 DI 10.1088/0004-637X/745/2/136 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 893AI UT WOS:000300326800034 ER PT J AU Testa, P Drake, JJ Landi, E AF Testa, Paola Drake, Jeremy J. Landi, Enrico TI TESTING EUV/X-RAY ATOMIC DATA FOR THE SOLAR DYNAMICS OBSERVATORY SO ASTROPHYSICAL JOURNAL LA English DT Article DE stars: coronae; stars: individual (Procyon); stars: late-type; Sun: corona; Sun: X-rays, gamma rays; X-rays: stars ID EXTREME-ULTRAVIOLET REGION; EMISSION-LINES; FE-VII; FUNDAMENTAL PARAMETERS; ELEMENTAL ABUNDANCES; CORONAL ACTIVITY; ACTIVE-REGION; NEARBY STARS; XMM-NEWTON; PROCYON AB The Atmospheric Imaging Assembly (AIA) and the Extreme-ultraviolet Variability Experiment (EVE) on board the Solar Dynamics Observatory (SDO) include spectral windows in the X-ray/EUV band. Accuracy and completeness of the atomic data in this wavelength range is essential for interpretation of the spectrum and irradiance of the solar corona, and of SDO observations made with the AIA and EVE instruments. Here, we test the X-ray/EUV data in the CHIANTI database to assess their completeness and accuracy in the SDO bands, with particular focus on the 94 angstrom and 131 angstrom AIA passbands. Given the paucity of solar observations adequate for this purpose, we use high-resolution X-ray spectra of the low-activity solar-like corona of Procyon obtained with the Chandra Low Energy Transmission Grating Spectrometer (LETGS). We find that while spectral models overall can reproduce quite well the observed spectra in the soft X-ray range lambda less than or similar to 50 angstrom, and at the EUV wavelengths lambda greater than or similar to 130 angstrom, they significantly underestimate the observed flux in the 50-130 angstrom wavelength range. The model underestimates the observed flux by a variable factor ranging from approximate to 1.5, at short wavelengths below approximate to 50 angstrom, up to approximate to 5-7 in the similar to 70-125 angstrom range. In the AIA bands covered by LETGS, i.e., 94 angstrom and 131 angstrom, we find that the observed flux can be underestimated by large factors (similar to 3 and similar to 1.9, respectively, for the case of Procyon presented here). We discuss the consequences for analysis of AIA data and possible empirical corrections to the AIA responses to model more realistically the coronal emission in these passbands. C1 [Testa, Paola; Drake, Jeremy J.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. [Landi, Enrico] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA. RP Testa, P (reprint author), Smithsonian Astrophys Observ, 60 Garden St,MS 58, Cambridge, MA 02138 USA. EM ptesta@cfa.harvard.edu RI Landi, Enrico/H-4493-2011 FU Lockheed-Martin [SP02H1701R]; NASA [NAS8-39073]; [NNX11AC20G]; [NNX10AM17G]; [SV1-81002] FX We thank Adam Foster for useful discussion, and the referee for comments that have helped improve the paper. P. T. was supported by contract SP02H1701R from Lockheed-Martin to the Smithsonian Astrophysical Observatory. J.J.D. was supported by NASA contract NAS8-39073 to the Chandra X-ray Center and thanks the Director, H. Tananbaum, for continuing support. The work of E. L. is supported by the NNX11AC20G and NNX10AM17G grants to the University of Michigan, and grant SV1-81002 to the Smithsonian Astrophysical Observatory. NR 47 TC 30 Z9 30 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 1 PY 2012 VL 745 IS 2 AR 111 DI 10.1088/0004-637X/745/2/111 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 893AI UT WOS:000300326800009 ER PT J AU Whitaker, KE Kriek, M van Dokkum, PG Bezanson, R Brammer, G Franx, M Labbe, I AF Whitaker, Katherine E. Kriek, Mariska van Dokkum, Pieter G. Bezanson, Rachel Brammer, Gabriel Franx, Marijn Labbe, Ivo TI A LARGE POPULATION OF MASSIVE COMPACT POST-STARBURST GALAXIES AT z > 1: IMPLICATIONS FOR THE SIZE EVOLUTION AND QUENCHING MECHANISM OF QUIESCENT GALAXIES SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: evolution; galaxies: formation; galaxies: high-redshift ID MEDIUM-BAND SURVEY; SIMILAR-TO 2; GMASS ULTRADEEP SPECTROSCOPY; STAR-FORMATION HISTORIES; HIGH-REDSHIFT GALAXIES; DIGITAL SKY SURVEY; ELLIPTIC GALAXIES; DEEP SURVEY; COLOR BIMODALITY; STELLAR MASSES AB We study the growth of the red sequence through the number density and structural evolution of a sample of young and old quiescent galaxies at 0 < z < 2. The galaxies are selected from the NEWFIRM Medium-Band Survey in the Cosmic Evolution Survey field. We find a large population of massive young recently quenched ("post-starburst") galaxies at z > 1 that are almost non-existent at z < 1; their number density is 5 x 10(-5) Mpc(-3) at z = 2, whereas it is a factor of 10 less at z = 0.5. The observed number densities of young and old quiescent galaxies at z > 1 are consistent with a simple model in which all old quiescent galaxies were once identified as post-starburst galaxies. We find that the overall population of quiescent galaxies have smaller sizes and slightly more elongated shapes at higher redshift, in agreement with other recent studies. Interestingly, the most recently quenched galaxies at 1 < z < 2 are not larger, and possibly even smaller, than older galaxies at those redshifts. This result is inconsistent with the idea that the evolution of the average size of quiescent galaxies is largely driven by continuous transformations of larger, star-forming galaxies: in that case, the youngest quiescent galaxies would also be the largest. Instead, mergers or other mechanisms appear to be required to explain the size growth of quiescent galaxies from z = 2 to the present. C1 [Whitaker, Katherine E.; van Dokkum, Pieter G.; Bezanson, Rachel] Yale Univ, Dept Astron, New Haven, CT 06511 USA. [Kriek, Mariska] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Brammer, Gabriel] European So Observ, Santiago 19, Chile. [Franx, Marijn; Labbe, Ivo] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. RP Whitaker, KE (reprint author), Yale Univ, Dept Astron, New Haven, CT 06511 USA. EM katherine.whitaker@yale.edu OI Bezanson, Rachel/0000-0001-5063-8254 FU NSF [AST-0807974]; NASA [NNX11AB08G] FX We thank the anonymous referee for useful comments and a careful reading of the paper. This study makes use of data from the NEWFIRM Medium-Band Survey, a multi-wavelength survey conducted with the NEWFIRM instrument at the KPNO, supported in part by the NSF and NASA. We thank the NMBS collaboration for their contribution to this work and the COSMOS and AEGIS teams for the release of high quality multi-wavelength data sets to the community. Support from NSF grant AST-0807974 and NASA grant NNX11AB08G is gratefully acknowledged. NR 70 TC 72 Z9 72 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 1 PY 2012 VL 745 IS 2 AR 179 DI 10.1088/0004-637X/745/2/179 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 893AI UT WOS:000300326800077 ER PT J AU Collins, CW Songsasen, NS Vick, MM Wolfe, BA Weiss, RB Keefer, CL Monfort, SL AF Collins, C. Wynne Songsasen, Nucharin S. Vick, Mandi M. Wolfe, Barbara A. Weiss, Rachael B. Keefer, Carol L. Monfort, Steven L. TI Abnormal Reproductive Patterns in Przewalski's Mares Are Associated with a Loss in Gene Diversity SO BIOLOGY OF REPRODUCTION LA English DT Article DE endocrinology; equids (horses, donkeys, zebras); estrous cycle; female infertility; follicular patterns; genetics; inbreeding; Przelwalski's horse; wildlife; zoo species (exotic species) ID SUCCESSFUL ARTIFICIAL-INSEMINATION; PANDA AILUROPODA-MELANOLEUCA; MONITORING OVARIAN-FUNCTION; ENZYME-IMMUNOASSAY; EQUUS-PRZEWALSKII; URINARY; SERUM; SPERMATOZOA; KISSPEPTIN; EXCRETION AB The ex situ population of the Przewalski's horse (Equus ferus przewalskii) is not self-sustaining (20% foaling rate), and the demography is skewed toward aging individuals with low gene diversity. We designed the present study to gain a better understanding of the reproductive biology of the Przewalski's mare and to determine whether age and gene diversity influenced reproductive function. Urine samples were collected 3-7 days/wk from 19 mares from May to September, and ultrasound examinations of follicular structures were performed 3 days/wk for 5 wk from May through July in nine individuals. A high proportion of mares exhibited abnormal (endocrine, 5 [26.3%] of 19; follicular, 2 [22.2%] of 9) or acyclic (endocrine, 4 [21.1%] of 19; follicular, 3 [33.3%] of 9) reproductive patterns. In four cyclic mares, estrous cycle length was 25.1 +/- 1.2 days, with 12.2 +/- 0.9 days of diestrus. Follicles in cyclic mares grew 1.2 +/- 0.6 mm per day and ovulated after reaching 40.4 +/- 8.9 mm. Mares with a high coefficient of inbreeding excreted reduced levels of mean urinary estrogens (r(2) = 0.476, P < 0.05), but age had no significant impact on reproductive patterns in this population. Overall, these data suggest that long-term genetic management of this population is necessary to maintain reproductive fitness. C1 [Collins, C. Wynne; Songsasen, Nucharin S.; Vick, Mandi M.; Monfort, Steven L.] Smithsonian Conservat Biol Inst, Front Royal, VA USA. [Vick, Mandi M.; Wolfe, Barbara A.; Weiss, Rachael B.] The Wilds, Cumberland, OH USA. [Collins, C. Wynne; Keefer, Carol L.] Univ Maryland, Dept Anim & Avian Sci, College Pk, MD 20742 USA. RP Collins, CW (reprint author), Univ Queensland, Sch Vet Sci, Gatton Campus, Gatton, Qld 4343, Australia. EM w.collins@uq.edu.au FU Morris Animal Foundation; Smithsonian Institution FX Supported by the Morris Animal Foundation, the Smithsonian Institution's Undersecretary for Science Endowment Fund, and generous donations from Ms. Shirley Sichel and Colonel and Mrs. Austin Bach. NR 33 TC 3 Z9 3 U1 4 U2 56 PU SOC STUDY REPRODUCTION PI MADISON PA 1691 MONROE ST,SUITE # 3, MADISON, WI 53711-2021 USA SN 0006-3363 EI 1529-7268 J9 BIOL REPROD JI Biol. Reprod. PD FEB PY 2012 VL 86 IS 2 AR 28 DI 10.1095/biolreprod.111.092676 PG 10 WC Reproductive Biology SC Reproductive Biology GA 897BS UT WOS:000300616700003 PM 21900686 ER PT J AU Lahoz, WA Peuch, VH Orphal, J Attie, JL Chance, K Liu, X Edwards, D Elbern, H Flaud, JM Claeyman, M El Amraoui, L AF Lahoz, W. A. Peuch, V. -H. Orphal, J. Attie, J. -L. Chance, K. Liu, X. Edwards, D. Elbern, H. Flaud, J. -M. Claeyman, M. El Amraoui, L. TI MONITORING AIR QUALITY FROM SPACE The Case for the Geostationary Platform SO BULLETIN OF THE AMERICAN METEOROLOGICAL SOCIETY LA English DT Article ID TROPOSPHERIC POLLUTION; UNITED-STATES; OZONE; RETRIEVAL; EMISSION; SPECTROSCOPY; ULTRAVIOLET; INSTRUMENT; SIMULATION; OUTFLOW C1 [Lahoz, W. A.] Norsk Inst Luftforskning, N-2027 Kjeller, Norway. [Lahoz, W. A.; Peuch, V. -H.; Attie, J. -L.; Claeyman, M.; El Amraoui, L.] CNRM GMGEC CARMA, F-31100 Toulouse, France. [Orphal, J.] Karlsruhe Inst Technol, IMK, Karlsruhe, Germany. [Attie, J. -L.; Claeyman, M.] Univ Toulouse, Lab Aerol, CNRS INSU, Toulouse, France. [Chance, K.; Liu, X.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Edwards, D.] Natl Ctr Atmospher Res, Boulder, CO 80307 USA. [Elbern, H.] Univ Cologne, Rhenish Inst Environm Res, D-50931 Cologne, Germany. [Elbern, H.] Forschungszentrum Julich, Inst Energy & Climate Res Troposphere, D-52425 Julich, Germany. [Flaud, J. -M.] Univ Paris Est, Lab Interuniv Syst Atmospher, CNRS UMR 7583, Creteil, France. RP Lahoz, WA (reprint author), Norsk Inst Luftforskning, POB 100,Inst Veien18, N-2027 Kjeller, Norway. EM wal@nilu.no RI Orphal, Johannes/A-8667-2012; Elbern, Hendrik/J-8672-2012; Liu, Xiong/P-7186-2014; OI Orphal, Johannes/0000-0002-1943-4496; Elbern, Hendrik/0000-0002-5746-4506; Liu, Xiong/0000-0003-2939-574X; Chance, Kelly/0000-0002-7339-7577 FU Centre National de la Recherche Scientifique (CNRS); EADS-ASTRIUM; Centre National de Recherches Meteorologiques (CNRM) of Meteo-France; RTRA/STAE; INFOAIR; Region Midi-Pyrenees; NASA; Smithsonian Institution; Helmholtz Association of German Research Centres FX This work was funded by the Centre National de la Recherche Scientifique (CNRS), EADS-ASTRIUM, the Centre National de Recherches Meteorologiques (CNRM) of Meteo-France, the RTRA/STAE (project POGEQA), and the INFOAIR project funded by Region Midi-Pyrenees. Work at NILU was funded by an internal project. Research at the Harvard-Smithsonian Center for Astrophysics was funded by NASA and the Smithsonian Institution. Work at Karlsruhe Institute of Technology was funded by the Helmholtz Association of German Research Centres. Work at the National Center for Atmospheric Research (NCAR) was funded by NASA. Thanks to Finn Bjorklid (NILU) and Matthieu Joly (CNRM) for helping with figures. We thank the reviewers and the editor for making suggestions that helped improve the paper. NR 70 TC 16 Z9 16 U1 0 U2 9 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0003-0007 EI 1520-0477 J9 B AM METEOROL SOC JI Bull. Amer. Meteorol. Soc. PD FEB PY 2012 VL 93 IS 2 BP 221 EP 233 DI 10.1175/BAMS-D-11-00045.1 PG 13 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 897FP UT WOS:000300632200009 ER PT J AU Roseboom, IG Ivison, RJ Greve, TR Amblard, A Arumugam, V Auld, R Aussel, H Bethermin, M Blain, A Bock, J Boselli, A Brisbin, D Buat, V Burgarella, D Castro-Rodriguez, N Cava, A Chanial, P Chapin, E Chapman, S Clements, DL Conley, A Conversi, L Cooray, A Dowell, CD Dunlop, JS Dwek, E Eales, S Elbaz, D Farrah, D Franceschini, A Glenn, J Griffin, M Halpern, M Hatziminaoglou, E Ibar, E Isaak, K Lagache, G Levenson, L Lu, N Madden, S Maffei, B Mainetti, G Marchetti, L Marsden, G Morrison, G Mortier, AMJ Nguyen, HT O'Halloran, B Oliver, SJ Omont, A Page, MJ Panuzzo, P Papageorgiou, A Pearson, CP Perez-Fournon, I Pohlen, M Rawlings, JI Raymond, G Rigopoulou, D Rizzo, D Rodighiero, G Rowan-Robinson, M Schulz, B Scott, D Seymour, N Shupe, DL Smith, AJ Stevens, JA Symeonidis, M Trichas, M Tugwell, KE Vaccari, M Valtchanov, I Vieira, JD Viero, MP Vigroux, L Wardlow, J Wang, L Wright, G Xu, CK Zemcov, M AF Roseboom, I. G. Ivison, R. J. Greve, T. R. Amblard, A. Arumugam, V. Auld, R. Aussel, H. Bethermin, M. Blain, A. Bock, J. Boselli, A. Brisbin, D. Buat, V. Burgarella, D. Castro-Rodriguez, N. Cava, A. Chanial, P. Chapin, E. Chapman, S. Clements, D. L. Conley, A. Conversi, L. Cooray, A. Dowell, C. D. Dunlop, J. S. Dwek, E. Eales, S. Elbaz, D. Farrah, D. Franceschini, A. Glenn, J. Griffin, M. Halpern, M. Hatziminaoglou, E. Ibar, E. Isaak, K. Lagache, G. Levenson, L. Lu, N. Madden, S. Maffei, B. Mainetti, G. Marchetti, L. Marsden, G. Morrison, G. Mortier, A. M. J. Nguyen, H. T. O'Halloran, B. Oliver, S. J. Omont, A. Page, M. J. Panuzzo, P. Papageorgiou, A. Pearson, C. P. Perez-Fournon, I. Pohlen, M. Rawlings, J. I. Raymond, G. Rigopoulou, D. Rizzo, D. Rodighiero, G. Rowan-Robinson, M. Schulz, B. Scott, Douglas Seymour, N. Shupe, D. L. Smith, A. J. Stevens, J. A. Symeonidis, M. Trichas, M. Tugwell, K. E. Vaccari, M. Valtchanov, I. Vieira, J. D. Viero, M. P. Vigroux, L. Wardlow, J. Wang, L. Wright, G. Xu, C. K. Zemcov, M. TI The Herschel Multi-tiered Extragalactic Survey: SPIRE-mm photometric redshifts SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies: high-redshift - galaxies: statistics - submillimetre: galaxies ID DEEP-FIELD-SOUTH; GOODS-N FIELD; FAR-INFRARED PROPERTIES; BRIGHTEST SUBMILLIMETER SOURCE; SPECTRAL ENERGY-DISTRIBUTIONS; STAR-FORMATION HISTORY; FAINT RADIO GALAXIES; MU-M OBSERVATIONS; LABOCA SURVEY; MIDINFRARED COUNTERPARTS AB We investigate the potential of submmmm and submmmmradio photometric redshifts using a sample of mm-selected sources as seen at 250, 350 and 500 mu m by the SPIRE instrument on Herschel. From a sample of 63 previously identified mm sources with reliable radio identifications in the Great Observatories Origins Deep Survey North and Lockman Hole North fields, 46 (73 per cent) are found to have detections in at least one SPIRE band. We explore the observed submm/mm colour evolution with redshift, finding that the colours of mm sources are adequately described by a modified blackbody with constant optical depth tau=(/nu0)beta, where beta=+1.8 and nu 0=c/100 mu m. We find a tight correlation between dust temperature and IR luminosity. Using a single model of the dust temperature and IR luminosity relation, we derive photometric redshift estimates for the 46 SPIRE-detected mm sources. Testing against the 22 sources with known spectroscopic or good quality optical/near-IR photometric redshifts, we find submm/mm photometric redshifts offer a redshift accuracy of vertical bar Delta z vertical bar/(1+z)= 0.16 (=0.51). Including constraints from the radiofar-IR correlation, the accuracy is improved to vertical bar Delta z vertical bar/(1+z)=0.15 (=0.45). We estimate the redshift distribution of mm-selected sources finding a significant excess at z > 3 when compared to similar to 850 mu m selected samples. C1 [Roseboom, I. G.; Farrah, D.; Oliver, S. J.; Smith, A. J.; Wang, L.] Univ Sussex, Ctr Astron, Dept Phys & Astron, Brighton BN1 9QH, E Sussex, England. [Roseboom, I. G.; Ivison, R. J.; Dunlop, J. S.] Univ Edinburgh, Inst Astron, Royal Observ, Edinburgh EH9 3HJ, Midlothian, Scotland. [Ivison, R. J.; Arumugam, V.; Ibar, E.; Wright, G.] UK Astron Technol Ctr, Royal Observ, Edinburgh EH9 3HJ, Midlothian, Scotland. [Greve, T. R.] Univ Copenhagen, Niels Bohr Inst, Dark Cosmol Ctr, DK-2100 Copenhagen, Denmark. [Amblard, A.; Cooray, A.; Wardlow, J.] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA. [Auld, R.; Eales, S.; Griffin, M.; Isaak, K.; Papageorgiou, A.; Pohlen, M.; Raymond, G.] Cardiff Univ, Cardiff Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales. [Aussel, H.; Bethermin, M.; Chanial, P.; Elbaz, D.; Madden, S.; Panuzzo, P.] Univ Paris Diderot, Lab AIM Paris Saclay, CE Saclay, CEA,DSM,Irfu,CNRS, F-91191 Gif Sur Yvette, France. [Bock, J.; Dowell, C. D.; Levenson, L.; Nguyen, H. T.; Zemcov, M.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Boselli, A.; Buat, V.; Burgarella, D.] Univ Aix Marseille, CNRS, Lab Astrophys Marseille, OAMP, F-13388 Marseille 13, France. [Brisbin, D.] Cornell Univ, Ithaca, NY 14853 USA. [Castro-Rodriguez, N.; Cava, A.; Perez-Fournon, I.] Inst Astrofis Canarias IAC, E-38200 Tenerife, Spain. [Castro-Rodriguez, N.; Cava, A.; Perez-Fournon, I.] Univ La Laguna ULL, Dept Astrofis, E-38205 Tenerife, Spain. [Chapin, E.; Halpern, M.; Marsden, G.; Scott, Douglas] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada. [Chapman, S.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Clements, D. L.; Mortier, A. M. J.; O'Halloran, B.; Rizzo, D.; Rowan-Robinson, M.] Univ London Imperial Coll Sci Technol & Med, Blackett Lab, Astrophys Grp, London SW7 2AZ, England. [Conley, A.] Univ Colorado, Ctr Astrophys & Space Astron, Boulder, CO 80309 USA. [Conversi, L.; Valtchanov, I.] European Space Astron Ctr, Herschel Sci Ctr, Madrid 28691, Spain. [Dwek, E.] NASA, Observat Cosmol Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Franceschini, A.; Mainetti, G.; Marchetti, L.; Rodighiero, G.; Vaccari, M.] Univ Padua, Dipartimento Astron, I-35122 Padua, Italy. [Glenn, J.] Univ Colorado, Dept Astrophys & Planetary Sci, Boulder, CO 80309 USA. [Hatziminaoglou, E.] ESO, D-85748 Garching, Germany. [Lagache, G.] Univ Paris 11, Inst Astrophys Spatiale IAS, F-91405 Orsay, France. [Lu, N.; Schulz, B.; Shupe, D. L.; Xu, C. K.] CALTECH, Infrared Proc & Anal Ctr, JPL, Pasadena, CA 91125 USA. [Maffei, B.] Univ Manchester, Sch Phys & Astron, Manchester M13 9PL, Lancs, England. [Morrison, G.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Morrison, G.] Canada France Hawaii Telescope Corp, Kamuela, HI 96743 USA. [Omont, A.; Vigroux, L.] UPMC Univ Paris 06, Inst Astrophys Paris, CNRS, UMR 7095, F-75014 Paris, France. [Page, M. J.; Rawlings, J. I.; Seymour, N.; Symeonidis, M.; Tugwell, K. E.] Univ Coll London, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England. [Pearson, C. P.; Rigopoulou, D.] Rutherford Appleton Lab, Space Sci & Technol Dept, Didcot OX11 0QX, Oxon, England. [Pearson, C. P.] Univ Lethbridge, Inst Space Imaging Sci, Lethbridge, AB T1K 3M4, Canada. [Rigopoulou, D.] Univ Oxford, Oxford OX1 3RH, England. [Stevens, J. A.] Univ Hertfordshire, Ctr Astrophys Res, Hatfield AL10 9AB, Herts, England. [Trichas, M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Roseboom, IG (reprint author), Univ Sussex, Ctr Astron, Dept Phys & Astron, Brighton BN1 9QH, E Sussex, England. EM igr@roe.ac.uk RI Dwek, Eli/C-3995-2012; amblard, alexandre/L-7694-2014; Wardlow, Julie/C-9903-2015; Ivison, R./G-4450-2011; Vaccari, Mattia/R-3431-2016; Cava, Antonio/C-5274-2017; OI amblard, alexandre/0000-0002-2212-5395; Wardlow, Julie/0000-0003-2376-8971; Ivison, R./0000-0001-5118-1313; Vaccari, Mattia/0000-0002-6748-0577; Cava, Antonio/0000-0002-4821-1275; Scott, Douglas/0000-0002-6878-9840; Marchetti, Lucia/0000-0003-3948-7621; Seymour, Nicholas/0000-0003-3506-5536; Bethermin, Matthieu/0000-0002-3915-2015; Rodighiero, Giulia/0000-0002-9415-2296 FU Science and Technology Facilities Council [ST/F002858/1]; Royal Society; European Research Council; Italian Space Agency (ASI) [I/005/07/0]; CSA (Canada); NAOC (China); CEA (France); CNES (France); CNRS (France); ASI (Italy); MCINN (Spain); SNSB (Sweden); STFC (UK); NASA (USA) FX LW and SJO were supported by the Science and Technology Facilities Council (ST/F002858/1).; JSD acknowledges the support of the Royal Society via a Wolfson Research Merit award, and the support of the European Research Council via the award of an Advanced Grant.; AF, GM, LM and MV were supported by the Italian Space Agency (ASI Herschel Science Contract I/005/07/0).; SPIRE has been developed by a consortium of institutes led by Cardiff University (UK) and including University of Lethbridge (Canada), NAOC (China), CEA, LAM(France), IFSI, University of Padua (Italy), IAC (Spain), Stockholm Observatory (Sweden), Imperial College London, RAL, UCL-MSSL, UK ATC, University of Sussex (UK), Caltech, JPL, NHSC, University of Colorado (USA). This development has been supported by national funding agencies: CSA (Canada); NAOC (China); CEA, CNES, CNRS (France); ASI (Italy); MCINN (Spain); SNSB (Sweden); STFC (UK) and NASA (USA). NR 89 TC 63 Z9 63 U1 0 U2 1 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD FEB PY 2012 VL 419 IS 4 BP 2758 EP 2773 DI 10.1111/j.1365-2966.2011.19827.x PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 873XZ UT WOS:000298920600002 ER PT J AU Kralj-Fiser, S Kuntner, M AF Kralj-Fiser, Simona Kuntner, Matjaz TI Eunuchs as better fighters? SO NATURWISSENSCHAFTEN LA English DT Article DE Aggression; Cannibalism; Emasculation; Guarding; Plugging; Nephilidae; Nephilengys livida ID LETHAL COMBAT; SPIDERS ARANEAE; CANNIBALISTIC SPIDER; INTERSEXUAL CONFLICT; NEPHILID SPIDERS; FIG WASP; COMPETITION; EVOLUTION; FEMALES; RELATIVES AB Male-male competition for females can significantly affect a male's reproductive success and hence his fitness. Game theory predicts that an individual should avoid fighting when its future reproductive potential is high, but should fight forcefully when its future reproductive potential is insignificant. When mates are scarce, extreme competition and fatal fighting is expected. We recently showed that Nephilengys malabarensis eunuchs, i.e. sterile spider males that lost their genitals during copulation, become more aggressive during male-male contests. Here, we add crucial comparative data by exploring eunuch fighting behaviour in Nephilengys livida from Madagascar, specifically by testing the 'better fighter hypotheses' in a laboratory setting. Similar to N. malabarensis, N. livida copulations resulted in total male castration with the severed palp plugging the female genitals in 70.83% cases, which mostly (63.63%) prevented subsequent copulations. Unexpectedly, however, N. livida eunuchs exhibited lower aggressiveness than virgin males. We interpret these results in the light of different mating biology between the so far studied species known for the eunuch phenomenon, which might reflect differing plug effectiveness due to variation in genital anatomy in N. livida, N. malabarensis and Herennia multipuncta. However, detected differences in aggressive behaviour of N. livida versus N. malabarensis eunuchs might also be explained by the species' ecology, with lower population densities resulting in a relaxed male-male competition making excessive aggression and mate guarding redundant. This study thus questions the generality of overt aggressiveness in mated males with no reproductive value, and highlights the importance of understanding the natural history of species in the question. C1 [Kuntner, Matjaz] Hubei Univ, Coll Life Sci, Wuhan 430062, Hubei, Peoples R China. [Kralj-Fiser, Simona; Kuntner, Matjaz] Slovenian Acad Sci & Arts, Inst Biol, Ctr Sci Res, Ljubljana, Slovenia. [Kralj-Fiser, Simona] Univ Hamburg, Biozentrum Grindel, D-20146 Hamburg, Germany. [Kuntner, Matjaz] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA. RP Kuntner, M (reprint author), Hubei Univ, Coll Life Sci, Wuhan 430062, Hubei, Peoples R China. EM kuntner@gmail.com FU Slovenian Research Agency [J1-2063]; National Geographic Society [8655-09]; Humboldt fellowship for postdoctoral researchers; Humboldt return fellowship FX We thank three anonymous reviewers and Jutta Schneider for comments on the manuscript, Matjaz Gregoric for the spider collection and laboratory help; Ziva Justinek for help with experiments and lab support; and Ingi Agnarsson, Sahondra Lalao Rahanitriniaina and Honore Rabarison for their help in field. This work was funded by the Slovenian Research Agency (grant J1-2063 to MK) and the National Geographic Society (grant 8655-09 to I. Agnarsson, M. Kuntner and T. Blackledge). SKF was supported by Humboldt fellowship for postdoctoral researchers and Humboldt return fellowship. NR 41 TC 7 Z9 7 U1 2 U2 22 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0028-1042 J9 NATURWISSENSCHAFTEN JI Naturwissenschaften PD FEB PY 2012 VL 99 IS 2 BP 95 EP 101 DI 10.1007/s00114-011-0873-1 PG 7 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 897UB UT WOS:000300682000002 PM 22167072 ER PT J AU Parr, CS Guralnick, R Cellinese, N Page, RDM AF Parr, Cynthia S. Guralnick, Robert Cellinese, Nico Page, Roderic D. M. TI Evolutionary informatics: unifying knowledge about the diversity of life SO TRENDS IN ECOLOGY & EVOLUTION LA English DT Review ID PHYLOGENETIC ANALYSIS; MAXIMUM-LIKELIHOOD; BIODIVERSITY INFORMATICS; MINIMUM INFORMATION; DATA INTEGRATION; UNIFICATION; ONTOLOGIES; BIOLOGY; TREES; PLACEMENT AB The accelerating growth of data and knowledge in evolutionary biology is indisputable. Despite this rapid progress, information remains scattered, poorly documented and in formats that impede discovery and integration. A grand challenge is the creation of a linked system of all evolutionary data, information and knowledge organized around Darwin's ever-growing Tree of Life. Such a system, accommodating topological disagreement where necessary, would consolidate taxon names, phenotypic and geographical distributional data across clades, and serve as an integrated community resource. The field of evolutionary informatics, reviewed here for the first time, has matured into a robust discipline that is developing the conceptual, infrastructure and community frameworks for meeting this grand challenge. C1 [Guralnick, Robert] Univ Colorado, Univ Colorado Museum Nat Hist, Boulder, CO 80309 USA. [Parr, Cynthia S.] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20013 USA. [Guralnick, Robert] Univ Colorado, Dept Ecol & Evolutionary Biol, Boulder, CO 80309 USA. [Cellinese, Nico] Univ Florida, Florida Museum Nat Hist, Gainesville, FL 32611 USA. [Page, Roderic D. M.] Univ Glasgow, Inst Biodivers Anim Hlth & Comparat Med, Coll Med Vet & Life Sci, Glasgow G12 8QQ, Lanark, Scotland. RP Guralnick, R (reprint author), Univ Colorado, Univ Colorado Museum Nat Hist, Bruce Curtis Bldg,UCB 265, Boulder, CO 80309 USA. EM Robert.Guralnick@colorado.edu RI Parr, Cynthia/E-8013-2010; OI Parr, Cynthia/0000-0002-8870-7099; Cellinese, Nico/0000-0002-7157-9414; Page, Roderic/0000-0002-7101-9767 FU MacArthur Foundation [93466-0]; NSF [NSF0960549, NSF0956350]; NSF-DEB [0953677]; NSF-DBI [0956371]; [NSF0531769 AToL] FX We thank our colleagues on the iEvoBio organizing committee for their contributions directly or indirectly to this paper: Hilmar Lapp, Dawn Field, Mark Holder. Andrea Thomer, Karen Cranston, Andrew Hill, David Schindel, Tom Orrell and William Piel, and an anonymous reviewer all provided invaluable comments on previous versions of the manuscript. Anne Bowser helped prepare Figure I in Box 3. C.S.P. acknowledges support from MacArthur Foundation support (grant #93466-0) for Encyclopedia of Life, and NSF0531769 AToL: Collaborative Research: Phylogeny of Lepidoptera: A Genomics-inspired, Community Collaboration. R.G. acknowledges support from the NSF on the following projects: NSF0960549 Collaborative Research: Map of Life: An Infrastructure for Integrating Global Species Distribution Knowledge; NSF0956350 Collaborative Research: BiSciCol Tracker: Towards a Tagging and Tracking Infrastructure for Biodiversity Science Collections. N.C. acknowledges support from NSF-DEB 0953677 CAREER: Evolution in the Eastern Mediterranean Campanulaceae - Integrating Information Management and Scientific Workflows in Daily Research and Teaching and NSF-DBI 0956371 BiSciCol Tracker: towards a tagging and tracking infrastructure for biodiversity science collections. NR 78 TC 49 Z9 50 U1 4 U2 62 PU ELSEVIER SCIENCE LONDON PI LONDON PA 84 THEOBALDS RD, LONDON WC1X 8RR, ENGLAND SN 0169-5347 J9 TRENDS ECOL EVOL JI Trends Ecol. Evol. PD FEB PY 2012 VL 27 IS 2 BP 94 EP 103 DI 10.1016/j.tree.2011.11.001 PG 10 WC Ecology; Evolutionary Biology; Genetics & Heredity SC Environmental Sciences & Ecology; Evolutionary Biology; Genetics & Heredity GA 897MQ UT WOS:000300655200008 PM 22154516 ER PT J AU Punyasena, SW Jaramillo, C de la Parra, F Du, YL AF Punyasena, Surangi W. Jaramillo, Carlos de la Parra, Felipe Du, Yuelin TI Probabilistic correlation of single stratigraphic samples: A generalized approach for biostratigraphic data SO AAPG BULLETIN LA English DT Article ID PATTERNS AB Existing quantitative methods for biostratigraphic dating and correlation commonly ignore one of the key strengths of the microfossil record-relative abundance data. In this study, we present a maximum likelihood-based biostratigraphic method that demonstrates how microfossil abundance can be used in the stratigraphic placement of isolated samples. Precise correlation and dating of isolated paleontological samples is not possible with current methods, which are primarily intended for the alignment of longer stratigraphic sequences. In contrast, the probabilistic approach provided by likelihood analysis results in sample age estimates with defined confidence intervals. Therefore, all the uncertainties inherent in our age assessment (resulting from small sample sizes, incomplete sampling, imperfect knowledge of stratigraphic distributions, lack of taxonomic resolution of biostratigraphic data, and underlying environmental, paleogeographic, and sedimento-logic processes) are explicit in our results. We conclude with a field test of the method, from data collected from an oil well from the Catatumbo Basin, Colombia, illustrating the use of our approach in a real-world case study and highlighting how our method could be generalized to a wide range of stratigraphic problems. C1 [Punyasena, Surangi W.] Univ Illinois, Dept Plant Biol, Urbana, IL 61801 USA. [Jaramillo, Carlos] Smithsonian Trop Res Inst, Panama City, Panama. [de la Parra, Felipe] Inst Colombiano Petr, Santander, Spain. [Du, Yuelin] Univ Illinois, Dept Elect & Comp Engn, Urbana, IL 61801 USA. RP Punyasena, SW (reprint author), Univ Illinois, Dept Plant Biol, 505 S Goodwin Ave, Urbana, IL 61801 USA. EM punyasena@life.illinois.edu; jaramilloc@si.edu; felipe.delaparra@ecopetrol.com.co; du6@illinois.edu RI Punyasena, Surangi/C-9134-2011 FU University of Illinois School of Integrative Biology; Colombian Petroleum Institute-Ecopetrol S.A.; Smithsonian Institute FX Support for this research came from the University of Illinois School of Integrative Biology, the Colombian Petroleum Institute-Ecopetrol S.A., and the Smithsonian Institute. NR 24 TC 4 Z9 4 U1 0 U2 3 PU AMER ASSOC PETROLEUM GEOLOGIST PI TULSA PA 1444 S BOULDER AVE, PO BOX 979, TULSA, OK 74119-3604 USA SN 0149-1423 J9 AAPG BULL JI AAPG Bull. PD FEB PY 2012 VL 96 IS 2 BP 235 EP 244 DI 10.1306/06201111026 PG 10 WC Geosciences, Multidisciplinary SC Geology GA 890FW UT WOS:000300131500003 ER PT J AU Wang, K Zhang, QZ Wu, YF Li, HB Zhang, HW AF Wang, Ke Zhang, Qizhou Wu, Yuefang Li, Hua-bai Zhang, Huawei TI PROTOSTELLAR OUTFLOW HEATING IN A GROWING MASSIVE PROTOCLUSTER SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE ISM: individual objects (G28.34+0.06); ISM: jets and outflows; ISM: magnetic fields; masers; stars: early-type; stars: formation ID INFRARED-DARK CLOUDS; STAR-FORMATION; MOLECULAR CLOUDS; RADIATION FEEDBACK; MAGNETIC-FIELDS; MU-M; FRAGMENTATION; AMMONIA; G28.34+0.06; CLUSTER AB The dense molecular clump P1 in the infrared dark cloud complex G28.34+0.06 harbors a massive protostellar cluster at its extreme youth. Our previous Submillimeter Array observations revealed several jet-like CO outflows emanating from the protostars, indicative of intense accretion and potential interaction with ambient natal materials. Here, we present the Expanded Very Large Array spectral line observations toward P1 in the NH3 (J,K) = (1,1), (2,2), (3,3) lines, as well as H2O and class I CH3OH masers. Multiple NH3 transitions reveal the heated gas widely spread in the 1 pc clump. The temperature distribution is highly structured; the heated gas is offset from the protostars, and morphologically matches the outflows very well. Hot spots of spatially compact, spectrally broad NH3 (3,3) emission features are also found coincident with the outflows. A weak NH3 (3,3) maser is discovered at the interface between an outflow jet and the ambient gas. These findings suggest that protostellar heating may not be effective in suppressing fragmentation during the formation of massive cores. C1 [Wang, Ke; Wu, Yuefang; Zhang, Huawei] Peking Univ, Sch Phys, Dept Astron, Beijing 100871, Peoples R China. [Wang, Ke; Zhang, Qizhou] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Li, Hua-bai] Max Planck Inst Astron, D-69117 Heidelberg, Germany. RP Wang, K (reprint author), Peking Univ, Sch Phys, Dept Astron, Beijing 100871, Peoples R China. EM kwang@cfa.harvard.edu OI Wang, Ke/0000-0002-7237-3856; Zhang, Qizhou/0000-0003-2384-6589 FU SMA; China Scholarship Council; Smithsonian Institution; NSFC [10733030, 10873019, 11073003] FX We thank Edward T. Chambers for providing the spectra of the masers detected in G28.34+0.06. K.W. acknowledges the support from the SMA predoctoral fellowship and the China Scholarship Council. Q.Z. acknowledges the support from the Smithsonian Institution Endowment Funds. This research was supported in part by the NSFC grants 10733030, 10873019, and 11073003. NR 37 TC 19 Z9 19 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 FEB 1 PY 2012 VL 745 IS 2 AR L30 DI 10.1088/2041-8205/745/2/L30 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 891PJ UT WOS:000300228800015 ER PT J AU Maloney, KO Schmid, M Weller, DE AF Maloney, Kelly O. Schmid, Matthias Weller, Donald E. TI Applying additive modelling and gradient boosting to assess the effects of watershed and reach characteristics on riverine assemblages SO METHODS IN ECOLOGY AND EVOLUTION LA English DT Article DE benthic macroinvertebrates; diversity; fish; generalized additive models; richness; spatial autocorrelation; streams ID COMMUNITY STRUCTURE; REGRESSION SPLINES; VARIABLE SELECTION; STREAM FISHES; PREDICTION; CLASSIFICATION; COEFFICIENT; ALGORITHMS; LASSO; TREES AB 1. Issues with ecological data (e.g. non-normality of errors, nonlinear relationships and autocorrelation of variables) and modelling (e.g. overfitting, variable selection and prediction) complicate regression analyses in ecology. Flexible models, such as generalized additive models (GAMs), can address data issues, and machine learning techniques (e.g. gradient boosting) can help resolve modelling issues. Gradient boosted GAMs do both. Here, we illustrate the advantages of this technique using data on benthic macroinvertebrates and fish from 1573 small streams in Maryland, USA. 2. We assembled a predictor matrix of 15 watershed attributes (e. g. ecoregion and land use), 15 stream attributes (e. g. width and habitat quality) and location (latitude and longitude). We built boosted and conventionally estimated GAMs for macroinvertebrate richness and for the relative abundances of macroinvertebrates in the Orders Ephemeroptera, Plecoptera and Trichoptera (% EPT); individuals that cling to substrate (% Clingers); and individuals in the collector/gatherer functional feeding group (% Collectors). For fish, models were constructed for taxonomic richness, benthic species richness, biomass and the relative abundance of tolerant individuals (% Tolerant Fish). 3. For several of the responses, boosted GAMs had lower pseudo R-s(2) than conventional GAMs for in-sample data but larger pseudo R-s(2) for out-of-bootstrap data, suggesting boosted GAMs do not overfit the data and have higher prediction accuracy than conventional GAMs. The models explained most variation in fish richness (pseudo R-2 = 0 97), least variation in % Clingers (pseudo R-2 = 0 28) and intermediate amounts of variation in the other responses (pseudo R(2)s between 0.41 and 0.60). Many relationships of macroinvertebrate responses to anthropogenic measures and natural watershed attributes were nonlinear. Fish responses were related to system size and local habitat quality. 4. For impervious surface, models predicted below model-average macroinvertebrate richness at levels above c.3 0%, lower % EPT above c. 1 5%, and lower % Clingers for levels above c.2 0%. Impervious surface did not affect% Collectors or any fish response. Prediction functions for% EPT and fish richness increased linearly with log(10) (watershed area), % Tolerant Fish decreased with log(10) (watershed area), and benthic fish richness and biomass both increased nonlinearly with log(10) (watershed area). 5. Gradient boosting optimizes the predictive accuracy of GAMs while preserving the structure of conventional GAMs, so that predictor-response relationships are more interpretable than with other machine learning methods. Boosting also avoids overfitting the data (by shrinking effect estimates towards zero and by performing variable selection), thus avoiding spurious predictor effects C1 [Maloney, Kelly O.; Weller, Donald E.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. [Maloney, Kelly O.] USGS, Leetown Sci Ctr, No Appalachian Res Lab, Wellsboro, PA 16901 USA. [Schmid, Matthias] Univ Erlangen Nurnberg, Dept Med Informat Biometry & Epidemiol, D-91054 Erlangen, Germany. RP Maloney, KO (reprint author), Smithsonian Environm Res Ctr, 647 Contees Wharf Rd,POB 28, Edgewater, MD 21037 USA. EM kmaloney@usgs.gov OI Weller, Donald/0000-0002-7629-5437 FU Smithsonian Institution; US Environmental Protection Agency National Center for Environmental Research (NCER) [R831369]; Interdisciplinary Center for Clinical Research (IZKF) at the University Hospital of the University of Erlangen-Nuremberg [J11] FX We thank the Maryland Department of Natural Resources for providing the MBSS data; Sergej Potapov for providing code to produce the marginal spatial effect plots and Mark Minton, Barbara St John White, Lori Davias, Eric Lind, Jana McPherson and three anonymous reviewers for comments that greatly improved the manuscript. Funding was provided by a Smithsonian Institution Postdoctoral Fellowship awarded to KOM and by the US Environmental Protection Agency National Center for Environmental Research (NCER) Science to Achieve Results (STAR) grant #R831369. The work of MS was supported by the Interdisciplinary Center for Clinical Research (IZKF) at the University Hospital of the University of Erlangen-Nuremberg (Project J11). Use of trade, product or firm names does not imply endorsement by the U.S. Government. NR 53 TC 10 Z9 10 U1 3 U2 44 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 2041-210X EI 2041-2096 J9 METHODS ECOL EVOL JI Methods Ecol. Evol. PD FEB PY 2012 VL 3 IS 1 BP 116 EP 128 DI 10.1111/j.2041-210X.2011.00124.x PG 13 WC Ecology SC Environmental Sciences & Ecology GA 884SK UT WOS:000299728300014 ER PT J AU Gratwicke, B Lovejoy, TE Wildt, DE AF Gratwicke, Brian Lovejoy, Thomas E. Wildt, David E. TI Will Amphibians Croak under the Endangered Species Act? SO BIOSCIENCE LA English DT Article DE amphibian; conservation; funding; Endangered Species Act; prioritization ID CHYTRID FUNGUS; CONSERVATION; EXTINCTIONS; POPULATION; RECOVERY; BIODIVERSITY; PRIORITIES; DECLINES; EXPENDITURES; WIDESPREAD AB Herpetologists often complain that, despite amphibians' being one of the most threatened vertebrate classes, there is a dearth of funding and capacity to tackle the global crisis afflicting them. We compared the average funding per species listed under the US Endangered Species Act (ESA) to quantify funding favoritism across vertebrate classes in the United States and compared ESA listings with NatureServe evaluations of endangerment in order to examine listing bias. We found that, on average, listed US amphibians receive one-quarter of the ESA funding that other vertebrate classes do. This inequality is compounded by listing bias, with 82% of the amphibians found to be at risk by NatureServe remaining unlisted under the ESA. We recommend that federal, state, and private conservation groups take reactive and proactive measures to build capacity to sustain this important class of vertebrates for future generations. C1 [Gratwicke, Brian; Wildt, David E.] Ctr Species Survival, Smithsonian Conservat Biol Inst, Washington, DC USA. [Lovejoy, Thomas E.] H John Heinz III Ctr Sci Econ & Environm, Washington, DC USA. RP Gratwicke, B (reprint author), Ctr Species Survival, Smithsonian Conservat Biol Inst, Washington, DC USA. EM brian.gratwicke@gmail.com NR 53 TC 8 Z9 8 U1 3 U2 27 PU AMER INST BIOLOGICAL SCI PI WASHINGTON PA 1444 EYE ST, NW, STE 200, WASHINGTON, DC 20005 USA SN 0006-3568 J9 BIOSCIENCE JI Bioscience PD FEB PY 2012 VL 62 IS 2 BP 197 EP 202 DI 10.1525/bio.2012.62.2.13 PG 6 WC Biology SC Life Sciences & Biomedicine - Other Topics GA 890DJ UT WOS:000300125000012 ER PT J AU Fuentes, B Dixon, E Mora, MD Turner, BL Bol, R AF Fuentes, Barbara Dixon, Elizabeth de la Luz Mora, Maria Turner, Benjamin L. Bol, Roland TI Dissolved phosphorus composition of grassland leachates following application of dairy-slurry size fractions SO JOURNAL OF PLANT NUTRITION AND SOIL SCIENCE LA English DT Article DE dairy slurry; leachate; dissolved P; total P; reactive P; unreactive P; dissolved organic carbon; grassland; 31P-nuclear magnetic-resonance spectroscopy ID MAGNETIC-RESONANCE-SPECTROSCOPY; P-31 NMR-SPECTROSCOPY; ORGANIC PHOSPHORUS; SOIL; CATTLE; MANURE; WATER; DUNG; SEPARATION; SPECIATION AB Appropriate management of P from slurry can increase crop production and decrease nutrient loss to water bodies. The present study examined how the application of different size fractions of dairy slurry influenced the quantity and composition of P leached from grassland in a temperate climate. Soil blocks were amended (day 0 = start of the experiment) with either whole slurry (WS), the > 425 mu m fraction (coarse slurry fraction, CSF), the <45 mu m slurry fraction (fine liquid slurry fraction, FLF), or not amended, i.e., the control soil (CON). Deionized water was added to the soil blocks to simulate six sequential rainfall events, equivalent to 250 mm (day 0.2, 1.2, 4.2, 11.2) or 500 mm of rainfall (day 18.2 and 25.2), with leachates collected the following day. The results showed that total dissolved P (TDP), dissolved reactive P (DRP), dissolved unreactive P (DUP), orthophosphate, phosphomonoester, and pyrophosphate concentrations generally decreased with the increasing number of simulated rain events. Total dissolved P was leached in the following order WS > FLF approximate to CSF > CON. Dissolved organic C was correlated with TDP, DRP, and DUP in leachates of all treatments. The highest concentrations of dissolved phosphomonoesters and pyrophosphate (147 mu g P L-1 and 57 mu g PL-1, respectively) were detected using solution 31P-NMR spectroscopy in the WS leachates. Overall, there were significant differences observed between slurry treatments (e.g., relative contributions of inorganic P vs. organic P of dissolved P in leachates). Differences were independent from the rate at which slurry P was applied, because the highest dissolved P losses per unit of slurry P applied were measured in the FLF, i.e., the treatment that received the smallest amount of P. We conclude that the specific particle-size composition of applied slurry influences dissolved P losses from grassland systems. This information should be taken in account in farm-management approaches which aim to minimizing dissolved slurry P losses from grassland systems. C1 [Dixon, Elizabeth; Bol, Roland] Rothamsted Res N Wyke, Sustainable Soils & Grassland Syst Dept, Okehampton EX20 2SB, Devon, England. [de la Luz Mora, Maria] Univ La Frontera, Dept Ciencias Quim, Temuco, Chile. [Turner, Benjamin L.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. [Fuentes, Barbara] Univ La Frontera, Programa Doctorado Ciencias Recursos Nat, Temuco, Chile. [Fuentes, Barbara] Univ Catolica Norte, Dept Ingn Quim, Antofagasta, Chile. RP Bol, R (reprint author), Rothamsted Res N Wyke, Sustainable Soils & Grassland Syst Dept, Okehampton EX20 2SB, Devon, England. EM roland.bol@rothamsted.ac.uk RI Turner, Benjamin/E-5940-2011; bol, roland/H-9324-2013 OI Turner, Benjamin/0000-0002-6585-0722; FU Fundacion Andes of Chile [C14055, FRO-0309]; CONICYT [AT-2406027]; UK Biotechnology and Biological Sciences Research Council (BBSRC) FX The project was supported by funding from the Fundacion Andes of Chile (Project C14055, Mecesup Grant FRO-0309, CONICYT Grant AT-2406027). We thank Alex Blumenfeld for analytical support. Rothamsted, North Wyke and the Cross Institute Programme on Sustainable Soil Function (Soil-CIP) are supported by core funding from the UK Biotechnology and Biological Sciences Research Council (BBSRC). NR 36 TC 8 Z9 8 U1 0 U2 30 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 1436-8730 J9 J PLANT NUTR SOIL SC JI J. Plant Nutr. Soil Sci. PD FEB PY 2012 VL 175 IS 1 BP 78 EP 85 DI 10.1002/jpln.201100126 PG 8 WC Agronomy; Plant Sciences; Soil Science SC Agriculture; Plant Sciences GA 888JH UT WOS:000299999300011 ER PT J AU Ishtiaq, F Beadell, JS Warren, BH Fleischer, RC AF Ishtiaq, Farah Beadell, Jon S. Warren, Ben H. Fleischer, Robert C. TI Diversity and distribution of avian haematozoan parasites in the western Indian Ocean region: a molecular survey SO PARASITOLOGY LA English DT Article DE Africa; Haemoproteus; haematozoan parasites; western Indian Ocean; Plasmodium ID ISLAND COLONIZATION HISTORY; BLOOD PARASITES; MALARIA PARASITES; EVOLUTIONARY RELATIONSHIPS; CYANISTES-CAERULEUS; HOST-SPECIFICITY; LESSER ANTILLES; BLUE TITS; PREVALENCE; BIRDS AB The genetic diversity of haematozoan parasites in island avifauna has only recently begun to be explored, despite the potential insight that these data can provide into the history of association between hosts and parasites and the possible threat posed to island endemics. We used mitochondrial DNA sequencing to characterize the diversity of 2 genera of vector-mediated parasites (Plasmodium and Haemoproteus) in avian blood samples from the western Indian Ocean region and explored their relationship with parasites from continental Africa. We detected infections in 68 out of 150 (45.3%) individuals and cytochrome b sequences identified 9 genetically distinct lineages of Plasmodium spp. and 7 lineages of Haemoproteus spp. We found considerable heterogeneity in parasite lineage composition across islands, although limited sampling may, in part, be responsible for perceived differences. Two lineages of Plasmodium spp. and 2 lineages of Haemoproteus spp. were shared by hosts in the Indian Ocean and also on mainland Africa, suggesting that these lineages may have arrived relatively recently. Polyphyly of island parasites indicated that these parasites were unlikely to constitute an endemic radiation and instead probably represent multiple colonization events. This study represents the first molecular survey of vector-mediated parasites in the western Indian Ocean, and has uncovered a diversity of parasites. Full understanding of parasite community composition and possible threats to endemic avian hosts will require comprehensive surveys across the avifauna of this region. C1 [Ishtiaq, Farah; Beadell, Jon S.; Fleischer, Robert C.] Smithsonian Inst, Ctr Conservat & Evolutionary Genet, Washington, DC 20008 USA. [Warren, Ben H.] Univ La Reunion, CIRAD, UMR PVBMT C53, Ligne Paradis 97410, St Pierre, Reunion. RP Ishtiaq, F (reprint author), Smithsonian Inst, Ctr Conservat & Evolutionary Genet, Natl Zool Pk,3001 Connecticut Ave NW, Washington, DC 20008 USA. EM farahishtiaq@yahoo.com FU National Institutes of Health [1R01GM063258] FX This study was funded by the National Institutes of Health grant no. 1R01GM063258. We thank C. McIntosh for facilitating laboratory analyses. We are grateful to S. Anli, T. Ghestemme, C. Moussa, Iboura, R. Nichols, F. Ratrimomanarivo and I. Said for help in the field in the Indian Ocean. We also thank the following Indian Ocean organizations for granting permission and logistical support for the fieldwork: CNDRS, CNDRS d'Anjouan, Conservation de la Biodiversite Moheli, DAF-SEF, MEF Madagascar, MHN La Reunion, MICET, MNPCS, MWF, Nature Seychelles, SBS, SDOE, SEOR and SIF. NR 59 TC 8 Z9 8 U1 0 U2 18 PU CAMBRIDGE UNIV PRESS PI NEW YORK PA 32 AVENUE OF THE AMERICAS, NEW YORK, NY 10013-2473 USA SN 0031-1820 EI 1469-8161 J9 PARASITOLOGY JI Parasitology PD FEB PY 2012 VL 139 IS 2 BP 221 EP 231 DI 10.1017/S0031182011001831 PG 11 WC Parasitology SC Parasitology GA 887LV UT WOS:000299929800006 PM 22075855 ER PT J AU Fesen, RA Kremer, R Patnaude, D Milisavljevic, D AF Fesen, Robert A. Kremer, Richard Patnaude, Daniel Milisavljevic, Dan TI THE SN 393-SNR RX J1713.7-3946 (G347.3-0.5) CONNECTION SO ASTRONOMICAL JOURNAL LA English DT Article DE ISM: individual objects (G347.3-0.5); ISM: supernova remnants; supernovae: general ID TYCHOS SUPERNOVA-REMNANT; X-RAY-EMISSION; ABSOLUTE MAGNITUDE DISTRIBUTIONS; LIGHT CURVES; CRAB-NEBULA; HISTORICAL SUPERNOVAE; PARTICLE-ACCELERATION; INTERSTELLAR-MEDIUM; HUBBLE CONSTANT; IA SUPERNOVAE AB Although the connection of the Chinese "guest" star of 393 AD with the Galactic supernova remnant RX J1713.7-3946 (G347.3-0.5) made by Wang et al. in 1997 is consistent with the remnant's relatively young properties and the guest star's projected position within the "tail" of the constellation Scorpius, there are difficulties with such an association. The brief Chinese texts concerning the 393 AD guest star make no comment about its apparent brightness, stating only that it disappeared after eight months. However, at the remnant's current estimated 1-1.3 kpc distance and A(V) similar or equal to 3, its supernova (SN) should have been a visually bright object at maximum light (-3.5 to -5.0 mag) if M-V = -17 to -18 and would have remained visible for over a year. The peak brightness similar or equal to 0 mag adopted by Wang et al. and others would require the RX J1713.7-3946 supernova to have been a very subluminous event similar to or fainter than SN 2005cs in M51. We also note problems connecting SN 393 with a European record in which the Roman poet Claudian describes a visually brilliant star in the heavens around 393 AD that could be readily seen even in midday. Although several authors have suggested this account may be a reference to the Chinese supernova of 393, Scorpius would not be visible near midday in March when the Chinese first reported the 393 guest star. We review both the Chinese and Roman accounts and calculate probable visual brightnesses for a range of SN subtypes and conclude that neither the Chinese nor the Roman descriptions are easily reconciled with an expected RX J1713.7-3946 supernova brightness and duration. C1 [Fesen, Robert A.; Milisavljevic, Dan] Dartmouth Coll, Dept Phys & Astron, Hanover, NH 03755 USA. [Kremer, Richard] Dartmouth Coll, Dept Hist, Hanover, NH 03755 USA. [Patnaude, Daniel] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Fesen, RA (reprint author), Dartmouth Coll, Dept Phys & Astron, 6127 Wilder Lab, Hanover, NH 03755 USA. NR 90 TC 10 Z9 10 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 FEB PY 2012 VL 143 IS 2 AR 27 DI 10.1088/0004-6256/143/2/27 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 885TL UT WOS:000299803600002 ER PT J AU Strader, J Seth, AC Caldwell, N AF Strader, Jay Seth, Anil C. Caldwell, Nelson TI OLD MASSIVE GLOBULAR CLUSTERS AND THE STELLAR HALO OF THE DWARF STARBURST GALAXY NGC 4449 SO ASTRONOMICAL JOURNAL LA English DT Article DE galaxies: evolution; galaxies: formation; galaxies: individual (NGC 4449); galaxies: star clusters: general; globular clusters: general ID HUBBLE-SPACE-TELESCOPE; DIGITAL SKY SURVEY; RED GIANT STARS; POPULATION SYNTHESIS; ADVANCED CAMERA; SPHEROIDAL GALAXY; SPIRAL GALAXIES; ACS SURVEY; MILKY-WAY; FORMATION EFFICIENCIES AB We use Hubble Space Telescope imaging to show that the nearby dwarf starburst galaxy NGC 4449 has an unusual abundance of luminous red star clusters. Joint constraints from integrated photometry, low-resolution spectroscopy, dynamical mass-to-light ratios, and resolved color magnitude diagrams provide evidence that some of these clusters are old globular clusters (GCs). Spectroscopic data for two massive clusters suggest intermediate metallicities ([Fe/H] similar to -1) and subsolar Mg enhancement ([Mg/Fe] similar to -0.1 to -0.2). One of these clusters may be the nucleus of a tidally disrupting dwarf galaxy; the other is very massive (similar to 3 x 10(6) M-circle dot). We have also identified a population of remote halo GCs. NGC 4449 is consistent with an emerging picture of the ubiquity of stellar halos among dwarf galaxies, and study of its GCs may help distinguish between accretion and in situ scenarios for such halos. C1 [Strader, Jay; Seth, Anil C.; Caldwell, Nelson] Harvard Smithsonian Ctr Astrophys, Dept Phys & Astron, Cambridge, MA 02138 USA. [Seth, Anil C.] Univ Utah, Salt Lake City, UT 84112 USA. RP Strader, J (reprint author), Harvard Smithsonian Ctr Astrophys, Dept Phys & Astron, 60 Garden St, Cambridge, MA 02138 USA. EM jstrader@cfa.harvard.edu FU Smithsonian Astrophysical Observatory; NASA FX We thank David Sand for help with data acquisition. We thank Susan Tokarz for help with the spectroscopic data reduction, and Perry Berlind and Michael Calkins for help acquiring the data. Ricardo Schiavon helped us to operate his EZ_Ages program. Some of the observations reported here were obtained at the MMT Observatory, a joint facility of the Smithsonian Institution and the University of Arizona. This paper uses data products produced by the OIR Telescope Data Center, supported by the Smithsonian Astrophysical Observatory. Based on observations made with the NASA/ESA Hubble Space Telescope, and obtained from the Hubble Legacy Archive, which is a collaboration between the Space Telescope Science Institute (STScI/NASA), the Space Telescope European Coordinating Facility (ST-ECF/ESA), and the Canadian Astronomy Data Centre (CADC/NRC/CSA). This work is based in part on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. This research has made use of the NASA/IPAC Infrared Science Archive, which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the NASA. We thank the anonymous referee for a helpful report. NR 74 TC 5 Z9 5 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 J9 ASTRON J JI Astron. J. PD FEB PY 2012 VL 143 IS 2 AR 52 DI 10.1088/0004-6256/143/2/52 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 885TL UT WOS:000299803600027 ER PT J AU Gotelli, NJ Chao, A Colwell, RK Hwang, WH Graves, GR AF Gotelli, Nicholas J. Chao, Anne Colwell, Robert K. Hwang, Wen-Han Graves, Gary R. TI Specimen-Based Modeling, Stopping Rules, and the Extinction of the Ivory-Billed Woodpecker SO CONSERVATION BIOLOGY LA English DT Article DE avian censuses; Campephilus principalis; extinction estimation; extinction probability; Ivory-billed Woodpecker; museum specimens; species richness estimators; stopping rules; Campephilus principalis; censos aviares; especimenes de museo; estimacion de la probabilidad de extincion; estimadores de la riqueza de especies; reglas de decision ID CONTINENTAL NORTH-AMERICA; INFERRING EXTINCTION; SIGHTING RECORD; ERADICATION; COLLECTIONS; POPULATION AB Assessing species survival status is an essential component of conservation programs. We devised a new statistical method for estimating the probability of species persistence from the temporal sequence of collection dates of museum specimens. To complement this approach, we developed quantitative stopping rules for terminating the search for missing or allegedly extinct species. These stopping rules are based on survey data for counts of co-occurring species that are encountered in the search for a target species. We illustrate both these methods with a case study of the Ivory-billed Woodpecker (Campephilus principalis), long assumed to have become extinct in the United States in the 1950s, but reportedly rediscovered in 2004. We analyzed the temporal pattern of the collection dates of 239 geo-referenced museum specimens collected throughout the southeastern United States from 1853 to 1932 and estimated the probability of persistence in 2011 as <6.4 x 10(-5), with a probable extinction date no later than 1980. From an analysis of avian census data (counts of individuals) at 4 sites where searches for the woodpecker were conducted since 2004, we estimated that at most 13 undetected species may remain in 3 sites (one each in Louisiana, Mississippi, Florida). At a fourth site on the Congaree River (South Carolina), no singletons (species represented by one observation) remained after 15,500 counts of individual birds, indicating that the number of species already recorded (56) is unlikely to increase with additional survey effort. Collectively, these results suggest there is virtually no chance the Ivory-billed Woodpecker is currently extant within its historical range in the southeastern United States. The results also suggest conservation resources devoted to its rediscovery and recovery could be better allocated to other species. The methods we describe for estimating species extinction dates and the probability of persistence are generally applicable to other species for which sufficient museum collections and field census results are available. C1 [Gotelli, Nicholas J.] Univ Vermont, Dept Biol, Burlington, VT 05405 USA. [Chao, Anne] Natl Tsing Hua Univ, Inst Stat, Hsinchu 30043, Taiwan. [Colwell, Robert K.] Univ Connecticut, Dept Ecol & Evolutionary Biol, Storrs, CT 06269 USA. [Hwang, Wen-Han] Natl Chung Hsing Univ, Dept Appl Math, Taichung 402, Taiwan. [Graves, Gary R.] Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Washington, DC 20013 USA. [Graves, Gary R.] Univ Copenhagen, Ctr Macroecol Evolut & Climate, DK-1168 Copenhagen, Denmark. RP Gotelli, NJ (reprint author), Univ Vermont, Dept Biol, Burlington, VT 05405 USA. EM ngotelli@uvm.edu RI Colwell, Robert/C-7276-2015; publist, CMEC/C-3010-2012; publicationpage, cmec/B-4405-2017 FU U.S. National Science Foundation; Taiwan National Science Council; Alexander Wetmore Fund; Smithsonian Institution; Center for Macroecology, Evolution, and Climate, University of Copenhagen; National Center for Ecological Analysis and Synthesis; National Science Foundation; University of California, Santa Barbara; State of California FX We thank S. Haber and P. Sweet for providing information on Ivory-billed Woodpecker specimens in the American Museum of Natural History, C. Elphick for extensive comments on the manuscript, and M. Rivadeneira and K. Roy for help in understanding their related work. N.J.G. and R. K. C. were supported by the U.S. National Science Foundation. A. C. and W. H. were funded by the Taiwan National Science Council. G. R. G. was supported by the Alexander Wetmore Fund, Smithsonian Institution, and the Center for Macroecology, Evolution, and Climate, University of Copenhagen. This study is a contribution of the Synthetic Macroecological Models of Species Diversity Working Group supported by the National Center for Ecological Analysis and Synthesis, a Center funded by the National Science Foundation, the University of California, Santa Barbara, and the State of California. NR 47 TC 7 Z9 7 U1 3 U2 45 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0888-8892 J9 CONSERV BIOL JI Conserv. Biol. PD FEB PY 2012 VL 26 IS 1 BP 47 EP 56 DI 10.1111/j.1523-1739.2011.01715.x PG 10 WC Biodiversity Conservation; Ecology; Environmental Sciences SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 881FS UT WOS:000299468600008 PM 21797923 ER PT J AU Fusco, G Garland, T Hunt, G Hughes, NC AF Fusco, Giuseppe Garland, Theodore, Jr. Hunt, Gene Hughes, Nigel C. TI DEVELOPMENTAL TRAIT EVOLUTION IN TRILOBITES SO EVOLUTION LA English DT Article DE Evolutionary trends; fossil arthropods; growth; molt cycle; ontogeny; phylogenetic signal ID WITHIN-SPECIES VARIATION; PHYLOGENETIC SIGNAL; GROWTH; SEGMENTATION; ONTOGENY; LARVAE; SYSTEMATICS; ADAPTATION; ERROR; SIZE AB We performed a tree-based analysis of trilobite postembryonic development in a sample of 60 species for which quantitative data on segmentation and growth increments between putative successive instars are available, and that spans much of the temporal, phylogenetic, and habitat range of the group. Three developmental traits were investigated: the developmental mode of trunk segmentation, the average per-molt growth rate, and the conformity to a constant per-molt growth rate (Dyar's rule), for which an original metric was devised. Growth rates are within the normal range with respect to other arthropods and show overall conformity to Dyar's rule. Randomization tests indicate statistically significant phylogenetic signal for growth in early juveniles but not in later stages. Among five evolutionary models fit via maximum likelihood, one in which growth rates vary independently among species, analogous to Brownian motion on a star phylogeny, is the best supported in all ontogenetic stages, although a model with a single, stationary peak to which growth rates are attracted also garners nontrivial support. These results are not consistent with unbounded, Brownian-motion-like evolutionary dynamics, but instead suggest the influence of an adaptive zone. Our results suggest that developmental traits in trilobites were relatively labile during evolutionary history. C1 [Fusco, Giuseppe] Univ Padua, Dept Biol, I-35100 Padua, Italy. [Garland, Theodore, Jr.] Univ Calif Riverside, Dept Biol, Riverside, CA 92521 USA. [Hunt, Gene] Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20560 USA. [Hughes, Nigel C.] Univ Calif Riverside, Dept Earth Sci, Riverside, CA 92521 USA. RP Fusco, G (reprint author), Univ Padua, Dept Biol, I-35100 Padua, Italy. EM nigel.hughes@ucr.edu RI Hunt, Gene/B-3783-2010 OI Hunt, Gene/0000-0001-6430-5020 FU NSF [EAR-0616574] FX NSF EAR-0616574 supported this work. We thank R. M. Owens and F. A. Sundberg for taxonomic advice, P. Dai Pra for help with AGI and IDC statistics, and B. Chatterton, M. Webster, and the editors for insightful comments during review. NR 51 TC 13 Z9 13 U1 0 U2 14 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0014-3820 EI 1558-5646 J9 EVOLUTION JI Evolution PD FEB PY 2012 VL 66 IS 2 BP 314 EP 329 DI 10.1111/j.1558-5646.2011.01447.x PG 16 WC Ecology; Evolutionary Biology; Genetics & Heredity SC Environmental Sciences & Ecology; Evolutionary Biology; Genetics & Heredity GA 882FG UT WOS:000299547200002 PM 22276531 ER PT J AU Goldbogen, JA Calambokidis, J Croll, DA McKenna, MF Oleson, E Potvin, J Pyenson, ND Schorr, G Shadwick, RE Tershy, BR AF Goldbogen, Jeremy A. Calambokidis, John Croll, Donald A. McKenna, Megan F. Oleson, Erin Potvin, Jean Pyenson, Nicholas D. Schorr, Greg Shadwick, Robert E. Tershy, Bernie R. TI Scaling of lunge-feeding performance in rorqual whales: mass-specific energy expenditure increases with body size and progressively limits diving capacity SO FUNCTIONAL ECOLOGY LA English DT Article DE allometry; balaenopteridae; diving; drag; energetics; engulfment; filter feeding; rorqual; scaling; whale ID FIN WHALES; BLUE WHALES; HYDRODYNAMIC PERFORMANCE; MEGAPTERA-NOVAEANGLIAE; BALAENOPTERA-PHYSALUS; BALAENA-MYSTICETUS; FORAGING BEHAVIOR; MARINE MAMMALS; DIVE DURATION; NORTH PACIFIC AB 1. Diving capacity generally increases with body size both within and among taxanomic groups because of the differential scaling between body oxygen stores and metabolic rate. 2. Despite being some of the largest animals of all time, rorqual whales exhibit very short dive times relative to other large divers because of the high energetic costs incurred during lunge feeding. This mode of filter feeding requires high drag for the engulfment of large volumes of preyladen water, and the magnitude of both drag and engulfment volume is largely determined by the size and shape of the skull. 3. The positive allometry of rorqual skulls increases mass-specific engulfment capacity in larger whales, but the energetic requirements of feeding are also predicted to increase and thus further limit diving capacity. 4. To test the hypothesis that the energetic cost of a lunge is disproportionately higher in larger rorquals, we compared diving and lunge-feeding performance among three different-sized species (blue, fin and humpback whales) foraging on krill. 5. Our hydrodynamic analyses indicate that the mass-specific energy expenditure will increase with body size if rorquals lunge at length-specific speeds (in body lengths per second) that are independent of body size, a condition that is supported by tag data. 6. Although the absolute time required to filter each volume of water increased with body size, maximum dive duration and depth were not significantly different among species. As a consequence, the maximum number of lunges executed per dive decreased with body size. 7. These data suggest that, unlike all other true divers, adult rorqual species do not exhibit a positive relationship between body size and diving capacity. Larger rorquals forfeit diving capacity for greater engulfment capacity, a trade-off that favours the efficient exploitation of patchily dense prey aggregations. Such a trade-off may underlie different foraging strategies associated with resource partitioning, life history and ecological niche. C1 [Goldbogen, Jeremy A.; Calambokidis, John; Schorr, Greg] Cascadia Res Collect, Olympia, WA 98501 USA. [Croll, Donald A.] Univ Calif Santa Cruz, Ctr Ocean Hlth, Dept Ecol & Evolutionary Biol, Santa Cruz, CA 95060 USA. [McKenna, Megan F.; Tershy, Bernie R.] Univ Calif San Diego, Scripps Inst Oceanog, La Jolla, CA 92093 USA. [Oleson, Erin] Pacific Islands Fisheries Sci Ctr, Honolulu, HI 96822 USA. [Potvin, Jean] St Louis Univ, Dept Phys, St Louis, MO 63103 USA. [Pyenson, Nicholas D.] Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20013 USA. [Shadwick, Robert E.] Univ British Columbia, Dept Zool, Vancouver, BC, Canada. RP Goldbogen, JA (reprint author), Cascadia Res Collect, 2181-2 W 4th Ave, Olympia, WA 98501 USA. EM jgoldbogen@gmail.com OI Goldbogen, Jeremy/0000-0002-4170-7294 FU Smithsonian Institution; SIO; NMFS; CINMS; ONR FX J.A.G. thanks P.J. Ponganis for financial support and stimulating discussion during the writing of this manuscript in Cape Washington, Antarctica. We thank Kelly Newton for assistance in data preparation. N.D.P. was supported with funding from the Smithsonian Institution. We thank John Hildebrand for providing initial support through subcontracts from SIO for tagging operations. NMFS, CINMS and ONR also provided funding support on several aspects of tagging operations. We are indebted to Erin Falcone, Kelli Stingle, Jim Harvey and Alexei Calambokidis for assistance in the field. NR 73 TC 30 Z9 30 U1 4 U2 54 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0269-8463 EI 1365-2435 J9 FUNCT ECOL JI Funct. Ecol. PD FEB PY 2012 VL 26 IS 1 BP 216 EP 226 DI 10.1111/j.1365-2435.2011.01905.x PG 11 WC Ecology SC Environmental Sciences & Ecology GA 877SZ UT WOS:000299204300024 ER PT J AU Steinman, KJ O'Brien, JK Monfort, SL Robeck, TR AF Steinman, K. J. O'Brien, J. K. Monfort, S. L. Robeck, T. R. TI Characterization of the estrous cycle in female beluga (Delphinapterus leucas) using urinary endocrine monitoring and transabdominal ultrasound: Evidence of facultative induced ovulation SO GENERAL AND COMPARATIVE ENDOCRINOLOGY LA English DT Article DE White whale; Estrous cycle; Prolactin; Induced ovulation; Follicular ultrasonography ID BOTTLE-NOSED-DOLPHIN; FOLLICLE-STIMULATING-HORMONE; ELEPHANTS LOXODONTA-AFRICANA; WHALES ORCINUS-ORCA; ARTIFICIAL-INSEMINATION; TURSIOPS-TRUNCATUS; CAMELUS-DROMEDARIUS; LUTEINIZING-HORMONE; STEROID-HORMONES; OVARIAN ACTIVITY AB Recent, successful application of assisted reproductive technologies in captive beluga has resulted from the extensive study of male beluga reproductive biology. Optimization of assisted reproduction requires additional detailed knowledge of the female estrous cycle. Our specific objectives were to: (1) validate urinary immunoassays for use in this species; (2) elucidate annual ovarian cycle dynamics through the combined use of hormone excretion patterns and transabdominal ultrasound: and (3) establish whether ovulation in this species is spontaneous or induced by male factors. Ovulation was observed in four of 15 estrous cycles monitored in four adult female beluga maintained in a single-sex group. After introduction of a breeding male, ovulation was observed in six of seven estrous cycles. All estrous cycles occurred from March through June. For spontaneous ovulations (n = 4), the inter-estrous interval was 34 d (range 33-35 d), with a follicular phase length (FPL) of 25 +/- 8 d (mean +/- SD). For all ovulatory estrous cycles (with and without a breeding male), urinary estrogen conjugates (EC, 15.3 +/- 7.9 ng/mg Cr) and ovulatory luteinizing hormone (ovLH, 17.1 +/- 6.6 ng/mg Cr) concentrations both peaked on Day 0, and EC concentrations returned to baseline 8 +/- 7 d later. For non-conceptive cycles, urinary progestagen (Pg) concentrations increased on Day 0 (3.5 +/- 1.7 ng/mg Cr), peaked on Day + 19 (19.7 +/- 17.1 ng/mg Cr), and were elevated above baseline for 27 +/- 4 d. Preovulatory follicular diameter and circumference on Day -2 +/- 2 (range: Day -4 to -1) from peak EC were 2.5 +/- 0.7 and 7.8 +/- 1.3 cm, respectively. The FPL in non-ovulatory estrous cycles (n = 11) lasted 24 +/- 10 d and EC concentrations gradually declined to baseline over a 21 +/- 10 d interval following the EC peak (27.8 +/- 28.8 ng/mg Cr). Non-ovulatory estrous cycles were characterized by the absence of an ovLH surge and no concomitant increase in Pg concentrations above baseline excretion: the mean follicular diameter at or near peak EC was 3.1 +/- 0.8 cm on Day 2 +/- 3 d from peak EC (range: -1 to +5 days from peak EC). Overall, these data confirm that captive beluga exhibit reproductive seasonality and demonstrate that the species is a facultative-induced ovulator. (C) 2011 Elsevier Inc. All rights reserved. C1 [Steinman, K. J.; O'Brien, J. K.; Robeck, T. R.] SeaWorld & Busch Gardens Reprod Res Ctr, San Diego, CA 92109 USA. [Steinman, K. J.; Monfort, S. L.] Natl Zool Pk, Smithsonian Conservat Biol Inst, Front Royal, VA 22630 USA. RP Steinman, KJ (reprint author), SeaWorld & Busch Gardens Reprod Res Ctr, 2595 Ingraham St, San Diego, CA 92109 USA. EM Karen.Steinman@SeaWorld.com FU SeaWorld Parks and Entertainment, Inc. FX We thank the animal care laboratory, white whale and dolphin training, animal care and veterinary staff at SeaWorld San Antonio for their assistance and dedication to this study. For technical assistance, we thank Jessica Beckman-Kersey, Julia Nagel, and Sarah Putman at the Endocrine Research Laboratory at the Smithsonian Conservation Biology Institute For HPLC assistance and guidance, we thank Dr. David Kersey. Brad Andrews is also thanked for his continued support of this project. This study was funded by SeaWorld Parks and Entertainment, Inc. and is a SeaWorld technical contribution #2011-17-C. NR 61 TC 8 Z9 8 U1 4 U2 31 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0016-6480 EI 1095-6840 J9 GEN COMP ENDOCR JI Gen. Comp. Endocrinol. PD FEB 1 PY 2012 VL 175 IS 3 BP 389 EP 397 DI 10.1016/j.ygcen.2011.11.008 PG 9 WC Endocrinology & Metabolism SC Endocrinology & Metabolism GA 885UC UT WOS:000299805300004 PM 22134179 ER PT J AU Kornis, MS Mercado-Silva, N Vander Zanden, MJ AF Kornis, M. S. Mercado-Silva, N. Vander Zanden, M. J. TI Twenty years of invasion: a review of round goby Neogobius melanostomus biology, spread and ecological implications SO JOURNAL OF FISH BIOLOGY LA English DT Review DE Baltic Sea; Great Lakes; invasive species ID WESTERN LAKE-ERIE; DOUBLE-CRESTED CORMORANTS; ST-CLAIR RIVER; DIEL VERTICAL MIGRATION; BALLAST WATER EXCHANGE; LAURENTIAN GREAT-LAKES; GOBIID SPECIES PISCES; NON-INDIGENOUS FISH; UPPER DETROIT RIVER; BALTIC SEA AB The round goby Neogobius melanostomus is one of the most wide-ranging invasive fish on earth, with substantial introduced populations within the Laurentian Great Lakes watershed, the Baltic Sea and several major European rivers. Rapid expansion and deleterious ecosystem effects have motivated extensive research on this species; here this research is synthesized. Maps of the global distribution are provided and the invasion history of N. melanostomus, which spread more rapidly at first in North America, but has undergone substantial expansion over the past decade in the Baltic Sea, is summarized. Meta-analyses comparing their size at age, diet, competitors and predators in North American and European ecosystems are provided. Size at age is region specific, with saline habitats typically supporting larger and faster growing individuals than fresh water. Neogobius melanostomus prey differs substantially between regions, demonstrating a capacity to adapt to locally abundant food sources. Neogobius melanostomus comprise at least 50% of the diet of eight taxa in at least one site or life stage; in total, 16 predator taxa are documented from the Laurentian Great Lakes v. five from Eurasia. Invasive N. melanostomus are the only common forage fish to heavily exploit mussels in the Laurentian Great Lakes and the Baltic Sea, facilitating the transfer of energy from mussels to higher trophic levels in both systems. Neogobius melanostomus morphology, life history, reproduction, habitat preferences, environmental tolerances, parasites, environmental effects, sampling strategies and management are also discussed. Neogobius melanostomus inhabit a wide range of temperate freshwater and brackish-water ecosystems and will probably continue to spread via ballast water, accidental bait release and natural dispersal worldwide. Climate change will probably enhance N. melanostomus expansion by elevating water temperatures closer to its energetic optimum of 26 degrees C. Future research needs are presented; most pressing are evaluating the economic effects of N. melanostomus invasion, determining long-term population level effects of egg predation on game-fish recruitment and comparing several variables (density, ecological effects morphology and life history) among invaded ecosystems. This review provides a central reference as researchers continue studying N. melanostomus, often as examples for advancing basic ecology and invasion biology. C1 [Kornis, M. S.; Vander Zanden, M. J.] Univ Wisconsin, Ctr Limnol, Madison, WI 53706 USA. [Mercado-Silva, N.] Univ Arizona, Sch Nat Resources & Environm, Tucson, AZ 85721 USA. RP Kornis, MS (reprint author), Smithsonian Environm Res Ctr, 647 Contees Wharf Rd, Edgewater, MD 21037 USA. EM kornism@si.edu RI Gebauer, Radek/G-6749-2015 FU Wisconsin Sea Grant Institute; Wisconsin Department of Natural Resources FX We thank M. Lynch, J. Lyons and J. Janssen for their valuable insights on earlier versions of this manuscript and M. Kneuer, Illinois Natural History Survey, University of Illinois, for preparing the drawings in Fig. 1. Personal communications with D. Jude, T. Paoli, J. Borwick and M. Poos also aided in our review. Finally, we thank A. Benson, U.S. Geological Survey Nonindigenous Aquatic Species Database, for providing records of round gobies in the Great Lakes. This work was financially supported by the Wisconsin Sea Grant Institute and the Wisconsin Department of Natural Resources. NR 205 TC 134 Z9 138 U1 23 U2 288 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0022-1112 EI 1095-8649 J9 J FISH BIOL JI J. Fish Biol. PD FEB PY 2012 VL 80 IS 2 BP 235 EP 285 DI 10.1111/j.1095-8649.2011.03157.x PG 51 WC Fisheries; Marine & Freshwater Biology SC Fisheries; Marine & Freshwater Biology GA 879ZW UT WOS:000299374400001 PM 22268429 ER PT J AU Littler, MM Littler, DS AF Littler, Mark M. Littler, Diane S. TI BLOOM OF THE GIANT ANADYOMENE GIGANTODICTYON SP NOV (ANADYOMENACEAE, CLADOPHORALES) FROM THE OUTER SLOPE (25-50 m) OF THE BELIZE BARRIER REEF SO JOURNAL OF PHYCOLOGY LA English DT Article DE algal bloom Anadyomene; Anadyomenaceae; Anadyomene gigantodictyon; Belize Barrier Reef; Cladophorales ID TROPICAL WESTERN ATLANTIC; CORAL-REEFS; CHLOROPHYTA; SYSTEMATICS; ALGAE AB A giant form of Anadyomene, most similar to Anadyomene pavonina (J. Agardh) Wille, a rare and diminutive alga endemic to Florida, appeared as up to 10 m long net-like strands covering 10%80% of a 0.5 km region of the 2550 m deep Belizean outer reef slope where none had been present up to 12 months earlier. This new species, described herein as Anadyomene gigantodictyon Littler et D. S. Littler, is characterized by a unistratose blade or cluster of blades formed by the polychotomous branching of uniseriate veins, with the interstices, or spaces between the veins, completely or partially filled with cells that are smaller than those of the veins, with cylindrical to ovate cells. The cells at mid-blade are 1.72.0 mm in length and 0.20.3 mm diameter; interstitial cells are parallel and not juxtaposed. All cells are joined in one plane and form species-specific, fan-shaped patterns with secondary interstitial cells loosely or tightly woven. C1 [Littler, Mark M.; Littler, Diane S.] Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, Washington, DC 20013 USA. RP Littler, MM (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, MRC166,POB 37012, Washington, DC 20013 USA. EM littlerm@si.edu FU Caribbean Coral Reef Ecosystems Program; Smithsonian Marine Station at Fort Pierce; National Museum of Natural History FX We thank diving partners Barrett Brooks, Cameron Brooks, Antonio Baeza, and Carla Piantoni for their help in the field. Support for this study came from the Caribbean Coral Reef Ecosystems Program, the Smithsonian Marine Station at Fort Pierce (Valerie Paul, Head Scientist) and the National Museum of Natural History. NR 23 TC 2 Z9 2 U1 0 U2 4 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0022-3646 J9 J PHYCOL JI J. Phycol. PD FEB PY 2012 VL 48 IS 1 BP 60 EP 63 DI 10.1111/j.1529-8817.2011.01108.x PG 4 WC Plant Sciences; Marine & Freshwater Biology SC Plant Sciences; Marine & Freshwater Biology GA 884TB UT WOS:000299730600005 PM 27009650 ER PT J AU Hong, T AF Hong, Terry TI Forgotten Country SO LIBRARY JOURNAL LA English DT Book Review C1 [Hong, Terry] Smithsonian BookDragon, Washington, DC USA. RP Hong, T (reprint author), Smithsonian BookDragon, Washington, DC USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU REED BUSINESS INFORMATION PI NEW YORK PA 360 PARK AVENUE SOUTH, NEW YORK, NY 10010 USA SN 0363-0277 J9 LIBR J JI Libr. J. PD FEB 1 PY 2012 VL 137 IS 2 BP 55 EP 55 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA 883BW UT WOS:000299608600060 ER PT J AU Twite, JW Conselice, CJ Buitrago, F Noeske, K Weiner, BJ Acosta-Pulido, JA Bauer, AE AF Twite, Jonathan W. Conselice, Christopher J. Buitrago, Fernando Noeske, Kai Weiner, Benjamin J. Acosta-Pulido, Jose A. Bauer, Amanda E. TI Ha star formation rates in massive galaxies at z similar to 1 SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies: evolution; galaxies: formation; galaxies: star formation ID ACTIVE GALACTIC NUCLEI; DIGITAL SKY SURVEY; ALPHA LUMINOSITY FUNCTION; HIGH-REDSHIFT GALAXIES; AEGIS FIELD GALAXIES; GOODS-NICMOS SURVEY; SIMILAR-TO 2; FORMING GALAXIES; STELLAR MASS; FORMATION HISTORIES AB We present a near-infrared spectroscopic study of a stellar mass selected sample of galaxies at z similar to 1 utilizing the Long-slit Intermediate Resolution Infrared Spectrograph multi-object spectrograph on the William Herschel Telescope. We detect continuum, and the Ha line for our sample, which is one of the better direct tracers of star formation in external galaxies. We spectroscopically measure the Ha emission from 41 massive (M* > 1010.5 M?) galaxies taken from the POWIR Survey with spectroscopic redshifts 0.4 < zspec < 1.4. We correct our Ha fluxes for dust extinction by using multiwavelength data, and investigate star formation rate (SFR) trends with mass and colour. We find a drop in the fraction of massive galaxies with M* > 1011 M? which are detected in Ha emission at z < 0.9. We furthermore find that the fraction of galaxies with Ha emission drops steadily and significantly with redder (U-B) colours at z similar to 1, and that the specific SFR (SSFR) drops with increasing (U-B) colour for galaxies at all masses. By investigating the SFRmass relation, we find that the SFR is roughly constant with mass, in possible contrast to previous work, and that the SSFR is lower in the most massive galaxies. The scatter in the SFR versus mass relationship is very small for those systems with ongoing star formation, which suggests that star formation in the most massive galaxies at z similar to 1 shuts off rather abruptly over <1 Gyr, without an obvious gradual decline. We furthermore investigate the SFR as a function of (U-B) colour divided into different mass bins, revealing a tracer of the epoch of transition from star forming to passive, as a form of star formation downsizing. This suggests that the shut off of star formation occurs before the change in a galaxys colour. We find that galaxy stellar mass is the primary driving mechanism behind the star formation history for these galaxies and discuss several possible mechanisms for regulating this process. C1 [Twite, Jonathan W.; Conselice, Christopher J.; Buitrago, Fernando; Bauer, Amanda E.] Univ Nottingham, Sch Phys & Astron, Nottingham NG7 2RD, England. [Noeske, Kai] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Weiner, Benjamin J.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Acosta-Pulido, Jose A.] IAC, E-38205 San Cristobal la Laguna, Spain. [Acosta-Pulido, Jose A.] Univ La Laguna, Fac Fis, Dept Astrofis, E-38207 San Cristobal la Laguna, Spain. RP Twite, JW (reprint author), Univ Nottingham, Sch Phys & Astron, Nottingham NG7 2RD, England. EM ppxjwt@nottingham.ac.uk RI Conselice, Christopher/B-4348-2013; OI Buitrago, Fernando/0000-0002-2861-9812; Conselice, Christopher/0000-0003-1949-7638 FU University of Nottingham; STFC; Leverhulme Trust FX Funding for the trip to the Obseratorio del Roque de los Muchachos was provided by the University of Nottingham. We thank Nathan Bourne for useful and informative discussions. We acknowledge support from the STFC as well as a Leverhulme Trust Prize to CJC. The William Herschel Telescope is operated on the island of La Palma by the Isaac Newton Group in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias. NR 92 TC 9 Z9 9 U1 0 U2 3 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD FEB PY 2012 VL 420 IS 2 BP 1061 EP 1078 DI 10.1111/j.1365-2966.2011.20057.x PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 880OU UT WOS:000299417600010 ER PT J AU Kalkofen, W AF Kalkofen, Wolfgang TI The Validity of Dynamical Models of the Solar Atmosphere SO SOLAR PHYSICS LA English DT Article DE Abundances; Acoustic waves; Line profiles; Radiative transfer; Sun: photosphere, chromosphere, granulation ID QUIET-SUN; RADIATIVE-TRANSFER; ACOUSTIC-WAVES; LINE FORMATION; CONVECTION SIMULATIONS; SEMIEMPIRICAL MODELS; STELLAR ATMOSPHERES; MODERATE RESOLUTION; SURFACE CONVECTION; CHROMOSPHERE AB Important results on the structure and dynamics of the nonmagnetic solar chromosphere are based on hydrodynamic models that oversimplify either the geometry of the atmosphere or the interaction of radiation and matter. Although the observed granulation pattern is well reproduced by the three-dimensional (3D) models, oversimplification of radiative relaxation leads to the prediction of temperature fluctuations that are too high (by a factor of 10 to 100) and result in a monotonic decrease with height in the chromosphere of the horizontally and temporally averaged temperature, and hence in the prediction of absorption lines at wavelengths where only emission lines are observed on the Sun. New values of solar abundances of oxygen and other metals are based on 3D hydrodynamic models with temporal and spatial fluctuations that are far greater than those observed. These new abundances destroy the previous agreement of observed modes with acoustic eigenmodes that had been predicted for the old abundances from a solar model for which the sound speed throughout most of the Sun was determined to an accuracy of a few parts in 10(4). One expects that, when radiative relaxation is properly accounted for, 3D models will reproduce the essential characteristics of the solar atmosphere, among them a positive temperature gradient in the outward direction and hence exclusively emission lines in the extreme ultraviolet at all times and positions in the nonmagnetic chromosphere. A minimum characteristic length of 0.1 arcsec is identified for the solar atmosphere, below which there is no significant structure in the actual Sun, only in wave models of the Sun. This criticism does not detract from the notable success of hydrodynamic modeling to explain the mechanism by which chromospheric H-2V and K-2V bright points are formed. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Kalkofen, W (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM wkalkofen@cfa.harvard.edu NR 63 TC 5 Z9 5 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 FEB PY 2012 VL 276 IS 1-2 BP 75 EP 95 DI 10.1007/s11207-011-9898-z PG 21 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 878YX UT WOS:000299295100006 ER PT J AU Scott, JT Martens, PCH McKenzie, DE AF Scott, J. T. Martens, P. C. H. McKenzie, D. E. TI EUV Analysis of a Quasi-static Coronal Loop Structure SO SOLAR PHYSICS LA English DT Article DE Sun: corona; Sun: EUV; Sun: coronal loops; Doppler velocity; Non-thermal spectral line broadening ID TRANSITION-REGION; SOLAR CORONA; IMAGING SPECTROMETER; NONTHERMAL VELOCITIES; HINODE; TRACE; EXPLORER; DENSITY; STEREO; MODELS AB Decaying active region 10942 is investigated from 4:00 -aEuro parts per thousand 16:00 UT on 24 February 2007 using a suite of EUV observing instruments. Results from Hinode/EIS, STEREO and TRACE show that, although the active region has decayed and no sunspot is present, the physical mechanisms that produce distinguishable loop structures, spectral line broadening, and plasma flows still occur. A coronal loop that appears as a blue-shifted structure in Doppler maps is apparent in intensity images of log(T)=6.0 -aEuro parts per thousand 6.3 ions. The loop structure is found to be anti-correlated with spectral line broadening generally attributed to non-thermal velocities. This coronal loop structure is investigated physically (temperature, density, geometry) and temporally. Light curves created from imaging instruments show brightening and dimming of the loop structure on two different time scales; short pulses of 10 -aEuro parts per thousand 20 min and long duration dimming of two -aEuro parts per thousand four hours until its disappearance. The coronal loop structure, formed from relatively blue-shifted material that is anti-correlated with spectral line broadening, shows a density of 10(10) to 10(9.3) cm(-3) and is visible for longer than characteristic cooling times. The maximum non-thermal spectral line broadenings are found to be adjacent to the footpoint of the coronal loop structure. C1 [Scott, J. T.; Martens, P. C. H.; McKenzie, D. E.] Montana State Univ, Dept Phys, Bozeman, MT 59717 USA. [Martens, P. C. H.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Scott, JT (reprint author), Montana State Univ, Dept Phys, Bozeman, MT 59717 USA. EM scott@solar.physics.montana.edu FU NASA; UK institutions by Science & Technology Facility Council; German institutions by Deutsches Zentrum fur Luftund Raumfahrt e.V. (DLR); Belgian institutions by Belgian Science Policy Office; French institutions by Centre National d'Etudes Spatiales (CNES); Centre National de la Recherche Scientifique (CNRS); USAF Space Test Program; Office of Naval Research FX The STEREO/SECCHI data used here were produced by an international consortium of the Naval Research Laboratory (USA), Lockheed Martin Solar and Astrophysics Lab (USA), NASA Goddard Space Flight Center (USA), Rutherford Appleton Laboratory (UK), University of Birmingham (UK), Max-Planck-Institut for Solar System Research (Germany), Centre Spatiale de Liege (Belgium), Institut d'Optique Thorique et Appliquee (France), and Institut d'Astrophysique Spatiale (France). The USA institutions were funded by NASA, the UK institutions by the Science & Technology Facility Council (which used to be the Particle Physics and Astronomy Research Council, PPARC), the German institutions by Deutsches Zentrum fur Luftund Raumfahrt e.V. (DLR), the Belgian institutions by Belgian Science Policy Office, and the French institutions by Centre National d'Etudes Spatiales (CNES) and the Centre National de la Recherche Scientifique (CNRS). The NRL effort was also supported by the USAF Space Test Program and the Office of Naval Research. The Transition Region and Coronal Explorer (TRACE) is a mission of the Stanford-Lockheed Institute for Space Research, and part of the NASA Small Explorer program. NR 28 TC 3 Z9 3 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 FEB PY 2012 VL 276 IS 1-2 BP 113 EP 131 DI 10.1007/s11207-011-9885-4 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 878YX UT WOS:000299295100008 ER PT J AU Hartzell, JL Jordan, TE AF Hartzell, Jeanne L. Jordan, Thomas E. TI Shifts in the relative availability of phosphorus and nitrogen along estuarine salinity gradients SO BIOGEOCHEMISTRY LA English DT Article DE Phosphorus; Salinity; Pore water; Iron; Estuaries; Nitrogen ID FRESH-WATER; CHESAPEAKE BAY; LIMITING NUTRIENT; SEDIMENTS; EUTROPHICATION; PHOSPHATE; LIMITATION; RELEASE; LAKES; BRACKISH AB Phosphorus (P) availability in estuaries may increase with increasing salinity because sulfate from sea salt supports production of sulfide in sediments, which combines with iron (Fe) making it less available to sequester P. Increased P availability with increased salinity may promote the generally observed switch from P limitation of primary production in freshwater ecosystems to nitrogen (N) limitation in coastal marine waters. To investigate this hypothesis, we analyzed pore water from sediment cores collected along the salinity gradients of four Chesapeake Bay estuaries (the Patuxent, Potomac, Choptank, and Bush Rivers) with watersheds differing in land cover and physiography. At salinities of 1-4 in each estuary, abrupt decreases in pore water Fe(2+) concentrations coincided with increases in sulfate depletion and PO(4) (3-) concentrations. Peaks in water column PO(4) (3-) concentrations also occur at about the same position along the salinity gradient of each estuary. Increases in pore water PO(4) (3-) concentration with increasing salinity led to distinct shifts in molar NH(4) (+):PO(4) (3-) ratios from > 16 (the Redfield ratio characteristic of phytoplankton N:P) in the freshwater cores to < 16 in the cores with salinities > 1 to 4, suggesting that release of PO(4) (3-) from Fe where sediments are first deposited in sulfate-rich waters could promote the commonly observed switch from P limitation in freshwater to N limitation in mesohaline waters. Finding this pattern at similar salinities in four estuaries with such different watersheds suggests that it may be a fundamental characteristic of estuaries generally. C1 [Jordan, Thomas E.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. RP Hartzell, JL (reprint author), 75 Wilderness Court, Stafford, VA 22556 USA. EM jeannehartzell@comcast.net; jordanth@si.edu FU National Science Foundation [DEB-0235884]; United States Environmental Protection Agency (EPA) FX Funding was provided by National Science Foundation grant DEB-0235884 and the United States Environmental Protection Agency (EPA) Science to Achieve Results (STAR) Graduate Fellowship Program. Technical assistance was provided by Nancy Goff, Joseph Miklas, Marc Sigrist, and Kim Cone. Gregory Foster generously provided laboratory space and technical guidance. Jeffrey Cornwell was instrumental in helping obtain samples from the Choptank River. The suggestions of Donald Kelso, Gregory Foster, J. Patrick Megonigal, and two anonymous reviewers improved this paper. NR 42 TC 13 Z9 16 U1 5 U2 58 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0168-2563 J9 BIOGEOCHEMISTRY JI Biogeochemistry PD FEB PY 2012 VL 107 IS 1-3 BP 489 EP 500 DI 10.1007/s10533-010-9548-9 PG 12 WC Environmental Sciences; Geosciences, Multidisciplinary SC Environmental Sciences & Ecology; Geology GA 864GV UT WOS:000298226700030 ER PT J AU Greenberg, R Danner, R Olsen, B Luther, D AF Greenberg, Russell Danner, Raymond Olsen, Brian Luther, David TI High summer temperature explains bill size variation in salt marsh sparrows SO ECOGRAPHY LA English DT Article ID SHARP-TAILED SPARROWS; HEAT-LOSS; ALLENS RULE; BIRDS; RADIATION; SELECTION; FINCHES AB Physiological factors are rarely proposed to account for variation in the morphology of feeding structures. Recently, bird bills have been demonstrated to be important convective and radiant heat sinks. Larger bills have greater surface area than smaller bills and could serve as more effective thermoregulatory organs under hot conditions. The heat radiating function of bills should be more important in open habitats with little shade and stronger convective winds. Furthermore, as a means of dumping heat without increasing water loss through evaporation, bills might play a particularly important thermoregulatory role in heat loss in windy habitat where fresh water is limited. North American salt marshes provide a latitudinal gradient of relatively homogeneous habitat that is windy, open, and fresh-water limited. To examine the potential role of thermoregulation in determining bill size variation among ten species or subspecies of tidal marsh sparrows, we plotted bill size against maximum summer and minimum winter temperatures. Bill surface areas increases with summer temperature, which explained 82-89% of the variance (depending upon sex) when we controlled for genus membership. Latitude alone predicted bill surface area much more poorly than summer temperature, and winter temperatures explained < 10% of the variance in winter bill size. Tidal marsh sparrow bill morphology may, to a large degree, reflect the role of the bill in expelling excess body heat in these unbuffered, fresh-water-limited environments. This new example of Allen's rule reaffirms the importance of physiological constraints on the evolution of vertebrate morphologies, even in bird bills, which have conventionally been considered as products of adaptation to foraging niche. C1 [Greenberg, Russell] Smithsonian Migratory Bird Ctr, Smithsonian Conservar Biol Inst, Washington, DC 20008 USA. [Danner, Raymond] Virginia Tech, Blacksburg, VA 24061 USA. [Olsen, Brian] Univ Maine, Sch Biol & Ecol, Orono, ME 04469 USA. [Luther, David] George Mason Univ, Dept Biol, Fairfax, VA 22030 USA. RP Greenberg, R (reprint author), Smithsonian Migratory Bird Ctr, Smithsonian Conservar Biol Inst, Natl Zool Pk, Washington, DC 20008 USA. EM greenbergr@si.edu RI Danner, Raymond/J-8350-2013; OI Danner, Raymond/0000-0002-3999-8141; Olsen, Brian/0000-0001-5608-2779 NR 37 TC 23 Z9 23 U1 8 U2 44 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0906-7590 EI 1600-0587 J9 ECOGRAPHY JI Ecography PD FEB PY 2012 VL 35 IS 2 BP 146 EP 152 DI 10.1111/j.1600-0587.2011.07002.x PG 7 WC Biodiversity Conservation; Ecology SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 880ND UT WOS:000299413000006 ER PT J AU Craddock, RA AF Craddock, Robert A. TI Aeolian processes on the terrestrial planets: Recent observations and future focus SO PROGRESS IN PHYSICAL GEOGRAPHY LA English DT Article DE aeolian processes; basaltic particles; dunes; Mars; planetary geomorphology; Titan; Venus ID HAWAIIAN PALAGONITIC SOIL; LINEAR DUNES; OMEGA/MARS EXPRESS; SAND DUNES; MAGNETIC-PROPERTIES; LONGITUDINAL DUNES; RADAR OBSERVATIONS; SPECTRAL EVIDENCE; SIMPSON DESERT; CASSINI RADAR AB Aeolian dune fields have been described on Earth, Mars, Venus, and Titan. The amount and fidelity of data being returned from orbiting spacecraft and landers have enabled a new era in aeolian studies. This progress report presents an overview of the latest planetary geomorphic studies characterizing aeolian processes on extraterrestrial surfaces. Our understanding of aeolian processes on other planetary surfaces comes largely from Earth analog studies, along with wind tunnel experiments and theoretical modeling. However, an important difference is that unlike terrestrial dunes most dunes on Venus and Mars are composed primarily of basaltic particles. Additional research is needed to understand how basaltic particles weather both physically and chemically so that it will be possible to apply traditional sedimentological concepts, such as sediment maturity, to understanding aeolian processes on Venus and Mars. It may also be possible to characterize sediment maturity and provenance through remote sensing data once we have a better understanding of basaltic sediments. Although there have been a variety of dune forms identified on the surfaces of the other terrestrial planets, the only dune form found on all of them is linear dunes. Even though linear dunes are the most common dune forms on Earth, we currently have a poor understanding as to how they are formed, and additional work is needed to understand these features. C1 Smithsonian Inst, Natl Air & Space Museum, Ctr Earth & Planetary Studies, Washington, DC 20560 USA. RP Craddock, RA (reprint author), Smithsonian Inst, Natl Air & Space Museum, Ctr Earth & Planetary Studies, MRC 315, Washington, DC 20560 USA. EM craddockb@si.edu RI Craddock, Robert/B-3884-2013 FU NASA [NNX09AC27G]; Smithsonian Institution FX Support for the research that is presented in part has come from NASA's Mars Fundamental Research Program Grant NNX09AC27G and funds from the George F. Becker Endowment at the Smithsonian Institution. NR 108 TC 4 Z9 5 U1 0 U2 18 PU SAGE PUBLICATIONS LTD PI LONDON PA 1 OLIVERS YARD, 55 CITY ROAD, LONDON EC1Y 1SP, ENGLAND SN 0309-1333 EI 1477-0296 J9 PROG PHYS GEOG JI Prog. Phys. Geogr. PD FEB PY 2012 VL 36 IS 1 BP 110 EP 124 DI 10.1177/0309133311425399 PG 15 WC Geography, Physical; Geosciences, Multidisciplinary SC Physical Geography; Geology GA 878XT UT WOS:000299291200007 ER PT J AU Benson, RBJ Butler, RJ Carrano, MT O'Connor, PM AF Benson, Roger B. J. Butler, Richard J. Carrano, Matthew T. O'Connor, Patrick M. TI Air-filled postcranial bones in theropod dinosaurs: physiological implications and the reptile'-bird transition SO BIOLOGICAL REVIEWS LA English DT Article DE pneumaticity; osteological correlates; bird origins; Dinosauria; Theropoda ID REPUBLIC-OF-CHINA; SAUROPOD DINOSAURS; PREDATORY DINOSAUR; AVIAN FLIGHT; VERTEBRAL PNEUMATICITY; SKELETAL PNEUMATICITY; CORRELATED EVOLUTION; TENDAGURU SAUROPODS; CERVICAL-VERTEBRAE; RESPIRATORY SYSTEM AB Pneumatic (air-filled) postcranial bones are unique to birds among extant tetrapods. Unambiguous skeletal correlates of postcranial pneumaticity first appeared in the Late Triassic (approximately 210 million years ago), when they evolved independently in several groups of bird-line archosaurs (ornithodirans). These include the theropod dinosaurs (of which birds are extant representatives), the pterosaurs, and sauropodomorph dinosaurs. Postulated functions of skeletal pneumatisation include weight reduction in large-bodied or flying taxa, and density reduction resulting in energetic savings during foraging and locomotion. However, the influence of these hypotheses on the early evolution of pneumaticity has not been studied in detail previously. We review recent work on the significance of pneumaticity for understanding the biology of extinct ornithodirans, and present detailed new data on the proportion of the skeleton that was pneumatised in 131 non-avian theropods and Archaeopteryx. This includes all taxa known from significant postcranial remains. Pneumaticity of the cervical and anterior dorsal vertebrae occurred early in theropod evolution. This common pattern was conserved on the line leading to birds, and is likely present in Archaeopteryx. Increases in skeletal pneumaticity occurred independently in as many as 12 lineages, highlighting a remarkably high number of parallel acquisitions of a bird-like feature among non-avian theropods. Using a quantitative comparative framework, we show that evolutionary increases in skeletal pneumaticity are significantly concentrated in lineages with large body size, suggesting that mass reduction in response to gravitational constraints at large body sizes influenced the early evolution of pneumaticity. However, the body size threshold for extensive pneumatisation is lower in theropod lineages more closely related to birds (maniraptorans). Thus, relaxation of the relationship between body size and pneumatisation preceded the origin of birds and cannot be explained as an adaptation for flight. We hypothesise that skeletal density modulation in small, non-volant, maniraptorans resulted in energetic savings as part of a multi-system response to increased metabolic demands. Acquisition of extensive postcranial pneumaticity in small-bodied maniraptorans may indicate avian-like high-performance endothermy. C1 [Benson, Roger B. J.] Univ Cambridge, Dept Earth Sci, Cambridge CB2 3EQ, England. [Butler, Richard J.] Bayer Staatssammlung Palaontol & Geol, D-80333 Munich, Germany. [Carrano, Matthew T.] Smithsonian Inst, Washington, DC 20013 USA. [O'Connor, Patrick M.] Ohio Univ, Dept Biomed Sci, Athens, OH USA. RP Benson, RBJ (reprint author), Univ Cambridge, Dept Earth Sci, Cambridge CB2 3EQ, England. EM rbb27@cam.ac.uk RI Benson, Roger/A-1252-2011; Butler, Richard/A-5239-2011; OConnor, Patrick/I-9383-2012; Carrano, Matthew/C-7601-2011; OI Butler, Richard/0000-0003-2136-7541; OConnor, Patrick/0000-0002-6762-3806; Carrano, Matthew/0000-0003-2129-1612; Benson, Roger/0000-0001-8244-6177 FU Trinity College, Cambridge; Alexander von Humboldt Research Fellowship; Ohio University College of Osteopathic Medicine; Ohio Center for Ecology and Evolutionary Studies FX We thank P. Barrett, S. Brusatte and O. Rauhut for critical discussions and reading of an early version of the manuscript. G. Hunt provided methodological guidance and A. Balanoff, P. Makovicky, J. Choiniere and L. Zanno clarified the anatomy of some taxa. S. Hartman provided a skeletal illustration of Allosaurus (Figs 2I, 3). Mathew Wedel and an anonymous referee provided critical comments that improved the manuscript. William Foster and Alison Cooper provided invaluable editorial assistance. R.B.J.B. is funded by Trinity College, Cambridge. R.J.B. is funded by an Alexander von Humboldt Research Fellowship. P.M.O. is supported by the Ohio University College of Osteopathic Medicine and the Ohio Center for Ecology and Evolutionary Studies. This is Paleobiology Database official publication 130. NR 210 TC 49 Z9 51 U1 9 U2 73 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1464-7931 EI 1469-185X J9 BIOL REV JI Biol. Rev. PD FEB PY 2012 VL 87 IS 1 BP 168 EP 193 DI 10.1111/j.1469-185X.2011.00190.x PG 26 WC Biology SC Life Sciences & Biomedicine - Other Topics GA 871IU UT WOS:000298732300009 PM 21733078 ER PT J AU Price, CA Wing, S Weitz, JS AF Price, Charles A. Wing, Scott Weitz, Joshua S. TI Scaling and structure of dicotyledonous leaf venation networks SO ECOLOGY LETTERS LA English DT Article DE Allometry; biological networks; branching; characteristic scale; fractal; functional trait; scale free; scaling; venation network; xylem ID GENERAL-MODEL; HYDRAULIC ARCHITECTURE; WOODY-PLANTS; WBE MODEL; BIOLOGY; DESIGN; LEAVES; TREES; SIZE; ALLOMETRY AB There have been numerous attempts to derive general models for the structure and function of resource delivery networks in biology. Such theories typically predict the quantitative structure of vascular networks across scales. For example, fractal branching models of plant structure predict that the network dimensions within plant stems or leaves should be scale-free. However, very few empirical examples of such networks are available with which to evaluate such hypotheses. Here, we apply recently developed leaf network extraction software to a global leaf dataset. We find that leaf networks are neither entirely scale-free nor governed entirely by a characteristic scale. Indeed, we find many network properties, such as vein length distributions, which are governed by characteristic scales, and other network properties, notably vein diameter distributions, which are typified by power-law behaviour. Our findings suggest that theories of network structure will remain incomplete until they address the multiple constraints on network architecture. C1 [Price, Charles A.] Univ Western Australia, Sch Plant Biol, Perth, WA 6009, Australia. [Wing, Scott] Smithsonian Inst, Dept Paleobiol, Natl Museum Nat Hist, Washington, DC 20013 USA. [Weitz, Joshua S.] Georgia Inst Technol, Sch Biol, Atlanta, GA 30332 USA. [Weitz, Joshua S.] Georgia Inst Technol, Sch Phys, Atlanta, GA 30332 USA. RP Price, CA (reprint author), Univ Western Australia, Sch Plant Biol, Perth, WA 6009, Australia. EM charles.price@uwa.edu.au; jsweitz@gatech.edu RI Price, Charles/B-1171-2011; Weitz, Joshua/I-6696-2012; OI Weitz, Joshua/0000-0002-3433-8312; Wing, Scott/0000-0002-2954-8905 FU Defense Advanced Research Projects Agency [HR0011-05-1-0057]; Burroughs Welcome Fund FX C.A.P. and J.S.W. acknowledge the support of the Defense Advanced Research Projects Agency under grant HR0011-05-1-0057. J.S.W. holds a Career Award at the Scientific Interface from the Burroughs Welcome Fund. S. L. W. acknowledges Dane Miller, Ian Tom, Erika Gonzalez, and Smithsonian volunteers who photographed specimens for this project and have helped with conservation of the cleared leaf collection. John Raven and Cathy Price provided helpful comments on an earlier version of this manuscript. The authors thank the three anonymous reviewers for their valuable comments and suggestions. NR 50 TC 20 Z9 20 U1 6 U2 38 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1461-023X J9 ECOL LETT JI Ecol. Lett. PD FEB PY 2012 VL 15 IS 2 BP 87 EP 95 DI 10.1111/j.1461-0248.2011.01712.x PG 9 WC Ecology SC Environmental Sciences & Ecology GA 872YU UT WOS:000298848200001 PM 22093803 ER PT J AU McMichael, CH Bush, MB Piperno, DR Silman, MR Zimmerman, AR Anderson, C AF McMichael, Crystal H. Bush, Mark B. Piperno, Dolores R. Silman, Miles R. Zimmerman, Andrew R. Anderson, Christina TI Spatial and temporal scales of pre-Columbian disturbance associated with western Amazonian lakes SO HOLOCENE LA English DT Article DE charcoal; disturbance; fire history; phytoliths; pre-Columbian agriculture; western Amazonia ID BRAZILIAN AMAZON; CLIMATE-CHANGE; HOLOCENE FIRE; FOREST; LANDSCAPES; CHARCOAL; HISTORY; BIODIVERSITY; AMERICA; RECORD AB The history of landscape alteration in Amazonia by humans prior to the arrival of Europeans remains poorly understood. Estimates of human population size at the time of European contact vary by several million, and the trajectories of cultural and agricultural development are equally uncertain. The extent to which human populations altered Amazonian ecosystems is a function of population size, land management style, radius of influence of each subpopulation, and the temporal development of settlements. Here we report evidence that relates to the temporal and spatial scales of human disturbance in western Amazonia. Three lake sediment records and 94 terrestrial soil cores located 0-12 km from the adjacent lake were used to examine scales of pre-Columbian human impacts at two sites in western Amazonian forests. Lake sediment and soil charcoal records indicate discontinuous and localized burning around the study areas. Terrestrial soil phytolith and nutrient analyses reveal a range in disturbance intensity between the two sites but contain no evidence of large-scale forest clearing or anthropogenic soil enrichment. Our data suggest that while all of the settings examined were occupied or used, the halo of influence around each was limited. It should not be assumed that intensive landscape transformations by prehistoric human populations occurred throughout Amazonia or that Amazonian forests were resilient in the face of heavy historical disturbance. C1 [McMichael, Crystal H.] Florida Inst Technol, Dept Biol Sci, Melbourne, FL 32901 USA. [Piperno, Dolores R.] Smithsonian Natl Museum Nat Hist, Washington, DC USA. [Piperno, Dolores R.] Smithsonian Trop Res Inst, Panama City, Panama. [Silman, Miles R.] Wake Forest Univ, Winston Salem, NC 27109 USA. [Zimmerman, Andrew R.] Univ Florida, Gainesville, FL 32611 USA. RP McMichael, CH (reprint author), Florida Inst Technol, Dept Biol Sci, 150 W Univ Blvd, Melbourne, FL 32901 USA. EM cmcmicha@my.fit.edu OI Bush, Mark/0000-0001-6894-8613; Zimmerman, Andrew/0000-0001-5137-4916 FU NSF [DEB 0742301]; Florida Institute of Technology; Smithsonian National Museum of Natural History; Smithsonian Tropical Research Institute FX Field work and 14C dating of charcoal fragments was funded by NSF Ecology Program: award DEB 0742301. Other funding was provided by Florida Institute of Technology, Smithsonian National Museum of Natural History, including a Restricted Endowment and Small Grant Award, and Smithsonian Tropical Research Institute. NR 52 TC 29 Z9 29 U1 1 U2 27 PU SAGE PUBLICATIONS LTD PI LONDON PA 1 OLIVERS YARD, 55 CITY ROAD, LONDON EC1Y 1SP, ENGLAND SN 0959-6836 J9 HOLOCENE JI Holocene PD FEB PY 2012 VL 22 IS 2 BP 131 EP 141 DI 10.1177/0959683611414932 PG 11 WC Geography, Physical; Geosciences, Multidisciplinary SC Physical Geography; Geology GA 871OG UT WOS:000298746900001 ER PT J AU Dickau, R Bruno, MC Iriarte, J Prumers, H Betancourt, CJ Holst, I Mayle, FE AF Dickau, Ruth Bruno, Maria C. Iriarte, Jose Pruemers, Heiko Betancourt, Carla Jaimes Holst, Irene Mayle, Francis E. TI Diversity of cultivars and other plant resources used at habitation sites in the Llanos de Mojos, Beni, Bolivia: evidence from macrobotanical remains, starch grains, and phytoliths SO JOURNAL OF ARCHAEOLOGICAL SCIENCE LA English DT Article DE Archaeobotanical remains; Subsistence; Llanos de Mojos; Bolivian Amazon ID COB PHYTOLITHS; ORINOCO VALLEY; STONE TOOLS; MAIZE; DOMESTICATION; CUCURBITA; AGRICULTURE; NEOTROPICS; VENEZUELA; SOILS AB Although sparsely populated today, the Llanos de Mojos, Bolivia, sustained large sedentary societies in the Late Holocene (ca. 500 to 1400 AD). In order to gain insight into the subsistence of these people, we undertook macrobotanical and phytolith analyses of sediment samples, and starch grain and phytolith analyses of artifact residues, from four large habitation sites within this region. Macrobotanical remains show the presence of maize (lea mays), squash (Cucurbita sp.), peanut (Arachis hypogaea), cotton (Gossypium sp.), and palm fruits (Arecaceae). Microbotanical results confirm the widespread use of maize at all sites, along with manioc (Manihot esculenta), squash, and yam (Dioscorea sp.). These integrated results present the first comprehensive archaeobotanical evidence of the diversity of plants cultivated, processed, and consumed, by the pre-Hispanic inhabitants of the Amazonian lowlands of Bolivia. (C) 2011 Elsevier Ltd. All rights reserved. C1 [Dickau, Ruth; Iriarte, Jose] Univ Exeter, Dept Archaeol, Exeter EX4 4QE, Devon, England. [Bruno, Maria C.] Dickinson Coll, Dept Anthropol & Archaeol, Carlisle, PA 17013 USA. [Pruemers, Heiko; Betancourt, Carla Jaimes] KAAK, DAI, D-53173 Bonn, Germany. [Holst, Irene] Smithsonian Trop Res Inst, Balboa, Panama. [Mayle, Francis E.] Univ Edinburgh, Sch GeoSci, Inst Geog, Edinburgh EH8 9XP, Midlothian, Scotland. RP Dickau, R (reprint author), Univ Exeter, Dept Archaeol, Laver Bldg,N Pk Rd, Exeter EX4 4QE, Devon, England. EM rdickau@gmail.com; mcbruno@artsci.wustl.edu; j.iriarte@exeter.ac.uk; pruemers@kaak.dainst.de; carla.jaimesbetancourt@gmail.com; holsti@si.edu; Francis.Mayle@ed.ac.uk RI Iriarte, Jose /A-1141-2010; OI Iriarte, Jose/0000-0002-8155-5360 FU German Research Foundation (DFG); Leverhulme Trust [F/00 158/CH] FX Excavations at the Mendoza, Salvatierra, and Bella Vista sites, as well as macrobotanical analysis, were supported by the German Research Foundation (DFG). Microbotancial analyses were supported by Leverhulme Trust Research Grant F/00 158/CH. Dolores Piperno provided helpful comments on some of the phytolith identifications and macrobotanical remains. Bruce Bradley assisted with the descriptions of the stone tools. Thanks to Sonia Zarrillo for insightful discussions regarding methodology. Artifact illustrations were done by Sean Goddard and additional figure preparation by Michael Roulliard. Comparative plant material was generously provided by the 'Herbario Regional del Oriente Boliviano' at the Museo de Historia Natural 'Noel Kempff Mercado', Santa Cruz, Bolivia. We thank two anonymous reviewers for their constructive comments. NR 109 TC 21 Z9 22 U1 2 U2 17 PU ACADEMIC PRESS LTD- ELSEVIER SCIENCE LTD PI LONDON PA 24-28 OVAL RD, LONDON NW1 7DX, ENGLAND SN 0305-4403 J9 J ARCHAEOL SCI JI J. Archaeol. Sci. PD FEB PY 2012 VL 39 IS 2 BP 357 EP 370 DI 10.1016/j.jas.2011.09.021 PG 14 WC Anthropology; Archaeology; Geosciences, Multidisciplinary SC Anthropology; Archaeology; Geology GA 867OS UT WOS:000298464300014 ER PT J AU Tobin, MF Wright, AJ Mangan, SA Schnitzer, SA AF Tobin, Michael F. Wright, Alexandra J. Mangan, Scott A. Schnitzer, Stefan A. TI Lianas have a greater competitive effect than trees of similar biomass on tropical canopy trees SO ECOSPHERE LA English DT Article DE Barro Colorado; competition; liana cutting; Panama; plant-plant interactions; sap velocity; tropical forests ID BARRO-COLORADO ISLAND; HEAT PULSE METHOD; FOREST CANOPY; SAP FLOW; SILVICULTURAL TREATMENTS; DRY FOREST; GROWTH; WATER; REGENERATION; ACCLIMATION AB Lianas (woody vines) reduce growth and survival of host trees in both temperate and tropical forests; however, the relative strength of liana-tree competition in comparison to tree-tree competition remains unexplored. When controlling for biomass, lianas may have greater competitive effects than trees because the unique morphology of lianas allows them to reach the forest canopy at relatively small stem diameters and deploy a substantial crown above their host. We tested the hypothesis that lianas have a greater negative effect on canopy trees than do trees of similar biomass with a liana- and tree sapling-cutting experiment in a seasonal tropical moist forest in Panama. The response of canopy trees to the cutting treatments was characterized as the change in their daily water use by measuring their sap velocity before and after cutting. We compared the responses of canopy trees around which a similar biomass of either lianas or tree saplings had been cut to control trees with no cutting. Liana cutting increased canopy-tree sap velocity by -8% from before to after cutting relative to control trees during the dry season. In contrast, canopy-tree sap velocity did not respond to tree cutting, probably because trees with biomass similar to lianas were confined to the forest understory. We observed a similar pattern of sap velocity changes during the wet season, but treatment differences were not significant. Our results demonstrate that release from liana competition, but not tree competition, resulted in increased water transport in canopy trees, and suggests that relative to their biomass, lianas have greater competitive effects on canopy tree performance than do competing trees. C1 [Tobin, Michael F.; Wright, Alexandra J.; Mangan, Scott A.; Schnitzer, Stefan A.] Univ Wisconsin, Dept Biol Sci, Milwaukee, WI 53201 USA. [Mangan, Scott A.; Schnitzer, Stefan A.] Smithsonian Trop Res Inst, Balboa, Panama. RP Tobin, MF (reprint author), Calif State Univ Bakersfield, Dept Biol, Bakersfield, CA 93311 USA. EM miketobin@alumni.reed.edu OI Schnitzer, Stefan/0000-0002-2715-9455 FU University of Wisconsin-Milwaukee Research Growth Initiative and Graduate School; National Science Foundation [NSF-DEB 0613666, NSF-DEB 0845071] FX We thank Tom Kursar and Phyllis Coley for use of laboratory space and equipment, Vanessa Boukili and Lou Santiago for technical advice on sap flow system construction, and Kristen Becklund for assistance with probe assembly. Evelyn Sanchez, Al Domeyko and Gemma Rutten provided valuable assistance in the field, and David Brassfield assisted with tree identification. Smithsonian Tropical Research Institute provided logistical support and the rainfall dataset (Terrestrial-Environmental Science Program). Funding was provided by the University of Wisconsin-Milwaukee Research Growth Initiative and Graduate School, and the National Science Foundation (NSF-DEB 0613666 and NSF-DEB 0845071). NR 45 TC 23 Z9 23 U1 3 U2 20 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 FEB PY 2012 VL 3 IS 2 AR UNSP 20 DI 10.1890/ES11-00322.1 PG 11 WC Ecology SC Environmental Sciences & Ecology GA 256HA UT WOS:000327299100008 ER PT J AU Bindi, L Eiler, JM Guan, YB Hollister, LS MacPherson, G Steinhardt, PJ Yao, N AF Bindi, Luca Eiler, John M. Guan, Yunbin Hollister, Lincoln S. MacPherson, Glenn Steinhardt, Paul J. Yao, Nan TI Evidence for the extraterrestrial origin of a natural quasicrystal SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA LA English DT Article ID HIGH-PRESSURE; SOLAR NEBULA; ELEMENTS; MICROANALYSIS; CONSTRAINTS; ABUNDANCES; MEGACRYSTS; SILICATES; OXIDES; PHASE AB We present evidence that a rock sample found in the Koryak Mountains in Russia and containing icosahedrite, an icosahedral quasicrystalline phase with composition Al63Cu24Fe13, is part of a meteorite, likely formed in the early solar system about 4.5 Gya. The quasicrystal grains are intergrown with diopside, forsterite, stishovite, and additional metallic phases [khatyrkite (CuAl2), cupalite (CuAl), and beta-phase (AlCuFe)]. This assemblage, in turn, is enclosed in a white rind consisting of diopside, hedenbergite, spinel (MgAl2O4), nepheline, and forsterite. Particularly notable is a grain of stishovite (from the interior), a tetragonal polymorph of silica that only occurs at ultrahigh pressures (>= 10 Gpa), that contains an inclusion of quasicrystal. An extraterrestrial origin is inferred from secondary ion mass spectrometry O-18/O-16 and O-17/O-16 measurements of the pyroxene and olivine intergrown with the metal that show them to have isotopic compositions unlike any terrestrial minerals and instead overlap those of anhydrous phases in carbonaceous chondrite meteorites. The spinel from the white rind has an isotopic composition suggesting that it was part of a calcium-aluminum-rich inclusion similar to those found in CV3 chondrites. The mechanism that produced this exotic assemblage is not yet understood. The assemblage (metallic copper-aluminum alloy) is extremely reduced, and the close association of aluminum (high temperature refractory lithophile) with copper (low temperature chalcophile) is unexpected. Nevertheless, our evidence indicates that quasicrystals can form naturally under astrophysical conditions and remain stable over cosmic timescales, giving unique insights on their existence in nature and stability. C1 [Steinhardt, Paul J.] Princeton Univ, Princeton Ctr Theoret Sci, Princeton, NJ 08544 USA. [Bindi, Luca] Univ Florence, Sez Mineral, Museo Storia Nat, I-50121 Florence, Italy. [Bindi, Luca] Univ Florence, Dipartimento Sci Terra, I-50121 Florence, Italy. [Eiler, John M.; Guan, Yunbin] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. [Hollister, Lincoln S.] Princeton Univ, Dept Geosci, Princeton, NJ 08544 USA. [MacPherson, Glenn] Smithsonian Inst, Natl Museum Nat Hist, Dept Mineral Sci, Washington, DC 20013 USA. [Steinhardt, Paul J.] Princeton Univ, Dept Phys, Princeton, NJ 08544 USA. [Yao, Nan] Princeton Univ, Princeton Inst Sci & Technol Mat, Princeton, NJ 08544 USA. RP Steinhardt, PJ (reprint author), Princeton Univ, Princeton Ctr Theoret Sci, Princeton, NJ 08544 USA. EM steinh@princeton.edu FU National Science Foundation Materials Research Science and Engineering Center through New York University [DMR-0820341]; Princeton Center for Complex Materials [DMR-0819860]; National Aeronautics and Space Administration [NNX11AD43G] FX We thank C. Ballhaus, J. Beckett, P. Bonazzi, K. Deffeyes, A. El Goresy, V. Distler, A. Ishiwatari, J. Jones, S. Menchetti, M. Morozov, G. Poirier, P. Robinson, V. Rudashevkij, E. Stolper, and P. Spry for useful discussions and assistance and to P.J. Lu for his contributions to the study of natural quasicrystals leading up to this paper. L.B. thanks Ministero dell'Istruzione, dell'Universita e della Ricerca, Progetti di Ricerca di Interesse Nazionale 2007 project Complexity in minerals: Modulation, phase transition, structural disorder issued to Silvio Menchetti, Centro di Microscopia Elettronica e Microanalisi, Florence, Italy and Centro Interdipartimentale di Cristallografia Strutturale, Sesto Fiorentino, Florence, Italy. This work is supported in part by the National Science Foundation Materials Research Science and Engineering Center program through New York University Grant DMR-0820341 (to P.J.S.), Princeton Center for Complex Materials Grant DMR-0819860 (to N.Y.), and National Aeronautics and Space Administration Grant NNX11AD43G (to G.J M.). NR 25 TC 28 Z9 28 U1 4 U2 27 PU NATL ACAD SCIENCES PI WASHINGTON PA 2101 CONSTITUTION AVE NW, WASHINGTON, DC 20418 USA SN 0027-8424 J9 P NATL ACAD SCI USA JI Proc. Natl. Acad. Sci. U. S. A. PD JAN 31 PY 2012 VL 109 IS 5 BP 1396 EP 1401 DI 10.1073/pnas.1111115109 PG 6 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 884TJ UT WOS:000299731400020 PM 22215583 ER PT J AU Grobman, A Bonavia, D Dillehay, TD Piperno, DR Iriarte, J Holst, I AF Grobman, Alexander Bonavia, Duccio Dillehay, Tom D. Piperno, Dolores R. Iriarte, Jose Holst, Irene TI Preceramic maize from Paredones and Huaca Prieta, Peru SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA LA English DT Article DE early crops; social complexity ID BALSAS RIVER VALLEY; ZEA-MAYS L.; STARCH GRAINS; DOMESTICATION; MEXICO; TEOSINTE; ECUADOR; ORIGIN; BP AB Maize (Zea mays ssp. mays) is among the world's most important and ancient domesticated crops. Although the chronology of its domestication and initial dispersals out of Mexico into Central and South America has become more clear due to molecular and multi-proxy archaeobotanical research, important problems remain. Among them is the paucity of information on maize's early morphological evolution and racial diversification brought about in part by the poor preservation of macrofossils dating to the pre-5000 calibrated years before the present period from obligate dispersal routes located in the tropical forest. We report newly discovered macrobotanical and microbotanical remains of maize that shed significant light on the chronology, land race evolution, and cultural contexts associated with the crop's early movements into South America and adaptation to new environments. The evidence comes from the coastal Peruvian sites of Paredones and Huaca Prieta, Peru; dates from the middle and late preceramic and early ceramic periods (between ca. 6700 and 3000 calibrated years before the present); and constitutes some of the earliest known cobs, husks, stalks, and tassels. The macrobotanical record indicates that a diversity of racial complexes characteristic of the Andean region emerged during the preceramic era. In addition, accelerator mass spectrometry radiocarbon determinations carried out directly on different structures of preserved maize plants strongly suggest that assays on burned cobs are more reliable than those on unburned cobs. Our findings contribute to knowledge of the early diffusion of maize and agriculture and have broader implications for understanding the development of early preindustrial human societies. C1 [Dillehay, Tom D.] Vanderbilt Univ, Dept Anthropol, Nashville, TN 37235 USA. [Grobman, Alexander] Univ Nacl Agr, Lima 1, Peru. [Bonavia, Duccio] Acad Nacl Hist, Lima 1, Peru. [Piperno, Dolores R.] Smithsonian Natl Museum Nat Hist, Dept Anthropol, Program Human Ecol & Archaeobiol, Washington, DC 20013 USA. [Piperno, Dolores R.; Holst, Irene] Smithsonian Trop Res Inst, Balboa, Panama. [Iriarte, Jose] Univ Exeter, Dept Archaeol, Exeter EX1 2LU, Devon, England. RP Dillehay, TD (reprint author), Vanderbilt Univ, Dept Anthropol, 221 Kirkland Hall, Nashville, TN 37235 USA. EM tom.d.dillehay@vanderbilt.edu; pipernod@si.edu RI Iriarte, Jose /A-1141-2010; OI Iriarte, Jose/0000-0002-8155-5360 FU National Science Foundation; National Geographic Society; Vanderbilt University; Smithsonian National Museum of Natural History; Smithsonian Tropical Research Institute; Direccion Regional del Ministerio de la Cultura, Trujillo; Lapinski and O'Leary families FX We thank two reviewers for their helpful comments on the manuscript and the Ministerio de Cultura, Lima, Peru, for granting us the permission to work at Huaca Prieta and Paredones. We are grateful to Cesar Galvez and Jesus Briceno (Direccion Regional del Ministerio de la Cultura, Trujillo) for their support. Additional support was provided by the Lapinski and O'Leary families. We thank Tim Messner for assistance with the starch grain study and Sandra Manrique for photographing the maize phytolith remains. The authors are grateful to the Department of Anthropology at the American Museum of Natural History for granting permission to study Junius Bird's notes and photographs from Huaca Prieta, as well as the artifacts that he recovered from the site. Financial support for this project came from the National Science Foundation, the National Geographic Society, Vanderbilt University, the Smithsonian National Museum of Natural History, and the Smithsonian Tropical Research Institute. NR 25 TC 22 Z9 22 U1 2 U2 21 PU NATL ACAD SCIENCES PI WASHINGTON PA 2101 CONSTITUTION AVE NW, WASHINGTON, DC 20418 USA SN 0027-8424 J9 P NATL ACAD SCI USA JI Proc. Natl. Acad. Sci. U. S. A. PD JAN 31 PY 2012 VL 109 IS 5 BP 1755 EP 1759 DI 10.1073/pnas.1120270109 PG 5 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 884TJ UT WOS:000299731400080 PM 22307642 ER PT J AU Mitovski, T Folkins, I Martin, RV Cooper, M AF Mitovski, Toni Folkins, Ian Martin, Randall V. Cooper, Matthew TI Testing convective transport on short time scales: Comparisons with mass divergence and ozone anomaly patterns about high rain events SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID TROPICAL CONVECTION; MESOSCALE CONVECTION; TROPOSPHERIC OZONE; MOIST CONVECTION; CONVERGENCE ZONE; DEEP CONVECTION; MODEL; PARAMETERIZATION; CIRCULATION; CHEMISTRY AB [1] High rain events in the western tropical Pacific were identified using the Tropical Rainfall Measuring Mission (TRMM) 3B42 gridded rainfall data set. Horizontal wind measurements from radiosonde arrays, cloud top frequency measurements from CALIPSO, and ozonesonde measurements from SHADOZ were used to construct anomaly patterns of divergence, cloud top frequency, and ozone mixing ratio about the high rain events. The observed divergence anomaly pattern was compared with patterns produced by the Goddard Earth Observing System version 4 (GEOS-4) and GEOS-5 assimilated meteorological data sets. The midlevel (similar to 6 km) divergence dipole seen in observations, consisting of a local maximum in divergence 8 h before peak rainfall and a local maximum in convergence 8 h after peak rainfall, is not represented in the GEOS-4 or GEOS-5 meteorology. The ozone anomaly pattern shows ozone decreases at midlevels (3-8 km) up to 16 h prior to peak rainfall. These decreases occur in association with increases in the frequency of midlevel cloud tops and are due to increased detrainment from cumulus congestus clouds. The observed ozone anomaly pattern was compared with anomaly patterns produced by the GEOS-Chem chemical transport model, driven by GEOS-4 and GEOS-5 assimilated winds and temperatures. The GEOS-Chem simulations also exhibit negative ozone anomalies at midlevels in association with high rain events. However, these anomalies are nearly symmetric about peak rainfall, rather than strongest prior to peak rainfall. The upper level negative ozone anomalies of the models are more persistent than the observations. These results help characterize some of the difficulties of meteorological data sets in capturing the layered character of tropical convective outflow and its timing with respect to high rain events. C1 [Mitovski, Toni; Folkins, Ian; Martin, Randall V.; Cooper, Matthew] Dalhousie Univ, Dept Phys & Atmospher Sci, Halifax, NS B3H 4R2, Canada. [Martin, Randall V.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Mitovski, T (reprint author), Dalhousie Univ, Dept Phys & Atmospher Sci, Halifax, NS B3H 4R2, Canada. EM mitovski@dal.ca RI Martin, Randall/C-1205-2014; Chem, GEOS/C-5595-2014 OI Martin, Randall/0000-0003-2632-8402; FU Natural Sciences and Engineering Research Council (NSERC) of Canada FX The authors acknowledge useful discussions with Kenneth Pickering, Mark Lawrence, and Jeffrey Pierce. We thank the following institutions for making their data public: NASA GSFC (TRMM 3B42 and SHADOZ), NCDC (IGRA), NASA GMAO (GEOS-4 and GEOS-5), and NASA LARC (CALIPSO). Comments and suggestions by three anonymous reviewers greatly improved the manuscript. This research was supported by the Natural Sciences and Engineering Research Council (NSERC) of Canada. NR 34 TC 5 Z9 5 U1 0 U2 8 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD JAN 26 PY 2012 VL 117 AR D02109 DI 10.1029/2011JD016321 PG 13 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 884JY UT WOS:000299702300001 ER PT J AU Welsh, WF Orosz, JA Carter, JA Fabrycky, DC Ford, EB Lissauer, JJ Prsa, A Quinn, SN Ragozzine, D Short, DR Torres, G Winn, JN Doyle, LR Barclay, T Batalha, N Bloemen, S Brugamyer, E Buchhave, LA Caldwell, C Caldwell, DA Christiansen, JL Ciardi, DR Cochran, WD Endl, M Fortney, JJ Gautier, TN Gilliland, RL Haas, MR Hall, JR Holman, MJ Howard, AW Howell, SB Isaacson, H Jenkins, JM Klaus, TC Latham, DW Li, J Marcy, GW Mazeh, T Quintana, EV Robertson, P Shporer, A Steffen, JH Windmiller, G Koch, DG Borucki, WJ AF Welsh, William F. Orosz, Jerome A. Carter, Joshua A. Fabrycky, Daniel C. Ford, Eric B. Lissauer, Jack J. Prsa, Andrej Quinn, Samuel N. Ragozzine, Darin Short, Donald R. Torres, Guillermo Winn, Joshua N. Doyle, Laurance R. Barclay, Thomas Batalha, Natalie Bloemen, Steven Brugamyer, Erik Buchhave, Lars A. Caldwell, Caroline Caldwell, Douglas A. Christiansen, Jessie L. Ciardi, David R. Cochran, William D. Endl, Michael Fortney, Jonathan J. Gautier, Thomas N., III Gilliland, Ronald L. Haas, Michael R. Hall, Jennifer R. Holman, Matthew J. Howard, Andrew W. Howell, Steve B. Isaacson, Howard Jenkins, Jon M. Klaus, Todd C. Latham, David W. Li, Jie Marcy, Geoffrey W. Mazeh, Tsevi Quintana, Elisa V. Robertson, Paul Shporer, Avi Steffen, Jason H. Windmiller, Gur Koch, David G. Borucki, William J. TI Transiting circumbinary planets Kepler-34 b and Kepler-35 b SO NATURE LA English DT Article ID HIERARCHICAL TRIPLE; ECLIPSING BINARIES; DATA RELEASE; STELLAR; STARS; SYSTEMS; STABILITY; CATALOG AB Most Sun-like stars in the Galaxy reside in gravitationally bound pairs of stars(1,2) (binaries). Although long anticipated(3-8), the existence of a 'circumbinary planet' orbiting such a pair of normal stars was not definitively established until the discovery(9) of the planet transiting (that is, passing in front of) Kepler-16. Questions remained, however, about the prevalence of circumbinary planets and their range of orbital and physical properties. Here we report two additional transiting circumbinary planets: Kepler-34 (AB)b and Kepler-35 (AB)b, referred to here as Kepler-34 b and Kepler-35 b, respectively. Each is a low-density gas-giant planet on an orbit closely aligned with that of its parent stars. Kepler-34 b orbits two Sun-like stars every 289 days, whereas Kepler-35 b orbits a pair of smaller stars (89% and 81% of the Sun's mass) every 131 days. The planets experience large multi-periodic variations in incident stellar radiation arising from the orbital motion of the stars. The observed rate of circumbinary planets in our sample implies that more than similar to 1% of close binary stars have giant planets in nearly coplanar orbits, yielding a Galactic population of at least several million. C1 [Welsh, William F.; Orosz, Jerome A.; Short, Donald R.; Windmiller, Gur] San Diego State Univ, Dept Astron, San Diego, CA 92182 USA. [Fabrycky, Daniel C.] Univ Calif Santa Cruz, Lick Observ, UCO, Santa Cruz, CA 95064 USA. [Ford, Eric B.] Univ Florida, Bryant Space Sci Ctr 211, Gainesville, FL 32611 USA. [Lissauer, Jack J.; Barclay, Thomas; Batalha, Natalie; Christiansen, Jessie L.; Haas, Michael R.; Howell, Steve B.; Jenkins, Jon M.; Li, Jie; Quintana, Elisa V.; Koch, David G.; Borucki, William J.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Carter, Joshua A.; Quinn, Samuel N.; Ragozzine, Darin; Torres, Guillermo; Holman, Matthew J.; Latham, David W.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Prsa, Andrej] Villanova Univ, Dept Astron & Astrophys, Villanova, PA 19085 USA. [Quinn, Samuel N.] Georgia State Univ, Dept Phys & Astron, Atlanta, GA 30302 USA. [Winn, Joshua N.] MIT, Dept Phys, Cambridge, MA 02139 USA. [Winn, Joshua N.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Doyle, Laurance R.; Caldwell, Douglas A.; Christiansen, Jessie L.; Jenkins, Jon M.; Li, Jie; Quintana, Elisa V.] SETI Inst, Carl Sagan Ctr Study Life Universe, Mountain View, CA 94043 USA. [Barclay, Thomas] Bay Area Environm Res Inst Inc, Sonoma, CA 95476 USA. [Batalha, Natalie] San Jose State Univ, Dept Phys & Astron, San Jose, CA 95192 USA. [Bloemen, Steven] Katholieke Univ Leuven, Inst Sterrenkunde, B-3001 Louvain, Belgium. [Buchhave, Lars A.] Univ Copenhagen, Ctr Star & Planet Format, Nat Hist Museum Denmark, DK-1350 Copenhagen, Denmark. [Brugamyer, Erik; Cochran, William D.; Endl, Michael] Univ Texas Austin, McDonald Observ, Austin, TX 78712 USA. [Buchhave, Lars A.] Univ Copenhagen, Niels Bohr Inst, DK-2100 Copenhagen, Denmark. [Ciardi, David R.] CALTECH, NASA Exoplanet Sci Inst, Pasadena, CA 91125 USA. [Fortney, Jonathan J.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. [Gautier, Thomas N., III] Jet Prop Lab, Pasadena, CA 91109 USA. [Gilliland, Ronald L.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Klaus, Todd C.] NASA, Orbital Sci Corp, Ames Res Ctr, Moffett Field, CA 94035 USA. [Marcy, Geoffrey W.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Mazeh, Tsevi] Tel Aviv Univ, Sch Phys & Astron, IL-69978 Tel Aviv, Israel. [Shporer, Avi] Las Cumbres Observ, Global Telescope Network, Santa Barbara, CA 93117 USA. [Shporer, Avi] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA. [Steffen, Jason H.] Fermilab Ctr Particle Astrophys, Batavia, IL 60510 USA. RP Welsh, WF (reprint author), San Diego State Univ, Dept Astron, 5500 Campanile Dr, San Diego, CA 92182 USA. EM wfw@sciences.sdsu.edu; jacarter@cfa.harvard.edu RI Steffen, Jason/A-4320-2013; Carter, Joshua/A-8280-2013; Ragozzine, Darin/C-4926-2013; Caldwell, Douglas/L-7911-2014; Howard, Andrew/D-4148-2015; OI Caldwell, Douglas/0000-0003-1963-9616; Howard, Andrew/0000-0001-8638-0320; Fortney, Jonathan/0000-0002-9843-4354; Buchhave, Lars A./0000-0003-1605-5666; Ciardi, David/0000-0002-5741-3047; Barclay, Thomas/0000-0001-7139-2724; Fabrycky, Daniel/0000-0003-3750-0183 FU NASA's Science Mission Directorate; Kepler Participating Scientist Program; NSF; NASA; STScI; European Research Council under the European Community; Research Council of KU Leuven; FAS Science Division Research Computing Group at Harvard University FX Kepler was selected as the tenth NASA Discovery mission with funding provided by NASA's Science Mission Directorate. We thank the many people who made the Kepler mission a reality. W. F. W., J.A.O., E. B. F., A. P., L. R. D., J.J.F., M.J.H., T. M. and J.H.S. were supported by the Kepler Participating Scientist Program. W. F. W., J.A.O., D. R. S. and G. W. were supported by the NSF. D. C. F. and J.A.C. acknowledge NASA support through Hubble Fellowship grants, awarded by STScI, operated by AURA. J.N.W. was supported by the NASA Origins programme. S. B. acknowledges funding from the European Research Council under the European Community's Seventh Framework Programme (PROSPERITY) and from the Research Council of KU Leuven. Some of the reported computations were run on the Odyssey cluster supported by the FAS Science Division Research Computing Group at Harvard University. This Letter is based in part on observations made with the Nordic Optical Telescope (operated on the island of La Palma jointly by Denmark, Finland, Iceland, Norway and Sweden, in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias), the W. M. Keck Observatory (operated by the University of California and the California Institute of Technology) and the Hobby-Eberly Telescope (HET; a joint project of the University of Texas at Austin, the Pennsylvania State University, Stanford University, Ludwig-Maximillians-Universitat Munchen, and Georg-August-Universitat Goettingen). NR 22 TC 200 Z9 201 U1 1 U2 17 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 0028-0836 J9 NATURE JI Nature PD JAN 26 PY 2012 VL 481 IS 7382 BP 475 EP U85 DI 10.1038/nature10768 PG 5 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 881GY UT WOS:000299471800033 PM 22237021 ER PT J AU Kuznetsova, E Bragdon, T Cote, R Yelin, SF AF Kuznetsova, Elena Bragdon, T. Cote, Robin Yelin, S. F. TI Cluster-state generation using van der Waals and dipole-dipole interactions in optical lattices SO PHYSICAL REVIEW A LA English DT Article ID RYDBERG BLOCKADE; ATOMS; ENTANGLEMENT AB We present a scalable method for generation of a cluster state for measurement-based quantum computing using van der Waals or dipole-dipole interactions between neutral atoms or polar molecules in an optical lattice. Nearest neighbor entanglement is accomplished by performing a phase gate using interaction of atoms in Rydberg states or molecules in large dipole moment states. All nearest neighbors are sequentially entangled in a finite number of operations, independent of the number of qubits, producing a one-dimensional (1D) cluster state. A universal two-dimensional (2D) cluster state can be generated in several milliseconds in a 2D optical lattice by producing a series of 1D cluster states in one lattice direction, followed by application of the entangling operations in another lattice direction. We discuss the viability of the scheme with Rb Rydberg atoms. C1 [Kuznetsova, Elena; Bragdon, T.; Cote, Robin; Yelin, S. F.] Univ Connecticut, Dept Phys, Storrs, CT 06269 USA. [Kuznetsova, Elena; Bragdon, T.; Yelin, S. F.] Harvard Smithsonian Ctr Astrophys, ITAMP, Cambridge, MA 02138 USA. RP Kuznetsova, E (reprint author), Univ Connecticut, Dept Phys, Storrs, CT 06269 USA. FU AFOSR under the MURI [FA9550-09-1-0588] FX The authors gratefully acknowledge financial support from AFOSR under the MURI award FA9550-09-1-0588. NR 35 TC 11 Z9 11 U1 0 U2 7 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 1050-2947 J9 PHYS REV A JI Phys. Rev. A PD JAN 25 PY 2012 VL 85 IS 1 AR 012328 DI 10.1103/PhysRevA.85.012328 PG 20 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA 886FP UT WOS:000299839000002 ER PT J AU Wynn, AH Reynolds, RP Buden, DW Falanruw, M Lynch, B AF Wynn, Addison H. Reynolds, Robert P. Buden, Donald W. Falanruw, Marjorie Lynch, Brian TI The unexpected discovery of blind snakes (Serpentes: Typhlopidae) in Micronesia: two new species of Ramphotyphlops from the Caroline Islands SO ZOOTAXA LA English DT Article DE Ant Atoll; arboreality; hemipenes; Oceania; Scolecophidia; Ulithi ID MARIANA ISLANDS; GUAM AB Two new blind snakes in the genus Ramphotyphlops are described from Ulithi (R. hatmaliyeb sp. nov.) and Ant Atoll (R. adocetus sp. nov.) in the Caroline Islands, the first blind snake species known from Micronesia east of Palau (excluding Ramphotyphlops braminus). Both species are unusual in being known only from small, low-lying atolls. They can be distinguished from other Ramphotyphlops by the combination of 22 scale rows over the length of the body; a wedge-shaped snout, without a keratinized keel; and a broad, pyriform (R. adocetus) or ovate (R. hatmaliyeb) rostral scale. C1 [Wynn, Addison H.] Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Washington, DC 20560 USA. [Reynolds, Robert P.] Natl Museum Nat Hist, USGS Patuxent Wildlife Res Ctr, Washington, DC 20013 USA. [Buden, Donald W.; Lynch, Brian] Coll Micronesia FSM, Div Nat Sci & Math, Kolonia 96941, Pohnpei, Micronesia. [Falanruw, Marjorie] Yap Inst Nat Sci, Yap 96943, Micronesia. RP Wynn, AH (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Washington, DC 20560 USA. EM wynna@si.edu; reynolds@si.edu; don_buden@comfsm.fm; mfalanruw@mail.fm; brianl@comfsm.fm FU Pacific Islands Educational Partnership Consortium; National Oceanic and Atmospheric Association (NOAA); Marine Resources Pacific Consortium (MAREPAC); European Union FX We thank Colin McCarthy (The Natural History Museum, London) for providing access to the holotype of R. willeyi, and Colin McCarthy and George Zug for providing photographs of its head. We also thank Rafe Brown for bringing the R. cumingii hemipenes to our attention. Jeremy Jacobs helped with the radiographs. James Poindexter took the specimen photographs. William Dickinson provided helpful discussion on Pacific atoll history. Terry Chesser, Robert Fisher, Van Wallach, Neal Woodman, and George Zug provided helpful comments on the manuscript. We also thank the College of Micronesia Marine Field Studies students and College of Micronesia maintenance staff for their assistance in collecting the series of 16 R. adocetus paratypes during their 30 August 2008 trip to Ant Atoll. This trip was supported by funding from the Pacific Islands Educational Partnership Consortium Program, the National Oceanic and Atmospheric Association (NOAA), and the Marine Resources Pacific Consortium (MAREPAC). M. Falanruw thanks the late Chief of Ngulu, Rinfal, who started her in 1965 on the quest that led to this paper when he told her about a "worm-like animal with scales and a tongue"; the traditional leadership of Ulithi; Steve Kolinski, who collected the specimen of R. hatmaliyeb from Piig Island; Jennifer Cruce, Bert Suwel, and the rest of the Ulithi Turtle Taggers for welcoming her to their project and Giilab, where she saw her first live R. hatmaliyeb; and Jennifer Cruce, Dewey Dipwek, Jim Stanford, Francis Ruegorong, Charlie Gilgaayan, Brian Greene, and William Marlemal, who were on the team on Soong Island. YINS work was partially funded by the European Union Conservation and Environmental Protection Program. NR 31 TC 3 Z9 5 U1 0 U2 3 PU MAGNOLIA PRESS PI AUCKLAND PA PO BOX 41383, AUCKLAND, ST LUKES 1030, NEW ZEALAND SN 1175-5326 EI 1175-5334 J9 ZOOTAXA JI Zootaxa PD JAN 25 PY 2012 IS 3172 BP 39 EP 54 PG 16 WC Zoology SC Zoology GA 891SU UT WOS:000300237700003 ER PT J AU Hawley, DM Fleischer, RC AF Hawley, Dana M. Fleischer, Robert C. TI Contrasting Epidemic Histories Reveal Pathogen-Mediated Balancing Selection on Class II MHC Diversity in a Wild Songbird SO PLOS ONE LA English DT Article ID MAJOR HISTOCOMPATIBILITY COMPLEX; FINCH CARPODACUS-MEXICANUS; HUMAN INFECTIOUS-DISEASES; COPY NUMBER VARIATION; IN-HOUSE FINCHES; MYCOPLASMA-GALLISEPTICUM; NATURAL-SELECTION; EVOLUTIONARY GENETICS; PARASITE RESISTANCE; POPULATION AB The extent to which pathogens maintain the extraordinary polymorphism at vertebrate Major Histocompatibility Complex (MHC) genes via balancing selection has intrigued evolutionary biologists for over half a century, but direct tests remain challenging. Here we examine whether a well-characterized epidemic of Mycoplasmal conjunctivitis resulted in balancing selection on class II MHC in a wild songbird host, the house finch (Carpodacus mexicanus). First, we confirmed the potential for pathogen-mediated balancing selection by experimentally demonstrating that house finches with intermediate to high multi-locus MHC diversity are more resistant to challenge with Mycoplasma gallisepticum. Second, we documented sequence and diversity-based signatures of pathogen-mediated balancing selection at class II MHC in exposed host populations that were absent in unexposed, control populations across an equivalent time period. Multi-locus MHC diversity significantly increased in exposed host populations following the epidemic despite initial compromised diversity levels from a recent introduction bottleneck in the exposed host range. We did not observe equivalent changes in allelic diversity or heterozygosity across eight neutral microsatellite loci, suggesting that the observations reflect selection rather than neutral demographic processes. Our results indicate that a virulent pathogen can exert sufficient balancing selection on class II MHC to rescue compromised levels of genetic variation for host resistance in a recently bottlenecked population. These results provide evidence for Haldane's long-standing hypothesis that pathogens directly contribute to the maintenance of the tremendous levels of genetic variation detected in natural populations of vertebrates. C1 [Hawley, Dana M.; Fleischer, Robert C.] Smithsonian Inst, Ctr Conservat & Evolutionary Genet, Washington, DC 20560 USA. RP Hawley, DM (reprint author), Virginia Tech, Dept Biol Sci, Blacksburg, VA 24061 USA. EM hawleyd@vt.edu OI Hawley, Dana/0000-0001-9573-2914 FU Smithsonian Institution (SI); SI Molecular Evolution Postdoctoral Fellowship; National Science Foundation/National Institutes of Health [DEB-0094456] FX This work was supported by the Smithsonian Institution (SI) Genetics Program and an SI Molecular Evolution Postdoctoral Fellowship, with partial support from the National Science Foundation/National Institutes of Health Ecology of Infectious Disease Program (DEB-0094456). The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 71 TC 17 Z9 17 U1 1 U2 26 PU PUBLIC LIBRARY SCIENCE PI SAN FRANCISCO PA 185 BERRY ST, STE 1300, SAN FRANCISCO, CA 94107 USA SN 1932-6203 J9 PLOS ONE JI PLoS One PD JAN 23 PY 2012 VL 7 IS 1 AR e30222 DI 10.1371/journal.pone.0030222 PG 11 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 909NE UT WOS:000301570600026 PM 22291920 ER PT J AU McCarthy, MC Lattanzi, V Kokkin, D Martinez, O Stanton, JF AF McCarthy, Michael C. Lattanzi, Valerio Kokkin, Damian Martinez, Oscar, Jr. Stanton, John F. TI On the molecular structure of HOOO SO JOURNAL OF CHEMICAL PHYSICS LA English DT Article ID MILLIMETER-WAVE SPECTROSCOPY; INFRARED ACTION SPECTROSCOPY; DOUBLE-RESONANCE SPECTROSCOPY; ROTATIONAL SPECTRUM; HYPERFINE-STRUCTURE; MICROWAVE-SPECTRUM; ATOMIC-HYDROGEN; WATER DIMER; OH; DISSOCIATION AB The molecular structure of trans, planar hydridotrioxygen (HOOO) has been examined by means of isotopic spectroscopy using Fourier transform microwave as well as microwave-millimeter-wave double resonance techniques, and high-level coupled cluster quantum-chemical calculations. Although this weakly bound molecule is readily observed in an electrical discharge of H2O and O-2 heavily diluted in an inert buffer gas, we find that HOOO can be produced with somewhat higher abundance using H-2 and O-2 as precursor gases. Using equal mixtures of normal and O-18(2), it has been possible to detect three new isotopic species, (HOOO)-O-18, (HOOO)-O-18-O-18, and (HOOO)-O-18-O-18-O-18. Detection of these species and not others provides compelling evidence that the dominant route to HOOO formation in our discharge is via the reaction OH + O-2 -> HOOO. By combining derived rotational constants with those for normal HOOO and DOOO, it has been possible to determine a fully experimental (r(0)) structure for this radical, in which all of the structural parameters (the three bond lengths and two angles) have been varied. This best-fit structure possesses a longer central O-O bond (1.684 angstrom), in agreement with earlier work, a markedly shorter O-H bond distance (0.913 angstrom), and a more acute angle HOO angle (92.4 degrees) when compared to equilibrium (r(e)) structures obtained from quantum-chemical calculations. To better understand the origin of these discrepancies, vibrational corrections have been obtained from coupled-cluster calculations. An empirical equilibrium (r(e)(emp)) structure, derived from the experimental rotational constants and theoretical vibrational corrections, gives only somewhat better agreement with the calculated equilibrium structure and large residual inertial defects, suggesting that still higher order vibrational corrections (i.e., gamma terms) are needed to properly describe large-amplitude motion in HOOO. Owing to the high abundance of this oxygen-chain radical in our discharge expansion, a very wide spectral survey for other oxygen-bearing species has been undertaken between 6 and 25 GHz. Only about 50% of the observed lines have been assigned to known hydrogen-oxygen molecules or complexes, suggesting that a rich, unexplored oxygen chemistry awaits detection and characterization. Somewhat surprisingly, we find no evidence in our expansion for rotational transitions of cis HOOO or from low-lying vibrationally excited states of trans HOOO under conditions which optimize its ground state lines. (C) 2012 American Institute of Physics. [doi:10.1063/1.3673875] C1 [McCarthy, Michael C.; Lattanzi, Valerio; Kokkin, Damian; Martinez, Oscar, Jr.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [McCarthy, Michael C.; Lattanzi, Valerio; Kokkin, Damian; Martinez, Oscar, Jr.] Harvard Univ, Sch Engn & Appl Sci, Cambridge, MA 02138 USA. [Stanton, John F.] Univ Texas Austin, Dept Chem & Biochem, Austin, TX 78712 USA. RP McCarthy, MC (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM mccarthy@cfa.harvard.edu; vlattanzi@cfa.harvard.edu; dkokkin@cfa.harvard.edu; omartinez@cfa.harvard.edu; jfstanton@mail.utexas.edu OI McCarthy, Michael/0000-0001-9142-0008 FU NSF [CHE-1058063]; U.S. National Science Foundation; Robert A. Welch Foundation of Houston, Texas [Grant F-1283] FX We thank C. A. Gottlieb, M. I. Lester, I. R. Sims, R. Dawes, and Y. Endo for helpful discussions. The work in Cambridge is supported by the NSF Grant No. CHE-1058063. J. F. S. has been supported by the U.S. National Science Foundation and the Robert A. Welch Foundation (Grant F-1283) of Houston, Texas. NR 65 TC 15 Z9 15 U1 2 U2 36 PU AMER INST PHYSICS PI MELVILLE PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1, MELVILLE, NY 11747-4501 USA SN 0021-9606 J9 J CHEM PHYS JI J. Chem. Phys. PD JAN 21 PY 2012 VL 136 IS 3 AR 034303 DI 10.1063/1.3673875 PG 10 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA 880EN UT WOS:000299387700021 PM 22280756 ER PT J AU Cardenas, MB Lagmay, AMF Andrews, BJ Rodolfo, RS Cabria, HB Zamora, PB Lapus, MR AF Cardenas, M. Bayani Lagmay, Alfredo Mahar F. Andrews, Benjamin J. Rodolfo, Raymond S. Cabria, Hillel B. Zamora, Peter B. Lapus, Mark R. TI Terrestrial smokers: Thermal springs due to hydrothermal convection of groundwater connected to surface water SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID VOLCANIC LAKE SYSTEMATICS; POAS VOLCANO; CRATER-LAKE; COSTA-RICA; CONSTRAINTS; NICARAGUA; DYNAMICS; BRINE; FLOW AB Thermal springs are ubiquitous features whose underground kinematic structure is mostly unknown but are typically thought to originate from deep sources. We documented a type of thermal springs at the banks of a volcanic lake that are discharge zones of hydrothermal convection cells circulating groundwater within the near shore environment. The convection captures lake water through the lakebed, mixes it with deeper groundwater at velocities of 100s of m d(-1), then returns the water to the lake via the spring. The convection cell is flushed in a few hours and turns over the lake's volume in a few days. Most volcanic lakes and other relatively cool surface water bodies in areas of elevated geothermal heat fluxes meet the conditions for the occurrence of local hydrothermal circulation of groundwater. The type of spring we studied, the terrestrial version of black smokers, is likely present but perhaps unrecognized at many areas. Citation: Bayani Cardenas, M., A. M. F. Lagmay, B. J. Andrews, R. S. Rodolfo, H. B. Cabria, P. B. Zamora, and M. R. Lapus (2012), Terrestrial smokers: Thermal springs due to hydrothermal convection of groundwater connected to surface water, Geophys. Res. Lett., 39, L02403, doi: 10.1029/2011GL050475. C1 [Cardenas, M. Bayani; Zamora, Peter B.] Univ Texas Austin, Austin, TX 78712 USA. [Lagmay, Alfredo Mahar F.; Rodolfo, Raymond S.; Lapus, Mark R.] Univ Philippines, Natl Inst Geol Sci, Quezon City, Philippines. [Andrews, Benjamin J.] Natl Museum Nat Hist, Smithsonian Inst, Washington, DC 20560 USA. [Cabria, Hillel B.] Geos Inc, Quezon City 1128, Philippines. RP Cardenas, MB (reprint author), Univ Texas Austin, Austin, TX 78712 USA. EM cardenas@jsg.utexas.edu RI Cardenas, Meinhard Bayani/B-4940-2011 OI Cardenas, Meinhard Bayani/0000-0001-6270-3105 FU Geology Foundation at the University of Texas at Austin FX We thank Editor, Paolo D'Odorico, for comments that improved the manuscript and Steve Ingebritsen and an anonymous reviewer for their careful and insightful reviews. This study was partly supported by the Geology Foundation at the University of Texas at Austin. NR 17 TC 5 Z9 5 U1 3 U2 17 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD JAN 21 PY 2012 VL 39 AR L02403 DI 10.1029/2011GL050475 PG 6 WC Geosciences, Multidisciplinary SC Geology GA 880GX UT WOS:000299394400003 ER PT J AU Barbary, K Aldering, G Amanullah, R Brodwin, M Connolly, N Dawson, KS Doi, M Eisenhardt, P Faccioli, L Fadeyev, V Fakhouri, HK Fruchter, AS Gilbank, DG Gladders, MD Goldhaber, G Goobar, A Hattori, T Hsiao, E Huang, X Ihara, Y Kashikawa, N Koester, B Konishi, K Kowalski, M Lidman, C Lubin, L Meyers, J Morokuma, T Oda, T Panagia, N Perlmutter, S Postman, M Ripoche, P Rosati, P Rubin, D Schlegel, DJ Spadafora, AL Stanford, SA Strovink, M Suzuki, N Takanashi, N Tokita, K Yasuda, N AF Barbary, K. Aldering, G. Amanullah, R. Brodwin, M. Connolly, N. Dawson, K. S. Doi, M. Eisenhardt, P. Faccioli, L. Fadeyev, V. Fakhouri, H. K. Fruchter, A. S. Gilbank, D. G. Gladders, M. D. Goldhaber, G. Goobar, A. Hattori, T. Hsiao, E. Huang, X. Ihara, Y. Kashikawa, N. Koester, B. Konishi, K. Kowalski, M. Lidman, C. Lubin, L. Meyers, J. Morokuma, T. Oda, T. Panagia, N. Perlmutter, S. Postman, M. Ripoche, P. Rosati, P. Rubin, D. Schlegel, D. J. Spadafora, A. L. Stanford, S. A. Strovink, M. Suzuki, N. Takanashi, N. Tokita, K. Yasuda, N. CA Supernova Cosmology Project TI THE HUBBLE SPACE TELESCOPE CLUSTER SUPERNOVA SURVEY. VI. THE VOLUMETRIC TYPE Ia SUPERNOVA RATE SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology: observations; supernovae: general; white dwarfs ID DIGITAL SKY SURVEY; SUBARU DEEP FIELD; SIMILAR-TO 1; GALAXY CLUSTERS; LEGACY SURVEY; STAR-FORMATION; COSMOLOGICAL CONSTRAINTS; XMMXCS J2215.9-1738; II SUPERNOVAE; LIGHT CURVES AB We present a measurement of the volumetric Type Ia supernova (SN Ia) rate out to z similar or equal to 1.6 from the Hubble Space Telescope Cluster Supernova Survey. In observations spanning 189 orbits with the Advanced Camera for Surveys we discovered 29 SNe, of which approximately 20 are SNe Ia. Twelve of these SNe Ia are located in the foregrounds and backgrounds of the clusters targeted in the survey. Using these new data, we derive the volumetric SN Ia rate in four broad redshift bins, finding results consistent with previous measurements at z greater than or similar to 1 and strengthening the case for an SN Ia rate that is greater than or similar to 0.6 x 10(-4) h(70)(3) yr(-1) Mpc(-3) at z similar to 1 and flattening out at higher redshift. We provide SN candidates and efficiency calculations in a form that makes it easy to rebin and combine these results with other measurements for increased statistics. Finally, we compare the assumptions about host-galaxy dust extinction used in different high-redshift rate measurements, finding that different assumptions may induce significant systematic differences between measurements. C1 [Barbary, K.; Amanullah, R.; Fakhouri, H. K.; Goldhaber, G.; Huang, X.; Meyers, J.; Perlmutter, S.; Rubin, D.; Strovink, M.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. [Barbary, K.; Aldering, G.; Dawson, K. S.; Fakhouri, H. K.; Goldhaber, G.; Hsiao, E.; Meyers, J.; Perlmutter, S.; Ripoche, P.; Rubin, D.; Schlegel, D. J.; Spadafora, A. L.; Strovink, M.; Suzuki, N.] EO Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA. [Amanullah, R.; Faccioli, L.; Goobar, A.] Oskar Klein Ctr Cosmo Particle Phys, SE-10691 Stockholm, Sweden. [Brodwin, M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Connolly, N.] Dept Phys, Hamilton Coll, Clinton, NY 13323 USA. [Dawson, K. S.] Univ Utah, Dept Phys & Astron, Salt Lake City, UT 84112 USA. [Doi, M.; Ihara, Y.; Morokuma, T.; Tokita, K.] Univ Tokyo, Inst Astron, Grad Sch Sci, Mitaka, Tokyo 1810015, Japan. [Eisenhardt, P.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Fadeyev, V.] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Santa Cruz, CA 94064 USA. [Fruchter, A. S.; Panagia, N.; Postman, M.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Gilbank, D. G.] Univ Waterloo, Dept Phys & Astron, Waterloo, ON N2L 3G1, Canada. [Gladders, M. D.; Koester, B.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. [Goobar, A.] Stockholm Univ, Albanova Univ Ctr, Dept Phys, SE-10691 Stockholm, Sweden. [Hattori, T.] Natl Astron Observ Japan, Subaru Telescope, Hilo, HI 96720 USA. [Kashikawa, N.; Morokuma, T.; Takanashi, N.] Univ Tokyo, Inst Ind Sci, Meguro Ku, Tokyo 1538505, Japan. [Koester, B.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Konishi, K.; Yasuda, N.] Univ Tokyo, Inst Cosm Ray Res, Kashiwa, Chiba 2778582, Japan. [Kowalski, M.] Univ Bonn, Inst Phys, Bonn, Germany. [Lidman, C.] Australian Astron Observ, Epping, NSW 1710, Australia. [Lubin, L.; Stanford, S. A.] Univ Calif Davis, Dept Phys, Davis, CA 95618 USA. [Oda, T.] Kyoto Univ, Dept Astron, Sakyo Ku, Kyoto 6068502, Japan. [Rosati, P.] ESO, D-85748 Garching, Germany. [Stanford, S. A.] Lawrence Livermore Natl Lab, Inst Geophys & Planetary Phys, Livermore, CA 94550 USA. RP Barbary, K (reprint author), Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. EM kbarbary@lbl.gov RI Kowalski, Marek/G-5546-2012; Perlmutter, Saul/I-3505-2015; OI Perlmutter, Saul/0000-0002-4436-4661; Strovink, Mark/0000-0001-7020-7769; Meyers, Joshua/0000-0002-2308-4230 FU NASA from Space Telescope Science Institute [GO-10496]; NASA [NAS 5-26555]; Office of Science, Office of High Energy and Nuclear Physics, of the U.S. Department of Energy [AC02-05CH11231]; JSPS [20040003] FX Financial support for this work was provided by NASA through program GO-10496 from the Space Telescope Science Institute, which is operated by AURA, Inc., under NASA contract NAS 5-26555. This work was also supported in part by the Director, Office of Science, Office of High Energy and Nuclear Physics, of the U.S. Department of Energy under Contract No. AC02-05CH11231, as well as a JSPS core-to-core program "International Research Network for Dark Energy" and by a JSPS research grant (20040003). 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. Finally, this work would not have been possible without the dedicated efforts of the daytime and nighttime support staff at the Cerro Paranal Observatory.; STScI is operated by the association of Universities for Research in Astronomy, Inc., under the NASA contract NAS 5-26555. The observations are associated with program GO-10496. NR 67 TC 15 Z9 15 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JAN 20 PY 2012 VL 745 IS 1 AR 31 DI 10.1088/0004-637X/745/1/31 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 892WP UT WOS:000300316600031 ER PT J AU Barbary, K Aldering, G Amanullah, R Brodwin, M Connolly, N Dawson, KS Doi, M Eisenhardt, P Faccioli, L Fadeyev, V Fakhouri, HK Fruchter, AS Gilbank, DG Gladders, MD Goldhaber, G Goobar, A Hattori, T Hsiao, E Huang, X Ihara, Y Kashikawa, N Koester, B Konishi, K Kowalski, M Lidman, C Lubin, L Meyers, J Morokuma, T Oda, T Panagia, N Perlmutter, S Postman, M Ripoche, P Rosati, P Rubin, D Schlegel, DJ Spadafora, AL Stanford, SA Strovink, M Suzuki, N Takanashi, N Tokita, K Yasuda, N AF Barbary, K. Aldering, G. Amanullah, R. Brodwin, M. Connolly, N. Dawson, K. S. Doi, M. Eisenhardt, P. Faccioli, L. Fadeyev, V. Fakhouri, H. K. Fruchter, A. S. Gilbank, D. G. Gladders, M. D. Goldhaber, G. Goobar, A. Hattori, T. Hsiao, E. Huang, X. Ihara, Y. Kashikawa, N. Koester, B. Konishi, K. Kowalski, M. Lidman, C. Lubin, L. Meyers, J. Morokuma, T. Oda, T. Panagia, N. Perlmutter, S. Postman, M. Ripoche, P. Rosati, P. Rubin, D. Schlegel, D. J. Spadafora, A. L. Stanford, S. A. Strovink, M. Suzuki, N. Takanashi, N. Tokita, K. Yasuda, N. CA Supernova Cosmology Project TI THE HUBBLE SPACE TELESCOPE CLUSTER SUPERNOVA SURVEY. II. THE TYPE Ia SUPERNOVA RATE IN HIGH-REDSHIFT GALAXY CLUSTERS SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology: observations; supernovae: general; white dwarfs ID DELAY-TIME DISTRIBUTION; DIGITAL SKY SURVEY; INTRACLUSTER PLANETARY-NEBULAE; CORE-COLLAPSE SUPERNOVAE; DIFFUSE OPTICAL LIGHT; IRAC SHALLOW SURVEY; SIMILAR-TO 1; X-RAY; LUMINOSITY FUNCTION; VIRGO-CLUSTER AB We report a measurement of the Type Ia supernova (SN Ia) rate in galaxy clusters at 0.9 < z < 1.46 from the Hubble Space Telescope Cluster Supernova Survey. This is the first cluster SN Ia rate measurement with detected z > 0.9 SNe. Finding 8 +/- 1 cluster SNe Ia, we determine an SN Ia rate of 0.50(-0.19)(+0.23) (stat) (+0.10)(-0.09) (sys) h(70)(2) SNuB (SNuB equivalent to 10(-12) SNe (L-1)circle dot(,B) yr(-1)). In units of stellar mass, this translates to 0.36(-0.13)(+0.16) (stat) (+0.07)(-0.06) (sys) h(70)(2) SNuM (SNuM = 10(-12) SNe M-1 circle dot yr(-1)). This represents a factor of approximate to 5 +/- 2 increase over measurements of the cluster rate at z < 0.2. We parameterize the late-time SN Ia delay time distribution (DTD) with a power law: Psi(t) t(s). Under the approximation of a single-burst cluster formation redshift of z(f) = 3, our rate measurement in combination with lower-redshift cluster SN Ia rates constrains s = -1.41(-0.40)(+0.47), consistent with measurements of the DTD in the field. This measurement is generally consistent with expectations for the "double degenerate" scenario and inconsistent with some models for the "single degenerate" scenario predicting a steeper DTD at large delay times. We check for environmental dependence and the influence of younger stellar populations by calculating the rate specifically in cluster red-sequence galaxies and in morphologically early-type galaxies, finding results similar to the full cluster rate. Finally, the upper limit of one hostless cluster SN Ia detected in the survey implies that the fraction of stars in the intra-cluster medium is less than 0.47 (95% confidence), consistent with measurements at lower redshifts. C1 [Barbary, K.; Amanullah, R.; Fakhouri, H. K.; Goldhaber, G.; Huang, X.; Meyers, J.; Perlmutter, S.; Rubin, D.; Strovink, M.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. [Barbary, K.; Aldering, G.; Dawson, K. S.; Faccioli, L.; Fakhouri, H. K.; Goldhaber, G.; Hsiao, E.; Meyers, J.; Perlmutter, S.; Ripoche, P.; Rubin, D.; Schlegel, D. J.; Spadafora, A. L.; Strovink, M.; Suzuki, N.] EO Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA. [Amanullah, R.; Goobar, A.] Oskar Klein Ctr Cosmo Particle Phys, SE-10691 Stockholm, Sweden. [Brodwin, M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Connolly, N.] Hamilton Coll, Dept Phys, Clinton, NY 13323 USA. [Dawson, K. S.] Univ Utah, Dept Phys & Astron, Salt Lake City, UT 84112 USA. [Doi, M.; Ihara, Y.; Morokuma, T.; Tokita, K.] Univ Tokyo, Grad Sch Sci, Inst Astron, Mitaka, Tokyo 1810015, Japan. [Eisenhardt, P.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Fadeyev, V.] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Santa Cruz, CA 94064 USA. [Fruchter, A. S.; Panagia, N.; Postman, M.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Gilbank, D. G.] Univ Waterloo, Dept Phys & Astron, Waterloo, ON N2L 3G1, Canada. [Gladders, M. D.; Koester, B.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. [Goobar, A.] Stockholm Univ, Albanova Univ Ctr, Dept Phys, SE-10691 Stockholm, Sweden. [Hattori, T.] Natl Astron Observ Japan, Subaru Telescope, Hilo, HI 96720 USA. [Kashikawa, N.; Morokuma, T.; Takanashi, N.] Natl Astron Observ Japan, Mitaka, Tokyo 1818588, Japan. [Koester, B.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Konishi, K.; Yasuda, N.] Univ Tokyo, Inst Cosm Ray Res, Kashiwa, Chiba 2778582, Japan. [Kowalski, M.] Univ Bonn, Inst Phys, Bonn, Germany. [Lidman, C.] Australian Astron Observ, Epping, NSW 1710, Australia. [Lubin, L.; Stanford, S. A.] Univ Calif Davis, Dept Phys, Davis, CA 95618 USA. [Oda, T.] Kyoto Univ, Dept Astron, Sakyo Ku, Kyoto 6068502, Japan. [Rosati, P.] ESO, D-85748 Garching, Germany. [Stanford, S. A.] Lawrence Livermore Natl Lab, Inst Geophys & Planetary Phys, Livermore, CA 94550 USA. RP Barbary, K (reprint author), Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. EM kbarbary@lbl.gov RI Kowalski, Marek/G-5546-2012; Perlmutter, Saul/I-3505-2015; OI Perlmutter, Saul/0000-0002-4436-4661; Strovink, Mark/0000-0001-7020-7769; Meyers, Joshua/0000-0002-2308-4230 FU Japan Society for the Promotion of Science (JSPS) [20040003]; Australian Research Council (ARC); NASA from Space Telescope Science Institute [GO-10496]; Office of Science, Office of High Energy and Nuclear Physics U.S. Department of Energy [AC02-05CH11231]; NASA [NAS 5-26555] FX We thank Eric Bell and DanMaoz for helpful discussion. T. M. is financially supported by the Japan Society for the Promotion of Science (JSPS) through the JSPS Research Fellowship. C. L. is financially supported by the Australian Research Council (ARC) through the ARC Future Fellowship program. Financial support for this work was provided by NASA through program GO-10496 from the Space Telescope Science Institute, which is operated by AURA, Inc., under NASA contract NAS 5-26555. This work was also supported in part by the Director, Office of Science, Office of High Energy and Nuclear Physics, of the U.S. Department of Energy under Contract No. AC02-05CH11231, as well as a JSPS core-to-core program "International Research Network for Dark Energy" and by a JSPS research grant (20040003). 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. Finally, this work would not have been possible without the dedicated efforts of the daytime and nighttime support staff at the Cerro Paranal Observatory. NR 147 TC 25 Z9 27 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JAN 20 PY 2012 VL 745 IS 1 AR 32 DI 10.1088/0004-637X/745/1/32 PG 28 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 892WP UT WOS:000300316600032 ER PT J AU Fressin, F Torres, G Pont, F Knutson, HA Charbonneau, D Mazeh, T Aigrain, S Fridlund, M Henze, CE Guillot, T Rauer, H AF Fressin, Francois Torres, Guillermo Pont, Frederic Knutson, Heather A. Charbonneau, David Mazeh, Tsevi Aigrain, Suzanne Fridlund, Malcolm Henze, Christopher E. Guillot, Tristan Rauer, Heike TI SPITZER INFRARED OBSERVATIONS AND INDEPENDENT VALIDATION OF THE TRANSITING SUPER- EARTH CoRoT-7 b SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries: eclipsing; planetary systems; stars: individual: CoRoT-7; stars: statistics; techniques: photometric ID SPACE-TELESCOPE; EMISSION-SPECTRUM; PLANET CANDIDATES; BLEND SCENARIOS; MULTIPLE SYSTEM; LIGHT CURVES; ARRAY CAMERA; HD 189733B; LOW-MASS; VARIABILITY AB The detection and characterization of the first transiting super-Earth, CoRoT-7 b, has required an unprecedented effort in terms of telescope time and analysis. Although the star does display a radial-velocity signal at the period of the planet, this has been difficult to disentangle from the intrinsic stellar variability and pinning down the velocity amplitude has been very challenging. As a result, the precise value of the mass of the planet-and even the extent to which it can be considered to be confirmed-has been debated in the recent literature, with six mass measurements published so far based on the same spectroscopic observations, ranging from about 2 to 8 Earth masses. Here we report on an independent validation of the planet discovery using one of the fundamental properties of a transit signal: its achromaticity. We observed four transits of CoRoT-7 b at 4.5 mu m and 8.0 mu m with the Infrared Array Camera (IRAC) on board the Spitzer Space Telescope in order to determine whether the depth of the transit signal in the near-infrared is consistent with that observed in the CoRoT bandpass, as expected for a planet. We detected the transit and found an average depth of 0.426 +/- 0.115 mmag at 4.5 mu m, which is in good agreement with the depth of 0.350 +/- 0.011 mmag (ignoring limb darkening) found by CoRoT. The observations at 8.0 mu m did not yield a significant detection. The 4.5 mu m observations place important constraints on the kinds of astrophysical false positives that could mimic the signal. Combining this with additional constraints reported earlier, we performed an exhaustive exploration of possible blend scenarios for CoRoT-7 b using the BLENDER technique. We are able to rule out the vast majority of false positives, and the remaining ones are found to be much less likely than a true transiting planet. We thus validate CoRoT-7 b as a bona fide planet with a very high degree of confidence, independently of any radial-velocity information. Our Spitzer observations have additionally allowed us to significantly improve the ephemeris of the planet, so that future transits should be recoverable well into the next decade. In its warm phase Spitzer is expected to be an essential tool for the validation, along the lines of the present analysis, of transiting planet candidates with shallow signals from CoRoT as well as from the Kepler mission, including potentially rocky planets in the habitable zones of their parent stars. C1 [Fressin, Francois; Torres, Guillermo; Charbonneau, David] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Pont, Frederic] Univ Exeter, Sch Phys, Exeter EX4 4QL, Devon, England. [Knutson, Heather A.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Mazeh, Tsevi] Tel Aviv Univ, Dept Astron & Astrophys, IL-69978 Tel Aviv, Israel. [Aigrain, Suzanne] Univ Oxford, Oxford OX1 3RH, England. [Fridlund, Malcolm] ESTEC ESA, NL-2200 AG Noordwijk, Netherlands. [Henze, Christopher E.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Guillot, Tristan] Observ Cote Azur, F-06304 Nice, France. [Rauer, Heike] Deutsch Zentrum Luft & Raumfahrt DLR, D-12489 Berlin, Germany. RP Fressin, F (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM ffressin@cfa.harvard.edu OI Charbonneau, David/0000-0002-9003-484X FU NASA FX We are grateful to the anonymous referee for many very helpful comments and suggestions. This work is based on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract to NASA. Support for this work was provided by NASA through an award issued by JPL/Caltech. This research has made use of the facilities at the NASA Advanced Supercomputing Division (NASA Ames Research Center). NR 42 TC 9 Z9 9 U1 1 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JAN 20 PY 2012 VL 745 IS 1 AR 81 DI 10.1088/0004-637X/745/1/81 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 892WP UT WOS:000300316600081 ER PT J AU Liu, HB Quintana-Lacaci, G Wang, K Ho, PTP Li, ZY Zhang, QZ Zhang, ZY AF Liu, Hauyu Baobab Quintana-Lacaci, Guillermo Wang, Ke Ho, Paul T. P. Li, Zhi-Yun Zhang, Qizhou Zhang, Zhi-Yu TI THE ORIGIN OF OB CLUSTERS: FROM 10 pc TO 0.1 pc SO ASTROPHYSICAL JOURNAL LA English DT Article DE H II regions; ISM: individual objects (G10.6-0.4); ISM: kinematics and dynamics; stars: evolution; stars: formation; stars: massive ID MASSIVE STAR-FORMATION; OUTFLOW-DRIVEN TURBULENCE; ULTRACOMPACT HII-REGIONS; INFRARED DARK CLOUD; MAGNETIC-FIELDS; MOLECULAR CLOUDS; ACCRETION FLOW; FORMING REGION; SUBMILLIMETER ARRAY; SHEET-LIKE AB We observe the 1.2 mm continuum emission around the OB cluster-forming region G10.6-0.4, using the MAMBO-2 bolometer array of the IRAM 30 m telescope and the Submillimeter Array (SMA). Comparison of the Spitzer 24 mu m and 8 mu m images with our 1.2 mm continuum maps reveal an ionization front of an H II region, the photon-dominated layer, and several 5 pc scale filaments that follow the outer edge of the photon-dominated layer. The filaments, which are resolved in the MAMBO-2 observations, show regularly spaced parsec-scale molecular clumps, embedded with a cluster of dense molecular cores as shown in the SMA 0.87 mm observations. Toward the center of the G10.6-0.4 region, the combined SMA+IRAM 30 m continuum image reveals several parsec-scale protrusions. They may continue down to within 0.1 pc of the geometric center of a dense 3 pc scale structure, where a 200 M-circle dot OB cluster resides. The observed filaments may facilitate mass accretion onto the central cluster-forming region in the presence of strong radiative and mechanical stellar feedback. Their filamentary geometry may also facilitate fragmentation. We did not detect any significant polarized emission at 0.87 mm in the inner 1 pc region with SMA. C1 [Ho, Paul T. P.] Acad Sinica, Inst Astron & Astrophys, Taipei 106, Taiwan. [Liu, Hauyu Baobab; Wang, Ke; Ho, Paul T. P.; Zhang, Qizhou] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Quintana-Lacaci, Guillermo] Inst Radioastron Milimetr, Granada 18012, Spain. [Wang, Ke] Peking Univ, Sch Phys, Dept Astron, Beijing 100871, Peoples R China. [Li, Zhi-Yun] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA. [Zhang, Zhi-Yu] Max Planck Inst Radioastron, D-53121 Bonn, Germany. RP Liu, HB (reprint author), Acad Sinica, Inst Astron & Astrophys, POB 23-141, Taipei 106, Taiwan. EM hlu@cfa.havard.edu; quintana@iram.es; kwang@cfa.harvard.edu; pho@asiaa.sinica.edu.tw; zl4h@virginia.edu; qzhang@cfa.harvard.edu; zzhang@mpifr.de OI Wang, Ke/0000-0002-7237-3856; Quintana-Lacaci, Guillermo/0000-0002-5417-1943; Zhang, Qizhou/0000-0003-2384-6589; Zhang, Zhiyu/0000-0002-7299-2876 FU SMA; China Scholarship Council; Smithsonian Institution; Academia Sinica; INSU/CNRS (France); MPG (Germany); IGN (Spain) FX The Submillimeter Array is a joint project between the Smithsonian Astrophysical Observatory and the Academia Sinica Institute of Astronomy and Astrophysics, and is funded by the Smithsonian Institution and the Academia Sinica.; IRAM is supported by INSU/CNRS (France), MPG (Germany), and IGN (Spain).; We thank the SMA staff for making these observations possible. We also thank the IRAM staff for help with the observations and for developing the data reduction routines. H. B. Liu thanks ASIAA for supporting this research. 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. We thank the GLIMPSE team (PI: E. Churchwell) and MIPSGAL team (PI: S. Carey) for making the IRAC and MIPS images available to the community. K. W. acknowledges the support from the SMA predoctoral fellowship and the China Scholarship Council. NR 56 TC 11 Z9 11 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JAN 20 PY 2012 VL 745 IS 1 AR 61 DI 10.1088/0004-637X/745/1/61 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 892WP UT WOS:000300316600061 ER PT J AU Liu, JF Orosz, J Bregman, JN AF Liu, Jifeng Orosz, Jerome Bregman, Joel N. TI DYNAMICAL MASS CONSTRAINTS ON THE ULTRALUMINOUS X-RAY SOURCE NGC 1313 X-2 SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; black hole physics; X-rays: binaries; X-rays: individual (NGC 1313 X-2) ID SOURCE NGC-1313 X-2; BLACK-HOLE; OPTICAL COUNTERPART; BINARY-SYSTEMS; STELLAR; MULTIWAVELENGTH; ENVIRONMENT; EMISSION; GALAXIES; CLUSTERS AB Dynamical mass measurements hold the key to answering whether ultraluminous X-ray sources (ULXs) are intermediate-mass black holes (IMBHs) or stellar-mass black holes with special radiation mechanisms. NGC 1313 X-2 is so far the only ULX with Hubble Space Telescope light curves, the orbital period, and the black hole's radial velocity amplitude based on the He II lambda 4686 disk emission line shift of similar to 200 km s(-1). We constrain its black hole mass and other parameters by fitting observations to a binary light curve code with accommodations for X-ray heating of the accretion disk and the secondary. Given the dynamical constraints from the observed light curves and the black hole radial motion and the observed stellar environment age, the only acceptable models are those with 40-50 Myr old intermediate-mass secondaries in their helium core and hydrogen shell burning phase filling 40%-80% of their Roche lobes. The black hole can be a massive black hole of a few tens of M-circle dot that can be produced from stellar evolution of low-metallicity stars, or an IMBH of a few hundred to above 1000 M-circle dot if its true radial velocity 2K' < 40 km s(-1). Further observations are required to better measure the black hole radial motion and the light curves in order to determine whether NGC1313 X-2 is a stellar-mass black hole or an IMBH. C1 [Liu, Jifeng] Natl Astron Observ China, Beijing 100012, Peoples R China. [Liu, Jifeng] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Orosz, Jerome] San Diego State Univ, Dept Astron, San Diego, CA 92182 USA. [Bregman, Joel N.] Univ Michigan, Dept Astron, Ann Arbor, MI USA. RP Liu, JF (reprint author), Natl Astron Observ China, Beijing 100012, Peoples R China. FU FAS Science Division Research Computing Group at Harvard University FX We thank Dr. Jeffery E. MaClintock and Rosanne Di Stefano for helpful discussions. The computations in this paper were run on the Odyssey cluster supported by the FAS Science Division Research Computing Group at Harvard University. NR 52 TC 11 Z9 11 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JAN 20 PY 2012 VL 745 IS 1 AR 89 DI 10.1088/0004-637X/745/1/89 PG 22 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 892WP UT WOS:000300316600089 ER PT J AU Liu, X Shen, Y Strauss, MA AF Liu, Xin Shen, Yue Strauss, Michael A. TI ACTIVE GALACTIC NUCLEUS PAIRS FROM THE SLOAN DIGITAL SKY SURVEY. II. EVIDENCE FOR TIDALLY ENHANCED STAR FORMATION AND BLACK HOLE ACCRETION SO ASTROPHYSICAL JOURNAL LA English DT Article DE black hole physics; galaxies: active; galaxies: interactions; galaxies: nuclei; galaxies: stellar content ID EARLY-TYPE GALAXIES; NARROW-LINE REGION; HUBBLE-SPACE-TELESCOPE; LOW-REDSHIFT GALAXIES; EXTENDED GROTH STRIP; XMM-NEWTON SURVEYS; RAY SELECTED AGN; HARD X-RAY; DATA RELEASE; INTERACTING GALAXIES AB Active galactic nuclei (AGNs) are occasionally seen in pairs, suggesting that tidal encounters are responsible for the accretion of material by both central supermassive black holes (BHs). In Paper I of this series, we selected a sample of AGN pairs with projected separations rp < 100 h(-1) 70 kpc and velocity offsets < 600 km s(-1) from the Seventh Data Release of the Sloan Digital Sky Survey and quantified their frequency. In this paper, we address the BH accretion and recent star formation properties in their host galaxies. AGN pairs experience stronger BH accretion, as measured by their [O III] lambda 5007 luminosities (corrected for contribution from star formation) and Eddington ratios, than do control samples of single AGNs matched in redshift and host-galaxy stellar mass. Their host galaxies have stronger post-starburst activity and younger mean stellar ages, as indicated by stronger Hd absorption and smaller 4000 angstrom break in their spectra. The BH accretion and recent star formation in the host galaxies both increase with decreasing projected separation in AGN pairs, for r(p) less than or similar to 10-30 h(70)(-1) kpc. The intensity of BH accretion, the post-starburst strength, and the mean stellar ages are correlated between the two AGNs in a pair. The luminosities and Eddington ratios of AGN pairs are correlated with recent star formation in their host galaxies, with a scaling relation consistent with that observed in single AGNs. Our results suggest that galaxy tidal interactions enhance both BH accretion and host-galaxy star formation in close AGN pairs, even though the majority of low-redshift AGNs are not coincident with on-going interactions. C1 [Liu, Xin; Shen, Yue] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Liu, Xin; Strauss, Michael A.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. RP Liu, X (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. FU NSF [AST-0707266, PF0-110076, NAS8-03060]; Clay Postdoctoral Fellowship FX X. L. thanks J. Goodman, J. Gunn, and J. Krolik for helpful comments on selection effects in the observed correlations. X. L. and M. A. S. acknowledge the support of NSF grant AST-0707266. Support for the work of X. L. was provided by NASA through Einstein Postdoctoral Fellowship grant number PF0-110076 awarded by the Chandra X-ray Center, which is operated by the Smithsonian Astrophysical Observatory for NASA under contract NAS8-03060. Y.S. acknowledges support from a Clay Postdoctoral Fellowship through the Smithsonian Astrophysical Observatory. NR 160 TC 35 Z9 35 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JAN 20 PY 2012 VL 745 IS 1 AR 94 DI 10.1088/0004-637X/745/1/94 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 892WP UT WOS:000300316600094 ER PT J AU Mainzer, A Masiero, J Grav, T Bauer, J Tholen, DJ McMillan, RS Wright, E Spahr, T Cutri, RM Walker, R Mo, W Watkins, J Hand, E Maleszewski, C AF Mainzer, A. Masiero, J. Grav, T. Bauer, J. Tholen, D. J. McMillan, R. S. Wright, E. Spahr, T. Cutri, R. M. Walker, R. Mo, W. Watkins, J. Hand, E. Maleszewski, C. TI NEOWISE STUDIES OF ASTEROIDS WITH SLOAN PHOTOMETRY: PRELIMINARY RESULTS SO ASTROPHYSICAL JOURNAL LA English DT Article DE atlases; catalogs; infrared: general; minor planets, asteroids: general; surveys ID DIGITAL SKY SURVEY; NEAR-EARTH ASTEROIDS; THERMAL-MODEL CALIBRATION; INFRARED-SURVEY-EXPLORER; MAIN BELT ASTEROIDS; SPECTROSCOPIC SURVEY; MINOR PLANETS; DATA RELEASE; PHASE-II; TAXONOMY AB We have combined the NEOWISE and Sloan Digital Sky Survey data to study the albedos of 24,353 asteroids with candidate taxonomic classifications derived using Sloan photometry. We find a wide range of moderate to high albedos for candidate S-type asteroids that are analogous to the S complex defined by previous spectrophotometrically based taxonomic systems. The candidate C-type asteroids, while generally very dark, have a tail of higher albedos that overlaps the S types. The albedo distribution for asteroids with a photometrically derived Q classification is extremely similar to those of the S types. Asteroids with similar colors to (4) Vesta have higher albedos than the S types, and most have orbital elements similar to known Vesta family members. Finally, we show that the relative reflectance at 3.4 and 4.6 mu m is higher for D-type asteroids and suggest that their red visible and near-infrared spectral slope extends out to these wavelengths. Understanding the relationship between size, albedo, and taxonomic classification is complicated by the fact that the objects with classifications were selected from the visible/near-infrared Sloan Moving Object Catalog, which is biased against fainter asteroids, including those with lower albedos. C1 [Mainzer, A.; Masiero, J.; Bauer, J.; Hand, E.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Grav, T.; Mo, W.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Bauer, J.; Cutri, R. M.] CALTECH, Ctr Infrared Proc & Anal, Pasadena, CA 91125 USA. [Tholen, D. J.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [McMillan, R. S.; Maleszewski, C.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA. [Wright, E.; Watkins, J.] UCLA Div Astron & Astrophys, Los Angeles, CA 90095 USA. [Spahr, T.] Harvard Smithsonian Ctr Astrophys, Minor Planet Ctr, Cambridge, MA 02138 USA. [Walker, R.] Monterey Inst Res Astron, Monterey, CA USA. RP Mainzer, A (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. OI Masiero, Joseph/0000-0003-2638-720X FU National Aeronautics and Space Administration; Planetary Science Division of the National Aeronautics and Space Administration FX This publication makes use of data products from the Widefield 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 publication also makes use of data products from NEOWISE, which is a project of the Jet Propulsion Laboratory/California Institute of Technology, funded by the Planetary Science Division of the National Aeronautics and Space Administration. We thank our referee, Dr. Schelte J. Bus, for his comments, which have greatly improved this paper. We gratefully acknowledge the extraordinary services specific to NEOWISE contributed by the International Astronomical Union's Minor Planet Center, operated by the Harvard-Smithsonian Center for Astrophysics, and the Central Bureau for Astronomical Telegrams, operated by Harvard University. This research has made use of the NASA/IPAC Infrared Science Archive, which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. NR 46 TC 13 Z9 13 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JAN 20 PY 2012 VL 745 IS 1 AR 7 DI 10.1088/0004-637X/745/1/7 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 892WP UT WOS:000300316600007 ER PT J AU Ness, JU Schaefer, BE Dobrotka, A Sadowski, A Drake, JJ Barnard, R Talavera, A Gonzalez-Riestra, R Page, KL Hernanz, M Sala, G Starrfield, S AF Ness, J. -U. Schaefer, B. E. Dobrotka, A. Sadowski, A. Drake, J. J. Barnard, R. Talavera, A. Gonzalez-Riestra, R. Page, K. L. Hernanz, M. Sala, G. Starrfield, S. TI FROM X-RAY DIPS TO ECLIPSE: WITNESSING DISK REFORMATION IN THE RECURRENT NOVA U Sco SO ASTROPHYSICAL JOURNAL LA English DT Article DE novae, cataclysmic variables; stars: individual (U Sco) ID PHOTON IMAGING CAMERA; XMM-NEWTON; LIGHT-CURVE; CATACLYSMIC VARIABLES; GRATING SPECTROMETER; LINE DIAGNOSTICS; V382 VELORUM; WHITE-DWARF; SSS SPECTRA; OUTBURST AB The tenth recorded outburst of the recurrent eclipsing nova U Sco was observed simultaneously in X-ray, UV, and optical by XMM-Newton on days 22.9 and 34.9 after the outburst. Two full passages of the companion in front of the nova ejecta were observed, as was the reformation of the accretion disk. On day 22.9, we observed smooth eclipses in UV and optical but deep dips in the X-ray light curve that disappeared by day 34.9, yielding clean eclipses in all bands. X-ray dips can be caused by clumpy absorbing material that intersects the line of sight while moving along highly elliptical trajectories. Cold material from the companion could explain the absence of dips in UV and optical light. The disappearance of X-ray dips before day 34.9 implies significant progress in the formation of the disk. The X-ray spectra contain photospheric continuum emission plus strong emission lines, but no clear absorption lines. Both continuum and emission lines in the X-ray spectra indicate a temperature increase from day 22.9 to day 34.9. We find clear evidence in the spectra and light curves for Thompson scattering of the photospheric emission from the white dwarf. Photospheric absorption lines can be smeared out during scattering in a plasma of fast electrons. We also find spectral signatures of resonant line scattering that lead to the observation of the strong emission lines. Their dominance could be a general phenomenon in high-inclination systems such as Cal 87. C1 [Ness, J. -U.; Talavera, A.; Gonzalez-Riestra, R.] ESA, XMM Newton Sci Operat Ctr, Madrid 28691, Spain. [Schaefer, B. E.] Louisiana State Univ, Dept Phys & Astron, Baton Rouge, LA 70803 USA. [Dobrotka, A.] Slovak Tech Univ Bratislava, Dept Phys, Inst Mat Sci, Fac Mat Sci & Technol, Trnava 91724, Slovakia. [Dobrotka, A.] Kyoto Univ, Grad Sch Sci, Dept Astron, Sakyo Ku, Kyoto 6068502, Japan. [Sadowski, A.] Polish Acad Sci, N Copernicus Astron Ctr, PL-00716 Warsaw, Poland. [Drake, J. J.; Barnard, R.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Page, K. L.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. [Hernanz, M.] Fac Ciencies, Inst Ciencies Espai CSIC IEEC, Bellaterra 08193, Barcelona, Spain. [Sala, G.] EUETIB UPC IEEC, Dept Fis & Engn Nucl, Barcelona 08036, Spain. [Starrfield, S.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA. RP Ness, JU (reprint author), ESA, XMM Newton Sci Operat Ctr, POB 78, Madrid 28691, Spain. EM juness@sciops.esa.int RI Hernanz, Margarita/K-1770-2014 OI Hernanz, Margarita/0000-0002-8651-7910 FU NASA [NAS8-39073]; National Science Foundation [AST 0708079]; MEXT; Slovak Grant Agency [VEGA-1/0520/10]; NASA+NSF; MICINN [AYA 2008-01839/ESP, AYA2008-04211-C02-01, AYA2010-15685]; AGAUR [SGR 315]; FEDER funds; GS MICINN [AYA 2008-04211-C02-01, AYA 2007-66256]; ESF EUROCORES [EUI2009-04167]; ESA Member States; STFC FX This paper is based on observations obtained with XMM-Newton, an ESA science mission with instruments and contributions directly funded by ESA Member States and NASA. We thank the XMM-Newton Science Operations Centre for efficient scheduling and for generously granting Director's Discretionary Time for the second observation. B.E.S. was supported under a grant from the National Science Foundation (AST 0708079). A.D. was supported in part by the Grant-in-Aid for the global COE programs on "The Next Generation of Physics, Spun from Diversity and Emergence" from MEXT and also by the Slovak Grant Agency, grant VEGA-1/0520/10. K. L. P. acknowledges support from STFC. J.J.D. was supported by NASA contract NAS8-39073 to the Chandra X-Ray Center. S.S. acknowledges support from NASA+NSF grants to ASU. M.H. acknowledges support from MICINN project AYA 2008-01839/ESP, AGAUR project 2009 SGR 315 and FEDER funds, and GS MICINN projects AYA 2008-04211-C02-01 and AYA 2007-66256. G. S. acknowledges MICINN grants AYA2008-04211-C02-01 and AYA2010-15685, and ESF EUROCORES Program EuroGENESIS grant EUI2009-04167. NR 51 TC 22 Z9 22 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JAN 20 PY 2012 VL 745 IS 1 AR 43 DI 10.1088/0004-637X/745/1/43 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 892WP UT WOS:000300316600043 ER PT J AU Quinn, SN Bakos, GA Hartman, J Torres, G Kovacs, G Latham, DW Noyes, RW Fischer, DA Johnson, JA Marcy, GW Howard, AW Szentgyorgyi, A Furesz, G Buchhave, LA Beky, B Sasselov, DD Stefanik, RP Perumpilly, G Everett, M Lazar, J Papp, I Sari, P AF Quinn, S. N. Bakos, G. A. Hartman, J. Torres, G. Kovacs, G. Latham, D. W. Noyes, R. W. Fischer, D. A. Johnson, J. A. Marcy, G. W. Howard, A. W. Szentgyorgyi, A. Furesz, G. Buchhave, L. A. Beky, B. Sasselov, D. D. Stefanik, R. P. Perumpilly, G. Everett, M. Lazar, J. Papp, I. Sari, P. TI HAT-P-25b: A HOT-JUPITER TRANSITING A MODERATELY FAINT G STAR SO ASTROPHYSICAL JOURNAL LA English DT Article DE planetary systems; stars: individual (HAT-P-25, GSC 1788-01237); techniques: photometric techniques: spectroscopic ID M-J PLANET; EXTRASOLAR PLANET; BRIGHT STAR; K-DWARF; RADIAL-VELOCITIES; ECCENTRIC ORBIT; KEPLER FIELD; STELLAR; MASS; EMISSION AB We report the discovery of HAT-P-25b, a transiting extrasolar planet orbiting the V = 13.19 G5 dwarf star GSC 1788-01237, with a period P = 3.652836 +/- 0.000019 days, transit epoch T-c = 2455176.85173 +/- 0.00047 (BJD-barycentric Julian dates throughout the paper are calculated from Coordinated Universal Time, UTC), and transit duration 0.1174 +/- 0.0017 days. The host star has a mass of 1.01 +/- 0.03 M-circle dot, radius of 0.96(-0.04)(+0.05)R(circle dot), effective temperature 5500 +/- 80 K, and metallicity [Fe/H] = +0.31 +/- 0.08. The planetary companion has a mass of 0.567 +/- 0.022 M-J and radius of 1.190(-0.056)(+0.081) R-J yielding a mean density of 0.42 +/- 0.07 g cm(-3). C1 [Quinn, S. N.; Bakos, G. A.; Hartman, J.; Torres, G.; Latham, D. W.; Noyes, R. W.; Szentgyorgyi, A.; Furesz, G.; Buchhave, L. A.; Beky, B.; Sasselov, D. D.; Stefanik, R. P.; Perumpilly, G.; Everett, M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Kovacs, G.] Konkoly Observ Budapest, Budapest, Hungary. [Fischer, D. A.] Yale Univ, Dept Astron, New Haven, CT 06511 USA. [Johnson, J. A.] CALTECH, Dept Astrophys, Pasadena, CA 91125 USA. [Marcy, G. W.; Howard, A. W.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Buchhave, L. A.] Univ Copenhagen, Niels Bohr Inst, DK-2100 Copenhagen, Denmark. [Perumpilly, G.] Univ S Dakota, Dept Phys, Vermillion, SD 57069 USA. [Lazar, J.; Papp, I.; Sari, P.] Hungarian Astron Assoc, Budapest, Hungary. RP Quinn, SN (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM gbakos@cfa.harvard.edu RI Howard, Andrew/D-4148-2015; OI Howard, Andrew/0000-0001-8638-0320; Buchhave, Lars A./0000-0003-1605-5666; Hartman, Joel/0000-0001-8732-6166 FU NASA [NNG04GN74G, NNX08AF23G, NNX09AF59G]; SAO IRD; NSF [AST-0702843, AST-0702821]; Kepler Mission under NASA [NCC2-1390]; Hungarian Scientific Research Foundation (OTKA) [K-81373] FX HATNet operations have been funded by NASA grants NNG04GN74G, NNX08AF23G, and SAO IR&D grants. Work of G.A.B. and J. Johnson were supported by the Postdoctoral Fellowship of the NSF Astronomy and Astrophysics Program (AST-0702843 and AST-0702821, respectively). G. T. acknowledges partial support from NASA grant NNX09AF59G. We acknowledge partial support also from the Kepler Mission under NASA Cooperative Agreement NCC2-1390 (PI: D. W. Latham). G. K. thanks the Hungarian Scientific Research Foundation (OTKA) for support through grant K-81373. This research has made use of Keck telescope time granted through NOAO (A201Hr), NASA (N018Hr and N167Hr), and the NASA Gemini-Keck time-exchange program (G329Hr). This research has also made use of the NASA/IPAC Infrared Science Archive, which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. NR 53 TC 12 Z9 12 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JAN 20 PY 2012 VL 745 IS 1 AR 80 DI 10.1088/0004-637X/745/1/80 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 892WP UT WOS:000300316600080 ER PT J AU Sanna, A Reid, MJ Dame, TM Menten, KM Brunthaler, A Moscadelli, L Zheng, XW Xu, Y AF Sanna, A. Reid, M. J. Dame, T. M. Menten, K. M. Brunthaler, A. Moscadelli, L. Zheng, X. W. Xu, Y. TI TRIGONOMETRIC PARALLAXES OF MASSIVE STAR-FORMING REGIONS. IX. THE OUTER ARM IN THE FIRST QUADRANT SO ASTROPHYSICAL JOURNAL LA English DT Article DE astrometry; Galaxy: fundamental parameters; Galaxy: kinematics and dynamics; masers; stars: formation; techniques: high angular resolution ID MILKY-WAY-GALAXY; SPIRAL ARMS; MOLECULAR CLOUDS; VELOCITY-FIELD; 3-DIMENSIONAL DISTRIBUTION; PERIODIC PATTERN; DISK; KINEMATICS; ASTROMETRY; DISTANCES AB We report a trigonometric parallax measurement with the Very Long Baseline Array for the water maser in the distant high-mass star-forming region G75.30+1.32. This source has a heliocentric distance of 9.25(-0.40)(+0.45) kpc, which places it in the Outer arm in the first Galactic quadrant. It lies 200 pc above the Galactic plane and is associated with a substantial H i enhancement at the border of a large molecular cloud. At a Galactocentric radius of 10.7 kpc, G75.30+1.32 is in a region of the Galaxy where the disk is significantly warped toward the North Galactic Pole. While the star-forming region has an instantaneous Galactic orbit that is nearly circular, it displays a significant motion of 18 km s(-1) toward the Galactic plane. The present results, when combined with two previous maser studies in the Outer arm, yield a pitch angle of about 12 degrees for a large section of the arm extending from the first quadrant to the third. C1 [Sanna, A.; Menten, K. M.; Brunthaler, A.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Reid, M. J.; Dame, T. M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Moscadelli, L.] Osserv Astrofis Arcetri, INAF, I-50125 Florence, Italy. [Zheng, X. W.] Nanjing Univ, Dept Astron, Nanjing 210093, Jiangsu, Peoples R China. [Xu, Y.] Chinese Acad Sci, Purple Mt Observ, Nanjing 210093, Jiangsu, Peoples R China. RP Sanna, A (reprint author), Max Planck Inst Radioastron, Hugel 69, D-53121 Bonn, Germany. EM asanna@mpifr-bonn.mpg.de OI Moscadelli, Luca/0000-0002-8517-8881 FU ERC [247078]; Chinese NSF [NSF 11073054, NSF 10733030, NSF 10621303] FX This work was partially funded by the ERC Advanced Investigator Grant GLOSTAR (247078). Y.X. was supported by the Chinese NSF through grants NSF 11073054, NSF 10733030, and NSF 10621303. NR 35 TC 22 Z9 22 U1 1 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JAN 20 PY 2012 VL 745 IS 1 AR 82 DI 10.1088/0004-637X/745/1/82 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 892WP UT WOS:000300316600082 ER PT J AU Strachan, L Panasyuk, AV Kohl, JL Lamy, P AF Strachan, L. Panasyuk, A. V. Kohl, J. L. Lamy, P. TI THE EVOLUTION OF PLASMA PARAMETERS ON A CORONAL SOURCE SURFACE AT 2.3 R-circle dot DURING SOLAR MINIMUM SO ASTROPHYSICAL JOURNAL LA English DT Article DE solar wind; Sun: corona; techniques: spectroscopic ID WHOLE SUN MONTH; ANISOTROPIC VELOCITY DISTRIBUTIONS; 3-DIMENSIONAL RECONSTRUCTION; OUTFLOW VELOCITIES; WIND ACCELERATION; DENSITY STRUCTURE; STREAMER BELT; SLOW WIND; INTERPLANETARY; IONS AB We analyze data from the Solar and Heliospheric Observatory to produce global maps of coronal outflow velocities and densities in the regions where the solar wind is undergoing acceleration. The maps use UV and white light coronal data obtained from the Ultraviolet Coronagraph Spectrometer and the Large Angle Spectroscopic Coronagraph, respectively, and a Doppler dimming analysis to determine the mean outflow velocities. The outflow velocities are defined on a sphere at 2.3 R-circle dot from Sun-center and are organized by Carrington Rotations during the solar minimum period at the start of solar cycle 23. We use the outflow velocity and density maps to show that while the solar minimum corona is relatively stable during its early stages, the shrinkage of the north polar hole in the later stages leads to changes in both the global areal expansion of the coronal hole and the derived internal flux tube expansion factors of the solar wind. The polar hole areal expansion factor and the flux tube expansion factors (between the coronal base and 2.3 R-circle dot) start out as super-radial but then they become more nearly radial as the corona progresses away from solar minimum. The results also support the idea that the largest flux tube expansion factors are located near the coronal hole/streamer interface, at least during the deepest part of the solar minimum period. C1 [Strachan, L.; Panasyuk, A. V.; Kohl, J. L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Lamy, P.] Univ Aix Marseille 1, CNRS, UMR6110, Lab Astrophys Marseille, F-13388 Marseille 13, France. RP Strachan, L (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM lstrachan@cfa.harvard.edu FU NASA [NNG06GE74G, NNX07AB98G, NNX08AQ96G]; Smithsonian Astrophysical Observatory; Centre National d'Etudes Spatiales (CNES) FX This work was supported in part by NASA grants NNG06GE74G, NNX07AB98G, and NNX08AQ96G to the Smithsonian Astrophysical Observatory. The LASCO-C2 project at the Laboratoire d'Astrophysique de Marseille (formerly Laboratoire d'Astronomie Spatiale) is funded by the Centre National d'Etudes Spatiales (CNES). UVCS and LASCO are part of SOHO, which is a project of international cooperation between ESA and NASA. The authors acknowledge the use of sunspot data from the World Data Center for the Sunspot Index, Royal Observatory of Belgium; and coronal source surface magnetic field data from the Wilcox Solar Observatory Web site at http://wso.stanford.edu/synsourcel.html. We also thank S. R. Cranmer for supplying the results of his theoretical model for comparing to our data and an anonymous referee for providing useful comments on the manuscript. NR 66 TC 6 Z9 6 U1 1 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JAN 20 PY 2012 VL 745 IS 1 AR 51 DI 10.1088/0004-637X/745/1/51 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 892WP UT WOS:000300316600051 ER PT J AU Temim, T Slane, P Arendt, RG Dwek, E AF Temim, Tea Slane, Patrick Arendt, Richard G. Dwek, Eli TI INFRARED AND X-RAY SPECTROSCOPY OF THE Kes 75 SUPERNOVA REMNANT SHELL: CHARACTERIZING THE DUST AND GAS PROPERTIES SO ASTROPHYSICAL JOURNAL LA English DT Article DE dust, extinction; infrared: ISM; ISM: individual objects (SNR G29.7-0.3); ISM: supernova remnants; pulsars: individual (PSR J1846-0258); X-rays: ISM ID SPITZER-SPACE-TELESCOPE; LARGE-MAGELLANIC-CLOUD; INTERSTELLAR-MEDIUM; EARLY UNIVERSE; RADIO OBSERVATIONS; GALACTIC PLANE; PSR J1846-0258; DESTRUCTION; CASSIOPEIA; PULSAR AB We present deep Chandra observations and Spitzer Space Telescope infrared (IR) spectroscopy of the shell in the composite supernova remnant (SNR) Kes 75 (G29.7-0.3). The remnant is composed of a central pulsar wind nebula and a bright partial shell in the south that is visible at radio, IR, and X-ray wavelengths. The X-ray emission can be modeled by either a single thermal component with a temperature of similar to 1.5 keV, or with two thermal components with temperatures of 1.5 and 0.2 keV. Previous studies suggest that the hot component may originate from reverse-shocked supernova (SN) ejecta. However, our new analysis shows no definitive evidence for enhanced abundances of Si, S, Ar, Mg, and Fe, as expected from SN ejecta, or for the IR spectral signatures characteristic of confirmed SN condensed dust, thus favoring a circumstellar or interstellar origin for the X-ray and IR emission. The X-ray and IR emission in the shell are spatially correlated, suggesting that the dust particles are collisionally heated by the X-ray emitting gas. The IR spectrum of the shell is dominated by continuum emission from dust with little, or no line emission. Modeling the IR spectrum shows that the dust is heated to a temperature of similar to 140 K by a relatively dense, hot plasma that also gives rise to the hot X-ray emission component. The density inferred from the IR emission is significantly higher than the density inferred from the X-ray models, suggesting a low filling factor for this X-ray emitting gas. The total mass of the warm dust component is at least 1.3 x 10(-2) M-circle dot, assuming no significant dust destruction has occurred in the shell. The IR data also reveal the presence of an additional plasma component with a cooler temperature, consistent with the 0.2 keV gas component. Our IR analysis therefore provides an independent verification of the cooler component of the X-ray emission. The complementary analyses of the X-ray and IR emission provide quantitative estimates of density and filling factors of the clumpy medium swept up by the SNR. C1 [Temim, Tea; Arendt, Richard G.] NASA, Goddard Space Flight Ctr, Observat Cosmol Lab, Greenbelt, MD 20771 USA. [Temim, Tea; Dwek, Eli] Oak Ridge Associated Univ, Oak Ridge, TN 37831 USA. [Slane, Patrick] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Arendt, Richard G.] Univ Maryland Baltimore Cty, CRESST, Baltimore, MD 21250 USA. RP Temim, T (reprint author), NASA, Goddard Space Flight Ctr, Observat Cosmol Lab, Code 665, Greenbelt, MD 20771 USA. EM tea.temim@nasa.gov RI Dwek, Eli/C-3995-2012; OI Arendt, Richard/0000-0001-8403-8548; Temim, Tea/0000-0001-7380-3144 FU NASA [RSA1343487, NAS8-03060] FX This work is partly 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 (RSA1343487). The research has made use of software provided by the CXC in the application packages CIAO, ChIPS, and Sherpa. P.O.S. acknowledges partial support from NASA Contract NAS8-03060. We acknowledge Stephen Reynolds and Kazik Borkwoski at North Carolina State University for the useful discussion and suggestions, and George Sonneborn at NASA GSFC for helpful comments. NR 44 TC 8 Z9 8 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JAN 20 PY 2012 VL 745 IS 1 AR 46 DI 10.1088/0004-637X/745/1/46 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 892WP UT WOS:000300316600046 ER PT J AU Tonry, JL Stubbs, CW Kilic, M Flewelling, HA Deacon, NR Chornock, R Berger, E Burgett, WS Chambers, KC Kaiser, N Kudritzki, RP Hodapp, KW Magnier, EA Morgan, JS Price, PA Wainscoat, RJ AF Tonry, J. L. Stubbs, C. W. Kilic, M. Flewelling, H. A. Deacon, N. R. Chornock, R. Berger, E. Burgett, W. S. Chambers, K. C. Kaiser, N. Kudritzki, R. -P. Hodapp, K. W. Magnier, E. A. Morgan, J. S. Price, P. A. Wainscoat, R. J. TI FIRST RESULTS FROM Pan-STARRS1: FAINT, HIGH PROPER MOTION WHITE DWARFS IN THE MEDIUM-DEEP FIELDS SO ASTROPHYSICAL JOURNAL LA English DT Article DE Galaxy: evolution; proper motions; surveys; white dwarfs ID DIGITAL-SKY-SURVEY; LUMINOSITY FUNCTION; SPECTROSCOPIC ANALYSIS; GALACTIC HALO; STELLAR LOCUS; DARK-MATTER; CATALOG; STARS; OLD; EVOLUTION AB The Pan-STARRS1 survey has obtained multi-epoch imaging in five bands (Pan-STARRS1 g(P1), r(P1), i(P1), z(P1), and y(P1)) on 12 "Medium-Deep fields," each of which spans a 3 degrees. 3 circle. For the period between 2009 April and 2011 April these fields were observed 50-200 times. Using a reduced proper motion diagram, we have extracted a list of 47 white dwarf (WD) candidates whose Pan-STARRS1 astrometry indicates a non-zero proper motion at the 6 sigma level, with a typical 1 sigma proper motion uncertainty of 10 mas yr(-1). We also used astrometry from the Sloan Digital Sky Survey (when available) and USNO-B to assess our proper motion fits. None of the WD candidates exhibits evidence of statistically significant parallaxes, with a typical 1s uncertainty of 8 mas. Twelve of these candidates are known WDs, including the high proper motion (1".7 yr(-1)) WD LIIS 291. We confirm seven more objects as WDs through optical spectroscopy. Based on the Pan-STARRS1 colors, ten of the stars are likely to be cool WDs with 4170 K < T-eff < 5000 K and cooling ages approximate to 8 Gyr. Based on their kinematics, these objects are likely thick disk WDs, but a subset may belong to the halo. Our current sample represents only a small fraction of the Pan-STARRS1 data. With continued coverage from the Medium-Deep Field Survey and the 3 pi survey, Pan-STARRS1 should find many more high proper motion WDs that are part of the old thick disk and halo. C1 [Tonry, J. L.; Flewelling, H. A.; Deacon, N. R.; Burgett, W. S.; Chambers, K. C.; Kaiser, N.; Kudritzki, R. -P.; Hodapp, K. W.; Magnier, E. A.; Morgan, J. S.; Wainscoat, R. J.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Stubbs, C. W.; Kilic, M.; Chornock, R.; Berger, E.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Stubbs, C. W.] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. [Kilic, M.] Univ Oklahoma, Homer L Dodge Dept Phys & Astron, Norman, OK 73019 USA. [Price, P. A.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. RP Tonry, JL (reprint author), Univ Hawaii, Inst Astron, 2680 Woodlawn Dr, Honolulu, HI 96822 USA. RI Stubbs, Christopher/C-2829-2012; OI Stubbs, Christopher/0000-0003-0347-1724; Chambers, Kenneth /0000-0001-6965-7789; Flewelling, Heather/0000-0002-1050-4056 FU National Science Foundation [AST-1009749]; Smithsonian Astrophysical Observatory; NASA's Astrophysics Data System Bibliographic Services; SIMBAD FX Support for this work was provided by National Science Foundation grant AST-1009749. The PS1 Surveys have been made possible through contributions of the Institute for Astronomy, the University of Hawaii, the Pan-STARRS Project Office, the Max-Planck Society and its participating institutes, the Max Planck Institute for Astronomy, Heidelberg and the Max Planck Institute for Extraterrestrial Physics, Garching, The Johns Hopkins University, Durham University, the University of Edinburgh, Queen's University Belfast, the Harvard-Smithsonian Center for Astrophysics, and the Las Cumbres Observatory Global Telescope Network, Incorporated, the National Central University of Taiwan, and the National Aeronautics and Space Administration under Grant No. NNX08AR22G issued through the Planetary Science Division of the NASA Science Mission Directorate.; The spectroscopic observations reported here were obtained at the MMT Observatory, a joint facility of the Smithsonian Institution and the University of Arizona. This paper uses data products produced by the OIR Telescope Data Center, supported by the Smithsonian Astrophysical Observatory, and we have benefited from NASA's Astrophysics Data System Bibliographic Services and the SIMBAD database, operated at CDS, Strasbourg, France. NR 43 TC 29 Z9 29 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JAN 20 PY 2012 VL 745 IS 1 AR 42 DI 10.1088/0004-637X/745/1/42 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 892WP UT WOS:000300316600042 ER PT J AU Ueda, J Iono, D Petitpas, G Yun, MS Ho, PTP Kawabe, R Mao, RQ Martin, S Matsushita, S Peck, AB Tamura, Y Wang, JZ Wang, Z Wilson, CD Zhang, QZ AF Ueda, Junko Iono, Daisuke Petitpas, Glen Yun, Min S. Ho, Paul T. P. Kawabe, Ryohei Mao, Rui-Qing Martin, Sergio Matsushita, Satoki Peck, Alison B. Tamura, Yoichi Wang, Junzhi Wang, Zhong Wilson, Christine D. Zhang, Qizhou TI UNVEILING THE PHYSICAL PROPERTIES AND KINEMATICS OF MOLECULAR GAS IN THE ANTENNAE GALAXIES (NGC 4038/9) THROUGH HIGH-RESOLUTION CO (J=3-2) OBSERVATIONS SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: individual (NGC 4038, NGC 4039); galaxies: interactions; galaxies: ISM; radio lines: galaxies ID LUMINOUS INFRARED GALAXIES; YOUNG STAR-CLUSTERS; X-RAY SOURCES; CHANDRA OBSERVATIONS; SUBMILLIMETER ARRAY; NEARBY GALAXIES; DISK GALAXIES; HIGH-REDSHIFT; CLOUDS; NGC-4038/4039 AB We present a similar to 1 '' (100 pc) resolution (CO)-C-12 (3-2) map of the nearby intermediate-stage interacting galaxy pair NGC 4038/9 (the Antennae galaxies) obtained with the Submillimeter Array. We find that half the CO (3-2) emission originates in the overlap region where most of the tidally induced star formation had been previously found in shorter wavelength images, with the rest being centered on each of the nuclei. The gross distribution is consistent with lower resolution single-dish images, but we show for the first time the detailed distribution of the warm and dense molecular gas across this galaxy pair at resolutions comparable to the size of a typical giant molecular complex. While we find that 58% (33/57) of the spatially resolved Giant Molecular Associations (a few x 100 pc) are located in the overlap region, only <= 30% spatially coincides with the optically detected star clusters, suggesting that the bulk of the CO (3-2) emission traces the regions with very recent or near future star formation activity. The spatial distribution of the CO (3-2)/CO (1-0) integrated brightness temperature ratios mainly ranges between 0.3 and 0.6, which suggests that on average the CO (3-2) line in the Antennae is not completely thermalized and similar to the average values of nearby spirals. A higher ratio is seen in both nuclei and the southern complexes in the overlap region. A higher radiation field associated with intense star formation can account for the nucleus of NGC 4038 and the overlap region, but the nuclear region of NGC 4039 shows relatively little star formation or active galactic nucleus activity and cannot be easily explained. We show kinematical evidence that the high line ratio in NGC 4039 is possibly caused by gas inflow into the counter-rotating central disk. C1 [Ueda, Junko; Iono, Daisuke; Kawabe, Ryohei; Tamura, Yoichi] Natl Inst Nat Sci, Natl Astron Observ Japan, Nobeyama Radio Observ, Minamisa Ku, Minamimaki, Nagano 3841305, Japan. [Ueda, Junko] Univ Tokyo, Sch Sci, Dept Astron, Bunkyo Ku, Tokyo 1330033, Japan. [Ueda, Junko; Iono, Daisuke; Petitpas, Glen; Ho, Paul T. P.; Peck, Alison B.; Wang, Zhong; Zhang, Qizhou] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Yun, Min S.] Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA. [Ho, Paul T. P.; Matsushita, Satoki] Acad Sinica, Inst Astron & Astrophys, Taipei 10617, Taiwan. [Mao, Rui-Qing] Chinese Acad Sci, Purple Mt Observ, Nanjing 210008, Peoples R China. [Martin, Sergio] European So Observ, Santiago 19, Chile. [Matsushita, Satoki; Peck, Alison B.] Joint ALMA Observ, Santiago 19, Chile. [Tamura, Yoichi] Univ Tokyo, Inst Astron, Mitaka, Tokyo 1810015, Japan. [Wang, Junzhi] Nanjing Univ, Dept Astron, Nanjing 210093, Peoples R China. [Wilson, Christine D.] McMaster Univ, Dept Phys & Astron, Hamilton, ON L8S 4M1, Canada. RP Ueda, J (reprint author), Natl Inst Nat Sci, Natl Astron Observ Japan, Nobeyama Radio Observ, Minamisa Ku, 462-2 Minamimaki, Minamimaki, Nagano 3841305, Japan. OI Zhang, Qizhou/0000-0003-2384-6589 NR 53 TC 24 Z9 24 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JAN 20 PY 2012 VL 745 IS 1 AR 65 DI 10.1088/0004-637X/745/1/65 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 892WP UT WOS:000300316600065 ER PT J AU Wilkes, BJ Lal, DV Worrall, DM Birkinshaw, M Haas, M Willner, SP Antonucci, R Ashby, MLN Avara, M Barthel, P Chini, R Fazio, GG Hardcastle, M Lawrence, C Leipski, C Ogle, P Schulz, B AF Wilkes, Belinda J. Lal, Dharam V. Worrall, D. M. Birkinshaw, Mark Haas, Martin Willner, S. P. Antonucci, Robert Ashby, M. L. N. Avara, Mark Barthel, Peter Chini, Rolf Fazio, G. G. Hardcastle, Martin Lawrence, Charles Leipski, Christian Ogle, Patrick Schulz, Bernhard TI CHANDRA X-RAY OBSERVATIONS OF THE REDSHIFT 1.53 RADIO-LOUD QUASAR 3C 270.1 SO ASTROPHYSICAL JOURNAL LA English DT Article DE quasars: individual: 3C 270.1; X-rays: galaxies: clusters ID ACTIVE GALACTIC NUCLEI; DUAL-FREQUENCY OBSERVATIONS; MAGNETIC-FIELD STRENGTHS; ASYMMETRIC DEPOLARIZATION; GALAXIES; JETS; LUMINOSITY; EMISSION; SPECTRA; VIEW AB Chandra X-ray observations of the high redshift (z = 1.532) radio-loud quasar 3C 270.1 in 2008 February show the nucleus to have a power-law spectrum, Gamma = 1.66 +/- 0.08, typical of a radio-loud quasar, and a marginally detected Fe K alpha emission line. The data also reveal extended X-ray emission, about half of which is associated with the radio emission from this source. The southern emission is co-spatial with the radio lobe and peaks at the position of the double radio hot spot. Modeling this hot spot, including Spitzer upper limits, rules out synchrotron emission from a single power-law population of electrons, favoring inverse Compton emission with a field of similar to 11 nT, roughly a third of the equipartition value. The northern emission is concentrated close to the location of a 40 degrees bend where the radio jet is presumed to encounter an external medium. It can be explained by inverse Compton emission involving cosmic microwave background photons with a field of similar to 3 nT, a factor of 7-10 below the equipartition value. The remaining, more diffuse X-ray emission is harder (HR = -0.09 +/- 0.22). With only 22.8 +/- 5.6 counts, the spectral form cannot be constrained. Assuming thermal emission with a temperature of 4 keV yields an estimate for the luminosity of 1.8 x 10(44) erg s(-1), consistent with the luminosity-temperature relation of lower-redshift clusters. However, deeper Chandra X-ray observations are required to delineate the spatial distribution and better constrain the spectrum of the diffuse emission to verify that we have detected X-ray emission from a high-redshift cluster. C1 [Wilkes, Belinda J.; Lal, Dharam V.; Willner, S. P.; Ashby, M. L. N.; Fazio, G. G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Worrall, D. M.; Birkinshaw, Mark] Univ Bristol, HH Wills Phys Lab, Bristol BS8 1TL, Avon, England. [Haas, Martin; Chini, Rolf] Ruhr Univ Bochum, Inst Astron, Bochum, Germany. [Antonucci, Robert] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA. [Avara, Mark] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Barthel, Peter] Univ Groningen, Kapteyn Astron Inst, Groningen, Netherlands. [Chini, Rolf] Univ Catolica Norte, Inst Astron, Antofagasta, Chile. [Hardcastle, Martin] Univ Hertfordshire, Sch Phys & Astron, Hatfield AL10 9AB, Herts, England. [Lawrence, Charles] JPL, Pasadena, CA 91109 USA. [Leipski, Christian] MPIA, Heidelberg, Germany. [Ogle, Patrick] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. [Schulz, Bernhard] CALTECH, IPAC, Pasadena, CA 91125 USA. RP Wilkes, BJ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Hardcastle, Martin/E-2264-2012; OI Hardcastle, Martin/0000-0003-4223-1117; Wilkes, Belinda/0000-0003-1809-2364 FU National Aeronautics and Space Administration [G08-9106X]; Chandra X-ray Center [NAS8-03060] FX Support for this work was provided by the National Aeronautics and Space Administration through Chandra Award Number G08-9106X issued by the Chandra X-ray Center, which is operated by the Smithsonian Astrophysical Observatory for and on behalf of the National Aeronautics Space Administration under contract NAS8-03060 (Chandra X-ray Center). The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. Observations reported here were obtained at the MMT Observatory, a joint facility of the Smithsonian Institution and the University of Arizona. 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. NR 32 TC 5 Z9 5 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JAN 20 PY 2012 VL 745 IS 1 AR 84 DI 10.1088/0004-637X/745/1/84 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 892WP UT WOS:000300316600084 ER PT J AU Lin, YT Stanford, SA Eisenhardt, PRM Vikhlinin, A Maughan, BJ Kravtsov, A AF Lin, Yen-Ting Stanford, S. Adam Eisenhardt, Peter R. M. Vikhlinin, Alexey Maughan, Ben J. Kravtsov, Andrey TI BARYON CONTENT OF MASSIVE GALAXY CLUSTERS AT z=0-0.6 SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE galaxies: clusters: general; galaxies: clusters: intracluster medium; galaxies: elliptical and lenticular, cD; galaxies: luminosity function, mass function ID LUMINOSITY FUNCTION; STELLAR; GAS; PROJECT; LIGHT AB We study the relationship between two major baryonic components in galaxy clusters, namely the stars in galaxies and the ionized gas in the intracluster medium (ICM), using 94 clusters that span the redshift range 0-0.6. Accurately measured total and ICM masses from Chandra observations and stellar masses derived from the Wide-field Infrared Survey Explorer and the Two Micron All Sky Survey allow us to trace the evolution of cluster baryon content in a self-consistent fashion. We find that, within r(500), the evolution of the ICM-mass-total-mass relation is consistent with the expectation of the self-similar model, while there is no evidence for redshift evolution in the stellar-mass-total-mass relation. This suggests that the stellar mass and ICM mass in the inner parts of clusters evolve differently. C1 [Lin, Yen-Ting] Acad Sinica, Inst Astron & Astrophys, Taipei 115, Taiwan. [Lin, Yen-Ting] Univ Tokyo, Todai Inst Adv Study, Inst Phys & Math Universe, Kashiwa, Chiba, Japan. [Stanford, S. Adam] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA. [Stanford, S. Adam] Lawrence Livermore Natl Lab, Inst Geophys & Planetary Phys, Livermore, CA 94551 USA. [Eisenhardt, Peter R. M.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Vikhlinin, Alexey] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Maughan, Ben J.] Univ Bristol, HH Wills Phys Lab, Bristol BS8 1TL, Avon, England. [Kravtsov, Andrey] Univ Chicago, Kavli Inst Cosmol Phys, Dept Astron & Astrophys, Chicago, IL 60637 USA. [Kravtsov, Andrey] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA. RP Lin, YT (reprint author), Acad Sinica, Inst Astron & Astrophys, Taipei 115, Taiwan. EM ytl@asiaa.sinica.edu.tw FU World Premier International Research Center Initiative, MEXT, Japan; NSF [NSF PHY05-51164]; NASA; 2MASS; UMass; IPAC/Caltech; Sloan Foundation FX We are very grateful to G. Bruzual and S. Charlot for providing an updated version of their model, to M. Tanaka and C. Mancone for help with the BC model predictions, and to an anonymous referee for very helpful comments. Y.T.L. thanks E. Komatsu, J. Gunn, C. Conroy, M. Fukugita, M. Takada, and D. Spergel for helpful discussions, and I. H. for constant encouragement. Y.T.L. acknowledges supports from the World Premier International Research Center Initiative, MEXT, Japan. This research was supported in part by the NSF under grant no. NSF PHY05-51164. This publication makes use of data products from WISE, a joint project of UCLA and JPL/Caltech, funded by NASA, and 2MASS, a joint project of UMass and IPAC/Caltech, funded by NASA and NSF. Funding for SDSS-III has been provided by the Sloan Foundation, the Participating Institutions, NSF, and DOE. This work makes use of data from CFHTLS and UKIDSS. NR 30 TC 39 Z9 39 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD JAN 20 PY 2012 VL 745 IS 1 AR L3 DI 10.1088/2041-8205/745/1/L3 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 891PC UT WOS:000300228100003 ER PT J AU Steiner, JF McClintock, JE Reid, MJ AF Steiner, James F. McClintock, Jeffrey E. Reid, Mark J. TI THE DISTANCE, INCLINATION, AND SPIN OF THE BLACK HOLE MICROQUASAR H1743-322 SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE black hole physics; stars: individual (H1743-322); X-rays: binaries ID QUASI-PERIODIC OSCILLATIONS; X-RAY JETS; XTE J1550-564; TRANSIENT H1743-322; MASS-DISTRIBUTION; HIGH-FREQUENCY; LARGE-SCALE; OUTBURST; CALIBRATION; EVOLUTION AB During its 2003 outburst, the black hole X-ray transient H1743-322 produced two-sided radio and X-ray jets. Applying a simple and symmetric kinematic model to the trajectories of these jets, we determine the source distance, 8.5 +/- 0.8 kpc, and the inclination angle of the jets, 75 degrees +/- 3 degrees. Using these values, we estimate the spin of the black hole by fitting its Rossi X-ray Timing Explorer spectra, obtained during the 2003 outburst, to a standard relativistic accretion-disk model. For its spin, we find a(*) = 0.2 +/- 0.3 (68% limits), -0.3 < a(*) < 0.7 at 90% confidence. We strongly rule against an extreme value of spin: a(*) < 0.92 at 99.7% confidence. H1743-322 is the third known microquasar (after A0620-00 and XTE J1550-564) that displays large-scale ballistic jets and has a moderate value of spin. Our result, which depends on an empirical distribution of black hole masses, takes into account all known sources of measurement error. C1 [Steiner, James F.; McClintock, Jeffrey E.; Reid, Mark J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Steiner, JF (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM jsteiner@cfa.harvard.edu FU Smithsonian Institution; NASA [NNX11AD08G]; FAS Science Division Research Computing Group at Harvard University FX J.F.S. was supported by the Smithsonian Institution Endowment Funds and J.E.M. acknowledges support from NASA Grant NNX11AD08G. Computations were performed using the Odyssey cluster which is supported by the FAS Science Division Research Computing Group at Harvard University. NR 28 TC 39 Z9 39 U1 1 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD JAN 20 PY 2012 VL 745 IS 1 AR L7 DI 10.1088/2041-8205/745/1/L7 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 891PC UT WOS:000300228100007 ER PT J AU Takahashi, S Ho, PTP AF Takahashi, Satoko Ho, Paul T. P. TI THE DISCOVERY OF THE YOUNGEST MOLECULAR OUTFLOW ASSOCIATED WITH AN INTERMEDIATE-MASS PROTOSTELLAR CORE, MMS-6/OMC-3 SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE ISM: individual objects (OMC3-MMS 6); ISM: jets and outflows; ISM: molecules; stars: evolution ID SUBMILLIMETER ARRAY; STELLAR OBJECTS; STAR-FORMATION; HIGH-VELOCITY; ORION; REGION; OMC-3; MILLIMETER; CHEMISTRY; CLOUDS AB We present subarcsecond resolution HCN (4-3) and CO (3-2) observations made with the Submillimeter Array, toward an extremely young intermediate-mass protostellar core, MMS 6-main, located in the Orion Molecular Cloud 3 region (OMC-3). We have successfully imaged a compact molecular outflow lobe (approximate to 1000 AU) associated with MMS 6-main, which is also the smallest molecular outflow ever found in the intermediate-mass protostellar cores. The dynamical timescale of this outflow is estimated to be <= 100 yr. The line width dramatically increases downstream at the end of the molecular outflow (Delta v similar to 25 km s(-1)) and clearly shows the bow-shock-type velocity structure. The estimated outflow mass (approximate to 10(-4) M-circle dot) and outflow size are approximately two to four orders and one to three orders of magnitude smaller, respectively, while the outflow force (approximate to 10(-4) M-circle dot km s(-1) yr(-1)) is similar, compared to the other molecular outflows studied in OMC-2/3. These results show that MMS6-main is a protostellar core at the earliest evolutionary stage, most likely shortly after the second core formation. C1 [Takahashi, Satoko; Ho, Paul T. P.] Acad Sinica, Inst Astron & Astrophys, Taipei 106, Taiwan. [Ho, Paul T. P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Takahashi, S (reprint author), Acad Sinica, Inst Astron & Astrophys, POB 23-141, Taipei 106, Taiwan. EM satoko_t@asiaa.sinica.edu.tw FU Smithsonian Institution; Academia Sinica; [NSC97-2112-M-001-007-MY3] FX The Submillimeter Array is a joint project between the Smithsonian Astrophysical Observatory and the Academia Sinica Institute of Astronomy and Astrophysics and is funded by the Smithsonian Institution and the Academia Sinica.; We acknowledge the staff at the Submillimeter Array for assistance with observations. We thank Naomi Hirano, Masanori Nakamura, and Keiichi Asada for fruitful discussions, and our anonymous referee whose suggestions improved this manuscript. S. T. and P. T. P. H. acknowledge the financial support from NSC97-2112-M-001-007-MY3. NR 34 TC 12 Z9 12 U1 1 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD JAN 20 PY 2012 VL 745 IS 1 AR L10 DI 10.1088/2041-8205/745/1/L10 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 891PC UT WOS:000300228100010 ER PT J AU Gagnon, PR Harms, KE Platt, WJ Passmore, HA Myers, JA AF Gagnon, Paul R. Harms, Kyle E. Platt, William J. Passmore, Heather A. Myers, Jonathan A. TI Small-Scale Variation in Fuel Loads Differentially Affects Two Co-Dominant Bunchgrasses in a Species-Rich Pine Savanna SO PLOS ONE LA English DT Article ID PLANT-POPULATIONS; FIRE; COMMUNITY; DISTURBANCE; PALUSTRIS; INVASIBILITY; COEXISTENCE; ECOSYSTEMS; DIVERSITY; DOMINANCE AB Ecological disturbances frequently control the occurrence and patterning of dominant plants in high-diversity communities like C-4 grasslands and savannas. In such ecosystems disturbance-related processes can have important implications for species, and for whole communities when those species are dominant, yet mechanistic understanding of such processes remains fragmentary. Multiple bunchgrass species commonly co-dominate disturbance-dependent and species-rich pine savannas, where small-scale fuel heterogeneity may influence bunchgrass survival and growth following fires. We quantified how fire in locally varying fuel loads influenced dynamics of dominant C-4 bunchgrasses in a species-rich pine savanna in southeastern Louisiana, USA. We focused on two congeneric, co-dominant species (Schizachyrium scoparium and S. tenerum) with similar growth forms, functional traits and reproductive strategies to highlight effects of fuel heterogeneity during fires. In experimental plots with either reduced or increased fuels versus controls with unmanipulated fuels, we compared: 1) bunchgrass damage and 2) mortality from fires; 3) subsequent growth and 4) flowering. Compared to controls, fire with increased fuels caused greater damage, mortality and subsequent flowering, but did not affect post-fire growth. Fire with reduced fuels had no effect on any of the four measures. The two species responded differently to fire with increased fuels - S. scoparium incurred measurably more damage and mortality than S. tenerum. Logistic regression indicated that the larger average size of S. tenerum tussocks made them resistant to more severe burning where fuels were increased. We speculate that locally increased fuel loading may be important in pine savannas for creating colonization sites because where fuels are light or moderate, dominant bunchgrasses persist through fires. Small-scale heterogeneity in fires, and differences in how species tolerate fire may together promote shared local dominance by different bunchgrasses. C1 [Gagnon, Paul R.; Harms, Kyle E.; Platt, William J.; Passmore, Heather A.; Myers, Jonathan A.] Louisiana State Univ, Dept Biol Sci, Baton Rouge, LA 70803 USA. [Harms, Kyle E.] Smithsonian Trop Res Inst, Balboa, Panama. RP Gagnon, PR (reprint author), Murray State Univ, Dept Biol Sci, Murray, KY 42071 USA. EM pgagnon@murraystate.edu FU National Science Foundation [DEB 0516175] FX The National Science Foundation (DEB 0516175) provided financial support. The funder had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 48 TC 7 Z9 7 U1 2 U2 23 PU PUBLIC LIBRARY SCIENCE PI SAN FRANCISCO PA 185 BERRY ST, STE 1300, SAN FRANCISCO, CA 94107 USA SN 1932-6203 J9 PLOS ONE JI PLoS One PD JAN 17 PY 2012 VL 7 IS 1 AR e29674 DI 10.1371/journal.pone.0029674 PG 7 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 907XU UT WOS:000301454400020 PM 22272241 ER PT J AU Brauer, M Amann, M Burnett, RT Cohen, A Dentener, F Ezzati, M Henderson, SB Krzyzanowski, M Martin, RV Van Dingenen, R van Donkelaar, A Thurston, GD AF Brauer, Michael Amann, Markus Burnett, Rick T. Cohen, Aaron Dentener, Frank Ezzati, Majid Henderson, Sarah B. Krzyzanowski, Michal Martin, Randall V. Van Dingenen, Rita van Donkelaar, Aaron Thurston, George D. TI Exposure Assessment for Estimation of the Global Burden of Disease Attributable to Outdoor Air Pollution SO ENVIRONMENTAL SCIENCE & TECHNOLOGY LA English DT Article ID PARTICULATE MATTER; OZONE; MORTALITY; LONG; SIMULATIONS; EMISSIONS; AEROCOM; QUALITY; MODELS; ASSOCIATION AB Ambient air pollution is associated with numerous adverse health impacts. Previous assessments of global attributable disease burden have been limited to urban areas or by coarse spatial resolution of concentration estimates. Recent developments in remote sensing, global chemical-transport models, and improvements in coverage of surface measurements facilitate virtually complete spatially resolved global air pollutant concentration estimates. We combined these data to generate global estimates of long-term average ambient concentrations of fine particles (PM2.5) and ozone at 0.10 degrees X 0.1 degrees spatial resolution for 1990 and 2005. In 2005, 89% of the world's population lived in areas where the World Health Organization Air Quality Guideline of 10 mu g/m(3) PM2.5 (annual average) was exceeded. Globally, 32% of the population lived in areas exceeding the WHO Level 1 Interim Target of 35 mu g/m(3), driven by high proportions in East (76%) and South (26%) Asia. The highest seasonal ozone levels were found in North and Latin America, Europe, South and East Asia, and parts of Africa. Between 1990 and 2005 a 6% increase in global population-weighted PM2.5 and a 1% decrease in global population-weighted ozone concentrations was apparent, highlighted by increased concentrations in East, South, and Southeast Asia and decreases in North America and Europe. Combined with spatially resolved population distributions, these estimates expand the evaluation, of the global health burden associated with outdoor air pollution. C1 [Brauer, Michael] Univ British Columbia, Sch Populat & Publ Hlth, Vancouver, BC V6T 1Z3, Canada. [Amann, Markus] Int Inst Appl Syst Anal, A-2361 Laxenburg, Austria. [Burnett, Rick T.] Hlth Canada, Biostat & Epidemiol Div, Ottawa, ON K1A 0L2, Canada. [Cohen, Aaron] Hlth Effects Inst, Boston, MA 02110 USA. [Dentener, Frank; Van Dingenen, Rita] Commiss European Communities, Joint Res Ctr, Inst Environm & Sustainabil, I-21027 Ispra, Italy. [Ezzati, Majid] Univ London Imperial Coll Sci Technol & Med, Sch Publ Hlth, London W2 1PG, England. [Henderson, Sarah B.] British Columbia Ctr Dis Control, Vancouver, BC V5Z4R4, Canada. [Krzyzanowski, Michal] World Hlth Org, European Ctr Environm & Hlth, D-53113 Bonn, Germany. [Martin, Randall V.; van Donkelaar, Aaron] Dalhousie Univ, Dept Phys & Atmospher Sci, Halifax, NS B3H 3J5, Canada. [Martin, Randall V.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Thurston, George D.] NYU, Inst Environm Med, Tuxedo Pk, NY 10987 USA. RP Brauer, M (reprint author), Univ British Columbia, Sch Populat & Publ Hlth, 3rd Floor,2206 East Mall, Vancouver, BC V6T 1Z3, Canada. EM michael.brauer@ubc.ca RI Martin, Randall/C-1205-2014; OI Martin, Randall/0000-0003-2632-8402; Brauer, Michael/0000-0002-9103-9343 FU NIEHS NIH HHS [P30 ES000260] NR 50 TC 152 Z9 155 U1 25 U2 181 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0013-936X EI 1520-5851 J9 ENVIRON SCI TECHNOL JI Environ. Sci. Technol. PD JAN 17 PY 2012 VL 46 IS 2 BP 652 EP 660 DI 10.1021/es2025752 PG 9 WC Engineering, Environmental; Environmental Sciences SC Engineering; Environmental Sciences & Ecology GA 876VQ UT WOS:000299136200014 PM 22148428 ER PT J AU Penna, RF AF Penna, Robert F. TI Apparent motion of a spherical shell collapsing onto a black hole SO PHYSICS LETTERS B LA English DT Article DE Black holes; Classical theories of gravity; Spacetime singularities ID STAR AB We model the collapse of a spherically symmetric, constant density, pressureless shell onto a preexisting black hole. Contrary to a recent claim of Liu and Zhang (2009), we show that an observer at infinity never sees any part of the shell cross the event horizon. The entire shell appears to "freeze" outside the black hole. We find that during intermediate stages of the collapse, the change in apparent size of the inner surface is non-monotonic. However, at late times, the apparent sizes of the inner and outer surfaces of the shell both approach 3 root 3GM/c(2) asymptotically, where M is the combined mass of the initial black hole and the shell. (C) 2011 Elsevier B.V. All rights reserved. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Penna, RF (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM rpenna@cfa.harvard.edu NR 17 TC 1 Z9 1 U1 1 U2 2 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0370-2693 J9 PHYS LETT B JI Phys. Lett. B PD JAN 16 PY 2012 VL 707 IS 1 BP 233 EP 236 DI 10.1016/j.physletb.2011.12.038 PG 4 WC Astronomy & Astrophysics; Physics, Nuclear; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA 885CV UT WOS:000299757000038 ER PT J AU Ryu, Y Baldocchi, DD Black, TA Detto, M Law, BE Leuning, R Miyata, A Reichstein, M Vargas, R Ammann, C Beringer, J Flanagan, LB Gu, LH Hutley, LB Kim, J McCaughey, H Moors, EJ Rambal, S Vesala, T AF Ryu, Youngryel Baldocchi, Dennis D. Black, T. Andrew Detto, Matteo Law, Beverly E. Leuning, Ray Miyata, Akira Reichstein, Markus Vargas, Rodrigo Ammann, Christof Beringer, Jason Flanagan, Lawrence B. Gu, Lianhong Hutley, Lindsay B. Kim, Joon McCaughey, Harry Moors, Eddy J. Rambal, Serge Vesala, Timo TI On the temporal upscaling of evapotranspiration from instantaneous remote sensing measurements to 8-day mean daily-sums SO AGRICULTURAL AND FOREST METEOROLOGY LA English DT Article DE Evapotranspiration; Eddy covariance; Temporal upscaling; FLUXNET; MODIS ID CARBON-DIOXIDE EXCHANGE; NET ECOSYSTEM PRODUCTIVITY; CO2 EXCHANGE; ENERGY FLUXES; WATER-VAPOR; HETEROGENEOUS LANDSCAPE; TEMPERATE GRASSLAND; DAILY EVAPORATION; SURFACE FLUXES; BOUNDARY-LAYER AB The regular monitoring of evapotranspiration from satellites has been limited because of discontinuous temporal coverage, resulting in snapshots at a particular point in space and time. We developed a temporal upscaling scheme using satellite-derived instantaneous estimates of evapotranspiration to produce a daily-sum evapotranspiration averaged over an 8-day interval. We tested this scheme against measured evapotranspiration data from 34 eddy covariance flux towers covering seven plant functional types from boreal to tropical climatic zones. We found that the ratio of a half-hourly-sum of potential solar radiation (extraterrestrial solar irradiance on a plane parallel to the Earth's surface) between 10:00 hh and 14:00 hh to a daily-sum of potential solar radiation provides a robust scaling factor to convert a half-hourly measured evapotranspiration to an estimate of a daily-sum; the estimated and measured daily sum evapotranspiration showed strong linear relation (r(2) = 0.92) and small bias (-2.7%). By comparison, assuming a constant evaporative fraction (the ratio of evapotranspiration to available energy) during the daytime, although commonly used for temporal upscaling, caused 13% underestimation of evapotranspiration on an annual scale. The proposed temporal upscaling scheme requires only latitude, longitude and time as input. Thus it will be useful for developing continuous evapotranspiration estimates in space and time, which will improve continuous monitoring of hydrological cycle from local to global scales. (C) 2011 Elsevier B.V. All rights reserved. C1 [Ryu, Youngryel; Baldocchi, Dennis D.] Univ Calif Berkeley, Dep Environm Sci Policy & Management, Berkeley, CA 94720 USA. [Black, T. Andrew] Univ British Columbia, Fac Land & Food Syst, Vancouver, BC V5Z 1M9, Canada. [Detto, Matteo] Smithsonian Trop Res Inst, Balboa, Panama. [Law, Beverly E.] Oregon State Univ, Dep Forest Ecosyst & Soc, Corvallis, OR 97331 USA. [Leuning, Ray] CSIRO Marine & Atmospher Res, Canberra, ACT, Australia. [Miyata, Akira] Natl Inst Agroenvironm Sci, Tsukuba, Ibaraki 305, Japan. [Reichstein, Markus] Max Planck Inst Biogeochem, Jena, Germany. [Vargas, Rodrigo] CICESE, Dept Biol Conservac, Ensenada, Baja California, Mexico. [Ammann, Christof] Agroscope ART, Fed Res Stn, Zurich, Switzerland. [Beringer, Jason] Monash Univ, Sch Geog & Environm Sci, Clayton, Vic 3800, Australia. [Flanagan, Lawrence B.] Univ Lethbridge, Dep Biol Sci, Lethbridge, AB T1K 3M4, Canada. [Gu, Lianhong] Oak Ridge Natl Lab, Div Environm Sci, Oak Ridge, TN USA. [Hutley, Lindsay B.] Charles Darwin Univ, Res Inst Environm & Livelihoods, Darwin, NT 0909, Australia. [McCaughey, Harry] Queens Univ, Dep Geog, Kingston, ON, Canada. [Moors, Eddy J.] Alterra Wageningen UR, ESS CC, Wageningen, Netherlands. [Rambal, Serge] CEFE CNRS, DREAM, Montpellier, France. [Vesala, Timo] Univ Helsinki, Dept Phys, Helsinki, Finland. [Ryu, Youngryel] Harvard Univ, Dep Organism & Evolutionary Biol, Cambridge, MA 02138 USA. [Ryu, Youngryel; Kim, Joon] Seoul Natl Univ, Dept Landscape Architecture & Rural Syst Engn, Seoul 151921, South Korea. RP Ryu, Y (reprint author), Seoul Natl Univ, Dept Landscape Architecture & Rural Syst Engn, Seoul 151921, South Korea. EM yryu@snu.ac.kr RI Ryu, Youngryel/C-3072-2008; Leuning, Ray/A-2793-2008; Hutley, Lindsay/A-7925-2011; Moors, Eddy/J-5165-2012; Flanagan, Lawrence/B-1307-2013; Reichstein, Markus/A-7494-2011; Baldocchi, Dennis/A-1625-2009; Vargas, Rodrigo/C-4720-2008; Gu, Lianhong/H-8241-2014; Vesala, Timo/C-3795-2017; Beringer, Jason/B-8528-2008; Law, Beverly/G-3882-2010 OI rambal, serge/0000-0001-5869-8382; Ryu, Youngryel/0000-0001-6238-2479; Hutley, Lindsay/0000-0001-5533-9886; Moors, Eddy/0000-0003-2309-2887; Flanagan, Lawrence/0000-0003-1748-0306; Reichstein, Markus/0000-0001-5736-1112; Baldocchi, Dennis/0000-0003-3496-4919; Vargas, Rodrigo/0000-0001-6829-5333; Gu, Lianhong/0000-0001-5756-8738; Vesala, Timo/0000-0002-4852-7464; Beringer, Jason/0000-0002-4619-8361; Law, Beverly/0000-0002-1605-1203 FU CFCAS; NSERC; BIOCAP; Environment Canada; NRCan; Sustainable Water Resources Center, Korea [1-8-3]; CarboEuropeIP; FAO-GTOS-TCO; iLEAPS; Max Planck Institute for Biogeochemistry; National Science Foundation; University of Tuscia; Universite Laval; US Department of Energy; Office of Science (BER), US Department of Energy [DE-FG02-06ER64318]; BIOCAP Canada; Natural Sciences and Engineering Research Council of Canada; Canadian Foundation for Climate and Atmospheric Sciences FX This work used eddy covariance data acquired by the FLUXNET community and in particular by the following networks: AmeriFlux (U.S. Department of Energy, Biological and Environmental Research, Terrestrial Carbon Program (DE-FG02-04ER63917 and DE-FG02-04ER63911)), AfriFlux, AsiaFlux, CarboAfrica, CarboEuropeIP, Carboltaly, CarboMont, ChinaFlux, Fluxnet-Canada (supported by CFCAS, NSERC, BIOCAP, Environment Canada, and NRCan), GreenGrass, KoFlux (supported by Sustainable Water Resources Center of 21C Frontier Research Program Code: 1-8-3 Korea), LBA, NECC, OzFlux, TCOS-Siberia, USCCC. We acknowledge the financial support to the eddy covariance data harmonization provided by CarboEuropeIP, FAO-GTOS-TCO, iLEAPS, Max Planck Institute for Biogeochemistry, National Science Foundation, University of Tuscia, Universite Laval and Environment Canada and US Department of Energy and the database development and technical support from Berkeley Water Center, Lawrence Berkeley National Laboratory, Microsoft Research eScience, Oak Ridge National Laboratory, University of California - Berkeley, University of Virginia. YR was supported by NASA Headquarters under the NASA Earth and Space Science Fellowship Program (NNX08AU25H) and the Berkeley Water Center/Microsoft eScience project. MODIS data processing was supported by Microsoft Azure cloud computing service. Drs. Andrew Richardson, John Norman, Oliver Sonnentag and Paul Stoy gave insightful comments. Data from the Tonzi and Vaira Ranches are supported by the Office of Science (BER), US Department of Energy, Grant DE-FG02-06ER64308. Data from Metolius sites are supported by the Office of Science (BER), US Department of Energy, Grant DE-FG02-06ER64318. Data collection at the Lethbridge grassland and western peatland sites in Canada were supported by the Natural Sciences and Engineering Research Council of Canada, the Canadian Foundation for Climate and Atmospheric Sciences, and BIOCAP Canada. NR 81 TC 32 Z9 34 U1 4 U2 55 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0168-1923 J9 AGR FOREST METEOROL JI Agric. For. Meteorol. PD JAN 15 PY 2012 VL 152 BP 212 EP 222 DI 10.1016/j.agrformet.2011.09.010 PG 11 WC Agronomy; Forestry; Meteorology & Atmospheric Sciences SC Agriculture; Forestry; Meteorology & Atmospheric Sciences GA 885ST UT WOS:000299801800019 ER PT J AU Huang, SC Farkas, J Yu, G Petaev, MI Jacobsen, SB AF Huang, Shichun Farkas, Juraj Yu, Gang Petaev, Michail I. Jacobsen, Stein B. TI Calcium isotopic ratios and rare earth element abundances in refractory inclusions from the Allende CV3 chondrite SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Article ID ALUMINUM-RICH INCLUSIONS; EARLY SOLAR-SYSTEM; METEORITES; FRACTIONATION; ANOMALIES; NEBULA; CONSTRAINTS; DELTA-CA-44/40; CONDENSATION; EVOLUTION AB Refractory inclusions in primitive meteorites are the oldest objects formed in the Solar System. They exhibit large mass-dependent isotopic effects in many elements, including Si, Mg and Ca, indicative of their complex origin. We report data for both mass-dependent (delta) and mass-independent (epsilon) Ca isotopic effects, and rare earth element (REE) abundances in six refractory inclusions from the Allende CV3 meteorite. Our data reveal large mass-dependent Ca isotopic effects in these refractory inclusions, with delta Ca-44/40 ranging from -5.60 to +0.35 (relative to NIST SRM 915a), which are significantly lower than that of the bulk silicate Earth (delta Ca-44/40 = 1.05 +/- 0.04). Importantly, delta Ca-44/40 is correlated with REE patterns: refractory inclusions with Group II REE patterns have lighter Ca isotope compositions compared to those with Group I REE patterns. Specifically, the studied refractory inclusions form negative Ca-44/Ca-40-Tm/Er and Ca-44/Ca-40-Nd/Er trends, implying segregation of up to 3% of an ultrarefractory evaporation residue from a chondritic reservoir prior to the formation of refractory inclusions. This residue would have to be characterized by high Ca-44/Ca-40 and low Tm/Er and Nd/Er. At 2 sigma levels of +/- 0.5 and +/- 1.5 for epsilon Ca-40/44 and epsilon Ca-43/44, respectively, the six refractory inclusions studied show no detectable Ca-40 or Ca-43 anomalies relative to the terrestrial standards. However, five out of the six refractory inclusions do show a Ca-48 excess of several epsilon-units, clearly resolvable from the terrestrial standards. (C) 2011 Elsevier Ltd. All rights reserved. C1 [Huang, Shichun; Farkas, Juraj; Yu, Gang; Petaev, Michail I.; Jacobsen, Stein B.] Harvard Univ, Dept Earth & Planetary Sci, Cambridge, MA 02138 USA. [Farkas, Juraj] Czech Geol Survey, Dept Geochem, Prague 15200 5, Czech Republic. [Petaev, Michail I.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Huang, SC (reprint author), Harvard Univ, Dept Earth & Planetary Sci, 20 Oxford St, Cambridge, MA 02138 USA. EM huang17@fas.harvard.edu; jacobsen@neodymium.harvard.edu RI Huang, Shichun/A-3596-2008; Yu, Gang/F-8701-2010; Jacobsen, Stein/B-1759-2013 FU NASA [NNX07AI80G, NNX11AK82G]; Harvard University Origins of Life Initiative; Canadian Institute for Advanced Research (CIFAR); Faculty of Environmental Sciences [42900/1312/3166] FX This work was supported by NASA Origins of Solar Systems Program awards NNX07AI80G and NNX11AK82G, and partial support form the Harvard University Origins of Life Initiative, the Canadian Institute for Advanced Research (CIFAR), and the Faculty of Environmental Sciences (Grant No. 42900/1312/3166) are greatly acknowledged. This work benefitted greatly from discussions with G.J. Wasserburg and D.A. Papanastassiou. We thank G.J. Wasserburg, J.I. Simon and A.M. Davis for their careful and constructive reviews and D.A. Papanastassiou for his editorial handling. NR 73 TC 25 Z9 28 U1 2 U2 26 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0016-7037 J9 GEOCHIM COSMOCHIM AC JI Geochim. Cosmochim. Acta PD JAN 15 PY 2012 VL 77 BP 252 EP 265 DI 10.1016/j.gca.2011.11.002 PG 14 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 875DK UT WOS:000299010400017 ER PT J AU Hodell, DA Turchyn, AV Wiseman, CJ Escobar, J Curtis, JH Brenner, M Gilli, A Mueller, AD Anselmetti, F Ariztegui, D Brown, ET AF Hodell, David A. Turchyn, Alexandra V. Wiseman, Camilla J. Escobar, Jaime Curtis, Jason H. Brenner, Mark Gilli, Adrian Mueller, Andreas D. Anselmetti, Flavio Ariztegui, Daniel Brown, Erik T. TI Late Glacial temperature and precipitation changes in the lowland Neotropics by tandem measurement of delta O-18 in biogenic carbonate and gypsum hydration water SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Article ID OXYGEN ISOTOPIC COMPOSITION; HEMISPHERE WARM POOL; YUCATAN PENINSULA; CENTRAL-AMERICA; CLIMATE-CHANGE; MAYA LOWLANDS; PETEN ITZA; DEEP-OCEAN; CRYSTALLIZATION; MAXIMUM AB We applied a new method to reconstruct paleotemperature in the tropics during the last deglaciation by measuring oxygen isotopes of co-occurring gypsum hydration water and biogenic carbonate in sediment cores from two lakes on the Yucatan Peninsula. Oxygen and hydrogen isotope values of interstitial and gypsum hydration water indicate that the crystallization water preserves the isotopic signal of the lake water, and has not undergone post-depositional isotopic exchange with sediment pore water. The estimated lake water delta O-18 is combined with carbonate delta O-18 to calculate paleotemperature. Three paired measurements of 1200-yr-old gypsum and gastropod aragonite from Lake Chichancanab, Mexico, yielded a mean temperature of 26 degrees C (range 23-29.5 degrees C), which is consistent with the mean and range of mean annual temperatures (MAT) in the region today. Paired measurements of ostracods, gastropods, and gypsum hydration water samples were measured in cores from Lake Peten Itza, Guatemala, spanning the Late Glacial and early Holocene period (18.5-10.4 ka). The lowest recorded temperatures occurred at the start of Heinrich Stadial (HS) 1 at 18.5 ka. Inferred temperatures from benthic ostracods ranged from 16 to 20 degrees C during HS 1, which is 6-10 degrees C cooler than MAT in the region today, whereas temperatures derived from shallow-water gastropods were generally warmer (20-25 degrees C), reflecting epilimnetic temperatures. The derived temperatures support previous findings of greater tropical cooling on land in Central America during the Late Glacial than indicated by nearby marine records. Temperature increased in two steps during the last deglaciation. The first occurred during the Bolling-Allerod (B-A; from 14.7 to 13 ka) when temperature rose to 20-24 degrees C towards the end of this period. The second step occurred at 10.4 ka near the beginning of the Holocene when ostracod-inferred temperature rose to 26 degrees C, reflecting modern hypolimnetic temperature set during winter, whereas gastropod-derived temperature attained 30 degrees C, reflecting modern summer epilimnetic temperature. (C) 2011 Elsevier Ltd. All rights reserved. C1 [Hodell, David A.; Turchyn, Alexandra V.; Wiseman, Camilla J.] Univ Cambridge, Dept Earth Sci, Godwin Lab Palaeoclimate Res, Cambridge CB2 3EQ, England. [Escobar, Jaime; Curtis, Jason H.; Brenner, Mark] Univ Florida, Dept Geol Sci, Land Use & Environm Change Inst, Gainesville, FL USA. [Escobar, Jaime] Smithsonian Trop Res Inst, CTPA, Panama City, Panama. [Gilli, Adrian; Mueller, Andreas D.] ETH, Inst Geol, CH-8092 Zurich, Switzerland. [Anselmetti, Flavio] Swiss Fed Inst Aquat Sci & Technol, Eawag, CH-8600 Dubendorf, Switzerland. RP Hodell, DA (reprint author), Univ Cambridge, Dept Earth Sci, Godwin Lab Palaeoclimate Res, Cambridge CB2 3EQ, England. EM dah73@cam.ac.uk RI Mueller, Andreas/D-6272-2013; OI Mueller, Andreas/0000-0003-3513-5776 FU Canadian Institute for Advanced Research; National Environmental Research Council [NE/I016716/1]; US National Science Foundation [ATM-0502030]; NSF; International Continental Scientific Drilling Program; Swiss Federal Institute of Technology; Swiss National Science Foundation; U.S. Department of Energy by Lawrence Livermore National Laboratory [DE-AC52-07NA27344] FX We thank Associate Editor B. Luz, Y. Kolodny and two anonymous reviewers for their insightful comments that improved the quality of the manuscript. We thank the many agencies and individuals in Guatemala who assisted this project. They include: Universidad del Valle, Universidad San Carlos, Ministerio de Ambiente y Recursos Naturales, Consejo Nacional de Areas Protegidas, Instituto de Antropologia e Historia, Autoridad Para el Manejo y Desarrollo Sostenible de la Cuenca del Lago Peten-Itza, Wildlife Conservation Society, Alex Arrivillaga, Cathy Lopez, Margaret Dix, Michael Dix, Margarita Palmieri, David, Rosita, & Kelsey Kuhn, and the staff at La Casa de Don David, Lico Godoy, Tony Ortiz, Franz Sperisen, Luis Toruno, Julian Tesucun, Melisa Orozco, Silja Ramirez, Gabriela Alfaro, and Jacobo Blijdenstein. We also thank the personnel of DOSECC (Drilling, Observation and Sampling of the Earth's Continental Crust) who were instrumental in obtaining the cores. We are indebted to Anders Noren, Kristina Brady and Amy Myrbo of LacCore (National Lacustrine Core Facility), Department of Earth Sciences, University of Minnesota-Twin Cities for their expertise in core acquisition, curation and sampling. We thank Gianna Browne and Briony Bowe for sample preparation and Mike Hall and James Rolfe for technical assistance with stable isotope measurements and John Higgins and Gilad Antler for help with the pore fluid modeling. AVT was supported by the Canadian Institute for Advanced Research. This project was funded by grants from the National Environmental Research Council (Award NE/I016716/1) and US National Science Foundation (ATM-0502030). Cores were collected with support from NSF, the International Continental Scientific Drilling Program, the Swiss Federal Institute of Technology, and the Swiss National Science Foundation. Radiocarbon analyses were performed under the auspices of the U.S. Department of Energy by Lawrence Livermore National Laboratory under contract DE-AC52-07NA27344. NR 62 TC 23 Z9 24 U1 3 U2 33 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0016-7037 EI 1872-9533 J9 GEOCHIM COSMOCHIM AC JI Geochim. Cosmochim. Acta PD JAN 15 PY 2012 VL 77 BP 352 EP 368 DI 10.1016/j.gca.2011.11.026 PG 17 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 875DK UT WOS:000299010400024 ER PT J AU Penniston-Dorland, SC Bebout, GE Pogge von Strandmann, PAE Elliott, T Sorensen, SS AF Penniston-Dorland, Sarah C. Bebout, Gray E. Pogge von Strandmann, Philip A. E. Elliott, Tim Sorensen, Sorena S. TI Lithium and its isotopes as tracers of subduction zone fluids and metasomatic processes: Evidence from the Catalina Schist, California, USA SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Article ID SLAB-MANTLE INTERFACE; CONVERGENT PLATE MARGINS; MELANGE FORMATION; SOUTHERN-CALIFORNIA; SEDIMENT SUBDUCTION; PRISM ACCRETION; METASEDIMENTARY ROCKS; HYDROTHERMAL SYSTEM; OROGENIC ECLOGITES; METAMORPHIC ROCKS AB The Catalina Schist, well-studied for its tectonometamorphic history and geochemical evolution, provides a field area in which to evaluate the extent of Li mobility in subduction-zone fluids and the degree to which Li isotopes can trace metamorphic fluid-rock interactions. A suite of 63 samples of the Catalina Schist that represent a range of metamorphic grades and diverse lithologies was analyzed for Li concentration and isotope composition. Metasedimentary rocks show no evidence for significant loss of Li, with increasing metamorphic grade, despite the wide range of prograde P-T histories represented by the five tectonometamorphic units (with the highest-grade rocks having experienced peak temperatures near 750 degrees C). Metamafic rocks similarly show no change in Li concentration, as a function of grade, that can be directly related to varying degrees of devolatilization. The Li concentrations and delta Li-7 of metasedimentary rocks appear to best correlate with a chemical alteration index that likely reflects differential extents of weathering in the sediment sources. The delta Li-7 of most metamafic rocks (including gabbroic metaconglomerate cobbles), veins and melange matrix reflects overprinting of the Li isotope compositions derived (through transfer of Li in fluids) from sedimentary lithologies in the same tectonometamorphic units. Thus it appears that Li was mobilized in fluids released from metasedimentary rocks but that the loss was insufficient to affect the bulk delta Li-7 and Li content of the metasedimentary rocks. Veins and melange matrix have the highest Li concentrations of all samples analyzed, ranging up to 70 ppm. Some veins and amphibolite-grade mafic rocks have low delta Li-7 suggestive of Li diffusion through an intergranular fluid. Taken together, these observations suggest mobilization of Li during high pressure/temperature (P/T) fluid-rock interactions that also resulted in enrichments in B, N, and some large ion lithophile elements (K, Rb, Cs, Ba) in the veins, melange matrix, and cobbles. This study demonstrates that, although Li is mobile in high P/T metamorphic fluids, it does not partition into fluids to the extent demonstrated for N, B, and Cs, the latter elements showing large depletions in the higher-grade Catalina Schist metasedimentary rocks. Thus, even in relatively warm subduction zones, deeply subducted metasedimentary rocks are expected to largely retain their Li inventory to depths of at least 40 km, the maximum depth at which units of the Catalina Schist experienced peak metamorphism. (C) 2011 Elsevier Ltd. All rights reserved. C1 [Penniston-Dorland, Sarah C.] Univ Maryland, Dept Geol, College Pk, MD 20742 USA. [Bebout, Gray E.] Lehigh Univ, Dept Earth & Environm Sci, Bethlehem, PA 18015 USA. [Pogge von Strandmann, Philip A. E.; Elliott, Tim] Univ Bristol, Sch Earth Sci, Bristol Isotope Grp, Bristol BS8 1RJ, Avon, England. [Sorensen, Sorena S.] Smithsonian Inst, Dept Mineral Sci, Washington, DC 20560 USA. RP Penniston-Dorland, SC (reprint author), Univ Maryland, Dept Geol, College Pk, MD 20742 USA. EM sarahpd@umd.edu RI Pogge von Strandmann, Philip/A-8638-2008; OI Pogge von Strandmann, Philip/0000-0001-7181-4165; Bebout, Gray/0000-0002-9768-9080 FU NSF [EAR-0911100]; NERC [NER/C510983/1]; Santa Catalina Island Conservancy FX We thank Richard Ash, Roberta Rudnick and William McDonough for assistance with Li isotope analysis. Roberta is additionally thanked for comments on the manuscript. We thank the NSF for support to SP-D, grant EAR-0911100. We thank undergraduate assistants Aleeza Harburger and Maureen Kelly for assisting with the analytical work at UMD and Greg Polley for assisting with sample collection. Measurements at Bristol were supported by NERC grant NER/C510983/1. The Santa Catalina Island Conservancy is acknowledged for support of sample collection logistics. Vincent Busigny, Ralf Halama, and Thomas Magna are thanked for constructive reviews, and Jeffrey Alt is thanked for his editorial handling of the manuscript. NR 98 TC 26 Z9 28 U1 3 U2 45 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0016-7037 J9 GEOCHIM COSMOCHIM AC JI Geochim. Cosmochim. Acta PD JAN 15 PY 2012 VL 77 BP 530 EP 545 DI 10.1016/j.gca.2011.10.038 PG 16 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 875DK UT WOS:000299010400036 ER PT J AU Timme, RE Bachvaroff, TR Delwiche, CF AF Timme, Ruth E. Bachvaroff, Tsvetan R. Delwiche, Charles F. TI Broad Phylogenomic Sampling and the Sister Lineage of Land Plants SO PLOS ONE LA English DT Article ID GREEN-ALGAE; CHARA-VULGARIS; EST ANALYSIS; SEQUENCE; CHLOROPLAST; ORIGIN; MITOCHONDRIAL; INTEGRATION; EVOLUTION; RELATIVES AB The tremendous diversity of land plants all descended from a single charophyte green alga that colonized the land somewhere between 430 and 470 million years ago. Six orders of charophyte green algae, in addition to embryophytes, comprise the Streptophyta s.l. Previous studies have focused on reconstructing the phylogeny of organisms tied to this key colonization event, but wildly conflicting results have sparked a contentious debate over which lineage gave rise to land plants. The dominant view has been that 'stoneworts,' or Charales, are the sister lineage, but an alternative hypothesis supports the Zygnematales (often referred to as "pond scum") as the sister lineage. In this paper, we provide a well-supported, 160-nuclear-gene phylogenomic analysis supporting the Zygnematales as the closest living relative to land plants. Our study makes two key contributions to the field: 1) the use of an unbiased method to collect a large set of orthologs from deeply diverging species and 2) the use of these data in determining the sister lineage to land plants. We anticipate this updated phylogeny not only will hugely impact lesson plans in introductory biology courses, but also will provide a solid phylogenetic tree for future green-lineage research, whether it be related to plants or green algae. C1 [Timme, Ruth E.; Delwiche, Charles F.] Univ Maryland, Maryland Agr Expt Stn, College Pk, MD 20742 USA. [Bachvaroff, Tsvetan R.] Smithsonian Inst, Smithsonian Environm Res Ctr, Edgewater, MD USA. RP Timme, RE (reprint author), Univ Maryland, Maryland Agr Expt Stn, College Pk, MD 20742 USA. EM retimme@gmail.com OI Delwiche, Charles/0000-0001-7854-8584 FU National Science Foundation (Division of Molecular and Cell Biosciences) [MCB-0523719] FX The study was supported in full by the National Science Foundation (Division of Molecular and Cell Biosciences, Microbial genome Sequencing Program), MCB-0523719. The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 42 TC 107 Z9 112 U1 3 U2 56 PU PUBLIC LIBRARY SCIENCE PI SAN FRANCISCO PA 1160 BATTERY STREET, STE 100, SAN FRANCISCO, CA 94111 USA SN 1932-6203 J9 PLOS ONE JI PLoS One PD JAN 13 PY 2012 VL 7 IS 1 AR e29696 DI 10.1371/journal.pone.0029696 PG 8 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 906QI UT WOS:000301361500019 PM 22253761 ER PT J AU Ackermann, M Ajello, M Ballet, J Barbiellini, G Bastieri, D Belfiore, A Bellazzini, R Berenji, B Blandford, RD Bloom, ED Bonamente, E Borgland, AW Bregeon, J Brigida, M Bruel, P Buehler, R Buson, S Caliandro, GA Cameron, RA Caraveo, PA Cavazzuti, E Cecchi, C Celik, O Charles, E Chaty, S Chekhtman, A Cheung, CC Chiang, J Ciprini, S Claus, R Cohen-Tanugi, J Corbel, S Corbet, RHD Cutini, S de Luca, A den Hartog, PR de Palma, F Dermer, CD Digel, SW Silva, EDE Donato, D Drell, PS Drlica-Wagner, A Dubois, R Dubus, G Favuzzi, C Fegan, SJ Ferrara, EC Focke, WB Fortin, P Fukazawa, Y Funk, S Fusco, P Gargano, F Gasparrini, D Gehrels, N Germani, S Giglietto, N Giordano, F Giroletti, M Glanzman, T Godfrey, G Grenier, IA Grove, JE Guiriec, S Hadasch, D Hanabata, Y Harding, AK Hayashida, M Hays, E Hill, AB Hughes, RE Johannesson, G Johnson, AS Johnson, TJ Kamae, T Katagiri, H Kataoka, J Kerr, M Knodlseder, J Kuss, M Lande, J Longo, F Loparco, F Lovellette, MN Lubrano, P Mazziotta, MN McEnery, JE Michelson, PF Mitthumsiri, W Mizuno, T Monte, C Monzani, ME Morselli, A Moskalenko, IV Murgia, S Nakamori, T Naumann-Godo, M Norris, JP Nuss, E Ohno, M Ohsugi, T Okumura, A Omodei, N Orlando, E Ozaki, M Paneque, D Parent, D Pesce-Rollins, M Pierbattista, M Piron, F Pivato, G Porter, TA Raino, S Rando, R Razzano, M Reimer, A Reimer, O Ritz, S Romani, RW Roth, M Parkinson, PMS Sgro, C Siskind, EJ Spandre, G Spinelli, P Suson, DJ Takahashi, H Tanaka, T Thayer, JG Thayer, JB Thompson, DJ Tibaldo, L Tinivella, M Torres, DF Tosti, G Troja, E Uchiyama, Y Usher, TL Vandenbroucke, J Vianello, G Vitale, V Waite, AP Winer, BL Wood, KS Wood, M Yang, Z Zimmer, S Coe, MJ Di Mille, F Edwards, PG Filipovic, MD Payne, JL Stevens, J Torres, MAP AF Ackermann, M. Ajello, M. Ballet, J. Barbiellini, G. Bastieri, D. Belfiore, A. Bellazzini, R. Berenji, B. Blandford, R. D. Bloom, E. D. Bonamente, E. Borgland, A. W. Bregeon, J. Brigida, M. Bruel, P. Buehler, R. Buson, S. Caliandro, G. A. Cameron, R. A. Caraveo, P. A. Cavazzuti, E. Cecchi, C. Celik, Oe. Charles, E. Chaty, S. Chekhtman, A. Cheung, C. C. Chiang, J. Ciprini, S. Claus, R. Cohen-Tanugi, J. Corbel, S. Corbet, R. H. D. Cutini, S. de Luca, A. den Hartog, P. R. de Palma, F. Dermer, C. D. Digel, S. W. do Couto e Silva, E. Donato, D. Drell, P. S. Drlica-Wagner, A. Dubois, R. Dubus, G. Favuzzi, C. Fegan, S. J. Ferrara, E. C. Focke, W. B. Fortin, P. Fukazawa, Y. Funk, S. Fusco, P. Gargano, F. Gasparrini, D. Gehrels, N. Germani, S. Giglietto, N. Giordano, F. Giroletti, M. Glanzman, T. Godfrey, G. Grenier, I. A. Grove, J. E. Guiriec, S. Hadasch, D. Hanabata, Y. Harding, A. K. Hayashida, M. Hays, E. Hill, A. B. Hughes, R. E. Johannesson, G. Johnson, A. S. Johnson, T. J. Kamae, T. Katagiri, H. Kataoka, J. Kerr, M. Knoedlseder, J. Kuss, M. Lande, J. Longo, F. Loparco, F. Lovellette, M. N. Lubrano, P. Mazziotta, M. N. McEnery, J. E. Michelson, P. F. Mitthumsiri, W. Mizuno, T. Monte, C. Monzani, M. E. Morselli, A. Moskalenko, I. V. Murgia, S. Nakamori, T. Naumann-Godo, M. Norris, J. P. Nuss, E. Ohno, M. Ohsugi, T. Okumura, A. Omodei, N. Orlando, E. Ozaki, M. Paneque, D. Parent, D. Pesce-Rollins, M. Pierbattista, M. Piron, F. Pivato, G. Porter, T. A. Raino, S. Rando, R. Razzano, M. Reimer, A. Reimer, O. Ritz, S. Romani, R. W. Roth, M. Parkinson, P. M. Saz Sgro, C. Siskind, E. J. Spandre, G. Spinelli, P. Suson, D. J. Takahashi, H. Tanaka, T. Thayer, J. G. Thayer, J. B. Thompson, D. J. Tibaldo, L. Tinivella, M. Torres, D. F. Tosti, G. Troja, E. Uchiyama, Y. Usher, T. L. Vandenbroucke, J. Vianello, G. Vitale, V. Waite, A. P. Winer, B. L. Wood, K. S. Wood, M. Yang, Z. Zimmer, S. Coe, M. J. Di Mille, F. Edwards, P. G. Filipovic, M. D. Payne, J. L. Stevens, J. Torres, M. A. P. CA Fermi LAT Collaboration TI Periodic Emission from the Gamma-Ray Binary 1FGL J1018.6-5856 SO SCIENCE LA English DT Article ID LARGE-AREA TELESCOPE; LS 5039; MICROQUASAR LS-5039; FERMI; MODULATION; DISCOVERY; PULSARS; CATALOG; STARS; MASS AB Gamma-ray binaries are stellar systems containing a neutron star or black hole, with gamma-ray emission produced by an interaction between the components. These systems are rare, even though binary evolution models predict dozens in our Galaxy. A search for gamma-ray binaries with the Fermi Large Area Telescope (LAT) shows that 1FGL J1018.6-5856 exhibits intensity and spectral modulation with a 16.6-day period. We identified a variable x-ray counterpart, which shows a sharp maximum coinciding with maximum gamma-ray emission, as well as an O6V((f)) star optical counterpart and a radio counterpart that is also apparently modulated on the orbital period. 1FGL J1018.6-5856 is thus a gamma-ray binary, and its detection suggests the presence of other fainter binaries in the Galaxy. C1 [Ackermann, M.; Ajello, M.; Berenji, B.; Blandford, R. D.; Bloom, E. D.; Borgland, A. W.; Buehler, R.; Cameron, R. A.; Charles, E.; Chiang, J.; Claus, R.; den Hartog, P. R.; Digel, S. W.; do Couto e Silva, E.; Drell, P. S.; Drlica-Wagner, A.; Dubois, R.; Focke, W. B.; Funk, S.; Glanzman, T.; Godfrey, G.; Hayashida, M.; Johnson, A. S.; Kamae, T.; Kerr, M.; Lande, J.; Michelson, P. F.; Mitthumsiri, W.; Monzani, M. E.; Moskalenko, I. V.; Murgia, S.; Okumura, A.; Omodei, N.; Orlando, E.; Paneque, D.; Porter, T. A.; Reimer, A.; Reimer, O.; Romani, R. W.; Tanaka, T.; Thayer, J. G.; Thayer, J. B.; Uchiyama, Y.; Usher, T. L.; Vandenbroucke, J.; Vianello, G.; Waite, A. P.; Wood, M.] Stanford Univ, Dept Phys, Kavli Inst Particle Astrophys & Cosmol, WW Hansen Expt Phys Lab, Stanford, CA 94305 USA. [Ackermann, M.; Ajello, M.; Berenji, B.; Blandford, R. D.; Bloom, E. D.; Borgland, A. W.; Buehler, R.; Cameron, R. A.; Charles, E.; Chiang, J.; Claus, R.; den Hartog, P. R.; Digel, S. W.; do Couto e Silva, E.; Drell, P. S.; Drlica-Wagner, A.; Dubois, R.; Focke, W. B.; Funk, S.; Glanzman, T.; Godfrey, G.; Hayashida, M.; Johnson, A. S.; Kamae, T.; Kerr, M.; Lande, J.; Michelson, P. F.; Mitthumsiri, W.; Monzani, M. E.; Moskalenko, I. V.; Murgia, S.; Okumura, A.; Omodei, N.; Orlando, E.; Paneque, D.; Porter, T. A.; Reimer, A.; Reimer, O.; Romani, R. W.; Tanaka, T.; Thayer, J. G.; Thayer, J. B.; Uchiyama, Y.; Usher, T. L.; Vandenbroucke, J.; Vianello, G.; Waite, A. P.; Wood, M.] Stanford Univ, SLAC Natl Accelerator Lab, Stanford, CA 94305 USA. [Ballet, J.; Chaty, S.; Corbel, S.; Grenier, I. A.; Naumann-Godo, M.; Pierbattista, M.] Univ Paris Diderot, CNRS, CEA IRFU, Lab AIM,Serv Astrophys,CEA Saclay, F-91191 Gif Sur Yvette, France. [Barbiellini, G.; Longo, F.] Ist Nazl Fis Nucl, Sez Trieste, I-34127 Trieste, Italy. [Barbiellini, G.; Longo, F.] Univ Trieste, Dipartimento Fis, I-34127 Trieste, Italy. [Bastieri, D.; Buson, S.; Rando, R.; Tibaldo, L.] Ist Nazl Fis Nucl, Sez Padova, I-35131 Padua, Italy. [Bastieri, D.; Buson, S.; Pivato, G.; Rando, R.; Tibaldo, L.] Univ Padua, Dipartimento Fis G Galilei, I-35131 Padua, Italy. [Belfiore, A.; Razzano, M.; Ritz, S.; Parkinson, P. M. Saz] Univ Calif Santa Cruz, Dept Phys, Santa Cruz Inst Particle Phys, Santa Cruz, CA 95064 USA. [Belfiore, A.; Razzano, M.; Ritz, S.; Parkinson, P. M. Saz] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. [Belfiore, A.] Univ Pavia, I-27100 Pavia, Italy. [Belfiore, A.; Caraveo, P. A.] INAF Ist Astrofis Spaziale & Fis Cosm, I-20133 Milan, Italy. [Bellazzini, R.; Bregeon, J.; Kuss, M.; Pesce-Rollins, M.; Razzano, M.; Sgro, C.; Spandre, G.; Tinivella, M.] Ist Nazl Fis Nucl, Sez Pisa, I-56127 Pisa, Italy. [Bonamente, E.; Cecchi, C.; Germani, S.; Lubrano, P.; Tosti, G.] Ist Nazl Fis Nucl, Sez Perugia, I-06123 Perugia, Italy. [Bonamente, E.; Cecchi, C.; Ciprini, S.; Germani, S.; Lubrano, P.; Tosti, G.] Univ Perugia, Dipartimento Fis, I-06123 Perugia, Italy. [Brigida, M.; de Palma, F.; Favuzzi, C.; Fusco, P.; Giglietto, N.; Giordano, F.; Loparco, F.; Monte, C.; Raino, S.; Spinelli, P.] Univ Bari, Dipartimento Fis M Merlin, I-70126 Bari, Italy. [Brigida, M.; de Palma, F.; Favuzzi, C.; Fusco, P.; Giglietto, N.; Giordano, F.; Loparco, F.; Monte, C.; Raino, S.; Spinelli, P.] Politecn Bari, I-70126 Bari, Italy. [Brigida, M.; de Palma, F.; Favuzzi, C.; Fusco, P.; Gargano, F.; Giglietto, N.; Giordano, F.; Loparco, F.; Mazziotta, M. N.; Monte, C.; Raino, S.; Spinelli, P.] Ist Nazl Fis Nucl, Sez Bari, I-70126 Bari, Italy. [Bruel, P.; Fegan, S. J.; Fortin, P.] Ecole Polytech, CNRS, IN2P3, Lab Leprince Ringuet, F-91128 Palaiseau, France. [Caliandro, G. A.; Hadasch, D.; Torres, D. F.] Inst Ciencies Espai IEEE CSIC, Barcelona 08193, Spain. [Cavazzuti, E.; Cutini, S.; Gasparrini, D.] Agenzia Spaziale Italiana ASI Sci Data Ctr, I-00044 Rome, Italy. [Celik, Oe.; Corbet, R. H. D.; Ferrara, E. C.; Gehrels, N.; Harding, A. K.; Hays, E.; McEnery, J. E.; Thompson, D. J.; Troja, E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Celik, Oe.; Donato, D.] Ctr Res & Explorat Space Sci & Technol, Greenbelt, MD 20771 USA. [Celik, Oe.; Corbet, R. H. D.] Univ Maryland Baltimore Cty, Ctr Space Sci & Technol, Baltimore, MD 21250 USA. [Chekhtman, A.] Artep Inc, Ellicott City, MD 21042 USA. [Cheung, C. C.; Johnson, T. J.] Natl Acad Sci, Natl Res Council, Washington, DC 20001 USA. [Ciprini, S.] ASI Sci Data Ctr, I-00044 Rome, Italy. [Cohen-Tanugi, J.; Nuss, E.; Piron, F.] Univ Montpellier 2, CNRS, IN2P3, Lab Universe & Particules Montpellier, Montpellier, France. [Corbel, S.] Inst Univ France, F-75005 Paris, France. [de Luca, A.] Ist Univ Super, I-27100 Pavia, Italy. [Dermer, C. D.; Grove, J. E.; Lovellette, M. N.; Wood, K. S.] USN, Res Lab, Div Space Sci, Washington, DC 20375 USA. [Donato, D.; McEnery, J. E.] Univ Maryland, Dept Phys, College Pk, MD 20742 USA. [Donato, D.; McEnery, J. E.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Dubus, G.] Univ Grenoble 1, CNRS, UMR 5274, Inst Planetol & Astrophys Grenoble,INSU, F-38041 Grenoble, France. [Fukazawa, Y.; Hanabata, Y.; Kataoka, J.; Mizuno, T.] Hiroshima Univ, Dept Phys Sci, Hiroshima 7398526, Japan. [Giroletti, M.] INAF Ist Radioastron, I-40129 Bologna, Italy. [Guiriec, S.] Univ Alabama, Ctr Space Plasma & Aeron Res, Huntsville, AL 35899 USA. [Hayashida, M.] Kyoto Univ, Grad Sch Sci, Dept Astron, Sakyo Ku, Kyoto 6068502, Japan. [Hill, A. B.; Coe, M. J.] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England. [Hughes, R. E.; Winer, B. L.] Ohio State Univ, Ctr Cosmol & Astroparticle Phys, Dept Phys, Columbus, OH 43210 USA. [Johannesson, G.] Univ Iceland, Inst Sci, IS-107 Reykjavik, Iceland. [Katagiri, H.] Ibaraki Univ, Coll Sci, Mito, Ibaraki 3108512, Japan. [Nakamori, T.] Waseda Univ, Res Inst Sci & Engn, Shinjuku Ku, Tokyo 1698555, Japan. [Knoedlseder, J.] IRAP, CNRS, F-31028 Toulouse 4, France. [Knoedlseder, J.] Univ Toulouse, UPS OMP, IRAP, GAHEC, Toulouse, France. [Morselli, A.] Ist Nazl Fis Nucl, Sez Roma Tor Vergata, I-00133 Rome, Italy. [Norris, J. P.; Vitale, V.] Boise State Univ, Dept Phys, Boise, ID 83725 USA. [Ohno, M.; Okumura, A.; Ozaki, M.] JAXA, Inst Space & Astronaut Sci, Chuo Ku, Sagamihara, Kanagawa 2525210, Japan. [Ohsugi, T.; Takahashi, H.] Hiroshima Univ, Hiroshima Astrophys Sci Ctr, Hiroshima 7398526, Japan. [Orlando, E.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Paneque, D.] Max Planck Inst Phys & Astrophys, D-80805 Munich, Germany. [Parent, D.] George Mason Univ, Coll Sci, Ctr Earth Observing & Space Res, Fairfax, VA 22030 USA. [Reimer, A.; Reimer, O.] Leopold Franzens Univ Innsbruck, Inst Astro & Teilchenphys, A-6020 Innsbruck, Austria. [Reimer, A.; Reimer, O.] Leopold Franzens Univ Innsbruck, Inst Theoret Phys, A-6020 Innsbruck, Austria. [Roth, M.] Univ Washington, Dept Phys, Seattle, WA 98195 USA. [Siskind, E. J.] NYCB Real Time Comp Inc, Lattingtown, NY 11560 USA. [Suson, D. J.] Purdue Univ Calumet, Dept Chem & Phys, Hammond, IN 46323 USA. [Torres, D. F.] ICREA, Barcelona, Spain. [Vianello, G.] CIFS, I-10133 Turin, Italy. [Vitale, V.] Univ Roma Tor Vergata, Dipartimento Fis, I-00133 Rome, Italy. [Yang, Z.; Zimmer, S.] Stockholm Univ, Dept Phys, SE-10691 Stockholm, Sweden. [Yang, Z.; Zimmer, S.] Oskar Klein Ctr Cosmoparticle Phys, SE-10691 Stockholm, Sweden. [Di Mille, F.] Las Campanas Observ, Australian Astron Observ, La Serena, Chile. [Edwards, P. G.] CSIRO Astron & Space Sci, Australia Telescope Natl Facil, Narrabri, NSW 2390, Australia. [Filipovic, M. D.; Payne, J. L.] Univ Western Sydney, Penrith, NSW 2751, Australia. [Stevens, J.] CSIRO Astron & Space Sci, Epping, NSW 1710, Australia. [Torres, M. A. P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Cheung, CC (reprint author), USN, Res Lab, Div Space Sci, Washington, DC 20375 USA. EM teddy.cheung.ctr@nrl.navy.mil; robin.corbet@nasa.gov; kerrm@stanford.edu RI Funk, Stefan/B-7629-2015; Johannesson, Gudlaugur/O-8741-2015; Loparco, Francesco/O-8847-2015; Gargano, Fabio/O-8934-2015; Moskalenko, Igor/A-1301-2007; Mazziotta, Mario /O-8867-2015; Sgro, Carmelo/K-3395-2016; Torres, Diego/O-9422-2016; Orlando, E/R-5594-2016; Thompson, David/D-2939-2012; Gehrels, Neil/D-2971-2012; Harding, Alice/D-3160-2012; Hays, Elizabeth/D-3257-2012; McEnery, Julie/D-6612-2012; lubrano, pasquale/F-7269-2012; Morselli, Aldo/G-6769-2011; Kuss, Michael/H-8959-2012; giglietto, nicola/I-8951-2012; Reimer, Olaf/A-3117-2013; Tosti, Gino/E-9976-2013; Saz Parkinson, Pablo Miguel/I-7980-2013; Ozaki, Masanobu/K-1165-2013; Rando, Riccardo/M-7179-2013 OI Chaty, Sylvain/0000-0002-5769-8601; Pesce-Rollins, Melissa/0000-0003-1790-8018; De Luca, Andrea/0000-0001-6739-687X; Giroletti, Marcello/0000-0002-8657-8852; Cutini, Sara/0000-0002-1271-2924; Gasparrini, Dario/0000-0002-5064-9495; Funk, Stefan/0000-0002-2012-0080; Johannesson, Gudlaugur/0000-0003-1458-7036; Loparco, Francesco/0000-0002-1173-5673; Gargano, Fabio/0000-0002-5055-6395; Moskalenko, Igor/0000-0001-6141-458X; Mazziotta, Mario /0000-0001-9325-4672; Torres, Diego/0000-0002-1522-9065; Caraveo, Patrizia/0000-0003-2478-8018; Sgro', Carmelo/0000-0001-5676-6214; Hill, Adam/0000-0003-3470-4834; Bastieri, Denis/0000-0002-6954-8862; Omodei, Nicola/0000-0002-5448-7577; Thompson, David/0000-0001-5217-9135; lubrano, pasquale/0000-0003-0221-4806; Morselli, Aldo/0000-0002-7704-9553; giglietto, nicola/0000-0002-9021-2888; Reimer, Olaf/0000-0001-6953-1385; FU NASA (United States); U.S. Department of Energy (United States); CEA/Irfu (France); IN2P3/CNRS (France); ASI (Italy); INFN (Italy); MEXT (Japan); KEK (Japan); JAXA (Japan); K. A. Wallenberg Foundation; Swedish Research Council; National Space Board (Sweden); CNES in France; European Community [ERC-StG-200911] FX The Fermi LAT Collaboration acknowledges support from a number of agencies and institutes for both development and the operation of the LAT as well as scientific data analysis. These include NASA and the U.S. Department of Energy (United States); CEA/Irfu and IN2P3/CNRS (France); ASI and INFN (Italy); MEXT, KEK, and JAXA (Japan); and the K. A. Wallenberg Foundation, the Swedish Research Council, and the National Space Board (Sweden). Additional support from INAF in Italy and CNES in France for science analysis during the operations phase is also gratefully acknowledged. Fermi LAT data are available from the Fermi Science Support Center (http://fermi.gsfc.nasa.gov/ssc). This work made use of data supplied by the UK Swift Science Data Centre at the University of Leicester. G. D. was supported by European Community contract ERC-StG-200911. NR 26 TC 37 Z9 37 U1 1 U2 17 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 JAN 13 PY 2012 VL 335 IS 6065 BP 189 EP 193 DI 10.1126/science.1213974 PG 6 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 875LZ UT WOS:000299033100045 ER PT J AU Andrews, SM Wilner, DJ Hughes, AM Qi, CH Rosenfeld, KA Oberg, KI Birnstiel, T Espaillat, C Cieza, LA Williams, JP Lin, SY Ho, PTP AF Andrews, Sean M. Wilner, David J. Hughes, A. M. Qi, Chunhua Rosenfeld, Katherine A. Oeberg, Karin I. Birnstiel, T. Espaillat, Catherine Cieza, Lucas A. Williams, Jonathan P. Lin, Shin-Yi Ho, Paul T. P. TI THE TW Hya DISK AT 870 mu m: COMPARISON OF CO AND DUST RADIAL STRUCTURES SO ASTROPHYSICAL JOURNAL LA English DT Article DE circumstellar matter; protoplanetary disks; stars: individual (TW Hya) ID MAIN-SEQUENCE STARS; PROTOPLANETARY DISKS; CIRCUMSTELLAR DISKS; HYDRAE ASSOCIATION; ACCRETION DISKS; SUBMILLIMETER ARRAY; PLANET FORMATION; GAS TEMPERATURE; YOUNG OBJECTS; GIANT PLANETS AB We present high-resolution (0.'' 3 = 16 AU), high signal-to-noise ratio Submillimeter Array observations of the 870 mu m (345 GHz) continuum and CO J = 3 - 2 line emission from the protoplanetary disk around TW Hya. Using continuum and line radiative transfer calculations, these data and the multiwavelength spectral energy distribution are analyzed together in the context of simple two-dimensional parametric disk structure models. Under the assumptions of a radially invariant dust population and gas-to-dust mass ratio, we are unable to simultaneously reproduce the CO and dust observations with model structures that employ either a single, distinct outer boundary or a smooth (exponential) taper at large radii. Instead, we find that the distribution of millimeter-sized dust grains in the TW Hya disk has a relatively sharp edge near 60 AU, contrary to the CO emission (and optical/ infrared scattered light) that extends to a much larger radius of at least 215 AU. We discuss some possible explanations for the observed radial distribution of millimeter-sized dust grains and the apparent CO-dust size discrepancy, and suggest that they may be hallmarks of substructure in the dust disk or natural signatures of the growth and radial drift of solids that might be expected for disks around older pre-main-sequence stars like TW Hya. C1 [Andrews, Sean M.; Wilner, David J.; Qi, Chunhua; Rosenfeld, Katherine A.; Oeberg, Karin I.; Espaillat, Catherine; Ho, Paul T. P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Hughes, A. M.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Birnstiel, T.] Univ Munich, Univ Observ Munich, D-81679 Munich, Germany. [Cieza, Lucas A.; Williams, Jonathan P.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Lin, Shin-Yi] Univ Calif San Diego, Ctr Astrophys & Space Sci, La Jolla, CA 92093 USA. [Ho, Paul T. P.] Acad Sinica, Inst Astron & Astrophys, Taipei 106, Taiwan. RP Andrews, SM (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. FU Smithsonian Institution; Academia Sinica FX We thank Mark Gurwell for his assistance with the multiepoch calibration of the SMA data, Elise Furlan and the Spitzer IRS Disks team for providing a reduced TW Hya spectrum, and an anonymous referee for thoughtful suggestions that contributed significant value to the article. We are especially grateful to Christian Brinch for his generous help with the LIME code, Kees Dullemond for technical support with the RADMC package, and Paola D'Alessio for her valuable advice on dust populations and optical constants. The Submillimeter Array (SMA) is a joint project between the Smithsonian Astrophysical Observatory and the Academia Sinica Institute of Astronomy and Astrophysics and is funded by the Smithsonian Institution and the Academia Sinica. NR 86 TC 102 Z9 102 U1 1 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JAN 10 PY 2012 VL 744 IS 2 AR 162 DI 10.1088/0004-637X/744/2/162 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 870JW UT WOS:000298666400082 ER PT J AU Bayliss, MB AF Bayliss, Matthew B. TI BROADBAND PHOTOMETRY OF 105 GIANT ARCS: REDSHIFT CONSTRAINTS AND IMPLICATIONS FOR GIANT ARC STATISTICS SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology: observations; galaxies: high-redshift; gravitational lensing: strong; large-scale structure of Universe ID LYMAN BREAK GALAXIES; STAR-FORMING GALAXIES; DIGITAL SKY SURVEY; HUBBLE DEEP FIELD; CLUSTER LENS POPULATION; DARK-MATTER HALOS; LINE-OF-SIGHT; GOODMAN SPECTROGRAPH; STELLAR POPULATION; CROSS-SECTIONS AB We measure the photometric properties of 105 giant arcs that were identified in systematic searches for galaxycluster- scale strong lenses in the Second Red- Sequence Cluster Survey and the Sloan Digital Sky Survey. The cluster lenses span 0.2 < z(l) < 1.2 in redshift, with a median (z) over bar (l) = 0.58. Using broadband color criteria we sort the entire arc sample into redshift bins based on u-g and g-r colors, and also r- z colors for the similar to 90% of arcs that have z- band data. This analysis yields broad redshift constraints with 71(-4)(+5)% of the arcs at z >= 1.0, 64(-4)(+6)% at z >= 1.4, 56(-4)(+5)% at z >= 1.9, and 21(-2)(+4)% at z >= 2.7. The remaining 29+(03)(5)% have z < 1. The inferred median redshift is <(z)over bar>(s) = 2.0 +/- 0.1, in good agreement with a previous determination from a smaller sample of brighter arcs (g less than or similar to 22.5). This agreement confirms that z(s) = 2.0 +/- 0.1 is the typical redshift for giant arcs with g less than or similar to 24 that are produced by cluster- scale strong lenses and that there is no evidence for strong evolution in the redshift distribution of arcs over a wide range of g- band magnitudes (20 <= g <= 24). Establishing that half of all giant arcs are at z greater than or similar to 2 contributes significantly toward relieving the tension between the number of arcs observed and the number expected in a.CDM cosmology, but there is considerable evidence to suggest that a discrepancy persists. Additionally, this work confirms that forthcoming large samples of giant arcs will supply the observational community with many magnified galaxies at z greater than or similar to 2. C1 [Bayliss, Matthew B.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. [Bayliss, Matthew B.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Bayliss, Matthew B.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Bayliss, Matthew B.] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. RP Bayliss, MB (reprint author), Univ Chicago, Dept Astron & Astrophys, 5640 S Ellis Ave, Chicago, IL 60637 USA. EM mbayliss@cfa.harvard.edu FU Illinois Space Grant Consortium FX Support for this work comes in part from the Illinois Space Grant Consortium in the form of a graduate fellowship. I want to first give my sincere thanks the SOAR observing and support staff for their help in obtaining the observations that drove this paper. I also want to thank Michael Gladders, David Gilbank, and Howard Yee for their work on RCS-2, Eva Wuyts for helpful discussions about giant arc photometry and SSP galaxy models, Felipe Barrientos and Mauricio Carrasco for graciously sharing unpublished spectroscopic redshifts, and Brad Holden for helpful discussion that expanded the scope of this work. I also want to thank my thesis committee members-Stephen Kent, Andrey Kravstov, and Richard Kron-for their helpful comments. Lastly, I want to thank Michael Gladders for his dedication and mentoring over the past four years. NR 81 TC 17 Z9 17 U1 1 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JAN 10 PY 2012 VL 744 IS 2 AR 156 DI 10.1088/0004-637X/744/2/156 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 870JW UT WOS:000298666400076 ER PT J AU Brown, JM Herczeg, GJ Pontoppidan, KM van Dishoeck, EF AF Brown, J. M. Herczeg, G. J. Pontoppidan, K. M. van Dishoeck, E. F. TI A 30 AU RADIUS CO GAS HOLE IN THE DISK AROUND THE HERBIG Ae STAR Oph IRS 48 SO ASTROPHYSICAL JOURNAL LA English DT Article DE planetary systems; protoplanetary disks; stars: individual (Oph IRS 48); stars: pre-main sequence ID INTERMEDIATE-MASS STARS; MAIN-SEQUENCE STARS; AE/BE STARS; PROTOPLANETARY DISK; TRANSITIONAL DISKS; MULTIPLE PLANETS; EMISSION-LINES; MOLECULAR GAS; GIANT PLANET; SPECTROSCOPY AB The physical processes leading to the disappearance of disks around young stars are not well understood. A subclass of transitional disks, the so-called cold disks with large inner dust holes, provides a crucial laboratory for studying disk dissipation processes. IRS 48 has a 30 AU radius hole previously measured from dust continuum imaging at 18.7 mu m. Using new optical spectra, we determine that IRS 48 is a pre-main-sequence A0 star. In order to characterize this disk's gas distribution, we obtained AO-assisted Very Large Telescope CRIRES high-resolution (R similar to 100,000) spectra of the CO fundamental rovibrational band at 4.7 mu m. All CO emission, including that from isotopologues and vibrationally excited molecules, is off-source and peaks at 30 AU. The gas is thermally excited to a rotational temperature of 260 K and is also strongly UV pumped, showing a vibrational excitation temperature of similar to 5000 K. We model the kinematics and excitation of the gas and posit that the CO emission arises from the dust hole wall. Prior imaging of UV-excited polycyclic aromatic hydrocarbon molecules, usually a gas tracer, within the hole makes the large CO hole even more unexpected. C1 [Brown, J. M.; Herczeg, G. J.; van Dishoeck, E. F.] Max Planck Inst Extraterr Phys, D-85741 Garching, Germany. [Brown, J. M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Pontoppidan, K. M.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [van Dishoeck, E. F.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. RP Brown, JM (reprint author), Max Planck Inst Extraterr Phys, Postfach 1312, D-85741 Garching, Germany. EM joannabrown@cfa.harvard.edu FU Smithsonian Astrophysical Observatory; Netherlands Organization for Scientific Research (NWO); Netherlands Research School for Astronomy (NOVA) FX The authors thank Vincent Geers for providing the reduced data from his 2007 paper and Eric Mamajek for a discussion of the cloud membership of IRS 48. J. M. Brown acknowledges the Smithsonian Astrophysical Observatory for support from an SMA fellowship. Astrochemistry at Leiden is supported by a Spinoza grant from the Netherlands Organization for Scientific Research (NWO) and by the Netherlands Research School for Astronomy (NOVA) grants. NR 49 TC 26 Z9 26 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 JAN 10 PY 2012 VL 744 IS 2 AR 116 DI 10.1088/0004-637X/744/2/116 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 870JW UT WOS:000298666400036 ER PT J AU Brown, WR Kilic, M Prieto, CA Kenyon, SJ AF Brown, Warren R. Kilic, Mukremin Allende Prieto, Carlos Kenyon, Scott J. TI THE ELM SURVEY. III. A SUCCESSFUL TARGETED SURVEY FOR EXTREMELY LOW MASS WHITE DWARFS SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries: close; Galaxy: stellar content; stars: individual (SDSS J011210.25+183503.7, SDSS J015213.77+074913.9, SDSS J144342.74+150938.6, SDSS J151826.68+065813.2, SDSS J174140.49+652638.7, SDSS J184037.78+642312.3); stars: neutron; white dwarfs ID DOUBLE DEGENERATE SYSTEM; DIGITAL SKY SURVEY; BINARY NLTT 11748; AM CVN STARS; HYPERVELOCITY STAR; SPY PROJECT; WILL MERGE; DISCOVERY; HELIUM; SUPERNOVAE AB Extremely low mass (ELM) white dwarfs (WDs) with masses < 0.25 M(circle dot) are rare objects that result from compact binary evolution. Here, we present a targeted spectroscopic survey of ELM WD candidates selected by color. The survey is 71% complete and has uncovered 18 new ELM WDs. Of the seven ELM WDs with follow-up observations, six are short-period binaries and four have merger times less than 5 Gyr. The most intriguing object, J1741+6526, likely has either a pulsar companion or a massive WD companion making the system a possible supernova Type Ia or an Ia progenitor. The overall ELM survey has now identified 19 double degenerate binaries with < 10 Gyr merger times. The significant absence of short orbital period ELM WDs at cool temperatures suggests that common envelope evolution creates ELM WDs directly in short period systems. At least one-third of the merging systems are halo objects, thus ELM WD binaries continue to form and merge in both the disk and the halo. C1 [Brown, Warren R.; Kenyon, Scott J.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. [Kilic, Mukremin] Univ Oklahoma, Homer L Dodge Dept Phys & Astron, Norman, OK 73019 USA. [Allende Prieto, Carlos] Inst Astrofis Canarias, E-38205 Tenerife, Spain. [Allende Prieto, Carlos] Univ La Laguna, Dept Astrofis, E-38206 Tenerife, Spain. RP Brown, WR (reprint author), Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA. EM wbrown@cfa.harvard.edu; kilic@ou.edu; callende@iac.es; skenyon@cfa.harvard.edu OI Kenyon, Scott/0000-0003-0214-609X FU Smithsonian Institution; NASA FX We thank M. Alegria, J. McAfee, and A. Milone for their assistance with observations obtained at the MMT Observatory, and P. Berlind and M. Calkins for their assistance with observations obtained at the Fred Lawrence Whipple Observatory. We thank A. Piro for a discussion about hot ELM WDs. This project makes use of data products from the Sloan Digital Sky Survey, which is managed by the Astrophysical Research Consortium for the Participating Institutions. This research makes use of NASA's Astrophysics Data System Bibliographic Services. This work was supported in part by the Smithsonian Institution. M. K. was supported in part by NASA through the Spitzer Space Telescope Fellowship Program, under an award from CalTech. NR 46 TC 52 Z9 52 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JAN 10 PY 2012 VL 744 IS 2 AR 142 DI 10.1088/0004-637X/744/2/142 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 870JW UT WOS:000298666400062 ER PT J AU Bussmann, RS Dey, A Armus, L Brown, MJI Desai, V Gonzalez, AH Jannuzi, BT Melbourne, J Soifer, BT AF Bussmann, R. S. Dey, Arjun Armus, L. Brown, M. J. I. Desai, V. Gonzalez, A. H. Jannuzi, B. T. Melbourne, J. Soifer, B. T. TI THE STAR FORMATION HISTORIES OF z similar to 2 DUST-OBSCURED GALAXIES AND SUBMILLIMETER-SELECTED GALAXIES SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: evolution; galaxies: fundamental parameters; galaxies: high-redshift; galaxies: stellar content ID STELLAR POPULATION SYNTHESIS; ULTRALUMINOUS INFRARED GALAXIES; SPITZER-SPACE-TELESCOPE; INITIAL MASS FUNCTION; DEGREE EXTRAGALACTIC SURVEY; GIANT BRANCH STARS; ARRAY CAMERA IRAC; WIDE-FIELD SURVEY; TP-AGB MODELS; HIGH-REDSHIFT AB The Spitzer Space Telescope has identified a population of ultraluminous infrared galaxies (ULIRGs) at z similar to 2 that may play an important role in the evolution of massive galaxies. We measure the stellar masses (M-*) of two populations of Spitzer-selected ULIRGs that have extremely red R-[24] colors (dust-obscured galaxies, or DOGs) and compare our results with submillimeter-selected galaxies (SMGs). One set of 39 DOGs has a local maximum in their mid-infrared (mid-IR) spectral energy distribution (SED) at rest frame 1.6 mu m associated with stellar emission ("bump DOGs"), while the other set of 51 DOGs have power-law mid-IR SEDs that are typical of obscured active galactic nuclei ("power-law DOGs"). We measure M-* by applying Charlot & Bruzual stellar population synthesis models to broadband photometry in the rest-frame ultraviolet, optical, and near-infrared of each of these populations. Assuming a simple stellar population and a Chabrier initial mass function, we find that power-law DOGs and bump DOGs are on average a factor of 2 and 1.5 more massive than SMGs, respectively (median and inter-quartile M values for SMGs, bump DOGs, and power-law DOGs are log(M-*/M-circle dot) = 10.42(-0.36)(+0.42), 10.62(-0.32)(+0.36), and 10.71(-0.34)(+0.40), respectively). More realistic star formation histories drawn from two competing theories for the nature of ULIRGs at z similar to 2 (major merger versus smooth accretion) can increase these mass estimates by up to 0.5 dex. A comparison of our stellar masses with the instantaneous star formation rate (SFR) in these z similar to 2 ULIRGs provides a preliminary indication supporting high SFRs for a given M-*, a situation that arises more naturally in major mergers than in smooth accretion-powered systems. C1 [Bussmann, R. S.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Bussmann, R. S.] Univ Arizona, Dept Astron, Steward Observ, Tucson, AZ 85721 USA. [Dey, Arjun; Jannuzi, B. T.] Natl Opt Astron Observ, Tucson, AZ 85719 USA. [Armus, L.; Desai, V.; Soifer, B. T.] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. [Brown, M. J. I.] Monash Univ, Sch Phys, Clayton, Vic 3800, Australia. [Gonzalez, A. H.] Univ Florida, Dept Astron, Gainesville, FL 32611 USA. [Melbourne, J.; Soifer, B. T.] CALTECH, Div Phys Math & Astron, Pasadena, CA 91125 USA. RP Bussmann, RS (reprint author), Harvard Smithsonian Ctr Astrophys, 160 Concord Ave, Cambridge, MA 02138 USA. EM rbussmann@cfa.harvard.edu RI Brown, Michael/B-1181-2015 OI Brown, Michael/0000-0002-1207-9137 FU HST [GO10890, GO11195]; NASA through Space Telescope Science Institute [HST-GO10890, HST-GO11195]; NASA [NAS5-26555]; NOAO FX R.S.B. gratefully acknowledges financial assistance from HST grants GO10890 and GO11195, without which this research would not have been possible. Support for Programs HST-GO10890 and HST-GO11195 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. The research activities of A. D. and B.T.J. are supported by NOAO, which is operated by the Association of Universities for Research in Astronomy (AURA, inc.) under a cooperative agreement with the National Science Foundation. NR 93 TC 20 Z9 20 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JAN 10 PY 2012 VL 744 IS 2 AR 150 DI 10.1088/0004-637X/744/2/150 PG 34 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 870JW UT WOS:000298666400070 ER PT J AU Grav, T Mainzer, AK Bauer, J Masiero, J Spahr, T McMillan, RS Walker, R Cutri, R Wright, E Eisenhardt, PR Blauvelt, E DeBaun, E Elsbury, D Gautier, T Gomillion, S Hand, E Wilkins, A AF Grav, T. Mainzer, A. K. Bauer, J. Masiero, J. Spahr, T. McMillan, R. S. Walker, R. Cutri, R. Wright, E. Eisenhardt, P. R. Blauvelt, E. DeBaun, E. Elsbury, D. Gautier, T. Gomillion, S. Hand, E. Wilkins, A. TI WISE/NEOWISE OBSERVATIONS OF THE HILDA POPULATION: PRELIMINARY RESULTS SO ASTROPHYSICAL JOURNAL LA English DT Article DE infrared: planetary systems; minor planets, asteroids: general; surveys ID ASTEROID SPECTROSCOPIC SURVEY; THERMAL-MODEL CALIBRATION; INFRARED-SURVEY-EXPLORER; LATE HEAVY BOMBARDMENT; NEAR-EARTH ASTEROIDS; SOLAR-SYSTEM; ORBITAL ARCHITECTURE; SURFACE-COMPOSITION; TROJAN ASTEROIDS; GIANT PLANETS AB We present the preliminary analysis of 1023 known asteroids in the Hilda region of the solar system observed by the NEOWISE component of the Wide-field Infrared Survey Explorer (WISE). The sizes of the Hildas observed range from similar to 3 to 200 km. We find no size-albedo dependency as reported by other projects. The albedos of our sample are low, with a weighted mean value of p(V) = 0.055 +/- 0.018, for all sizes sampled by the NEOWISE survey. We observed a significant fraction of the objects in the two known collisional families in the Hilda population. It is found that the Hilda collisional family is brighter, with a weighted mean albedo of p(V) = 0.061 +/- 0.011, than the general population and dominated by D-type asteroids, while the Schubart collisional family is darker, with a weighted mean albedo of p(V) = 0.039 +/- 0.013. Using the reflected sunlight in the two shortest WISE bandpasses, we are able to derive a method for taxonomic classification of similar to 10% of the Hildas detected in the NEOWISE survey. For the Hildas with diameter larger than 30 km, there are 67(-15)(+7) % D-type asteroids and 26(-5)(+17) % C-/P-type asteroids (with the majority of these being P-types). C1 [Grav, T.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Mainzer, A. K.; Bauer, J.; Masiero, J.; Eisenhardt, P. R.; Blauvelt, E.; DeBaun, E.; Elsbury, D.; Gautier, T.; Gomillion, S.; Hand, E.; Wilkins, A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Bauer, J.; Cutri, R.] CALTECH, Ctr Infrared Proc & Anal, Pasadena, CA 91125 USA. [Spahr, T.] Harvard Smithsonian Ctr Astrophys, Minor Planet Ctr, Cambridge, MA 02138 USA. [McMillan, R. S.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA. [Walker, R.] Monterey Inst Res Astron, Marina, CA 93933 USA. [Wright, E.] UCLA Astron, Los Angeles, CA 90095 USA. [Wilkins, A.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. RP Grav, T (reprint author), Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. EM tgrav@pha.jhu.edu OI Blauvelt, Erin/0000-0002-2944-5818; Masiero, Joseph/0000-0003-2638-720X FU National Aeronautics and Space Administration; Planetary Science Division of the National Aeronautics and Space Administration FX 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 publication also makes use of data products from NEOWISE, which is a project of the Jet Propulsion Laboratory/California Institute of Technology, funded by the Planetary Science Division of the National Aeronautics and Space Administration. We gratefully acknowledge the extraordinary services specific to NEOWISE contributed by the International Astronomical Union's Minor Planet Center, operated by the Harvard-Smithsonian Center for Astrophysics, and the Central Bureau for Astronomical Telegrams, operated by Harvard University. We also thank the worldwide community of dedicated amateur and professional astronomers devoted to minor planet follow-up observations. This research has made use the NASA/IPAC Infrared Science Archive, which is operated by the Jet Propulsion Laboratory/California Institute of Technology, under contract with the National Aeronautics and Space Administration. NR 52 TC 24 Z9 24 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JAN 10 PY 2012 VL 744 IS 2 AR 197 DI 10.1088/0004-637X/744/2/197 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 870JW UT WOS:000298666400116 ER PT J AU Hainline, LJ Morgan, CW Beach, JN Kochanek, CS Harris, HC Tilleman, T Fadely, R Falco, EE Le, TX AF Hainline, Laura J. Morgan, Christopher W. Beach, Joseph N. Kochanek, C. S. Harris, Hugh C. Tilleman, Trudy Fadely, Ross Falco, Emilio E. Le, Truong X. TI A NEW MICROLENSING EVENT IN THE DOUBLY IMAGED QUASAR Q 0957+561 SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion; accretion disks; gravitational lensing: micro; gravitational lensing: strong; quasars: individual (Q0957+561) ID GRAVITATIONAL LENS 0957+561; TIME-DELAY; ACCRETION DISK; LIGHT CURVES; X-RAY; EMISSION REGIONS; MASS FUNCTION; PG 1115+080; Q0957+561; QSO-0957+561 AB We present evidence for ultraviolet/optical microlensing in the gravitationally lensed quasar Q 0957+561. We combine new measurements from our optical monitoring campaign at the United States Naval Observatory, Flagstaff, with measurements from the literature and find that the time-delay-corrected r-band flux ratio m(A) - m(B) has increased by similar to 0.1 mag over a period of five years beginning in the fall of 2005. We apply our Monte Carlo microlensing analysis procedure to the composite light curves, obtaining a measurement of the optical accretion disk size, log{(r(s)/cm)[ cos(i)/0.5](1/2)} = 16.2 +/- 0.5, that is consistent with the quasar accretion disk size-black hole mass relation. C1 [Hainline, Laura J.; Morgan, Christopher W.; Beach, Joseph N.; Le, Truong X.] USN Acad, Dept Phys, Annapolis, MD 21402 USA. [Kochanek, C. S.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. [Harris, Hugh C.; Tilleman, Trudy] US Naval Observ, Flagstaff Stn, Flagstaff, AZ 86001 USA. [Fadely, Ross] Haverford Coll, Dept Astron, Haverford, PA 19041 USA. [Falco, Emilio E.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Hainline, LJ (reprint author), USN Acad, Dept Phys, 572C Holloway Rd, Annapolis, MD 21402 USA. EM hainline@usna.edu; cmorgan@usna.edu; m110480@usna.edu; ckochanek@astronomy.ohio-state.edu; hch@nofs.navy.mil; trudy@nofs.navy.mil; rfadely@haverford.edu; falco@cfa.harvard.edu; m113678@usna.edu FU National Science Foundation [AST-0907848, AST-0708082, AST-1009756]; Research Corporation for Science Advancement; Chandrasekhar X-Ray Center [11700501] FX The authors thank L. Goicoechea, E. Turner, and R. McMillan for their assistance in obtaining historical photometric data for Q0957. We also thank the anonymous referee for suggestions which improved the data presented in this paper. This material is based upon work supported by the National Science Foundation under grant no AST-0907848 (to C. W. M.), AST-0708082, and AST-1009756 (to C. S. K.). C. W. M. also gratefully acknowledges support from the Research Corporation for Science Advancement and Chandrasekhar X-Ray Center award 11700501. NR 53 TC 10 Z9 10 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JAN 10 PY 2012 VL 744 IS 2 AR 104 DI 10.1088/0004-637X/744/2/104 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 870JW UT WOS:000298666400024 ER PT J AU Parker, AH Kavelaars, JJ AF Parker, Alex H. Kavelaars, J. J. TI COLLISIONAL EVOLUTION OF ULTRA-WIDE TRANS-NEPTUNIAN BINARIES SO ASTROPHYSICAL JOURNAL LA English DT Article DE Kuiper belt: general; planets and satellites: formation ID KUIPER-BELT OBJECTS; SIZE DISTRIBUTION; TIDAL FRICTION; MINOR PLANETS; KOZAI CYCLES; ORBITS; SEARCH; BODIES AB The widely separated, near-equal mass binaries hosted by the cold classical Kuiper Belt are delicately bound and subject to disruption by many perturbing processes. We use analytical arguments and numerical simulations to determine their collisional lifetimes given various impactor size distributions and include the effects of mass loss and multiple impacts over the lifetime of each system. These collisional lifetimes constrain the population of small (R greater than or similar to 1 km) objects currently residing in the Kuiper Belt and confirm that the size distribution slope at small size cannot be excessively steep-likely q less than or similar to 3.5. We track mutual semimajor axis, inclination, and eccentricity evolution through our simulations and show that it is unlikely that the wide binary population represents an evolved tail of the primordially tight binary population. We find that if the wide binaries are a collisionally eroded population, their primordial mutual orbit planes must have preferred to lie in the plane of the solar system. Finally, we find that current limits on the size distribution at small radii remain high enough that the prospect of detecting dust-producing collisions in real time in the Kuiper Belt with future optical surveys is feasible. C1 [Parker, Alex H.] Univ Victoria, Dept Astron, Victoria, BC, Canada. [Parker, Alex H.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Kavelaars, J. J.] Natl Res Council Canada, Herzberg Inst Astrophys, Saanich, BC, Canada. RP Parker, AH (reprint author), Univ Victoria, Dept Astron, Victoria, BC, Canada. EM alexhp@uvic.ca FU NSF-GRFP [DGE-0836694] FX Alex Parker is funded by the NSF-GRFP award DGE-0836694. We acknowledge the constructive conversations with Jean-Marc Petit and Wesley Fraser regarding the details of our collisional code, and with Mark Booth with respect to dust generation in collisions. We also thank Stephen Gwyn and John Ouellette for their assistance with the computational challenges of this work. NR 27 TC 12 Z9 12 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JAN 10 PY 2012 VL 744 IS 2 AR 139 DI 10.1088/0004-637X/744/2/139 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 870JW UT WOS:000298666400059 ER PT J AU Winston, E Wolk, SJ Bourke, TL Megeath, ST Gutermuth, R Spitzbart, B AF Winston, E. Wolk, S. J. Bourke, T. L. Megeath, S. T. Gutermuth, R. Spitzbart, B. TI SPITZER OBSERVATIONS OF BOW SHOCKS AND OUTFLOWS IN RCW 38 SO ASTROPHYSICAL JOURNAL LA English DT Article DE circumstellar matter; infrared: stars; ISM: jets and outflows; stars: pre-main sequence; stars: winds, outflows; X-rays: ISM; X-rays: stars ID FORMING REGION RCW-38; YOUNG STELLAR OBJECTS; X-RAY-EMISSION; PLANETARY-NEBULAE; INFRARED SOURCES; CARINA-NEBULA; MASSIVE STARS; O-STARS; GAS; DISCOVERY AB We report Spitzer observations of five newly identified bow shocks in the massive star-forming region RCW 38. Four are visible at Infrared Array Camera (IRAC) wavelengths, the fifth is only visible at 24 mu m. Chandra X-ray emission indicates that winds from the central O5.5 binary, IRS 2, have caused an outflow to the northeast and southwest of the central subcluster. The southern lobe of hot ionized gas is detected in X-rays; shocked gas and heated dust from the shock front are detected with Spitzer at 4.5 and 24 mu m. The northern outflow may have initiated the present generation of star formation, based on the filamentary distribution of the protostars in the central subcluster. Further, the bow-shock driving star, YSO 129, is photo-evaporating a pillar of gas and dust. No point sources are identified within this pillar at near-to mid-IR wavelengths. We also report on IRAC 3.6 and 5.8 mu m observations of the cluster DBS2003-124, northeast of RCW 38, where 33 candidate young stellar objects (YSOs) are identified. One star associated with the cluster drives a parsec-scale jet. Two Herbig-Haro objects associated with the jet are visible at IRAC and Multiband Imaging Photometer for Spitzer (MIPS) wavelengths. The jet extends over a distance of similar to 3 pc. Assuming a velocity of 100 km s(-1) for the jet material gives an age of 3 x 10(4) yr, indicating that the star (and cluster) are likely to be very young, with a similar or possibly younger age than RCW 38, and that star formation is ongoing in the extended RCW 38 region. C1 [Winston, E.] ESA ESTEC SRE SA, NL-2201 AZ Noordwijk, Netherlands. [Wolk, S. J.; Bourke, T. L.; Spitzbart, B.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Megeath, S. T.] Univ Toledo, Dept Phys & Astron, Ritter Observ, Toledo, OH 43606 USA. [Gutermuth, R.] Smith Coll, Coll Astron Dept 5, Northampton, MA 01027 USA. [Gutermuth, R.] Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA. RP Winston, E (reprint author), ESA ESTEC SRE SA, Keplerlaan 1, NL-2201 AZ Noordwijk, Netherlands. EM ewinston@rssd.esa.int OI Wolk, Scott/0000-0002-0826-9261 FU National Aeronautics and Space Administration [1407, 1256790, 960541, NAS5-26555]; National Science Foundation; National Aeronautics and Space Administration's Earth Science Technology Office [NCC5-626]; NASA through HST from Space Telescope Science Institute [11123] FX This work is based on observations made with the Spitzer Space Telescope (PID 20127), which is operated by the Jet Propulsion Laboratory, California Institute of Technology under NASA contract 1407. Support for this work was provided by NASA through contract 1256790 issued by JPL/Caltech. Support for the IRAC instrument was provided by NASA through contract 960541 issued by JPL. This publication makes use of data products from the Two Micron All Sky Survey, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology, funded by the National Aeronautics and Space Administration and the National Science Foundation. This research has made use of the NASA/IPAC Infrared Science Archive, which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. This research made use of Montage, funded by the National Aeronautics and Space Administration's Earth Science Technology Office, Computation Technologies Project, under Cooperative Agreement Number NCC5-626 between NASA and the California Institute of Technology. Montage is maintained by the NASA/IPAC Infrared Science Archive. T.L.B. acknowledges support from NASA through a grant for HST program 11123 from the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Incorporated, under NASA contract NAS5-26555. NR 44 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 J9 ASTROPHYS J JI Astrophys. J. PD JAN 10 PY 2012 VL 744 IS 2 AR 126 DI 10.1088/0004-637X/744/2/126 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 870JW UT WOS:000298666400046 ER EF